FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Mckay, CP Garcia, VP AF McKay, Christopher P. Parro Garcia, Victor TI HOW TO SEARCH FOR LIFE ON MARS SO SCIENTIFIC AMERICAN LA English DT Article C1 [McKay, Christopher P.] NASA, Ames Res Ctr, Pasadena, CA 91109 USA. RP Mckay, CP (reprint author), NASA, Ames Res Ctr, Pasadena, CA 91109 USA. NR 0 TC 0 Z9 0 U1 0 U2 21 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 0036-8733 J9 SCI AM JI Sci.Am. PD JUN PY 2014 VL 310 IS 6 BP 44 EP 49 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AH6JG UT WOS:000336236600031 PM 25004574 ER PT J AU Rubinstein, R Zhou, Y AF Rubinstein, Robert Zhou, Ye TI Constant Flux States in Anisotropic Turbulence SO JOURNAL OF FLUIDS ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article ID ISOTROPIC TURBULENCE AB An elementary closure theory is used to compute the scaling of anisotropic contributions to the correlation function in homogeneous turbulence. These contributions prove to decay with wave-number more rapidly than the energy spectrum; this property is sometimes called the "recovery of isotropy" at small scales and is a key hypothesis of the Kolmogorov theory. Although comparisons with a more comprehensive theory suggest that the present theory is too crude, its elementary character makes the scaling analysis straightforward. The analysis reveals some characteristic features of anisotropic turbulence, including "angular" energy transfer in wavevector space. C1 [Rubinstein, Robert] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. [Zhou, Ye] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. RP Rubinstein, R (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. EM r.rubinstein@nasa.gov; zhou3@llnl.gov NR 12 TC 0 Z9 0 U1 0 U2 3 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0098-2202 EI 1528-901X J9 J FLUID ENG-T ASME JI J. Fluids Eng.-Trans. ASME PD JUN PY 2014 VL 136 IS 6 AR 060914 DI 10.1115/1.4026283 PG 3 WC Engineering, Mechanical SC Engineering GA AH2KW UT WOS:000335951200015 ER PT J AU Shebalin, JV AF Shebalin, John V. TI Temperature and Entropy in Ideal Magnetohydrodynamic Turbulence SO JOURNAL OF FLUIDS ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article ID BROKEN ERGODICITY; MAGNETIC-FIELDS; ABSOLUTE EQUILIBRIUM; HELICITY; DYNAMO AB Fourier analysis of incompressible, homogeneous magnetohydrodynamic (MHD) turbulence produces a model dynamical system on which to perform numerical experiments. Statistical methods are used to understand the results of ideal (i.e., nondissipative) MHD turbulence simulations, with the goal of finding those aspects that survive the introduction of dissipation. This statistical mechanics is based on a Boltzmannlike probability density function containing three "inverse temperatures," one associated with each of the three ideal invariants: energy, cross helicity, and magnetic helicity. However, these inverse temperatures are seen to be functions of a single parameter that may defined as the "temperature" in a statistical and thermodynamic sense: the average magnetic energy per Fourier mode. Here, we discuss temperature and entropy in ideal MHD turbulence and their use in understanding numerical experiments and physical observations. C1 NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. RP Shebalin, JV (reprint author), NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. EM john.v.shebalin@nasa.gov NR 25 TC 2 Z9 2 U1 0 U2 0 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0098-2202 EI 1528-901X J9 J FLUID ENG-T ASME JI J. Fluids Eng.-Trans. ASME PD JUN PY 2014 VL 136 IS 6 AR 060901 DI 10.1115/1.4025674 PG 5 WC Engineering, Mechanical SC Engineering GA AH2KW UT WOS:000335951200002 ER PT J AU Zelensky, NP Lemoine, FG Chinn, DS Melachroinos, S Beckley, BD Beall, JW Bordyugov, O AF Zelensky, Nikita P. Lemoine, Frank G. Chinn, Douglas S. Melachroinos, Stavros Beckley, Brian D. Beall, Jennifer Wiser Bordyugov, Oleg TI Estimated SLR station position and network frame sensitivity to time-varying gravity SO JOURNAL OF GEODESY LA English DT Article DE SLR; Time-varying gravity; LAGEOS; Precise orbit determination; Terrestrial reference frame ID PRECISION ORBIT DETERMINATION; GEOCENTER MOTION; FIELD MODELS; SEA-LEVEL; JASON-2; GPS; REDISTRIBUTION; ALTIMETRY; MISSIONS; SYSTEM AB This paper evaluates the sensitivity of ITRF2008-based satellite laser ranging (SLR) station positions estimated weekly using LAGEOS-1/2 data from 1993 to 2012 to non-tidal time-varying gravity (TVG). Two primary methods for modeling TVG from degree-2 are employed. The operational approach applies an annual GRACE-derived field, and IERS recommended linear rates for five coefficients. The experimental approach uses low-order/degree coefficients estimated weekly from SLR and DORIS processing of up to 11 satellites (tvg4x4). This study shows that the LAGEOS-1/2 orbits and the weekly station solutions are sensitive to more detailed modeling of TVG than prescribed in the current IERS standards. Over 1993-2012 tvg4x4 improves SLR residuals by 18 % and shows 10 % RMS improvement in station stability. Tests suggest that the improved stability of the tvg4x4 POD solution frame may help clarify geophysical signals present in the estimated station position time series. The signals include linear and seasonal station motion, and motion of the TRF origin, particularly in Z. The effect on both POD and the station solutions becomes increasingly evident starting in 2006. Over 2008-2012, the tvg4x4 series improves SLR residuals by 29 %. Use of the GRGS RL02 series shows similar improvement in POD. Using tvg4x4, secular changes in the TRF origin Z component double over the last decade and although not conclusive, it is consistent with increased geocenter rate expected due to continental ice melt. The test results indicate that accurate modeling of TVG is necessary for improvement of station position estimation using SLR data. C1 [Zelensky, Nikita P.; Chinn, Douglas S.; Melachroinos, Stavros; Beckley, Brian D.; Bordyugov, Oleg] SGT Inc, Div Sci, Greenbelt, MD 20770 USA. [Lemoine, Frank G.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Beall, Jennifer Wiser] Emergent Space Technol, Greenbelt, MD 20770 USA. RP Zelensky, NP (reprint author), SGT Inc, Div Sci, 7701 Greenbelt Rd, Greenbelt, MD 20770 USA. EM nzelensky@sgt-inc.com; frank.g.lemoine@nasa.gov; douglas.s.chinn@nasa.gov; SMelachroinos@sgt-inc.com; Brian.D.Beckley@nasa.gov; jennifer.beall@emergentspace.com; OBordyugov@sgt-inc.com RI Lemoine, Frank/D-1215-2013 FU International Laser Ranging Service (ILRS); U.S. National Aeronautics and Space Administration (NASA) under the program "IDS Program in Mean Sea Level" FX We acknowledge the International Laser Ranging Service (ILRS) for its support and leadership in providing satellite laser ranging data (Pearlman et al. 2002). Many thanks to Dave Rowlands and Scott Luthcke of NASA/GSFC and Mark Torrence of SGT for the useful discussions. We thank the three anonymous reviewers for their very constructive help evaluating this paper. This research was supported by the U.S. National Aeronautics and Space Administration (NASA) under the program "IDS Program in Mean Sea Level." NR 75 TC 6 Z9 6 U1 1 U2 11 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0949-7714 EI 1432-1394 J9 J GEODESY JI J. Geodesy PD JUN PY 2014 VL 88 IS 6 BP 517 EP 537 DI 10.1007/s00190-014-0701-4 PG 21 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA AH3KC UT WOS:000336021100001 ER PT J AU Georgiadis, NJ Yoder, DA Vyas, MA Engblom, WA AF Georgiadis, Nicholas J. Yoder, Dennis A. Vyas, Manan A. Engblom, William A. TI Status of turbulence modeling for hypersonic propulsion flowpaths SO THEORETICAL AND COMPUTATIONAL FLUID DYNAMICS LA English DT Article DE Turbulence; Hypersonic propulsion; Scramjet; Turbulence model ID LARGE-EDDY SIMULATION; LAYER INTERACTIONS; DENSITY-FUNCTION; REACTING FLOWS; COMBUSTION; COMPRESSIBILITY; EQUATION AB This report provides an assessment of current turbulent flow calculation methods for hypersonic propulsion flowpaths, particularly the scramjet engine. Emphasis is placed on Reynolds-averaged Navier-Stokes (RANS) methods, but some discussion of newer methods such as large eddy simulation (LES) is also provided. The report is organized by considering technical issues throughout the scramjet-powered vehicle flowpath, including laminar-to-turbulent boundary layer transition, shock wave/turbulent boundary layer interactions, scalar transport modeling (specifically the significance of turbulent Prandtl and Schmidt numbers), and compressible mixing. Unit problems are primarily used to conduct the assessment. In the combustor, results from calculations of a direct connect supersonic combustion experiment are also used to address the effects of turbulence model selection and in particular settings for the turbulent Prandtl and Schmidt numbers. It is concluded that RANS turbulence modeling shortfalls are still a major limitation to the accuracy of hypersonic propulsion simulations, whether considering individual components or an overall system. Newer methods such as LES-based techniques may be promising, but are not yet at a maturity to be used routinely by the hypersonic propulsion community. The need for fundamental experiments to provide data for turbulence model development and validation is discussed. C1 [Georgiadis, Nicholas J.; Yoder, Dennis A.; Vyas, Manan A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Engblom, William A.] Embry Riddle Aeronaut Univ, Daytona Beach, FL 32114 USA. RP Georgiadis, NJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM georgiadis@nasa.gov FU Test Resource Management Center (TRMC); Test and Evaluation/Science and Technology (TE/ST) Program; T&E/S&T Program through the High Speed Systems Test area; NASA Fundamental Aeronautics Program-Hypersonic Project FX The authors would like to thank Test Resource Management Center (TRMC) and the Test and Evaluation/Science and Technology (T&E/S&T) Program for their support. This work was funded by the T&E/S&T Program through the High Speed Systems Test area and the NASA Fundamental Aeronautics Program-Hypersonic Project. NR 88 TC 2 Z9 2 U1 2 U2 32 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0935-4964 EI 1432-2250 J9 THEOR COMP FLUID DYN JI Theor. Comput. Fluid Dyn. PD JUN PY 2014 VL 28 IS 3 BP 295 EP 318 DI 10.1007/s00162-013-0316-z PG 24 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA AH1VE UT WOS:000335908500003 ER PT J AU Yingst, RA Cohen, BA Hynek, B Schmidt, ME Schrader, C Rodriguez, A AF Yingst, R. A. Cohen, B. A. Hynek, B. Schmidt, M. E. Schrader, C. Rodriguez, A. TI Testing Mars Exploration Rover-inspired operational strategies for semi-utonomous rovers on the moon II: The GeoHeuristic operational Strategies Test in Alaska SO ACTA ASTRONAUTICA LA English DT Article DE MER; Science operations; Rover; Analog; Field test ID PLANETARY SCIENCE; MERIDIANI-PLANUM; WATER; MISSION; IMPACT; ICE; SURFACE; CRATER AB We used MER-derived semi-autonomous rover science operations strategies to determine best practices suitable for remote semi-autonomous lunar rover geology. Two field teams studied two glacial moraines as analogs for potential ice-bearing lunar regolith. At each site a Rover Team commanded a human rover to execute observations based on common MER sequences; the resulting data were used to identify and characterize targets of interest. A Tiger Team followed the Rover Team using traditional terrestrial field methods, and the results of the two teams were compared. Narrowly defined goals that can be addressed using cm-scale or coarser resolution may be met sufficiently by the operational strategies adapted from MER survey mode. When reconnaissance is the primary goal, the strategies tested are necessary but not sufficient. Further, there may be a set of optimal observations for such narrowly defined, hypothesis-driven science goals, such that collecting further data would result in diminishing returns. We confirm results of previous tests that indicated systematic observations might improve efficiency during strategic planning, and improve science output during data analysis. This strategy does not markedly improve the rate at which a science team can ingest data to feed back into tactical decision-making. Other methods should be tested to separate the strategic and tactical processes, and to build in time for data analysis. (C) 2014 The Authors. Published by Elsevier Ltd. on behalf of IAA. All rights reserved. C1 [Yingst, R. A.; Rodriguez, A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Cohen, B. A.; Schrader, C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Hynek, B.] Univ Colorado, Lab Atmospher & Space Phys & Geol Sci, Boulder, CO 80309 USA. [Schmidt, M. E.] Brock Univ, Dept Earth Sci, St Catharines, ON L2S 3A1, Canada. [Schrader, C.] Colorado Coll, Dept Geol, Colorado Springs, CO 80903 USA. RP Yingst, RA (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA. EM barbara.a.cohen@nasa.gov; hynek@lasp.colorado.edu; mschmidt2@brocku.ca; christian.schrader@coloradocollege.edu; yingst@psi.edu FU Moon and Mars Analog Mission Activities Program [NNGO5GL66G] FX We gratefully acknowledge the efforts of field assistant Ross Nova, our "rover" for the field test. Professor John Luczaj provided valuable insight in post-field discussions, and Dr. Dean Eppler's and Professor Tracy Gregg's constructive comments greatly improved the manuscript. This research was supported through Moon and Mars Analog Mission Activities Program grant NNGO5GL66G to RAY. NR 56 TC 2 Z9 2 U1 0 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUN-JUL PY 2014 VL 99 BP 24 EP 36 DI 10.1016/j.actaastro.2014.01.019 PG 13 WC Engineering, Aerospace SC Engineering GA AG7QD UT WOS:000335612000003 ER PT J AU Marlier, ME Voulgarakis, A Shindell, DT Faluvegi, G Henry, CL Randerson, JT AF Marlier, Miriam E. Voulgarakis, Apostolos Shindell, Drew T. Faluvegi, Greg Henry, Candise L. Randerson, James T. TI The role of temporal evolution in modeling atmospheric emissions from tropical fires SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Fire emissions; Atmospheric modeling; Air quality ID BIOMASS BURNING EMISSIONS; FUTURE CLIMATE SIMULATIONS; SATELLITE-OBSERVATIONS; AIR-POLLUTION; GLOBAL-MODEL; AEROSOLS; DEFORESTATION; GASES; VARIABILITY; RESOLUTION AB Fire emissions associated with tropical land use change and maintenance influence atmospheric composition, air quality, and climate. In this study, we explore the effects of representing fire emissions at daily versus monthly resolution in a global composition-climate model. We find that simulations of aerosols are impacted more by the temporal resolution of fire emissions than trace gases such as carbon monoxide or ozone. Daily-resolved datasets concentrate emissions from fire events over shorter time periods and allow them to more realistically interact with model meteorology, reducing how often emissions are concurrently released with precipitation events and in turn increasing peak aerosol concentrations. The magnitude of this effect varies across tropical ecosystem types, ranging from smaller changes in modeling the low intensity, frequent burning typical of savanna ecosystems to larger differences when modeling the short-term, intense fires that characterize deforestation events. The utility of modeling fire emissions at a daily resolution also depends on the application, such as modeling exceedances of particulate matter concentrations over air quality guidelines or simulating regional atmospheric heating patterns. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Marlier, Miriam E.; Henry, Candise L.] Columbia Univ, Lamont Doherty Earth Observ, New York, NY 10027 USA. [Marlier, Miriam E.; Henry, Candise L.] Columbia Univ, Dept Earth & Environm Sci, New York, NY 10027 USA. [Voulgarakis, Apostolos] Imperial Coll London, Dept Phys, London, England. [Shindell, Drew T.; Faluvegi, Greg] NASA, Goddard Inst Space Studies, Washington, DC USA. [Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. RP Marlier, ME (reprint author), Columbia Univ, Lamont Doherty Earth Observ, New York, NY 10027 USA. EM marlier@ldeo.columbia.edu RI Shindell, Drew/D-4636-2012; OI Voulgarakis, Apostolos/0000-0002-6656-4437 FU NSF; NASA MAP; ACMAP; NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS); NASA [NNX11AF96G] FX The authors would like to thank Ruth DeFries for helpful discussions regarding this work. We acknowledge funding support from the NSF Graduate Research Fellowship Program, NASA MAP and ACMAP programs, the NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS), and NASA grant NNX11AF96G. NR 41 TC 8 Z9 8 U1 0 U2 22 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD JUN PY 2014 VL 89 BP 158 EP 168 DI 10.1016/j.atmosenv.2014.02.039 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AH1IT UT WOS:000335874500018 ER PT J AU Chudnovsky, AA Koutrakis, P Kloog, I Melly, S Nordio, F Lyapustin, A Wang, YJ Schwartz, J AF Chudnovsky, Alexandra A. Koutrakis, Petros Kloog, Itai Melly, Steven Nordio, Francesco Lyapustin, Alexei Wang, Yujie Schwartz, Joel TI Fine particulate matter predictions using high resolution Aerosol Optical Depth (AOD) retrievals SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Particulate matter; PM2.5; Aerosol Optical Depth (AOD); High resolution aerosol retrieval; MAIAC; Intra-urban pollution; Variability in PM2.5 levels; Scales of pollution ID LAND-USE REGRESSION; PM2.5 CONCENTRATIONS; AIR-POLLUTION; UNITED-STATES; EFFECTS MODELS; SATELLITE; EXPOSURE; MORTALITY AB To date, spatial-temporal patterns of particulate matter (PM) within urban areas have primarily been examined using models. On the other hand, satellites extend spatial coverage but their spatial resolution is too coarse. In order to address this issue, here we report on spatial variability in PM levels derived from high 1 km resolution AOD product of Multi-Angle Implementation of Atmospheric Correction (MAIAC) algorithm developed for MODIS satellite. We apply day-specific calibrations of AOD data to predict PM2.5 concentrations within the New England area of the United States. To improve the accuracy of our model, land use and meteorological variables were incorporated. We used inverse probability weighting (IPW) to account for nonrandom missingness of AOD and nested regions within days to capture spatial variation. With this approach we can control for the inherent day-to-day variability in the AOD-PM2.5 relationship, which depends on time-varying parameters such as particle optical properties, vertical and diurnal concentration profiles and ground surface reflectance among others. Out-of-sample "ten-fold" cross-validation was used to quantify the accuracy of model predictions. Our results show that the model-predicted PM2.5 mass concentrations are highly correlated with the actual observations, with out-of-sample R-2 of 0.89. Furthermore, our study shows that the model captures the pollution levels along highways and many urban locations thereby extending our ability to investigate the spatial patterns of urban air quality, such as examining exposures in areas with high traffic. Our results also show high accuracy within the cities of Boston and New Haven thereby indicating that MAIAC data can be used to examine intra-urban exposure contrasts in PM2.5 levels. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Chudnovsky, Alexandra A.; Koutrakis, Petros; Kloog, Itai; Melly, Steven; Nordio, Francesco; Schwartz, Joel] Harvard Univ, Sch Publ Hlth, Dept Environm Hlth, Boston, MA 02115 USA. [Chudnovsky, Alexandra A.] Tel Aviv Univ, Dept Geog & Human Environm, IL-69978 Tel Aviv, Israel. [Kloog, Itai] Ben Gurion Univ Negev, Dept Geog & Environm Dev, IL-84105 Beer Sheva, Israel. [Lyapustin, Alexei] NASA, GEST UMBC, Goddard Space Flight Ctr, Baltimore, MD USA. [Wang, Yujie] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. RP Chudnovsky, AA (reprint author), Tel Aviv Univ, Dept Geog & Human Environm, IL-69978 Tel Aviv, Israel. EM achudnov@post.tau.ac.il RI Lyapustin, Alexei/H-9924-2014 OI Lyapustin, Alexei/0000-0003-1105-5739 FU USEPA [RD 83479801]; NASA Terra and Aqua Science Program FX This work was made possible by USEPA grant RD 83479801. Its contents are solely the responsibility of the grantee and do not necessarily represent the official views of the USEPA. Further, USEPA does not endorse the purchase of any commercial products or services mentioned in the publication. The support for A. Lyapustin and Y. Wang is provided by the NASA Terra and Aqua Science Program. The authors wish to thank the anonymous reviewers for their constructive comments. Inspiring discussions with Prof. Alex Kostinski from Michigan Technological University and Dr. Eran Ben Elia from Tel-Aviv University are greatly acknowledged. NR 41 TC 22 Z9 24 U1 5 U2 60 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD JUN PY 2014 VL 89 BP 189 EP 198 DI 10.1016/j.atmosenv.2014.02.019 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AH1IT UT WOS:000335874500021 ER PT J AU Kolev, OI Reschke, MF AF Kolev, Ognyan I. Reschke, Millard F. TI Internally versus externally mediated triggers in the acquisition of visual targets in the horizontal plane SO BEHAVIOURAL BRAIN RESEARCH LA English DT Article DE Target acquisition; Internal trigger; External trigger; Delay ID EYE-HEAD COORDINATION; MOVEMENTS; MONKEYS; SHIFTS AB In an operational setting acquisition of visual targets using both head and eye movements can be driven by memorized sequence of commands - internal triggering (IT) or by commands issued through secondary operator - external triggering (ET). The primary objective of our research was to examine differences in target acquisition using IT compared with ET. Using a forced time optimal strategy eight subjects were required to acquire targets with angular offsets of +/- 20 degrees, 30 degrees and 60 degrees along the horizontal plane in both IT and ET conditions. The data showed that the eye/head latency difference in IT condition is longer than that for ET, the target acquisition time is also longer for IT commands. Consistent with this finding were similar results when examining the peak head velocity and peak head acceleration. Under IT protocol head amplitude is higher than when using ET. In conclusion, the study demonstrates that the pattern of performance of target acquisition task is influenced by the way of command triggering. (C) 2014 Elsevier B.V. All rights reserved. C1 [Kolev, Ognyan I.; Reschke, Millard F.] NASA, Lyndon B Johnson Space Ctr, Neurosci Labs, Houston, TX 77058 USA. RP Kolev, OI (reprint author), NASA, Lyndon B Johnson Space Ctr, Neurosci Labs, Houston, TX 77058 USA. EM kolev_ogi@yahoo.com NR 14 TC 2 Z9 2 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-4328 EI 1872-7549 J9 BEHAV BRAIN RES JI Behav. Brain Res. PD JUN 1 PY 2014 VL 266 BP 131 EP 136 DI 10.1016/j.bbr.2014.03.003 PG 6 WC Behavioral Sciences; Neurosciences SC Behavioral Sciences; Neurosciences & Neurology GA AH0JN UT WOS:000335805300016 PM 24613978 ER PT J AU Padula, SA Gaydosh, D Saleeb, A Dhakal, B AF Padula, S. A., II Gaydosh, D. Saleeb, A. Dhakal, B. TI Transients and Evolution in NiTi SO EXPERIMENTAL MECHANICS LA English DT Article DE Shape memory alloy; Evolution; Transients; Stabilization; Attraction; Load-bias ID SHAPE-MEMORY ALLOY; STRAIN; TRANSFORMATION AB Many of the applications that seek to utilize shape memory alloys for their unique set of properties inevitably must deal, on some level, with the dimensional instability that is inherent to these materials under cyclic thermomechanical loading conditions. As a result, a better understanding of the transient and evolutionary behavior of a shape memory alloy is critical to both the successful design of useful actuation systems and development of accurate material models that can adequately capture the types of dimensional instability that can arise during component design. To this end, a set of experiments were conducted wherein the temperature cycling excursion was held fixed while the applied stress was varied. The results indicated that the extent of strain evolution produced under the initially applied stress has a significant impact on both the amount of transient that is observed as well as the rate of evolution observed under subsequent stress levels. In particular, lowering the applied stress to 50 MPa after cycling under an initial stress of 75 MPa did not stabilize the strain. However, lowering the applied stress to 50 MPa after cycling under an initial stress of 150 MPa produced a nearly saturated strain/temperature response. The thermomechanical observations are discussed in terms of the nature of strain evolution and its connection to the concept of a local/global minimization of the energy of the system, however, the exact mechanisms associated with these strain evolutions were not determined. C1 [Padula, S. A., II] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Gaydosh, D.] Ohio Aerosp Inst, Cleveland, OH 44142 USA. [Saleeb, A.; Dhakal, B.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA. RP Padula, SA (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM Santo.A.Padula@nasa.gov NR 24 TC 2 Z9 2 U1 1 U2 8 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0014-4851 EI 1741-2765 J9 EXP MECH JI Exp. Mech. PD JUN PY 2014 VL 54 IS 5 BP 709 EP 715 DI 10.1007/s11340-013-9840-4 PG 7 WC Materials Science, Multidisciplinary; Mechanics; Materials Science, Characterization & Testing SC Materials Science; Mechanics GA AG9TG UT WOS:000335762100001 ER PT J AU Misra, S de Matthaeis, P AF Misra, Sidharth de Matthaeis, Paolo TI Passive Remote Sensing and Radio Frequency Interference (RFI): An Overview of Spectrum Allocations and RFI Management Algorithms SO IEEE GEOSCIENCE AND REMOTE SENSING MAGAZINE LA English DT Editorial Material C1 [Misra, Sidharth] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [de Matthaeis, Paolo] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Misra, S (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 23 TC 5 Z9 5 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2168-6831 J9 IEEE GEOSC REM SEN M JI IEEE Geosci. Remote Sens. Mag. PD JUN PY 2014 VL 2 IS 2 BP 68 EP 73 DI 10.1109/MGRS.2014.2320879 PG 6 WC Geochemistry & Geophysics; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Remote Sensing; Imaging Science & Photographic Technology GA V45PU UT WOS:000209829300011 ER PT J AU Moreno-Madrinan, MJ Crosson, WL Eisen, L Estes, SM Estes, MG Hayden, M Hemmings, SN Irwin, DE Lozano-Fuentes, S Monaghan, AJ Quattrochi, D Welsh-Rodriguez, CM Zielinski-Gutierrez, E AF Moreno-Madrinan, Max J. Crosson, William L. Eisen, Lars Estes, Sue M. Estes, Maurice G., Jr. Hayden, Mary Hemmings, Sarah N. Irwin, Dan E. Lozano-Fuentes, Saul Monaghan, Andrew J. Quattrochi, Dale Welsh-Rodriguez, Carlos M. Zielinski-Gutierrez, Emily TI Correlating Remote Sensing Data with the Abundance of Pupae of the Dengue Virus Mosquito Vector, Aedes aegypti, in Central Mexico SO ISPRS INTERNATIONAL JOURNAL OF GEO-INFORMATION LA English DT Article DE MODIS; TRMM; DEM; Aqua; remote sensing; elevation; mosquito; rainfall; temperature ID LIFE TABLE MODEL; RIO-DE-JANEIRO; CLIMATE-CHANGE; INFECTIOUS-DISEASES; HELMINTH INFECTIONS; POTENTIAL INFLUENCE; BORNE DISEASES; UNITED-STATES; HUMAN HEALTH; VARIABILITY AB Using a geographic transect in Central Mexico, with an elevation/climate gradient, but uniformity in socio-economic conditions among study sites, this study evaluates the applicability of three widely-used remote sensing (RS) products to link weather conditions with the local abundance of the dengue virus mosquito vector, Aedes aegypti (Ae. aegypti). Field-derived entomological measures included estimates for the percentage of premises with the presence of Ae. aegypti pupae and the abundance of Ae. aegypti pupae per premises. Data on mosquito abundance from field surveys were matched with RS data and analyzed for correlation. Daily daytime and nighttime land surface temperature (LST) values were obtained from Moderate Resolution Imaging Spectroradiometer (MODIS)/Aqua cloud-free images within the four weeks preceding the field survey. Tropical Rainfall Measuring Mission (TRMM)-estimated rainfall accumulation was calculated for the four weeks preceding the field survey. Elevation was estimated through a digital elevation model (DEM). Strong correlations were found between mosquito abundance and RS-derived night LST, elevation and rainfall along the elevation/climate gradient. These findings show that RS data can be used to predict Ae. aegypti abundance, but further studies are needed to define the climatic and socio-economic conditions under which the correlations observed herein can be assumed to apply. C1 [Moreno-Madrinan, Max J.] Indiana Univ, IUPUI, Fairbanks Sch Publ Hlth, Dept Environm Hlth, Indianapolis, IN 46202 USA. [Crosson, William L.; Hemmings, Sarah N.] USRA, Inst Sci & Technol, Huntsville, AL 35805 USA. [Eisen, Lars; Lozano-Fuentes, Saul] Colorado State Univ, Dept Microbiol Immunol & Pathol, Ft Collins, CO 80523 USA. [Estes, Sue M.; Estes, Maurice G., Jr.] Univ Alabama, Earth & Syst Sci Ctr, Huntsville, AL 35805 USA. [Hayden, Mary; Monaghan, Andrew J.] Natl Ctr Atmospher Res, Res Applicat Lab, Boulder, CO 80307 USA. [Hemmings, Sarah N.] NASA Headquarters, Div Earth Sci, Appl Sci Program, Washington, DC 20024 USA. [Irwin, Dan E.; Quattrochi, Dale] NASA Marshall Space Flight Ctr, Earth Sci, Huntsville, AL 35811 USA. [Welsh-Rodriguez, Carlos M.] Veracruz Univ, Ctr Earth Sci, Xalapa 91090, Veracruz, Mexico. [Zielinski-Gutierrez, Emily] Ctr Dis Control & Prevent, Div Vector Borne Dis, Natl Ctr Emerging & Zoonot Infect Dis, Ft Collins, CO 80521 USA. RP Moreno-Madrinan, MJ (reprint author), Indiana Univ, IUPUI, Fairbanks Sch Publ Hlth, Dept Environm Hlth, Indianapolis, IN 46202 USA. EM mmorenom@iu.edu; bill.crosson@nasa.gov; lars.eisen@colostate.edu; sue.m.estes@nasa.gov; maury.estes@nsstc.uah.edu; monaghan@ucar.edu; sarah.n.hemmings@nasa.gov; daniel.irwin@nasa.gov; saul.lozano-fuentes@colostate.edu; mhayden@ucar.edu; dale.quattrochi@nasa.gov; cwelsh@uv.mx; Ebz0@cdc.gov OI Monaghan, Andrew/0000-0002-8170-2359 FU National Aeronautic and Space Administration (NASA); National Science Foundation (NSF); NASA through ROSES: Earth Science Applications Feasibility Studies: Public Health [A.31]; NASA [10-PHFEAS10-0010]; NSF [GEO-1010204]; SERVIR FX This study was funded by grants from the National Aeronautic and Space Administration (NASA) and the National Science Foundation (NSF). The NASA funds were granted through ROSES-2010: Earth Science Applications Feasibility Studies: Public Health (A.31); and to the Applied Earth Sciences group at the Marshall Space Flight Center (MSFC) (10-PHFEAS10-0010). The NSF funds were granted to the University Corporation for Atmospheric Research (GEO-1010204). The National Center for Atmospheric Research is partially funded by NSF. A partial contribution was provided by an appointment to the NASA Postdoctoral Program at the Marshall Space Flight Center/National Space Science and Technology Center/NASA Global Hydrology and Climate Center in Huntsville, AL, USA; administered by Oak Ridge Associated Universities through a contract with NASA. We express our appreciation to Douglas Rickman and Mohammad Z. Al-Hamdan for their guidance in the processing of remote sensing applications, as well as to SERVIR for providing logistics and support. We thank Gina Wade for helping with the proposal. We also thank Carolina Ochoa-Martinez and Berenice Tapia-Santos for running the field teams and to Kevin Kobylinski and Chris Uejio for helping out in the field. Lastly but not the least we thank the students from Veracruz University who helped with the field work completing the survey and collecting the in situ data. NR 61 TC 1 Z9 2 U1 2 U2 11 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2220-9964 J9 ISPRS INT J GEO-INF JI ISPRS Int. Geo-Inf. PD JUN PY 2014 VL 3 IS 2 BP 732 EP 749 DI 10.3390/ijgi3020732 PG 18 WC Geography, Physical; Remote Sensing SC Physical Geography; Remote Sensing GA CO1RO UT WOS:000358933100018 ER PT J AU Thomas-Keprta, KL Clemett, SJ Messenger, S Ross, DK Le, L Rahman, Z McKay, DS Gibson, EK Gonzalez, C Peabody, W AF Thomas-Keprta, Kathie L. Clemett, Simon J. Messenger, Scott Ross, Daniel K. Le, Loan Rahman, Zia McKay, David S. Gibson, Everett K., Jr. Gonzalez, Carla Peabody, William TI Organic matter on the Earth's Moon SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID INTERPLANETARY DUST PARTICLES; SINGLE-PHOTON IONIZATION; RAMAN-SPECTROSCOPY; AMORPHOUS-CARBON; GRAPHITE; METEORITES; ORIGIN; IMPACT; WATER; IDENTIFICATION AB Carbonaceous matter on the surfaces of black pyroclastic beads, collected from Shorty crater during the Apollo 17 mission, represents the first identification of complex organic material associated with any lunar sample. We report the chemical, physical and isotopic properties of this organic matter that together support a pre-terrestrial origin. We suggest the most probable source is through the accretion of exogenous meteoritic kerogen from micrometeorite impacts into the lunar regolith. Abiotic organic matter has been continuously delivered to the surfaces of the terrestrial planets and their moons by accretion of asteroidal and cometary material. Determining the nature, distribution and evolution of such matter in the lunar regolith has important implications for understanding the prebiotic chemical inventory of the terrestrial planets. C1 [Thomas-Keprta, Kathie L.; Clemett, Simon J.; Ross, Daniel K.; Le, Loan; Rahman, Zia; Gonzalez, Carla] NASA, Lyndon B Johnson Space Ctr, Jacobs JETS, Houston, TX 77058 USA. [Messenger, Scott; McKay, David S.; Gibson, Everett K., Jr.] NASA, Lyndon B Johnson Space Ctr, KR, Houston, TX 77058 USA. [Peabody, William] Keyence, Microanal Grp, Dallas, TX 75252 USA. RP Thomas-Keprta, KL (reprint author), NASA, Lyndon B Johnson Space Ctr, Jacobs JETS, Mail Code KR,Bldg 31, Houston, TX 77058 USA. FU NASA [11 COS11-0049] FX Funding was provided by the NASA Cosmochemistry program, grant 11 COS11-0049. We thank L. Watts and J. Allton for their contribution to the history of Apollo sample 74220. We express our sincere gratitude to Dr. Scott Kopetz and Dr. George Chang and their staffs for their support. We also thank S. Keprta, N. Keprta, M. Walheim, S. Wentworth, O. Clemett and C. Clemett for their continued encouragment. We thank the reviewers for comments that improved the quality of the manuscript. We gratefully acknowledge the guidance and friendship of world-renowned lunar scientist, Dr. David McKay, who passed away on February 19, 2013. NR 67 TC 10 Z9 10 U1 1 U2 32 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 JUN 1 PY 2014 VL 134 BP 1 EP 15 DI 10.1016/j.gca.2014.02.047 PG 48 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AG0WM UT WOS:000335136400001 ER PT J AU Hallis, LJ Ishii, HA Bradley, JP Taylor, GJ AF Hallis, L. J. Ishii, H. A. Bradley, J. P. Taylor, G. J. TI Transmission electron microscope analyses of alteration phases in martian meteorite MIL 090032 SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID AQUEOUS ALTERATION; ALTERATION ASSEMBLAGES; ANTARCTIC METEORITES; MINERAL ASSEMBLAGES; NAKHLA METEORITE; SNC METEORITE; IGNEOUS ROCKS; MARS; RANGE; SOILS AB The nakhlite group of martian meteorites found in the Antarctic contain varying abundances of both martian and terrestrial secondary alteration phases. The aim of this study was to use transmission electron microscopy (TEM) to compare martian and terrestrial alteration embodied within a single nakhlite martian meteorite find - MIL 090032. Martian alteration veins in MIL 090032 are composed of poorly ordered Fe-smectite phyllosilicate. This poorly-ordered smectite appears to be equivalent to the nanocrystalline phyllosilicate/hydrated amorphous gel phase previously described in the martian alteration veins of other nakhlites. Chemical differences in this nanocrystalline phyllosilicate between different nakhlites imply localised alteration, which occurred close to the martian surface in MIL 090032. Both structurally and compositionally the nakhlite nanocrystalline phyllosilicate shows similarities to the amorphous/poorly ordered phase recently discovered in martian soil by the Mars Curiosity Rover at Rocknest, Gale Crater. Terrestrially derived alteration phases in MIL 090032 include jarosite and gypsum, amorphous silicates, and Fe-oxides and hydroxides. Similarities between the mineralogy and chemistry of the MIL 090032 terrestrial and martian alteration phases suggest the alteration conditions on Mars were similar to those in the Antarctic. At both sites a small amount of fluid at low temperatures infiltrated the rock and became acidic as a result of the conversion of Fe2+ to Fe3+ under oxidising conditions. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Hallis, L. J.; Taylor, G. J.] Univ Hawaii, Inst Astron, NASA Astrobiol Inst, Honolulu, HI 96822 USA. [Hallis, L. J.; Taylor, G. J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Ishii, H. A.; Bradley, J. P.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. RP Hallis, LJ (reprint author), Univ Hawaii, Inst Astron, NASA Astrobiol Inst, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM lydh@higp.hawaii.edu FU National Aeronautics and Space Administration through the NASA Astrobiology Institute, Office of Space Science [NNA09-DA77A]; U. S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344] FX This material is based upon work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement No. NNA09-DA77A, issued through the Office of Space Science. A portion of this work was performed under the auspices of the U. S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. We thank the NASA Johnson Space Center for allocation of the Miller Range nakhlite thin-sections, and Eric Hellebrand and Nick Teslich for their assistance with EMP analysis and FIB section preparation, respectively. Hitesh Changela is thanked for his helpful suggestions relating to nakhlite iddingsite fluid evolution. Martin Lee, John Bridges and one anonymous reviewer are thanked for their helpful suggestions, as is the Associate Editor Wolf Uwe Reimold. NR 64 TC 7 Z9 7 U1 1 U2 20 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 JUN 1 PY 2014 VL 134 BP 275 EP 288 DI 10.1016/j.gca.2014.02.007 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AG0WM UT WOS:000335136400016 ER PT J AU Kim, HJ Liou, MS AF Kim, Hyoungjin Liou, Meng-Sing TI Adaptive directional local search strategy for hybrid evolutionary multiobjective optimization SO APPLIED SOFT COMPUTING LA English DT Article DE Evolutionary multiobjective optimization; Memetic algorithms; Directional operator; Adaptive local search ID MEMETIC ALGORITHMS; ADAPTATION AB A novel adaptive local search method is developed for hybrid evolutionary multiobjective algorithms (EMOA) to improve convergence to the Pareto front in multiobjective optimization. The concepts of local and global effectiveness of a local search operator are suggested for dynamic adjustment of adaptation parameters. Local effectiveness is measured by quantitative comparison of improvements in convergence made by local and genetic operators based on a composite objective. Global effectiveness is determined by the ratio of number of local search solutions to genetic search solutions in the nondominated solution set. To be consistent with the adaptation strategy, a new directional local search operator, eLS (efficient Local Search), minimizing the composite objective function is designed. The search direction is determined using a centroid solution of existing neighbor solutions without making explicit calculations of gradient information. The search distance of eLS decreases adaptively as the optimization process converges. Performances of hybrid methods NSGA-II + eLS are compared with the baseline NSGA-II and NSGA-II + HCS1 for multiobjective test problems, such as ZDT and DTLZ functions. The neighborhood radius and local search probability are selected as adaptation parameters. Results show that the present adaptive local search strategy can provide significant convergence enhancement from the baseline EMOA by dynamic adjustment of adaptation parameters monitoring the properties of multiobjective problems on the fly. (C) 2014 Elsevier B.V. All rights reserved. C1 [Kim, Hyoungjin] Sci Applicat Int Corp, Cleveland, OH 44135 USA. [Liou, Meng-Sing] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Kim, HJ (reprint author), MS 5-10,21000 Brookpark Rd, Cleveland, OH 44135 USA. EM hyoungjinkim1@gmail.com FU NASA's Fixed Wing Project of the Fundamental Aeronautics Program FX The authors are grateful for the support by the NASA's Fixed Wing Project of the Fundamental Aeronautics Program. NR 47 TC 14 Z9 15 U1 0 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1568-4946 EI 1872-9681 J9 APPL SOFT COMPUT JI Appl. Soft. Comput. PD JUN PY 2014 VL 19 BP 290 EP 311 DI 10.1016/j.asoc.2014.07.019 PG 22 WC Computer Science, Artificial Intelligence; Computer Science, Interdisciplinary Applications SC Computer Science GA AF5QU UT WOS:000334768800027 ER PT J AU Chesley, SR Farnocchia, D Nolan, MC Vokrouhlicky, D Chodas, PW Milani, A Spoto, F Rozitis, B Benner, LAM Bottke, WF Busch, MW Emery, JP Howell, ES Lauretta, DS Margot, JL Taylor, PA AF Chesley, Steven R. Farnocchia, Davide Nolan, Michael C. Vokrouhlicky, David Chodas, Paul W. Milani, Andrea Spoto, Federica Rozitis, Benjamin Benner, Lance A. M. Bottke, William F. Busch, Michael W. Emery, Joshua P. Howell, Ellen S. Lauretta, Dante S. Margot, Jean-Luc Taylor, Patrick A. TI Orbit and bulk density of the OSIRIS-REx target Asteroid (101955) Bennu SO ICARUS LA English DT Article DE Near-Earth objects; Orbit determination; Celestial mechanics; Asteroids, dynamics; Radar observations ID NEAR-EARTH ASTEROIDS; THERMAL INFRARED OBSERVATIONS; MAIN BELT; CELESTIAL MECHANICS; ASTROMETRIC MASSES; MUTUAL ORBITS; 99942 APOPHIS; 1999 RQ(36); YARKOVSKY; RADAR AB The target asteroid of the OSIRIS-REx asteroid sample return mission, (101955) Bennu (formerly 1999 RQ(36)), is a half-kilometer near-Earth asteroid with an extraordinarily well constrained orbit. An extensive data set of optical astrometry from 1999 to 2013 and high-quality radar delay measurements to Bennu in 1999, 2005, and 2011 reveal the action of the Yarkovsky effect, with a mean semimajor axis drift rate da/dt = (-19.0 0.1) x 10(-4) au/Myr or 284 +/- 1.5 m/year. The accuracy of this result depends critically on the fidelity of the observational and dynamical model. As an example, neglecting the relativistic perturbations of the Earth during close approaches affects the orbit with 3 sigma significance in da/dt. The orbital deviations from purely gravitational dynamics allow us to deduce the acceleration of the Yarkovsky effect, while the known physical characterization of Bennu allows us to independently model the force due to thermal emissions. The combination of these two analyses yields a bulk density of rho = 1260 +/- 70 kg/m(3), which indicates a macroporosity in the range 40 +/- 10% for the bulk densities of likely analog meteorites, suggesting a rubble-pile internal structure. The associated mass estimate is (7.8 +/- 0.9) x 10(10) kg and GM = 5.2 +/- 0.6 m(3)/s(2). Bennu's Earth close approaches are deterministic over the interval 1654-2135, beyond which the predictions are statistical in nature. In particular, the 2135 close approach is likely within the lunar distance and leads to strong scattering and numerous potential impacts in subsequent years, from 2175 to 2196. The highest individual impact probability is 9.5 x 10(-5) in 2196, and the cumulative impact probability is 3.7 x 10(-4), leading to a cumulative Palermo Scale of -1.70. (C) 2014 Elsevier Inc. All rights reserved. C1 [Chesley, Steven R.; Farnocchia, Davide; Chodas, Paul W.; Benner, Lance A. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nolan, Michael C.; Howell, Ellen S.; Taylor, Patrick A.] Arecibo Observ, Arecibo, PR 00612 USA. [Vokrouhlicky, David] Charles Univ Prague, Prague, Czech Republic. [Milani, Andrea; Spoto, Federica] Univ Pisa, Pisa, Italy. [Rozitis, Benjamin] Open Univ, Milton Keynes MK7 6AA, Bucks, England. [Bottke, William F.] Southwest Res Inst, Boulder, CO 80302 USA. [Busch, Michael W.] SETI Inst, Mountain View, CA 94043 USA. [Emery, Joshua P.] Univ Tennessee, Knoxville, TN 37996 USA. [Lauretta, Dante S.] Univ Arizona, Tucson, AZ 85721 USA. [Margot, Jean-Luc] Univ Calif Los Angeles, Los Angeles, CA 90295 USA. RP Chesley, SR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM steve.chesley@jpl.nasa.gov RI Margot, Jean-Luc/A-6154-2012; OI Margot, Jean-Luc/0000-0001-9798-1797; Nolan, Michael/0000-0001-8316-0680 NR 61 TC 51 Z9 51 U1 4 U2 16 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUN PY 2014 VL 235 BP 5 EP 22 DI 10.1016/j.icarus.2014.02.020 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG3BU UT WOS:000335291600002 ER PT J AU Hicks, MD Buratti, BJ Lawrence, KJ Hillier, J Li, JY Reddy, V Schroder, S Nathues, A Hoffmann, M Le Corre, L Duffard, R Zhao, HB Raymond, C Russell, C Roatsch, T Jaumann, R Rhoades, H Mayes, D Barajas, T Truong, TT Foster, J McAuley, A AF Hicks, Michael D. Buratti, Bonnie J. Lawrence, Kenneth J. Hillier, John Li, Jian-Yang Reddy, Vishnu Schroeder, Stefan Nathues, Andreas Hoffmann, Martin Le Corre, Lucille Duffard, Rene Zhao, Hai-Bin Raymond, Carol Russell, Christopher Roatsch, Thomas Jaumann, Ralf Rhoades, Heath Mayes, Deronda Barajas, Tzitlaly Thien-Tin Truong Foster, James McAuley, Amanda TI Spectral diversity and photometric behavior of main-belt and near-Earth vestoids and (4) Vesta: A study in preparation for the Dawn encounter SO ICARUS LA English DT Article DE Asteroid Vesta; Near-Earth objects; Photometry; Spectroscopy ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; DIGITAL SKY SURVEY; V-TYPE ASTEROIDS; BASALTIC ASTEROIDS; HED METEORITES; MINERALOGICAL ANALYSIS; RADIATIVE-TRANSFER; PHASE-II; SATELLITES; OBJECTS AB In anticipation of the Dawn Mission to 4 Vesta, we conducted a ground-based campaign of Bessel BVRI filter photometry of five V-type near-Earth asteroids over a wide range of solar phase angles. We also obtained medium-resolution optical spectroscopy (0.38 mu m < lambda < 0.92 mu m; R similar to 500) of sixteen near-Earth and main-belt V-type asteroids in order to investigate their spectral diversity and to draw connections between spacecraft data of Vesta and V-type asteroids. Our disk-integrated photometry extended the excursion in solar phase angle beyond the maximum of 24 degrees available from Earth for Vesta to 87 degrees, which is more typical of the geometry during the Dawn approach and mapping phases. The majority of our broad-band observations were obtained at the JPL 0.6-m Table Mountain Observatory but multiple nights were also contributed by the Calar Alto 1.2-m and 2.2-m telescopes, as well as by the Purple Mountain 1-m Schmidt. Our results include a determination of rotation periods for 4 asteroids, identification of a binary candidate and four new V-type asteroids, including a confirmation of two main-belt V-type asteroids beyond the Jupiter 1:3 resonance (Cruikshank, D.P., Tholen, DJ., Bell, J.F., Hartmann, W.K., Brown, R.H. [1991]. Icarus 89,1-13; Lazzaro, D. et al. [2000]. Science 288, 2033-2035; Roig, F., Gil-Hutton, R.[20061. Icarus 183(2), 411-419; Moskovitz, N.A., Jedicke, R., Gaidos, E., Willman, M., Nesvorny, D., Fevig, R., Ivezic, Z. [2008]. Icarus 198,77-90). This latter finding supports the hypothesis that some vestoids may be crustal fragments of a disrupted basaltic parent body compositionally similar to 4 Vesta. We also obtained rotationally resolved medium resolution spectra of Vesta during the Dawn orbit insertion phase, which will be valuable for calibration and comparison of spacecraft data. Modeling of a composite V-type asteroid phase curve yielded a generic photometric model for V asteroids. We also find that a significant amount of the spectral diversity in the V class comes from changes in solar phase angle. A fit of a composite solar phase curve containing our vestoid observations, previously published groundbased observations of Vesta, and early disk-integrated Dawn observations show important differences with other asteroids. The macroscopic surface roughness of V-type asteroids is significantly larger than that of C-type or S-types (Helfenstein, P., Veverka, J. [1989]. Physical characterization of asteroid surfaces from photometric analysis. In: Binzel, R., Gehrels, T., Matthews, M.S. (Eds.), Asteroids II. University of Arizona Press, Tucson, pp. 557-593). This result is consistent with radar studies showing that igneous rocky asteroids - the E and V types - exhibit the largest surface roughness (Benner, L et al. [2008]. Icarus 198,294-304). The effects of what appears to be space weathering can be largely explained by phase reddening in our collection of V-type NEOs, but our finding that smaller vestoids, which have shorter lifetimes, are more similar to Vesta suggests that some type of alteration of the surface through time occurs. Our observations confirm that the south polar region of Vesta has a more diogenitic composition than its equatorial regions. The south pole, which is dominated by a large impact feature, thus may offer a view into the interior of Vesta. We derive a visible phase integral of 0.44 +/- 0.02 and a corresponding Bond albedo of 0.15 +/- 0.03 from our composite V-type asteroid solar phase curve. (C) 2014 Published by Elsevier Inc. C1 [Hicks, Michael D.; Buratti, Bonnie J.; Lawrence, Kenneth J.; Raymond, Carol; Rhoades, Heath; Mayes, Deronda] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hillier, John] Grays Harbor Coll, Aberdeen, WA 98520 USA. [Li, Jian-Yang] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Reddy, Vishnu; Schroeder, Stefan; Nathues, Andreas; Hoffmann, Martin; Le Corre, Lucille] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Duffard, Rene] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Zhao, Hai-Bin] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Russell, Christopher] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Roatsch, Thomas; Jaumann, Ralf] Deutsch Zentrum Luft & Raumfahrt, Inst Planetary Res, D-80302 Berlin, Germany. [Barajas, Tzitlaly; Thien-Tin Truong; Foster, James; McAuley, Amanda] Calif State Univ Los Angeles, Los Angeles, CA 90032 USA. RP Hicks, MD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Michael.Hicks@jpl.nasa.gov; jyli@astro.umd.edu; duffard@iaa.es RI Duffard, Rene/A-2233-2009; Schroder, Stefan/D-9709-2013; OI Schroder, Stefan/0000-0003-0323-8324; Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932 FU NASA Near Earth Objects Observation (NEO-O) Program; Dawn Participating Scientist program; Alfred P. Sloan Foundation; National Aeronautics and Space Administration; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; University of Chicago; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Korean Scientist Group; Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology under contract to the National Aeronautics and Space Administration. We acknowledge support from the Dawn Participating Scientist program and the NASA Near Earth Objects Observation (NEO-O) Program. Funding for the creation and distribution of the SDSS Archive has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, the Korean Scientist Group, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. This work was in part based on observations collected at the Centro Astronomico Hispano Aleman (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut fur Astronomie and the Instituto de Astrofisica de Andalucia (CSIC). NR 73 TC 7 Z9 7 U1 0 U2 13 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUN PY 2014 VL 235 BP 60 EP 74 DI 10.1016/j.icarus.2013.11.011 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG3BU UT WOS:000335291600006 ER PT J AU Ahn, J de Weck, OL Steele, M AF Ahn, Jaemyung de Weck, Olivier L. Steele, Martin TI Credibility Assessment of Models and Simulations Based on NASA's Models and Simulation Standard Using the Delphi Method SO SYSTEMS ENGINEERING LA English DT Article DE models and simulations; Delphi method; credibility assessment; SpaceNet ID FACE-TO-FACE; DECISION-MAKING; NOMINAL GROUPS AB This paper introduces a procedure to assess the credibility of models and simulations (M&S) as a group activity based on NASA's new standard for M&S NASA-STD-7009. The Delphi method, which is characterized by iterative surveys with controlled feedback, was selected to implement the assessment. The proposed procedure is expected to address the issues in the M&S assessment related to a high level of required expertise and group decision making. An actual credibility assessment study using the proposed procedure on an M&S platform referred to as SpaceNet has been carried out by ten panel members through a two-round Delphi. The study concluded that the overall credibility of SpaceNet version 1.3 was between the development level and production level. The variances of the assessments in the second-round survey were significantly reduced compared with the first-round results, which indicates the effectiveness of the proposed procedure. C1 [Ahn, Jaemyung] Korea Adv Inst Sci & Technol, Taejon 305701, South Korea. [de Weck, Olivier L.] MIT, Cambridge, MA 02139 USA. [Steele, Martin] NASA, John F Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA. RP Ahn, J (reprint author), Korea Adv Inst Sci & Technol, Taejon 305701, South Korea. EM jaemyung.ahn@kaist.ac.kr RI Ahn, Jaemyung/C-1822-2011 NR 28 TC 3 Z9 3 U1 2 U2 20 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1098-1241 EI 1520-6858 J9 SYSTEMS ENG JI Syst. Eng. PD SUM PY 2014 VL 17 IS 2 BP 237 EP 248 DI 10.1002/sys.21266 PG 12 WC Engineering, Industrial; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA AE8XF UT WOS:000334285600009 ER PT J AU Lee, JS Ray, RI Little, BJ Duncan, KE Aktas, DF Oldham, AL Davidova, IA Suflita, JM AF Lee, Jason S. Ray, Richard I. Little, Brenda J. Duncan, Kathleen E. Aktas, Deniz F. Oldham, Athenia L. Davidova, Irene A. Suflita, Joseph M. TI Issues for storing plant-based alternative fuels in marine environments SO BIOELECTROCHEMISTRY LA English DT Article DE Biodiesel; Altemative fuel; Seawater; Corrosion; Carbon steel ID CONVENTIONAL PETROLEUM FUELS; CORROSION; DIESEL; BIODEGRADABILITY; BIOFUELS; BIOMASS; STEEL AB Two coastal seawaters (Key West, FL USA and the Persian Gulf, Bahrain, representing oligotrophic and eutrophic environments, respectively) were used to evaluate potential biodegradation and corrosion problems during exposure to alternative and conventional fuels. Uncoated carbon steel was exposed at the fuel/seawater interface and polarization resistance was monitored. Under typical marine storage conditions, dioxygen in natural seawater exposed to fuel and carbon steel was reduced to <0.1 parts-per-million within 2 d due to consumption by corrosion reactions and aerobic microbial respiration. Sulfides, produced by anaerobic sulfate-reducing bacteria, and chlorides were co-located in corrosion products. Transient dioxygen influenced both metabolic degradation pathways and resulting metabolites. Catechols, indicative of aerobic biodegradation, persisted after 90 d exposures. Detection of catechols suggested that initial exposure to dioxygen resulted in the formation of aerobic metabolites that exacerbated subsequent corrosion processes. Published by Elsevier B.V. C1 [Lee, Jason S.; Ray, Richard I.; Little, Brenda J.] Stennis Space Ctr, Naval Res Lab, Stennis Space Ctr, MS 39529 USA. [Duncan, Kathleen E.; Aktas, Deniz F.; Oldham, Athenia L.; Davidova, Irene A.; Suflita, Joseph M.] Univ Oklahoma, Dept Microbiol & Plant Biol, Norman, OK 73019 USA. RP Lee, JS (reprint author), Stennis Space Ctr, Naval Res Lab, 1009 Balch Blvd, Stennis Space Ctr, MS 39529 USA. EM jason.lee@nrissc.navy.mil FU Sharon Beermann-Curtin at the Office of Naval Research (ONR Code 332) [N0001411WX21441]; NRL publication [NRL/JA/7330-12-1550]; Office of Naval Research [N000141010946] FX NRL personnel were funded by Sharon Beermann-Curtin at the Office of Naval Research (ONR Code 332) under award N0001411WX21441. NRL publication NRL/JA/7330-12-1550. The study was also supported by grant N000141010946 from the Office of Naval Research. NR 20 TC 4 Z9 4 U1 0 U2 7 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 1567-5394 EI 1521-186X J9 BIOELECTROCHEMISTRY JI Bioelectrochemistry PD JUN PY 2014 VL 97 SI SI BP 145 EP 153 DI 10.1016/j.bioelechem.2013.12.003 PG 9 WC Biochemistry & Molecular Biology; Biology; Biophysics; Electrochemistry SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Biophysics; Electrochemistry GA AE6EL UT WOS:000334083300018 PM 24411308 ER PT J AU Cheng, YB Zhang, QY Lyapustin, AI Wang, YJ Middleton, EM AF Cheng, Yen-Ben Zhang, Qingyuan Lyapustin, Alexei I. Wang, Yujie Middleton, Elizabeth M. TI Impacts of light use efficiency and fPAR parameterization on gross primary production modeling SO AGRICULTURAL AND FOREST METEOROLOGY LA English DT Article DE Carbon modeling; Fraction of photosynthetically active radiation; fAPAR(chl); Light use efficiency ID DECIDUOUS BROADLEAF FOREST; PHOTOSYNTHETICALLY ACTIVE RADIATION; NET PRIMARY PRODUCTION; LEAF-AREA INDEX; TERRESTRIAL GROSS; MODIS DATA; CHLOROPHYLL FAPAR(CHL); VEGETATION INDEXES; DATA ASSIMILATION; REMOTE ESTIMATION AB This study examines the impact of parameterization of two variables, light use efficiency (LUE) and the fraction of absorbed photosynthetically active radiation (fPAR or fAPAR), on gross primary production (GPP) modeling. Carbon sequestration by terrestrial plants is a key factor to a comprehensive understanding of the carbon budget at global scale. In this context, accurate measurements and estimates of GPP will allow us to achieve improved carbon monitoring and to quantitatively assess impacts from climate changes and human activities. Spacebome remote sensing observations can provide a variety of land surface parameterizations for modeling photosynthetic activities at various spatial and temporal scales. This study utilizes a simple GPP model based on LUE concept and different land surface parameterizations to evaluate the model and monitor GPP. Two maize-soybean rotation fields in Nebraska, USA and the Bartlett Experimental Forest in New Hampshire, USA were selected for study. Tower-based eddy-covariance carbon exchange and PAR measurements were collected from the FLUXNET Synthesis Dataset. For the model parameterization, we utilized different values of LUE and the fPAR derived from various algorithms. We adapted the approach and parameters from the MODIS MOD17 Biome Properties Look-Up Table (BPLUT) to derive LUE. We also used a site-specific analytic approach with tower-based Net Ecosystem Exchange (NEE) and PAR to estimate maximum potential LUE (LUEmax.) to derive LUE. For the fPAR parameter, the MODIS MOD 15A2 fPAR product was used. We also utilized fAPAR(chl), a parameter accounting for the fAPAR linked to the chlorophyll-containing canopy fraction. fAPAR(chl) was obtained by inversion of a radiative transfer model, which used the MODIS-based reflectances in bands 1-7 produced by Multi-Angle Implementation of Atmospheric Correction (MAIAC) algorithm. fAPAR(chl) exhibited seasonal dynamics more similar with the flux tower based GPP than MOD15A2 fPAR, especially in the spring and fall at the agricultural sites. When using the MODIS MOD17-based parameters to estimate LUE, fAPAR(chl) generated better agreements with GPP (r(2) = 0.79-0.91) than MOD15A2 fPAR (r(2) = 0.57-0.84). However, underestimations of GPP were also observed, especially for the crop fields. When applying the site-specific LUEmax value to estimate in situ LUE, the magnitude of estimated GPP was closer to in situ GPP; this method produced a slight overestimation for the MOD15A2 fPAR at the Bartlett forest. This study highlights the importance of accurate land surface parameterizations to achieve reliable carbon monitoring capabilities from remote sensing information. (C) 2014 Elsevier B.V. All rights reserved. C1 [Cheng, Yen-Ben] Earth Resources Technol Inc, Laurel, MD 20707 USA. [Zhang, Qingyuan] Univ Space Res Assoc, Columbia, MD 21044 USA. [Lyapustin, Alexei I.] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA. [Wang, Yujie] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. [Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. RP Cheng, YB (reprint author), NASA, Goddard Space Flight Ctr, Code 618, Greenbelt, MD 20771 USA. EM Yen-Ben.Cheng@nasa.gov RI Lyapustin, Alexei/H-9924-2014 OI Lyapustin, Alexei/0000-0003-1105-5739 FU NASA ROSES project "Carbon Monitoring and Ecosystem Feedbacks Prediction Using fAPARch1 and the Community Land Model (CLM)" [NNX12AJ51G]; NASA Earth Sciences Program; AmeriFlux (U.S. Department of Energy, Biological and Environmental Research); Terrestrial Carbon Program [DE-FG02-04ER63917, DE-FG02-04ER63911]; AfriFlux; AsiaFlux; CarboAfrica; CarboEuropeIP; CarboItaly; CarboMont; ChinaFlux; Fluxnet-Canada; CFCAS; NSERC; BIOCAP; Environment Canada; NRCan; FAO-GTOS-TCO; iLEAPS; Max Planck Institute for Biogeochemistry; National Science Foundation; University of Tuscia; Universite Laval and Environment Canada; US Department of Energy; Berkeley Water Center; Lawrence Berkeley National Laboratory; Microsoft Research eScience; Oak Ridge National Laboratory; University of California - Berkeley; University of Virginia FX This study was supported by a NASA ROSES project, Grant No. NNX12AJ51G "Carbon Monitoring and Ecosystem Feedbacks Prediction Using fAPARch1 and the Community Land Model (CLM)" (PI, Q. Zhang), through the Terrestrial Ecology Program (Diane Wickland, manager). The work of A. Lyapustin and Y. Wang was supported by the NASA Earth Sciences Program. This work used eddy covariance data acquired by the FLUXNET community and in particular by the following networks: AmeriFlux (U.S. Department of Energy, Biological and Environmental Research, Terrestrial Carbon Program (DE-FG02-04ER63917 and DE-FG02-04ER63911), AfriFlux, AsiaFlux, CarboAfrica, CarboEuropeIP, CarboItaly, CarboMont, ChinaFlux, Fluxnet-Canada (supported by CFCAS, NSERC, BIOCAP, Environment Canada, and NRCan), GreenGrass, KoFlux, LBA, NECC, OzFlux, TCOS-Siberia, USCCC. We acknowledge the financial support to the eddy covariance data harmonization provided by CarboEuropeIP, FAO-GTOS-TCO, iLEAPS, Max Planck Institute for Biogeochemistry, National Science Foundation, University of Tuscia, Universite Laval and Environment Canada and US Department of Energy and the database development and technical support from Berkeley Water Center, Lawrence Berkeley National Laboratory, Microsoft Research eScience, Oak Ridge National Laboratory, University of California - Berkeley, University of Virginia. The authors thank the anonymous reviewers for their very valuable suggestions and critiques. NR 61 TC 17 Z9 17 U1 3 U2 79 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 JUN 1 PY 2014 VL 189 BP 187 EP 197 DI 10.1016/j.agrformet.2014.01.006 PG 11 WC Agronomy; Forestry; Meteorology & Atmospheric Sciences SC Agriculture; Forestry; Meteorology & Atmospheric Sciences GA AE3BW UT WOS:000333852900020 ER PT J AU Davami, K Shaygan, M Kheirabi, N Zhao, J Kovalenko, DA Rummeli, MH Opitz, J Cuniberti, G Lee, JS Meyyappan, M AF Davami, Keivan Shaygan, Mehrdad Kheirabi, Nazli Zhao, Jiong Kovalenko, Dana A. Ruemmeli, Mark H. Opitz, Joerg Cuniberti, Gianaurelio Lee, Jeong-Soo Meyyappan, M. TI Synthesis and characterization of carbon nanowalls on different substrates by radio frequency plasma enhanced chemical vapor deposition SO CARBON LA English DT Article ID MAGNETIC-PROPERTIES; RAMAN-SPECTRA; THIN-FILMS; GRAPHENE; NANOSHEETS; GROWTH; FERROMAGNETISM AB A radio frequency plasma enhanced chemical vapor deposition system was used for the successful growth of thin vertical carbon nanowalls, also known as vertical graphene, on various substrates. Transmission electron microscopy studies confirmed the presence of vertical graphene walls, which are tapered, typically consisting of 10 layers at the base tapering off to 2 or 3 layers at the top. The sides of the walls are facetted at quantized angles of 30 degrees and the facetted sides are usually seamless. Growth occurs at the top open edge which is not facetted. Hydrogen induced etching allows for nucleation of branch walls apparently involving a carbon onion-like structure at the root base. Characterization by a superconducting quantum interference device showed magnetic hysteresis loops and weak ferromagnetic responses from the samples at room temperature and below. Temperature dependence of the magnetization revealed a magnetic phase transition around T = 50 K highlighting the coexistence of antiferromagnetic interactions as well as ferromagnetic order. Published by Elsevier Ltd. C1 [Davami, Keivan; Shaygan, Mehrdad; Kheirabi, Nazli; Cuniberti, Gianaurelio; Lee, Jeong-Soo] Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang, South Korea. [Zhao, Jiong; Ruemmeli, Mark H.] IFW Dresden, D-01069 Dresden, Germany. [Kovalenko, Dana A.; Opitz, Joerg; Cuniberti, Gianaurelio] Tech Univ Dresden, D-01062 Dresden, Germany. [Kovalenko, Dana A.; Opitz, Joerg] Fraunhofer Inst Nondestruct Testing, Dresden Branch, D-01109 Dresden, Germany. [Ruemmeli, Mark H.] Sungkyunkwan Univ, Ctr Integrated Nanostruct Phys, Inst Basic Sci, Dept Energy Sci, Seoul, South Korea. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lee, JS (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM ljs6951@postech.ac.kr; m.meyyappan@nasa.gov RI Cuniberti, Gianaurelio/B-7192-2008; Davami, Keivan/Q-5283-2016; OI Cuniberti, Gianaurelio/0000-0002-6574-7848; Opitz, Joerg/0000-0003-3142-2479; Rummeli, Mark Hermann/0000-0003-3736-6439; Zhao, Jiong/0000-0002-7411-0734 FU World Class University program; Ministry of Education, Science and Technology through the National Research Foundation of Korea [R31-10100]; DAAD; Siemens [A/08/98783]; German Excellence Initiative via the Cluster of Excellence EXC 1056 "Center for Advancing Electronics Dresden" (cfAED) FX This research was supported by the World Class University program funded by the Ministry of Education, Science and Technology through the National Research Foundation of Korea (R31-10100) and DAAD and Siemens (A/08/98783). Support from the German Excellence Initiative via the Cluster of Excellence EXC 1056 "Center for Advancing Electronics Dresden" (cfAED) is also acknowledged. Preliminary TEM analysis by Hessam Ghassemi is acknowledged. NR 40 TC 27 Z9 27 U1 10 U2 72 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0008-6223 EI 1873-3891 J9 CARBON JI Carbon PD JUN PY 2014 VL 72 BP 372 EP 380 DI 10.1016/j.carbon.2014.02.025 PG 9 WC Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA AE5EM UT WOS:000334010600043 ER PT J AU Chaturvedi, P Hauser, BA Foster, JS Karplus, E Levine, LH Coutts, JL Richards, JT Vanegas, DC McLamore, ES AF Chaturvedi, P. Hauser, B. A. Foster, J. S. Karplus, E. Levine, L. H. Coutts, J. L. Richards, J. T. Vanegas, D. C. McLamore, E. S. TI A multiplexing fiber optic microsensor system for monitoring spatially resolved oxygen patterns SO SENSORS AND ACTUATORS B-CHEMICAL LA English DT Article DE Oxygen; multiplexing; Fiber optic; Lifetime; Frequency-modulated excitation ID MODERN MARINE STROMATOLITES; MICROBIAL DIVERSITY; HIGHBORNE CAY; THROMBOLITIC MATS; PLANT; FLUORESCENCE; TRANSPORT; BAHAMAS; FLUXES; SEED AB Single channel luminescent oxygen-quenched optrodes and micro optrodes have been commercially available for over a decade. However, many field experiments in biological research require multiple oxygen sensors to collect large spatial datasets, or to monitor real time oxygen transport in various regions of interest. This paper demonstrates the design, validation, and application of a fiber optic oxygen microsensor system that is designed to conduct real-time measurements of multiple samples in field studies. The ten channel system was validated in laboratory conditions and then used to monitor spatially resolved, real time oxygen concentration in marine microbial mats, agricultural soil, and developing seeds. Sensor stability, drift, sensitivity, and response time were similar to a single channel commercial technology. The effects of temperature and salinity were analyzed and compared to a commercial micro optrode system (there was no statistical difference in performance between the two systems). In addition to the multiplexing capability, an advantage of the system developed here is the ability to map oxygen gradients in three dimensions. The multiplexing system is a minimally invasive tool for in vivo monitoring of form-function relationships with sub-millimeter spatial resolution. (C) 2014 Elsevier B.V. All rights reserved. C1 [Chaturvedi, P.; Vanegas, D. C.; McLamore, E. S.] Univ Florida, Gainesville, FL 32611 USA. [Hauser, B. A.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Foster, J. S.] Univ Florida, Dept Microbiol & Cell Sci, Gainesville, FL 32611 USA. [Foster, J. S.] NASA, Kennedy Space Ctr, Space Life Sci Lab, Pasadena, CA USA. [Karplus, E.] Sci Wares Inc, Falmouth, MA USA. [Levine, L. H.] Enterprise Advisory Serv Inc, ESC Team QNA, Kennedy Space Ctr, FL USA. [Coutts, J. L.; Richards, J. T.] ESC Team QNA, Kennedy Space Ctr, FL USA. [Vanegas, D. C.] Univ Valle, Dept Food Engn, Cali, Colombia. RP McLamore, ES (reprint author), Univ Florida, Gainesville, FL 32611 USA. EM emclamor@ufl.edu RI Vanegas, Diana/J-3770-2013 OI Vanegas, Diana/0000-0001-9858-0960 FU UF Agricultural & Biological Engineering Fellowship; UF Excellence Award (EMC; CRIS) [005062]; UF Early Career Award (EMC; CRIS) [005062]; NASA's Planetary Biology Internship Program; USDA National Research Initiative (BAH) [2008-35100-19244] FX This manuscript is dedicated to the memory of Dr. Lanfang Levine. The authors would like to thank the UF Agricultural & Biological Engineering Fellowship for support (PC), the UF Excellence Award (EMC; CRIS No. 005062), and the UF Early Career Award for funding (EMC; CRIS No. 005062)), the NASA's Planetary Biology Internship Program for a summer working in Dr. Lanfang Levine's lab and the USDA National Research Initiative (BAH; grant number 2008-35100-19244) A special thanks to PIKL (Baltimore, MD) for help with graphic images. NR 54 TC 3 Z9 3 U1 2 U2 28 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-4005 J9 SENSOR ACTUAT B-CHEM JI Sens. Actuator B-Chem. PD JUN PY 2014 VL 196 BP 71 EP 79 DI 10.1016/j.snb.2014.01.094 PG 9 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation SC Chemistry; Electrochemistry; Instruments & Instrumentation GA AE0KC UT WOS:000333652400010 ER PT J AU Ma, WP Jacobs, G Sparks, DE Spicer, RL Davis, BH Klettlinger, JLS Yen, CH AF Ma, Wenping Jacobs, Gary Sparks, Dennis E. Spicer, Robert L. Davis, Burtron H. Klettlinger, Jennifer L. S. Yen, Chia H. TI Fischer-Tropsch synthesis: Kinetics and water effect study over 25%Co/Al2O3 catalysts SO CATALYSIS TODAY LA English DT Article DE Fischer-Tropsch synthesis; Kinetics; Kinetic water effect; Co/Al2O3 ID SUPPORTED COBALT CATALYSTS; INTRINSIC KINETICS; CO/AL2O3 CATALYSTS; PARTIAL-PRESSURE; CO ACTIVATION; SLURRY-PHASE; SELECTIVITY; IRON; DEACTIVATION; HYDROGENATION AB The kinetics of Fischer-Tropsch synthesis (FTS) over a 25%Co/Al2O3 catalyst was studied using a 1-L continuously stirred tank reactor (CSTR) under the conditions of 205-230 degrees C, 1.4-2.5 MPa, H-2/CO = 1.0-2.5 and 3-16 NL/g-cat/h (X-CO = 7-54%). Thirty-one sets of kinetic data collected at 220 degrees C with a low extent of deactivation were used for kinetic parameter regression. The CAER empirical kinetic model (r(FT) = kP(CO)(a) P-H2(b)/(1 broken vertical bar mP(H2O)/PH2)) was employed to study the kinetic effect of water. A positive kinetic water effect was first evidenced using the kinetic approach, consistent with the results of the effect of co-fed water on cobalt FTS in this work and the literature (e.g. Loegdberg et al., 2011 [21]) for CO/Al2O3 catalysts. The current kinetic results are based on kinetic data taken following an initial catalyst induction period, where the CO conversion had stabilized. These data are different from our earlier investigations where reversible oxidation of small cobalt crystallites and/or catalyst support effects likely impacted the cobalt site densities, resulting in a negative water effect. Thus, in this study, we decoupled the effect of reversible oxidation from the kinetics, so that the effect of water on stable (i.e., presumably larger) metallic cobalt particles could be assessed. In this study, an additional eleven classical FT kinetic models for Co catalysts were tested using the kinetic data. Five of them were also found to adequately describe the kinetic data, including two mechanistic models developed based on carbide mechanisms. The CAER model containing a water effect term and the mechanistic model of Botes et al. (2009) [31] yielded comparable reaction orders for the partial pressures of H-2 and CO, resulted in a better fit of the kinetic data. (C) 2013 Elsevier B.V. All rights reserved. C1 [Ma, Wenping; Jacobs, Gary; Sparks, Dennis E.; Spicer, Robert L.; Davis, Burtron H.] Univ Kentucky, Ctr Appl Energy Res, Lexington, KY 40511 USA. [Klettlinger, Jennifer L. S.; Yen, Chia H.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Davis, BH (reprint author), Univ Kentucky, Ctr Appl Energy Res, 2540 Res Pk Dr, Lexington, KY 40511 USA. EM burtron.davis@uky.edu RI Jacobs, Gary/M-5349-2015 OI Jacobs, Gary/0000-0003-0691-6717 FU NASA [NNX07AB93A]; Commonwealth of Kentucky FX This work was supported by NASA contract, NNX07AB93A and the Commonwealth of Kentucky. NR 49 TC 16 Z9 16 U1 3 U2 83 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5861 EI 1873-4308 J9 CATAL TODAY JI Catal. Today PD JUN 1 PY 2014 VL 228 BP 158 EP 166 DI 10.1016/j.cattod.2013.10.014 PG 9 WC Chemistry, Applied; Chemistry, Physical; Engineering, Chemical SC Chemistry; Engineering GA AD7NB UT WOS:000333449800020 ER PT J AU Sun, JQ Xiong, XX Angal, A Chen, HD Wu, AS Geng, X AF Sun, Junqiang Xiong, Xiaoxiong Angal, Amit Chen, Hongda Wu, Aisheng Geng, Xu TI Time-Dependent Response Versus Scan Angle for MODIS Reflective Solar Bands SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Aqua; desert; Moderate Resolution Imaging Spectroradiometer (MODIS); moon; reflective solar bands (RSBs); response versus scan angle (RVS); scan mirror; solar diffuser (SD); Terra ID ON-ORBIT CALIBRATION; RESOLUTION IMAGING SPECTRORADIOMETER; TERRA MODIS; AQUA MODIS; PERFORMANCE; SENSORS AB The Moderate Resolution Imaging Spectroradiometer (MODIS) instruments currently operate onboard the National Aeronautics and Space Administration (NASA's) Terra and Aqua spacecraft, launched on December 18, 1999 and May 4, 2002, respectively. MODIS has 36 spectral bands, among which 20 are reflective solar bands (RSBs) covering a spectral range from 0.412 to 2.13 mu m. The RSBs are calibrated on orbit using a solar diffuser (SD) and an SD stability monitor and with additional measurements from lunar observations via a space view (SV) port. Selected pseudo-invariant desert sites are also used to track the RSB on-orbit gain change, particularly for short-wavelength bands. MODIS views the Earth surface, SV, and the onboard calibrators using a two-sided scan mirror. The response versus scan angle (RVS) of the scan mirror was characterized prior to launch, and its changes are tracked using observations made at different angles of incidence from onboard SD, lunar, and Earth view (EV) measurements. These observations show that the optical properties of the scan mirror have experienced large wavelength-dependent degradation in both the visible and near infrared spectral regions. Algorithms have been developed to track the on-orbit RVS change using the calibrators and the selected desert sites. These algorithms have been applied to both Terra and Aqua MODIS Level 1B (L1B) to improve the EV data accuracy since L1B Collection 4, refined in Collection 5, and further improved in the latest Collection 6 (C6). In C6, two approaches have been used to derive the time-dependent RVS for MODIS RSB. The first approach relies on data collected from sensor onboard calibrators and mirror side ratios from EV observations. The second approach uses onboard calibrators and EV response trending from selected desert sites. This approach is mainly used for the bands with much larger changes in their time-dependent RVS, such as the Terra MODIS bands 1-4, 8, and 9 and the Aqua MODIS bands 8 and 9. In this paper, the algorithms of these approaches are described, their performance is demonstrated, and their impact on L1B products is discussed. In general, the shorter wavelength bands have experienced a larger on-orbit RVS change, which, in general, are mirror side and detector dependent. The on-orbit RVS change due to the degradation of band 8 can be as large as 35% for Terra MODIS and 20% for Aqua MODIS. Vital to maintaining the accuracy of the MODIS L1B products is an accurate characterization of the on-orbit RVS change. The derived time-independent RVS, implemented in C6, makes an important improvement to the quality of the MODIS L1B products. C1 [Sun, Junqiang; Chen, Hongda; Wu, Aisheng; Geng, Xu] Sigma Space Corp, Lanham, MD 20706 USA. [Xiong, Xiaoxiong] NASA, Sci & Explorat Directorate, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Angal, Amit] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. RP Sun, JQ (reprint author), Sigma Space Corp, Lanham, MD 20706 USA. EM junqiang.sun@sigmaspace.com NR 28 TC 42 Z9 42 U1 1 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUN PY 2014 VL 52 IS 6 BP 3159 EP 3174 DI 10.1109/TGRS.2013.2271448 PG 16 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AC4QB UT WOS:000332504700011 ER PT J AU Liu, Z Jung, HS Lu, Z AF Liu, Zhen Jung, Hyung-Sup Lu, Zhong TI Joint Correction of Ionosphere Noise and Orbital Error in L-Band SAR Interferometry of Interseismic Deformation in Southern California SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE ALOS PALSAR; interferometric SAR (InSAR); ionospheric correction; ionosphere noise; multiple-aperture interferometry (MAI); orbital error; synthetic aperture radar (SAR) ID SURFACE DEFORMATION AB The accuracy of L-band synthetic aperture radar (SAR) differential interferometry (InSAR) on crustal deformation studies is largely compromised by ionosphere path delays on the radar signals. The ionosphere effects cause severe ionospheric distortion such as azimuth streaking and long wavelength phase distortion similar to orbital ramp error. Effective detection and correction of ionospheric phase distortion from L-band InSAR images are necessary to measure and accurately interpret surface displacement. In this paper, we investigate the performance improvement of L-band InSAR interseismic deformation measurements in southern California through the joint correction of both ionosphere noise and orbital error. Our results show that this method can effectively remove orbit and ionosphere phase distortions. In comparison with in situ GPS measurements, the achieved InSAR measurement accuracy is improved from similar to 30 mm to similar to 10 mm by the proposed joint correction method. We show that, after the joint correction, the remaining atmosphere noise can be further mitigated through stacking, leading to an RMS error of similar to 4.7 mm/year in resultant line-of-sight velocity, as compared with similar to 11.3 mm/year before the correction. Our results demonstrate that the proposed joint correction technique provides a promising way to jointly correct orbital and ionospheric artifacts in L-band InSAR studies of crustal deformation. C1 [Liu, Zhen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jung, Hyung-Sup] Univ Seoul, Dept Geoinformat, Seoul 130743, South Korea. [Lu, Zhong] US Geol Survey, Cascades Volcano Observ, Vancouver, WA 98683 USA. RP Liu, Z (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Zhen.liu@jpl.nasa.gov; hsjung@uos.ac.kr; lu@usgs.gov RI Liu, Zhen/D-8334-2017; OI Jung, Hyung-Sup/0000-0003-2335-8438 FU Jet Propulsion Laboratory, California Institute of Technology under National Aeronautics and Space Administration; The University of Seoul; Space Core Technology Development Program through the National Research Foundation of Korea; Ministry of Education, Science and Technology [2012M1A3A3A02033465]; State-of-the-Art Remote Sensing Technology Development of Disaster Management Research Program; National Disaster Management Institute [NDMI-M-2012-09] FX Manuscript received March 27, 2013; revised June 17, 2013; accepted July 1, 2013. This work was supported in part by the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration and in part by the The University of Seoul under financial support from Space Core Technology Development Program through the National Research Foundation of Korea funded by the Ministry of Education, Science and Technology under Grant 2012M1A3A3A02033465 and State-of-the-Art Remote Sensing Technology Development of Disaster Management Research Program funded by the National Disaster Management Institute under Grant NDMI-M-2012-09. NR 22 TC 11 Z9 12 U1 0 U2 28 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUN PY 2014 VL 52 IS 6 BP 3421 EP 3427 DI 10.1109/TGRS.2013.2272791 PG 7 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AC4QB UT WOS:000332504700033 ER PT J AU He, T Liang, SL Wang, DD Shuai, YM Yu, YY AF He, Tao Liang, Shunlin Wang, Dongdong Shuai, Yanmin Yu, Yunyue TI Fusion of Satellite Land Surface Albedo Products Across Scales Using a Multiresolution Tree Method in the North Central United States SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Albedo; data fusion; Enhanced Thematic Mapper Plus (ETM plus ); Moderate Resolution Imaging Spectroradiometer (MODIS); Multiangle Imaging Spectroradiometer (MISR); multiresolution tree (MRT); Thematic Mapper (TM) ID IN-SITU MEASUREMENTS; BROAD-BAND ALBEDO; ATMOSPHERIC CORRECTION; MODIS; REFLECTANCE; MODEL; VALIDATION; PREDICTION; RETRIEVAL; ALGORITHM AB Land surface albedo is a key factor in climate change and land surface modeling studies, which affects the surface radiation budget. Many satellite albedo products have been generated during the last several decades. However, due to the problems resulting from the sensor characteristics (spectral bands, spatial and temporal resolutions, etc.) and/or the retrieving procedures, surface albedo estimations from different satellite sensors are inconsistent and often contain gaps, which limit their applications. Many approaches have been developed to generate the complete albedo data set; however, most of them suffer from either the persistent systematic bias of relying on only one data set or the problem of subpixel heterogeneity. In this paper, a data fusion method is prototyped using multiresolution tree (MRT) models to develop spatially and temporally continuous albedo maps from different satellite albedo/reflectance data sets. Data from the Multiangle Imaging Spectroradiometer (MISR), Moderate Resolution Imaging Spectroradiometer (MODIS), and Landsat Thematic Mapper/Enhanced Thematic Mapper Plus are used as examples, at a study area in the north central United States mostly covered by crop, grass, and forest, from June to September 2005. Results show that the MRT data fusion method is capable of integrating the three satellite data sets at different spatial resolutions to fill the gaps and to reduce the inconsistencies between different products. The validation results indicate that the uncertainties of the three satellite products have been reduced significantly through the data fusion procedure. Further efforts are needed to evaluate and improve the current algorithm over other locations, time periods, and land cover types. C1 [He, Tao; Liang, Shunlin; Wang, Dongdong] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Liang, Shunlin] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China. [Shuai, Yanmin] Earth Resources Technol Inc, Laurel, MD 20707 USA. [Shuai, Yanmin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yu, Yunyue] NOAA, Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res, Camp Springs, MD 20746 USA. RP He, T (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. RI Yu, Yunyue/F-5636-2010; Wang, Dongdong/M-1969-2014; liang, shunlin/C-2809-2015; He, Tao/H-5130-2012 OI Wang, Dongdong/0000-0002-2076-576X; He, Tao/0000-0003-2079-7988 FU Center for Satellite Applications and Research (STAR); National Oceanic and Atmospheric Administration [NA17EC1483] FX Manuscript received July 19, 2012; revised March 5, 2013 and May 17, 2013; accepted July 7, 2013. This work was supported by the Center for Satellite Applications and Research (STAR), National Oceanic and Atmospheric Administration, under Grant NA17EC1483. NR 45 TC 9 Z9 10 U1 3 U2 40 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUN PY 2014 VL 52 IS 6 BP 3428 EP 3439 DI 10.1109/TGRS.2013.2272935 PG 12 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AC4QB UT WOS:000332504700034 ER PT J AU Ahmed, R Siqueira, P Hensley, S AF Ahmed, Razi Siqueira, Paul Hensley, Scott TI Analyzing the Uncertainty of Biomass Estimates From L-Band Radar Backscatter Over the Harvard and Howland Forests SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Biomass; errors; Harvard Forest; Howland Forest; radar backscatter ID VEGETATION STRUCTURE; SAR DATA; EQUATIONS AB A better understanding of ecosystem processes requires accurate estimates of forest biomass and structure on global scales. Recently, there have been demonstrations of the ability of remote sensing instruments, such as radar and lidar, for the estimation of forest parameters from spaceborne platforms in a consistent manner. These advances can be exploited for global forest biomass accounting and structure characterization, leading to a better understanding of the global carbon cycle. The popular techniques for the estimation of forest parameters from radar instruments, in particular, use backscatter intensity, interferometry, and polarimetric interferometry. This paper analyzes the uncertainty in biomass estimates derived from single-season L-band cross-polarized (HV) radar backscatter over temperate forests of the Northeastern United States. An empirical approach is adopted, relying on ground-truth data collected during field campaigns over the Harvard and Howland Forests in 2009. The accuracy of field biomass estimates, including the impact of the diameter-biomass allometry, is characterized for the field sites. A single-season radar data set from the National Aeronautics and Space Administration Jet Propulsion Laboratory's L-band Uninhabited Aerial Vehicle Synthetic Aperture Radar instrument is analyzed to assess the accuracy of the backscatter-biomass relationships with a theoretical radar error model. C1 [Ahmed, Razi; Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Siqueira, Paul] Univ Massachusetts, Dept Elect & Comp Engn, Amherst, MA 01002 USA. RP Ahmed, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM razi.u.ahmed@jpl.nasa.gov RI Siqueira, Paul/D-9760-2016 OI Siqueira, Paul/0000-0001-5781-8282 NR 34 TC 2 Z9 2 U1 1 U2 25 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUN PY 2014 VL 52 IS 6 BP 3568 EP 3586 DI 10.1109/TGRS.2013.2273738 PG 19 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AC4QB UT WOS:000332504700045 ER PT J AU Bhatt, R Doelling, DR Morstad, D Scarino, BR Gopalan, A AF Bhatt, Rajendra Doelling, David R. Morstad, Daniel Scarino, Benjamin R. Gopalan, Arun TI Desert-Based Absolute Calibration of Successive Geostationary Visible Sensors Using a Daily Exoatmospheric Radiance Model SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Geostationary visible imager calibration; pseudoinvariant calibration targets; spectral band adjustment factor (SBAF) ID CHANNEL CALIBRATION; SATELLITE SENSORS; SITES; METEOSAT; DEGRADATION; TARGETS AB A desert daily exoatmospheric radiance model (DERM) based on a well-calibrated (reference) geostationary Earth orbit (GEO) satellite visible sensor can be used to transfer the calibration to a (target) GEO sensor located at the same equatorial longitude location. The DERM is based on the reference GEO daily radiances observed over a single pseudoinvariant calibration site (PICS) being that the daily angular conditions are repeated annually for any historical or successive colocated GEO. The GEO-specific PICSs used in the study are first inspected using the well-calibrated Aqua-MODerate Resolution Imaging Spectroradiometer (MODIS) exoatmospheric reflectances for stability. The Libyan Desert site was found to be stable within 1% over ten years. The average clear-sky daily local-noon interannual variability based on Meteosat-9 0.65-mu m top-of-atmosphere radiances over the Libyan Desert is 0.74%, which implies that the combined surface and atmospheric column is invariant. A spectral band adjustment factor, based on Scanning Imaging Absorption Spectrometer for Atmospheric Cartography spectral radiances, is used to account for sensor spectral response function (SRF) differences between the reference and target GEO. The GEO reference calibration was based on the GEO/Aqua-MODIS ray-matched radiance intercalibration transfer technique. The reference Meteosat-9 DERM and ray-matched calibration consistency was within 0.4% and 1.9% for Meteosat-8 and Meteosat-7, respectively. Similarly, GOES-10 and GOES-15 were calibrated based on the GOES-11 DERM using the Sonoran Desert and were found to have a consistency within 1% and 3%, respectively. C1 [Bhatt, Rajendra; Morstad, Daniel; Scarino, Benjamin R.; Gopalan, Arun] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Doelling, David R.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. RP Bhatt, R (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA. EM rajendra.bhatt@nasa.gov; david.r.doelling@nasa.gov; Daniel.morstad@nasa.gov; Benjamin.r.scarino@nasa.gov; arun.gopalan-1@nasa.gov RI Richards, Amber/K-8203-2015 FU National Aeronautics and Space Administration (NASA) Satellite Intercalibration Consistency Program; NASA Clouds and the Earth's Radiant Energy System mission to calibrate geostationary sensors FX The National Aeronautics and Space Administration (NASA) Satellite Intercalibration Consistency Program and NASA Clouds and the Earth's Radiant Energy System mission to calibrate geostationary sensors supported this study. The authors would like to thank J. Xiong and the MODIS team for the assistance with the MODIS data. The MODIS data were obtained from the NASA Langley Distributed Active Archive Center. The geostationary Earth observing satellite data were obtained from the University of Wisconsin Space Science and Engineering Center, Madison, WI, USA. This study could not have been completed without the SCanning Imaging Absorption spectroMeter for Atmospheric CartograpHY (SCIAMACHY) data provided by the European Space Agency Environmental Satellite program. The authors would also like to thank J. Burrows, S. Noel, and K. Bramstedt at Bremen University, R. Snel at the Netherlands Institute for Space Research, and C. Lukashin at the NASA Langley Research Center for their assistance with the SCIAMACHY data. NR 30 TC 11 Z9 11 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUN PY 2014 VL 52 IS 6 BP 3670 EP 3682 DI 10.1109/TGRS.2013.2274594 PG 13 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AC4QB UT WOS:000332504700054 ER PT J AU Biradar, S Goornavar, V Periyakaruppan, A Koehne, J Hall, JC Ramesh, V Ramesh, GT AF Biradar, Santoshkumar Goornavar, Virupaxi Periyakaruppan, Adaikkappan Koehne, Jessica Hall, Joseph C. Ramesh, Vani Ramesh, Govindarajan T. TI Agarose Gel Tailored Calcium Carbonate Nanoparticles-Synthesis and Biocompatibility Evaluation SO JOURNAL OF NANOSCIENCE AND NANOTECHNOLOGY LA English DT Article DE Calcium Carbonate Nanoparticles; Agarose Gel; XRD; FESEM; TEM ID FACTOR-KAPPA-B; OXIDATIVE STRESS; FILLERS; DRUG; SIZE AB In this study, a novel approach to tailor the calcium carbonate nanoparticles was exploited based on agarose gel as polymer medium. The size of nanoparticles formed was governed by ionic diffusion and affected by weight percent of agarose and reaction temperature. The size, shape, purity, composition and allotropy of the synthesized nanoparticles were analyzed by different characterization techniques. Purity of nanoparticles as small as 37 nm demonstrates their suitability for broad range of industrial applications. The exposure of rat lung epithelial cells to these nanoparticles even at a higher concentration (50 mu g/ml) did not induce considerable oxidative stress or cell death authenticating their fidelity to potential applications in the field of biotechnology and medicine. Through the simple and economic method of synthesis adopted in this study, separation of nanoparticles from the gel was easy, and process parameters could be optimized to control the particle size. C1 [Biradar, Santoshkumar; Goornavar, Virupaxi; Hall, Joseph C.; Ramesh, Vani; Ramesh, Govindarajan T.] Norfolk State Univ, Dept Biol, Ctr Biotechnol & Biomed Sci, Mol Toxicol Lab, Norfolk, VA 23504 USA. [Periyakaruppan, Adaikkappan; Koehne, Jessica] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ramesh, GT (reprint author), Norfolk State Univ, Dept Biol, Ctr Biotechnol & Biomed Sci, Mol Toxicol Lab, 700 Pk Ave, Norfolk, VA 23504 USA. FU NASA NSTI; NSF-CREST FX Authors acknowledge the help of Center for Materials Research and Center for Biotechnology and Biomedical Sciences, Norfolk State University, Norfolk, VA for their resources, in particular Dr. A. K. Pradhan, for his help in the use of XRD equipment. Authors also acknowledge the help of Jefferson Lab, Newport News, VA for FESEM/EDX analysis and NASA AMES Research Center, San Francisco, CA for TEM images. This work was supported by NASA NSTI and NSF-CREST. NR 24 TC 1 Z9 1 U1 1 U2 24 PU AMER SCIENTIFIC PUBLISHERS PI VALENCIA PA 26650 THE OLD RD, STE 208, VALENCIA, CA 91381-0751 USA SN 1533-4880 EI 1533-4899 J9 J NANOSCI NANOTECHNO JI J. Nanosci. Nanotechnol. PD JUN PY 2014 VL 14 IS 6 BP 4257 EP 4263 DI 10.1166/jnn.2014.8252 PG 7 WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA AC2NY UT WOS:000332339500037 PM 24738380 ER PT J AU Reginald, NL Davila, JM St Cyr, OC Rastaetter, L AF Reginald, Nelson L. Davila, Joseph M. St Cyr, O. C. Rastaetter, Lutz TI Evaluating the Uncertainties in the Electron Temperature and Radial Speed Measurements Using White Light Corona Eclipse Observations SO SOLAR PHYSICS LA English DT Article DE Solar corona; K-corona; Electron temperature; Solar wind; Electron bulk flow speed ID TOTAL SOLAR ECLIPSE; SPECTRUM; MACS AB We examine the uncertainties in two plasma parameters from their true values in a simulated asymmetric corona. We use the Corona Heliosphere (CORHEL) and Magnetohydrodynamics Around the Sphere (MAS) models in the Community Coordinated Modeling Center (CCMC) to investigate the differences between an assumed symmetric corona and a more realistic, asymmetric one. We were able to predict the electron temperatures and electron bulk flow speeds to within +/- 0.5 MK and +/- 100 km s(-1), respectively, over coronal heights up to 5.0 R-aS (TM) from Sun center. We believe that this technique could be incorporated in next-generation white-light coronagraphs to determine these electron plasma parameters in the low solar corona. We have conducted experiments in the past during total solar eclipses to measure the thermal electron temperature and the electron bulk flow speed in the radial direction in the low solar corona. These measurements were made at different altitudes and latitudes in the low solar corona by measuring the shape of the K-coronal spectra between 350 nm and 450 nm and two brightness ratios through filters centered at 385.0 nm/410.0 nm and 398.7 nm/423.3 nm with a bandwidth of a parts per thousand aEuro parts per thousand 4 nm. Based on symmetric coronal models used for these measurements, the two measured plasma parameters were expected to represent those values at the points where the lines of sight intersected the plane of the solar limb. C1 [Reginald, Nelson L.] NASA, Catholic Univ Amer, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Davila, Joseph M.; St Cyr, O. C.; Rastaetter, Lutz] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Reginald, NL (reprint author), NASA, Catholic Univ Amer, Goddard Space Flight Ctr, MC 671, Greenbelt, MD 20771 USA. EM Nelson.L.Reginald@nasa.gov RI Rastaetter, Lutz/D-4715-2012 OI Rastaetter, Lutz/0000-0002-7343-4147 NR 10 TC 0 Z9 0 U1 0 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD JUN PY 2014 VL 289 IS 6 BP 2021 EP 2039 DI 10.1007/s11207-013-0467-5 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB1FE UT WOS:000331536100007 ER PT J AU Pesnell, WD AF Pesnell, W. Dean TI Predicting Solar Cycle 24 Using a Geomagnetic Precursor Pair SO SOLAR PHYSICS LA English DT Article DE Solar cycle, predictions ID SEMIANNUAL VARIATION; BEHAVIOR; INDEXES; FLUX AB We describe using Ap and F-10.7 as a geomagnetic-precursor pair to predict the amplitude of Solar Cycle 24. The precursor is created by using F-10.7 to remove the direct solar-activity component of Ap. Four peaks are seen in the precursor function during the decline of Solar Cycle 23. A recurrence index that is generated by a local correlation of Ap is then used to determine which peak is the correct precursor. The earliest peak is the most prominent but coincides with high levels of non-recurrent solar activity associated with the intense solar activity of October and November 2003. The second and third peaks coincide with some recurrent activity on the Sun and show that a weak cycle precursor closely following a period of strong solar activity may be difficult to resolve. A fourth peak, which appears in early 2008 and has recurrent activity similar to precursors of earlier solar cycles, appears to be the "true" precursor peak for Solar Cycle 24 and predicts the smallest amplitude for Solar Cycle 24. To determine the timing of peak activity it is noted that the average time between the precursor peak and the following maximum is a parts per thousand aEuro parts per thousand 6.4 years. Hence, Solar Cycle 24 would peak during 2014. Several effects contribute to the smaller prediction when compared with other geomagnetic-precursor predictions. During Solar Cycle 23 the correlation between sunspot number and F-10.7 shows that F-10.7 is higher than the equivalent sunspot number over most of the cycle, implying that the sunspot number underestimates the solar-activity component described by F-10.7. During 2003 the correlation between aa and Ap shows that aa is 10 % higher than the value predicted from Ap, leading to an overestimate of the aa precursor for that year. However, the most important difference is the lack of recurrent activity in the first three peaks and the presence of significant recurrent activity in the fourth. While the prediction is for an amplitude of Solar Cycle 24 of 65 +/- 20 in smoothed sunspot number, a below-average amplitude for Solar Cycle 24, with maximum at 2014.5 +/- 0.5, we conclude that Solar Cycle 24 will be no stronger than average and could be much weaker than average. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Pesnell, WD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM william.d.pesnell@nasa.gov RI Pesnell, William/D-1062-2012 OI Pesnell, William/0000-0002-8306-2500 FU Solar Dynamics Observatory at NASA Goddard Space Flight Center FX This work was supported by the Solar Dynamics Observatory at NASA Goddard Space Flight Center. Daily values of RZ and Adjusted F10.7 (normalized to 1 AU) were obtained from the National Geophysical Data Center in Boulder, CO, USA. Values of Ap were obtained from the monthly files at ftp.ngdc.noaa.gov/STP/GEOMAGNETIC_DATA/INDICES/KP_AP/. Values of aa through 2007 were obtained from ftp.ngdc.noaa.gov/STP/GEOMAGNETIC_DATA/AASTAR/aaindex. More recent values of aa were obtained from isgi.cetp.ipsl.fr/des_aa.htm. NR 37 TC 9 Z9 9 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD JUN PY 2014 VL 289 IS 6 BP 2317 EP 2331 DI 10.1007/s11207-013-0470-x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB1FE UT WOS:000331536100021 ER PT J AU Wang, ZP Xiong, XX AF Wang, Zhipeng Xiong, Xiaoxiong TI VIIRS On-Orbit Spatial Characterization Using the Moon SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Band-to-band registration (BBR); modulation transfer function (MTF); spatial characterization; visible infrared imaging radiometer suite (VIIRS) ID PERFORMANCE AB The VIIRS instrument onboard the Suomi-NPP satellite was launched in October 2011. The design and operation of its on-orbit calibration system are strongly based on MODIS heritage. However, VIIRS has no onboard calibrator similar to the spectro-radiometric calibration assembly (SRCA) on MODIS to perform the sensor on-orbit spatial characterization of band-to-band registration (BBR) and modulation transfer function (MTF). The Moon has been known as a spectrally, radiometrically, and geometrically stable source that can be used for sensor on-orbit calibration and characterization. In this letter, the algorithms developed and validated for MODIS spatial characterization using the Moon are briefly summarized and extended to VIIRS. The BBR in both along-scan and along-track directions and the MTF in the along-track direction are calculated with the scheduled VIIRS lunar observations and presented. These early results confirm that the VIIRS spatial characterization parameters have been stable since launch and are within the performance specification. The along-scan MTF cannot be accurately determined using the same algorithm and is not included in this study because the movement of the Moon in this direction is too limited to construct an edge spread function for MTF derivation. As part of the VIIRS on-orbit calibration and validation effort, the BBR and MTF parameters will be continuously monitored and evaluated throughout its mission lifetime. C1 [Wang, Zhipeng] Sigma Space Corp, Lanham, MD 20706 USA. [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wang, ZP (reprint author), Sigma Space Corp, Lanham, MD 20706 USA. EM zhipeng.wang@sigmaspace.com; Xiaoxiong.Xiong-1@nasa.gov OI Wang, Zhipeng/0000-0002-9108-9009 NR 14 TC 5 Z9 5 U1 0 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD JUN PY 2014 VL 11 IS 6 BP 1116 EP 1120 DI 10.1109/LGRS.2013.2287791 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AA5NJ UT WOS:000331146200018 ER PT J AU Yatheendradas, S Narapusetty, B Peters-Lidard, C Funk, C Verdin, J AF Yatheendradas, Soni Narapusetty, Balachandrudu Peters-Lidard, Christa Funk, Christopher Verdin, James TI Comment on 'Shang S. 2012. Calculating actual crop evapotranspiration under soil water stress conditions with appropriate numerical methods and time step. Hydrological Processes 26: 3338-3343. DOI: 10.1002/hyp.8405' SO HYDROLOGICAL PROCESSES LA English DT Editorial Material DE numerical method; crop; evapotranspiration; water stress AB A previous study analyzed errors in the numerical calculation of actual crop evapotranspiration (ETa) under soil water stress. Assuming no irrigation or precipitation, it constructed equations for ETa over limited soil-water ranges in a root zone drying out due to evapotranspiration. It then used a single crop-soil composite to provide recommendations about the appropriate usage of numerical methods under different values of the time step and the maximum crop evapotranspiration (ETc). This comment reformulates those ETa equations for applicability over the full range of soil water values, revealing a dependence of the relative error in numerical ETa on the initial soil water that was not seen in the previous study. It is shown that the recommendations based on a single crop-soil composite can be invalid for other crop-soil composites. Finally, a consideration of the numerical error in the time-cumulative value of ETa is discussed besides the existing consideration of that error over individual time steps as done in the previous study. This cumulative ETa is more relevant to the final crop yield. Published 2014. This article is a U.S. Government work and is in the public domain in the USA. C1 [Yatheendradas, Soni] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Yatheendradas, Soni; Narapusetty, Balachandrudu; Peters-Lidard, Christa] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Narapusetty, Balachandrudu] Sci Applicat Int Corp, Beltsville, MD 20705 USA. [Funk, Christopher] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA. [Funk, Christopher; Verdin, James] USGS, Earth Resources Observat Syst EROS Data Ctr, Sioux Falls, SD 57198 USA. RP Yatheendradas, S (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. EM soni.yatheendradas@nasa.gov RI Peters-Lidard, Christa/E-1429-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876 NR 5 TC 0 Z9 0 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 MAY 30 PY 2014 VL 28 IS 11 BP 3833 EP 3840 DI 10.1002/hyp.10138 PG 8 WC Water Resources SC Water Resources GA AH4YY UT WOS:000336136300013 ER PT J AU Urquhart, EA Zaitchik, BF Waugh, DW Guikema, SD Del Castillo, CE AF Urquhart, Erin A. Zaitchik, Benjamin F. Waugh, Darryn W. Guikema, Seth D. Del Castillo, Carlos E. TI Uncertainty in Model Predictions of Vibrio vulnificus Response to Climate Variability and Change: A Chesapeake Bay Case Study SO PLOS ONE LA English DT Article ID SEASONAL DYNAMICS; COASTAL WATERS; UNITED-STATES; PARAHAEMOLYTICUS; SALINITY; CHOLERAE; INFECTIONS; OYSTERS; ECOLOGY AB The effect that climate change and variability will have on waterborne bacteria is a topic of increasing concern for coastal ecosystems, including the Chesapeake Bay. Surface water temperature trends in the Bay indicate a warming pattern of roughly 0.3-0.4 degrees C per decade over the past 30 years. It is unclear what impact future warming will have on pathogens currently found in the Bay, including Vibrio spp. Using historical environmental data, combined with three different statistical models of Vibrio vulnificus probability, we explore the relationship between environmental change and predicted Vibrio vulnificus presence in the upper Chesapeake Bay. We find that the predicted response of V. vulnificus probability to high temperatures in the Bay differs systematically between models of differing structure. As existing publicly available datasets are inadequate to determine which model structure is most appropriate, the impact of climatic change on the probability of V. vulnificus presence in the Chesapeake Bay remains uncertain. This result points to the challenge of characterizing climate sensitivity of ecological systems in which data are sparse and only statistical models of ecological sensitivity exist. C1 [Urquhart, Erin A.; Zaitchik, Benjamin F.; Waugh, Darryn W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Guikema, Seth D.] Johns Hopkins Univ, Dept Geog & Environm Engn, Baltimore, MD 21218 USA. [Del Castillo, Carlos E.] NASA, Ocean Ecol Lab, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Urquhart, EA (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. EM erinu@jhu.edu RI Urquhart, Erin/A-2336-2015; Waugh, Darryn/K-3688-2016 OI Urquhart, Erin/0000-0001-7141-9499; Waugh, Darryn/0000-0001-7692-2798 FU Johns Hopkins University Department of Earth and Planetary Sciences FX This work was financially supported by the Johns Hopkins University Department of Earth and Planetary Sciences. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 37 TC 5 Z9 5 U1 0 U2 17 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 29 PY 2014 VL 9 IS 5 AR e98256 DI 10.1371/journal.pone.0098256 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AI3UR UT WOS:000336790800029 PM 24874082 ER PT J AU Goossens, S Sabaka, TJ Nicholas, JB Lemoine, FG Rowlands, DD Mazarico, E Neumann, GA Smith, DE Zuber, MT AF Goossens, Sander Sabaka, Terence J. Nicholas, Joseph B. Lemoine, Frank G. Rowlands, David D. Mazarico, Erwan Neumann, Gregory A. Smith, David E. Zuber, Maria T. TI High-resolution local gravity model of the south pole of the Moon from GRAIL extended mission data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE lunar gravity; local analysis; GRAIL; planetary geodesy ID TRACKING DATA; MASS ANOMALIES; FIELD; LINE; GANYMEDE; SPHERE AB We estimated a high-resolution local gravity field model over the south pole of the Moon using data from the Gravity Recovery and Interior Laboratory's extended mission. Our solution consists of adjustments with respect to a global model expressed in spherical harmonics. The adjustments are expressed as gridded gravity anomalies with a resolution of 1/6 degrees by 1/6 degrees (equivalent to that of a degree and order 1080 model in spherical harmonics), covering a cap over the south pole with a radius of 40 degrees. The gravity anomalies have been estimated from a short-arc analysis using only Ka-band range-rate (KBRR) data over the area of interest. We apply a neighbor-smoothing constraint to our solution. Our local model removes striping present in the global model; it reduces the misfit to the KBRR data and improves correlations with topography to higher degrees than current global models. C1 [Goossens, Sander] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21228 USA. [Goossens, Sander; Sabaka, Terence J.; Nicholas, Joseph B.; Lemoine, Frank G.; Rowlands, David D.; Mazarico, Erwan; Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nicholas, Joseph B.] Emergent Space Technol, Greenbelt, MD USA. [Mazarico, Erwan; Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. RP Goossens, S (reprint author), Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21228 USA. EM sander.j.goossens@nasa.gov RI Mazarico, Erwan/N-6034-2014; Lemoine, Frank/D-1215-2013; Rowlands, David/D-2751-2012; Neumann, Gregory/I-5591-2013; Goossens, Sander/K-2526-2015 OI Mazarico, Erwan/0000-0003-3456-427X; Neumann, Gregory/0000-0003-0644-9944; Goossens, Sander/0000-0002-7707-1128 FU GRAIL Project under the auspices of the NASA Discovery Program; Jet Propulsion Laboratory, California Institute of Technology FX The data used in this analysis are available at the Geosciences Node of the Planetary Data System (http://pds-geosciences.wustl.edu/missions/grail/default.htm). This work was supported by the GRAIL Project under the auspices of the NASA Discovery Program, performed under contract to the Massachusetts Institute of Technology and the Jet Propulsion Laboratory, California Institute of Technology. This work made extensive use of the supercomputers of the NASA Center for Climate Simulation (NCCS) at NASA Goddard Space Flight Center, and we acknowledge their support. Localized correlations were computed using the freely available SHTOOLS library (http://shtools.ipgp.fr). All figures were generated with the free Generic Mapping Tools (GMT) software [Wessel and Smith, 1991]. NR 35 TC 1 Z9 1 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2014 VL 41 IS 10 BP 3367 EP 3374 DI 10.1002/2014GL060178 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AJ4AC UT WOS:000337610200007 ER PT J AU Wilson, RJ Guzewich, SD AF Wilson, R. John Guzewich, Scott D. TI Influence of water ice clouds on nighttime tropical temperature structure as seen by the Mars Climate Sounder SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Mars; atmosphere; clouds; tides ID ATMOSPHERE AB An analysis of nighttime temperature and water ice cloud extinction profiles from the Mars Climate Sounder aboard the Mars Reconnaissance Orbiter provides evidence for the close relationship between tropical temperature structure and water ice clouds. The tropical temperature structure that evolves over the spring and summer seasons is closely coupled to the waxing and waning of tropical cloud activity. The presence of strong elevated nighttime temperature inversions in the Tharsis region is a robust feature of the equatorial atmosphere during the L-s=0-135 degrees season, with little interannual variation seen in the three Mars years examined. Mars global circulation model simulations imply that cloud radiative forcing plays a dominant role in the seasonal modulation of the observed longitude distribution of warm and cold anomalies in surface and low-altitude air temperatures, respectively. C1 [Wilson, R. John] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA. [Guzewich, Scott D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wilson, RJ (reprint author), NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA. EM John.Wilson@noaa.gov OI Guzewich, Scott/0000-0003-1149-7385 FU NASA FX The MCS temperature and clouds data are archived in the Planetary Data System. MGCM results are available from the authors upon request. This work was supported by grants from the NASA Planetary Atmospheres and Mars Data Analysis programs. Guzewich was supported by a NASA Postdoctoral Fellowship. We thank Ehouarn Millour and Francois Forget for access to data from the version 5 LMD Mars Climate Database. NR 18 TC 10 Z9 10 U1 3 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2014 VL 41 IS 10 BP 3375 EP 3381 DI 10.1002/2014GL060086 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AJ4AC UT WOS:000337610200008 ER PT J AU Lemoine, FG Goossens, S Sabaka, TJ Nicholas, JB Mazarico, E Rowlands, DD Loomis, BD Chinn, DS Neumann, GA Smith, DE Zuber, MT AF Lemoine, Frank G. Goossens, Sander Sabaka, Terence J. Nicholas, Joseph B. Mazarico, Erwan Rowlands, David D. Loomis, Bryant D. Chinn, Douglas S. Neumann, Gregory A. Smith, David E. Zuber, Maria T. TI GRGM900C: A degree 900 lunar gravity model from GRAIL primary and extended mission data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE lunar gravity; orbit determination; KBRR data; planetary geodesy; GRAIL; Moon ID RECOVERY; CRUST; FIELD; MOON AB We have derived a gravity field solution in spherical harmonics to degree and order 900, GRGM900C, from the tracking data of the Gravity Recovery and Interior Laboratory (GRAIL) Primary (1 March to 29 May 2012) and Extended Missions (30 August to 14 December 2012). A power law constraint of 3.6 x10(-4)/l(2) was applied only for degree l greater than 600. The model produces global correlations of gravity, and gravity predicted from lunar topography of >= 0.98 through degree 638. The model's degree strength varies from a minimum of 575-675 over the central nearside and farside to 900 over the polar regions. The model fits the Extended Mission Ka-Band Range Rate data through 17 November 2012 at 0.13 mu m/s RMS, whereas the last month of Ka-Band Range-Rate data obtained from altitudes of 2-10 km fit at 0.98 mu m/s RMS, indicating that there is still signal inherent in the tracking data beyond degree 900. C1 [Lemoine, Frank G.; Goossens, Sander; Sabaka, Terence J.; Nicholas, Joseph B.; Mazarico, Erwan; Rowlands, David D.; Loomis, Bryant D.; Chinn, Douglas S.; Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Goossens, Sander] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21228 USA. [Nicholas, Joseph B.] Emergent Space Technol, Greenbelt, MD USA. [Mazarico, Erwan; Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [Loomis, Bryant D.; Chinn, Douglas S.] Stinger Ghaffarian Technol Inc, Greenbelt, MD USA. RP Lemoine, FG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Frank.G.Lemoine@nasa.gov RI Mazarico, Erwan/N-6034-2014; Lemoine, Frank/D-1215-2013; Rowlands, David/D-2751-2012; Neumann, Gregory/I-5591-2013; Goossens, Sander/K-2526-2015 OI Mazarico, Erwan/0000-0003-3456-427X; Neumann, Gregory/0000-0003-0644-9944; Goossens, Sander/0000-0002-7707-1128 FU GRAIL Project; NASA Discovery Program FX The work described herein was supported by the GRAIL Project and the NASA Discovery Program. We acknowledge Gerhard Kruizinga and his team at the Jet Propulsion Laboratory (JPL) for their meticulous work in developing the GRAIL Level 1B data sets. We also acknowledge the NASA Center for Climate Simulation (NCCS) at the NASA Goddard Space Flight Center for their assistance in optimizing the performance of the supercomputers to obtain the GRAIL degree 900 solutions. The GRAIL Level 1B data used in this study are available from the Geosciences Node of the Planetary Data System http://pds-geosciences.wustl.edu/missions/grail/default.htm. NR 30 TC 32 Z9 33 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2014 VL 41 IS 10 BP 3382 EP 3389 DI 10.1002/2014GL060027 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AJ4AC UT WOS:000337610200009 ER PT J AU de Viron, O Dickey, JO AF de Viron, O. Dickey, J. O. TI The two types of El-Nino and their impacts on the length of day SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Earth rotation; El Nino; torque approach; length of day ID ATMOSPHERIC ANGULAR-MOMENTUM; OF-DAY VARIATION; SOUTHERN-OSCILLATION; PACIFIC; WINTER; TORQUES; EVENTS; ENSO AB At the interannual to decadal time scale, the changes in the Earth rotation rate are linked with the El-Nino-Southern Oscillation phenomena through changes in the atmospheric angular momentum. As climatic studies demonstrate that there were two types of El-Nino events, namely, eastern Pacific (EP) and central Pacific (CP) events, we investigate how each of them affects the atmospheric angular momentum. We show in particular that EP events are associated with stronger variations of the atmospheric angular momentum and length of day. We explain this difference by the stronger pressure gradient over the major mountain ranges, due to a stronger and more efficiently localized pressure dipole over the Pacific Ocean in the case of EP events. C1 [de Viron, O.] Univ Paris Diderot, Sorbonne Paris Cite, Paris, France. [de Viron, O.] Inst Phys Globe Paris, UMR7159, Paris, France. [Dickey, J. O.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP de Viron, O (reprint author), Univ La Rochelle, CNRS, UMR Littoral Environm & Soc LIENSs 7266, La Rochelle, France. EM deviron@ipgp.fr RI de Viron, Olivier/N-6647-2014 OI de Viron, Olivier/0000-0003-3112-9686 FU CNES through the TOSCA program; Institut Universitaire de France (OdV); National Aeronautics and Space Administration (NASA) FX We gratefully acknowledge discussions with Tong Lee regarding the two ENSO-type literatures. This study was supported by the CNES through the TOSCA program and by the Institut Universitaire de France (OdV). The work of J.O.D is a phase of research carried out at the Jet Propulsion Laboratory, California Institute of Technology, sponsored by the National Aeronautics and Space Administration (NASA). It is a pleasure to thank the Editor (Eric Calais) and two anonymous reviewers for their help in improving the paper. NR 28 TC 2 Z9 2 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2014 VL 41 IS 10 BP 3407 EP 3412 DI 10.1002/2014GL059948 PG 6 WC Geosciences, Multidisciplinary SC Geology GA AJ4AC UT WOS:000337610200012 ER PT J AU Rignot, E Mouginot, J Morlighem, M Seroussi, H Scheuchl, B AF Rignot, E. Mouginot, J. Morlighem, M. Seroussi, H. Scheuchl, B. TI Widespread, rapid grounding line retreat of Pine Island, Thwaites, Smith, and Kohler glaciers, West Antarctica, from 1992 to 2011 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Antarctica; mass balance; interferometry; glacier dynamics; marine instability ID ICE-SHELF; MASS-LOSS; STABILITY; BED; ACCELERATION; GREENLAND; SHEETS AB We measure the grounding line retreat of glaciers draining the Amundsen Sea sector of West Antarctica using Earth Remote Sensing (ERS-1/2) satellite radar interferometry from 1992 to 2011. Pine Island Glacier retreated 31 km at its center, with most retreat in 2005-2009 when the glacier ungrounded from its ice plain. Thwaites Glacier retreated 14 km along its fast flow core and 1 to 9 km along the sides. Haynes Glacier retreated 10 km along its flanks. Smith/Kohler glaciers retreated the most, 35 km along its ice plain, and its ice shelf pinning points are vanishing. These rapid retreats proceed along regions of retrograde bed elevation mapped at a high spatial resolution using a mass conservation technique that removes residual ambiguities from prior mappings. Upstream of the 2011 grounding line positions, we find no major bed obstacle that would prevent the glaciers from further retreat and draw down the entire basin. C1 [Rignot, E.; Mouginot, J.; Morlighem, M.; Scheuchl, B.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Rignot, E.; Seroussi, H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Rignot, E (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. EM erignot@uci.edu RI Morlighem, Mathieu/O-9942-2014; Mouginot, Jeremie/G-7045-2015; Rignot, Eric/A-4560-2014; OI Morlighem, Mathieu/0000-0001-5219-1310; Rignot, Eric/0000-0002-3366-0481; Mouginot, Jeremie/0000-0001-9155-5455 FU National Aeronautics and Space Administration FX We thank two anonymous reviewers for their comments on the manuscript. Grounding line positions and ice velocities are available at the National Snow and Ice Data Center as part of the NASA MeASUREs project. Reconstruction of bed topography is available upon request from the authors until a finished, larger scale product is posted at NSIDC. This work was performed at the University of California Irvine and at the Jet Propulsion Laboratory, California Institute of Technology under a grant from the National Aeronautics and Space Administration's Cryospheric Science Program and Interdisciplinary Science Program. NR 32 TC 149 Z9 151 U1 8 U2 94 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2014 VL 41 IS 10 BP 3502 EP 3509 DI 10.1002/2014GL060140 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AJ4AC UT WOS:000337610200024 ER PT J AU Kang, D Lee, MI Im, J Kim, D Kim, HM Kang, HS Schubert, SD Arribas, A MacLachlan, C AF Kang, Daehyun Lee, Myong-In Im, Jungho Kim, Daehyun Kim, Hye-Mi Kang, Hyun-Suk Schubert, Siegfried D. Arribas, Alberto MacLachlan, Craig TI Prediction of the Arctic Oscillation in boreal winter by dynamical seasonal forecasting systems SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE coupled models of the climate system; climate variability ID UNIFIED PARAMETERIZATION; CLIMATE VARIABILITY; OROGRAPHIC DRAG; ANNULAR MODES; UNITED-STATES; PART I; TEMPERATURE; PREDICTABILITY; EXTREMES; EVENTS AB This study assesses the skill of boreal winter Arctic Oscillation (AO) predictions with state-of-the-art dynamical ensemble prediction systems (EPSs): GloSea4, CFSv2, GEOS-5, CanCM3, CanCM4, and CM2.1. Long-term reforecasts with the EPSs are used to evaluate how well they represent the AO and to assess the skill of both deterministic and probabilistic forecasts of the AO. The reforecasts reproduce the observed changes in the large-scale patterns of the Northern Hemispheric surface temperature, upper level wind, and precipitation associated with the different phases of the AO. The results demonstrate that most EPSs improve upon persistence skill scores for lead times up to 2months in boreal winter, suggesting some potential for skillful prediction of the AO and its associated climate anomalies at seasonal time scales. It is also found that the skill of AO forecasts during the recent period (1997-2010) is higher than that of the earlier period (1983-1996). C1 [Kang, Daehyun; Lee, Myong-In; Im, Jungho] Ulsan Natl Inst Sci & Technol, Sch Urban & Environm Engn, Ulsan, South Korea. [Kim, Daehyun] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Kim, Hye-Mi] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. [Kang, Hyun-Suk] Korea Meteorol Adm, Climate Res Div, Seoul, South Korea. [Schubert, Siegfried D.] NASA Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA. [Arribas, Alberto; MacLachlan, Craig] Met Off Hadley Ctr, Exeter, Devon, England. RP Lee, MI (reprint author), Ulsan Natl Inst Sci & Technol, Sch Urban & Environm Engn, Ulsan, South Korea. EM milee@unist.ac.kr OI Im, Jungho/0000-0002-4506-6877; Lee, Myong-In/0000-0001-8983-8624 FU Korea Meteorological Administration Research and Development Program [APCC 2013-3141] FX This study was supported by the Korea Meteorological Administration Research and Development Program under grant APCC 2013-3141. The authors are grateful for the computing resources provided by the Supercomputing Center at Korea Institute of Science and Technology Information (KSC-2013-C2-011). NR 33 TC 15 Z9 15 U1 1 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2014 VL 41 IS 10 BP 3577 EP 3585 DI 10.1002/2014GL060011 PG 9 WC Geosciences, Multidisciplinary SC Geology GA AJ4AC UT WOS:000337610200035 ER PT J AU Su, H Jiang, JH Zhai, CX Shen, TJ Neelin, JD Stephens, GL Yung, YL AF Su, Hui Jiang, Jonathan H. Zhai, Chengxing Shen, Tsaepyng J. Neelin, J. David Stephens, Graeme L. Yung, Yuk L. TI Weakening and strengthening structures in the Hadley Circulation change under global warming and implications for cloud response and climate sensitivity SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SEA-SURFACE TEMPERATURE; INTERANNUAL VARIABILITY; SATELLITE-OBSERVATIONS; TROPICAL CIRCULATION; SOUTHERN-OCEAN; FEEDBACKS; MODEL; PRECIPITATION; FUTURE; ATMOSPHERE AB It has long been recognized that differences in climate model-simulated cloud feedbacks are a primary source of uncertainties for the model-predicted surface temperature change induced by increasing greenhouse gases such as CO2. Large-scale circulation broadly determines when and where clouds form and how they evolve. However, the linkage between large-scale circulation change and cloud radiative effect (CRE) change under global warming has not been thoroughly studied. By analyzing 15 climate models, we show that the change of the Hadley Circulation exhibits meridionally varying weakening and strengthening structures, physically consistent with the cloud changes in distinct cloud regimes. The regions that experience a weakening (strengthening) of the zonal-mean circulation account for 54% (46%) of the multimodel-mean top-of-atmosphere (TOA) CRE change integrated over 45 degrees S-40 degrees N. The simulated Hadley Circulation structure changes per degree of surface warming differ greatly between the models, and the intermodel spread in the Hadley Circulation change is well correlated with the intermodel spread in the TOA CRE change. This correlation underscores the close interactions between large-scale circulation and clouds and suggests that the uncertainties of cloud feedbacks and climate sensitivity reside in the intimate coupling between large-scale circulation and clouds. New model performance metrics proposed in this work, which emphasize how models reproduce satellite-observed spatial variations of zonal-mean cloud fraction and relative humidity associated with the Hadley Circulation, indicate that the models closer to the satellite observations tend to have equilibrium climate sensitivity higher than the multimodel mean. C1 [Su, Hui; Jiang, Jonathan H.; Zhai, Chengxing; Shen, Tsaepyng J.; Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Neelin, J. David] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Su, H (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Hui.Su@jpl.nasa.gov FU NASA NEWS program; NASA COUND program; NASA AST program; Aura MLS project; CloudSat project; NOAA [NA11OAR4310099]; NSF [AGS-1102838]; University of Houston [UHOUST.130027]; NASA FX We are thankful to Jay Mace, Eric J. Fetzer, and William G. Read for helpful discussions of data quality. Discussions with Kevin Bowman, Duane Waliser, and Michael Gunson are appreciated. This paper is greatly improved owing to the detailed comments and constructive suggestions by Mark Zelinka and two other reviewers. We acknowledge the World Climate Research Programme's Working Group on Coupled Modelling, which is responsible for CMIP. We thank the climate modeling groups listed in Table 1 for producing and making available their model output. The U.S. Department of Energy (DOE) Program for Climate Model Diagnosis and Intercomparison provides coordinating support and led development of software infrastructure in partnership with the Global Organization for Earth System Science Portals. The A-Train satellite data are available at NASA Distributed Active Archive Centers (DAAC). H. S., J. H. J., C.Z., and J. T. S. acknowledge funding support from NASA NEWS, COUND, and AST programs and Aura MLS and CloudSat projects. J.D.N. was supported by NOAA NA11OAR4310099 and NSF AGS-1102838. Y.L.Y. was supported by UHOUST.130027 subcontract from the University of Houston. This work was performed at Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 64 TC 25 Z9 25 U1 0 U2 27 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2014 VL 119 IS 10 BP 5787 EP 5805 DI 10.1002/2014JD021642 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ5YQ UT WOS:000337766600003 ER PT J AU Wang, JF Bras, RL Nieves, V Deng, Y AF Wang, Jingfeng Bras, Rafael L. Nieves, Veronica Deng, Yi TI A model of energy budgets over water, snow, and ice surfaces SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ATMOSPHERE RESPONSE EXPERIMENT; HEAT-FLUX; SOIL-MOISTURE; TOGA COARE; COOL-SKIN; BULK PARAMETERIZATION; SOLAR IRRADIANCE; TURBULENT HEAT; OCEAN; TEMPERATURE AB The recently formulated maximum entropy production (MEP) model over land surfaces has been generalized to water-snow-ice surfaces. Analytical solutions of energy budget in terms of the partition of surface radiative fluxes into (turbulent and/or conductive) heat fluxes at the earth-atmosphere interface are derived as functions of surface temperature (e. g., sea surface temperature). The MEP model does not require data of wind speed, air temperature-humidity, and surface roughness. Test of the MEP model using observations from several field experiments is encouraging. Potential applications of the proposed model for understanding long-term trends in surface heat fluxes and for closing global surface energy budget at the Earth's atmosphere are suggested. C1 [Wang, Jingfeng; Bras, Rafael L.; Deng, Yi] Georgia Inst Technol, Atlanta, GA 30332 USA. [Nieves, Veronica] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Wang, JF (reprint author), Georgia Inst Technol, Atlanta, GA 30332 USA. EM jingfeng.wang@ce.gatech.edu FU NSF [EAR-0943356, EAR-1138611]; ARO [W911NF-10-1-0236/W911NF-12-1-0095] FX This work was supported by NSF grants EAR-0943356 and EAR-1138611 and ARO grants W911NF-10-1-0236/W911NF-12-1-0095. We thank Judith A. Curry of Georgia Institute of Technology and Carol Anne Clayson of Florida State University for their generosity in preparing the SEAFLUX data product, Sven Halldin of Uppsala University to provide the NOPEX data product, and Chris W. Fairall of NOAA ESRL to offer the CALNEX 2010 cruise air-sea fluxes data used in this study. We thank Charmaine Hrynkiw of Meteorological Service of Canada, Betsy Sheffield of NSIDC User Service at University of Colorado, and Mary J. Saddington of NASA Langley ASDC User Service for making the FLUXNET data available. We are grateful to Soroosh Sorooshian and Dan Braithwaite for providing computer support at University of California at Irvine where part of the work reported in this paper was conducted. The comments of two anonymous reviewers greatly improved the quality of this paper. NR 75 TC 3 Z9 3 U1 2 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2014 VL 119 IS 10 BP 6034 EP 6051 DI 10.1002/2013JD021150 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ5YQ UT WOS:000337766600019 ER PT J AU Saraiva, ACV Campos, LZS Williams, ER Zepka, GS Alves, J Pinto, O Heckman, S Buzato, TS Bailey, JC Morales, CA Blakeslee, RJ AF Saraiva, A. C. V. Campos, L. Z. S. Williams, E. R. Zepka, G. S. Alves, J. Pinto, O., Jr. Heckman, S. Buzato, T. S. Bailey, J. C. Morales, C. A. Blakeslee, R. J. TI High-speed video and electromagnetic analysis of two natural bipolar cloud-to-ground lightning flashes SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID HOKURIKU DISTRICT; NEW-MEXICO; THUNDERSTORMS; DISCHARGES; COMPONENTS; CURRENTS; LEADERS AB High-speed video records of two bipolar cloud-to-ground flashes were analyzed in detail. They both began with a single positive return stroke that was followed by more than one subsequent weak negative stroke. Due to the elevated cloud base height of its parent thunderstorm, the preparatory processes of each subsequent negative stroke were documented optically below cloud base. In the first event (Case 1) it was observed that all four subsequent negative strokes were initiated by recoil leaders that retraced one horizontal channel segment previously ionized by the positive leader. Those recoil leaders connected to the original vertical channel segment and propagated toward ground, producing four subsequent strokes that had the same ground contact point as the original positive discharge. The second event (Case 2), in contrast, presented 15 subsequent strokes that were initiated by recoil leaders that did not reach the original channel of the positive stroke. They diverged vertically toward ground, making contact approximately 11 km away from the original positive strike point. These results constitute the first optical evidence that both single-and multiple-channel bipolar flashes occur as a consequence of recoil leader activity in the branches of the initial positive return stroke. For both events their total channel length increased continuously at a rate of the order of 10(4) m s(-1), comparable to speeds reported for typical positive leaders. C1 [Saraiva, A. C. V.; Campos, L. Z. S.; Zepka, G. S.; Alves, J.; Pinto, O., Jr.; Buzato, T. S.] Natl Inst Space Res, Sao Jose Dos Campos, Brazil. [Williams, E. R.] MIT, Dept Civil & Environm Engn, Cambridge, MA 02139 USA. [Heckman, S.] Earth Networks, Germantown, MD USA. [Bailey, J. C.] Univ Alabama, Earth Syst Sci Ctr, Huntsville, AL 35899 USA. [Morales, C. A.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Sao Paulo, Brazil. [Blakeslee, R. J.] NASA Marshall Space Flight Ctr, Huntsville, AL USA. RP Saraiva, ACV (reprint author), Natl Inst Space Res, Sao Jose Dos Campos, Brazil. EM acvsaraiva@gmail.com RI Campos, Leandro/F-3435-2010; Saraiva, Antonio/G-6400-2013 OI Campos, Leandro/0000-0002-0173-3199; Saraiva, Antonio/0000-0001-6036-7611 FU FAPESP [08/56711-4, 2010/01742-2]; CHUVA project [FAPESP 2009/15235-8] FX The authors would like to thank FAPESP for their financial support under the projects 08/56711-4 and 2010/01742-2. This work was also partially supported by the CHUVA project (project FAPESP 2009/15235-8). We specially thank UNIVAP (Universidade do Vale do Paraiba) and Rede Vanguarda de Televisao for their support in hosting the sensors during the observations and helping with maintenance. The authors are also grateful to all CHUVA participants responsible for the installation and maintenance of the several sensors present at the 2012 campaign and whose data were vital to the development of this work. NR 55 TC 9 Z9 9 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2014 VL 119 IS 10 BP 6105 EP 6127 DI 10.1002/2013JD020974 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ5YQ UT WOS:000337766600023 ER PT J AU Wu, XQ Liu, QH Zeng, J Grotenhuis, M Qian, HF Caponi, M Flynn, L Jaross, G Sen, B Buss, RH Johnsen, W Janz, S Pan, CH Niu, JG Beck, T Beach, E Yu, W Raja, MKRV Stuhmer, D Cumpton, D Owen, C Li, WH AF Wu, Xiangqian Liu, Quanhua Zeng, Jian Grotenhuis, Michael Qian, Haifeng Caponi, Maria Flynn, Larry Jaross, Glen Sen, Bhaswar Buss, Richard H., Jr. Johnsen, William Janz, Scott Pan, Chunhui Niu, Jianguo Beck, Trevor Beach, Eric Yu, Wei Raja, M. K. Rama Varma Stuhmer, Derek Cumpton, Daniel Owen, Cristina Li, Wen-Hao TI Evaluation of the Sensor Data Record from the nadir instruments of the Ozone Mapping Profiler Suite (OMPS) SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Editorial Material ID RADIATIVE-TRANSFER MODEL; INFRARED CHANNELS; INTER-CALIBRATION; PERFORMANCE; RETRIEVAL; SYSTEM AB This paper evaluates the first 15 months of the Ozone Mapping and Profiler Suite (OMPS) Sensor Data Record (SDR) acquired by the nadir sensors and processed by the National Oceanic and Atmospheric Administration Interface Data Processing Segment. The evaluation consists of an inter-comparison with a similar satellite instrument, an analysis using a radiative transfer model, and an assessment of product stability. This is in addition to the evaluation of sensor calibration and the Environment Data Record product that are also reported in this Special Issue. All these are parts of synergetic effort to provide comprehensive assessment at every level of the products to ensure its quality. It is found that the OMPS nadir SDR quality is satisfactory for the current Provisional maturity. Methods used in the evaluation are being further refined, developed, and expanded, in collaboration with international community through the Global Space-based Inter-Calibration System, to support the upcoming long-term monitoring. C1 [Wu, Xiangqian; Flynn, Larry; Beck, Trevor] NOAA NESDIS, Ctr Satellite Applicat & Res, College Pk, MD 20740 USA. [Liu, Quanhua; Pan, Chunhui] Univ Maryland, Cooperat Inst Climate & Satellites, College Pk, MD 20742 USA. [Zeng, Jian; Grotenhuis, Michael] NOAA NESDIS, Ctr Satellite Applicat & Res, ERT Inc, College Pk, MD USA. [Qian, Haifeng; Beach, Eric; Yu, Wei] NOAA NESDIS, Ctr Satellite Applicat & Res, IMSG Inc, College Pk, MD USA. [Caponi, Maria] SEAMM S Caponi & Associates, Manhattan Beach, CA USA. [Jaross, Glen; Janz, Scott] NASA GSFC, Greenbelt, MD USA. [Sen, Bhaswar; Li, Wen-Hao] Northrop Grumman Aerosp Syst, Redondo Beach, CA USA. [Buss, Richard H., Jr.] Innovim, Lanham, MD USA. [Johnsen, William; Cumpton, Daniel] Raytheon Co, Raytheon Intelligence, Informat & Serv, Aurora, CO USA. [Niu, Jianguo] NOAA NESDIS, Ctr Satellite Applicat & Res, SRG, College Pk, MD USA. [Raja, M. K. Rama Varma] Sci Syst & Applicat Inc, Lanham, MD USA. [Stuhmer, Derek; Owen, Cristina] Raytheon Intelligence, Informat & Serv, Omaha, NE USA. RP Wu, XQ (reprint author), NOAA NESDIS, Ctr Satellite Applicat & Res, College Pk, MD 20740 USA. EM Xiangqian.Wu@noaa.gov RI Grotenhuis, Michael/G-1195-2010; Flynn, Lawrence/B-6321-2009; Liu, Quanhua/B-6608-2008; Beach, Eric/F-5576-2010; Qian, Haifeng/F-1987-2011; Wu, Xiangqian/F-5634-2010 OI Grotenhuis, Michael/0000-0002-6236-864X; Flynn, Lawrence/0000-0001-6856-2614; Liu, Quanhua/0000-0002-3616-351X; Wu, Xiangqian/0000-0002-7804-5650 NR 34 TC 5 Z9 5 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2014 VL 119 IS 10 BP 6170 EP 6180 DI 10.1002/2013JD020484 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ5YQ UT WOS:000337766600027 ER PT J AU Stolarski, RS Waugh, DW Wang, L Oman, LD Douglass, AR Newman, PA AF Stolarski, Richard S. Waugh, Darryn W. Wang, Lei Oman, Luke D. Douglass, Anne R. Newman, Paul A. TI Seasonal variation of ozone in the tropical lower stratosphere: Southern tropics are different from northern tropics SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TRACER TRANSPORT; ANNUAL CYCLE; PIPE MODEL; TROPOPAUSE; VARIABILITY; AGE; CIRCULATION; AIR AB We examine the seasonal behavior of ozone by using measurements from various instruments including ozonesondes, Aura Microwave Limb Sounder, and Stratospheric Aerosol and Gas Experiment II. We find that the magnitude of the annual variation in ozone, as a percentage of the mean ozone, exhibits a maximum at or slightly above the tropical tropopause. The maximum is larger in the northern tropics than in the southern tropics, and the annual maximum of ozone in the southern tropics occurs 2 months later than that in the northern tropics, in contrast to usual assumption that the tropics can be treated as a horizontally homogeneous region. The seasonal cycles of ozone and other species in this part of the lower stratosphere result from a combination of the seasonal variation of the Brewer-Dobson circulation and the seasonal variation of tropical and midlatitude mixing. In the Northern Hemisphere, the impacts of upwelling and mixing between the tropics and midlatitudes on ozone are in phase and additive. In the Southern Hemisphere, they are not in phase. We apply a tropical leaky pipe model independently to each hemisphere to examine the relative roles of upwelling and mixing in the northern and southern tropical regions. Reasonable assumptions of the seasonal variation of upwelling and mixing yield a good description of the seasonal magnitude and phase in both the southern and northern tropics. The differences in the tracers and transport between the northern and southern tropical stratospheres suggest that the paradigm of well-mixed tropics needs to be revised to consider latitudinal variations within the tropics. C1 [Stolarski, Richard S.; Waugh, Darryn W.; Wang, Lei] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Oman, Luke D.; Douglass, Anne R.; Newman, Paul A.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. RP Stolarski, RS (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. EM rstolar1@jhu.edu RI Oman, Luke/C-2778-2009; Stolarski, Richard/B-8499-2013; Douglass, Anne/D-4655-2012; Wang, Lei/F-1269-2015; Waugh, Darryn/K-3688-2016 OI Oman, Luke/0000-0002-5487-2598; Stolarski, Richard/0000-0001-8722-4012; Wang, Lei/0000-0002-1618-1796; Waugh, Darryn/0000-0001-7692-2798 NR 33 TC 8 Z9 8 U1 0 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2014 VL 119 IS 10 BP 6196 EP 6206 DI 10.1002/2013JD021294 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ5YQ UT WOS:000337766600029 ER PT J AU Kim, D Chin, M Yu, HB Diehl, T Tan, Q Kahn, RA Tsigaridis, K Bauer, SE Takemura, T Pozzoli, L Bellouin, N Schulz, M Peyridieu, S Chedin, A Koffi, B AF Kim, Dongchul Chin, Mian Yu, Hongbin Diehl, Thomas Tan, Qian Kahn, Ralph A. Tsigaridis, Kostas Bauer, Susanne E. Takemura, Toshihiko Pozzoli, Luca Bellouin, Nicolas Schulz, Michael Peyridieu, Sophie Chedin, Alain Koffi, Brigitte TI Sources, sinks, and transatlantic transport of North African dust aerosol: A multimodel analysis and comparison with remote sensing data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MINERAL DUST; OPTICAL DEPTH; GOCART MODEL; SAHARAN DUST; DESERT DUST; ATLANTIC; CLIMATE; AEROCOM; AERONET; MODIS AB This study evaluates model-simulated dust aerosols over North Africa and the North Atlantic from five global models that participated in the Aerosol Comparison between Observations and Models phase II model experiments. The model results are compared with satellite aerosol optical depth (AOD) data from Moderate Resolution Imaging Spectroradiometer (MODIS), Multiangle Imaging Spectroradiometer (MISR), and Sea-viewing Wide Field-of-view Sensor, dust optical depth (DOD) derived from MODIS and MISR, AOD and coarse-mode AOD (as a proxy of DOD) from ground-based Aerosol Robotic Network Sun photometer measurements, and dust vertical distributions/centroid height from Cloud Aerosol Lidar with Orthogonal Polarization and Atmospheric Infrared Sounder satellite AOD retrievals. We examine the following quantities of AOD and DOD: (1) the magnitudes over land and over ocean in our study domain, (2) the longitudinal gradient from the dust source region over North Africa to the western North Atlantic, (3) seasonal variations at different locations, and (4) the dust vertical profile shape and the AOD centroid height (altitude above or below which half of the AOD is located). The different satellite data show consistent features in most of these aspects; however, the models display large diversity in all of them, with significant differences among the models and between models and observations. By examining dust emission, removal, and mass extinction efficiency in the five models, we also find remarkable differences among the models that all contribute to the discrepancies of model-simulated dust amount and distribution. This study highlights the challenges in simulating the dust physical and optical processes, even in the best known dust environment, and stresses the need for observable quantities to constrain the model processes. C1 [Kim, Dongchul; Diehl, Thomas; Tan, Qian] Univ Space Res Assoc, Columbia, MD 21046 USA. [Kim, Dongchul; Chin, Mian; Yu, Hongbin; Diehl, Thomas; Tan, Qian; Kahn, Ralph A.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA. [Yu, Hongbin] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Tsigaridis, Kostas; Bauer, Susanne E.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Tsigaridis, Kostas; Bauer, Susanne E.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Takemura, Toshihiko] Kyushu Univ, Res Inst Appl Mech, Fukuoka 812, Japan. [Pozzoli, Luca] Istanbul Tech Univ, Eurasia Inst Earth Sci, TR-80626 Istanbul, Turkey. [Bellouin, Nicolas] Met Off Hadley Ctr, Exeter, Devon, England. [Schulz, Michael] Norwegian Meteorol Inst, Oslo, Norway. [Peyridieu, Sophie; Chedin, Alain] Meteorol Dynam Lab, Palaiseau, France. [Koffi, Brigitte] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, Air & Climate Unit, I-21020 Ispra, Italy. RP Kim, D (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA. EM dongchul.kim@nasa.gov RI Takemura, Toshihiko/C-2822-2009; Bauer, Susanne/P-3082-2014; Yu, Hongbin/C-6485-2008; Kyushu, RIAM/F-4018-2015; Schulz, Michael/A-6930-2011; U-ID, Kyushu/C-5291-2016; Kim, Dongchul/H-2256-2012; Chin, Mian/J-8354-2012; OI Takemura, Toshihiko/0000-0002-2859-6067; Yu, Hongbin/0000-0003-4706-1575; Schulz, Michael/0000-0003-4493-4158; Kim, Dongchul/0000-0002-5659-1394; Bellouin, Nicolas/0000-0003-2109-9559 FU NASA Modeling, Analysis and Prediction (MAP); EOS; NASA [NNX11AH66G]; NASA-MAP (NASA award) [NNX09AK32G]; European Commission [AA AMITO 070307/ENV/2012/636596/C3] FX This work is supported by NASA Modeling, Analysis and Prediction (MAP) and EOS Programs. H.Y. acknowledges the NASA support via NNX11AH66G. K. T. and S. E. B. were supported by NASA-MAP (NASA award: NNX09AK32G) and B. K. by the European Commission (AA AMITO 070307/ENV/2012/636596/C3). We would like to thank the MODIS, MISR, SeaWiFS, CALIOP, and AERONET teams for the data used in this study. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center. NR 68 TC 21 Z9 21 U1 2 U2 40 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2014 VL 119 IS 10 BP 6259 EP 6277 DI 10.1002/2013JD021099 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ5YQ UT WOS:000337766600034 ER PT J AU Aasi, J Abbott, BP Abbott, R Abbott, T Abernathy, MR Acernese, F Ackley, K Adams, C Adams, T Addesso, P Adhikari, RX Affeldt, C Agathos, M Aggarwal, N Aguiar, OD Ain, A Ajith, P Alemic, A Allen, B Allocca, A Amariutei, D Andersen, M Anderson, R Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, C Areeda, J Aston, SM Astone, P Aufmuth, P Aulbert, C Austin, L Aylott, BE Babak, S Baker, PT Ballardin, G Ballmer, SW Barayoga, JC Barbet, M Barish, BC Barker, D Barone, F Barr, B Barsotti, L Barsuglia, M Barton, MA Bartos, I Bassiri, R Basti, A Batch, JC Bauchrowitz, J Bauer, TS Bavigadda, V Behnke, B Bejger, M Beker, MG Belczynski, C Bell, AS Bell, C Benacquista, M Bergmann, G Bersanetti, D Bertolini, A Betzwieser, J Beyersdorf, PT Bilenko, IA Billingsley, G Birch, J Biscans, S Bitossi, M Bizouard, MA Black, E Blackburn, JK Blackburn, L Blair, D Bloemen, S Bock, O Bodiya, TP Boer, M Bogaert, G Bogan, C Bond, C Bondu, F Bonelli, L Bonnand, R Bork, R Born, M Boschi, V Bose, S Bosi, L Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brau, JE Briant, T Bridges, DO Brillet, A Brinkmann, M Brisson, V Brooks, AF Brown, DA Brown, DD Brukner, F Buchman, S Bulik, T Bulten, HJ Buonanno, A Burman, R Buskulic, D Buy, C Cadonati, L Cagnoli, G Bustillo, JC Calloni, E Camp, JB Campsie, P Cannon, KC Canuel, B Cao, J Capano, CD Carbognani, F Carbone, L Caride, S Castiglia, A Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Celerier, C Cella, G Cepeda, C Cesarini, E Chakraborty, R Chalermsongsak, T Chamberlin, SJ Chao, S Charlton, P Chassande-Mottin, E Chen, X Chen, Y Chincarini, A Chiummo, A Cho, HS Chow, J Christensen, N Chu, Q Chua, SSY Chung, S Ciani, G Clara, F Clark, JA Cleva, F Coccia, E Cohadon, PF Colla, A Collette, C Colombini, M Cominsky, L Constancio, M Conte, A Cook, D Corbitt, TR Cordier, M Cornish, N Corpuz, A Corsi, A Costa, CA Coughlin, MW Coughlin, S Coulon, JP Countryman, S Couvares, P Coward, DM Cowart, M Coyne, DC Coyne, R Craig, K Creighton, JDE Crowder, SG Cumming, A Cunningham, L Cuoco, E Dahl, K Dal Canton, T Damjanic, M Danilishin, SL D'Antonio, S Danzmann, K Dattilo, V Daveloza, H Davier, M Davies, GS Daw, EJ Day, R Dayanga, T Debreczeni, G Degallaix, J Deleglise, S Del Pozzo, W Denker, T Dent, T Dereli, H Dergachev, V De Rosa, R DeRosa, RT DeSalvo, R Dhurandhar, S Diaz, M Di Fiore, L Di Lieto, A Di Palma, I Di Virgilio, A Dolique, V Donath, A Donovan, F Dooley, KL Doravari, S Dossa, S Douglas, R Downes, TP Drago, M Drever, RWP Driggers, JC Du, Z Ducrot, M Dwyer, S Eberle, T Edo, T Edwards, M Effler, A Eggenstein, H Ehrens, P Eichholz, J Eikenberry, SS Endroczi, G Essick, R Etzel, T Evans, M Evans, T Factourovich, M Fafone, V Fairhurst, S Fang, Q Farinon, S Farr, B Farr, WM Favata, M Fehrmann, H Fejer, MM Feldbaum, D Feroz, F Ferrante, I Ferrini, F Fidecaro, F Finn, LS Fiori, I Fisher, RP Flaminio, R Fournier, JD Franco, S Frasca, S Frasconi, F Frede, M Frei, Z Freise, A Frey, R Fricke, TT Fritschel, P Frolov, VV Fulda, P Fyffe, M Gair, J Gammaitoni, L Gaonkar, S Garufi, F Gehrels, N Gemme, G Gendre, B Genin, E Gennai, A Ghosh, S Giaime, JA Giardina, KD Giazotto, A Gill, C Gleason, J Goetz, E Goetz, R Goggin, LM Gondan, L Gonzalez, G Gordon, N Gorodetsky, ML Gossan, S Gossler, S Gouaty, R Graf, C Graff, PB Granata, M Grant, A Gras, S Gray, C Greenhalgh, RJS Gretarsson, AM Groot, P Grote, H Grover, K Grunewald, S Guidi, GM Guido, C Gushwa, K Gustafson, EK Gustafson, R Hammer, D Hammond, G Hanke, M Hanks, J Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Hart, M Hartman, MT Haster, CJ Haughian, K Heidmann, A Heintze, M Heitmann, H Hello, P Hemming, G Hendry, M Heng, IS Heptonstall, AW Heurs, M Hewitson, M Hild, S Hoak, D Hodge, KA Holt, K Hooper, S Hopkins, P Hosken, DJ Hough, J Howell, EJ Hu, Y Huerta, E Hughey, B Husa, S Huttner, SH Huynh, M Huynh-Dinh, T Ingram, DR Inta, R Isogai, T Ivanov, A Iyer, BR Izumi, K Jacobson, M James, E Jang, H Jaranowski, P Ji, Y Jimenez-Forteza, F Johnson, WW Jones, DI Jones, R Jonker, RJG Ju, L Haris, K Kalmus, P Kalogera, V Kandhasamy, S Kang, G Kanner, JB Karlen, J Kasprzack, M Katsavounidis, E Katzman, W Kaufer, H Kawabe, K Kawazoe, F Kefelian, F Keiser, GM Keitel, D Kelley, DB Kells, W Khalaidovski, A Khalili, FY Khazanov, EA Kim, C Kim, K Kim, N Kim, NG Kim, YM King, EJ King, PJ Kinzel, DL Kissel, JS Klimenko, S Kline, J Koehlenbeck, S Kokeyama, K Kondrashov, V Koranda, S Korth, WZ Kowalska, I Kozak, DB Kremin, A Kringel, V Krishnan, B Krolak, A Kuehn, G Kumar, A Kumar, DN Kumar, P Kumar, R Kuo, L Kutynia, A Kwee, P Landry, M Lantz, B Larson, S Lasky, PD Lawrie, C Lazzarini, A Lazzaro, C Leaci, P Leavey, S Lebigot, EO Lee, CH Lee, HK Lee, HM Lee, J Leonardi, M Leong, JR Le Roux, A Leroy, N Letendre, N Levin, Y Levine, B Lewis, J Li, TGF Libbrecht, K Libson, A Lin, AC Littenberg, TB Litvine, V Lockerbie, NA Lockett, V Lodhia, D Loew, K Logue, J Lombardi, AL Lorenzini, M Loriette, V Lormand, M Losurdo, G Lough, J Lubinski, MJ Luck, H Luijten, E Lundgren, AP Lynch, R Ma, Y Macarthur, J Macdonald, EP MacDonald, T Machenschalk, B MacInnis, M Macleod, DM Magana-Sandoval, F Mageswaran, M Maglione, C Mailand, K Majorana, E Maksimovic, I Malvezzi, V Man, N Manca, GM Mandel, I Mandic, V Mangano, V Mangini, N Mantovani, M Marchesoni, F Marion, F Marka, S Marka, Z Markosyan, A Maros, E Marque, J Martelli, F Martin, IW Martin, RM Martinelli, L Martynov, D Marx, JN Mason, K Masserot, A Massinger, TJ Matichard, F Matone, L Matzner, RA Mavalvala, N Mazumder, N Mazzolo, G McCarthy, R McClelland, DE McGuire, SC McIntyre, G McIver, J Mclin, K Meacher, D Meadors, GD Mehmet, M Meidam, J Meinders, M Melatos, A Mendell, G Mercer, RA Meshkov, S Messenger, C Meyers, P Miao, H Michel, C Mikhailov, EE Milano, L Milde, S Miller, J Minenkov, Y Mingarelli, CMF Mishra, C Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Moe, B Moesta, P Moggi, A Mohan, M Mohapatra, SRP Moraru, D Moreno, G Morgado, N Morriss, SR Mossavi, K Mours, B Mow-Lowry, CM Mueller, CL Mueller, G Mukherjee, S Mullavey, A Munch, J Murphy, D Murray, PG Mytidis, A Nagy, MF Nardecchia, I Naticchioni, L Nayak, RK Necula, V Nelemans, G Neri, I Neri, M Newton, G Nguyen, T Nitz, A Nocera, F Nolting, D Normandin, MEN Nuttall, LK Ochsner, E O'Dell, J Oelker, E Oh, JJ Oh, SH Ohme, F Oppermann, P O'Reilly, B O'Shaughnessy, R Osthelder, C Ottaway, DJ Ottens, RS Overmier, H Owen, BJ Padilla, C Pai, A Palashov, O Palomba, C Pan, H Pan, Y Pankow, C Paoletti, F Papa, MA Paris, H Pasqualetti, A Passaquieti, R Passuello, D Pedraza, M Penn, S Perreca, A Phelps, M Pichot, M Pickenpack, M Piergiovanni, F Pierro, V Pinard, L Pinto, IM Pitkin, M Poeld, J Poggiani, R Poteomkin, A Powell, J Prasad, J Premachandra, S Prestegard, T Price, LR Prijatelj, M Privitera, S Prodi, GA Prokhorov, L Puncken, O Punturo, M Puppo, P Qin, J Quetschke, V Quintero, E Quiroga, G Quitzow-James, R Raab, FJ Rabeling, DS Racz, I Radkins, H Raffai, P Raja, S Rajalakshmi, G Rakhmanov, M Ramet, C Ramirez, K Rapagnani, P Raymond, V Razzano, M Re, V Read, J Recchia, S Reed, CM Regimbau, T Reid, S Reitze, DH Rhoades, E Ricci, F Riles, K Robertson, NA Robinet, F Rocchi, A Rodruck, M Rolland, L Rollins, JG Romano, R Romanov, G Romie, JH Rosinska, D Rowan, S Rudiger, A Ruggi, P Ryan, K Salemi, F Sammut, L Sandberg, V Sanders, JR Sannibale, V Santiago-Prieto, I Saracco, E Sassolas, B Sathyaprakash, BS Saulson, PR Savage, R Scheuer, J Schilling, R Schnabel, R Schofield, RMS Schreiber, E Schuette, D Schutz, BF Scott, J Scott, SM Sellers, D Sengupta, AS Sentenac, D Sequino, V Sergeev, A Shaddock, D Shah, S Shahriar, MS Shaltev, M Shapiro, B Shawhan, P Shoemaker, DH Sidery, TL Siellez, K Siemens, X Sigg, D Simakov, D Singer, A Singer, L Singh, R Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, M 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CA LIGO Sci Collaborat Virgo Collaborat TI Search for gravitational wave ringdowns from perturbed intermediate mass black holes in LIGO-Virgo data from 2005-2010 SO PHYSICAL REVIEW D LA English DT Article ID SPACE-TELESCOPE EVIDENCE; GLOBULAR-CLUSTER M15; STAR-CLUSTERS; BINARY; GALAXY; PERTURBATIONS; COLLAPSE; MERGERS; CORE; SEGREGATION AB We report results from a search for gravitational waves produced by perturbed intermediate mass black holes ( IMBH) in data collected by LIGO and Virgo between 2005 and 2010. The search was sensitive to astrophysical sources that produced damped sinusoid gravitational wave signals, also known as ringdowns, with frequency 50 <= f(0)/Hz <= 2000 and decay timescale 0.0001 less than or similar to tau/s less than or similar to 0.1 characteristic of those produced in mergers of IMBH pairs. No significant gravitational wave candidate was detected. We report upper limits on the astrophysical coalescence rates of IMBHs with total binary mass 50 <= M/ M circle dot <= 450 and component mass ratios of either 1: 1 or 4: 1. For systems with total mass 100 <= M/M circle dot <= 150, we report a 90% confidence upper limit on the rate of binary IMBH mergers with nonspinning and equal mass components of 6.9 x 10(-8) Mpc(-3) yr(-1). We also report a rate upper limit for ringdown waveforms from perturbed IMBHs, radiating 1% of their mass as gravitational waves in the fundamental, l = m = 2, oscillation mode, that is nearly three orders of magnitude more stringent than previous results. C1 [Aasi, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Anderson, R.; Anderson, S. B.; Arai, K.; Araya, M. C.; Austin, L.; Barayoga, J. C.; Barish, B. C.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chakraborty, R.; Chalermsongsak, T.; Coyne, D. C.; Dergachev, V.; Drever, R. W. P.; Driggers, J. C.; Ehrens, P.; Etzel, T.; Gushwa, K.; Gustafson, E. K.; Harms, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; James, E.; Kalmus, P.; Kanner, J. B.; Kells, W.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D. B.; Lazzarini, A.; Lewis, J.; Li, T. G. F.; Libbrecht, K.; Litvine, V.; Mageswaran, M.; Mailand, K.; Maros, E.; Martynov, D.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Osthelder, C.; Pedraza, M.; Phelps, M.; Price, L. R.; Privitera, S.; Quintero, E.; Raymond, V.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Singer, A.; Singer, L.; Smith, M.; Smith, R. J. E.; Smith-Lefebvre, N. D.; Taylor, R.; Thirugnanasambandam, M. P.; Thrane, E.; Torrie, C. I.; Vass, S.; Wallace, L.; Weinstein, A. J.; Whitcomb, S. E.; Williams, R.; Yamamoto, H.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Abbott, T.; Corbitt, T. R.; DeRosa, R. T.; Effler, A.; Giaime, J. A.; Gonzalez, G.; Johnson, W. W.; Kokeyama, K.; Macleod, D. M.; Mullavey, A.; Singh, R.; Walker, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Acernese, F.; Barone, F.; Calloni, E.; De Rosa, R.; Di Fiore, L.; Garufi, F.; Milano, L.; Romano, R.] Complesso Univ Monte S Angelo, Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy. [Acernese, F.; Addesso, P.; Barone, F.; Romano, R.] Univ Salerno, I-84084 Salerno, Italy. [Ackley, K.; Amariutei, D.; Barbet, M.; Ciani, G.; Eichholz, J.; Eikenberry, S. S.; Feldbaum, D.; Fulda, P.; Gleason, J.; Goetz, R.; Hartman, M. T.; Heintze, M.; Klimenko, S.; Kumar, D. Nanda; Martin, R. M.; Mitselmakher, G.; Mueller, C. L.; Mueller, G.; Mytidis, A.; Necula, V.; Ottens, R. S.; Reitze, D. H.; Tanner, D. B.; Tiwari, V.; Whiting, B. F.; Williams, L.] Univ Florida, Gainesville, FL 32611 USA. [Adams, C.; Aston, S. M.; Betzwieser, J.; Birch, J.; Bridges, D. O.; Cowart, M.; Doravari, S.; Evans, T.; Feldbaum, D.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. 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[Boer, M.; Bogaert, G.; Brillet, A.; Cleva, F.; Coulon, J. -P.; Dereli, H.; Fournier, J. -D.; Gendre, B.; Heitmann, H.; Kefelian, F.; Man, N.; Martinelli, L.; Meacher, D.; Pichot, M.; Regimbau, T.; Siellez, K.; Vinet, J. -Y.; Wei, L. -W.] Univ Nice Sophia Antipolis, Observ Cote Azur, CNRS, F-06304 Nice, France. [Bondu, F.] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France. [Bonnand, R.; Buskulic, D.; Ducrot, M.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Verkindt, D.; Yvert, M.] Univ Savoie, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France. [Bose, Sukanta; Dayanga, T.; Ghosh, S.; Steplewski, S.] Washington State Univ, Pullman, WA 99164 USA. [Bosi, L.; Colombini, M.; Gammaitoni, L.; Marchesoni, F.; Neri, I.; Punturo, M.; Travasso, F.; Vocca, H.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Branchesi, M.; Guidi, G. 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[Mikhailov, E. E.; Romanov, G.] Coll William & Mary, Williamsburg, VA 23187 USA. [Nayak, R. K.] IISER Kolkata, Mohanpur 741252, W Bengal, India. [Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Taejon 305390, South Korea. [Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [Raja, S.] RRCAT, Indore 452013, Madhya Pradesh, India. [Rajalakshmi, G.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Reid, S.] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland. [Rosinska, D.] Inst Astron, PL-65265 Zielona, Gora, Poland. [Sengupta, A. S.] Indian Inst Technol, Ahmadabad 382424, Gujarat, India. [Sturani, R.] Univ Estadual Paulista, Inst Fis Teor, South Amer Inst Fundamental Res, ICTP, BR-01140070 Sao Paulo, Brazil. [Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA. [Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA. [Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA. [Williams, T.; Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA. [Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA. RP Aasi, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. RI Iyer, Bala R./E-2894-2012; Gemme, Gianluca/C-7233-2008; Kumar, Prem/B-6691-2009; Luijten, Erik/E-3899-2010; Bell, Angus/E-7312-2011; Costa, Cesar/G-7588-2012; Huerta, Eliu/J-5426-2014; Losurdo, Giovanni/K-1241-2014; Steinlechner, Sebastian/D-5781-2013; prodi, giovanni/B-4398-2010; Hild, Stefan/A-3864-2010; Danilishin, Stefan/K-7262-2012; Gammaitoni, Luca/B-5375-2009; Howell, Eric/H-5072-2014; Canuel, Benjamin/C-7459-2014; Prokhorov, Leonid/I-2953-2012; Lee, Chang-Hwan/B-3096-2015; Khalili, Farit/D-8113-2012; Gorodetsky, Michael/C-5938-2008; McClelland, David/E-6765-2010; M, Manjunath/N-4000-2014; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Strigin, Sergey/I-8337-2012; Leonardi, Matteo/G-9694-2015; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Ottaway, David/J-5908-2015; Garufi, Fabio/K-3263-2015; Deleglise, Samuel/B-1599-2015; Neri, Igor/F-1482-2010; Aggarwal, Nancy/M-7203-2015; Shaddock, Daniel/A-7534-2011; Vicere, Andrea/J-1742-2012; Rocchi, Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Strain, Kenneth/D-5236-2011; Miao, Haixing/O-1300-2013; Gehring, Tobias/A-8596-2016; Heidmann, Antoine/G-4295-2016; Nelemans, Gijs/D-3177-2012; Marchesoni, Fabio/A-1920-2008; Zhu, Xingjiang/E-1501-2016; Frasconi, Franco/K-1068-2016; Groot, Paul/K-4391-2016; Lazzaro, Claudia/L-2986-2016; Pinto, Innocenzo/L-3520-2016; Ferrante, Isidoro/F-1017-2012; Travasso, Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Cesarini, Elisabetta/C-4507-2017; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Ward, Robert/I-8032-2014; OI Vetrano, Flavio/0000-0002-7523-4296; Addesso, Paolo/0000-0003-0895-184X; Denker, Timo/0000-0003-1259-5315; Naticchioni, Luca/0000-0003-2918-0730; calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Papa, M.Alessandra/0000-0002-1007-5298; Vocca, Helios/0000-0002-1200-3917; Aulbert, Carsten/0000-0002-1481-8319; Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Swinkels, Bas/0000-0002-3066-3601; Guidi, Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431; Collette, Christophe/0000-0002-4430-3703; Pierro, Vincenzo/0000-0002-6020-5521; Coccia, Eugenio/0000-0002-6669-5787; Iyer, Bala R./0000-0002-4141-5179; Gemme, Gianluca/0000-0002-1127-7406; Luijten, Erik/0000-0003-2364-1866; Bell, Angus/0000-0003-1523-0821; Losurdo, Giovanni/0000-0003-0452-746X; Steinlechner, Sebastian/0000-0003-4710-8548; prodi, giovanni/0000-0001-5256-915X; Danilishin, Stefan/0000-0001-7758-7493; Gammaitoni, Luca/0000-0002-4972-7062; Sorazu, Borja/0000-0002-6178-3198; Stuver, Amber/0000-0003-0324-5735; Bondu, Francois/0000-0001-6487-5197; Zweizig, John/0000-0002-1521-3397; Del Pozzo, Walter/0000-0003-3978-2030; O'Shaughnessy, Richard/0000-0001-5832-8517; Gendre, Bruce/0000-0002-9077-2025; Whelan, John/0000-0001-5710-6576; Vedovato, Gabriele/0000-0001-7226-1320; Howell, Eric/0000-0001-7891-2817; Fairhurst, Stephen/0000-0001-8480-1961; Boschi, Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418; Husa, Sascha/0000-0002-0445-1971; Lee, Chang-Hwan/0000-0003-3221-1171; Gorodetsky, Michael/0000-0002-5159-2742; McClelland, David/0000-0001-6210-5842; M, Manjunath/0000-0001-8710-0730; Vecchio, Alberto/0000-0002-6254-1617; Sigg, Daniel/0000-0003-4606-6526; Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168; Deleglise, Samuel/0000-0002-8680-5170; Neri, Igor/0000-0002-9047-9822; Shaddock, Daniel/0000-0002-6885-3494; Vicere, Andrea/0000-0003-0624-6231; Rocchi, Alessio/0000-0002-1382-9016; Martelli, Filippo/0000-0003-3761-8616; Strain, Kenneth/0000-0002-2066-5355; Miao, Haixing/0000-0003-4101-9958; Gehring, Tobias/0000-0002-4311-2593; Heidmann, Antoine/0000-0002-0784-5175; Nelemans, Gijs/0000-0002-0752-2974; Marchesoni, Fabio/0000-0001-9240-6793; Zhu, Xingjiang/0000-0001-7049-6468; Frasconi, Franco/0000-0003-4204-6587; Groot, Paul/0000-0002-4488-726X; Lazzaro, Claudia/0000-0001-5993-3372; Ferrante, Isidoro/0000-0002-0083-7228; Travasso, Flavio/0000-0002-4653-6156; Punturo, Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Dolique, Vincent/0000-0001-5644-9905; Whiting, Bernard F/0000-0002-8501-8669; Murphy, David/0000-0002-8538-815X; Pitkin, Matthew/0000-0003-4548-526X; Veitch, John/0000-0002-6508-0713; Davies, Gareth/0000-0002-4289-3439; Allen, Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Vitale, Salvatore/0000-0003-2700-0767; Kanner, Jonah/0000-0001-8115-0577; Freise, Andreas/0000-0001-6586-9901; Nitz, Alexander/0000-0002-1850-4587; Mandel, Ilya/0000-0002-6134-8946 FU United States National Science Foundation; Science and Technology Facilities Council of the United Kingdom; Max-Planck-Society; State of Niedersachsen/Germany; Italian Istituto Nazionale di Fisica Nucleare; French Centre National de la Recherche Scientifique; Australian Research Council; International Science Linkages program of the Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Educacion y Ciencia; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Foundation for Fundamental Research on Matter; Netherlands Organisation for Scientific Research; Polish Ministry of Science and Higher Education; FOCUS Programme of Foundation for Polish Science; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; Carnegie Trust; Leverhulme Trust; David and Lucille Packard Foundation; Research Corporation; Alfred P. Sloan Foundation FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Educacion y Ciencia, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme Trust, the David and Lucille Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. NR 106 TC 16 Z9 16 U1 1 U2 42 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 MAY 27 PY 2014 VL 89 IS 10 AR 102006 DI 10.1103/PhysRevD.89.102006 PG 18 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AI1YR UT WOS:000336652000002 ER PT J AU Turyshev, SG Sazhin, MV Toth, VT AF Turyshev, Slava G. Sazhin, Mikhail V. Toth, Viktor T. TI General relativistic laser interferometric observables of the GRACE-Follow-On mission SO PHYSICAL REVIEW D LA English DT Article ID EXPERIMENTAL TESTS; ASTROMETRY; TIME AB We develop a high-precision model for laser ranging interferometric (LRI) observables of the GRACE Follow-On (GRACE-FO) mission. For this, we study the propagation of an electromagnetic wave in the gravitational field in the vicinity of an extended body, in the post-Newtonian approximation of the general theory of relativity. We present a general relativistic model for the phase of a plane wave that accounts for contributions of all the multipoles of the gravitating body and its angular momentum, as well as the contribution of tidal fields produced by external sources. We develop a new approach to model a coherent signal transmission in the gravitational field of the Solar System that relies on a relativistic treatment of the phase. We use this approach to describe high-precision interferometric measurements on GRACE-FO and formulate the key LRI observables, namely, the phase and phase rate of a coherent laser link between the two spacecraft. We develop a relativistic model for the LRI-enabled range between the two GRACE-FO spacecraft, accurate to less than 1 nm, and a high-precision model for the corresponding range rate, accurate to better than 0.1 nm/s. We also formulate high-precision relativistic models for the double one-way range (DOWR) and DOWR-enabled range-rate observables originally used on GRACE and now studied for interferometric measurements on GRACE-FO. Our formulation justifies the basic assumptions behind the design of the GRACE-FO mission and highlights the importance of achieving nearly circular and nearly identical orbits for the GRACE-FO spacecraft. C1 [Turyshev, Slava G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sazhin, Mikhail V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. RP Turyshev, SG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Toth, Viktor/D-3502-2009 OI Toth, Viktor/0000-0003-3651-9843 FU National Aeronautics and Space Administration FX We thank William F. Folkner, Gerhard L. Kruizinga, Robert E. Spero, Michael M. Watkins, and Dah-Ning Yuan of JPL for their interest and many useful comments provided during the work and preparation of this manuscript. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 30 TC 3 Z9 3 U1 0 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD MAY 27 PY 2014 VL 89 IS 10 AR 105029 DI 10.1103/PhysRevD.89.105029 PG 30 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AI1YR UT WOS:000336652000015 ER PT J AU Pettorelli, N Safi, K Turner, W AF Pettorelli, Nathalie Safi, Kamran Turner, Woody TI Satellite remote sensing, biodiversity research and conservation of the future SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Editorial Material DE integrative approaches; multi-disciplinary work; data accessibility; data sharing; capacity building ID MONITORING BIODIVERSITY; ECOLOGY; SPACE; MANAGEMENT; HUMANITY; SYSTEM AB Assessing and predicting ecosystem responses to global environmental change and its impacts on human well-being are high priority targets for the scientific community. The potential for synergies between remote sensing science and ecology, especially satellite remote sensing and conservation biology, has been highlighted by many in the past. Yet, the two research communities have only recently begun to coordinate their agendas. Such synchronization is the key to improving the potential for satellite data effectively to support future environmental management decision-making processes. With this themed issue, we aim to illustrate how integrating remote sensing into ecological research promotes a better understanding of the mechanisms shaping current changes in biodiversity patterns and improves conservation efforts. Added benefits include fostering innovation, generating new research directions in both disciplines and the development of new satellite remote sensing products. C1 [Pettorelli, Nathalie] Zool Soc London, Inst Zool, London NW1 4RY, England. [Safi, Kamran] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, D-78315 Radolfzell am Bodensee, Germany. [Safi, Kamran] Univ Konstanz, Dept Biol, D-78464 Constance, Germany. [Turner, Woody] NASA, Div Earth Sci, Washington, DC 20546 USA. RP Pettorelli, N (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England. EM nathalie.pettorelli@ioz.ac.uk RI Safi, Kamran/B-2079-2008 OI Safi, Kamran/0000-0002-8418-6759 NR 47 TC 22 Z9 24 U1 8 U2 54 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 EI 1471-2970 J9 PHILOS T R SOC B JI Philos. Trans. R. Soc. B-Biol. Sci. PD MAY 26 PY 2014 VL 369 IS 1643 SI SI AR 20130190 DI 10.1098/rstb.2013.0190 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AF3EN UT WOS:000334594400001 PM 24733945 ER PT J AU Stampoulis, D Haddad, ZS Anagnostou, EN AF Stampoulis, Dimitrios Haddad, Ziad S. Anagnostou, Emmanouil N. TI Assessing the drivers of biodiversity in Madagascar by quantifying its hydrologic properties at the watershed scale SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Remote sensing; Hydrology; Biodiversity ID SEA-ICE; CONSERVATION PRIORITIES; SCATTEROMETER DATA; PASSIVE-MICROWAVE; SOIL-MOISTURE; SEAWINDS DATA; EVOLUTION; RETRIEVAL; DIVERSITY; PATTERNS AB Motivated by a theory developed by Wilme et al. (2006) according to which, watersheds of Madagascar with headwaters at high altitude respond differently to drought from those with headwaters confined to relatively low elevations, with possibly profound effects on the biodiversity patterns of the island, we analyzed multi-year basin-specific observations of soil moisture and vegetation water content (derived from NRL's WindSat radiometer) and their response to precipitation departures (derived from TRMM 3B42 V7) from its local mean. These datasets were analyzed to investigate the hydrologic properties at the basin scale, including the speed with which vegetation and soil moisture respond to precipitation anomalies. We also looked at the basin-specific normalized radar surface-backscattering cross-sections from NASA's QuikSCAT Scatterometer, to obtain information on the vegetation regimes of the various Malagasy basins. Finally, we correlated the basin response to the precipitation forcing, and compared the amplitude and time lag of the correlations across watersheds with high elevation headwaters versus those with low elevation headwaters in the aim of evaluating the drought-response hypothesis of Wilme et al. (2006). Our results indicate that the vegetation water content time series exhibit several features that are consistent with those of the majority of the bioclimatic zones of the island. Specifically, although the speed of the response of the vegetation water content varies significantly among the different basins, it is inter-annually consistent for each watershed, while the soil-moisture time series are less consistent than the vegetation water content time series. This study is a first step in the quantification of the hydrologic properties derived from microwave remote sensing, and which could potentially shed new light on the different intra-annual responses of watersheds to precipitation anomalies. Furthermore, this analysis offers important insights into the hydro-geomorphologic drivers associated with biodiversity patterns in Madagascar, contributing to a better understanding of the mechanisms that determine biotic diversification across the various bioclimatic regions of the island. (C) 2014 Elsevier Inc. All rights reserved. C1 [Stampoulis, Dimitrios; Anagnostou, Emmanouil N.] Univ Connecticut, Dept Civil & Environm Engn, Storrs, CT 06269 USA. [Stampoulis, Dimitrios; Haddad, Ziad S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Stampoulis, D (reprint author), Univ Connecticut, CEE, Storrs, CT 06269 USA. EM das09011@engr.uconn.edu FU NASA Precipitation Measurement Mission award [NNX07AE31G] FX This work was supported by a NASA Precipitation Measurement Mission award (NNX07AE31G). We also acknowledge and appreciate Dr. Joe F. Turk from the Jet Propulsion Laboratory (JPL) as well as Dr. Li Li from the Naval Research Laboratory (NRL) for providing the WindSat VWC and SM data. Z.S. Haddad's contribution was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 49 TC 2 Z9 2 U1 2 U2 29 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAY 25 PY 2014 VL 148 BP 1 EP 15 DI 10.1016/j.rse.2014.03.005 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AI3PE UT WOS:000336773600001 ER PT J AU Ermida, SL Trigo, IF DaCamara, CC Gottsche, FM Olesen, FS Hulley, G AF Ermida, Sofia L. Trigo, Isabel F. DaCamara, Carlos C. Goettsche, Frank M. Olesen, Folke S. Hulley, Glynn TI Validation of remotely sensed surface temperature over an oak woodland landscape - The problem of viewing and illumination geometries SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Land Surface Temperature; Geometric effects; LST validation; Land surface anisotropy ID BIDIRECTIONAL REFLECTANCE; PLANT CANOPIES; EMISSIVITY; ALGORITHM; PRODUCTS; MSG/SEVIRI; ANISOTROPY; PORTUGAL; SPACE; ASTER AB Satellite retrieved values of Land Surface Temperature (LST) over structured heterogeneous pixels generally depend on viewing and illumination angles as well as on the characteristics of the land cover. Here we present a method to quantify such dependencies on land surface characteristics, sun illumination and satellite position. The method uses a geometric model to describe the surface elements viewed by an air-borne sensor and relies on parallel-ray geometry to calculate the projections of tree canopies and sunlit and shaded ground: these are considered as basic surface elements responsible for most of the spatial variability of LST. For a woodland landscape we demonstrate that modeling the fractions of these basic surface elements within the sensor field-of-view allows us to quantify the directional effects observed on satellite LST with sufficient accuracy. Geometric models are an effective tool to upscale in situ measurements for the validation of LST over discontinuous canopies (e.g. forests). Here we present the application of a model to observations of brightness temperature from the LSA-SAF validation site in Evora (Portugal), an area of oak woodland, over the one-year period from October 2011 to September 2012. The resulting composite temperature is compared against LSA SAF LST products from the Spinning Enhanced Visible and InfraRed Imager (SEVIRI) onboard Meteosat as well as against MYD11A1/MOD11A1 (collection 5) products from the MODerate resolution Imaging Spectroradiometer (MODIS) onboard AQUA and TERRA. Comparisons with modeled ground LST show that SEVIRI LST has a bias of 0.26 degrees C and a RMSE of 1.34 degrees C, whereas MODIS LST (MYD11A1 and MOD11A1, collection 5) has a bias of -1.54 degrees C and a RMSE of 2.37 degrees C. Both MODIS and SEVIRI LST are closer to in situ values obtained with the geometric model than to those obtained when disregarding the effects of viewing and illumination geometry. These results demonstrate the need to consider the directional character of LST products, especially for validation purposes over heterogeneous land covers. For the new MODIS LST product (MOD21), which is based on the Temperature-Emissivity Separation (TES) algorithm, comparisons with in-situ LST show an improved bias of 0.81 degrees C and a RMSE of 1.48 degrees C (daytime values only). The TES based product presents lower emissivity values than those used for retrieving MYD11A1/MOD11A1 LST, which may partially explain the improved match with in-situ LST. Discrepancies between LST retrievals obtained from different sensors, especially those on different orbits can also be partly explained by their viewing/illumination geometries. In this study the geometric model is used to correct LST deviations between simultaneous MODIS and SEVIRI LST estimations related to those effects. When the model is used to correct the variable MODIS viewing geometry there is a reduction in standard deviation of about 0.5 degrees C. (C) 2014 Elsevier Inc. All rights reserved. C1 [Ermida, Sofia L.; DaCamara, Carlos C.] Univ Lisbon, Inst Dom Luiz, P-1749016 Lisbon, Portugal. [Trigo, Isabel F.] Inst Portugues Mar & Atmosfera, Lisbon, Portugal. [Goettsche, Frank M.; Olesen, Folke S.] Karlsruhe Inst Technol, D-76021 Karlsruhe, Germany. [Hulley, Glynn] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Ermida, SL (reprint author), Univ Lisbon, Fac Ciencias, Ed C8,Sala 8-3-15, P-1749016 Lisbon, Portugal. EM snermida@fc.ul.pt RI Trigo, Isabel/H-1630-2011; Ermida, Sofia/K-8885-2014; DaCamara, Carlos/A-2555-2013; Gottsche, Frank-Michael/A-7362-2013 OI Trigo, Isabel/0000-0001-8640-9170; Ermida, Sofia/0000-0003-0737-0824; DaCamara, Carlos/0000-0003-1699-9886; Gottsche, Frank-Michael/0000-0001-5836-5430 FU EUMETSAT (LSA SAF) FX This work was carried out within the context of the LSA SAF project (http://landsaf.ipma.pt) funded by EUMETSAT (LSA SAF: CDOP-2 proposal). NR 49 TC 19 Z9 20 U1 2 U2 24 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 MAY 25 PY 2014 VL 148 BP 16 EP 27 DI 10.1016/j.rse.2014.03.016 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AI3PE UT WOS:000336773600002 ER PT J AU Vermote, E Justice, C Csiszar, I AF Vermote, Eric Justice, Chris Csiszar, Ivan TI Early evaluation of the VIIRS calibration, cloud mask and surface reflectance Earth data records SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Remote sensing; Atmospheric correction; Surface reflectance ID RADIATIVE-TRANSFER CODE; ATMOSPHERIC CORRECTION; MODIS DATA; VECTOR VERSION; SATELLITE DATA; VALIDATION; PRODUCTS; LAND; 6S; SIMULATION AB Surface reflectance is one of the key products from VIIRS and as with MODIS, is used in developing several higher-order land products. The VIIRS Surface Reflectance(SR) Intermediate Product (IP) is based on the heritage MODIS Collection 5 product (Vermote, El Saleous, & Justice, 2002). The quality and character of surface reflectance depend on the accuracy of the VIIRS Cloud Mask (VCM), the aerosol algorithms and the adequate calibration of the sensor. The focus of this paper is the early evaluation of the VIIRS SR product in the context of the maturity of the operational processing system, the Interface Data Processing System (IDPS). After a brief introduction, the paper presents the calibration performance and the role of the surface reflectance in calibration monitoring. The analysis of the performance of the cloud mask with a focus on vegetation monitoring (no snow conditions) showstypical problems over bright surfaces and high elevation sites. Also discussed is the performance of the aerosol input used in the atmospheric correction and in particular the artifacts generated by the use of the Navy Aerosol Analysis and Prediction System. Early quantitative results of the performance of the SR product over the AERONET sites show that with the few adjustments recommended, the accuracy is within the threshold specifications. The analysis of the adequacy of the SR product (Land PEATE adjusted version) in applications of societal benefits is then presented. We conclude with a set of recommendations to ensure consistency and continuity of the JPSS mission with the MODIS Land Climate Data Record. Published by Elsevier Inc. C1 [Vermote, Eric] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA. [Justice, Chris] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Csiszar, Ivan] NOAA NESDIS, Ctr Satellite Applicat & Res, College Pk, MD USA. RP Vermote, E (reprint author), NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Mail Code 619,Bldg 32,S036H, Greenbelt, MD 20771 USA. EM Eric.F.Vermote@nasa.gov RI Csiszar, Ivan/D-2396-2010 NR 27 TC 14 Z9 14 U1 5 U2 23 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 MAY 25 PY 2014 VL 148 BP 134 EP 145 DI 10.1016/j.rse.2014.03.028 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AI3PE UT WOS:000336773600012 ER PT J AU De Lannoy, GJM Reichle, RH Vrugt, JA AF De Lannoy, Gabrielle J. M. Reichle, Rolf H. Vrugt, Jasper A. TI Uncertainty quantification of GEOS-5 L-band radiative transfer model parameters using Bayesian inference and SMOS observations SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Radiative transfer modeling; Brightness temperature; Bayesian parameter estimation; Uncertainty; Markov Chain Monte Carlo simulation; SMOS ID LAND-SURFACE PROCESSES; SOIL-MOISTURE; MICROWAVE EMISSION; BRIGHTNESS TEMPERATURES; FIELD; SENSITIVITY; CALIBRATION; ROUGHNESS; BEHAVIOR; MISSION AB Uncertainties in L-band (1.4 GHz) microwave radiative transfer modeling (RTM) affect the simulation of brightness temperatures (Tb) over land and the inversion of satellite-observed Tb into soil moisture retrievals. In particular, accurate estimates of the microwave soil roughness, vegetation optical depth and scattering albedo for large-scale applications are difficult to obtain from field studies and often lack an estimate of uncertainty. Here, a Markov Chain Monte Carlo (MCMC) simulation method is used to determine satellite-scale estimates of RTM parameters and their posterior uncertainty by minimizing the misfit between long-term averages and standard deviations of simulated and observed Tb at multiple incidence angles, at horizontal and vertical polarizations, and for morning and evening overpasses. Tb simulations are generated with the land model component of the Goddard Earth Observing System (version 5) and confronted with Tb observations from the Soil Moisture Ocean Salinity satellite mission. The maximum a posteriori density (MAP) parameter values reduce the root-mean-square differences between observed and simulated long-term Tb averages and standard deviations to 3.4 K and 23 K, respectively. The relative uncertainty of the posterior RTM parameter estimates is typically less than 25% of the MAP parameter value, whereas it exceeds 100% for literature-based prior parameter estimates. It is also shown that the parameter values estimated through Particle Swarm Optimization are in close agreement with those obtained from MCMC simulation. The MCMC results for the RTM parameter values and the uncertainties presented herein are directly relevant to the need for accurate Tb modeling in global land data assimilation systems. (C) 2014 Elsevier Inc. All rights reserved. C1 [De Lannoy, Gabrielle J. M.; Reichle, Rolf H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [De Lannoy, Gabrielle J. M.] Univ Space Res Assoc, GESTAR, Columbia, MD 21044 USA. [Vrugt, Jasper A.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92697 USA. [Vrugt, Jasper A.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Vrugt, Jasper A.] Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, NL-1098 XH Amsterdam, Netherlands. RP De Lannoy, GJM (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM Gabrielle.DeLannoy@nasa.gov RI Reichle, Rolf/E-1419-2012 FU NASA Soil Moisture Active Passive mission FX Gabrielle De Lannoy and Rolf Reichle were supported by the NASA Soil Moisture Active Passive mission. The authors thank Yann Kerr and Ali Mahmoodi for their help with the SMOS data, Valentijn Pauwels for discussions about PSO and the reviewers for their constructive comments. NR 39 TC 8 Z9 8 U1 0 U2 19 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 MAY 25 PY 2014 VL 148 BP 146 EP 157 DI 10.1016/j.rse.2014.03.030 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AI3PE UT WOS:000336773600013 ER PT J AU Kang, JH Siochi, EJ Penner, RK Turner, TL AF Kang, Jin Ho Siochi, Emilie J. Penner, Ronald K. Turner, Travis L. TI Enhanced adhesive strength between shape memory polymer nanocomposite and titanium alloy SO COMPOSITES SCIENCE AND TECHNOLOGY LA English DT Article DE Adhesive joint; Carbon nanotubes; Alloys; Interfacial strength; Shape memory polymer ID FRACTURE-TOUGHNESS; MECHANICAL-PROPERTIES; POLYURETHANE; FILMS AB Due to their unique shape memory capability, shape memory materials have been studied in numerous areas that require shape reconfiguration. This capability enables the adaptive wing structural concept. The structure prototype required enhanced interfacial strength between the shape memory polymer composite and structural metal alloys to enable the use of the shape memory polymer composite in this application. The interfacial adhesion properties between the shape memory polymer composite and a titanium alloy were systematically investigated. Surface modification of the titanium alloy with silane coupling agents improved the adhesion strength. The shape memory polymer was toughened using amphiphilic poly(n-butylene oxide)-b-poly(ethylene oxide) and with carbon nanotubes. The toughened shape memory polymer composite showed enhanced adhesion strength compared to the non-toughened system. Toughened shape memory polymer with both 5 wt% poly(n-butylene oxide)-b-poly(ethylene oxide) and 2 wt% carbon nanotube against surface-modified titanium alloy showed up to 113.5% increase in the adhesion strength, compared to the control. To investigate the adhesion mechanism, the adhesive fracture surface was investigated by tracking the locus of failure using high-resolution electron microscopy and energy dispersive X-ray spectroscopy. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Kang, Jin Ho] Natl Inst Aerosp, Hampton, VA 23666 USA. [Siochi, Emilie J.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. [Penner, Ronald K.] Sci & Technol Corp, Hampton, VA 23666 USA. [Turner, Travis L.] NASA, Langley Res Ctr, Struct Acoust Branch, Hampton, VA 23681 USA. RP Kang, JH (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA. EM jin.h.kang@nasa.gov; emilie.j.siochi@nasa.gov FU Fundamental Aeronautics Program (FAP), Fixed Wing (FW) Project of the National Aeronautics and Space Administration (NASA), USA FX This work was supported by the Fundamental Aeronautics Program (FAP), Fixed Wing (FW) Project of the National Aeronautics and Space Administration (NASA), USA. NR 29 TC 6 Z9 6 U1 4 U2 37 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 MAY 23 PY 2014 VL 96 BP 23 EP 30 DI 10.1016/j.compscitech.2014.03.003 PG 8 WC Materials Science, Composites SC Materials Science GA AH7WB UT WOS:000336345000004 ER PT J AU Jordan, JL Simons, RN Zorman, CA AF Jordan, J. L. Simons, R. N. Zorman, C. A. TI Contactless radio frequency probes for high-temperature characterisation of microwave integrated circuits SO ELECTRONICS LETTERS LA English DT Article AB The first ever demonstration of a viable contactless radio frequency (RF) probing technique at elevated temperatures is presented. The design utilises an inverted microstrip design for the probe, which is suspended over and placed in close proximity to the input/output microstrip lines of the device under test to couple signals in and out. To demonstrate the efficacy of the contactless RF probing technique, three example circuits, namely, a microstrip spurline bandstop filter, a microstrip pin diode series switch and a monolithic microwave integrated circuit amplifier mounted on a microstrip line were designed, fabricated and performance measured against temperature up to 200 degrees C. C1 [Jordan, J. L.; Simons, R. N.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Zorman, C. A.] Case Western Reserve Univ, Dept Elect Engn & Comp Sci, Cleveland, OH 44106 USA. RP Jordan, JL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM jennifer.l.jordan@nasa.gov OI Zorman, Christian/0000-0001-9773-9351 FU NASA Glenn Research Center (GRC); Center Innovation Fund (CIF) FX The NASA Glenn Research Center (GRC), Center Innovation Fund (CIF) supported this development work. NR 6 TC 0 Z9 0 U1 0 U2 1 PU INST ENGINEERING TECHNOLOGY-IET PI HERTFORD PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND SN 0013-5194 EI 1350-911X J9 ELECTRON LETT JI Electron. Lett. PD MAY 22 PY 2014 VL 50 IS 11 BP 817 EP 818 DI 10.1049/el.2014.1009 PG 2 WC Engineering, Electrical & Electronic SC Engineering GA AJ7WM UT WOS:000337911200021 ER PT J AU Lundgren, P AF Lundgren, Paul TI EARTH SCIENCE Fertile fields for seismicity SO NATURE LA English DT Editorial Material ID SAN-ANDREAS FAULT; SIERRA-NEVADA; ROCK UPLIFT; CALIFORNIA C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lundgren, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM paul.r.lundgren@jpl.nasa.gov NR 13 TC 0 Z9 0 U1 2 U2 18 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAY 22 PY 2014 VL 509 IS 7501 BP 436 EP 437 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AH4VE UT WOS:000336126000028 PM 24828039 ER PT J AU Gal-Yam, A Arcavi, I Ofek, EO Ben-Ami, S Cenko, SB Kasliwal, MM Cao, Y Yaron, O Tal, D Silverman, JM Horesh, A De Cia, A Taddia, F Sollerman, J Perley, D Vreeswijk, PM Kulkarni, SR Nugent, PE Filippenko, AV Wheeler, JC AF Gal-Yam, Avishay Arcavi, I. Ofek, E. O. Ben-Ami, S. Cenko, S. B. Kasliwal, M. M. Cao, Y. Yaron, O. Tal, D. Silverman, J. M. Horesh, A. De Cia, A. Taddia, F. Sollerman, J. Perley, D. Vreeswijk, P. M. Kulkarni, S. R. Nugent, P. E. Filippenko, A. V. Wheeler, J. C. TI A Wolf-Rayet-like progenitor of SN 2013cu from spectral observations of a stellar wind SO NATURE LA English DT Article ID SUPERNOVA PROGENITORS; IIB SUPERNOVA; MASSIVE STARS; DISCOVERY; 2011DH; TELESCOPE; EVOLUTION; GALAXY; MODEL; IB/C AB The explosive fate of massive Wolf-Rayet stars(1) (WRSs) is a key open question in stellar physics. An appealing option is that hydrogen-deficient WRSs are the progenitors of some hydrogen-poor supernova explosions of types IIb, Ib and Ic (ref. 2). A blue object, having luminosity and colours consistent with those of some WRSs, has recently been identified in pre-explosion images at the location of a supernova of type Ib (ref. 3), but has not yet been conclusively determined to have been the progenitor. Similar work has so far only resulted in non-detections(4). Comparison of early photometric observations of type Ic supernovae with theoretical models suggests that the progenitor stars had radii of less than 1012 centimetres, as expected for some WRSs(5). The signature of WRSs, their emission line spectra, cannot be probed by such studies. Here we report the detection of strong emission lines in a spectrum of type IIb supernova 2013cu (iPTF13ast) obtained approximately 15.5 hours after explosion (by 'flash spectroscopy', which captures the effects of the supernova explosion shock breakout flash on material surrounding the progenitor star). We identify Wolf-Rayet-like wind signatures, suggesting a progenitor of the WN(h) subclass (those WRSs with winds dominated by helium and nitrogen, with traces of hydrogen). The extent of this dense wind may indicate increased mass loss from the progenitor shortly before its explosion, consistent with recent theoretical predictions(6). C1 [Gal-Yam, Avishay; Arcavi, I.; Ofek, E. O.; Ben-Ami, S.; Yaron, O.; Tal, D.; De Cia, A.; Vreeswijk, P. M.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Cenko, S. B.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kasliwal, M. M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Cao, Y.; Horesh, A.; Perley, D.; Kulkarni, S. R.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Silverman, J. M.; Wheeler, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Taddia, F.; Sollerman, J.] Stockholm Univ, Oskar Klein Ctr, Dept Astron, AlbaNova, S-10691 Stockholm, Sweden. [Nugent, P. E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94701 USA. RP Gal-Yam, A (reprint author), Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. EM avishay.gal-yam@weizmann.ac.il RI Horesh, Assaf/O-9873-2016; OI Horesh, Assaf/0000-0002-5936-1156; Sollerman, Jesper/0000-0003-1546-6615 FU I-CORE programme 'The Quantum Universe' of the Planning and Budgeting Committee; Israel Science Foundation; ISF; BSF; GIF; Minerva; FP7/ERC; Kimmel Investigator award; Hubble fellowship; Israeli MOST; NSF; TABASGO Foundation; Richard and Rhoda Goldman Fund; Christopher R. Redlich Fund; Swedish Research Council; W. M. Keck Foundation; Carnegie-Princeton fellowship FX This research was supported by the I-CORE programme 'The Quantum Universe' of the Planning and Budgeting Committee and The Israel Science Foundation. A.G.-Y. acknowledges support by grants from the ISF, BSF, GIF, Minerva and FP7/ERC, and a Kimmel Investigator award. M. M. K. acknowledges support from Hubble and Carnegie-Princeton fellowships. E.O.O. acknowledges the Arye Dissentshik Career Development Chair and a grant from the Israeli MOST. J.C.W. is supported in part by the NSF. J.M.S. is supported by an NSF Postdoctoral Fellowship. A. V. F. acknowledges financial support from the TABASGO Foundation, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund and the NSF. The National Energy Research Scientific Computing Center, supported by the Office of Science of the US Department of Energy, provided staff, computational resources and data storage for this project. The Oskar Klein Centre is funded by the Swedish Research Council. We thank K. Clubb, O. Fox, P. Kelly, S. Tang and B. Sesar for their help with observations, and J. Groh, P. Crowther, M. Bersten, C. Fransson and E. Nakar for advice. Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA. The observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 40 TC 54 Z9 54 U1 0 U2 5 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAY 22 PY 2014 VL 509 IS 7501 BP 471 EP + DI 10.1038/nature13304 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AH4VE UT WOS:000336126000034 PM 24848059 ER PT J AU Martin, J Winnie, WN Caillat, T Yonenaga, I Green, ML AF Martin, Joshua Winnie Wong-Ng Caillat, Thierry Yonenaga, I. Green, Martin L. TI Thermocyclic stability of candidate Seebeck coefficient standard reference materials at high temperature SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID PRECIPITATION; ALLOYS AB The Seebeck coefficient is the most widely measured property specific to thermoelectric materials. There is currently no consensus on measurement protocols, and researchers employ a variety of techniques to measure the Seebeck coefficient. The implementation of standardized measurement protocols and the use of reliable Seebeck Coefficient Standard Reference Materials (SRMs (R)) will allow the accurate interlaboratory comparison and validation of materials data, thereby accelerating the development and commercialization of more efficient thermoelectric materials and devices. To enable members of the thermoelectric materials community the means to calibrate Seebeck coefficient measurement equipment, NIST certified SRM (R) 3451 "Low Temperature Seebeck Coefficient Standard (10K to 390 K)". Due to different practical requirements in instrumentation, sample contact methodology, and thermal stability, a complementary SRM (R) is required for the high temperature regime (300K to 900 K). The principal requirement of a SRM (R) for the Seebeck coefficient at high temperature is thermocyclic stability. We therefore characterized the thermocyclic behavior of the Seebeck coefficient for a series of candidate materials: constantan, p-type single crystal SiGe, and p-type polycrystalline SiGe, by measuring the temperature dependence of the Seebeck coefficient as a function of 10 sequential thermal cycles, between 300K and 900 K. We employed multiple regression analysis to interpolate and analyze the thermocyclic variability in the measurement curves. (C) 2014 AIP Publishing LLC. C1 [Martin, Joshua; Winnie Wong-Ng; Green, Martin L.] NIST, Mat Measurement Lab, Gaithersburg, MD 20899 USA. [Caillat, Thierry] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Yonenaga, I.] Tohoku Univ, Inst Mat Res, Sendai, Miyagi 9808577, Japan. RP Martin, J (reprint author), NIST, Mat Measurement Lab, Gaithersburg, MD 20899 USA. EM joshua.martin@nist.gov RI Yonenaga, Ichiro/A-4852-2011 NR 19 TC 3 Z9 3 U1 2 U2 22 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD MAY 21 PY 2014 VL 115 IS 19 AR 193501 DI 10.1063/1.4876909 PG 6 WC Physics, Applied SC Physics GA AI5PA UT WOS:000336920200013 ER PT J AU Solnik, S Pazin, N Coelho, CJ Rosenbaum, DA Zatsiorsky, VM Latash, ML AF Solnik, Stanislaw Pazin, Nemanja Coelho, Chase J. Rosenbaum, David A. Zatsiorsky, Vladimir M. Latash, Mark L. TI Postural sway and perceived comfort in pointing tasks SO NEUROSCIENCE LETTERS LA English DT Article DE End-state comfort; Pointing; Postural sway; Rambling; Trembling ID COMPONENTS AB In this study, we explored relations between indices of postural sway and perceived comfort during pointing postures performed by standing participants. The participants stood on a force plate, grasped a pointer with the dominant (right) hand, and pointed to targets located at four positions and at two distances from the body. We quantified postural sway over 60-s intervals at each pointing posture, and found no effects of target location or distance on postural sway indices. In contrast, comfort ratings correlated significantly with indices of one of the sway components, trembling. Our observations support the hypothesis that rambling and trembling sway components involve different neurophysiological mechanisms. They also suggest that subjective perception of comfort may be more important than the actual posture for postural sway. (C) 2014 Elsevier Ireland Ltd. All rights reserved. C1 [Solnik, Stanislaw; Pazin, Nemanja; Zatsiorsky, Vladimir M.; Latash, Mark L.] Penn State Univ, Dept Kinesiol, University Pk, PA 16802 USA. [Coelho, Chase J.; Rosenbaum, David A.] Penn State Univ, Dept Psychol, University Pk, PA 16802 USA. [Solnik, Stanislaw] Univ Sch Phys Educ Wroclaw, Wroclaw, Poland. [Pazin, Nemanja] Univ Belgrade, Fac Sport & Phys Educ, Belgrade, Serbia. [Coelho, Chase J.] Johnson Space Ctr, Lockheed Martin, ISS Flight Crew Integrat, Operat Habitabil Grp, Houston, TX USA. RP Solnik, S (reprint author), Penn State Univ, Dept Kinesiol, Motor Control Lab, 20 Rec Hall Bldg, University Pk, PA 16802 USA. EM szs13@psu.edu FU NIH [NS-035032, AR-048563] FX The study was in part supported by NIH grants NS-035032 and AR-048563. NR 17 TC 1 Z9 1 U1 2 U2 10 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0304-3940 EI 1872-7972 J9 NEUROSCI LETT JI Neurosci. Lett. PD MAY 21 PY 2014 VL 569 BP 18 EP 22 DI 10.1016/j.neulet.2014.03.034 PG 5 WC Neurosciences SC Neurosciences & Neurology GA AH8AI UT WOS:000336356100004 PM 24686189 ER PT J AU Ackermann, M Ajello, M Albert, A Allafort, A Atwood, WB Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Bloom, ED Bonamente, E Bottacini, E Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cavazzuti, E Chaves, RCG Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J D'Ammando, F de Angelis, A de Palma, F Dermer, CD Digel, SW Drell, PS Drlica-Wagner, A Favuzzi, C Franckowiak, A Funk, S Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giordano, F Giroletti, M Godfrey, G Gomez-Vargas, GA Grenier, IA Guiriec, S Gustafsson, M Hadasch, D Hayashida, M Hewitt, J Hughes, RE Jeltema, TE Johannesson, G Johnson, AS Kamae, T Kataoka, J Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Garde, ML Longo, F Loparco, F Lovellette, MN Lubrano, P Mayer, M Mazziotta, MN McEnery, JE Michelson, PF Mitthumsiri, W Mizuno, T Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nemmen, R Nuss, E Ohsugi, T Orienti, M Orlando, E Ormes, JF Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Raino, S Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Ruan, J Sanchez-Conde, M Schulz, A Sgro, C Siskind, EJ Spandre, G Spinelli, P Storm, E Strong, AW Suson, DJ Takahashi, H Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Torres, DF Troja, E Uchiyama, Y Usher, TL Vandenbroucke, J Vianello, G Vitale, V Winer, BL Wood, KS Zimmer, S Pinzke, A Pfrommer, C AF Ackermann, M. Ajello, M. Albert, A. Allafort, A. Atwood, W. B. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Bloom, E. D. Bonamente, E. Bottacini, E. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cavazzuti, E. Chaves, R. C. G. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. D'Ammando, F. de Angelis, A. de Palma, F. Dermer, C. D. Digel, S. W. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Franckowiak, A. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Godfrey, G. Gomez-Vargas, G. A. Grenier, I. A. Guiriec, S. Gustafsson, M. Hadasch, D. Hayashida, M. Hewitt, J. Hughes, R. E. Jeltema, T. E. Johannesson, G. Johnson, A. S. Kamae, T. Kataoka, J. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Garde, M. Llena Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Mayer, M. Mazziotta, M. N. McEnery, J. E. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nemmen, R. Nuss, E. Ohsugi, T. Orienti, M. Orlando, E. Ormes, J. F. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Raino, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Ruan, J. Sanchez-Conde, M. Schulz, A. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Storm, E. Strong, A. W. Suson, D. J. Takahashi, H. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Torres, D. F. Troja, E. Uchiyama, Y. Usher, T. L. Vandenbroucke, J. Vianello, G. Vitale, V. Winer, B. L. Wood, K. S. Zimmer, S. Pinzke, A. Pfrommer, C. CA Fermi-LAT Collaboration TI SEARCH FOR COSMIC-RAY-INDUCED GAMMA-RAY EMISSION IN GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: intracluster medium; gamma rays: galaxies: clusters ID LARGE-AREA TELESCOPE; COSMOLOGICAL SHOCK-WAVES; DIFFUSE RADIO-EMISSION; X-RAY; MAGNETIC-FIELDS; COMA CLUSTER; MAGIC TELESCOPES; HADRONIC MODELS; NGC 1275; PARTICLE REACCELERATION AB Current theories predict relativistic hadronic particle populations in clusters of galaxies in addition to the already observed relativistic leptons. In these scenarios hadronic interactions give rise to neutral pions which decay into gamma rays that are potentially observable with the Large Area Telescope (LAT) on board the Fermi space telescope. We present a joint likelihood analysis searching for spatially extended gamma-ray emission at the locations of 50 galaxy clusters in four years of Fermi-LAT data under the assumption of the universal cosmic-ray (CR) model proposed by Pinzke & Pfrommer. We find an excess at a significance of 2.7 sigma, which upon closer inspection, however, is correlated to individual excess emission toward three galaxy clusters: A400, A1367, and A3112. We discuss these cases in detail and conservatively attribute the emission to unmodeled background systems (for example, radio galaxies within the clusters). Through the combined analysis of 50 clusters, we exclude hadronic injection efficiencies in simple hadronic models above 21% and establish limits on the CR to thermal pressure ratio within the virial radius, R-200, to be below 1.25%-1.4% depending on the morphological classification. In addition, we derive new limits on the gamma-ray flux from individual clusters in our sample. C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Albert, A.; Hughes, R. E.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA. [Allafort, A.; Bechtol, K.; Bloom, E. D.; Bottacini, E.; Cameron, R. A.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Drlica-Wagner, A.; Franckowiak, A.; Funk, S.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Orlando, E.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA. [Allafort, A.; Bechtol, K.; Bloom, E. D.; Bottacini, E.; Cameron, R. A.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Drlica-Wagner, A.; Franckowiak, A.; Funk, S.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Orlando, E.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Atwood, W. B.; Jeltema, T. E.; Razzano, M.; Storm, E.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Jeltema, T. E.; Razzano, M.; Storm, E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Chaves, R. C. G.; Grenier, I. A.] CEA IRFU CNRS Univ Paris Diderot, CEA Saclay, Lab AIM, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Germani, S.; Lubrano, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Germani, S.; Lubrano, P.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brandt, T. J.; Guiriec, S.; Hewitt, J.; McEnery, J. E.; Nemmen, R.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cavazzuti, E.; Ciprini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [Ciprini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00044 Rome, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34095 Montpellier, France. [Conrad, J.; Larsson, S.; Garde, M. Llena; Zimmer, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.; Larsson, S.; Garde, M. Llena; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden. [D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dermer, C. D.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Gomez-Vargas, G. A.; Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Gomez-Vargas, G. A.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. [Gomez-Vargas, G. A.] Univ Autonoma Madrid, CSIC, Inst Fis Teor IFT UAM, E-28049 Madrid, Spain. [Gustafsson, M.] Univ Libre Bruxelles, Serv Phys Theor, B-1050 Brussels, Belgium. [Hayashida, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, UPS OMP, IRAP, GAHEC, F-91191 Toulouse, France. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [McEnery, J. E.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Razzaque, S.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Ruan, J.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Torres, D. F.] Inst Catalana Recerca & Estudis Avancats, E-08034 Barcelona, Spain. [Vianello, G.] Consorzio Interuniv Fis Spaziale, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Pinzke, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Pfrommer, C.] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. RP Ackermann, M (reprint author), DESY, D-15738 Zeuthen, Germany. EM conrad@fysik.su.se; olr@slac.stanford.edu; zimmer@fysik.su.se; apinzke@fysik.su.se; christoph.pfrommer@h-its.org RI Reimer, Olaf/A-3117-2013; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Gomez-Vargas, German/C-7138-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Orlando, E/R-5594-2016; OI Giordano, Francesco/0000-0002-8651-2394; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Zimmer, Stephan/0000-0002-5735-0082; Bastieri, Denis/0000-0002-6954-8862; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Reimer, Olaf/0000-0001-6953-1385; Torres, Diego/0000-0002-1522-9065; Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726 FU K. A. Wallenberg Foundation FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation. NR 126 TC 43 Z9 43 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 18 DI 10.1088/0004-637X/787/1/18 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200018 ER PT J AU Ackermann, M Ajello, M Albert, A Allafort, A Baldini, L Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Bissaldi, E Bonamente, E Bottacini, E Bouvier, A Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cecchi, C Charles, E Chekhtman, A Chen, Q Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S D'Ammando, F de Angelis, A de Palma, F Dermer, CD Desiante, R Digel, SW Di Venere, L Silva, EDE Drell, PS Drlica-Wagner, A Favuzzi, C Fegan, SJ Focke, WB Franckowiak, A Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Hadasch, D Hayashida, M Hays, E Horan, D Hughes, RE Inoue, Y Jackson, MS Jogler, T Johannesson, G Johnson, WN Kamae, T Kawano, T Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Lemoine-Goumard, M Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Mayer, M Mazziotta, MN McEnery, JE Michelson, PF Mizuno, T Moiseev, AA Monte, C Monzani, ME Moretti, E Morselli, A Moskalenko, IV Murgia, S Murphy, R Nemmen, R Nuss, E Ohno, M Ohsugi, T Okumura, A Omodei, N Orienti, M Orlando, E Ormes, JF Paneque, D Panetta, JH Perkins, JS Pesce-Rollins, M Petrosian, V Piron, F Pivato, G Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Ritz, S Schulz, A Sgro, C Siskind, EJ Spandre, G Spinelli, P Takahashi, H Takeuchi, Y Tanaka, Y Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Tosti, G Troja, E Tronconi, V Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Werner, M Winer, BL Wood, DL Wood, KS Wood, M Yang, Z AF Ackermann, M. Ajello, M. Albert, A. Allafort, A. Baldini, L. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Bissaldi, E. Bonamente, E. Bottacini, E. Bouvier, A. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cecchi, C. Charles, E. Chekhtman, A. Chen, Q. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. D'Ammando, F. de Angelis, A. de Palma, F. Dermer, C. D. Desiante, R. Digel, S. W. Di Venere, L. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Fegan, S. J. Focke, W. B. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Hadasch, D. Hayashida, M. Hays, E. Horan, D. Hughes, R. E. Inoue, Y. Jackson, M. S. Jogler, T. Johannesson, G. Johnson, W. N. Kamae, T. Kawano, T. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lemoine-Goumard, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Mayer, M. Mazziotta, M. N. McEnery, J. E. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Moretti, E. Morselli, A. Moskalenko, I. V. Murgia, S. Murphy, R. Nemmen, R. Nuss, E. Ohno, M. Ohsugi, T. Okumura, A. Omodei, N. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Perkins, J. S. Pesce-Rollins, M. Petrosian, V. Piron, F. Pivato, G. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Ritz, S. Schulz, A. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Takahashi, H. Takeuchi, Y. Tanaka, Y. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Tosti, G. Troja, E. Tronconi, V. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Werner, M. Winer, B. L. Wood, D. L. Wood, K. S. Wood, M. Yang, Z. TI HIGH-ENERGY GAMMA-RAY EMISSION FROM SOLAR FLARES: SUMMARY OF FERMI LARGE AREA TELESCOPE DETECTIONS AND ANALYSIS OF TWO M-CLASS FLARES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: flares; Sun: X-rays, gamma rays ID STOCHASTIC ACCELERATION; PARTICLE-ACCELERATION; EGRET; CALIBRATION; ELECTRONS; COMPTON; SHOCKS; WAVES; GRO AB We present the detections of 18 solar flares detected in high-energy gamma-rays (above 100 MeV) with the Fermi Large Area Telescope (LAT) during its first 4 yr of operation. This work suggests that particle acceleration up to very high energies in solar flares is more common than previously thought, occurring even in modest flares, and for longer durations. Interestingly, all these flares are associated with fairly fast coronal mass ejections (CMEs). We then describe the detailed temporal, spatial, and spectral characteristics of the first two long-lasting events: the 2011 March 7 flare, a moderate (M3.7) impulsive flare followed by slowly varying gamma-ray emission over 13 hr, and the 2011 June 7 M2.5 flare, which was followed by gamma-ray emission lasting for 2 hr. We compare the Fermi LAT data with X-ray and proton data measurements from GOES and RHESSI. We argue that the gamma-rays are more likely produced through pion decay than electron bremsstrahlung, and we find that the energy spectrum of the proton distribution softens during the extended emission of the 2011 March 7 flare. This would disfavor a trapping scenario for particles accelerated during the impulsive phase of the flare and point to a continuous acceleration process at play for the duration of the flares. CME shocks are known for accelerating the solar energetic particles (SEPs) observed in situ on similar timescales, but it might be challenging to explain the production of gamma-rays at the surface of the Sun while the CME is halfway to the Earth. A stochastic turbulence acceleration process occurring in the solar corona is another likely scenario. Detailed comparison of characteristics of SEPs and gamma-ray-emitting particles for several flares will be helpful to distinguish between these two possibilities. C1 [Ackermann, M.; Mayer, M.; Schulz, A.] DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Albert, A.; Hughes, R. E.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA. [Allafort, A.; Bechtol, K.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chen, Q.; Chiang, J.; Claus, R.; Digel, S. W.; Di Venere, L.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Inoue, Y.; Jogler, T.; Kamae, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Allafort, A.; Bechtol, K.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chen, Q.; Chiang, J.; Claus, R.; Desiante, R.; Digel, S. W.; Di Venere, L.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Inoue, Y.; Jogler, T.; Kamae, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.] Ist Nazl Fis Nucl, I-56127 Pisa, Italy. [Barbiellini, G.; Desiante, R.; Longo, F.] Ist Nazl Fis Nucl, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.; Tronconi, V.] Univ Padua, Dipartimento Fis Astron G Galilei, I-35131 Padua, Italy. [Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bissaldi, E.; Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Bissaldi, E.; Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Bouvier, A.; Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Brandt, T. J.; Guiriec, S.; Hays, E.; McEnery, J. E.; Moiseev, A. A.; Nemmen, R.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, Lab Leprince Ringuet, CNRS, IN2P3, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.] CSIC, Inst Ciencies Espai, IEEE, E-08193 Barcelona, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Ist Nazl Astrofis, Osservatorio Astron Roma, I-00040 Rome, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univ & Particules Montpellier, CNRS, IN2P3, F-34095 Montpellier, France. [Conrad, J.; Larsson, S.; Yang, Z.] Univ Stockholm, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Jackson, M. S.; Larsson, S.; Moretti, E.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden. [D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Murphy, R.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Fukazawa, Y.; Kawano, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Grenier, I. A.] Univ Paris Diderot, CEA Saclay, Lab AIM, Serv Astrophys,CEA IRFU CNRS, F-91191 Gif Sur Yvette, France. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Jackson, M. S.; Moretti, E.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, GAHEC, F-31100 Toulouse, France. [Larsson, S.] Univ Stockholm, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Lemoine-Goumard, M.; Lott, B.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Moiseev, A. A.; Perkins, J. S.] Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Ohno, M.; Tanaka, Y.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Okumura, A.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Takeuchi, Y.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Vianello, G.] Consorzio Interuniv Fis Spaziale, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartmento Fis, I-00133 Rome, Italy. [Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA. RP Ackermann, M (reprint author), DESY, D-15738 Zeuthen, Germany. EM vahep@stanford.edu; allafort@stanford.edu; nico.giglietto@ba.infn.it; nicola.omodei@stanford.edu; tanaka@astro.isas.jaxa.jp RI Di Venere, Leonardo/C-7619-2017; Bissaldi, Elisabetta/K-7911-2016; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Orlando, E/R-5594-2016; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016 OI Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Di Venere, Leonardo/0000-0003-0703-824X; Giordano, Francesco/0000-0002-8651-2394; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Inoue, Yoshiyuki/0000-0002-7272-1136; Bastieri, Denis/0000-0002-6954-8862; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Bissaldi, Elisabetta/0000-0001-9935-8106; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; FU National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden FX The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT, as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States; the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy; the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK), and Japan Aerospace Exploration Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden. NR 31 TC 16 Z9 16 U1 1 U2 22 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 15 DI 10.1088/0004-637X/787/1/15 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200015 ER PT J AU Beck, SC Lacy, J Turner, J Greathouse, T Neff, S AF Beck, Sara C. Lacy, John Turner, Jean Greathouse, Thomas Neff, Susan TI IONIZED GAS KINEMATICS AT HIGH RESOLUTION. IV. STAR FORMATION AND A ROTATING CORE IN THE MEDUSA (NGC 4194) SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 4194); galaxies: kinematics and dynamics; galaxies: starburst; galaxies: star formation ID H II REGIONS; GALAXIES; EMISSION; NGC-4194; MERGERS; SAMPLE; M82 AB NGC 4194 is a post-merger starburst known as The Medusa for its striking tidal features. We present here a detailed study of the structure and kinematics of ionized gas in the central 0.65 kpc of the Medusa. The data include radio continuum maps with resolution up to 0."18 (35 pc) and a 12.8 mu m [Ne II] data cube with spectral resolution similar to 4 km s(-1): the first high-resolution, extinction-free observations of this remarkable object. The ionized gas has the kinematic signature of a core in solid-body rotation. The starburst has formed a complex of bright compact H II regions, probably excited by deeply embedded super star clusters, but none of these sources is a convincing candidate for a Galactic nucleus. The nuclei of the merger partners that created the Medusa have not yet been identified. C1 [Beck, Sara C.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Ramat Aviv, Israel. [Lacy, John] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Turner, Jean] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Greathouse, Thomas] SW Res Inst, San Antonio, TX 78228 USA. [Neff, Susan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Beck, SC (reprint author), Tel Aviv Univ, Sch Phys & Astron, IL-69978 Ramat Aviv, Israel. EM becksarac@gmail.com OI Beck, Sara/0000-0002-5770-8494 FU NSF [AST-0607312, AST-0708074] FX TEXES observations at the IRTF were supported by NSF AST-0607312 and by AST-0708074 to Matt Richter. This research has made use of the NASA and IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, Caltech, under contract with NASA. We thank an anonymous referee for careful and thoughtful comments. NR 27 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 85 DI 10.1088/0004-637X/787/1/85 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200085 ER PT J AU Boyajian, TS von Braun, K van Belle, G Farrington, C Schaefer, G Jones, J White, R McAlister, HA ten Brummelaar, TA Ridgway, S Gies, D Sturmann, L Sturmann, J Turner, NH Goldfinger, PJ Vargas, N AF Boyajian, Tabetha S. von Braun, Kaspar van Belle, Gerard Farrington, Chris Schaefer, Gail Jones, Jeremy White, Russel McAlister, Harold A. ten Brummelaar, Theo A. Ridgway, Stephen Gies, Douglas Sturmann, Laszlo Sturmann, Judit Turner, Nils H. Goldfinger, P. J. Vargas, Norm TI STELLAR DIAMETERS AND TEMPERATURES. III. MAIN SEQUENCE A, F, G, AND K STARS: ADDITIONAL HIGH-PRECISION MEASUREMENTS AND EMPIRICAL RELATIONS (vol 771, pg 40, 2013) SO ASTROPHYSICAL JOURNAL LA English DT Correction ID INFRARED FLUX METHOD; ANGULAR DIAMETERS; MAGNITUDES; PHOTOMETRY; SUBDWARFS; CALIBRATION C1 [Boyajian, Tabetha S.; Jones, Jeremy; White, Russel; McAlister, Harold A.; Gies, Douglas] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA. [Boyajian, Tabetha S.; Jones, Jeremy; White, Russel; McAlister, Harold A.; Gies, Douglas] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Boyajian, Tabetha S.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [von Braun, Kaspar] CALTECH, Exoplanet Sci Inst, NASA, Pasadena, CA 91125 USA. [von Braun, Kaspar] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [van Belle, Gerard] Lowell Observ, Flagstaff, AZ 86001 USA. [Farrington, Chris; Schaefer, Gail; ten Brummelaar, Theo A.; Sturmann, Laszlo; Sturmann, Judit; Turner, Nils H.; Goldfinger, P. J.; Vargas, Norm] Mt Wilson Observ, CHARA Array, Mt Wilson, CA 91023 USA. [Ridgway, Stephen] Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Boyajian, TS (reprint author), Georgia State Univ, Ctr High Angular Resolut Astron, POB 4106, Atlanta, GA 30302 USA. OI Boyajian, Tabetha/0000-0001-9879-9313 NR 22 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 92 DI 10.1088/0004-637X/787/1/92 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200092 ER PT J AU LaMassa, SM Yaqoob, T Ptak, AF Jia, JJ Heckman, TM Gandhi, P Urry, CM AF LaMassa, Stephanie M. Yaqoob, Tahir Ptak, Andrew F. Jia, Jianjun Heckman, Timothy M. Gandhi, Poshak Urry, C. Meg TI DELVING INTO X-RAY OBSCURATION OF TYPE 2 AGN, NEAR AND FAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: Seyfert; X-rays: general ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; PHOTOIONIZATION CROSS-SECTIONS; SEYFERT 2 GALAXIES; BLACK-HOLE MASS; EMISSION-LINE; XMM-NEWTON; INFRARED GALAXIES; UNIFIED SCHEMES; OBSCURING TORUS AB Using self-consistent, physically motivated models, we investigate the X-ray obscuration in 19 Type 2 [O III] 5007 angstrom selected active galactic nuclei (AGNs), 9 of which are local Seyfert 2 galaxies and 10 of which are Type 2 quasar candidates. We derive reliable line-of-sight and global column densities for these objects, which is the first time this has been reported for an AGN sample; four AGNs have significantly different global and line-of-sight column densities. Five sources are heavily obscured to Compton-thick. We comment on interesting sources revealed by our spectral modeling, including a candidate "naked" Sy2. After correcting for absorption, we find that the ratio of the rest-frame, 2-10 keV luminosity (L-2-10 keV,L-in) to L-[O III] is 1.54 +/- 0.49 dex which is essentially identical to the mean Type 1 AGN value. The Fe K alpha luminosity is significantly correlated with L-[O III] but with substantial scatter. Finally, we do not find a trend between L-2-10 keV,L-in and global or line-of-sight column density, between column density and redshift, between column density and scattering fraction, or between scattering fraction and redshift. C1 [LaMassa, Stephanie M.; Urry, C. Meg] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Yaqoob, Tahir; Ptak, Andrew F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jia, Jianjun; Heckman, Timothy M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Gandhi, Poshak] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP LaMassa, SM (reprint author), Yale Univ, Yale Ctr Astron & Astrophys, POB 208120, New Haven, CT 06520 USA. FU STFC [ST/J003697/1]; Alfred P. Sloan Foundation; National Science Foundation; U. S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab, the Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX We thank the referee for a careful reading of this manuscript and for helpful suggestions. P. G. acknowledges support from STFC (grant reference ST/J003697/1).; This work has made use of data from the SDSS. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U. S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 58 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 61 DI 10.1088/0004-637X/787/1/61 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200061 ER PT J AU Leake, JE Linton, MG Antiochos, SK AF Leake, James E. Linton, Mark G. Antiochos, Spiro K. TI SIMULATIONS OF EMERGING MAGNETIC FLUX. II. THE FORMATION OF UNSTABLE CORONAL FLUX ROPES AND THE INITIATION OF CORONAL MASS EJECTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); Sun: atmosphere; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: magnetic fields ID SOLAR ATMOSPHERE; EMERGENCE; MODEL; ERUPTION; EVOLUTION; BREAKOUT; FLARES; RECONNECTION; MORPHOLOGY; TOPOLOGY AB We present results from three-dimensional magnetohydrodynamic simulations of the emergence of a twisted convection zone flux tube into a pre-existing coronal dipole field. As in previous simulations, following the partial emergence of the sub-surface flux into the corona, a combination of vortical motions and internal magnetic reconnection forms a coronal flux rope. Then, in the simulations presented here, external reconnection between the emerging field and the pre-existing dipole coronal field allows further expansion of the coronal flux rope into the corona. After sufficient expansion, internal reconnection occurs beneath the coronal flux rope axis, and the flux rope erupts up to the top boundary of the simulation domain (similar to 36 Mm above the surface). We find that the presence of a pre-existing field, orientated in a direction to facilitate reconnection with the emerging field, is vital to the fast rise of the coronal flux rope. The simulations shown in this paper are able to self-consistently create many of the surface and coronal signatures used by coronal mass ejection (CME) models. These signatures include surface shearing and rotational motions, quadrupolar geometry above the surface, central sheared arcades reconnecting with oppositely orientated overlying dipole fields, the formation of coronal flux ropes underlying potential coronal field, and internal reconnection which resembles the classical flare reconnection scenario. This suggests that proposed mechanisms for the initiation of a CME, such as "magnetic breakout", are operating during the emergence of new active regions. C1 [Leake, James E.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Linton, Mark G.] US Naval Res Lab, Washington, DC 20375 USA. [Antiochos, Spiro K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20711 USA. RP Leake, JE (reprint author), George Mason Univ, Coll Sci, 4400 Univ Dr, Fairfax, VA 22030 USA. EM jleake@gmu.edu RI Antiochos, Spiro/D-4668-2012 OI Antiochos, Spiro/0000-0003-0176-4312 FU NASA Living With a Star and Solar and Heliospheric Physics programs; Office of Naval Research 6.1 Program; DoD HPC program FX This work has been supported by the NASA Living With a Star and Solar and Heliospheric Physics programs, and the Office of Naval Research 6.1 Program. The simulations were performed under a grant of computer time from the DoD HPC program. NR 38 TC 11 Z9 11 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 46 DI 10.1088/0004-637X/787/1/46 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200046 ER PT J AU Marinucci, A Matt, G Miniutti, G Guainazzi, M Parker, ML Brenneman, L Fabian, AC Kara, E Arevalo, P Ballantyne, DR Boggs, SE Cappi, M Christensen, FE Craig, WW Elvis, M Hailey, CJ Harrison, FA Reynolds, CS Risaliti, G Stern, DK Walton, DJ Zhang, W AF Marinucci, A. Matt, G. Miniutti, G. Guainazzi, M. Parker, M. L. Brenneman, L. Fabian, A. C. Kara, E. Arevalo, P. Ballantyne, D. R. Boggs, S. E. Cappi, M. Christensen, F. E. Craig, W. W. Elvis, M. Hailey, C. J. Harrison, F. A. Reynolds, C. S. Risaliti, G. Stern, D. K. Walton, D. J. Zhang, W. TI THE BROADBAND SPECTRAL VARIABILITY OF MCG-6-30-15 OBSERVED BY NUSTAR AND XMM-NEWTON SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: Seyfert; X-rays: individual (MCG-6-30-015) ID ACTIVE GALACTIC NUCLEI; 1 GALAXY MCG-6-30-15; X-RAY VARIABILITY; K-ALPHA LINE; PHOTON IMAGING CAMERA; DUSTY WARM ABSORBER; BLACK-HOLE; IRON LINE; SUZAKU OBSERVATIONS; SEYFERT-1 GALAXIES AB MCG-6-30-15, at a distance of 37 Mpc (z = 0.008), is the archetypical Seyfert 1 galaxy showing very broad Fe K alpha emission. We present results from a joint NuSTAR and XMM-Newton observational campaign that, for the first time, allows a sensitive, time-resolved spectral analysis from 0.35 keV up to 80 keV. The strong variability of the source is best explained in terms of intrinsic X-ray flux variations and in the context of the light-bending model: the primary, variable emission is reprocessed by the accretion disk, which produces secondary, less variable, reflected emission. The broad Fe K alpha profile is, as usual for this source, well explained by relativistic effects occurring in the innermost regions of the accretion disk around a rapidly rotating black hole. We also discuss the alternative model in which the broadening of the Fe K alpha is due to the complex nature of the circumnuclear absorbing structure. Even if this model cannot be ruled out, it is disfavored on statistical grounds. We also detected an occultation event likely caused by broad-line region clouds crossing the line of sight. C1 [Marinucci, A.; Matt, G.] Univ Rome, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Marinucci, A.; Miniutti, G.] ESAC, Dep Astrofis, Ctr Astrobiol CSIC INTA, Madrid, Spain. [Guainazzi, M.] European Space Astron Ctr ESA, E-28080 Madrid, Spain. [Parker, M. L.; Fabian, A. C.; Kara, E.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Brenneman, L.; Elvis, M.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Arevalo, P.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 22, Chile. [Arevalo, P.] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Cappi, M.] IASF Bologna, INAF, I-40129 Bologna, Italy. [Christensen, F. E.] Danish Tech Univ, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Craig, W. W.; Hailey, C. J.; Walton, D. J.] Columbia Univ, New York, NY 10027 USA. [Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Stern, D. K.] 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, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy. RI Miniutti, Giovanni/L-2721-2014; Boggs, Steven/E-4170-2015; Cappi, Massimo/F-4813-2015; OI Miniutti, Giovanni/0000-0003-0707-4531; Boggs, Steven/0000-0001-9567-4224; Cappi, Massimo/0000-0001-6966-8920; Risaliti, Guido/0000-0002-3556-977X FU Fondazione Angelo Della Riccia.; Italian Space Agency [ASI/INAF I/037/12/0-011/13]; European Union Seventh Framework Programme (FP7) [312789]; Anillo [ACT1101]; NASA [NNG08FD60C]; California Institute of Technology; National Aeronautics and Space Administration.; NuSTAR Operations, Software, and Calibration; NuSTAR Data Analysis Software (NuSTARDAS); ASI Science Data Center (ASDC, Italy); California Institute of Technology (USA) FX A. M. acknowledges financial support from Fondazione Angelo Della Riccia. A. M. and G. M. acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. A. M., G. Matt, G. Miniutti, A. C. F., and E. K. acknowledge financial support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789. P. A. acknowledges financial support from Anillo ACT1101. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). NR 76 TC 26 Z9 26 U1 3 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 83 DI 10.1088/0004-637X/787/1/83 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200083 ER PT J AU Moore, CS Chamberlin, PC Hock, R AF Moore, Christopher Samuel Chamberlin, Phillip Clyde Hock, Rachel TI MEASUREMENTS AND MODELING OF TOTAL SOLAR IRRADIANCE IN X-CLASS SOLAR FLARES SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: flare; Sun: chromosphere; Sun: flares; Sun: photosphere; Sun: transition region; Sun: UV radiation ID MONITOR TIM; EMISSION; EVENTS AB The Total Irradiance Monitor (TIM) from NASA's SOlar Radiation and Climate Experiment can detect changes in the total solar irradiance (TSI) to a precision of 2 ppm, allowing observations of variations due to the largest X-class solar flares for the first time. Presented here is a robust algorithm for determining the radiative output in the TIM TSI measurements, in both the impulsive and gradual phases, for the four solar flares presented in Woods et al., as well as an additional flare measured on 2006 December 6. The radiative outputs for both phases of these five flares are then compared to the vacuum ultraviolet (VUV) irradiance output from the Flare Irradiance Spectral Model (FISM) in order to derive an empirical relationship between the FISM VUV model and the TIM TSI data output to estimate the TSI radiative output for eight other X-class flares. This model provides the basis for the bolometric energy estimates for the solar flares analyzed in the Emslie et al. study. C1 [Moore, Christopher Samuel] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Moore, Christopher Samuel] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Moore, Christopher Samuel] Univ Colorado, Astrophys & Planetary Sci Dept, Boulder, CO 80309 USA. [Chamberlin, Phillip Clyde] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Hock, Rachel] Air Force Res Lab, Space Vehicle Directorate, Kirtland AFB, NM 87117 USA. RP Moore, CS (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, UCB 389, Boulder, CO 80309 USA. RI Chamberlin, Phillip/C-9531-2012 OI Chamberlin, Phillip/0000-0003-4372-7405 FU Laboratory for Atmospheric and Space Physics (LASP); NSF REU program FX The authors thank the Laboratory for Atmospheric and Space Physics (LASP) for their funding and support, as well as support from the NSF REU program. NR 25 TC 4 Z9 4 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 32 DI 10.1088/0004-637X/787/1/32 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200032 ER PT J AU Morley, CV Marley, MS Fortney, JJ Lupu, R Saumon, D Greene, T Lodders, K AF Morley, Caroline V. Marley, Mark S. Fortney, Jonathan J. Lupu, Roxana Saumon, Didier Greene, Tom Lodders, Katharina TI WATER CLOUDS IN Y DWARFS AND EXOPLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; planets and satellites: atmospheres; planets and satellites: detection; stars: atmospheres ID EXTRASOLAR GIANT PLANETS; COOLEST BROWN DWARFS; COLLISION-INDUCED ABSORPTION; HR 8799 PLANETS; T-DWARFS; ATMOSPHERIC CHEMISTRY; CHEMICAL-EQUILIBRIUM; MODEL ATMOSPHERES; CARBON-MONOXIDE; L/T TRANSITION AB The formation of clouds affects brown dwarf and planetary atmospheres of nearly all effective temperatures. Iron and silicate condense in L dwarf atmospheres and dissipate at the L/T transition. Minor species such as sulfides and salts condense in mid- to late T dwarfs. For brown dwarfs below T-eff similar to 450 K, water condenses in the upper atmosphere to form ice clouds. Currently, over a dozen objects in this temperature range have been discovered, and few previous theoretical studies have addressed the effect of water clouds on brown dwarf or exoplanetary spectra. Here we present a new grid of models that include the effect of water cloud opacity. We find that they become optically thick in objects below T-eff similar to 350-375 K. Unlike refractory cloud materials, water-ice particles are significantly nongray absorbers; they predominantly scatter at optical wavelengths through the J band and absorb in the infrared with prominent features, the strongest of which is at 2.8 mu m. H2O, NH3, CH4, and H-2 CIA are dominant opacity sources; less abundant species may also be detectable, including the alkalis, H2S, and PH3. PH3, which has been detected in Jupiter, is expected to have a strong signature in the mid-infrared at 4.3 mu m in Y dwarfs around T-eff = 450 K; if disequilibrium chemistry increases the abundance of PH3, it may be detectable over a wider effective temperature range than models predict. We show results incorporating disequilibrium nitrogen and carbon chemistry and predict signatures of low gravity in planetary mass objects. Finally, we make predictions for the observability of Y dwarfs and planets with existing and future instruments, including the James Webb Space Telescope and Gemini Planet Imager. C1 [Morley, Caroline V.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Marley, Mark S.; Lupu, Roxana; Greene, Tom] NASA, Ames Res Ctr, Naval Air Stn, Mountain View, CA 94035 USA. [Saumon, Didier] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Lodders, Katharina] Washington Univ, St Louis, MO 63130 USA. RP Morley, CV (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. EM cmorley@ucolick.org RI Marley, Mark/I-4704-2013; Lupu, Roxana/P-9060-2014; OI Lupu, Roxana/0000-0003-3444-5908; Marley, Mark/0000-0002-5251-2943 FU NSF [AST-1312545]; NASA Astrophysics Theory [NNH11AQ54I]; NASA Astrophysics Theory and Origins Programs FX The authors acknowledge Gregory Mace, Michael Liu, and the anonymous referee for comments that improved the paper. We also thank Andy Skemer for information on the observing capabilities of the LBT. We also acknowledge the Database of Ultracool Parallaxes maintained by Trent Dupuy. J.J.F. acknowledges the support of NSF grant AST-1312545, D.S. acknowledges the support of NASA Astrophysics Theory grant NNH11AQ54I, and M.S.M. and K.L. acknowledge the support of the NASA Astrophysics Theory and Origins Programs. We thank Ian Crossfield for identifying an error in a figure within a previous version of this manuscript. NR 102 TC 40 Z9 40 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 78 DI 10.1088/0004-637X/787/1/78 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200078 ER PT J AU Naud, ME Artigau, E Malo, L Albert, L Doyon, R Lafreniere, D Gagne, J Saumon, D Morley, CV Allard, F Homeier, D Beichman, CA Gelino, CR Boucher, A AF Naud, Marie-Eve Artigau, Etienne Malo, Lison Albert, Loic Doyon, Rene Lafreniere, David Gagne, Jonathan Saumon, Didier Morley, Caroline V. Allard, France Homeier, Derek Beichman, Charles A. Gelino, Christopher R. Boucher, Anne TI DISCOVERY OF A WIDE PLANETARY-MASS COMPANION TO THE YOUNG M3 STAR GU PSC SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: planetary systems; planetary systems; planets and satellites: detection; stars: imaging; stars: individual (GU Psc); stars: low-mass ID VERY-LOW-MASS; DIGITAL SKY SURVEY; ANGULAR-MOMENTUM EVOLUTION; COLOR-MAGNITUDE DIAGRAMS; BRIGHT SOURCE CATALOG; DORADUS MOVING GROUP; INFRARED FILTER SET; T-DWARF TRANSITION; GAS GIANT PLANETS; BROWN DWARFS AB We present the discovery of a comoving planetary-mass companion similar to 42 '' (similar to 2000AU) from a young M3 star, GU Psc, a likely member of the young AB Doradus Moving Group (ABDMG). The companion was first identified via its distinctively red i - z color (> 3.5) through a survey made with Gemini-S/GMOS. Follow-up Canada-France-Hawaii Telescope/WIRCam near-infrared (NIR) imaging, Gemini-N/GNIRS NIR spectroscopy and Wide-field Infrared Survey Explorer photometry indicate a spectral type of T3.5 +/- 1 and reveal signs of low gravity which we attribute to youth. Keck/Adaptive Optics NIR observations did not resolve the companion as a binary. A comparison with atmosphere models indicates T-eff = 1000-1100 K and log g = 4.5-5.0. Based on evolution models, this temperature corresponds to a mass of 9-13 M-Jup for the age of ABDMG (70-130 Myr). The relatively well-constrained age of this companion and its very large angular separation to its host star will allow its thorough characterization and will make it a valuable comparison for planetary-mass companions that will be uncovered by forthcoming planet-finder instruments such as Gemini Planet Imager and SPHERE. C1 [Naud, Marie-Eve; Artigau, Etienne; Malo, Lison; Albert, Loic; Doyon, Rene; Lafreniere, David; Gagne, Jonathan; Boucher, Anne] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Naud, Marie-Eve; Artigau, Etienne; Malo, Lison; Albert, Loic; Doyon, Rene; Lafreniere, David; Gagne, Jonathan; Boucher, Anne] Univ Montreal, Observ Mt Megantic, Montreal, PQ H3C 3J7, Canada. [Saumon, Didier] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Morley, Caroline V.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Allard, France; Homeier, Derek] Univ Lyon, Ecole Normale Super Lyon, UMR CNRS 5574, Ctr Rech Astrophys Lyon, F-69364 Lyon 07, France. [Beichman, Charles A.; Gelino, Christopher R.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Gelino, Christopher R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. RP Naud, ME (reprint author), Univ Montreal, Dept Phys, CP 6128, Montreal, PQ H3C 3J7, Canada. EM naud@astro.umontreal.ca OI Homeier, Derek/0000-0002-8546-9128; Gagne, Jonathan/0000-0002-2592-9612; Boucher, Anne/0000-0001-9427-1642; Lafreniere, David/0000-0002-6780-4252 FU Natural Sciences and Engineering Research Council (NSERC) of Canada; Fond de Recherche Quebecois-Nature et Technologie (FRQNT; Quebec); NASA [NNH11AQ54I]; European Research Council under the European Community [247060]; Gemini-S/PHOENIX: program [GS-2010B-Q-89]; Gemini-S/GMOS: program [GS-2011B-Q-74]; Gemini-S/NICI [GS-2011BQ-24, GS-2012B-Q-54]; Gemini-N/GNIRS: program [GN-2012B-Q-58]; European Southern Observatory Very Large Telescope under program [087.D-0510, 091.D-0641]; Universite de Montreal; Universite Laval and the Canada Foundation for Innovation; W.M. Keck Foundation; NASA InfraRed Telescope Facility, with SpeX [2013B025]; National Aeronautics and Space Administration, from the Two Micron All Sky Survey; National Aeronautics and Space Administration; National Science Foundation, of the NASA's Astrophysics Data System Bibliographic Services, SIMBAD database, the VizieR catalog access tool and the SIMBAD database operated at CDS, Strasbourg, France FX We would like to thank the anonymous referee for constructive comments and suggestions that greatly improved the overall quality of the paper. This work was financially supported by the Natural Sciences and Engineering Research Council (NSERC) of Canada and the Fond de Recherche Quebecois-Nature et Technologie (FRQNT; Quebec). D.S. is supported by NASA Astrophysics Theory grant NNH11AQ54I. D.H. acknowledges support from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013 Grant Agreement no. 247060). Based on observations obtained at the Gemini Observatory (Gemini-S/PHOENIX: program GS-2010B-Q-89, Gemini-S/GMOS: program GS-2011B-Q-74, Gemini-S/NICI: programs GS-2011BQ-24 and GS-2012B-Q-54 and Gemini-N/GNIRS: program GN-2012B-Q-58), 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 Cincia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologa e Innovacin Productiva (Argentina). Observations were also collected at CFHT with WIRCam (run IDs: 11BC20 and 12BC20) and ESPaDOnS (run ID: 12AC23), at the European Southern Observatory Very Large Telescope under program ID: 087.D-0510, 091.D-0641 and on CPAPIR infrared camera, at Observatoire du mont Megantic, which is funded by the Universite de Montreal, Universite Laval and the Canada Foundation for Innovation. 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 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. Finally, we also obtained data from the NASA InfraRed Telescope Facility, with SpeX, under the program number 2013B025. 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, from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, and funded by the National Aeronautics and Space Administration and the National Science Foundation, of the NASA's Astrophysics Data System Bibliographic Services, SIMBAD database, the VizieR catalog access tool and the SIMBAD database operated at CDS, Strasbourg, France. The BT-Settl model atmospheres have been computed at the Pole Scientifique de Modelisation Numerique of the ENS de Lyon, and at the Gesellschaft fur Wissenschaftliche Datenverarbeitung Gottingen in co-operation with the Institut fur Astrophysik Gottingen. This publication has made use of the L and T dwarf data archive, http://staff.gemini.edu/similar to sleggett/LTdata.html. NR 147 TC 39 Z9 39 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 5 DI 10.1088/0004-637X/787/1/5 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200005 ER PT J AU Rhoads, JE Malhotra, S Allam, S Carilli, C Combes, F Finkelstein, K Finkelstein, S Frye, B Gerin, M Guillard, P Nesvadba, N Rigby, J Spaans, M Strauss, MA AF Rhoads, James E. Malhotra, Sangeeta Allam, Sahar Carilli, Chris Combes, Francoise Finkelstein, Keely Finkelstein, Steven Frye, Brenda Gerin, Maryvonne Guillard, Pierre Nesvadba, Nicole Rigby, Jane Spaans, Marco Strauss, Michael A. TI HERSCHEL EXTREME LENSING LINE OBSERVATIONS: DYNAMICS OF TWO STRONGLY LENSED STAR-FORMING GALAXIES NEAR REDSHIFT z=2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift ID FRAME OPTICAL-SPECTRA; LYMAN BREAK GALAXIES; GAS; SPECTROSCOPY; EMISSION; ORIGIN; KINEMATICS; STELLAR; BRIGHT; DISK AB We report on two regularly rotating galaxies at redshift z approximate to 2, using high-resolution spectra of the bright [C II] 158 mu m emission line from the HIFI instrument on the Herschel Space Observatory. Both SDSS090122.37+181432.3 ("S0901") and SDSSJ120602.09+514229.5 ("the Clone") are strongly lensed and show the double-horned line profile that is typical of rotating gas disks. Using a parametric disk model to fit the emission line profiles, we find that S0901 has a rotation speed of nu sin(i) approximate to 120 +/- 7 kms(-1) and a gas velocity dispersion of sigma(g) < 23 km s-1 (1 sigma). The best-fitting model for the Clone is a rotationally supported disk having nu sin(i) approximate to 79 +/- 11 km s(-1) and sigma(g) less than or similar to 4 kms-1 (1 sigma). However, the Clone is also consistent with a family of dispersion-dominated models having sigma(g) = 92 +/- 20 km s (1). Our results showcase the potential of the [C II] line as a kinematic probe of high-redshift galaxy dynamics: [C II] is bright, accessible to heterodyne receivers with exquisite velocity resolution, and traces dense star-forming interstellar gas. Future [C II] line observations with ALMA would offer the further advantage of spatial resolution, allowing a clearer separation between rotation and velocity dispersion. C1 [Rhoads, James E.; Malhotra, Sangeeta] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Allam, Sahar] Space Telescope Inst, Baltimore, MD 21218 USA. [Carilli, Chris] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Combes, Francoise] CNRS, LERMA, Observ Paris, F-75014 Paris, France. [Finkelstein, Keely; Finkelstein, Steven] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Frye, Brenda] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Gerin, Maryvonne] LERMA, F-75231 Paris 05, France. [Guillard, Pierre; Nesvadba, Nicole] Ctr Univ Orsay, Inst Astrophys Spatiale, F-91405 Orsay, France. [Rigby, Jane] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Spaans, Marco] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Rhoads, JE (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM James.Rhoads@asu.edu RI Rigby, Jane/D-4588-2012; OI Rigby, Jane/0000-0002-7627-6551; Combes, Francoise/0000-0003-2658-7893 FU NASA through Herschel GO FX We are grateful to the DARK Cosmology Centre in Copenhagen, Denmark, Nordea Fonden in Copenhagen, the Institute for Advanced Study in Princeton, NJ, and Princeton University's Department of Astrophysical Sciences for hospitality during the completion of this work. We thank the staff at the NASA Herschel Science Center, and Adwin Boogert, in particular, for assistance in planning the observations. We thank Mike Gladders, Casey Papovich, and Min-Su Shin for their contributions to the HELLO project. We thank Scott Tremaine and Chuck Keeton for helpful discussions. We thank an anonymous referee for constructive suggestions. This work has been supported by NASA through Herschel GO funding. NR 33 TC 2 Z9 2 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 8 DI 10.1088/0004-637X/787/1/8 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200008 ER PT J AU Sankrit, R Raymond, JC Bautista, M Gaetz, TJ Williams, BJ Blair, WP Borkowski, KJ Long, KS AF Sankrit, Ravi Raymond, John C. Bautista, Manuel Gaetz, Terrance J. Williams, Brian J. Blair, William P. Borkowski, Kazimierz J. Long, Knox S. TI SPITZER IRS OBSERVATIONS OF THE XA REGION IN THE CYGNUS LOOP SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; ISM: abundances; ISM: individual objects (Cygnus Loop); ISM: supernova remnants ID SPACE-TELESCOPE; INFRARED SPECTROGRAPH; INTERSTELLAR-MEDIUM; ATOMIC DATABASE; EMISSION-LINES; SHOCK-WAVE; SPECTROSCOPY; EXCITATION; RAY; DUST AB We report on spectra of two positions in the XA region of the Cygnus Loop supernova remnant obtained with the InfraRed Spectrograph on the Spitzer Space Telescope. The spectra span the 10-35 mu m wavelength range, which contains a number of collisionally excited forbidden lines. These data are supplemented by optical spectra obtained at the Whipple Observatory and an archival UV spectrum from the International Ultraviolet Explorer. Coverage from the UV through the IR provides tests of shock wave models and tight constraints on model parameters. Only lines from high ionization species are detected in the spectrum of a filament on the edge of the remnant. The filament traces a 180 km s(-1) shock that has just begun to cool, and the oxygen to neon abundance ratio lies in the normal range found for Galactic H II regions. Lines from both high and low ionization species are detected in the spectrum of the cusp of a shock-cloud interaction, which lies within the remnant boundary. The spectrum of the cusp region is matched by a shock of about 150 km s(-1) that has cooled and begun to recombine. The post-shock region has a swept-up column density of about 1.3 x 10(18) cm(-2), and the gas has reached a temperature of 7000-8000 K. The spectrum of the Cusp indicates that roughly half of the refractory silicon and iron atoms have been liberated from the grains. Dust emission is not detected at either position. C1 [Sankrit, Ravi] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Raymond, John C.; Gaetz, Terrance J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Bautista, Manuel] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Williams, Brian J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Borkowski, Kazimierz J.] N Carolina State Univ, Raleigh, NC 27607 USA. [Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Sankrit, R (reprint author), NASA, Ames Res Ctr, SOFIA Sci Ctr, M-S N211-3, Moffett Field, CA 94035 USA. OI Blair, William/0000-0003-2379-6518 FU JPL Award [1278412]; North Carolina State University, Raleigh; USRA at the SOFIA Science Center; NASA [NAS8-03060]; Chandra X-ray Center FX This work was supported in part by the JPL Award 1278412 to the University of California, Berkeley, and North Carolina State University, Raleigh. We thank the anonymous referee for several useful suggestions, one of which led to Figure 9, providing a visual comparison of model predictions with observations. RS acknowledges support from USRA at the SOFIA Science Center. T.J.G. acknowledges support under NASA contract NAS8-03060 with the Chandra X-ray Center. NR 49 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 3 DI 10.1088/0004-637X/787/1/3 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200003 ER PT J AU Wardlow, JL Malhotra, S Zheng, Z Finkelstein, S Bock, J Bridge, C Calanog, J Ciardullo, R Conley, A Cooray, A Farrah, D Gawiser, E Gronwall, C Heinis, S Ibar, E Ivison, RJ Marsden, G Oliver, SJ Rhoads, J Riechers, D Schulz, B Smith, AJ Viero, M Wang, L Zemcov, M AF Wardlow, Julie L. Malhotra, S. Zheng, Z. Finkelstein, S. Bock, J. Bridge, C. Calanog, J. Ciardullo, R. Conley, A. Cooray, A. Farrah, D. Gawiser, E. Gronwall, C. Heinis, S. Ibar, E. Ivison, R. J. Marsden, G. Oliver, S. J. Rhoads, J. Riechers, D. Schulz, B. Smith, A. J. Viero, M. Wang, L. Zemcov, M. TI CONSTRAINING THE Ly alpha ESCAPE FRACTION WITH FAR- INFRARED OBSERVATIONS OF Ly alpha EMITTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: star formation; submillimeter: general ID DEEP-FIELD-SOUTH; STAR-FORMATION RATE; LYMAN-BREAK GALAXIES; DEGREE EXTRAGALACTIC SURVEY; FORMATION RATE INDICATOR; ACTIVE GALACTIC NUCLEI; INITIAL MASS FUNCTION; 2-10 KEV LUMINOSITY; SIMILAR-TO 4.5; HIGH-REDSHIFT AB We study the far-infrared properties of 498 Ly alpha emitters (LAEs) at z = 2.8, 3.1, and 4.5 in the Extended Chandra Deep Field-South, using 250, 350, and 500 mu m data from the Herschel Multi-tiered Extragalactic Survey and 870 mu m data from the LABOCA ECDFS Submillimeter Survey. None of the 126, 280, or 92 LAEs at z = 2.8, 3.1, and 4.5, respectively, are individually detected in the far-infrared data. We use stacking to probe the average emission to deeper flux limits, reaching 1 sigma depths of similar to 0.1 to 0.4 mJy. The LAEs are also undetected at >= 3 sigma in the stacks, although a 2.5 sigma signal is observed at 870 mu m for the z = 2.8 sources. We consider a wide range of far-infrared spectral energy distributions (SEDs), including an M82 and an Sd galaxy template, to determine upper limits on the far-infrared luminosities and far-infrared-derived star formation rates of the LAEs. These star formation rates are then combined with those inferred from the Ly alpha and UV emission to determine lower limits on the LAEs' Lya escape fraction (f(esc)(Ly alpha)). For the Sd SED template, the inferred LAEs fesc(Ly alpha) are greater than or similar to 30% (1 sigma) at z = 2.8, 3.1, and 4.5, which are all significantly higher than the global fesc(Ly alpha) at these redshifts. Thus, if the LAEs fesc(Ly alpha) follows the global evolution, then they have warmer far-infrared SEDs than the Sd galaxy template. The average and M82 SEDs produce lower limits on the LAE fesc(Ly alpha) of similar to 10%-20% (1 sigma), all of which are slightly higher than the global evolution of fesc(Ly alpha), but consistent with it at the 2 sigma-3 sigma level. C1 [Wardlow, Julie L.; Calanog, J.; Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Wardlow, Julie L.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Malhotra, S.; Zheng, Z.; Rhoads, J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Finkelstein, S.] Univ Texas Austin, Austin, TX 78712 USA. [Bock, J.; Bridge, C.; Cooray, A.; Schulz, B.; Viero, M.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ciardullo, R.; Gronwall, C.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Ciardullo, R.; Gronwall, C.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Gawiser, E.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Heinis, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ibar, E.] Catholic Univ Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Marsden, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Oliver, S. J.; Smith, A. J.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Riechers, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Schulz, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Wang, L.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. RP Wardlow, JL (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. EM jwardlow@dark-cosmology.dk RI Wardlow, Julie/C-9903-2015; Ivison, R./G-4450-2011 OI Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313 FU European Organisation for Astronomical Research in the Southern Hemisphere, Chile [078.F-9028(A), 079.F-9500(A), 080.A-3023(A), 081.F-9500(A)]; CSA (Canada; NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA) FX Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, under programmes 078.F-9028(A), 079.F-9500(A), 080.A-3023(A), and 081.F-9500(A). This research has made use of data from the HerMES project (http://hermes.sussex.ac.uk). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists, and a mission scientist. HerMES is described in Oliver et al. (2012). The data presented in this paper will be released through the HerMES Database in Marseille, HeDaM (http://hedam.oamp.fr/HerMES). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); 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). NR 104 TC 10 Z9 10 U1 2 U2 16 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 9 DI 10.1088/0004-637X/787/1/9 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200009 ER PT J AU Winebarger, AR Cirtain, J Golub, L DeLuca, E Savage, S Alexander, C Schuler, T AF Winebarger, Amy R. Cirtain, Jonathan Golub, Leon DeLuca, Edward Savage, Sabrina Alexander, Caroline Schuler, Timothy TI DISCOVERY OF FINELY STRUCTURED DYNAMIC SOLAR CORONA OBSERVED IN THE Hi-C TELESCOPE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: corona ID LOOPS; MOSS AB In the Summer of 2012, the High-resolution Coronal Imager (Hi-C) flew on board a NASA sounding rocket and collected the highest spatial resolution images ever obtained of the solar corona. One of the goals of the Hi-C flight was to characterize the substructure of the solar corona. We therefore examine how the intensity scales from AIA resolution to Hi-C resolution. For each low-resolution pixel, we calculate the standard deviation in the contributing high-resolution pixel intensities and compare that to the expected standard deviation calculated from the noise. If these numbers are approximately equal, the corona can be assumed to be smoothly varying, i.e., have no evidence of substructure in the Hi-C image to within Hi-C's ability to measure it given its throughput and readout noise. A standard deviation much larger than the noise value indicates the presence of substructure. We calculate these values for each low-resolution pixel for each frame of the Hi-C data. On average, 70% of the pixels in each Hi-C image show no evidence of substructure. The locations where substructure is prevalent is in the moss regions and in regions of sheared magnetic field. We also find that the level of substructure varies significantly over the roughly 160 s of the Hi-C data analyzed here. This result indicates that the finely structured corona is concentrated in regions of heating and is highly time dependent. C1 [Winebarger, Amy R.; Cirtain, Jonathan; Savage, Sabrina; Alexander, Caroline] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Golub, Leon; DeLuca, Edward] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schuler, Timothy] SUNY Coll Buffalo, Buffalo, NY 14222 USA. RP Winebarger, AR (reprint author), NASA, George C Marshall Space Flight Ctr, ZP 13, Huntsville, AL 35812 USA. EM amy.r.winebarger@nasa.gov RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Golub, Leon/0000-0001-9638-3082 FU NASA FX We thank the referee for many important observations and comments. We acknowledge the High-resolution Coronal Imager instrument grant funded by NASA's Low Cost Access to Space program. MSFC/NASA led the mission, and partners include the Smithsonian Astrophysical Observatory in Cambridge, MA; Lockheed Martin's Solar Astrophysical Laboratory in Palo Alto, Calif.; the University of Central Lancashire in Lancashire, England; and the Lebedev Physical Institute of the Russian Academy of Sciences in Moscow. NR 10 TC 5 Z9 5 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 20 PY 2014 VL 787 IS 1 AR L10 DI 10.1088/2041-8205/787/1/L10 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH3PE UT WOS:000336035800010 ER PT J AU Xiong, XX Butler, J Chiang, KF Efremova, B Fulbright, J Lei, N McIntire, J Oudrari, H Sun, JQ Wang, ZP Wu, AS AF Xiong, Xiaoxiong Butler, James Chiang, Kwofu Efremova, Boryana Fulbright, Jon Lei, Ning McIntire, Jeff Oudrari, Hassan Sun, Junqiang Wang, Zhipeng Wu, Aisheng TI VIIRS on-orbit calibration methodology and performance SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID REFLECTIVE SOLAR BANDS; MODIS; SENSORS AB The Visible Infrared Imaging Radiometer Suite (VIIRS) sensor aboard the Suomi National Polar-orbiting Partnership spacecraft has successfully operated since its launch in October 2011. The VIIRS collects data in 22 spectral bands that are calibrated by a set of onboard calibrators (OBC). In addition, lunar observations are made to independently track VIIRS long-term calibration stability for the reflective solar bands (RSB). This paper provides an overview of VIIRS OBC functions as well as its on-orbit operation and calibration activities. It also describes sensor calibration methodologies and demonstrates VIIRS on-orbit performance from launch to present. Results reported in this paper include on-orbit changes in sensor spectral band responses, detector noise characterization, and key calibration parameters. Issues identified and their potential impacts on sensor calibration are also discussed. Since launch, the VIIRS instrument nominal operation temperature has been stable to within +/- 1.0 K. The cold focal plane temperatures have been well controlled, with variations of less than 20 mK over a period of 1.5 years. In general, changes in thermal emissive bands (TEB) detector responses have been less than 0.5%. Despite large response degradation in several near-infrared and short-wave infrared bands and large SD degradation at short visible wavelengths, the VIIRS sensor and OBC overall performance has been excellent postlaunch. The degradation caused by the telescope mirror coating contamination has been modeled and its impact addressed through the use of modulated relative spectral response in the improved calibration and the current sensor data record data production. Based on current instrument characteristics and performance, it is expected that the VIIRS calibration will continue to meet its design requirements, including RSB detector signal to noise ratio and TEB detector noise equivalent temperature difference, throughout its 7 year design lifetime. C1 [Xiong, Xiaoxiong; Butler, James] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. [Chiang, Kwofu; Efremova, Boryana; Fulbright, Jon; Lei, Ning; McIntire, Jeff; Oudrari, Hassan; Sun, Junqiang; Wang, Zhipeng; Wu, Aisheng] Sigma Space Corp, Lanham, MD USA. RP Xiong, XX (reprint author), NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. EM Xiaoxiong.Xiong-1@nasa.gov OI Wang, Zhipeng/0000-0002-9108-9009 NR 33 TC 70 Z9 70 U1 5 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 19 PY 2014 VL 119 IS 9 BP 5065 EP 5078 DI 10.1002/2013JD020423 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AK3QS UT WOS:000338340400003 ER PT J AU Ueyama, R Jensen, EJ Pfister, L Diskin, GS Bui, TP Dean-Day, JM AF Ueyama, Rei Jensen, Eric J. Pfister, Leonhard Diskin, Glenn S. Bui, T. P. Dean-Day, Jonathan M. TI Dehydration in the tropical tropopause layer: A case study for model evaluation using aircraft observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID STRATOSPHERIC WATER-VAPOR; ICE NUCLEATION; KELVIN WAVES; TRANSPORT; HYGROMETER; SYSTEM; CIRRUS AB The dynamical and microphysical processes that influence water vapor concentrations in the tropical tropopause layer (TTL) are investigated in simulations of ice clouds along backward trajectories of air parcels sampled during three flights of the Airborne Tropical Tropopause Experiment over the central to eastern tropical Pacific in boreal fall 2011. ERA-Interim reanalysis temperatures interpolated onto the flight tracks have a negligible (-0.09 K) cold bias compared to aircraft measurements of tropical cold point temperature thus permitting case study simulations of TTL dehydration. When the effects of subgrid-scale waves, cloud microphysical processes, and convection are considered, the simulated water vapor mixing ratios on the final day of 40 day backward trajectories exhibit a mean profile that is within 20-30% of the mean of the aircraft measurements collected during vertical profiling maneuvers between the 350 and 410 K potential temperature levels. Averaged over the three flights, temperature variability driven by subgrid-scale waves dehydrated the 360-390 K layer by approximately -0.5 ppmv, whereas including homogeneous freezing of aqueous aerosols and subsequent sublimation and rehydration of ice crystals increased water vapor below the 380 K level by about +1 ppmv. The predominant impact of convection was to moisten the TTL, resulting in an average enhancement below the 370 K level by +1 to 5 ppmv. Accurate (to within 0.5-1 ppmv) predictions of TTL water vapor using trajectory models require proper representations of waves, in situ ice cloud formation, and convective influence, which together determine the saturation history of air parcels. C1 [Ueyama, Rei; Jensen, Eric J.; Pfister, Leonhard; Bui, T. P.; Dean-Day, Jonathan M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Diskin, Glenn S.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Dean-Day, Jonathan M.] Bay Area Environm Res Inst, Sonoma, CA USA. RP Ueyama, R (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM rei.ueyama@nasa.gov FU NASA Airborne Tropical Tropopause Experiment; NASA Postdoctoral Program FX ATTREX data are publicly available at the NASA Earth Science Project Office web-site (http://espo.nasa.gov/missions/attrex/). We thank the Aura Science Team for the MLS data and three anonymous reviewers for their thoughtful comments and suggestions on the manuscript. This work was funded by the NASA Airborne Tropical Tropopause Experiment and the NASA Postdoctoral Program. NR 52 TC 9 Z9 9 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 19 PY 2014 VL 119 IS 9 BP 5299 EP 5316 DI 10.1002/2013JD021381 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AK3QS UT WOS:000338340400018 ER PT J AU Oman, LD Douglass, AR AF Oman, Luke D. Douglass, Anne R. TI Improvements in total column ozone in GEOSCCM and comparisons with a new ozone-depleting substances scenario SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID QUASI-BIENNIAL OSCILLATION; STRATOSPHERIC OZONE; CLIMATE-CHANGE; DATA RECORD; CHEMISTRY; UNCERTAINTY; SOUTHERN; EESC AB The evolution of ozone is examined in the latest version of the Goddard Earth Observing System Chemistry-Climate Model (GEOSCCM) using old and new ozone-depleting substances (ODS) scenarios. This version of GEOSCCM includes a representation of the quasi-biennial oscillation, a more realistic implementation of ozone chemistry at high solar zenith angles, an improved air/sea roughness parameterization, and an extra 5 parts per trillion of CH3Br to account for brominated very short-lived substances. Together these additions improve the representation of ozone compared to observations. This improved version of GEOSCCM was used to simulate the ozone evolution for the A1 2010 and the new Stratosphere-troposphere Processes and their Role in Climate (SPARC) 2013 ODS scenario derived using the SPARC Lifetimes Report 2013. This new ODS scenario results in a maximum Cl-tot increase of 65 parts per trillion by volume (pptv), decreasing slightly to 60 pptv by 2100. Approximately 72% of the increase is due to the longer lifetime of CFC-11. The quasi-global (60 degrees S-60 degrees N) total column ozone difference is relatively small and less than 1 Dobson unit on average and consistent with the 3-4% larger 2050-2080 average Cl-y in the new SPARC 2013 scenario. Over high latitudes, this small change in Cl-y compared to the relatively large natural variability makes it not possible to discern a significant impact on ozone in the second half of the 21st century in a single set of simulations. C1 [Oman, Luke D.; Douglass, Anne R.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. RP Oman, LD (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. EM luke.d.oman@nasa.gov RI Oman, Luke/C-2778-2009; Douglass, Anne/D-4655-2012 OI Oman, Luke/0000-0002-5487-2598; FU NASA MAP FX The NASA MAP program supported this research. We would like to thank Susan Strahan for helpful comments on this manuscript and Guus Velders for providing the new ODS scenario. We would like to thank four anonymous reviewers for their helpful comments and suggestions for improving this manuscript. We would also like to thank those involved in model development at GSFC and the high-performance computing resources that were provided by NASA's Advanced Supercomputing Division. NR 41 TC 12 Z9 12 U1 0 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 19 PY 2014 VL 119 IS 9 BP 5613 EP 5624 DI 10.1002/2014JD021590 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AK3QS UT WOS:000338340400038 ER PT J AU Kim, E Lyu, CHJ Anderson, K Leslie, RV Blackwell, WJ AF Kim, Edward Lyu, Cheng-Hsuan J. Anderson, Kent Leslie, R. Vincent Blackwell, William J. TI S-NPP ATMS instrument prelaunch and on-orbit performance evaluation SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TECHNOLOGY MICROWAVE SOUNDER; CALIBRATION; UNIT AB The first of a new generation of microwave sounders was launched aboard the Suomi-National Polar-Orbiting Partnership satellite in October 2011. The Advanced Technology Microwave Sounder (ATMS) combines the capabilities and channel sets of three predecessor sounders into a single package to provide information on the atmospheric vertical temperature and moisture profiles that are the most critical observations needed for numerical weather forecast models. Enhancements include size/mass/power approximately one third of the previous total, three new sounding channels, the first space-based, Nyquist-sampled cross-track microwave temperature soundings for improved fusion with infrared soundings, plus improved temperature control and reliability. This paper describes the ATMS characteristics versus its predecessor, the advanced microwave sounding unit (AMSU), and presents the first comprehensive evaluation of key prelaunch and on-orbit performance parameters. Two-year on-orbit performance shows that the ATMS has maintained very stable radiometric sensitivity, in agreement with prelaunch data, meeting requirements for all channels (with margins of similar to 40% for channels 1-15), and improvements over AMSU-A when processed for equivalent spatial resolution. The radiometric accuracy, determined by analysis from ground test measurements, and using on-orbit instrument temperatures, also shows large margins relative to requirements (specified as <1.0 K for channels 1, 2, and 16-22 and <0.75 K for channels 3-15). A thorough evaluation of the performance of ATMS is especially important for this first proto-flight model unit of what will eventually be a series of ATMS sensors providing operational sounding capability for the U.S. and its international partners well into the next decade. C1 [Kim, Edward] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lyu, Cheng-Hsuan J.] NASA, Goddard Space Flight Ctr, IM Syst Grp, Greenbelt, MD 20771 USA. [Anderson, Kent] Northrop Grumman Elect Syst, Azusa, CA USA. [Leslie, R. Vincent; Blackwell, William J.] MIT Lincoln Lab, Lexington, MA USA. RP Kim, E (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM ed.kim@nasa.gov NR 23 TC 8 Z9 8 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 19 PY 2014 VL 119 IS 9 BP 5653 EP 5670 DI 10.1002/2013JD020483 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AK3QS UT WOS:000338340400041 ER PT J AU Ziemke, JR Olsen, MA Witte, JC Douglass, AR Strahan, SE Wargan, K Liu, X Schoeberl, MR Yang, K Kaplan, TB Pawson, S Duncan, BN Newman, PA Bhartia, PK Heney, MK AF Ziemke, J. R. Olsen, M. A. Witte, J. C. Douglass, A. R. Strahan, S. E. Wargan, K. Liu, X. Schoeberl, M. R. Yang, K. Kaplan, T. B. Pawson, S. Duncan, B. N. Newman, P. A. Bhartia, P. K. Heney, M. K. TI Assessment and applications of NASA ozone data products derived from Aura OMI/MLS satellite measurements in context of the GMI chemical transport model SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPICAL TROPOSPHERIC OZONE; VARIATIONAL STATISTICAL-ANALYSIS; 1997-1998 EL-NINO; COLUMN OZONE; INTERANNUAL VARIABILITY; MONITORING INSTRUMENT; RECURSIVE FILTERS; NUMERICAL ASPECTS; MLS MEASUREMENTS; ARCTIC OZONE AB Measurements from the Ozone Monitoring Instrument (OMI) and Microwave Limb Sounder (MLS), both on board the Aura spacecraft, have been used to produce daily global maps of column and profile ozone since August 2004. Here we compare and evaluate three strategies to obtain daily maps of tropospheric and stratospheric ozone from OMI and MLS measurements: trajectory mapping, direct profile retrieval, and data assimilation. Evaluation is based on an assessment that includes validation using ozonesondes and comparisons with the Global Modeling Initiative (GMI) chemical transport model. We investigate applications of the three ozone data products from near-decadal and interannual time scales to day-to-day case studies. Interannual changes in zonal mean tropospheric ozone from all of the products in any latitude range are of the order 1-2 Dobson units while changes (increases) over the 8 year Aura record investigated vary by 2-4 Dobson units. It is demonstrated that all of the ozone products can measure and monitor exceptional tropospheric ozone events including major forest fire and pollution transport events. Stratospheric ozone during the Aura record has several anomalous interannual events including split stratospheric warmings in the Northern Hemisphere extratropics that are well captured using the data assimilation ozone profile product. Data assimilation with continuous daily global coverage and vertical ozone profile information is the best of the three strategies at generating a global tropospheric and stratospheric ozone product for science applications. C1 [Ziemke, J. R.; Olsen, M. A.] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA. [Ziemke, J. R.; Olsen, M. A.; Douglass, A. R.; Strahan, S. E.; Wargan, K.; Pawson, S.; Duncan, B. N.; Newman, P. A.; Bhartia, P. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Witte, J. C.; Wargan, K.; Heney, M. K.] Sci Syst & Applicat Inc, Lanham, MD USA. [Strahan, S. E.] Univ Space Res Assoc, Columbia, MD USA. [Liu, X.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schoeberl, M. R.] Sci & Technol Corp, Lanham, MD USA. [Yang, K.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Kaplan, T. B.] INNOVIM, Greenbelt, MD USA. RP Ziemke, JR (reprint author), Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA. EM jerald.r.ziemke@gsfc.nasa.gov RI Douglass, Anne/D-4655-2012; Liu, Xiong/P-7186-2014; Bhartia, Pawan/A-4209-2016; Pawson, Steven/I-1865-2014; Duncan, Bryan/A-5962-2011; OI Liu, Xiong/0000-0003-2939-574X; Bhartia, Pawan/0000-0001-8307-9137; Pawson, Steven/0000-0003-0200-717X; Wargan, Krzysztof/0000-0002-3795-2983 FU NASA [NNH07ZDA001N-AST] FX The authors thank the Aura MLS and OMI instrument and algorithm teams for the extensive satellite measurements used in this study. We also thank the Editor and three reviewers for valuable comments that were very beneficial in improving the paper. OMI is a Dutch-Finnish contribution to the Aura mission. Funding for this research was provided in part by NASA NNH07ZDA001N-AST. NR 57 TC 10 Z9 10 U1 4 U2 23 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 19 PY 2014 VL 119 IS 9 BP 5671 EP 5699 DI 10.1002/2013JD020914 PG 29 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AK3QS UT WOS:000338340400042 ER PT J AU Parrish, DD Lamarque, JF Naik, V Horowitz, L Shindell, DT Staehelin, J Derwent, R Cooper, OR Tanimoto, H Volz-Thomas, A Gilge, S Scheel, HE Steinbacher, M Frohlich, M AF Parrish, D. D. Lamarque, J. -F. Naik, V. Horowitz, L. Shindell, D. T. Staehelin, J. Derwent, R. Cooper, O. R. Tanimoto, H. Volz-Thomas, A. Gilge, S. Scheel, H. -E. Steinbacher, M. Froehlich, M. TI Long-term changes in lower tropospheric baseline ozone concentrations: Comparing chemistry-climate models and observations at northern midlatitudes SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID INTERCOMPARISON PROJECT ACCMIP; BIOMASS BURNING EMISSIONS; ATMOSPHERIC CHEMISTRY; PREINDUSTRIAL; SIMULATIONS; TRENDS; OH AB Two recent papers have quantified long-term ozone (O-3) changes observed at northern midlatitude sites that are believed to represent baseline (here understood as representative of continental to hemispheric scales) conditions. Three chemistry-climate models (NCAR CAM-chem, GFDL-CM3, and GISS-E2-R) have calculated retrospective tropospheric O-3 concentrations as part of the Atmospheric Chemistry and Climate Model Intercomparison Project and Coupled Model Intercomparison Project Phase 5 model intercomparisons. We present an approach for quantitative comparisons of model results with measurements for seasonally averaged O-3 concentrations. There is considerable qualitative agreement between the measurements and the models, but there are also substantial and consistent quantitative disagreements. Most notably, models (1) overestimate absolute O3 mixing ratios, on average by similar to 5 to 17 ppbv in the year 2000, (2) capture only similar to 50% of O-3 changes observed over the past five to six decades, and little of observed seasonal differences, and (3) capture similar to 25 to 45% of the rate of change of the long-term changes. These disagreements are significant enough to indicate that only limited confidence can be placed on estimates of present-day radiative forcing of tropospheric O-3 derived from modeled historic concentration changes and on predicted future O-3 concentrations. Evidently our understanding of tropospheric O-3, or the incorporation of chemistry and transport processes into current chemical climate models, is incomplete. Modeled O-3 trends approximately parallel estimated trends in anthropogenic emissions of NOx, an important O-3 precursor, while measured O-3 changes increase more rapidly than these emission estimates. C1 [Parrish, D. D.; Cooper, O. R.] NOAA, ESRL, Div Chem Sci, Boulder, CO 80307 USA. [Lamarque, J. -F.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Naik, V.] NOAA, UCAR, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Horowitz, L.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Shindell, D. T.] Natl Aeronaut & Space Agcy, Goddard Inst Space Studies, New York, NY USA. [Staehelin, J.] ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland. [Derwent, R.] Rdscientific, Newbury, Berks, England. [Cooper, O. R.] Univ Colorado, CIRES, Boulder, CO 80309 USA. [Tanimoto, H.] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan. [Volz-Thomas, A.] Forschungszentrum Julich, IEK 8, D-52425 Julich, Germany. [Gilge, S.] Hohenpeissenberg Meteorol Observ, German Meteorol Serv, Hohenpeissenberg, Germany. [Scheel, H. -E.] Karlsruhe Inst Technol, IMK IFU, Garmisch Partenkirchen, Germany. [Steinbacher, M.] Swiss Fed Labs Mat Sci & Technol, Dubendorf, Switzerland. [Froehlich, M.] Environm Agcy, Air Pollut Control & Climate Change Mitigat, Vienna, Austria. RP Parrish, DD (reprint author), NOAA, ESRL, Div Chem Sci, Boulder, CO 80307 USA. EM David.D.Parrish@noaa.gov RI Steinbacher, Martin/B-7424-2009; Naik, Vaishali/A-4938-2013; Shindell, Drew/D-4636-2012; Manager, CSD Publications/B-2789-2015; Lamarque, Jean-Francois/L-2313-2014; Parrish, David/E-8957-2010; Cooper, Owen/H-4875-2013; Horowitz, Larry/D-8048-2014; Volz-Thomas, Andreas/J-7223-2012; Tanimoto, Hiroshi/E-6779-2010 OI Steinbacher, Martin/0000-0002-7195-8115; Naik, Vaishali/0000-0002-2254-1700; Derwent, Richard/0000-0003-4498-645X; Lamarque, Jean-Francois/0000-0002-4225-5074; Parrish, David/0000-0001-6312-2724; Horowitz, Larry/0000-0002-5886-3314; Volz-Thomas, Andreas/0000-0003-3700-1667; Tanimoto, Hiroshi/0000-0002-5424-9923 FU National Science Foundation; Office of Science (BER) of the U. S. Department of Energy; Global Environment Research Fund of the Ministry of the Environment, Japan [S-7-1] FX The CESM project (which includes the CAM-chem model) is supported by the National Science Foundation and the Office of Science (BER) of the U. S. Department of Energy. NCAR is operated by the University Corporation of Atmospheric Research under sponsorship of the National Science Foundation. The authors are grateful to the Umweltamt of Graubunden and J. Thudium for providing the Arosa data sets, to the German Umweltbundesamt for providing recent data from Zingst, and to P. G. Simmonds and T. G Spain for providing the Mace Head data, to A. J. Manning for sorting the Mace Head data into baseline and non-baseline observations, to NOAA Earth System Research Laboratory, Global Monitoring Division, for providing data from Trinidad Head, to U. S. National Park Service 2002 for providing Lassen NP data, and to Acid Deposition Monitoring Network in East Asia for providing the Mount Happo and Japanese MBL data. The data analyzed here are available from the sources acknowledged above or the authors themselves. D. Parrish acknowledges support from NOAA's Health of the Atmosphere and Atmospheric Chemistry and Climate Programs. H. Tanimoto acknowledges support from the Global Environment Research Fund of the Ministry of the Environment, Japan (S-7-1). NR 42 TC 43 Z9 44 U1 10 U2 96 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 19 PY 2014 VL 119 IS 9 BP 5719 EP 5736 DI 10.1002/2013JD021435 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AK3QS UT WOS:000338340400044 ER PT J AU Strekalov, DV Kulikov, I Yu, N AF Strekalov, Dmitry V. Kulikov, Igor Yu, Nan TI Imaging dark objects with intensity interferometry SO OPTICS EXPRESS LA English DT Article ID PHASE RETRIEVAL; SCINTILLATION AB We have developed a technique for imaging dark, i.e. non-radiating, objects by intensity interferometry measurements using a thermal light source in the background. This technique is based on encoding the dark object's profile into the spatial coherence of such light. We demonstrate the image recovery using an adaptive error-minimizing Gerchberg-Saxton algorithm in case of a completely opaque object, and outline the steps for imaging purely refractive objects. (C) 2014 Optical Society of America C1 [Strekalov, Dmitry V.; Kulikov, Igor; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Strekalov, DV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Dmitry.V.Strekalov@jpl.nasa.gov FU NIAC program; National Aeronautics and Space Administration FX This work was funded by the NIAC program and carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. NR 18 TC 5 Z9 7 U1 3 U2 9 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD MAY 19 PY 2014 VL 22 IS 10 BP 12339 EP 12348 DI 10.1364/OE.22.012339 PG 10 WC Optics SC Optics GA AI6CP UT WOS:000336957700094 PM 24921352 ER PT J AU Kim, Y Kimball, JS Zhang, K Didan, K Velicogna, I McDonald, KC AF Kim, Youngwook Kimball, J. S. Zhang, K. Didan, K. Velicogna, I. McDonald, K. C. TI Attribution of divergent northern vegetation growth responses to lengthening non-frozen seasons using satellite optical-NIR and microwave remote sensing SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Review ID ATMOSPHERIC CARBON-DIOXIDE; NET PRIMARY PRODUCTION; CANADA BOREAL FORESTS; ARCTIC SEA-ICE; CLIMATE-CHANGE; FIRE DISTURBANCE; AIR-TEMPERATURE; TRENDS; NDVI; CYCLE AB The non-frozen (NF) season duration strongly influences the northern carbon cycle where frozen (FR) temperatures are a major constraint to biological processes. The landscape freeze-thaw (FT) signal from satellite microwave remote sensing provides a surrogate measure of FR temperature constraints to ecosystem productivity, trace gas exchange, and surface water mobility. We analysed a new global satellite data record of daily landscape FT dynamics derived from temporal classification of overlapping SMMR and SSM/I 37GHz frequency brightness temperatures (T-b). The FT record was used to quantify regional patterns, annual variability, and trends in the NF season over northern (>= 45 degrees N) vegetated land areas. The ecological significance of these changes was evaluated against satellite normalized difference vegetation index (NDVI) anomalies, estimated moisture and temperature constraints to productivity determined from meteorological reanalysis, and atmospheric CO2 records. The FT record shows a lengthening (2.4daysdecade(-1); p<0.005) mean annual NF season trend (1979-2010) for the high northern latitudes that is 26% larger than the Northern Hemisphere trend. The NDVI summer growth response to these changes is spatially complex and coincides with local dominance of cold temperature or moisture constraints to productivity. Longer NF seasons are predominantly enhancing productivity in cold temperature-constrained areas, whereas these effects are reduced or reversed in more moisture-constrained areas. Longer NF seasons also increase the atmospheric CO2 seasonal amplitude by enhancing both regional carbon uptake and emissions. We find that cold temperature constraints to northern growing seasons are relaxing, whereas potential benefits for productivity and carbon sink activity are becoming more dependent on the terrestrial water balance and supply of plant-available moisture needed to meet additional water use demands under a warming climate. C1 [Kim, Youngwook; Kimball, J. S.] Univ Montana, Flathead Lake Biol Stn, Polson, MT 59860 USA. [Kim, Youngwook; Kimball, J. S.] Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. [Zhang, K.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Didan, K.] Univ Arizona, Dept Elect & Comp Engn, Tucson, AZ 85721 USA. [Velicogna, I.] Univ Calif Irvine, Irvine, CA 92697 USA. [McDonald, K. C.] CUNY City Coll, New York, NY 10031 USA. [McDonald, K. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kim, Y (reprint author), Univ Montana, Flathead Lake Biol Stn, Polson, MT 59860 USA. EM youngwook.kim@ntsg.umt.edu RI Zhang, Ke/B-3227-2012 OI Zhang, Ke/0000-0001-5288-9372 FU NASA FX This work was conducted at the University of Montana under contract to the National Aeronautics and Space Administration, with funding support provided by the NASA Terrestrial Ecology and Hydrology programmes. The FT-ESDR and VIP NDVI data records used for this investigation were provided by the National Snow and Ice Data Center (NSIDC) and the University of Arizona, with funding support provided by the NASA measures (Making Earth System Data Records for Use in Research Environments) programme. The GLOBALVIEW-CO2 data record used for this study was provided by the NOAA ESRL (Earth System Research Laboratory). NR 110 TC 9 Z9 9 U1 3 U2 42 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 EI 1366-5901 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD MAY 19 PY 2014 VL 35 IS 10 BP 3700 EP 3721 DI 10.1080/01431161.2014.915595 PG 22 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA AH1DR UT WOS:000335860500016 ER PT J AU De Sanctis, MC Ammannito, E Buczkowski, D Raymond, CA Jaumann, R Mittlefehldt, DW Capaccioni, F Capria, MT Frigeri, A Magni, G Tosi, F Zambon, F Russell, CT AF De Sanctis, M. C. Ammannito, E. Buczkowski, D. Raymond, C. A. Jaumann, R. Mittlefehldt, D. W. Capaccioni, F. Capria, M. T. Frigeri, A. Magni, G. Tosi, F. Zambon, F. Russell, C. T. TI Compositional evidence of magmatic activity on Vesta SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ASTEROID 4 VESTA; DAWN; OLIVINE; SURFACE; 4-VESTA; BODIES; CORE AB Like the Earth and other terrestrial planets, the asteroid Vesta has a basaltic crust and a large iron core; its surface is dominated by impact craters of all sizes and has tectonic features. The presence of basaltic compositions, olivine, howardite-eucrite-diogenite meteorites, and models of Vesta's formation, suggests that volcanic and/or magmatic activity could have occurred on Vesta. A global search for lobate structures did not find unequivocal evidence of volcanic features. Nevertheless, several morphological properties of Brumalia Tholus on Vestalia Terra suggest that this topographic high most likely formed as a magmatic intrusion. The presence of more orthopyroxene-rich material relative to surrounding terrain in the ejecta of Teia, a fresh impact crater on the northern face of Brumalia Tholus, supports the hypothesis of magmatic intrusions on Vesta. C1 [De Sanctis, M. C.; Ammannito, E.; Capaccioni, F.; Capria, M. T.; Frigeri, A.; Magni, G.; Tosi, F.; Zambon, F.] INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy. [Buczkowski, D.] JHU APL, Laurel, MD USA. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Jaumann, R.] DLR, Inst Planetary Res, Berlin, Germany. [Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. RP De Sanctis, MC (reprint author), INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy. EM mariacristina.desanctis@iaps.inaf.it RI Frigeri, Alessandro/F-2151-2010; Buczkowski, Debra/I-7842-2015; OI Capaccioni, Fabrizio/0000-0003-1631-4314; Tosi, Federico/0000-0003-4002-2434; Frigeri, Alessandro/0000-0002-9140-3977; Buczkowski, Debra/0000-0002-4729-7804; Zambon, Francesca/0000-0002-4190-6592; capria, maria teresa/0000-0002-9814-9588; De Sanctis, Maria Cristina/0000-0002-3463-4437 FU Italian Space Agency (ASI); NASA through the Dawn project; NASA through Dawn at Vesta Participating Scientists Program; Italian Space Agency FX The authors gratefully acknowledge the support of the Dawn Instrument, Operations, Science Teams, and FC team. This work is supported by an Italian Space Agency (ASI) and by NASA through the Dawn project and the Dawn at Vesta Participating Scientists Program. VIR is funded by the Italian Space Agency and was developed under the leadership of INAF-Instituto di Astrofisica e Planetologia Spaziali, Rome, Italy. The instrument was built by Selex-Galileo, Florence, Italy. The data for this paper are available at PDS Node (http://sbn.pds.nasa.gov/data_sb/index.shtml). The authors thank Noah Petro and Leslie F. Bleamaster III for their helpful comments. NR 36 TC 10 Z9 10 U1 1 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 16 PY 2014 VL 41 IS 9 BP 3038 EP 3044 DI 10.1002/2014GL059646 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AK1SP UT WOS:000338196700004 ER PT J AU Reul, N Chapron, B Lee, T Donlon, C Boutin, J Alory, G AF Reul, N. Chapron, B. Lee, T. Donlon, C. Boutin, J. Alory, G. TI Sea surface salinity structure of the meandering Gulf Stream revealed by SMOS sensor SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID WARM-CORE RING; DIAGNOSTIC MODEL; OCEAN; TEMPERATURE; CURRENTS AB Measurements from the Soil Moisture Ocean Salinity (SMOS) satellite acquired during 2012 in the western North Atlantic are used to reveal the evolution of the sea surface salinity (SSS) structure of the meandering Gulf Stream with an unprecedented space and time resolution. Combined with in situ surface and profile measurements, satellite-derived surface currents, sea surface height (SSH), surface temperature (SST), and chlorophyll (Chl) data, SMOS SSS observations are shown to coherently delineate meanders pinching off from the current to form well-identified salty-(warm-) and fresh-(cold-) core Gulf Stream rings. A covariance analysis at two locations along the separated Gulf stream path (south of Nova Scotia and in the Gulf Stream Extension) reveals a systematically higher correlation between SSS and sea level variability than between SST and SSH during the warmer half of the year. Within (75 degrees W-40 degrees W; 30 degrees N-50 degrees N), Chl concentration is also found to significantly depend on the SSS as SST increases above 20 degrees C. C1 [Reul, N.; Chapron, B.] IFREMER, Lab Oceanog Spatiale, Plouzane, France. [Lee, T.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA. [Donlon, C.] European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands. [Boutin, J.] Lab Oceanog & Climat Expt & Approches Numer, Paris, France. [Alory, G.] Univ Toulouse 3, LEGOS, F-31062 Toulouse, France. RP Reul, N (reprint author), IFREMER, Lab Oceanog Spatiale, Plouzane, France. EM nreul@ifremer.fr RI Chapron, Bertrand/O-6527-2015; reul, nicolas/C-4895-2009; Boutin, Jacqueline/M-2253-2016; OI Reul, Nicolas/0000-0003-4881-2967 FU ESA; CNES of the Centre Aval de Traitement des Donnees SMOS (CATDS) project; CNES of the SMOS/ESA GLOSCAL Cal/Val project; French Ministry of Research and Education of the LabexMER project; French Ministry of Research and Education of the ANR program "REDHOTS" FX Work presented in this paper was partly done under ESA support in the context of the development of the SMOS level 2/Expert Support Laboratory, ESA Support to Science Element SMOS SOS project. CNES also partly funded these activities in the frame of the Centre Aval de Traitement des Donnees SMOS (CATDS) and of the SMOS/ESA GLOSCAL Cal/Val projects. The French Ministry of Research and Education also funded this activity in the frame of the LabexMER project and of the ANR program "REDHOTS" (high-resolution 3-D reconstruction of the dynamics of the upper layers of the ocean). VOS TSG data were collected and processed by the SSS observation service at LEGOS. We thank Gilles Reverdin for his advices concerning Oleander data and Fabienne Gaillard for providing SSS climatology. The data for this paper are freely available at the following data centers: SMOS SSS can be obtained at the Cnes/Ifremer CATDS center; ODYSSEA SST and in situ data at the Ifremer/CERSAT and CORIOLIS centers, respectively; SSH fields at the Cnes/AVISO center; and the chlorophyll concentration from Aqua/MODIS are available at NASA Goddard Space Flight Center. NR 26 TC 23 Z9 23 U1 1 U2 21 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 16 PY 2014 VL 41 IS 9 BP 3141 EP 3148 DI 10.1002/2014GL059215 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AK1SP UT WOS:000338196700018 ER PT J AU Reale, O Lau, KM da Silva, A Matsui, T AF Reale, O. Lau, K. M. da Silva, A. Matsui, T. TI Impact of assimilated and interactive aerosol on tropical cyclogenesis SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SAHARAN AIR LAYER; GLOBAL DATA ASSIMILATION; AFRICAN EASTERLY JET; FORECAST SYSTEM; SOP-3 NAMMA; ATLANTIC AB This article investigates the impact of Saharan dust on the development of tropical cyclones in the Atlantic. A global data assimilation and forecast system, the NASA GEOS-5, is used to assimilate all satellite and conventional data sets used operationally for numerical weather prediction. In addition, this new GEOS-5 version includes assimilation of aerosol optical depth from the Moderate Resolution Imaging Spectroradiometer. The analysis so obtained comprises atmospheric quantities and a realistic 3-D aerosol and cloud distribution, consistent with the meteorology and validated against Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation and CloudSat data. These improved analyses are used to initialize GEOS-5 forecasts, explicitly accounting for aerosol direct radiative effects and their impact on the atmospheric dynamics. Parallel simulations with/without aerosol radiative effects show that effects of dust on static stability increase with time, becoming highly significant after day 5 and producing an environment less favorable to tropical cyclogenesis. C1 [Reale, O.; Lau, K. M.; Matsui, T.] NASA, Goddard Space Flight Ctr, Earth Sci Div Atmospheres, Greenbelt, MD 20771 USA. [Reale, O.] Univ Space Res Assoc, Columbia, MD USA. [da Silva, A.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Matsui, T.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Reale, O (reprint author), NASA, Goddard Space Flight Ctr, Earth Sci Div Atmospheres, Greenbelt, MD 20771 USA. EM oreste.reale-1@nasa.gov RI Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 FU CALIPSO-CloudSat grant FX The authors thank Hal Maring for support through a CALIPSO-CloudSat grant and Tsengdar Lee for allocations on NASA High-End Computing systems. Thanks are due to Ravi Govindaraju for valuable help with the numerical experiments and to the two anonymous reviewers for their valuable suggestions. The output of the GEOS-5 experiments can be obtained by sending a written request to the corresponding author. NR 21 TC 7 Z9 7 U1 6 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 16 PY 2014 VL 41 IS 9 BP 3282 EP 3288 DI 10.1002/2014GL059918 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AK1SP UT WOS:000338196700038 ER PT J AU Ren, YX Xie, GD Huang, H Bao, CJ Yan, Y Ahmed, N Lavery, MPJ Erkmen, BI Dolinar, S Tur, M Neifeld, MA Padgett, MJ Boyd, RW Shapiro, JH Willner, AE AF Ren, Yongxiong Xie, Guodong Huang, Hao Bao, Changjing Yan, Yan Ahmed, Nisar Lavery, Martin P. J. Erkmen, Baris I. Dolinar, Samuel Tur, Moshe Neifeld, Mark A. Padgett, Miles J. Boyd, Robert W. Shapiro, Jeffrey H. Willner, Alan E. TI Adaptive optics compensation of multiple orbital angular momentum beams propagating through emulated atmospheric turbulence SO OPTICS LETTERS LA English DT Article ID WAVE-FRONT SENSOR; SPACE; LIGHT; LINK; POLARIZATION AB We propose an adaptive optics compensation scheme to simultaneously compensate multiple orbital angular momentum (OAM) beams propagating through atmospheric turbulence. A Gaussian beam on one polarization is used to probe the turbulence-induced wavefront distortions and derive the correction pattern for compensating the OAM beams on the orthogonal polarization. By using this scheme, we experimentally demonstrate simultaneous compensation of multiple OAM beams, each carrying a 100 Gbit/s data channel through emulated atmospheric turbulence. The experimental results indicate that the correction pattern obtained from the Gaussian probe beam could be used to simultaneously compensate multiple turbulence-distorted OAM beams with different orders. It is found that the turbulence-induced crosstalk effects on neighboring modes are efficiently reduced by 12.5 dB, and the system power penalty is improved by 11 dB after compensation. (C) 2014 Optical Society of America C1 [Ren, Yongxiong; Xie, Guodong; Huang, Hao; Bao, Changjing; Yan, Yan; Ahmed, Nisar; Willner, Alan E.] Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA. [Lavery, Martin P. J.; Padgett, Miles J.] Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Erkmen, Baris I.; Dolinar, Samuel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tur, Moshe] Tel Aviv Univ, Sch Elect Engn, IL-69978 Tel Aviv, Israel. [Neifeld, Mark A.] Univ Arizona, Dept Elect & Comp Engn, Tucson, AZ 85721 USA. [Boyd, Robert W.] Univ Rochester, Dept Phys & Astron, Inst Opt, Rochester, NY 14627 USA. [Shapiro, Jeffrey H.] MIT, Elect Res Lab, Cambridge, MA 02139 USA. RP Ren, YX (reprint author), Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA. EM yongxior@usc.edu RI Padgett, Miles/B-7625-2008; Lavery, Martin/H-2265-2015 OI Padgett, Miles/0000-0001-6643-0618; FU DARPA under the InPho program FX We acknowledge Jerome Ballesta from Imagine Optic Inc. for helpful discussions. Our work is supported by DARPA under the InPho program. NR 21 TC 21 Z9 24 U1 3 U2 25 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 EI 1539-4794 J9 OPT LETT JI Opt. Lett. PD MAY 15 PY 2014 VL 39 IS 10 BP 2845 EP 2848 DI 10.1364/OL.39.002845 PG 4 WC Optics SC Optics GA AI6KI UT WOS:000336982500006 PM 24978218 ER PT J AU Jones, WV AF Jones, William Vernon TI Evolution of scientific ballooning and its impact on astrophysics research SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Ballooning; Antarctica; NASA balloons; Super-pressure balloons; LDB; ULDB ID COSMIC-RAYS; ENERGIES; ORIGIN AB As we celebrate the centennial year of the discovery of cosmic rays on a manned balloon, it seems appropriate to reflect on the evolution of ballooning and its scientific impact. Balloons have been used for scientific research since they were invented in France more than 200 years ago. Ballooning was revolutionized in 1950 with the introduction of the so-called natural shape balloon with integral load tapes. This basic design has been used with more or less continuously improved materials for scientific balloon flights for more than a half century, including long-duration balloon (LDB) flights around Antarctica for the past two decades. The U.S. National Aeronautics and Space Administration (NASA) is currently developing the next generation super-pressure balloon that would enable extended duration missions above 99.5% of the Earth's atmosphere at any latitude. The Astro2010 Decadal Survey report supports super-pressure balloon development and the giant step forward it offers with ultra-long-duration balloon (ULDB) flights at constant altitudes for about 100 days. Published by Elsevier Ltd. on behalf of COSPAR. C1 NASA Headquarters, Astrophys Div DH000, Washington, DC 20546 USA. RP Jones, WV (reprint author), NASA Headquarters, Astrophys Div DH000, Washington, DC 20546 USA. EM w.vernon.jones@nasa.gov NR 24 TC 3 Z9 3 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD MAY 15 PY 2014 VL 53 IS 10 BP 1405 EP 1414 DI 10.1016/j.asr.2013.12.028 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA AI6UY UT WOS:000337013700004 ER PT J AU Abe, K Fuke, H Haino, S Hams, T Hasegawa, M Horikoshi, A Itazaki, A Kim, KC Kumazawa, T Kusumoto, A Lee, MH Makida, Y Matsuda, S Matsukawa, Y Matsumoto, K Mitchell, JW Moiseev, AA Nishimura, J Nozaki, M Orito, R Ormes, JF Picot-Clemente, N Sakai, K Sasaki, M Seo, ES Shikaze, Y Shinoda, R Streitmatter, RE Suzuki, J Takasugi, Y Takeuchi, K Tanaka, K Thakur, N Yamagami, T Yamamoto, A Yoshida, T Yoshimura, K AF Abe, K. Fuke, H. Haino, S. Hams, T. Hasegawa, M. Horikoshi, A. Itazaki, A. Kim, K. C. Kumazawa, T. Kusumoto, A. Lee, M. H. Makida, Y. Matsuda, S. Matsukawa, Y. Matsumoto, K. Mitchell, J. W. Moiseev, A. A. Nishimura, J. Nozaki, M. Orito, R. Ormes, J. F. Picot-Clemente, N. Sakai, K. Sasaki, M. Seo, E. S. Shikaze, Y. Shinoda, R. Streitmatter, R. E. Suzuki, J. Takasugi, Y. Takeuchi, K. Tanaka, K. Thakur, N. Yamagami, T. Yamamoto, A. Yoshida, T. Yoshimura, K. TI Time variations of cosmic-ray helium isotopes with BESS-Polar I SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Cosmic-ray isotopes; Cosmic-ray flux time variations; Solar modulation; Solar activity ID INTENSITY AB The Balloon-borne Experiment with a Superconducting Spectrometer (BESS) is configured with a solenoidal superconducting magnet and a suite of precision particle detectors, including time-of-flight hodoscopes based on plastic scintillators, a silica-aerogel Cherenkov detector, and a high resolution tracking system with a central jet-type drift chamber. The charges of incident particles are determined from energy losses in the scintillators. Their magnetic rigidities (momentum/charge) are measured by reconstructing each particle trajectory in the magnetic field, and their velocities are obtained by using the time-of-flight system. Together, these measurements can accurately identify helium isotopes among the incoming cosmic-ray helium nuclei up to energies in the GeV per nucleon region. The BESS-Polar I instrument flew for 8.5 days over Antarctica from December 13th to December 21st, 2004. Its long-duration flight and large geometric acceptance allow the time variations of isotopic fluxes to be studied for the first time. The time variations of helium isotope fluxes are presented here for rigidities from 1.2 to 2.5 GV and results are compared to previously reported proton data and neutron monitor data. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Abe, K.; Itazaki, A.; Kusumoto, A.; Matsukawa, Y.; Orito, R.; Shikaze, Y.; Takasugi, Y.; Takeuchi, K.] Kobe Univ, Kobe, Hyogo 6578501, Japan. [Fuke, H.; Yoshida, T.] Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. [Haino, S.; Hasegawa, M.; Horikoshi, A.; Kumazawa, T.; Makida, Y.; Matsuda, S.; Matsumoto, K.; Nozaki, M.; Suzuki, J.; Tanaka, K.; Yamagami, T.; Yamamoto, A.; Yoshimura, K.] High Energy Accelerator Res Org, KEK, Tsukuba, Ibaraki 3050801, Japan. [Hams, T.; Mitchell, J. W.; Moiseev, A. A.; Sakai, K.; Sasaki, M.; Streitmatter, R. E.] NASA, Goddard Space Flight Ctr NASA GFSC, Greenbelt, MD 20771 USA. [Kim, K. C.; Lee, M. H.; Nishimura, J.; Picot-Clemente, N.; Seo, E. S.] Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. [Ormes, J. F.; Thakur, N.] Univ Denver, Denver, CO 80208 USA. [Shinoda, R.] Univ Tokyo, Bunkyo Ku, Tokyo 1130033, Japan. RP Picot-Clemente, N (reprint author), Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. EM picot@umd.edu OI Seo, Eun-Suk/0000-0001-8682-805X FU KAKEN-Hi [13001004, 18104006]; NASA in the US; NSF [ATM-0000315] FX The BESS-Polar experiment is a Japan-U.S. collaboration, supported by KAKEN-Hi (13001004 and 18104006) in Japan, and by NASA in the US. The authors thank NASA Headquarters, the NASA Balloon Program Office at Goddard Space Flight Center/Wallops Flight Facility, and the NASA Columbia Scientific Balloon Facility, as well as ISAS/JAXA and KEK for their support. Thanks to the US National Science Foundation (NSF) and Raytheon Polar Services Company for their professional support in the USA and in Antarctica. The authors thank the Bartol Research Institute neutron monitor program, supported by the NSF (Grant ATM-0000315), for providing their data. The authors thank the ACE SWEPAM, MAG, EPAM, and SIS instrument teams and the ACE Science Center for providing the ACE data.ss NR 13 TC 1 Z9 1 U1 0 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD MAY 15 PY 2014 VL 53 IS 10 BP 1426 EP 1431 DI 10.1016/j.asr.2013.09.028 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA AI6UY UT WOS:000337013700006 ER PT J AU Seo, ES Anderson, T Angelaszek, D Baek, SJ Baylon, J Buenerd, M Copley, M Coutu, S Derome, L Fields, B Gupta, M Han, JH Howley, I Huh, HG Hwang, YS Hyun, HJ Jeong, IS Kah, DH Kang, KH Kim, DY Kim, HJ Kim, KC Kim, MH Kwashnak, K Lee, J Lee, MH Link, JT Lutz, L Malinin, A Menchaca-Rocha, A Mitchell, JW Nutter, S Ofoha, O Park, H Park, IH Park, JM Patterson, P Smita, JR Wu, J Yoon, YS AF Seo, E. S. Anderson, T. Angelaszek, D. Baek, S. J. Baylon, J. Buenerd, M. Copley, M. Coutu, S. Derome, L. Fields, B. Gupta, M. Han, J. H. Howley, Ij Huh, H. G. Hwang, Y. S. Hyun, H. J. Jeong, I. S. Kah, D. H. Kang, K. H. Kim, D. Y. Kim, H. J. Kim, K. C. Kim, M. H. Kwashnak, K. Lee, J. Lee, M. H. Link, J. T. Lutz, L. Malinin, A. Menchaca-Rocha, A. Mitchell, J. W. Nutter, S. Ofoha, O. Park, H. Park, I. H. Park, J. M. Patterson, P. Smita, J. R. Wu, J. Yoon, Y. S. TI Cosmic Ray Energetics And Mass for the International Space Station (ISS-CREAM) SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Cosmic rays; Elemental spectra; CREAM; Direct measurements ID SUPERNOVA-REMNANTS; SPECTRA; ENERGIES AB The Cosmic Ray Energetics And Mass (CREAM) instrument is configured with a suite of particle detectors to measure TeV cosmic-ray elemental spectra from protons to iron nuclei over a wide energy range. The goal is to extend direct measurements of cosmic-ray composition to the highest energies practical, and thereby have enough overlap with ground based indirect measurements to answer questions on cosmic-ray origin, acceleration and propagation. The balloon-borne CREAM was flown successfully for about 161 days in six flights over Antarctica to measure elemental spectra of Z = 1-26 nuclei over the energy range 10(10) to >10(14) eV. Transforming the balloon instrument into ISS-CREAM involves identification and replacement of components that would be at risk in the International Space Station (ISS) environment, in addition to assessing safety and mission assurance concerns. The transformation process includes rigorous testing of components to reduce risks and increase survivability on the launch vehicle and operations on the ISS without negatively impacting the heritage of the successful CREAM design. The project status, including results from the ongoing analysis of existing data and, particularly, plans to increase the exposure factor by another order of magnitude utilizing the International Space Station are presented. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Seo, E. S.; Angelaszek, D.; Copley, M.; Fields, B.; Gupta, M.; Han, J. H.; Howley, Ij; Huh, H. G.; Kim, D. Y.; Kim, K. C.; Kim, M. H.; Kwashnak, K.; Lee, M. H.; Lutz, L.; Malinin, A.; Ofoha, O.; Patterson, P.; Smita, J. R.; Wu, J.; Yoon, Y. S.] Univ Maryland, Inst Phys Sci & Tech, College Pk, MD 20742 USA. [Seo, E. S.; Angelaszek, D.; Yoon, Y. S.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Anderson, T.; Coutu, S.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Baek, S. J.; Jeong, I. S.; Lee, J.; Park, I. H.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea. [Baylon, J.; Menchaca-Rocha, A.] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 04510, DF, Mexico. [Buenerd, M.; Derome, L.] UJF CNRS IN2P3 INP, Lab Phys Subatom & Cosmol, F-38026 Grenoble, France. [Hwang, Y. S.; Hyun, H. J.; Kah, D. H.; Kang, K. H.; Kim, H. J.; Park, H.; Park, J. M.] Kyungpook Natl Univ, Dept Phys, Taegu 702701, South Korea. [Link, J. T.; Mitchell, J. W.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Nutter, S.] No Kentucky Univ, Dept Phys & Geol, Highland Hts, KY 41099 USA. RP Seo, ES (reprint author), Univ Maryland, Inst Phys Sci & Tech, College Pk, MD 20742 USA. EM seo@umd.edu RI Yoon, Young Soo/O-8580-2014; OI Yoon, Young Soo/0000-0001-7023-699X; Seo, Eun-Suk/0000-0001-8682-805X FU NASA [NNX11AC52G, NNX08AC15G, NNX08AC16G]; RTOP funds; Creative Research Initiatives of MEST/NRF; National Research Foundation [NRF-2011-0016260, NRF-2011-0021196]; IN2P3/CNRS; CNES; DGAPA-UNAM; CONACYT FX The authors thank NASA GSFC WFF for project management and engineering support, and NASA JSC ISS Program Office for the launch support and the ISS accommodation. This work was supported in the U.S. by NASA grants NNX11AC52G, NNX08AC15G, NNX08AC16G and their predecessor grants, as well as by directed RTOP funds to NASA GSFC WFF. It is supported in Korea by the Creative Research Initiatives of MEST/NRF and by National Research Foundation Grants NRF-2011-0016260 and NRF-2011-0021196. It is supported in France by IN2P3/CNRS and CNES and in Mexico by DGAPA-UNAM and CONACYT. NR 27 TC 10 Z9 10 U1 1 U2 15 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD MAY 15 PY 2014 VL 53 IS 10 BP 1451 EP 1455 DI 10.1016/j.asr.2014.01.013 PG 5 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA AI6UY UT WOS:000337013700010 ER PT J AU Adams, JH Christl, MJ Csorna, SE Sarazin, F Wiencke, LR AF Adams, J. H., Jr. Christl, M. J. Csorna, S. E. Sarazin, F. Wiencke, L. R. CA JEM-EUSO Collaboration TI Calibration for extensive air showers observed during the JEM-EUSO mission SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Extragalactic cosmic-rays; Ultra-high energy cosmic rays; Extreme Universe Space Observatory; JEM-EUSO ID COSMIC-RAY; FLUORESCENCE RELEVANT; DEPENDENCE; DETECTOR AB The Extreme Universe Space Observatory is a mission to investigate the highest energy cosmic rays by recording the extensive air showers they create in the Earth's atmosphere. This will be done by observing these showers from low Earth orbit. These observations will be used to measure the flux, energies and arrival directions of these cosmic rays. This paper describes how the accuracy of these measurements will be tested and improved during the mission using the Global Light System (consisting of calibrated xenon flash lamps and lasers) located deep in the Earth's atmosphere. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Adams, J. H., Jr.] Univ Alabama, Huntsville, AL 35805 USA. [Christl, M. J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Csorna, S. E.] Vanderbilt Univ, Nashville, TN 37235 USA. [Sarazin, F.; Wiencke, L. R.] Colorado Sch Mines, Golden, CO 80401 USA. RP Adams, JH (reprint author), Univ Alabama, Huntsville, AL 35805 USA. EM jha0003@uah.edu; mark.christl@nasa.gov; steven.e.csorna@vanderbilt.edu; lwiencke@mines.edu NR 30 TC 2 Z9 2 U1 1 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD MAY 15 PY 2014 VL 53 IS 10 BP 1506 EP 1514 DI 10.1016/j.asr.2013.10.009 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA AI6UY UT WOS:000337013700017 ER PT J AU Li, WQ Beard, BL Li, CX Johnson, CM AF Li, Weigiang Beard, Brian L. Li, Chengxiang Johnson, Clark M. TI Magnesium isotope fractionation between brucite [Mg(OH)(2)] and Mg aqueous species: Implications for silicate weathering and biogeochemical processes SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Mg isotope; brucite; weathering; Mg(OH)(2); fractionation; EDTA ID CRYSTAL STRUCTURE; PLANT-GROWTH; DEGREES-C; PRECIPITATION; EQUILIBRIUM; DISSOLUTION; KINETICS; EXCHANGE; OXYGEN; SYSTEMATICS AB Brucite, with its octahedral structure, has a lattice configuration that is similar to the Mg-bearing octahedral layers in phyllosilicates. Understanding stable Mg isotope fractionation between brucite and aqueous solution therefore bears on interpretation of Mg isotope data in natural weathering systems. In this study, we experimentally determined Mg isotope fractionation between brucite and two Mg aqueous species, the free Mg aquo ion ([Mg(OH2)(6)](2+)) and EDTA-bonded Mg (Mg-EDTA(2-)). Results from recrystallization and brucite synthesis experiments suggest mild preferential partitioning of light Mg isotopes into brucite compared to Mg aquo ions at low temperatures, where measured Delta Mg-26(brucite-Mg2+) fractionation increased from ca. -0.3 parts per thousand at 7 degrees C, to ca. -0.2 parts per thousand at 22 degrees C, to ca. 0 parts per thousand at 40 degrees C. MgO hydrolysis experiments in EDTA-bearing solutions suggest that the Delta Mg-26(brucite-Mg-EDTA) fractionation is >= + 2.0 parts per thousand at 22 degrees C, indicating that light Mg isotopes strongly partition into Mg-EDTA complex relative to brucite, as well as relative to Mg aquo ions. Magnesium atoms in brucite, Mg aquo ions, and Mg-EDTA complexes are all octahedrally coordinated, and the measured Mg isotope fractionations correlate with average bond lengths for Mg. Aqueous Mg ions have the shortest bond length among the three phases, and enrich heavy Mg isotopes relative to brucite and Mg-EDTA. In contrast, Mg-EDTA has the longest average bond length for Mg, and enriches light Mg isotopes relative to Mg aquo ions and brucite; the relatively long Mg-EDTA bond suggests that organically bound Mg may commonly have low Mg-26/Mg-24 ratios, which may explain proposed "vital" effects for stable Mg isotopes. Such relations between bond length and Mg isotope fractionation could be extended to other phyllosilicates such as serpentine- and clay-group minerals where Mg is also octahedrally coordinated. (C) 2014 Elsevier B.V. All rights reserved. C1 [Li, Weigiang; Beard, Brian L.; Johnson, Clark M.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Li, Weigiang; Beard, Brian L.; Johnson, Clark M.] NASA, Astrobiol Inst, Washington, DC USA. [Li, Chengxiang] Nanjing Univ, Sch Earth Sci & Engn, State Key Lab Mineral Deposits Res, Nanjing 210093, Peoples R China. RP Li, WQ (reprint author), Univ Wisconsin, Dept Geosci, 1215 W Dayton St, Madison, WI 53706 USA. EM liweig@gmail.com RI Li, Weiqiang/D-2975-2011 OI Li, Weiqiang/0000-0003-2648-7630 FU NASA Astrobiology Institute; Department of Energy FX Fangfu Zhang assisted in BET analysis, Zhizhang Shen assisted in XRD analysis and mineral lattice data interpretation. Jim Kern and Reinhard Kozdon assisted in gold coating of brucite samples. Prof. Huifang Xu provided a natural magnesite sample and access to water bath. This paper benefited from constructive comments from J. Wimpenny, P. Pogge von Strandmann, and two anonymous reviewers, as well as editorial comments by G. Henderson. This study was supported by grants from the NASA Astrobiology Institute and the Department of Energy. NR 79 TC 16 Z9 17 U1 3 U2 43 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD MAY 15 PY 2014 VL 394 BP 82 EP 93 DI 10.1016/j.epsl.2014.03.022 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AG7QQ UT WOS:000335613300009 ER PT J AU Malavergne, V Cordier, P Righter, K Brunet, F Zanda, B Addad, A Smith, T Bureau, H Surble, S Raepsaet, C Charon, E Hewins, RH AF Malavergne, Valerie Cordier, Patrick Righter, Kevin Brunet, Fabrice Zanda, Brigitte Addad, Ahmed Smith, Thomas Bureau, Helene Surble, Suzy Raepsaet, Caroline Charon, Emeline Hewins, Roger H. TI How Mercury can be the most reduced terrestrial planet and still store iron in its mantle SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Mercury; planetary differentiation; primitive mantle; sulfides; enstatite chondrites ID SILICATE MELTS; CORE FORMATION; MESSENGER; SURFACE; SULFUR; SPECTROMETRY; EVOLUTION; PRESSURE; ORIGIN; ALLOYS AB Mercury is notorious as the most reduced planet with the highest metal/silicate ratio, yet paradoxically data from the MESSENGER spacecraft show that its iron-poor crust is high in sulfur (up to similar to 6 wt%, similar to 80x Earth crust abundance) present mainly as Ca-rich sulfides on its surface. These particularities are simply impossible on the other terrestrial planets. In order to understand the role played by sulfur during the formation of Mercury, we investigated the phase relationships in Mercurian analogs of enstatite chondrite-like composition experimentally under conditions relevant to differentiation of Mercury (similar to 1 GPa and 1300-2000 degrees C). Our results show that Mg-rich and Ca-rich sulfides, which both contain Fe, crystallize successively from reduced silicate melts upon cooling below 1550 degrees C. As the iron concentration in the reduced silicates stays very low (<< 1 wt%), these sulfides represent new host phases for both iron and sulfur in the run products. Extrapolated to Mercury, these results show that Mg-rich sulfide crystallization provides the first viable and fundamental means for retaining iron as well as sulfur in the mantle during differentiation, while sulfides richer in Ca would crystallize at shallower levels. The distribution of iron in the differentiating mantle of Mercury was mainly determined by its partitioning between metal (or troilite) and Mg-Fe-Ca-rich sulfides rather than by its partitioning between metal (or troilite) and silicates. Moreover, the primitive mantle might also be boosted in Fe by a reaction at the core mantle boundary (CMB) between Mg-rich sulfides of the mantle and FeS-rich outer core materials to produce (Fe, Mg)S. The stability of Mg-Fe-Ca-rich sulfides over a large range of depths up to the surface of Mercury would be consistent with sulfur, calcium and iron abundances measured by MESSENGER. (C) 2014 Elsevier B.V. All rights reserved. C1 [Malavergne, Valerie] Univ Paris Est Marne La Vallee, Lab Geomat & Environm, F-77454 Champs Sur Marne, France. [Malavergne, Valerie; Charon, Emeline] Ecole Normale Super, Geol Lab, F-75005 Paris, France. [Cordier, Patrick; Addad, Ahmed] Univ Lille 1, UMR CNRS 8207, Unite Mat & Transformat, F-59655 Villeneuve Dascq, France. [Righter, Kevin] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Brunet, Fabrice] Univ Grenoble 1, ISTerre CNRS, F-38041 Grenoble 9, France. [Zanda, Brigitte; Hewins, Roger H.] Univ Paris 06, Univ Sorbonne, IMIPMC, UMR CNRS 7590,IRD UMR 206,Museum Natl Hist Nat, F-75005 Paris, France. [Zanda, Brigitte; Hewins, Roger H.] Rutgers State Univ, Dept Earth & Planetary Sci, Piscataway, NJ 08854 USA. [Smith, Thomas; Surble, Suzy; Raepsaet, Caroline] CEA Saclay, CEA CNRS SIS2M, UMR 3299, F-91191 Gif Sur Yvette, France. [Bureau, Helene] Univ Paris 06, Inst Mineral & Phys Milieux Condenses, F-75005 Paris, France. RP Malavergne, V (reprint author), Univ Paris Est Marne La Vallee, Lab Geomat & Environm, F-77454 Champs Sur Marne, France. EM Valerie.Malavergne@u-pem.fr RI Cordier, Patrick/D-2357-2012; Surble, Suzy/B-5652-2014; Zanda, Brigitte/D-6787-2015; OI Cordier, Patrick/0000-0002-1883-2994; Zanda, Brigitte/0000-0002-4210-7151; surble, suzy/0000-0001-6228-5919 FU Programme National de Planetologie of the Institut National des Sciences de l'Univers (INSU); Lunar and Planetary Institute; NASA Johnson Space Center (Houston, TX, USA); Conseil Regional du Nord-Pas de Calais; European Regional Development Fund (ERDF); INSU, CNRS FX The Programme National de Planetologie of the Institut National des Sciences de l'Univers (INSU), the Lunar and Planetary Institute and the NASA Johnson Space Center (Houston, TX, USA) funded this work. The TEM national facility in Lille (France) is supported by the Conseil Regional du Nord-Pas de Calais, the European Regional Development Fund (ERDF), and INSU, CNRS. The authors wish to thank the nuclear microprobe committee for accepting the project. We are also grateful to Didier Guillier, Yvan Kilisky and Francois Saillant for the accelerator operation, Hicham Khodja for his precious advice. We thank Damien Deldicque, Stephan Borensztajn and Imene Esteve for their helpful assistance with SEM. Thank you to Matthieu Agranier-Malavergne for his precious help with Fig. 5. We also thank Fabrice Gaillard and an anonymous reviewer for insightful and relevant reviews of this manuscript. NR 50 TC 5 Z9 5 U1 2 U2 39 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD MAY 15 PY 2014 VL 394 BP 186 EP 197 DI 10.1016/j.eps1.2014.03.028 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AG7QQ UT WOS:000335613300019 ER PT J AU Greiner, E Kumar, K Sumit, M Giuffre, A Zhao, WL Pedersen, J Sahai, N AF Greiner, Edward Kumar, Kartik Sumit, Madhuresh Giuffre, Anthony Zhao, Weilong Pedersen, Joel Sahai, Nita TI Adsorption of L-glutamic acid and L-aspartic acid to gamma-Al2O3 SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID AMINO-ACIDS; SURFACE COMPLEXATION; AQUEOUS-SOLUTION; CARBOXYLATE-BINDING; RUTILE ALPHA-TIO2; MINERAL SURFACES; INFRARED-SPECTRA; OXIDE SURFACES; METAL-OXIDES; ATR-FTIR AB The interactions of amino acids with mineral surfaces have potential relevance for processes ranging from pre-biotic chemistry to biomineralization to protein adsorption on biomedical implants in vivo. Here, we report the results of experiments investigating the adsorption of L-glutamic (Glu) and L-aspartic (Asp) acids to gamma-Al2O3. We examined the extent of Glu and Asp coverage as a function of pH and solution concentration (pH edges and isotherms) in solution-depletion experiments and used in situ Attenuated Total Refkectance Fourier Transform Infrared (ATR-FTIR) spectroscopy to estimate the molecular conformations of the adsorbed molecules. Glu and Asp exhibited similar adsorption behavior on gamma-Al2O3 with respect to pH and solution concentration. In general, adsorption decreased as pH increased. At low and high amino acid concentrations, the isotherms exhibited two apparent saturation coverages, which could be interpreted as 1:4 or 1:2 ratios of adsorbed molecule/surface Al sites. Tetradentate tetranuclear and bidentate binuclear species were the dominant conformations inferred independently from FTIR spectra. In these conformations, both carboxylate groups are involved in bonding to either four or to two Al surface atoms, through direct covalent bonds or via H-bonds. An outer sphere species, in which one carboxylate group interacts with a surface Al atom, could not be ruled out based on the FTIR spectra. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Greiner, Edward; Giuffre, Anthony] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Greiner, Edward] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA. [Kumar, Kartik; Pedersen, Joel] Univ Wisconsin, Mol & Environm Toxicol Program, Madison, WI 53706 USA. [Sumit, Madhuresh] Univ Wisconsin, Khorana Program, Madison, WI 53706 USA. [Sumit, Madhuresh] Univ Michigan, Program Biomed Sci, Ann Arbor, MI 48109 USA. [Giuffre, Anthony] VirginiaTech, Dept Geol Sci, Blacksburg, VA 24060 USA. [Pedersen, Joel] Univ Wisconsin, Dept Soil Sci, Madison, WI 53706 USA. [Zhao, Weilong; Sahai, Nita] Univ Akron, Dept Polymer Sci, Akron, OH 44325 USA. [Sahai, Nita] Univ Akron, NASA Astrobiol Inst, Akron, OH 44325 USA. RP Sahai, N (reprint author), Univ Akron, Dept Polymer Sci, 170 Univ Ave, Akron, OH 44325 USA. EM sahai@uakron.edu FU NSF EAR CAREER grant [EAR 0346689]; NASA Astrobiology Institute Director's Discretionary Funds (NAI DDF) grant; University of Akron; Simons Collaboration on the Origins of Life Grant from the Simons Foundation, NY; Department of Geosciences, University of Wisconsin, Madison FX The authors are grateful for the assistance provided by Dr. Jie Xu in characterizing the crystalline gamma-Al2O3; C. M. Jonsson with the amino acid analysis protocol. We appreciate helpful discussions with Drs. H. James Cleaves, Jason Dworkin, Jie Xu, Nianli Zhang, Yang Yang, Zhijun Xu and Tim Oleson; Profs. Eric Roden, Dimitri Sverjensky and Huifang Xu; Ms. Chunxiao Zhu and Mr. C. L. Jonsson. Financial support was provided to N. Sahai by NSF EAR CAREER grant EAR 0346689, NASA Astrobiology Institute Director's Discretionary Funds (NAI DDF) grant, "start-up" funds from University of Akron, and the Simons Collaboration on the Origins of Life Grant from the Simons Foundation, NY; and a Week's Graduate Fellowship to E. Greiner from the Department of Geosciences, University of Wisconsin, Madison. NR 81 TC 10 Z9 10 U1 4 U2 51 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY 15 PY 2014 VL 133 BP 142 EP 155 DI 10.1016/j.gca.2014.01.004 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AF6OE UT WOS:000334833600008 ER PT J AU Couturier-Tamburelli, I Gudipati, MS Lignell, A Jacovi, R Pietri, N AF Couturier-Tamburelli, Isabelle Gudipati, Murthy S. Lignell, Antti Jacovi, Ronen Pietri, Nathalie TI Spectroscopic studies of non-volatile residue formed by photochemistry of solid C4N2: A model of condensed aerosol formation on Titan SO ICARUS LA English DT Article DE Titan; Astrobiology; Ices, IR Spectroscopy; Photochemistry; Prebiotic environments ID POLYCYCLIC AROMATIC-HYDROCARBONS; NC-CC-CN; UPPER-ATMOSPHERE; OPTICAL-CONSTANTS; ORGANIC-CHEMISTRY; AMINO-ACIDS; MATRIX-ISOLATION; RAMAN-SPECTRA; CLIMATE MODEL; THOLINS AB Following our recent communication (Gudipati, M.S. et al. [2013]. Nat. Commun. 4, 1648. http://dx.doi.org/10.1038/ncomms2649) on the discovery of condensed-phase non-volatile polymeric material with similar spectral features as tholins, we present here a comprehensive spectroscopic study of photochemical formation of polymeric material from condensed dicyanoacetylene (C4N2) ice films. C4N2 is chosen as starting material for the laboratory simulations because of the detection of this and similar molecules (nitriles and cyanoacetylenes) in Titan's atmosphere. UV-Vis and infrared spectra obtained during long-wavelength (>300 nm) photon irradiation and subsequent warming of the ice films are used to analyze changes in C4N2 ice, evolution of tholins, and derive photopolymerization mechanisms. Our data analysis revealed that many processes occur during the photolysis of condensed Titan's aerosol analogs, including isomerization and polymerization leading to the formation of long-chain as well as aromatic cyclic polymer molecules. In the light of tremendous new data from the Cassini mission on the seasonal variations in Titan's atmosphere, our laboratory study and its results provide fresh insight into the formation and evolution of aerosols and haze in Titan's atmosphere. (c) 2014 Elsevier Inc. All rights reserved. C1 [Couturier-Tamburelli, Isabelle; Pietri, Nathalie] Aix Marseille Univ, CNRS, PIIM, UMR 7345, F-13013 Marseille, France. [Gudipati, Murthy S.; Lignell, Antti; Jacovi, Ronen] CALTECH, Jet Prop Lab, Div Sci, Ice Spect Lab, Pasadena, CA 91109 USA. RP Couturier-Tamburelli, I (reprint author), Aix Marseille Univ, CNRS, PIIM, UMR 7345, F-13013 Marseille, France. EM isabelle.couturier@univ-amu.fr; gudipati@jpl.nasa.gov RI Gudipati, Murthy/F-7575-2011; Lignell, Antti/C-2146-2009 OI Lignell, Antti/0000-0001-7664-5583 FU French National Program Environnements Planetaires et Origines de la Vie (EPOV); NASA Astrobiology Institute team "Titan as a Prebiotic Chemical System"; Jet Propulsion Laboratory Director's Research and Development Fund; JPL Research and Technology Development funding for the infrastructure of the Ice Spectroscopy Laboratory (ISL); Titan Organic Aerosol Spectroscopy and Chemistry (TOAST) Laboratory at JPL; National Aeronautics and Space Administration FX This work has been funded by the French National Program Environnements Planetaires et Origines de la Vie (EPOV). The JPL part of the work is partly supported by several of the following funding sources: NASA Astrobiology Institute team "Titan as a Prebiotic Chemical System", the Jet Propulsion Laboratory Director's Research and Development Fund, and the JPL Research and Technology Development funding for the infrastructure of the Ice Spectroscopy Laboratory (ISL) and Titan Organic Aerosol Spectroscopy and Chemistry (TOAST) Laboratory at JPL. Research carried out at the Jet Propulsion Laboratory, California Institute of Technology was under a contract with the National Aeronautics and Space Administration. We thank Dr. Briana Henderson for her helpful comments in improving the quality of the manuscript. NR 81 TC 6 Z9 6 U1 7 U2 38 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAY 15 PY 2014 VL 234 BP 81 EP 90 DI 10.1016/j.icarus.2014.02.016 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF2RU UT WOS:000334560500007 ER PT J AU Paranicas, C Roussos, E Decker, RB Johnson, RE Hendrix, AR Schenk, P Cassidy, TA Dalton, JB Howett, CJA Kollmann, P Patterson, W Hand, KP Nordheim, TA Krupp, N Mitchell, DG AF Paranicas, C. Roussos, E. Decker, R. B. Johnson, R. E. Hendrix, A. R. Schenk, P. Cassidy, T. A. Dalton, J. B., III Howett, C. J. A. Kollmann, P. Patterson, W. Hand, K. P. Nordheim, T. A. Krupp, N. Mitchell, D. G. TI The lens feature on the inner saturnian satellites SO ICARUS LA English DT Article DE Saturn, satellites; Saturn, magnetosphere; Satellites, general ID ION IRRADIATION; WATER ICE; MAGNETOSPHERE; EUROPA; PROTONS; SURFACE; TETHYS; MOTION; ORIGIN; MIMAS AB We have modeled an electron precipitation pattern expected on Mimas, Tethys, and Dione, using two different approaches. In the first approach, we adapt a previously developed model to compute an integrated energy flux into the surfaces of Mimas, Tethys, and Dione. This is a guiding-center, bounceaveraged model. In the second approach, we track individual particles in an electromagnetic field for an inert or slightly magnetized satellite. This second approach allows us to include the effects of electron pitch angle and gyrophase on the weathering pattern. Both methods converge on an enhanced dose pattern on each satellite's leading hemisphere that is lens-shaped. We also present mission-averaged electron energy spectra obtained near these satellites by Cassini's Magnetosphere Imaging Instrument (MIMI). These data are interpreted using our current understanding of both the environment and the instrument's response. Fits to the data are integrated to find an energy flux into each satellite's surface, as a function of longitude and latitude. Using positions on the moon accessible to energetic electrons from the modeling and the integrated energy flux based on data, we find lens patterns that fall off with increasing moon latitude. The predicted patterns are qualitatively consistent with some but not all of the optical observations made of these hemispheres. (c) 2014 Elsevier Inc. All rights reserved. C1 [Paranicas, C.; Decker, R. B.; Kollmann, P.; Patterson, W.; Mitchell, D. G.] APL, Laurel, MD 20723 USA. [Roussos, E.; Krupp, N.] Max Planck Inst Solar Syst Res, Gottingen, Germany. [Johnson, R. E.] Univ Virginia, Charlottesville, VA 22903 USA. [Schenk, P.] LPI, Houston, TX 77058 USA. [Hendrix, A. R.] PSI, Tucson, AZ 85737 USA. [Cassidy, T. A.] LASP, Boulder, CO 80303 USA. [Dalton, J. B., III; Hand, K. P.] JPL, Pasadena, CA 91109 USA. [Howett, C. J. A.] SWRI, Boulder, CO 80302 USA. [Nordheim, T. A.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Paranicas, C (reprint author), APL, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM chris.paranicas@jhuapl.edu; Roussos@mps.mpg.de; Rob.decker@jhuapl.edu; rej@virginia.edu; ahendrix@psi.edu; schenk@lpi.usra.edu; Timothy.Cassidy@lasp.colorado.edu; James.B.Dalton@jpl.nasa.gov; howett@boulder.swri.edu; peter.kollmann@jhuapl.edu; wes.patterson@jhuapl.edu; Kevin.P.Hand@jpl.nasa.gov; Tan2@mssl.ucl.ac.uk; krupp@mps.mpg.de; Donald.g.mitchell@jhuapl.edu RI Paranicas, Christopher/B-1470-2016; Kollmann, Peter/C-2583-2016; OI Paranicas, Christopher/0000-0002-4391-8255; Kollmann, Peter/0000-0002-4274-9760; Roussos, Elias/0000-0002-5699-0678 FU Cassini grants; NASA; Johns Hopkins University FX The APL authors appreciate Cassini grants and contracts between NASA and the Johns Hopkins University. NR 33 TC 8 Z9 8 U1 1 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAY 15 PY 2014 VL 234 BP 155 EP 161 DI 10.1016/j.icarus.2014.02.026 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF2RU UT WOS:000334560500012 ER PT J AU Marley, MS AF Marley, Mark S. TI Saturn ring seismology: Looking beyond first order resonances SO ICARUS LA English DT Article DE Saturn, Rings; Saturn, interior; Saturn; Resonances, rings ID NONRADIAL OSCILLATIONS; GIANT PLANETS AB Some wave features found in the C-ring of Saturn appear to be excited by resonances with normal mode oscillations of the planet. The waves are found at locations in the rings where the ratio of orbital to oscillation frequencies is given by m : m + 1 where m is a small integer. I suggest here that it is plausible that ring waves may also be launched at second order resonances where the frequency ratio would be m : m + 2. Indeed otherwise unassociated wave features are found at such locations in the C-ring. If confirmed the association of planetary modes with additional C-ring wave features would measure additional oscillation frequencies of Saturn and improve the utility of the waves for constraining the internal structure of the planet. Second-order resonances in general do not lie near first order ring resonance locations and thus are not the explanation for the apparent frequency splitting of modes. Published by Elsevier Inc. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Marley, MS (reprint author), NASA, Ames Res Ctr, Mail Stop 245-3,POB 1, Moffett Field, CA 94035 USA. RI Marley, Mark/I-4704-2013; OI Marley, Mark/0000-0002-5251-2943 FU NASA OPR Program FX I thank Jeff Cuzzi and Jack Lissauer for helpful discussions and comments on this manuscript. I also gratefully acknowledge the reviewers for thoughtful and helpful comments. This work was supported by the NASA OPR Program. NR 15 TC 3 Z9 3 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAY 15 PY 2014 VL 234 BP 194 EP 199 DI 10.1016/j.icarus.2014.02.002 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF2RU UT WOS:000334560500015 ER PT J AU Sjogreen, B Yee, HC Vinokur, M AF Sjoegreen, Bjoern Yee, H. C. Vinokur, Marcel TI On high order finite-difference metric discretizations satisfying GCL on moving and deforming grids SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE GCL; High order metric; Moving and deforming grids; High order numerical methods ID GEOMETRIC CONSERVATION LAW; SCHEMES AB In this note we generalize our previous treatment of the discretizations of geometric conservation laws on steady grids (Vinokur and Yee, 2000) to general time dependent grids. The commutative property of mixed difference operators is generalized to apply to time metrics and Jacobians. Our treatment uses half the number of terms as those used in a recent paper by Abe et al. (2012). We also derive the proper temporal discretizations of both Runge-Kutta and linear multistep methods to satisfy the commutativity property for higher than first order. (C) 2014 Published by Elsevier Inc. C1 [Sjoegreen, Bjoern] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. [Yee, H. C.; Vinokur, Marcel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Sjogreen, B (reprint author), Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. EM Helen.M.Yee@nasa.gov FU US Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344] FX Work by the first author performed under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. This is contribution LLNL-TR-637397. NR 10 TC 8 Z9 8 U1 1 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 EI 1090-2716 J9 J COMPUT PHYS JI J. Comput. Phys. PD MAY 15 PY 2014 VL 265 BP 211 EP 220 DI 10.1016/j.jcp.2014.01.045 PG 10 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA AC3KH UT WOS:000332416300013 ER PT J AU Polk, JE Mikellides, IG Capece, AM Katz, I AF Polk, James E. Mikellides, Ioannis G. Capece, Angela M. Katz, Ira TI The effect of cathode geometry on barium transport in hollow cathode plasmas SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID IMPREGNATED-CATHODE; OPERATION; MECHANISM; LIFE AB The effect of barium transport on the operation of dispenser hollow cathodes was investigated in numerical modeling of a cathode with two different orifice sizes. Despite large differences in cathode emitter temperature, emitted electron current density, internal xenon neutral and plasma densities, and size of the plasma-surface interaction region, the barium transport in the two geometries is qualitatively very similar. Barium is produced in the insert and flows to the surface through the porous structure. A buildup of neutral Ba pressure in the plasma over the emitter surface can suppress the reactions supplying the Ba, restricting the net production rate. Neutral Ba flows into the dense Xe plasma and has a high probability of being ionized at the periphery of this zone. The steady state neutral Ba density distribution is determined by a balance between pressure gradient forces and the drag force associated with collisions between neutral Ba and neutral Xe atoms. A small fraction of the neutral Ba is lost upstream. The majority of the neutral Ba is ionized in the high temperature Xe plasma and is pushed back to the emitter surface by the electric field. The steady state Ba+ ion density distribution results from a balance between electrostatic and pressure forces, neutral Xe drag and Xe+ ion drag with the dominant forces dependent on location in the discharge. These results indicate that hollow cathodes are very effective at recycling Ba within the discharge and therefore maintain a high coverage of Ba on the emitter surface, which reduces the work function and sustains high electron emission current densities at moderate temperatures. Barium recycling is more effective in the cathode with the smaller orifice because the Ba is ionized in the dense Xe plasma concentrated just upstream of the orifice and pushed back into the hollow cathode. Despite a lower emitter temperature, the large orifice cathode has a higher Ba loss rate through the orifice because the Xe plasma density peaks further upstream. (C) 2014 AIP Publishing LLC. C1 [Polk, James E.; Mikellides, Ioannis G.; Katz, Ira] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Capece, Angela M.] CALTECH, Pasadena, CA 91125 USA. RP Polk, JE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM james.e.polk@jpl.nasa.gov NR 15 TC 1 Z9 1 U1 4 U2 12 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD MAY 14 PY 2014 VL 115 IS 18 AR 183301 DI 10.1063/1.4873168 PG 11 WC Physics, Applied SC Physics GA AI5OT UT WOS:000336919400003 ER PT J AU Meador, MAB McMillon, E Sandberg, A Barrios, E Wilmoth, NG Mueller, CH Miranda, FA AF Meador, Mary Ann B. McMillon, Emily Sandberg, Anna Barrios, Elizabeth Wilmoth, Nathan G. Mueller, Carl H. Miranda, Felix A. TI Dielectric and Other Properties of Polyimide Aerogels Containing Fluorinated Blocks SO ACS APPLIED MATERIALS & INTERFACES LA English DT Article DE aerogels; polyimides; low dielectric; antennas; mesoporous ID CONSTANT POLYIMIDES; POROUS POLYIMIDE; FILMS AB The dielectric and other properties of a series of low-density polyimide block copolymer aerogels have been characterized. Two different anhydride-capped polyimide oligomers were synthesized: one from 2,2-bis(3,4-dicarboxyphenyl)hexafluoropropane dianhydride (6FDA) and 4,4'-caidianiline (ODA) and the other from biphenyl-3,3',4,4'-tetracarboxylic dianhydride and ODA: The oligorners were combined with 1,3,5-triaminophenoxybenzene to form a block copolymer networked structure that gelled in under 1 h. The polyimide gels were supercritically dried to give aerogels with relative dielectric constants as low as 1.08. Increasing the amount of 6FDA blocks by up to 50% of the total dianhydride decreased the density of the aerogels, presumably by increasing the free volume and also by decreasing the amount of shrinkage seen upon processing, resulting in a concomitant decrease in the dielectric properties. In this study, we have also altered the density independent of fluorine substitution by changing the polymer concentration in the gelation reactions and showed that the change in dielectric due to density is the same with and without fluorine substitution. The aerogels with the lowest dielectric properties and lowest densities still had compressive moduli of 4-8 MPa (40 times higher than silica aerogels at the same density), making them suitable as low dielectric substrates for lightweight antennas for aeronautic and space applications. C1 [Meador, Mary Ann B.; Miranda, Felix A.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Wilmoth, Nathan G.] Vantage Partners LLC, Brighton, MA USA. RP Meador, MAB (reprint author), NASA Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM maryann.meador@nasa.gov OI Meador, Mary Ann/0000-0003-2513-7372 FU NASA Aeronautics Mission Directorate Seedling Fund FX We thank the NASA Aeronautics Mission Directorate Seedling Fund for support of this work. We also thank Dan Scheiman and Linda McCorkle of the Ohio Aerospace Institute for analysis of the aerogels. NR 19 TC 35 Z9 39 U1 13 U2 79 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1944-8244 J9 ACS APPL MATER INTER JI ACS Appl. Mater. Interfaces PD MAY 14 PY 2014 VL 6 IS 9 BP 6062 EP 6068 DI 10.1021/am405106h PG 7 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA AH4CV UT WOS:000336075300008 PM 24483208 ER PT J AU Miller, SG Williams, TS Baker, JS Sola, F Lebion-Colon, M McCorkle, LS Wilmoth, NG Gaier, J Chen, M Meador, MA AF Miller, Sandi G. Williams, Tiffany S. Baker, James S. Sola, Francisco Lebion-Colon, Marisabel McCorkle, Linda S. Wilmoth, Nathan G. Gaier, James Chen, Michelle Meador, Michael A. TI Increased Tensile Strength of Carbon Nanotube Yarns and Sheets through Chemical Modification and Electron Beam Irradiation SO ACS APPLIED MATERIALS & INTERFACES LA English DT Article DE carbon nanotube; tensile strength; functionalization; electron-beam irradiation; cross-link; focused ion beam ID NANOFIBERS; BUNDLES AB The inherent strength of individual carbon nanotubes (CNTs) offers considerable opportunity for the development of advanced, lightweight composite structures. Recent work in the fabrication and application of CNT forms such as yarns and sheets has addressed early nanocomposite limitations with respect to nanotube dispersion and loading and has pushed the technology toward structural composite applications. However, the high tensile strength of an individual CNT has not directly translated into that of sheets and yarns, where the bulk material strength is limited by intertube electrostatic attractions and slippage. The focus of this work was to assess postprocessing of CNT sheets and yarns to improve the macro-scale strength of these material forms. Both small-molecule functionalization and electron-beam irradiation were evaluated as means to enhance the tensile strength and Young's modulus of the bulk CNT materials. Mechanical testing revealed a 57% increase in tensile strength of CNT sheets upon functionalization compared with unfunctionalized sheets, while an additional 48% increase in tensile strength was observed when functionalized sheets were irradiated. Similarly, small-molecule functionalization increased tensile strength of yarn by up to 25%, whereas irradiation of the functionalized yarns pushed the tensile strength to 88% beyond that of the baseline yarn. C1 [Miller, Sandi G.; Williams, Tiffany S.; Sola, Francisco; Lebion-Colon, Marisabel; McCorkle, Linda S.; Gaier, James; Chen, Michelle; Meador, Michael A.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Baker, James S.] Oak Ridge Associated Univ, Cleveland, OH 44135 USA. [Wilmoth, Nathan G.] Vantage Partners LLC, Cleveland, OH 44135 USA. [McCorkle, Linda S.] Ohio Aerosp Inst, Cleveland, OH 44135 USA. RP Miller, SG (reprint author), NASA Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM sandi.g.miller@nasa.gov FU NASA Game Changing Development Program/Nanotechnology Project; NASA Postdoctoral Program at the Glenn Research Center FX This work was funded through the NASA Game Changing Development Program/Nanotechnology Project. J.S.B. was supported under the NASA Postdoctoral Program at the Glenn Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. The authors thank Dr. Jeffrey Eldridge for his assistance with Raman spectroscopy and Ms. Dorothy Lukco for her assitance with XPS. NR 18 TC 13 Z9 13 U1 3 U2 36 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1944-8244 J9 ACS APPL MATER INTER JI ACS Appl. Mater. Interfaces PD MAY 14 PY 2014 VL 6 IS 9 BP 6120 EP 6126 DI 10.1021/am4058277 PG 7 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA AH4CV UT WOS:000336075300013 PM 24720450 ER PT J AU Hees, A Folkner, WM Jacobson, RA Park, RS AF Hees, A. Folkner, W. M. Jacobson, R. A. Park, R. S. TI Constraints on modified Newtonian dynamics theories from radio tracking data of the Cassini spacecraft SO PHYSICAL REVIEW D LA English DT Article ID DARK-MATTER; SOLAR-SYSTEM; SATURNIAN SYSTEM; GRAVITY-FIELD; MOND; INERTIA; MOTION; TITAN AB The modified Newtonian dynamics (MOND) is an attempt to modify the gravitation theory to solve the dark matter problem. This phenomenology is very successful at the galactic level. The main effect produced by MOND in the Solar System is called the external field effect parametrized by the parameter Q(2). We have used nine years of Cassini range and Doppler measurements to constrain Q(2). Our estimate of this parameter based on Cassini data is given by Q(2) = (3 +/- 3) x 10(-27) s(-2), which shows no deviation from General Relativity and excludes a large part of the relativistic MOND theories. This limit can also be interpreted as a limit on an external tidal potential acting on the Solar System coming from the internal mass of our Galaxy (including dark matter) or from a new hypothetical body. C1 [Hees, A.; Folkner, W. M.; Jacobson, R. A.; Park, R. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hees, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 63 TC 29 Z9 29 U1 0 U2 2 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 MAY 13 PY 2014 VL 89 IS 10 AR 102002 DI 10.1103/PhysRevD.89.102002 PG 9 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AH0SC UT WOS:000335829600002 ER PT J AU Wang, Y Wang, MH Zhang, RY Ghan, SJ Lin, Y Hu, JX Pan, BW Levy, M Jiang, JH Molina, MJ AF Wang, Yuan Wang, Minghuai Zhang, Renyi Ghan, Steven J. Lin, Yun Hu, Jiaxi Pan, Bowen Levy, Misti Jiang, Jonathan H. Molina, Mario J. TI Assessing the effects of anthropogenic aerosols on Pacific storm track using a multiscale global climate model SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE aerosol-cloud-climate interaction; convective storms, cloud invigoration ID LONG-TERM IMPACTS; PNNL-MMF; PRECIPITATION; INTENSIFICATION; MICROPHYSICS; ATMOSPHERE; OXIDATION; PRODUCT; TROPICS; CLOUDS AB Atmospheric aerosols affect weather and global general circulation by modifying cloud and precipitation processes, but the magnitude of cloud adjustment by aerosols remains poorly quantified and represents the largest uncertainty in estimated forcing of climate change. Here we assess the effects of anthropogenic aerosols on the Pacific storm track, using a multiscale global aerosol-climate model (GCM). Simulations of two aerosol scenarios corresponding to the present day and preindustrial conditions reveal long-range transport of anthropogenic aerosols across the north Pacific and large resulting changes in the aerosol optical depth, cloud droplet number concentration, and cloud and ice water paths. Shortwave and long-wave cloud radiative forcing at the top of atmosphere are changed by -2.5 and +1.3 W m(-2), respectively, by emission changes from preindustrial to present day, and an increased cloud top height indicates invigorated midlatitude cyclones. The overall increased precipitation and poleward heat transport reflect intensification of the Pacific storm track by anthropogenic aerosols. Hence, this work provides, for the first time to the authors' knowledge, a global perspective of the effects of Asian pollution outflows from GCMs. Furthermore, our results suggest that the multiscale modeling framework is essential in producing the aerosol invigoration effect of deep convective clouds on a global scale. C1 [Wang, Yuan; Zhang, Renyi; Lin, Yun; Hu, Jiaxi; Pan, Bowen; Levy, Misti] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Wang, Yuan; Jiang, Jonathan H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wang, Minghuai; Ghan, Steven J.] Pacific NW Natl Lab, Richland, WA 99354 USA. [Zhang, Renyi] Peking Univ, Coll Environm Sci & Engn, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100871, Peoples R China. [Molina, Mario J.] Univ Calif San Diego, Dept Chem & Biochem, San Diego, CA 92093 USA. RP Zhang, RY (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM renyi-zhang@tamu.edu; mjmolina@ucsd.edu RI Zhang, Renyi/A-2942-2011; Ghan, Steven/H-4301-2011; Levy, Misti/G-8660-2014; Wang, Minghuai/E-5390-2011; Lin, Yun/B-1906-2013 OI Ghan, Steven/0000-0001-8355-8699; Levy, Misti/0000-0002-4832-7753; Lin, Yun/0000-0001-8222-0346; Wang, Minghuai/0000-0002-9179-228X; FU National Aeronautics and Space Administration (NASA) Graduate Student Fellowship in Earth System Science; Ministry of Science and Technology of China [2013CB955800]; NASA Research Opportunities in Space and Earth Sciences Enhancing the Capability of Computational Earth System Models and Using NASA Data for Operation and Assessment program at the Jet Propulsion Laboratory, California Institute of Technology under NASA; Department of Energy (DOE) Office of Science, Decadal and Regional Climate Prediction using Earth System Models program; DOE [DE-AC06-76RLO 1830]; Office of Science of the US Department of Energy [DE-AC05-00OR22725] FX The authors acknowledge T. Yuan and P. Liss for providing additional comments. This work was supported by a National Aeronautics and Space Administration (NASA) Graduate Student Fellowship in Earth System Science (to Y.W.), Ministry of Science and Technology of China Award (2013CB955800 to R.Z.), the NASA Research Opportunities in Space and Earth Sciences Enhancing the Capability of Computational Earth System Models and Using NASA Data for Operation and Assessment program at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA (Y.W. and J.H.J.), and the Department of Energy (DOE) Office of Science, Decadal and Regional Climate Prediction using Earth System Models program (M.W. and S.J.G.). PNNL is operated by Battelle for the DOE under Contract DE-AC06-76RLO 1830. This research used resources of the Oak Ridge Leadership Computing Facility at the Oak Ridge National Laboratory, which is supported by the Office of Science of the US Department of Energy under Contract DE-AC05-00OR22725. NR 43 TC 35 Z9 37 U1 10 U2 59 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAY 13 PY 2014 VL 111 IS 19 BP 6894 EP 6899 DI 10.1073/pnas.1403364111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AH0GS UT WOS:000335798000044 PM 24733923 ER PT J AU Achterberg, RK Gierasch, PJ Conrath, BJ Fletcher, LN Hesman, BE Bjoraker, GL Flasar, FM AF Achterberg, R. K. Gierasch, P. J. Conrath, B. J. Fletcher, L. N. Hesman, B. E. Bjoraker, G. L. Flasar, F. M. TI CHANGES TO SATURN'S ZONAL-MEAN TROPOSPHERIC THERMAL STRUCTURE AFTER THE 2010-2011 NORTHERN HEMISPHERE STORM SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: atmospheres; planets and satellites: individual (Saturn) ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; PARA-HYDROGEN FRACTION; OUTER PLANETS; JUPITERS ATMOSPHERE; 2.2-CM WAVELENGTH; CASSINI/CIRS; DYNAMICS; PAIRS; TEMPERATURES; EVOLUTION AB We use far-infrared (20-200 mu m) data from the Composite Infrared Spectrometer on the Cassini spacecraft to determine the zonal-mean temperature and hydrogen para-fraction in Saturn's upper troposphere from observations taken before and after the large northern hemisphere storm in 2010-2011. During the storm, zonal mean temperatures in the latitude band between approximately 25 degrees N and 45 degrees N (planetographic latitude) increased by about 3 K, while the zonal mean hydrogen para-fraction decreased by about 0.04 over the same latitudes, at pressures greater than about 300 mbar. These changes occurred over the same latitude range as the disturbed cloud band seen in visible images. The observations are consistent with low para-fraction gas being brought up from the level of the water cloud by the strong convective plume associated with the storm, while being heated by condensation of water vapor, and then advected zonally by the winds near the plume tops in the upper troposphere. C1 [Achterberg, R. K.; Hesman, B. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Gierasch, P. J.; Conrath, B. J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Fletcher, L. N.] Univ Oxford, Clarenden Lab, Oxford OX1 3PU, England. [Bjoraker, G. L.; Flasar, F. M.] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. RP Achterberg, RK (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM Richard.K.Achterberg@nasa.gov RI Fletcher, Leigh/D-6093-2011; Flasar, F Michael/C-8509-2012 OI Fletcher, Leigh/0000-0001-5834-9588; FU NASA Cassini Project; NASA Cassini Data Analysis and Participating Scientists Program [NNX12AC24G]; Royal Society Research Fellowship at the University of Oxford FX This work was supported by the NASA Cassini Project and NASA Cassini Data Analysis and Participating Scientists Program grant number NNX12AC24G. Fletcher was supported by a Royal Society Research Fellowship at the University of Oxford. NR 27 TC 10 Z9 10 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 92 DI 10.1088/0004-637X/786/2/92 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500016 ER PT J AU Ackermann, M Ajello, M Allafort, A Antolini, E Barbiellini, G Bastieri, D Bellazzini, R Bissaldi, E Bonamente, E Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cavazzuti, E Cecchi, C Chaves, RCG Chekhtman, A Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S D'Ammando, F De Palma, F Dermer, CD Silva, EDE Donato, D Drell, PS Favuzzi, C Finke, J Focke, WB Franckowiak, A Fukazawa, Y Fusco, P Gargano, F Gasparrini, D Gehrels, N Giglietto, N Giordano, F Giroletti, M Godfrey, G Grenier, IA Guiriec, S Hayashida, M Hewitt, JW Horan, D Hughes, RE Iafrate, G Johnson, AS Knoedlseder, J Kuss, M Lande, J Larsson, S Latronico, L Longo, F Loparco, F Lovellette, MN Lubrano, P Mayer, M Mazziotta, MN McEnery, JE Michelson, PF Mizuno, T Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nemmen, R Nuss, E Ohsugi, T Orienti, M Orlando, E Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Porter, TA Raino, S Razzano, M Reimer, A Reimer, O Sanchez, DA Schulz, A Sgro, C Siskind, EJ Spandre, G Spinelli, P Stawarz, L Takahashi, H Takahashi, T Thayer, JG Thayer, JB Thompson, DJ Tinivella, M Torres, DF Tosti, G Troja, E Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Werner, M Winer, BL Wood, DL Wood, KS Aleksic, J Ansoldi, S Antonelli, LA Antoranz, P Babic, A Bangale, P de Almeida, UB Barrio, JA Gonzalez, JB Bednarek, W Berger, K Bernardini, E Biland, A Blanch, O Bock, RK Bonnefoy, S Bonnoli, G Borracci, F Bretz, T Carmona, E Carosi, A Fidalgo, DC Colin, P Colombo, E Contreras, JL Cortina, J Covino, S Da Vela, P Dazzi, F De Angelis, A De Caneva, G De Lotto, B Mendez, CD Doert, M Dominguez, A Prester, DD Dorner, D Doro, M Einecke, S Eisenacher, D Elsaesser, D Farina, E Ferenc, D Fonseca, MV Font, L Frantzen, K Fruck, C Lopez, RJG Garczarczyk, M Terrats, DG Gaug, M Giavitto, G Godinovic, N Munoz, AG Gozzini, SR Hadasch, D Herrero, A Hildebrand, D Hose, J Hrupec, D Idec, W Kadenius, V Kellermann, H Knoetig, ML Kodani, K Konno, Y Krause, J Kubo, H Kushida, J La Barbera, A Lelas, D Lewandowska, N Lindfors, E Lombardi, S Lopez, M Lopez-Coto, R Lopez-Oramas, A Lorenz, E Lozano, I Makariev, M Mallot, K Maneva, G Mankuzhiyil, N Mannheim, K Maraschi, L Marcote, B Mariotti, M Martinez, M Mazin, D Menzel, U Meucci, M Miranda, JM Mirzoyan, R Moralejo, A Munar-Adrover, P Nakajima, D Niedzwiecki, A Nishijima, K Nilsson, K Nowak, N Orito, R Overkemping, A Paiano, S Palatiello, M Paneque, D Paoletti, R Paredes, JM Paredes-Fortuny, X Partini, S Persic, M Prada, F Moroni, PGP Prandini, E Preziuso, S Puljak, I Reinthal, R Rhode, W Ribo, M Rico, J Garcia, JR Rugamer, S Saggion, A Saito, T Saito, K Salvati, M Satalecka, K Scalzotto, V Scapin, V Schultz, C Schweizer, T Shore, SN Sillanpaa, A Sitarek, J Snidaric, I Sobczynska, D Spanier, F Stamatescu, V Stamerra, A Steinbring, T Storz, J Sun, S Suric, T Takalo, L Takami, H Tavecchio, F Temnikov, P Terzic, T Tescaro, D Teshima, M Thaele, J Tibolla, O Toyama, T Treves, A Vogler, P Wagner, RM Zandanel, F Zanin, R Aller, MF Angelakis, E Blinov, DA Djorgovski, SG Drake, AJ Efimova, NV Gurwell, MA Homan, DC Jordan, B Kopatskaya, EN Kovalev, YY Kurtanidze, OM Lahteenmaki, A Larionov, VM Lister, ML Nieppola, E Nikolashvili, MG Ros, E Savolainen, T Sigua, LA Tornikoski, M AF Ackermann, M. Ajello, M. Allafort, A. Antolini, E. Barbiellini, G. Bastieri, D. Bellazzini, R. Bissaldi, E. Bonamente, E. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cavazzuti, E. Cecchi, C. Chaves, R. C. G. Chekhtman, A. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. D'Ammando, F. De Palma, F. Dermer, C. D. do Couto e Silva, E. Donato, D. Drell, P. S. Favuzzi, C. Finke, J. Focke, W. B. Franckowiak, A. Fukazawa, Y. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Giglietto, N. Giordano, F. Giroletti, M. Godfrey, G. Grenier, I. A. Guiriec, S. Hayashida, M. Hewitt, J. W. Horan, D. Hughes, R. E. Iafrate, G. Johnson, A. S. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Mayer, M. Mazziotta, M. N. McEnery, J. E. Michelson, P. F. Mizuno, T. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nemmen, R. Nuss, E. Ohsugi, T. Orienti, M. Orlando, E. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Porter, T. A. Raino, S. Razzano, M. Reimer, A. Reimer, O. Sanchez, D. A. Schulz, A. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Stawarz, L. Takahashi, H. Takahashi, T. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Werner, M. Winer, B. L. Wood, D. L. Wood, K. S. Aleksic, J. Ansoldi, S. Antonelli, L. A. Antoranz, P. Babic, A. Bangale, P. de Almeida, U. Barres Barrio, J. A. Becerra Gonzalez, J. Bednarek, W. Berger, K. Bernardini, E. Biland, A. Blanch, O. Bock, R. K. Bonnefoy, S. Bonnoli, G. Borracci, F. Bretz, T. Carmona, E. Carosi, A. Fidalgo, D. Carreto Colin, P. Colombo, E. Contreras, J. L. Cortina, J. Covino, S. Da Vela, P. Dazzi, F. De Angelis, A. De Caneva, G. De Lotto, B. Mendez, C. Delgado Doert, M. Dominguez, A. Prester, D. Dominis Dorner, D. Doro, M. Einecke, S. Eisenacher, D. Elsaesser, D. Farina, E. Ferenc, D. Fonseca, M. V. Font, L. Frantzen, K. Fruck, C. Lopez, R. J. Garcia Garczarczyk, M. Terrats, D. Garrido Gaug, M. Giavitto, G. Godinovic, N. Munoz, A. Gonzalez Gozzini, S. R. Hadasch, D. Herrero, A. Hildebrand, D. Hose, J. Hrupec, D. Idec, W. Kadenius, V. Kellermann, H. Knoetig, M. L. Kodani, K. Konno, Y. Krause, J. Kubo, H. Kushida, J. La Barbera, A. Lelas, D. Lewandowska, N. Lindfors, E. Lombardi, S. Lopez, M. Lopez-Coto, R. Lopez-Oramas, A. Lorenz, E. Lozano, I. Makariev, M. Mallot, K. Maneva, G. Mankuzhiyil, N. Mannheim, K. Maraschi, L. Marcote, B. Mariotti, M. Martinez, M. Mazin, D. Menzel, U. Meucci, M. Miranda, J. M. Mirzoyan, R. Moralejo, A. Munar-Adrover, P. Nakajima, D. Niedzwiecki, A. Nishijima, K. Nilsson, K. Nowak, N. Orito, R. Overkemping, A. Paiano, S. Palatiello, M. Paneque, D. Paoletti, R. Paredes, J. M. Paredes-Fortuny, X. Partini, S. Persic, M. Prada, F. Moroni, P. G. Prada Prandini, E. Preziuso, S. Puljak, I. Reinthal, R. Rhode, W. Ribo, M. Rico, J. Garcia, J. Rodriguez Ruegamer, S. Saggion, A. Saito, T. Saito, K. Salvati, M. Satalecka, K. Scalzotto, V. Scapin, V. Schultz, C. Schweizer, T. Shore, S. N. Sillanpaeae, A. Sitarek, J. Snidaric, I. Sobczynska, D. Spanier, F. Stamatescu, V. Stamerra, A. Steinbring, T. Storz, J. Sun, S. Suric, T. Takalo, L. Takami, H. Tavecchio, F. Temnikov, P. Terzic, T. Tescaro, D. Teshima, M. Thaele, J. Tibolla, O. Toyama, T. Treves, A. Vogler, P. Wagner, R. M. Zandanel, F. Zanin, R. Aller, M. F. Angelakis, E. Blinov, D. A. Djorgovski, S. G. Drake, A. J. Efimova, N. V. Gurwell, M. A. Homan, D. C. Jordan, B. Kopatskaya, E. N. Kovalev, Y. Y. Kurtanidze, O. M. Laehteenmaeki, A. Larionov, V. M. Lister, M. L. Nieppola, E. Nikolashvili, M. G. Ros, E. Savolainen, T. Sigua, L. A. Tornikoski, M. CA Fermi Large Area Telescope Collab MAGIC Collaboration TI MULTIFREQUENCY STUDIES OF THE PECULIAR QUASAR 4C+21.35 DURING THE 2010 FLARING ACTIVITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; gamma rays: general; quasars: general; quasars: individual (4C +21.35); radiation mechanisms: non-thermal ID RAY BRIGHT BLAZARS; BLACK-HOLE MASS; EXTRAGALACTIC BACKGROUND LIGHT; SPECTRUM RADIO QUASARS; LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS; GAMMA-RAY; GALACTIC NUCLEI; X-RAY; EMISSION-LINE AB The discovery of rapidly variable Very High Energy ( VHE; E > 100 GeV). - ray emission from 4C + 21.35 ( PKS 1222+ 216) by MAGIC on 2010 June 17, triggered by the high activity detected by the Fermi Large Area Telescope ( LAT) in high energy ( HE; E > 100 MeV). - rays, poses intriguing questions on the location of the. - ray emitting region in this flat spectrum radio quasar. We present multifrequency data of 4C + 21.35 collected from centimeter to VHE during 2010 to investigate the properties of this source and discuss a possible emission model. The first hint of detection at VHE was observed by MAGIC on 2010 May 3, soon after a gamma- ray flare detected by Fermi-LAT that peaked on April 29. The same emission mechanism may therefore be responsible for both the HE and VHE emission during the 2010 flaring episodes. Two optical peaks were detected on 2010 April 20 and June 30, close in time but not simultaneous with the two gamma- ray peaks, while no clear connection was observed between the X-ray and gamma- ray emission. An increasing flux density was observed in radio and mm bands from the beginning of 2009, in accordance with the increasing gamma- ray activity observed by Fermi-LAT, and peaking on 2011 January 27 in the mm regime ( 230 GHz). We model the spectral energy distributions ( SEDs) of 4C + 21.35 for the two periods of the VHE detection and a quiescent state, using a one-zone model with the emission coming from a very compact region outside the broad line region. The three SEDs can be fit with a combination of synchrotron self-Compton and external Compton emission of seed photons from a dust torus, changing only the electron distribution parameters between the epochs. The fit of the optical/UV part of the spectrum for 2010 April 29 seems to favor an inner disk radius of < six gravitational radii, as one would expect from a prograde-rotating Kerr black hole. C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.; Bernardini, E.; De Caneva, G.; Gozzini, S. R.; Mallot, K.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Allafort, A.; Caliandro, G. A.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Godfrey, G.; Johnson, A. S.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Porter, T. A.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Allafort, A.; Caliandro, G. A.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Godfrey, G.; Johnson, A. S.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Porter, T. A.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Antolini, E.; Bonamente, E.; Cecchi, C.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Antolini, E.; Bonamente, E.; Cecchi, C.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. 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Dominis; Ferenc, D.; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Suric, T.; Terzic, T.] Univ Rijeka, Rudjer Boskov Inst, Croatian MAGIC Consortium, HR-10000 Zagreb, Croatia. [Babic, A.; Prester, D. Dominis; Ferenc, D.; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Suric, T.; Terzic, T.] Univ Split, HR-10000 Zagreb, Croatia. [Bangale, P.; de Almeida, U. Barres; Bock, R. K.; Borracci, F.; Colin, P.; Fruck, C.; Hose, J.; Kellermann, H.; Knoetig, M. L.; Krause, J.; Lorenz, E.; Mazin, D.; Menzel, U.; Mirzoyan, R.; Nakajima, D.; Nowak, N.; Paneque, D.; Garcia, J. Rodriguez; Schweizer, T.; Sun, S.; Teshima, M.; Toyama, T.; Wagner, R. M.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Barrio, J. A.; Bonnefoy, S.; Contreras, J. L.; Fonseca, M. V.; Lopez, M.; Lozano, I.; Satalecka, K.; Scapin, V.] Univ Complutense, E-28040 Madrid, Spain. [Becerra Gonzalez, J.; Berger, K.; Colombo, E.; Lopez, R. J. Garcia; Garczarczyk, M.; Herrero, A.; Tescaro, D.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Bednarek, W.; Idec, W.; Niedzwiecki, A.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland. [Biland, A.; Hildebrand, D.; Vogler, P.] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland. [Bretz, T.; Fidalgo, D. Carreto; Dorner, D.; Eisenacher, D.; Elsaesser, D.; Lewandowska, N.; Mannheim, K.; Ruegamer, S.; Spanier, F.; Steinbring, T.; Storz, J.; Tibolla, O.] Univ Wurzburg, D-97074 Wurzburg, Germany. [Carmona, E.; Mendez, C. Delgado] Ctr Invest Energet Medioambient & Tecnol, E-28040 Madrid, Spain. [Doert, M.; Einecke, S.; Frantzen, K.; Overkemping, A.; Rhode, W.; Thaele, J.] Tech Univ Dortmund, D-44221 Dortmund, Germany. [Dominguez, A.; Prada, F.; Zandanel, F.] Inst Astrofis Andalucia CSIC, E-18080 Granada, Spain. [Farina, E.; Treves, A.] Univ Insubria, I-22100 Como, Italy. [Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiac, Bellaterra 08193, Spain. [Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain. [Kadenius, V.; Lindfors, E.; Nilsson, K.; Reinthal, R.; Takalo, L.] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland. [Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nishijima, K.; Orito, R.; Saito, T.; Saito, K.; Takami, H.] Kyoto Univ, Div Phys & Astron, Japanese MAGIC Consortium, Kyoto 6068501, Japan. [Makariev, M.; Maneva, G.; Temnikov, P.] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria. [Marcote, B.; Munar-Adrover, P.; Paredes, J. M.; Paredes-Fortuny, X.; Ribo, M.; Zanin, R.] Univ Barcelona ICC IEEC, E-08028 Barcelona, Spain. [Moroni, P. G. Prada; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy. [Moroni, P. G. Prada; Shore, S. N.] INFN Pisa, I-56126 Pisa, Italy. [Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Angelakis, E.; Kovalev, Y. Y.; Ros, E.; Savolainen, T.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Blinov, D. A.; Efimova, N. V.; Larionov, V. M.] Pulkovo Observ, St Petersburg 196140, Russia. [Djorgovski, S. G.; Drake, A. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Efimova, N. V.; Kopatskaya, E. N.; Larionov, V. M.] St Petersburg State Univ, Astron Inst, St Petersburg 199034, Russia. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Homan, D. C.] Denison Univ, Dept Phys, Granville, OH 43023 USA. [Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Kovalev, Y. Y.] Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Kurtanidze, O. M.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Abastumani, Rep of Georgia. [Kurtanidze, O. M.] Kazan Fed Univ, Engelhardt Astron Observ, Tatarstan, Russia. [Laehteenmaeki, A.; Nieppola, E.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Nieppola, E.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikio, Finland. [Ros, E.] Univ Valencia, E-46010 Valencia, Spain. [Larionov, V. M.] St Petersburg Branch, Isaac Newton Inst Chile, St Petersburg, Russia. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM dammando@ira.inaf.it; justin.finke@nrl.navy.mil; davide.donato-1@nasa.gov; tterzic@uniri.hr; jbecerragonzalez@gmail.com RI Fonseca Gonzalez, Maria Victoria/I-2004-2015; Contreras Gonzalez, Jose Luis/K-7255-2014; Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Temnikov, Petar/L-6999-2016; Maneva, Galina/L-7120-2016; Makariev, Martin/M-2122-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Barrio, Juan/L-3227-2014; Martinez Rodriguez, Manel/C-2539-2017; Cortina, Juan/C-2783-2017; Ribo, Marc/B-3579-2015; Antoranz, Pedro/H-5095-2015; Miranda, Jose Miguel/F-2913-2013; Delgado, Carlos/K-7587-2014; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Blinov, Dmitry/G-9925-2013; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; Stamatescu, Victor/C-9945-2016; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Fernandez, Ester/K-9734-2014; Lopez Moya, Marcos/L-2304-2014; GAug, Markus/L-2340-2014; Font, Lluis/L-4197-2014; Moralejo Olaizola, Abelardo/M-2916-2014; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Babic, Ana/B-9599-2014; Lahteenmaki, Anne/L-5987-2013; Reimer, Olaf/A-3117-2013; Kovalev, Yuri/J-5671-2013; Kurtanidze, Omar/J-6237-2014; Rico, Javier/K-8004-2014; OI Bonnoli, Giacomo/0000-0003-2464-9077; Doro, Michele/0000-0001-9104-3214; Stamerra, Antonio/0000-0002-9430-5264; Prandini, Elisa/0000-0003-4502-9053; Becerra Gonzalez, Josefa/0000-0002-6729-9022; Caraveo, Patrizia/0000-0003-2478-8018; Giordano, Francesco/0000-0002-8651-2394; Prada Moroni, Pier Giorgio/0000-0001-9712-9916; LA BARBERA, ANTONINO/0000-0002-5880-8913; Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; De Lotto, Barbara/0000-0003-3624-4480; Sgro', Carmelo/0000-0001-5676-6214; Savolainen, Tuomas/0000-0001-6214-1085; SPINELLI, Paolo/0000-0001-6688-8864; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Bissaldi, Elisabetta/0000-0001-9935-8106; Temnikov, Petar/0000-0002-9559-3384; Torres, Diego/0000-0002-1522-9065; Barrio, Juan/0000-0002-0965-0259; Cortina, Juan/0000-0003-4576-0452; Iafrate, Giulia/0000-0002-6185-8292; Antoranz, Pedro/0000-0002-3015-3601; Miranda, Jose Miguel/0000-0002-1472-9690; Delgado, Carlos/0000-0002-7014-4101; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Blinov, Dmitry/0000-0003-0611-5784; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; Stamatescu, Victor/0000-0001-9030-7513; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Lopez Moya, Marcos/0000-0002-8791-7908; GAug, Markus/0000-0001-8442-7877; Font, Lluis/0000-0003-2109-5961; Moralejo Olaizola, Abelardo/0000-0002-1344-9080; Morselli, Aldo/0000-0002-7704-9553; Babic, Ana/0000-0001-9549-9710; Reimer, Olaf/0000-0001-6953-1385; Kovalev, Yuri/0000-0001-9303-3263; Rico, Javier/0000-0003-4137-1134; Ros, Eduardo/0000-0001-9503-4892; Angelakis, Emmanouil/0000-0001-7327-5441; Covino, Stefano/0000-0001-9078-5507; Paredes, Josep M./0000-0002-1566-9044; Gasparrini, Dario/0000-0002-5064-9495; Tavecchio, Fabrizio/0000-0003-0256-0995; Persic, Massimo/0000-0003-1853-4900; Dominguez, Alberto/0000-0002-3433-4610; Bastieri, Denis/0000-0002-6954-8862; Farina, Emanuele Paolo/0000-0002-6822-2254; Ribo, Marc/0000-0002-9931-4557; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Ahnen, Max Ludwig/0000-0003-1000-0082 FU CPAN [CSD2007- 00042]; MultiDark [CSD2009-00064] FX MAGIC Collaboration would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de losMuchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. Thisworkwas also supported by the CPAN CSD2007- 00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence "Origin and Structure of the Universe," by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. We thank the Swift team for making these observations possible, the duty scientists, and science planners. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2009, AJ, 137, 3718). The MOJAVE project is supported under NASA-Fermi grant 11-Fermi11-0019. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work made use of the Swinburne University of Technology software correlator (Deller et al. 2011, PASP, 123, 275), developed as part of the Australian Major National Research Facilities Programme and operated under license. The OVRO 40-m monitoring program is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST-1109911. This paper is partly based on observations with the 100m telescope of the MPIfR ( Max-Planck-Institut fur Radioastronomie) at Effelsberg and the Medicina telescope operated by INAF-Istituto di Radioastronomia. We acknowledge A. Orlati, S. Righini, and the Enhanced Single-dish Control System (ESCS) Development Team. We acknowledge financial contribution from agreement ASI-INAF I/009/10/0. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Data from the Steward Observatory spectropolarimetric monitoring project were used. This program is supported by Fermi Guest Investigator grants NNX08AW56G, NNX09AU10G, and NNX12AO93G. The St. Petersburg University team acknowledges support from Russian RFBR foundation, grants 12-02-00452 and 12-02-31193. The Abastumani team acknowledges financial support of the project FR/638/6-320/12 by the Shota Rustaveli National Science Foundation under contract 31/77. The Metsahovi team acknowledges support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). E. R. was partially supported by the Spanish MINECO projectsAYA2009-13036-C02-02 and AYA2012-38491-C02-01 and by the Generalitat Valenciana project PROMETEO/2009/104, as well as by the COST MP0905 action " Black Holes in a Violent Universe." Y.Y.K. was partly supported by the Russian Foundation for Basic Research (project 13-02-12103) and the Dynasty Foundation. We thank the anonymous referee for useful comments and suggestions. J.F. would like to thank J. Steiner for useful discussions regarding the black hole spin of 4C+21.35. F. D. thanks P. Smith for useful discussions about the polarimetric observations of 4C +21.35. NR 88 TC 12 Z9 12 U1 2 U2 37 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 157 DI 10.1088/0004-637X/786/2/157 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500080 ER PT J AU Croll, B Rappaport, S DeVore, J Gilliland, RL Crepp, JR Howard, AW Star, KM Chiang, E Levine, AM Jenkins, J Albert, L Bonomo, AS Fortney, JJ Isaacson, H AF Croll, Bryce Rappaport, Saul DeVore, John Gilliland, Ronald L. Crepp, Justin R. Howard, Andrew W. Star, Kimberly M. Chiang, Eugene Levine, Alan M. Jenkins, Jonm. Albert, Loic Bonomo, Aldo S. Fortney, Jonathan J. Isaacson, Howard TI MULTIWAVELENGTH OBSERVATIONS OF THE CANDIDATE DISINTEGRATING SUB-MERCURY KIC 12557548B SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; infrared: planetary systems; planetary systems; stars: individual (KIC 12557548); techniques: photometric ID INTERSTELLAR SILICATE MINERALOGY; INFRARED THERMAL EMISSION; SECONDARY ECLIPSE; PLANET CANDIDATE; GIANT PLANET; TELESCOPE; EXOPLANET; CURVE; WAVELENGTHS; GRAINS AB We present multiwavelength photometry, high angular resolution imaging, and radial velocities of the unique and confounding disintegrating low-mass planet candidate KIC 12557548b. Our high angular resolution imaging, which includes space-based Hubble Space TelescopeWide Field Camera 3 (HST/WFC3) observations in the optical (similar to 0.53 mu m and similar to 0.77 mu m), and ground-based Keck/NIRC2 observations in K' band (similar to 2.12 mu m), allow us to rule out background and foreground candidates at angular separations greater than 0 ''.2 that are bright enough to be responsible for the transits we associate with KIC 12557548. Our radial velocity limit from Keck/HIRES allows us to rule out bound, low-mass stellar companions (similar to 0.2 M-circle dot) to KIC 12557548 on orbits less than 10 yr, as well as placing an upper limit on the mass of the candidate planet of 1.2 Jupiter masses; therefore, the combination of our radial velocities, high angular resolution imaging, and photometry are able to rule out most false positive interpretations of the transits. Our precise multiwavelength photometry includes two simultaneous detections of the transit of KIC 12557548b usingCanada-France-Hawaii Telescope/Wide-field InfraRedCamera (CFHT/WIRCam) at 2.15 mu m and the Kepler space telescope at 0.6 mu m, as well as simultaneous null-detections of the transit by Kepler and HST/WFC3 at 1.4 mu m. Our simultaneous HST/WFC3 and Kepler null-detections provide no evidence for radically different transit depths at these wavelengths. Our simultaneous CFHT/WIRCam detections in the near-infrared and with Kepler in the optical reveal very similar transit depths (the average ratio of the transit depths at similar to 2.15 mu m compared with similar to 0.6 mu m is: 1.02 +/- 0.20). This suggests that if the transits we observe are due to scattering from single-size particles streaming from the planet in a comet-like tail, then the particles must be similar to 0.5 mu m in radius or larger, which would favor that KIC 12557548b is a sub-Mercury rather than super-Mercury mass planet. C1 [Croll, Bryce; Rappaport, Saul; Levine, Alan M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [DeVore, John] Visidyne Inc, Santa Barbara, CA 93105 USA. [Gilliland, Ronald L.; Star, Kimberly M.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Howard, Andrew W.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Chiang, Eugene] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Chiang, Eugene] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Jenkins, Jonm.] NASA Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Albert, Loic] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Bonomo, Aldo S.] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, Italy. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Croll, B (reprint author), MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. EM croll@space.mit.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354 FU California Institute of Technology - NASA through the Sagan Fellowship Program; Natural Sciences and Engineering Research Council of Canada; NASA through a grant from the Space Telescope Science Institute [GO-12987]; University of Hawaii and the University of California FX B.C.' s work was performed under a contract with the California Institute of Technology funded by NASA through the Sagan Fellowship Program. The Natural Sciences and Engineering Research Council of Canada supports the research of B. C. Support for program GO-12987 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555 This work was based on observations at the W. M. Keck Observatory granted by the University of Hawaii and the University of California. We thank the observers who contributed to the measurements reported here and acknowledge the efforts of the Keck Observatory staff. We extend special thanks to those of Hawaiian ancestry onwhose sacred mountain of Mauna Kea we are privileged to be guests. The authors thank the referee, Jan Budaj, for helpful comments that have improved this manuscript and for providing us with very convenient tables of indices of refraction for various minerals. The authors especially appreciate the hard work and diligence of the CFHT staff for both scheduling the challenging CFHT observations described here and ensuring these "Staring Mode" observations were successful. The authors thank Geoff Marcy for contributing to and assisting with the Keck/ HIRES RV observations of KIC 1255b that we discuss in this work. We also thank Ray Jayawardhana, David Lafreniere, Magali Deleuil, and Claire Moutou for contributing to the CFHT observing proposal, and Josh Winn for contributing to the HST observing proposal, on which this work is partially based. NR 47 TC 21 Z9 22 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 100 DI 10.1088/0004-637X/786/2/100 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500024 ER PT J AU Enoto, T Sasano, M Yamada, S Tamagawa, T Makishima, K Pottschmidt, K Marcu, D Corbet, RHD Fuerst, F Wilms, J AF Enoto, Teruaki Sasano, Makoto Yamada, Shin'ya Tamagawa, Toru Makishima, Kazuo Pottschmidt, Katja Marcu, Diana Corbet, Robin H. D. Fuerst, Felix Wilms, Joern TI SPECTRAL AND TIMING NATURE OF THE SYMBIOTIC X-RAY BINARY 4U 1954+319: THE SLOWEST ROTATING NEUTRON STAR IN AN X-RAY BINARY SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries: symbiotic; magnetic fields; stars: individual (3A 1954+319, 4U 1954+319); stars: neutron; X-rays : binaries ID ACCRETION-INDUCED COLLAPSE; MAGNETIC-FIELDS; BROAD-BAND; INFRARED-SPECTROSCOPY; SUZAKU OBSERVATION; IGR J16194-2810; CROSS-SECTIONS; 4TH EDITION; CYGNUS X-1; GX 1+4 AB The symbiotic X-ray binary (SyXB) 4U 1954+ 319 is a rare system hosting a peculiar neutron star (NS) and an M-type optical companion. Its similar to 5.4 hr NS spin period is the longest among all known accretion-powered pulsars and exhibited large (similar to 7%) fluctuations over 8 yr. A spin trend transition was detected with Swift/BAT around an X-ray brightening in 2012. The source was in quiescent and bright states before and after this outburst based on 60 ks Suzaku observations in 2011 and 2012. The observed continuum is well described by a Comptonized model with the addition of a narrow 6.4 keV Fe-K alpha line during the outburst. Spectral similarities to slowly rotating pulsars in high-mass X-ray binaries, its high pulsed fraction (similar to 60%-80%), and the location in the Corbet diagram favor high B-field (greater than or similar to 10(12) G) over a weak field as in low-mass X-ray binaries. The observed low X-ray luminosity (10(33)-10(35) erg s(-1)), probable wide orbit, and a slow stellar wind of this SyXB make quasi-spherical accretion in the subsonic settling regime a plausible model. Assuming a similar to 10(13) G NS, this scheme can explain the similar to 5.4 hr equilibrium rotation without employing the magnetar-like field (similar to 10(16) G) required in the disk accretion case. The timescales of multiple irregular flares (similar to 50 s) can also be attributed to the free-fall time from the Alfven shell for a similar to 10(13) G field. A physical interpretation of SyXBs beyond the canonical binary classifications is discussed. C1 [Enoto, Teruaki; Pottschmidt, Katja; Marcu, Diana; Corbet, Robin H. D.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Enoto, Teruaki; Yamada, Shin'ya; Tamagawa, Toru; Makishima, Kazuo] RIKEN Nishina Ctr, High Energy Astrophys Lab, Wako, Saitama 3510198, Japan. [Sasano, Makoto; Makishima, Kazuo] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Pottschmidt, Katja; Marcu, Diana; Corbet, Robin H. D.] CRESST, Baltimore, MD 21250 USA. [Pottschmidt, Katja; Marcu, Diana; Corbet, Robin H. D.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Fuerst, Felix] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Wilms, Joern] Univ Erlangen Nurnberg, Dr Remeis Sternwarte & Erlangen Ctr Astroparticle, D-96049 Bamberg, Germany. RP Enoto, T (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 662, Greenbelt, MD 20771 USA. EM teruaki.enoto@nasa.gov RI Wilms, Joern/C-8116-2013; XRAY, SUZAKU/A-1808-2009 OI Wilms, Joern/0000-0003-2065-5410; FU JSPS KAKENHI; Deutsches Zentrum fur Luftund Raumfahrt [50 OR 1207]; [24-3320] FX The authors would like to express their thanks to the Suzaku team for their prompt observation during the 2012 flaring activity. T. E. was supported by JSPS KAKENHI, Grant- in-Aid for JSPS Fellows, 24-3320. We thank Pranab Ghosh and Hiromitsu Takahashi for useful discussions on this source, Kunugawa Tomoya and Kenta Hotokezaka for comments on the binary evolution. We thank the Deutsches Zentrum fur Luftund Raumfahrt for partial funding under DLR grant number 50 OR 1207. NR 92 TC 4 Z9 4 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 127 DI 10.1088/0004-637X/786/2/127 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500051 ER PT J AU Hanabata, Y Katagiri, H Hewitt, JW Ballet, J Fukazawa, Y Fukui, Y Hayakawa, T Lemoine-Goumard, M Pedaletti, G Strong, AW Torres, DF Yamazaki, R AF Hanabata, Y. Katagiri, H. Hewitt, J. W. Ballet, J. Fukazawa, Y. Fukui, Y. Hayakawa, T. Lemoine-Goumard, M. Pedaletti, G. Strong, A. W. Torres, D. F. Yamazaki, R. TI DETAILED INVESTIGATION OF THE GAMMA-RAY EMISSION IN THE VICINITY OF SNR W28 WITH FERMI-LAT SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; diffusion; gamma rays: ISM; ISM: supernova remnants ID LARGE-AREA TELESCOPE; SUPERNOVA REMNANT W28; DIFFUSIVE SHOCK ACCELERATION; GALACTIC COSMIC-RAYS; MHZ OH MASERS; H-II REGIONS; MOLECULAR CLOUDS; HIGH-ENERGY; IC 443; STREAMING INSTABILITY AB We present a detailed investigation of the gamma-ray emission in the vicinity of the supernova remnant (SNR) W28 (G6.4-0.1) observed by the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope. We detected significant gamma-ray emission spatially coincident with TeV sources HESS J1800-240A, B, and C, located outside the radio boundary of the SNR. Their spectra in the 2-100 GeV band are consistent with the extrapolation of the power-law spectra of the TeV sources. We also identified a new source of GeV emission, dubbed Source W, which lies outside the boundary of TeV sources and coincides with radio emission from the western part of W28. All of the GeV gamma-ray sources overlap with molecular clouds in the velocity range from 0 to 20 km s(-1). Under the assumption that the gamma-ray emission toward HESS J1800-240A, B, and C comes from pi(0) decay due to the interaction between the molecular clouds and cosmic rays (CRs) escaping from W28, they can be naturally explained by a single model in which the CR diffusion coefficient is smaller than the theoretical expectation in the interstellar space. The total energy of the CRs escaping from W28 is constrained through the same modeling to be larger than similar to 2 x 10(49) erg. The emission from Source W can also be explained with the same CR escape scenario. C1 [Hanabata, Y.] Univ Tokyo, Inst Cosmic Ray Res, Kashiwa, Chiba 2778582, Japan. [Katagiri, H.] Ibaraki Univ, Coll Sci, Bunkyo Ku, Mito, Ibaraki 3108512, Japan. [Hewitt, J. W.] Univ Maryland, CRESST, Baltimore, MD 21250 USA. [Hewitt, J. W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ballet, J.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, CNRS,CEA IRFU,Lab AIM, F-91191 Gif Sur Yvette, France. [Fukazawa, Y.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Fukui, Y.; Hayakawa, T.] Nagoya Univ, Dept Phys & Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Lemoine-Goumard, M.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Pedaletti, G.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain. [Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Torres, D. F.] ICREA, Barcelona, Spain. [Yamazaki, R.] Aoyama Gakuin Univ, Dept Math & Phys, Sagamihara, Kanagawa 2525258, Japan. RP Hanabata, Y (reprint author), Univ Tokyo, Inst Cosmic Ray Res, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778582, Japan. EM hanabata@icrr.u-tokyo.ac.jp; katagiri@mx.ibaraki.ac.jp RI Torres, Diego/O-9422-2016 OI Torres, Diego/0000-0002-1522-9065 FU Friedrich Wilhelm Bessel Award of the Alexander von Humboldt Foundation; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; [AYA2012-39303]; [iLINK2011-0303] FX The research of D.F.T. and G.P. has been done in the framework of the grant AYA2012-39303 and iLINK2011-0303. D.F.T. was additionally supported by a Friedrich Wilhelm Bessel Award of the Alexander von Humboldt Foundation.; The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States; the Commissariat a l' Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy; the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK), and Japan Aerospace Exploration Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden.; Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. NR 65 TC 11 Z9 11 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 145 DI 10.1088/0004-637X/786/2/145 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500068 ER PT J AU Jian, LK Wei, HY Russell, CT Luhmann, JG Klecker, B Omidi, N Isenberg, PA Goldstein, ML Figueroa-Vinas, A Blanco-Cano, X AF Jian, L. K. Wei, H. Y. Russell, C. T. Luhmann, J. G. Klecker, B. Omidi, N. Isenberg, P. A. Goldstein, M. L. Figueroa-Vinas, A. Blanco-Cano, X. TI ELECTROMAGNETIC WAVES NEAR THE PROTON CYCLOTRON FREQUENCY: STEREO OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE interplanetary medium; magnetic fields; solar wind; waves ID SOLAR-WIND PROTONS; HELIOSPHERIC MAGNETIC-FIELDS; RING-PLASMA INSTABILITY; AMPLITUDE ALFVEN WAVES; POLAR CORONAL HOLE; INTERPLANETARY MEDIUM; GRIGG-SKJELLERUP; PICKUP IONS; 1 AU; VELOCITY DISTRIBUTIONS AB Transverse, near-circularly polarized, parallel-propagating electromagnetic waves around the proton cyclotron frequency were found sporadically in the solar wind throughout the inner heliosphere. They could play an important role in heating and accelerating the solar wind. These low-frequency waves (LFWs) are intermittent but often occur in prolonged bursts lasting over 10 minutes, named "LFW storms." Through a comprehensive survey of them from Solar Terrestrial Relations Observatory A using dynamic spectral wave analysis, we have identified 241 LFW storms in 2008, present 0.9% of the time. They are left-hand (LH) or right-hand (RH) polarized in the spacecraft frame with similar characteristics, probably due to Doppler shift of the same type of waves or waves of intrinsically different polarities. In rare cases, the opposite polarities are observed closely in time or even simultaneously. Having ruled out interplanetary coronal mass ejections, shocks, energetic particles, comets, planets, and interstellar ions as LFW sources, we discuss the remaining generation scenarios: LH ion cyclotron instability driven by greater perpendicular temperature than parallel temperature or by ring-beam distribution, and RH ion fire hose instability driven by inverse temperature anisotropy or by cool ion beams. The investigation of solar wind conditions is compromised by the bias of the one-dimensional Maxwellian fit used for plasma data calibration. However, the LFW storms are preferentially detected in rarefaction regions following fast winds and when the magnetic field is radial. This preference may be related to the ion cyclotron anisotropy instability in fast wind and the minimum in damping along the radial field. C1 [Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Jian, L. K.; Goldstein, M. L.; Figueroa-Vinas, A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Wei, H. Y.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Klecker, B.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Omidi, N.] Solana Sci Inc, Solana Beach, CA 92075 USA. [Isenberg, P. A.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Blanco-Cano, X.] Univ Nacl Autonoma Mexico, Inst Geofis, Coyoacan, DF, Mexico. RP Jian, LK (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM lan.jian@nasa.gov RI Jian, Lan/B-4053-2010 OI Jian, Lan/0000-0002-6849-5527 FU NASA [NNX13AI65G, NNX12AB29G, NNX11AJ37G, NNX13AF97G]; NASA's STEREO mission, through IMPACT [NAS5-00133]; PLASTIC [NAS5-00132]; NSF [AGS0962506] FX This work is supported by NASA grants NNX13AI65G and NNX12AB29G and by NASA's STEREO mission, through IMPACT (Contract NAS5-00133) and PLASTIC (Contract NAS5-00132). We thank the STEREO/PLASTIC team for providing the plasma data. Jian thanks S. P. Gary for the helpful discussion and H. R. Lai and Y. D. Jia for assisting with the comet catalog. Isenberg is supported by NASA grants NNX11AJ37G and NNX13AF97G and NSF grant AGS0962506. NR 126 TC 14 Z9 14 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 MAY 10 PY 2014 VL 786 IS 2 AR 123 DI 10.1088/0004-637X/786/2/123 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500047 ER PT J AU Kaspi, VM Archibald, RF Bhalerao, V Dufour, F Gotthelf, EV An, HJ Bachetti, M Beloborodov, AM Boggs, SE Christensen, FE Craig, WW Grefenstette, BW Hailey, CJ Harrison, FA Kennea, JA Kouveliotou, C Madsen, KK Mori, K Markwardt, CB Stern, D Vogel, JK Zhang, WW AF Kaspi, Victoria M. Archibald, Robert F. Bhalerao, Varun Dufour, Francois Gotthelf, Eric V. An, Hongjun Bachetti, Matteo Beloborodov, Andrei M. Boggs, Steven E. Christensen, Finn E. Craig, William W. Grefenstette, Brian W. Hailey, Charles J. Harrison, Fiona A. Kennea, Jamie A. Kouveliotou, Chryssa Madsen, Kristin K. Mori, Kaya Markwardt, Craig B. Stern, Daniel Vogel, Julia K. Zhang, William W. TI TIMING AND FLUX EVOLUTION OF THE GALACTIC CENTER MAGNETAR SGR J1745-2900 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; pulsars: general; stars: magnetic field; stars: neutron; X-rays: stars ID SOFT GAMMA REPEATER; RAY PULSAR 1E-1048.1-5937; LARGE TORQUE VARIATIONS; SAGITTARIUS A-ASTERISK; X-RAY; NEUTRON-STARS; 2002 OUTBURST; VORTEX CREEP; VELA PULSAR; 1E 2259+586 AB We present the X-ray timing and spectral evolution of the Galactic Center magnetar SGR J1745-2900 for the first similar to 4 months post-discovery using data obtained with the Nuclear Spectroscopic Telescope Array and Swift observatories. Our timing analysis reveals a large increase in the magnetar spin-down rate by a factor of 2.60 +/- 0.07 over our data span. We further show that the change in spin evolution was likely coincident with a bright X-ray burst observed in 2013 June by Swift, and if so, there was no accompanying discontinuity in the frequency. We find that the source 3-10 keV flux has declined monotonically by a factor of similar to 2 over an 80 day period post-outburst accompanied by a similar to 20% decrease in the source's blackbody temperature, although there is evidence for both flux and kT having leveled off. We argue that the torque variations are likely to be magnetospheric in nature and will dominate over any dynamical signatures of orbital motion around Sgr A*. C1 [Kaspi, Victoria M.; Archibald, Robert F.; Dufour, Francois; An, Hongjun] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Bhalerao, Varun] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Gotthelf, Eric V.; Beloborodov, Andrei M.; Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Bachetti, Matteo] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Bachetti, Matteo] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, William W.; Vogel, Julia K.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Kennea, Jamie A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Kouveliotou, Chryssa] NASA, Marshall Space Flight Ctr, Astrophys Off, Huntsville, AL 35812 USA. [Markwardt, Craig B.; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kaspi, VM (reprint author), McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. EM vkaspi@physics.mcgill.ca RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Bhalerao, Varun/0000-0002-6112-7609; Bachetti, Matteo/0000-0002-4576-9337; An, Hongjun/0000-0002-6389-9012; Madsen, Kristin/0000-0003-1252-4891 FU NASA [NNG08FD60C, NNX-10-AI72G, NNX-13-AI34G, NAS5-00136]; National Aeronautics and Space Administration; NSERC Discovery Grant FX This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software ( NuSTARDAS) jointly developed by the ASI Science Data Center ( ASDC, Italy) and the California Institute of Technology (USA). We acknowledge the use of public data from the Swift data archive. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. We thank the Swift SOT team for their work in scheduling. V.M.K. receives support from an NSERC Discovery Grant and Accelerator Supplement, from the Centre de Recherche en Astrophysique du Quebec, an R. Howard Webster Foundation Fellowship from the Canadian Institute forAdvanced Study, the Canada Research Chairs Program and the Lorne Trottier Chair in Astrophysics and Cosmology. R.F.A. receives support from a Walter C. Sumner Memorial Fellowship. A.M.B. was supported by NASA grants NNX-10-AI72G and NNX-13-AI34G. J.A.K. was supported by supported by NASA contract NAS5-00136. J.K.V.'s work was performed under the auspices of the U. S. Department of Energy by Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344. NR 51 TC 33 Z9 34 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 84 DI 10.1088/0004-637X/786/2/84 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500008 ER PT J AU Mommert, M Hora, JL Farnocchia, D Chesley, SR Vokrouhlicky, D Trilling, DE Mueller, M Harris, AW Smith, HA Fazio, GG AF Mommert, M. Hora, J. L. Farnocchia, D. Chesley, S. R. Vokrouhlicky, D. Trilling, D. E. Mueller, M. Harris, A. W. Smith, H. A. Fazio, G. G. TI CONSTRAINING THE PHYSICAL PROPERTIES OF NEAR-EARTH OBJECT 2009 BD SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: planetary systems; minor planets, asteroids: individual (2009 BD) ID THERMAL-INFRARED OBSERVATIONS; SPITZER-SPACE-TELESCOPE; RADIATION PRESSURE; ASTEROIDAL FRAGMENTS; YARKOVSKY; POPULATION; TARGET; RADAR; MISSION; HAYABUSA AB We report on Spitzer Space Telescope Infrared Array Camera observations of near-Earth object 2009 BD that were carried out in support of the NASA Asteroid Robotic Retrieval Mission concept. We did not detect 2009 BD in 25 hr of integration at 4.5 mu m. Based on an upper-limit flux density determination from our data, we present a probabilistic derivation of the physical properties of this object. The analysis is based on the combination of a thermophysical model with an orbital model accounting for the non-gravitational forces acting upon the body. We find two physically possible solutions. The first solution shows 2009 BD as a 2.9 +/- 0.3 m diameter rocky body (rho = 2.9 +/- 0.5 g cm(-3)) with an extremely high albedo of 0.85(-0.10)(+0.20) that is covered with regolith-like material, causing it to exhibit a low thermal inertia (Gamma = 30(-10)(+20) SI units). The second solution suggests 2009 BD to be a 4 +/- 1 m diameter asteroid with pv = 0.45(-0.15)(+0.35) that consists of a collection of individual bare rock slabs (Gamma = 2000 +/- 1000 SI units, rho = 1.7(-0.4)(+0.7) g cm(-3)). We are unable to rule out either solution based on physical reasoning. 2009 BD is the smallest asteroid for which physical properties have been constrained, in this case using an indirect method and based on a detection limit, providing unique information on the physical properties of objects in the size range smaller than 10 m. C1 [Mommert, M.; Trilling, D. E.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Hora, J. L.; Smith, H. A.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Farnocchia, D.; Chesley, S. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vokrouhlicky, D.] Charles Univ Prague, Inst Astron, CZ-18000 Prague 8, Czech Republic. [Mueller, M.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Harris, A. W.] DLR Inst Planetary Res, D-12489 Berlin, Germany. RP Mommert, M (reprint author), No Arizona Univ, Dept Phys & Astron, POB 6010, Flagstaff, AZ 86011 USA. EM michael.mommert@nau.edu OI Mueller, Michael/0000-0003-3217-5385 FU NASA Postdoctoral Program at the Jet Propulsion Laboratory; California Institute of Technology; Grant Agency of the Czech Republic [P209-13- 01308S]; Propulsion Laboratory RSA [1367413] FX The authors of this work thank Tom Soifer, Director of the Spitzer Space Telescope, for the time allocation to observe 2009 BD. We also would like to thank Paul Chodas for his support and many informative conversations. We thank an anonymous referee for useful suggestions that improved this manuscript. D. Farnocchia was supported for this research by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. The work of S. Chesley was conducted at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. The work of D. Vokrouhlicky was partially supported by the Grant Agency of the Czech Republic (grant P209-13- 01308S). J. L. Hora and H. A. Smith acknowledge partial support from Jet Propulsion Laboratory RSA No. 1367413. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 71 TC 7 Z9 7 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 148 DI 10.1088/0004-637X/786/2/148 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500071 ER PT J AU Pullen, AR Dore, O Bock, J AF Pullen, Anthony R. Dore, Olivier Bock, Jamie TI INTENSITY MAPPING ACROSS COSMIC TIMES WITH THE Ly alpha LINE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; diffuse radiation; intergalactic medium; large-scale structure of universe ID STAR-FORMATION HISTORY; LUMINOSITY FUNCTION; NEUTRAL HYDROGEN; ESCAPE FRACTION; INTERGALACTIC MEDIUM; GALEX SPECTROSCOPY; RADIATIVE-TRANSFER; REDSHIFT GALAXIES; EMITTING GALAXIES; MASS FUNCTION AB We present a quantitative model of Ly alpha emission throughout cosmic history and determine the prospects for intensity mapping spatial fluctuations in the Lya signal. Since (1) our model assumes at z > 6 the minimum star formation required to sustain reionization and (2) is based atz < 6 on a luminosity function (LF) extrapolated from the few observed bright Lya emitters, this should be considered a lower limit. Mapping the line emission allows probes of reionization, star formation, and large-scale structure (LSS) as a function of redshift. While Lya emission during reionization has been studied, we also predict the postreionization signal to test predictions of the intensity and motivate future intensity mapping probes of reionization. We include emission from massive dark matter halos and the intergalactic medium (IGM) in our model. We find agreement with current, measured LFs of Lya emitters at z < 8. However, diffuse IGM emission, not associated with Lya emitters, dominates the intensity up to z similar to 10. While our model is applicable for deep-optical or near-infrared observers like the James Webb Space Telescope, only intensity mapping will detect the diffuse IGM emission. We also construct a three-dimensional power spectrum model of the Lya emission. Finally, we consider the prospects of an intensity mapper for measuring Lya fluctuations while identifying interloper contamination for removal. Our results suggest that while the reionization signal is challenging, Lya fluctuations can be an interesting new probe of LSS at late times when used in conjunction with other lines, e.g., Ha, to monitor low-redshift foreground confusion. C1 [Pullen, Anthony R.; Dore, Olivier; Bock, Jamie] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [Dore, Olivier; Bock, Jamie] CALTECH, Pasadena, CA 91125 USA. RP Pullen, AR (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr,MS 169-237, Pasadena, CA 91109 USA. EM anthony.r.pullen@jpl.nasa.gov RI Pullen, Anthony/I-7007-2015 OI Pullen, Anthony/0000-0002-2091-8738 FU NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology; administered by Oak Ridge Associated Universities through a contract with NASA; Keck Institute of Space Studies FX We thank P. Capak, A. Cooray, S. Furlanetto, Y. Gong, C. Hirata, A. Lidz, G. Rudie, M. Viero, and M. Zemcov for helpful comments and useful discussions. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. A. P. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. This work was supported by the Keck Institute of Space Studies and we thank colleagues at the "First Billion Years" for stimulating discussions, in particular J. Bowman and A. Readhead for organizing it. NR 68 TC 19 Z9 19 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 111 DI 10.1088/0004-637X/786/2/111 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500035 ER PT J AU Puzia, TH Paolillo, M Goudfrooij, P Maccarone, TJ Fabbiano, G Angelini, L AF Puzia, Thomas H. Paolillo, Maurizio Goudfrooij, Paul Maccarone, Thomas J. Fabbiano, Giuseppina Angelini, Lorella TI WIDE-FIELD HUBBLE SPACE TELESCOPE OBSERVATIONS OF THE GLOBULAR CLUSTER SYSTEM IN NGC 1399 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: individual (NGC 1399); galaxies: star clusters: general; globular clusters: general ID EARLY-TYPE GALAXIES; ACS-VIRGO CLUSTER; SURFACE-BRIGHTNESS PROFILES; LARGE-MAGELLANIC-CLOUD; NEARBY DWARF GALAXIES; MASSIVE STAR-CLUSTERS; POINT-SPREAD FUNCTION; HALF-LIGHT RADII; STRUCTURAL PARAMETERS; FORNAX CLUSTER AB We present a comprehensive high spatial resolution imaging study of globular clusters (GCs) in NGC 1399, the central giant elliptical cD galaxy in the Fornax galaxy cluster, conducted with the Advanced Camera for Surveys (ACS) aboard the Hubble Space Telescope (HST). Using a novel technique to construct drizzled point-spread function libraries for HST/ACS data, we accurately determine the fidelity of GC structural parameter measurements from detailed artificial star cluster experiments and show the superior robustness of the GC half-light radius, r(h), compared with other GC structural parameters, such as King core and tidal radius. The measurement of r(h) for the major fraction of the NGC 1399 GC system reveals a trend of increasing r(h) versus galactocentric distance, R-gal, out to about 10 kpc and a flat relation beyond. This trend is very similar for blue and red GCs, which are found to have a mean size ratio of r(h),(red)/r(h),(blue) = 0.82 +/- 0.11 at all galactocentric radii from the core regions of the galaxy out to similar to 40 kpc. This suggests that the size difference between blue and red GCs is due to internal mechanisms related to the evolution of their constituent stellar populations. Modeling the mass density profile of NGC 1399 shows that additional external dynamical mechanisms are required to limit the GC size in the galaxy halo regions to r(h) approximate to 2 pc. We suggest that this may be realized by an exotic GC orbit distribution function, an extended dark matter halo, and/or tidal stress induced by the increased stochasticity in the dwarf halo substructure at larger galactocentric distances. We compare our results with the GC r(h) distribution functions in various galaxies and find that the fraction of extended GCs with r(h) >= 5 pc is systematically larger in late-type galaxies compared with GC systems in early-type galaxies. This is likely due to the dynamically more violent evolution of early-type galaxies. We match our GC r(h) measurements with radial velocity data from the literature and split the resulting sample at the median r(h) value into compact and extended GCs. We find that compact GCs show a significantly smaller line-of-sight velocity dispersion, = 225 +/- 25 km s(-1), than their extended counterparts, = 317 +/- 21 km s(-1). Considering the weaker statistical correlation in the GC r(h) color and the GC r(h)-R-gal relations, the more significant GC size-dynamics relation appears to be astrophysically more relevant and hints at the dominant influence of the GC orbit distribution function on the evolution of GC structural parameters. C1 [Puzia, Thomas H.] Pontificia Univ Catolica Chile, Natl Res Council Canada, Santiago 7820436, Chile. [Puzia, Thomas H.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Paolillo, Maurizio] Univ Naples Federico II, Dept Phys Sci, I-80126 Naples, Italy. [Paolillo, Maurizio] Ist Nazl Fis Nucl, Dept Phys Sci, Napoli Unit, I-80126 Naples, Italy. [Paolillo, Maurizio] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy. [Goudfrooij, Paul] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Maccarone, Thomas J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Fabbiano, Giuseppina] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Angelini, Lorella] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. RP Puzia, TH (reprint author), Pontificia Univ Catolica Chile, Natl Res Council Canada, Ave Vicuna Mackenna 4860, Santiago 7820436, Chile. EM tpuzia@astro.puc.cl RI Paolillo, Maurizio/J-1733-2012 OI Paolillo, Maurizio/0000-0003-4210-7693 FU NASA [NAS5-26555]; FONDECYT [1121005]; BASAL Center for Astrophysics and Associated Technologies [PFB-06]; National Research Council of Canada; University of Napoli Federico II; Chandra X-ray Center (CXC) [NAS8-03060] FX Support for HST program GO- 10129 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. This research was supported by FONDECYT Regular Project grant 1121005 and BASAL Center for Astrophysics and Associated Technologies (PFB-06). T. H. P. is thankful for the hospitality and support during his visits at the University of Napoli Federico II, where parts of this work were completed; he also gratefully acknowledges support in the form of a Plaskett Research Fellowship from the National Research Council of Canada. M. P. acknowledges financial support from the FARO 2011 project of the University of Napoli Federico II. This work was partially supported by the Chandra X-ray Center (CXC), which is operated by the Smithsonian Astrophysical Observatory (SAO) under NASA contract NAS8-03060. We are grateful to Anton Koekemoer and Andy Fruchter for their technical support and useful discussions on the MultiDrizzle code and to Chien Y. Peng for his help with the implementation and testing of the modified GALFIT routine. We thank TomRichtler and Ylva Schuberth for providing their radial velocity measurements ahead of publication, as well as Luis Ho and Zhao-Yu Li for kindly making available to us their latest NGC 1399 surface brightness profile measurements from the Carnegie-Irvine Galaxy Survey, again prior to publication. Avon Huxor has very kindly supplied M31 GC data prior to publication. We are grateful to the referee, Bill Harris, for providing a thoughtful and constructive report that helped improve the presentation of the results. We thank Jeremy Webb, Mark Gieles, Andres Jordan, Eric Peng, Chunyan Jiang, Stephen Zepf, and Arunav Kundu for valuable discussions and providing data in electronic format. Some of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Figures 2 and 3 were created with the help of the ESA/ESO/NASA Photoshop FITS Liberator. This research has made use of NASA's Astrophysics Data System. Facility: HST(ACS) NR 171 TC 22 Z9 22 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 78 DI 10.1088/0004-637X/786/2/78 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500002 ER PT J AU Rivers, E Markowitz, A Rothschild, R Bamba, A Fukazawa, Y Okajima, T Reeves, J Terashima, Y Ueda, Y AF Rivers, Elizabeth Markowitz, Alex Rothschild, Richard Bamba, Aya Fukazawa, Yasushi Okajima, Takashi Reeves, James Terashima, Yuichi Ueda, Yoshihiro TI TRACKING THE COMPLEX ABSORPTION IN NGC 2110 WITH TWO SUZAKU OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 2110); X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; LINE GALAXY NGC-2110; X-RAY BINARIES; BLACK-HOLE; XMM-NEWTON; INTERSTELLAR-MEDIUM; SEYFERT-GALAXIES; EMISSION; SPECTROSCOPY; REFLECTION AB We present spectral analysis of two Suzaku observations of the Seyfert 2 galaxy, NGC 2110. This source has been known to show complex, variable absorption which we study in depth by analyzing these two observations set 7 yr apart and by comparing them to previously analyzed observations with the XMM-Newton and Chandra observatories. We find that there is a relatively stable, full-covering absorber with a column density of similar to 3 x 10(22) cm(-2), with an additional patchy absorber that is likely variable in both column density and covering fraction over timescales of years, consistent with clouds in a patchy torus or in the broad line region. We model a soft emission line complex, likely arising from ionized plasma and consistent with previous studies. We find no evidence for reflection from an accretion disk in this source with contribution from neither relativistically broadened Fe K alpha line emission, nor from a Compton reflection hump. C1 [Rivers, Elizabeth; Markowitz, Alex; Rothschild, Richard] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Rivers, Elizabeth] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Markowitz, Alex] Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany. [Bamba, Aya] Aoyama Gakuin Univ, Dept Math & Phys, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan. [Fukazawa, Yasushi] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Okajima, Takashi] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reeves, James] Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Terashima, Yuichi] Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan. [Ueda, Yoshihiro] Kyoto Univ, Dept Astron, Kyoto 6068502, Japan. RP Rivers, E (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM erivers@caltech.edu RI XRAY, SUZAKU/A-1808-2009 FU NASA/GSFC; NASA/IPAC Extragalactic Database; [NNX13AF33G] FX This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). This work has made use of HEASARC online services, supported by NASA/GSFC, and the NASA/IPAC Extragalactic Database, operated by JPL/California Institute of Technology under contract with NASA. This research was supported by Grant NNX13AF33G. NR 42 TC 9 Z9 9 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 126 DI 10.1088/0004-637X/786/2/126 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500050 ER PT J AU Tian, H DeLuca, E Reeves, KK McKillop, S De Pontieu, B Martinez-Sykora, J Carlsson, M Hansteen, V Kleint, L Cheung, M Golub, L Saar, S Testa, P Weber, M Lemen, J Title, A Boerner, P Hurlburt, N Tarbell, TD Wuelser, JP Kankelborg, C Jaeggli, S McIntosh, SW AF Tian, H. DeLuca, E. Reeves, K. K. McKillop, S. De Pontieu, B. Martinez-Sykora, J. Carlsson, M. Hansteen, V. Kleint, L. Cheung, M. Golub, L. Saar, S. Testa, P. Weber, M. Lemen, J. Title, A. Boerner, P. Hurlburt, N. Tarbell, T. D. Wuelser, J. P. Kankelborg, C. Jaeggli, S. McIntosh, S. W. TI HIGH-RESOLUTION OBSERVATIONS OF THE SHOCK WAVE BEHAVIOR FOR SUNSPOT OSCILLATIONS WITH THE INTERFACE REGION IMAGING SPECTROGRAPH SO ASTROPHYSICAL JOURNAL LA English DT Article DE line: profiles; Sun: chromosphere; Sun: oscillations; Sun: transition region; waves ID RUNNING PENUMBRAL WAVES; TRANSITION REGION; DYNAMIC FIBRILS; SPECTROSCOPIC OBSERVATIONS; MAGNETOACOUSTIC SHOCKS; NUMERICAL SIMULATIONS; PROPAGATING WAVES; ATOMIC DATABASE; UMBRAL FLASHES; CORONAL LOOPS AB We present the first results of sunspot oscillations from observations by the Interface Region Imaging Spectrograph. The strongly nonlinear oscillation is identified in both the slit-jaw images and the spectra of several emission lines formed in the transition region and chromosphere. We first apply a single Gaussian fit to the profiles of the Mg II 2796.35 angstrom, C II 1335.71 angstrom, and Si IV 1393.76 angstrom lines in the sunspot. The intensity change is similar to 30%. The Doppler shift oscillation reveals a saw tooth pattern with an amplitude of similar to 10 km s(-1) in Si IV. The Si IV oscillation lags those of C II and Mg II by similar to 6 and similar to 25 s, respectively. The line width suddenly increases as the Doppler shift changes from redshift to blueshift. However, we demonstrate that this increase is caused by the superposition of two emission components. We then perform detailed analysis of the line profiles at a few selected locations on the slit. The temporal evolution of the line core is dominated by the following behavior: a rapid excursion to the blue side, accompanied by an intensity increase, followed by a linear decrease of the velocity to the red side. The maximum intensity slightly lags the maximum blueshift in Si IV, whereas the intensity enhancement slightly precedes the maximum blueshift in Mg II. We find a positive correlation between the maximum velocity and deceleration, a result that is consistent with numerical simulations of upward propagating magnetoacoustic shock waves. C1 [Tian, H.; DeLuca, E.; Reeves, K. K.; McKillop, S.; Golub, L.; Saar, S.; Testa, P.; Weber, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [De Pontieu, B.; Martinez-Sykora, J.; Kleint, L.; Cheung, M.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Martinez-Sykora, J.; Kleint, L.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Carlsson, M.; Hansteen, V.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Kleint, L.] NASA, Ames Res Ctr, Moffett Field, CA 94305 USA. [Kankelborg, C.; Jaeggli, S.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [McIntosh, S. W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. RP Tian, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hui.tian@cfa.harvard.edu RI Reeves, Katharine/P-9163-2014; DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Carlsson, Mats/0000-0001-9218-3139 FU NASA [NNG09FA40C]; Lockheed Martin Independent Research Program; European Research Council [291058]; LMSAL [8100002705] FX IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research center and major contributions to downlink communications funded by the Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract. This work is supported by NASA under contract NNG09FA40C (IRIS) and the Lockheed Martin Independent Research Program, the European Research Council grant agreement No. 291058, and contract 8100002705 from LMSAL to SAO. H. T. thanks Luc Rouppe van der Voort and Jorrit Leenaarts for useful discussion. NR 56 TC 35 Z9 35 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 137 DI 10.1088/0004-637X/786/2/137 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500060 ER PT J AU Vinas, AF Moya, PS Araneda, JA Maneva, YG AF Vinas, Adolfo F. Moya, Pablo S. Araneda, Jaime A. Maneva, Yana G. TI RECONSTRUCTION OF A BROADBAND SPECTRUM OF ALFVENIC FLUCTUATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; methods: analytical; turbulence; waves ID SOLAR-WIND TURBULENCE; MAGNETIC HELICITY; INTERPLANETARY SHOCKS; HYBRID SIMULATIONS; CYCLOTRON WAVES; INSTABILITY; EVOLUTION; DECAY; ANGLE; FIELD AB Alfvenic fluctuations in the solar wind exhibit a high degree of velocities and magnetic field correlations consistent with Alfven waves propagating away and toward the Sun. Two remarkable properties of these fluctuations are the tendencies to have either positive or negative magnetic helicity (-1 <= sigma(m) <= + 1) associated with either left-or righttopological handedness of the fluctuations and to have a constant magnetic field magnitude. This paper provides, for the first time, a theoretical framework for reconstructing both the magnetic and velocity field fluctuations with a divergence-free magnetic field, with any specified power spectral index and normalized magnetic-and cross-helicity spectrum field fluctuations for any plasma species. The spectrum is constructed in the Fourier domain by imposing two conditions-a divergence-free magnetic field and the preservation of the sense of magnetic helicity in both spaces-as well as using Parseval's theorem for the conservation of energy between configuration and Fourier spaces. Applications to the one-dimensional spatial Alfvenic propagation are presented. The theoretical construction is in agreement with typical time series and power spectra properties observed in the solar wind. The theoretical ideas presented in this spectral reconstruction provide a foundation for more realistic simulations of plasma waves, solar wind turbulence, and the propagation of energetic particles in such fluctuating fields. C1 [Vinas, Adolfo F.; Moya, Pablo S.; Maneva, Yana G.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Moya, Pablo S.; Maneva, Yana G.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Araneda, Jaime A.] Univ Concepcion, Fac Ciencias Fis & Matemat, Dept Fis, Concepcion, Chile. RP Vinas, AF (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Mail Code 673, Greenbelt, MD 20771 USA. EM adolfo.vinas@nasa.gov RI Moya, Pablo/C-3163-2011; Araneda, Jaime/J-9245-2015; OI Moya, Pablo/0000-0002-9161-0888; Maneva, Yana/0000-0002-2422-6050 FU NASA Wind/SWE program; Comision Nacional de Ciencia y Tecnologia (CONICyT, Chile); NASA Wind program; FONDECYT [1110880]; CUA post-doctoral program FX We thank Dr. Robert Wicks for providing critical suggestions and comments on this paper, and the NASA Wind/SWE program for the support of this research. We also thank the Comision Nacional de Ciencia y Tecnologia (CONICyT, Chile) for providing financial support for P.S.M.'s postdoctoral fellowship. Y.M. thanks the NASA Wind and CUA post-doctoral programs for their financial support. J.A.A. thanks FONDECYT (No. 1110880) for providing financial support. NR 25 TC 3 Z9 3 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 86 DI 10.1088/0004-637X/786/2/86 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500010 ER PT J AU Yu, SS Pearson, JC AF Yu, Shanshan Pearson, John C. TI TERAHERTZ MEASUREMENTS OF THE HOT HYDRONIUM ION WITH AN EXTENDED NEGATIVE GLOW DISCHARGE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: molecules; line: identification; molecular data; techniques: spectroscopic ID SIDE-BAND SPECTROSCOPY; LABORATORY MEASUREMENT; H3O+; H2O+; OH+; FREQUENCY; ASTRONOMY; SPECTRUM; SOFIA AB Terahertz absorption spectroscopy was employed to detect the ground-state inversion transitions of the hydronium ion (H3O+). The highly excited ions were created with an extended negative glow discharge through a gas mixture of 1 mtorr of H2O, 2 mtorr of H-2, and 12 mtorr of Ar, which allowed observation of transitions with J and K up to 12. In total, 47 transitions were measured in the 0.9-2.0 THz region and 22 of these were observed for the first time. The experimental uncertainties range from 100 to 300 kHz, which are much better than the range 0.3-1.2 MHz reported in previous work. Differences of up to 25.6 MHz were found between the observed positions and the catalog values that have been used for Herschel data analysis of observations of Sagittarius B2(N), NGC 4418, and Arp 220. The new and improved measurements were fit to experimental accuracies with an updated Hamiltonian, and better H3O+ predictions are reported to support the proper analysis of astronomical observations by high-resolution spectroscopy telescopes, such as Herschel, SOFIA, and ALMA. C1 [Yu, Shanshan; Pearson, John C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Yu, SS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM shanshan.yu@jpl.nasa.gov RI Yu, Shanshan/D-8733-2016 FU National Science Foundation Graduate Research Fellowship Program [DGE 1144083]; NASA Nancy Grace Roman Fellowship FX This material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE 1144083. The data presented here were obtained as part of HST Observing program 12034. K. F. acknowledges support through a NASA Nancy Grace Roman Fellowship during this work. NR 21 TC 2 Z9 2 U1 2 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 133 DI 10.1088/0004-637X/786/2/133 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500056 ER PT J AU Strekalov, DV Kowligy, AS Huang, YP Kumar, P AF Strekalov, Dmitry V. Kowligy, Abijith S. Huang, Yu-Ping Kumar, Prem TI Optical sum-frequency generation in a whispering-gallery-mode resonator SO NEW JOURNAL OF PHYSICS LA English DT Article DE nonlinear optics; sum-frequency generation; whispering-gallery-mode resonators ID UP-CONVERSION; MICROCAVITIES AB We demonstrate sum-frequency generation between a telecom wavelength and the Rb D2 line, achieved through natural phase matching in a nonlinear whispering gallery mode resonator. Due to the strong optical field confinement and ultra high Q of the cavity, the process saturates already at sub-mW pump peak power, at least two orders of magnitude lower than in existing waveguide-based devices. The experimental data are in agreement with the nonlinear dynamics and phase matching theory based on spherical geometry. Our experimental and theoretical results point toward a new platform for manipulating the color and quantum states of light waves for applications such as atomic memory based quantum networking and logic operations with optical signals. C1 [Strekalov, Dmitry V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kowligy, Abijith S.; Huang, Yu-Ping; Kumar, Prem] Northwestern Univ, Dept EECS, Ctr Photon Commun & Comp, Evanston, IL 60208 USA. RP Strekalov, DV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM dmitry.v.strekalov@jpl.nasa.gov RI Kumar, Prem/B-6691-2009 FU DARPA Zeno-based Opto-Electronics program [W31P4Q-09-1-0014]; National Aeronautics and Space Administration FX This work was supported by the DARPA Zeno-based Opto-Electronics program (grant no. W31P4Q-09-1-0014). It was partly carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. We thank J U Furst and T Beckmann for useful discussions. NR 31 TC 13 Z9 13 U1 1 U2 16 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 MAY 9 PY 2014 VL 16 AR 053025 DI 10.1088/1367-2630/16/5/053025 PG 15 WC Physics, Multidisciplinary SC Physics GA AL0VB UT WOS:000338843900005 ER PT J AU Wiersema, K Covino, S Toma, K van der Horst, AJ Varela, K Min, M Greiner, J Starling, RLC Tanvir, NR Wijers, RAMJ Campana, S Curran, PA Fan, Y Fynbo, JPU Gorosabel, J Gomboc, A Gotz, D Hjorth, J Jin, ZP Kobayashi, S Kouveliotou, C Mundell, C O'Brien, PT Pian, E Rowlinson, A Russell, DM Salvaterra, R Alighieri, SD Tagliaferri, G Vergani, SD Elliott, J Farina, C Hartoog, OE Karjalainen, R Klose, S Knust, F Levan, AJ Schady, P Sudilovsky, V Willingale, R AF Wiersema, K. Covino, S. Toma, K. van der Horst, A. J. Varela, K. Min, M. Greiner, J. Starling, R. L. C. Tanvir, N. R. Wijers, R. A. M. J. Campana, S. Curran, P. A. Fan, Y. Fynbo, J. P. U. Gorosabel, J. Gomboc, A. Goetz, D. Hjorth, J. Jin, Z. P. Kobayashi, S. Kouveliotou, C. Mundell, C. O'Brien, P. T. Pian, E. Rowlinson, A. Russell, D. M. Salvaterra, R. Alighieri, S. di Serego Tagliaferri, G. Vergani, S. D. Elliott, J. Farina, C. Hartoog, O. E. Karjalainen, R. Klose, S. Knust, F. Levan, A. J. Schady, P. Sudilovsky, V. Willingale, R. TI Circular polarization in the optical afterglow of GRB 121024A SO NATURE LA English DT Article ID GAMMA-RAY BURSTS; RELATIVISTIC COLLISIONLESS SHOCKS; MAGNETIC-FIELD STRUCTURE; LINEAR-POLARIZATION; LIGHT CURVES; EMISSION; POLARIMETRY; DUST; JETS; EXTINCTION AB Gamma-ray bursts (GRBs) are most probably powered by collimated relativistic outflows (jets) from accreting black holes at cosmological distances. Bright afterglows are produced when the outflow collides with the ambient medium. Afterglow polarization directly probes the magnetic properties of the jet when measured minutes after the burst, and it probes the geometric properties of the jet and the ambient medium when measured hours to days after the burst(1-5). High values of optical polarization detected minutes after the burst of GRB 120308A indicate the presence of large-scale ordered magnetic fields originating from the central engine(5) (the power source of the GRB). Theoretical models predict low degrees of linear polarization and no circular polarization at late times(6-8), when the energy in the original ejecta is quickly transferred to the ambient medium and propagates farther into the medium as a blast wave. Here we report the detection of circularly polarized light in the afterglow of GRB 121024A, measured 0.15 days after the burst. We show that the circular polarization is intrinsic to the afterglow and unlikely to be produced by dust scattering or plasma propagation effects. A possible explanation is to invoke anisotropic (rather than the commonly assumed isotropic) electron pitch-angle distributions, and we suggest that new models are required to produce the complex microphysics of realistic shocks in relativistic jets(9-11). C1 [Wiersema, K.; Starling, R. L. C.; Tanvir, N. R.; O'Brien, P. T.; Willingale, R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Covino, S.; Campana, S.; Tagliaferri, G.; Vergani, S. D.] INAF Brera Astron Observ, I-23807 Merate, LC, Italy. [Toma, K.] Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Toma, K.] Tohoku Univ, Astron Inst, Sendai, Miyagi 9808578, Japan. [Toma, K.] Tohoku Univ, Frontier Res Inst Interdisciplinary Sci, Sendai, Miyagi 9808578, Japan. [van der Horst, A. J.; Min, M.; Wijers, R. A. M. J.; Rowlinson, A.; Hartoog, O. E.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 SJ Amsterdam, Netherlands. [Varela, K.; Greiner, J.; Elliott, J.; Knust, F.; Schady, P.; Sudilovsky, V.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Curran, P. A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Fan, Y.; Jin, Z. P.] Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Astron, Nanjing 210008, Peoples R China. [Fynbo, J. P. U.; Hjorth, J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Gorosabel, J.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Gorosabel, J.] Univ Pais Vasco UPV EHU, ETS Ingn, Dept Fis Aplicada, Unidad Asociada Grp Ciencia Planetarias UPV EHU I, E-48013 Bilbao, Spain. [Gorosabel, J.] Basque Fdn Sci, Ikerbasque, E-48008 Bilbao, Spain. [Gomboc, A.] Univ Ljubljana, Fac Math & Phys, Ljubljana 1000, Slovenia. [Goetz, D.] Univ Paris Diderot, CNRS, DSM, AIM UMR CEA 7158,Irfu Serv Astrophys, F-91191 Gif Sur Yvette, France. [Kobayashi, S.; Mundell, C.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, ZP12, Huntsville, AL 35812 USA. [Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Pian, E.] INAF IASF Bologna, I-40129 Bologna, Italy. [Russell, D. M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Russell, D. M.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Russell, D. M.] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates. [Salvaterra, R.] INAF IASF Milano, I-20133 Milan, Italy. [Alighieri, S. di Serego] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Farina, C.; Karjalainen, R.] Isaac Newton Grp Telescopes, E-38700 Santa Cruz De La Palma, Canary Islands, Spain. [Klose, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Wiersema, K (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. EM kw113@le.ac.uk RI Curran, Peter/B-5293-2013; Hjorth, Jens/M-5787-2014; OI Tagliaferri, Gianpiero/0000-0003-0121-0723; Curran, Peter/0000-0003-3003-4626; Hjorth, Jens/0000-0002-4571-2306; Salvaterra, Ruben/0000-0002-9393-8078; Pian, Elena/0000-0001-8646-4858; Russell, David/0000-0002-3500-631X; Campana, Sergio/0000-0001-6278-1576; Wijers, Ralph/0000-0002-3101-1808; di Serego Alighieri, Sperello/0000-0001-8769-2692; Covino, Stefano/0000-0001-9078-5507 FU STFC; JSPS [231446]; European Research Council [247295]; Royal Society Fellowship; 973 Programme of China [2013CB837000]; Marie Curie Intra European Fellowship within the 7th European Community [IEF 274805]; Australian Research Council [DP120102393]; UK Space Agency FX This work is based on observations made with ESO telescopes at the Paranal Observatory under programme 090.D-0789. We thank all ING staff for their support of ACAM ToO observations. K. W. thanks J. Hinton for discussions. K. W. was supported by STFC. K. T. was supported by a JSPS Research Fellowship for Young Scientists no. 231446. A.J.v.d.H., R.A.M.J.W. and A. R. were supported by the European Research Council via Advanced Investigator grant no. 247295. R. L. C. S. was supported by a Royal Society Fellowship. Y.F. was supported by the 973 Programme of China, under grant 2013CB837000. D. M. R. was supported by a Marie Curie Intra European Fellowship within the 7th European Community Framework Programme under contract no. IEF 274805. This work was supported by the Australian Research Council (grant DP120102393). The William Herschel telescope and its override programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester, funded by the UK Space Agency. NR 45 TC 18 Z9 18 U1 0 U2 24 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAY 8 PY 2014 VL 509 IS 7499 BP 201 EP + DI 10.1038/nature13237 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AG5JC UT WOS:000335454300033 PM 24776800 ER PT J AU Ward, RL Fleddermann, R Francis, S Mow-Lowry, C Wuchenich, D Elliot, M Gilles, F Herding, M Nicklaus, K Brown, J Burke, J Dligatch, S Farrant, D Green, K Seckold, J Blundell, M Brister, R Smith, C Danzmann, K Heinzel, G Schutze, D Sheard, BS Klipstein, W McClelland, DE Shaddock, DA AF Ward, R. L. Fleddermann, R. Francis, S. Mow-Lowry, C. Wuchenich, D. Elliot, M. Gilles, F. Herding, M. Nicklaus, K. Brown, J. Burke, J. Dligatch, S. Farrant, D. Green, K. Seckold, J. Blundell, M. Brister, R. Smith, C. Danzmann, K. Heinzel, G. Schuetze, D. Sheard, B. S. Klipstein, W. McClelland, D. E. Shaddock, D. A. TI The design and construction of a prototype lateral-transfer retro-reflector for inter-satellite laser ranging SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article DE satellite interferometry; gravity measurement; precision optics; satellite optics AB The Gravity Recovery and Climate Experiment (GRACE) mission, launched in 2002, is nearing an end, and a continuation mission (GRACE Follow-on) is on a fast-tracked development. GRACE Follow-on will include a laser ranging interferometer technology demonstrator, which will perform the first laser interferometric ranging measurement between separate spacecraft. This necessitates the development of lightweight precision optics that can operate in this demanding environment. In particular, this beam routing system, called the triple mirror assembly, for the GRACE Follow-on mission presents a significant manufacturing challenge. Here we report on the design and construction of a prototype triple mirror assembly for the GRACE Follow-on mission. Our constructed prototype has a co-alignment error between the incoming and outgoing beams of 9 mu rad, which meets the requirement that this error must be less than 10 mu rad. C1 [Ward, R. L.; Fleddermann, R.; Francis, S.; Mow-Lowry, C.; Wuchenich, D.; Elliot, M.; McClelland, D. E.; Shaddock, D. A.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Mow-Lowry, C.; Danzmann, K.; Heinzel, G.; Schuetze, D.; Sheard, B. S.] Leibniz Univ Hannover, Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-30167 Hannover, Germany. [Mow-Lowry, C.; Heinzel, G.; Schuetze, D.; Sheard, B. S.] Leibniz Univ Hannover, Inst Gravitat Phys, D-30167 Hannover, Germany. [Gilles, F.; Herding, M.; Nicklaus, K.] SpaceTech GmbH, D-88090 Immenstaad, Germany. [Brown, J.; Dligatch, S.; Farrant, D.; Green, K.; Seckold, J.] CSIRO, Mat Sci & Engn, Lindfield, NSW 2070, Australia. [Burke, J.] BIAS, Opt Metrol & Optoelect Syst, D-28359 Bremen, Germany. [Blundell, M.; Brister, R.; Smith, C.] Mt Stromlo & Siding Spring Observ, EOS Space Syst, Weston, ACT 2611, Australia. [Klipstein, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ward, RL (reprint author), Australian Natl Univ, GPO Box 4, Canberra, ACT 0200, Australia. EM robert.ward@anu.edu.au RI McClelland, David/E-6765-2010; Mow-Lowry, Conor/F-8843-2015; Farrant, David/A-4028-2008; Shaddock, Daniel/A-7534-2011; Ward, Robert/I-8032-2014 OI McClelland, David/0000-0001-6210-5842; Shaddock, Daniel/0000-0002-6885-3494; Ward, Robert/0000-0001-5503-5241 FU German Federal Ministry of Education and Research; Deutsche Forschungsgemeinschaft (DFG) Cluster of Excellence QUEST (Centre for Quantum Engineering and Space-Time Research FX The TMA development was funded by the Australian Space Research Program, an initiative of the Australian Government, with contributions from the German Federal Ministry of Education and Research, the German Aerospace Centre, Australia's Commonwealth Scientific and Industrial Research Organisation, and the Deutsche Forschungsgemeinschaft (DFG) within the Cluster of Excellence QUEST (Centre for Quantum Engineering and Space- Time Research). The authors thank Bill Folkner for invaluable help in the early stages of the TMA design. NR 19 TC 7 Z9 8 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD MAY 7 PY 2014 VL 31 IS 9 AR 095015 DI 10.1088/0264-9381/31/9/095015 PG 11 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AF4HF UT WOS:000334671900016 ER PT J AU Frankenberg, C O'Dell, C Berry, J Guanter, L Joiner, J Kohler, P Pollock, R Taylor, TE AF Frankenberg, Christian O'Dell, Chris Berry, Joseph Guanter, Luis Joiner, Joanna Koehler, Philipp Pollock, Randy Taylor, Thomas E. TI Prospects for chlorophyll fluorescence remote sensing from the Orbiting Carbon Observatory-2 SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Chlorophyll fluorescence; GPP; OCO; OCO-2; Atmospheric carbon ID FOURIER-TRANSFORM SPECTROMETER; GASES OBSERVING SATELLITE; RADIATIVE-TRANSFER MODEL; CO2 RETRIEVAL; SPACE; PHOTOSYNTHESIS; GOSAT; WATER; PHYTOPLANKTON; SCIAMACHY AB The Orbiting Carbon Observatory-2 (OCO-2), scheduled to launch in July 2014, is a NASA mission designed to measure atmospheric CO2. Its main purpose is to allow inversions of net flux estimates of CO2 on regional to continental scales using the total column CO2 retrieved using high-resolution spectra in the 0.76, 1.6, and 2.0 mu m ranges. Recently, it was shown that solar-induced chlorophyll fluorescence (SIP), a proxy for gross primary production (GPP, carbon uptake through photosynthesis), can be accurately retrieved from space using high spectral resolution radiances in the 750 nm range from the Japanese GOSAT and European GOME-2 instruments. Here, we use real OCO-2 thermal vacuum test data as well as a full repeat cycle (16 days) of simulated OCO-2 spectra under realistic conditions to evaluate the potential of OCO-2 for retrievals of chlorophyll fluorescence and also its dependence on clouds and aerosols. We find that the single-measurement precision is 03-0.5 Wm(-2)sr(-1) mu m(-1) (15-25% of typical peak values), better than current measurements from space but still difficult to interpret on a single-sounding basis. The most significant advancement will come from smaller ground-pixel sizes and increased measurement frequency, with a 100-fold increase compared to GOSAT (and about 8 times higher than GOME-2). This will largely decrease the need for coarse spatial and temporal averaging in data analysis and pave the way to accurate local studies. We also find that the lack of full global mapping from the OCO-2 only incurs small representativeness errors on regional averages. Eventually, the combination of net ecosystem exchange (NEE) derived from CO2 source/sink inversions and SIF as proxy for GPP from the same satellite will provide a more process-based understanding of the global carbon cycle. (C) 2014 Elsevier Inc. All rights reseved. C1 [Frankenberg, Christian; Pollock, Randy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [O'Dell, Chris; Taylor, Thomas E.] Colorado State Univ, Ft Collins, CO 80523 USA. [Berry, Joseph] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA USA. [Guanter, Luis; Koehler, Philipp] Free Univ Berlin, Berlin, Germany. [Joiner, Joanna] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Frankenberg, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Christian.Frankenberg@jpl.nasa.gov RI Joiner, Joanna/D-6264-2012; Guanter, Luis/I-1588-2015; Frankenberg, Christian/A-2944-2013 OI Guanter, Luis/0000-0002-8389-5764; Frankenberg, Christian/0000-0002-0546-5857 FU NASA [1439002] FX Part of the research described in this paper was carried out by the jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. (c) 2013. All rights reserved. The Colorado State University contributions to the ACOS task were supported by NASA contract 1439002. We thank 4 anonymous reviewers for thorough and constructive reviews that strengthened the manuscript substantially. NR 43 TC 46 Z9 46 U1 17 U2 133 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 MAY 5 PY 2014 VL 147 BP 1 EP 12 DI 10.1016/j.rse.2014.02.007 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AH5QR UT WOS:000336186400001 ER PT J AU Mattar, C Franch, B Sobrino, JA Corbari, C Jimenez-Munoz, JC Olivera-Guerra, L Skokovic, D Soria, G Oltra-Carrio, R Julien, Y Mancini, M AF Mattar, C. Franch, B. Sobrino, J. A. Corbari, C. Jimenez-Munoz, J. C. Olivera-Guerra, L. Skokovic, D. Soria, G. Oltra-Carrio, R. Julien, Y. Mancini, M. TI Impacts of the broadband albedo on actual evapotranspiration estimated by S-SEBI model over an agricultural area SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Surface broadband albedo; BRDF; AHS; Angular variation; Heat fluxes; Evapotranspiration; S-SEBI ID SURFACE-ENERGY BALANCE; EMISSIVITY SEPARATION ALGORITHM; BIDIRECTIONAL REFLECTANCE MODEL; SPACEBORNE THERMAL EMISSION; LAND-SURFACE; HEAT-FLUX; HOT-SPOT; DIRECTIONAL SIGNATURES; VEGETATION CANOPY; RADIOMETER ASTER AB Surface albedo and emissivity are essential variables in surface energy balance. In recent decades, several land surface energy models have used both surface broadband albedo and emissivity in order to achieve reliable evapotranspiration retrievals on a daily basis. Despite these improvements in surface energy models, we noticed an assumption that most studies make when using this framework. It assumes that the surface broadband albedo and emissivity can be estimated directly as a weighted average of spectral surface bi-directional reflectances, and as a weighted average of spectral surface emissivities retrieved at a given view angle, respectively. However, this approach does not take into account surface anisotropy, which is described by the Bi-directional Reflectance Distribution Function (BRDF) in the case of the surface albedo. In this paper, we analyze the influence that estimating land surface albedo directly from the surface reflectance (alpha(REF)) or through the BRDF integration (alpha(BRDF)) has on the estimation of energy balance components (net radiation, latent and sensible heat fluxes and evapotranspiration) by using the Simplified Surface Energy Balance Index (S-SEBI). To this end, in-situ data and remote sensing images acquisitioned at different view zenith angles (VZA) such as 0 degrees, +/- 40 degrees and +/- 57 degrees by the Airborne Hyperspectral Scanner (AHS) over an agricultural area were used. Results show high variation in alpha(REF) depending on the VZA when compared to alpha(BRDF), with the highest difference observed in the backward scattering direction along the hot spot region (RMSE of 0.11 and relative error of 65%). Net radiation gives relative errors from 6 to 17%, with the maximum error obtained in the images that include the hot spot effect, whereas significant changes are not observed in case of the ground heat flux and the evaporative fraction. However, sensible heat flux, latent heat flux and daily evapotranspiration show relative errors ranging between 23-39%, 6-18% and 5-15% respectively. In a future study, the influence of estimating surface emissivity directly from the average of spectral emissivities under a given view angle or using a hemispherical value will be analyzed. (C) 2014 Elsevier Inc. All rights reserved. C1 [Mattar, C.; Sobrino, J. A.; Jimenez-Munoz, J. C.; Skokovic, D.; Soria, G.; Oltra-Carrio, R.; Julien, Y.] Univ Valencia, Image Proc Lab, Global Change Unit, Valencia 46980, Spain. [Mattar, C.; Olivera-Guerra, L.] Univ Chile, LAB, Santiago, Chile. [Franch, B.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Franch, B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Corbari, C.; Mancini, M.] Politecn Milan, Dept Civil & Environm Engn, I-20133 Milan, Italy. RP Mattar, C (reprint author), Univ Valencia, Image Proc Lab, Global Change Unit, Sci Pk,C Catedrtitico Jose Beltran 2, Valencia 46980, Spain. EM cristian.mattar@uv.es RI Soria Barres, Guillem/L-9462-2014; Sobrino, Jose/M-1585-2014; Julien, Yves/M-5224-2014; Mattar, Cristian/P-6711-2014; Jimenez-Munoz, Juan Carlos/K-2903-2015 OI Soria Barres, Guillem/0000-0002-3148-9238; Sobrino, Jose/0000-0003-3787-9373; Julien, Yves/0000-0001-5334-7137; Jimenez-Munoz, Juan Carlos/0000-0001-7562-4895 FU European Union (CEOP-AEGIS) [212921]; Ministerio de Economia y Competitividad (EODIX) [AYA2008-0595-C04-01]; CEOS-Spain [AYA2011-29334-C02-01]; Program U-INICIA VID [U-INICIA 4/0612]; Santander Fellowship-University of Chile for young scientist; Fondecyt-Initial [CONICYT/ref-11130359] FX We acknowledge funding from the European Union (CEOP-AEGIS, project FP7-ENV-2007-1 Proposal No. 212921) and the Ministerio de Economia y Competitividad (EODIX, project AYA2008-0595-C04-01; CEOS-Spain, project AYA2011-29334-C02-01. This work was also partially funded by Program U-INICIA VID 2012, grant U-INICIA 4/0612; Santander Fellowship-University of Chile for young scientist and Fondecyt-Initial (CONICYT/ref-11130359). NR 93 TC 12 Z9 12 U1 4 U2 49 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 MAY 5 PY 2014 VL 147 BP 23 EP 42 DI 10.1016/j.rse.2014.02.011 PG 20 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AH5QR UT WOS:000336186400003 ER PT J AU Gitelson, AA Peng, Y Huemmrich, KF AF Gitelson, Anatoly A. Peng, Yi Huemmrich, Karl F. TI Relationship between fraction of radiation absorbed by photosynthesizing maize and soybean canopies and NDVI from remotely sensed data taken at close range and from MODIS 250 m resolution data SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Absorbed photosynthetically active radiation; NDVI; Reflectance ID LEAF-AREA INDEX; PHOTOSYNTHETICALLY ACTIVE RADIATION; GROSS PRIMARY PRODUCTION; HIGHER-PLANT LEAVES; SPECTRAL REFLECTANCE; CHLOROPHYLL CONTENT; VEGETATION INDEXES; SOLAR-RADIATION; TRANSFER MODELS; CORN CANOPIES AB The fraction of incident photosynthetically active radiation absorbed by the photosynthesizing tissue in a canopy (fAPAR) is a key variable in the assessment of vegetation productivity. It also plays tremendous role in accurate retrieval of light use efficiency, which is essential for assessing vegetation health status. The main goal of this work was to study in detail relationships of fAPAR absorbed by photosynthetically active vegetation (fAPAR(green)) and Normalized Difference Vegetation Index (NDVI) for two crops with contrasting leaf structures (C3 vs. C4) and canopy architectures, using close range (6 m above the canopy) radiometric data and daily MODIS data taken during eight growing seasons over three irrigated and rainfed maize and soybean sites. Our specific goal was to understand differences in fAPAR(green)/NDVI relationship when crop canopy was almost vertically homogeneous (with respect to leaf area and leaf chlorophyll content), as in vegetative stage, and vertically heterogeneous as in reproduction stage. Firstly, we established fAPAR(green)/NDVI relationships for NDVI, taken at close range, and assessed noise equivalent of fAPAR(green) estimation by NDVI, and then we established relationships for NDVI retrieved from daily MODIS 250 m data. Daily MODIS data illuminated fine details of this relationship and detected effects of canopy heterogeneity on fAPAR(green)/NDVI relationship. In vegetative stage, the fAPAR/NDVI relationships for contrasting in leaf structures and canopy architectures crops were almost linear allowing accurate estimation of fAPAR(green) as it is below 0.7. However, very different fAPAR(green)/NDVI relationships in reproductive stages for both crops were observed, showing that canopy architecture and leaf structure greatly affect the relationship as leaf chlorophyll content changes and vertical distribution of chlorophyll content and green LAI inside the canopy becomes heterogeneous. We have found fine details of the fAPAR(green)/NDVI relationships with two types of hysteresis that prevent the use of a single relationship for fAPAR(green) estimation by NDVI over the whole growing season and suggested mechanisms for each type of hysteresis that should be further studied using radiative transfer models. (C) 2014 Elsevier Inc. All rights reserved. C1 [Gitelson, Anatoly A.; Peng, Yi] Univ NE Lincoln, CALMIT, Sch Nat Resources, Lincoln, NE 68588 USA. [Huemmrich, Karl F.] Univ MD Baltimore Cty, NASA, Goddard Space Flight Ctr, Joint Ctr Earth Syst Technol, Greenbelt, MD USA. RP Peng, Y (reprint author), Univ NE Lincoln, CALMIT, Sch Nat Resources, Lincoln, NE 68588 USA. EM agitelson2@unl.edu NR 58 TC 18 Z9 22 U1 3 U2 51 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 MAY 5 PY 2014 VL 147 BP 108 EP 120 DI 10.1016/j.rse.2014.02.014 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AH5QR UT WOS:000336186400010 ER PT J AU Garcia, RA Fearns, PRCS McKinna, LIW AF Garcia, Rodrigo A. Fearns, Peter R. C. S. McKinna, Lachlan I. W. TI Detecting trend and seasonal changes in bathymetry derived from HICO imagery: A case study of Shark Bay, Western Australia SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE HICO; Hyperspectral; Bathymetry; Change detection; Time series; Atmospheric correction; Tide correction; Shallow water inversion model; Propagating uncertainty; Geolocation accuracy ID GENERALIZED RATIO ASSUMPTION; SHALLOW-WATER BATHYMETRY; OCEAN COLOR; SEMIANALYTICAL MODEL; COASTAL ZONE; DEPTH; MISREGISTRATION; REFLECTANCE; RETRIEVAL; SEAGRASS AB The Hyperspectral Imager for the Coastal Ocean (HICO) aboard the International Space Station has offered for the first time a dedicated space-borne hyperspectral sensor specifically designed for remote sensing of the coastal environment. However, several processing steps are required to convert calibrated top-of-atmosphere radiances to the desired geophysical parameter(s). These steps add various amounts of uncertainty that can cumulatively render the geophysical parameter imprecise and potentially unusable if the objective is to analyze trends and/or seasonal variability. This research presented here has focused on: (1) atmospheric correction of HICO imagery; (2) retrieval of bathymetry using an improved implementation of a shallow water inversion algorithm; (3) propagation of uncertainty due to environmental noise through the bathymetry retrieval process; (4) issues relating to consistent geo-location of HICO imagery necessary for time series analysis, and; (5) tide height corrections of the retrieved bathymetric dataset The underlying question of whether a temporal change in depth is detectable above uncertainty is also addressed. To this end, nine HICO images spanning November 2011 to August 2012, over the Shark Bay World Heritage Area, Western Australia, were examined. The results presented indicate that precision of the bathymetric retrievals is dependent on the shallow water inversion algorithm used. Within this study, an average of 70% of pixels for the entire HICO-derived bathymetry dataset achieved a relative uncertainty of less than +/- 20%. A per-pixel t-test analysis between derived bathymetry images at successive timestamps revealed observable changes in depth to as low as 0.4 m. However, the present geolocation accuracy of HICO is relatively poor and needs further improvements before extensive time series analysis can be performed. (C) 2014 Elsevier Inc All rights reserved. C1 [Garcia, Rodrigo A.; Fearns, Peter R. C. S.; McKinna, Lachlan I. W.] Curtin Univ, Dept Imaging & Appl Phys, Remote Sensing & Satellite Res Grp, Perth, WA 6845, Australia. [McKinna, Lachlan I. W.] NASA, Ocean Ecol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Garcia, RA (reprint author), Curtin Univ, Dept Imaging & Appl Phys, Remote Sensing & Satellite Res Grp, GPO Box U1987, Perth, WA 6845, Australia. EM rodrigo.garcia@postgrad.curtin.edu.au NR 65 TC 12 Z9 12 U1 2 U2 30 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAY 5 PY 2014 VL 147 BP 186 EP 205 DI 10.1016/j.rse.2014.03.010 PG 20 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AH5QR UT WOS:000336186400016 ER PT J AU Smith, DD Chang, H Myneni, K Rosenberger, AT AF Smith, David D. Chang, H. Myneni, Krishna Rosenberger, A. T. TI Fast-light enhancement of an optical cavity by polarization mode coupling SO PHYSICAL REVIEW A LA English DT Article ID INDUCED TRANSPARENCY; RESONATOR; SYSTEM; GYROSCOPES AB We present an entirely linear all-optical method of cavity scale factor enhancement that relies on mode coupling between the orthogonal polarization modes of a single optical cavity, eliminating the necessity of using an atomic medium to produce the required anomalous dispersion, which decreases the dependence of the scale factor on temperature and increases signal-to-noise ratio by reducing absorption and nonlinear effects. The use of a single cavity results in common mode rejection of the noise and drift that would be present in a system of two coupled cavities. We show that the scale-factor-to-mode-width ratio is increased above unity for this system, and demonstrate tuning of the scale factor by (i) directly varying the polarization mode coupling via rotation of an intracavity half-wave plate, and (ii) coherent control of the cavity reflectance which is achieved simply by varying the incident polarization superposition. These tuning methods allow us to closely approach the critical anomalous dispersion condition and achieve unprecedented enhancements in scale factor and in the scale-factor-to-mode-width ratio. Based on these findings, we propose an adaptation of the traditional optical cavity gyroscope that takes advantage of polarization mode coupling to enhance the gyro scale factor, and demonstrate how the bandwidth of the scale factor enhancement for this gyroscope can be effectively broadened in comparison with fast-light gyroscopes based on atomic media. C1 [Smith, David D.] NASA, George C Marshall Space Flight Ctr, Space Syst Dept, Huntsville, AL 35812 USA. [Chang, H.] Ducommun Miltec, Huntsville, AL 35806 USA. [Myneni, Krishna] US Army AMRDEC, RDMR WDS WO, Redstone Arsenal, AL 35898 USA. [Rosenberger, A. T.] Oklahoma State Univ, Dept Phys, Stillwater, OK 74078 USA. RP Smith, DD (reprint author), NASA, George C Marshall Space Flight Ctr, Space Syst Dept, ES31, Huntsville, AL 35812 USA. FU NASA Office of Chief Technologist Game Changing Development Program; U. S. Army Aviation and Missile Research Development and Engineering Center (AMRDEC) Missile ST Program; Summer Research and Travel Program of the Oklahoma State University College of Arts and Sciences FX This work was sponsored by the NASA Office of Chief Technologist Game Changing Development Program and the U. S. Army Aviation and Missile Research Development and Engineering Center (AMRDEC) Missile S&T Program. The participation of ATR was sponsored by the Summer Research and Travel Program of the Oklahoma State University College of Arts and Sciences. NR 22 TC 15 Z9 15 U1 1 U2 16 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD MAY 5 PY 2014 VL 89 IS 5 AR 053804 DI 10.1103/PhysRevA.89.053804 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AH4LY UT WOS:000336100500008 ER PT J AU Wuchenich, DMR Mahrdt, C Sheard, BS Francis, SP Spero, RE Miller, J Mow-Lowry, CM Ward, RL Klipstein, WM Heinzel, G Danzmann, K McClelland, DE Shaddock, DA AF Wuchenich, Danielle M. R. Mahrdt, Christoph Sheard, Benjamin S. Francis, Samuel P. Spero, Robert E. Miller, John Mow-Lowry, Conor M. Ward, Robert L. Klipstein, William M. Heinzel, Gerhard Danzmann, Karsten McClelland, David E. Shaddock, Daniel A. TI Laser link acquisition demonstration for the GRACE Follow-On mission SO OPTICS EXPRESS LA English DT Article ID LTP INTERFEROMETER; COMMUNICATION; PHASEMETER; ALIGNMENT; SYSTEM AB We experimentally demonstrate an inter-satellite laser link acquisition scheme for GRACE Follow-On. In this strategy, dedicated acquisition sensors are not required-instead we use the photodetectors and signal processing hardware already required for science operation. To establish the laser link, a search over five degrees of freedom must be conducted (+/- 3 mrad in pitch/yaw for each laser beam, and +/- 1 GHz for the frequency difference between the two lasers). This search is combined with a FFT-based peak detection algorithm run on each satellite to find the heterodyne beat note resulting when the two beams are interfered. We experimentally demonstrate the two stages of our acquisition strategy: a +/- 3 mrad commissioning scan and a +/- 300 mu rad reacquisition scan. The commissioning scan enables each beam to be pointed at the other satellite to within 142 mu rad of its best alignment point with a frequency difference between lasers of less than 20 MHz. Scanning over the 4 alignment degrees of freedom in our commissioning scan takes 214 seconds, and when combined with sweeping the laser frequency difference at a rate of 88 kHz/s, the entire commissioning sequence completes within 6.3 hours. The reacquisition sequence takes 7 seconds to complete, and optimizes the alignment between beams to allow a smooth transition to differential wavefront sensing-based auto-alignment. (C) 2014 Optical Society of America C1 [Wuchenich, Danielle M. R.; Francis, Samuel P.; Miller, John; Mow-Lowry, Conor M.; Ward, Robert L.; McClelland, David E.; Shaddock, Daniel A.] Australian Natl Univ, Dept Quantum Sci, Ctr Gravitat Phys, Canberra, ACT 0200, Australia. [Mahrdt, Christoph; Sheard, Benjamin S.; Heinzel, Gerhard; Danzmann, Karsten] Leibniz Univ Hannover, Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Mahrdt, Christoph; Sheard, Benjamin S.; Heinzel, Gerhard; Danzmann, Karsten] Leibniz Univ Hannover, Inst Gravitat Phys, D-30167 Hannover, Germany. [Spero, Robert E.; Klipstein, William M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Wuchenich, DMR (reprint author), Australian Natl Univ, Dept Quantum Sci, Ctr Gravitat Phys, Canberra, ACT 0200, Australia. EM danielle.wuchenich@anu.edu.au RI McClelland, David/E-6765-2010; Mow-Lowry, Conor/F-8843-2015; Shaddock, Daniel/A-7534-2011; Ward, Robert/I-8032-2014 OI McClelland, David/0000-0001-6210-5842; Shaddock, Daniel/0000-0002-6885-3494; Ward, Robert/0000-0001-5503-5241 FU Australian Government; Australian Research Council; "Deutsche Forschungsgemeinschaft" (DFG) through the Cluster of Excellence QUEST (Centre for Quantum Engineering and Space-Time Research); National Aeronautics and Space Administration FX The authors gratefully acknowledge discussions and advice from Kirk McKenzie and Andrew Sutton. This work was supported in part under the Australian Government's Australian Space Research Programme, grants from the Australian Research Council, and by the "Deutsche Forschungsgemeinschaft" (DFG) through the Cluster of Excellence QUEST (Centre for Quantum Engineering and Space-Time Research). Some of the work described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 35 TC 6 Z9 6 U1 1 U2 22 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD MAY 5 PY 2014 VL 22 IS 9 BP 11351 EP 11366 DI 10.1364/OE.22.011351 PG 16 WC Optics SC Optics GA AH1TZ UT WOS:000335905300160 PM 24921832 ER PT J AU Collins, MJ Kirk, JP Pettit, J DeGaetano, AT McCown, MS Peterson, TC Means, TN Zhang, XB AF Collins, Mathias J. Kirk, Johnathan P. Pettit, Joshua DeGaetano, Arthur T. McCown, M. Sam Peterson, Thomas C. Means, Tiffany N. Zhang, Xuebin TI Annual floods in New England (USA) and Atlantic Canada: synoptic climatology and generating mechanisms SO PHYSICAL GEOGRAPHY LA English DT Article DE synoptic climatology; hydroclimatology; trends; floods; flood seasonality ID NORTHEASTERN UNITED-STATES; WINTER CLIMATE; TRENDS; PRECIPITATION; 20TH-CENTURY; VARIABILITY; MAGNITUDE; FREQUENCY; COAST; OSCILLATION AB New England and Atlantic Canada are characterized by mixed flood regimes that reflect different storm types, antecedent land surface conditions, and flood seasonality. Mixed flood regimes are known to complicate flood risk analyses, yet the synoptic climatology and precipitation mechanisms that generate annual floods in this region have not been described in detail. We analyzed a set of long-term annual flood records at climate-sensitive stream gauges across the region and classified the synoptic climatology of each annual flood, quantitatively describing the precipitation mechanisms, and characterize flood seasonality. We find that annual floods here are dominantly generated by Great Lakes-sourced storms and Coastal lows, known locally as 'nor'easters.' Great Lakes storms tend to be associated with lower magnitude annual floods (<75th percentile) and Coastal lows are more clearly associated with higher magnitude events (>75th percentile). Tropical cyclones account for few of all annual floods, including extreme events, despite causing some of the region's largest and most destructive floods. Late winter/early spring is when the greatest number of annual floods occur region wide, and rainfall is the dominant flood-producing mechanism. Rainfall in combination with snowmelt is also important. Both mechanisms are expected to be impacted by projected regional climate change. We find little evidence for associations between flood-producing synoptic storm types or precipitation mechanisms and large-scale atmospheric circulation indices or time periods, despite upward trends in New England annual flood magnitudes. To more completely investigate such associations, partial duration flood series that include more floods than just the largest of each year, and their associated synoptic climatologies and precipitation mechanisms, should be analyzed. C1 [Collins, Mathias J.] NOAA, Natl Marine Fisheries Serv, Gloucester, MA 01930 USA. [Kirk, Johnathan P.] Kent State Univ, Dept Geog, Kent, OH 44242 USA. [Pettit, Joshua] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [DeGaetano, Arthur T.] Cornell Univ, Dept Earth & Atmospher Sci, Ithaca, NY USA. [McCown, M. Sam; Peterson, Thomas C.] NOAA, Natl Climat Data Ctr, Asheville, NC USA. [Means, Tiffany N.] Baldwin Grp Inc, Asheville, NC USA. [Zhang, Xuebin] Environm Canada, Climate Res Div, Toronto, ON, Canada. RP Collins, MJ (reprint author), NOAA, Natl Marine Fisheries Serv, 55 Great Republ Dr, Gloucester, MA 01930 USA. EM mathias.collins@noaa.gov OI Collins, Mathias/0000-0003-4238-2038 FU Cornell University's Department of Earth and Atmospheric Sciences and Northeast Regional Climate Center; Environment Canada's Climate Research Division; NOAA Fisheries Office of Habitat Conservation; NOAA's National Climatic Data Center FX We thank Cornell University's Department of Earth and Atmospheric Sciences and Northeast Regional Climate Center, Environment Canada's Climate Research Division, NOAA Fisheries Office of Habitat Conservation, and NOAA's National Climatic Data Center for supporting this project. Numerous staff at Environment Canada and the United States Geological Survey were responsive to our data requests. William Armstrong and Zachary Zambreski provided data analysis support. We thank Associate Editor Brent Yarnal, Katherine Hirschboeck, and two anonymous referees for thorough reviews that improved the manuscript. NR 54 TC 10 Z9 10 U1 4 U2 30 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0272-3646 EI 1930-0557 J9 PHYS GEOGR JI Phys. Geogr. PD MAY 4 PY 2014 VL 35 IS 3 BP 195 EP 219 DI 10.1080/02723646.2014.888510 PG 25 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Physical Geography; Geology; Meteorology & Atmospheric Sciences GA AH1EN UT WOS:000335862700002 ER PT J AU Horta, LG Reaves, MC AF Horta, Lucas G. Reaves, Mercedes C. TI Evaluation of two crew module boilerplate tests using newly developed calibration metrics SO INTERNATIONAL JOURNAL OF CRASHWORTHINESS LA English DT Article DE capsule; test calibration; uncertainty analysis; water impact; model calibration ID VALIDATION METRICS AB The paper discusses an application of multi-dimensional calibration metrics to evaluate pressure data from water drop tests of the Max Launch Abort System crew module boilerplate. Specifically, three metrics are discussed: (1) a metric to assess the probability of enveloping the measured data with the model, (2) a multi-dimensional orthogonality metric to assess model adequacy between test and analysis, and (3) a prediction error metric to conduct sensor placement to minimise pressure prediction errors. Data from similar (nearly repeated) capsule drop tests show significant variability in the measured pressure responses. When compared to expected variability using model predictions, it is demonstrated that the measured variability cannot be explained by the model under the current uncertainty assumptions. C1 [Horta, Lucas G.; Reaves, Mercedes C.] NASA, Langley Res Ctr, Struct Dynam Branch, Hampton, VA 23665 USA. RP Horta, LG (reprint author), NASA, Langley Res Ctr, Struct Dynam Branch, Hampton, VA 23665 USA. EM lucas.g.horta@nasa.gov NR 23 TC 0 Z9 0 U1 0 U2 2 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1358-8265 EI 1754-2111 J9 INT J CRASHWORTHINES JI Int. J. Crashworthiness PD MAY 4 PY 2014 VL 19 IS 3 BP 264 EP 274 DI 10.1080/13588265.2014.883912 PG 11 WC Engineering, Manufacturing; Engineering, Mechanical SC Engineering GA AE3MD UT WOS:000333879700005 ER PT J AU Moore, RH Ziemba, LD Dutcher, D Beyersdorf, AJ Chan, K Crumeyrolle, S Raymond, TM Thornhill, KL Winstead, EL Anderson, BE AF Moore, Richard H. Ziemba, Luke D. Dutcher, Dabrina Beyersdorf, Andreas J. Chan, Kevin Crumeyrolle, Suzanne Raymond, Timothy M. Thornhill, Kenneth L. Winstead, Edward L. Anderson, Bruce E. TI Mapping the Operation of the Miniature Combustion Aerosol Standard (Mini-CAST) Soot Generator SO AEROSOL SCIENCE AND TECHNOLOGY LA English DT Article ID DIESEL EXHAUST PARTICLES; FISCHER-TROPSCH FUELS; HIGH-RESOLUTION; ORGANIC-CARBON; BLACK CARBON; PARTICULATE-EMISSIONS; HYGROSCOPIC GROWTH; CATALYTIC STRIPPER; MASS-SPECTROMETER; ACTIVATION AB The Jing Ltd. miniature combustion aerosol standard (Mini-CAST) soot generator is a portable, commercially available burner that is widely used for laboratory measurements of soot processes. While many studies have used the Mini-CAST to generate soot with known size, concentration, and organic carbon fraction under a single or few conditions, there has been no systematic study of the burner operation over a wide range of operating conditions. Here, we present a comprehensive characterization of the microphysical, chemical, morphological, and hygroscopic properties of Mini-CAST soot over the full range of oxidation air and mixing N-2 flow rates. Very fuel-rich and fuel-lean flame conditions are found to produce organic-dominated soot with mode diameters of 10-60nm, and the highest particle number concentrations are produced under fuel-rich conditions. The lowest organic fraction and largest diameter soot (70-130nm) occur under slightly fuel-lean conditions. Moving from fuel-rich to fuel-lean conditions also increases the O:C ratio of the soot coatings from similar to 0.05 to similar to 0.25, which causes a small fraction of the particles to act as cloud condensation nuclei near the Kelvin limit (kappa similar to 0-10(-3)). Comparison of these property ranges to those reported in the literature for aircraft and diesel engine soots indicates that the Mini-CAST soot is similar to real-world primary soot particles, which lends itself to a variety of process-based soot studies. The trends in soot properties uncovered here will guide selection of burner operating conditions to achieve optimum soot properties that are most relevant to such studies. Copyright 2014 American Association for Aerosol Research C1 [Moore, Richard H.; Crumeyrolle, Suzanne] NASA, Langley Res Ctr, Postdoctoral Program, Hampton, VA 30332 USA. [Moore, Richard H.; Ziemba, Luke D.; Beyersdorf, Andreas J.; Chan, Kevin; Crumeyrolle, Suzanne; Thornhill, Kenneth L.; Winstead, Edward L.; Anderson, Bruce E.] NASA, Langley Res Ctr, Hampton, VA 30332 USA. [Dutcher, Dabrina; Raymond, Timothy M.] Bucknell Univ, Dept Chem Engn, Lewisburg, PA 17837 USA. [Thornhill, Kenneth L.; Winstead, Edward L.] Sci Syst & Applicat Inc, Hampton, VA USA. RP Moore, RH (reprint author), NASA, Langley Res Ctr, 8 Lindbergh Way, Hampton, VA 30332 USA. EM richard.h.moore@nasa.gov FU NASA Fundamental Aeronautics and Fixed Wing Programs FX The authors thank the NASA Fundamental Aeronautics and Fixed Wing Programs for funding support. The CFD code was developed by A. Nenes (http://nenes.eas.gatech.edu/CFD). NR 55 TC 17 Z9 17 U1 3 U2 36 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0278-6826 EI 1521-7388 J9 AEROSOL SCI TECH JI Aerosol Sci. Technol. PD MAY 4 PY 2014 VL 48 IS 5 BP 467 EP 479 DI 10.1080/02786826.2014.890694 PG 13 WC Engineering, Chemical; Engineering, Mechanical; Environmental Sciences; Meteorology & Atmospheric Sciences SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AE3MO UT WOS:000333880800002 ER PT J AU Raatikainen, T Lin, JJ Cerully, KM Lathem, TL Moore, RH Nenes, A AF Raatikainen, Tomi Lin, Jack J. Cerully, Kate M. Lathem, Terry L. Moore, Richard H. Nenes, Athanasios TI CCN Data Interpretation Under Dynamic Operation Conditions SO AEROSOL SCIENCE AND TECHNOLOGY LA English DT Article ID SECONDARY ORGANIC AEROSOL; DROPLET GROWTH-KINETICS; ANALYSIS-A METHOD; ACTIVATION KINETICS; HYGROSCOPICITY; CHAMBER; SPECTRA; COUNTER AB We have developed a new numerical model for the non-steady-state operation of the Droplet Measurement Technologies (DMT) Cloud Condensation Nuclei (CCN) counter. The model simulates the Scanning Flow CCN Analysis (SFCA) instrument mode, where a wide supersaturation range is continuously scanned by cycling the flow rate over 20-120s. Model accuracy is verified using a broad set of data which include ammonium sulfate calibration data (under conditions of low CCN concentration) and airborne measurements where either the instrument pressure was not controlled or where exceptionally high CCN loadings were observed. It is shown here for the first time that small pressure and flow fluctuations can have a disproportionately large effect on the instrument supersaturation due to localized compressive/expansive heating and cooling. The model shows that, for fast scan times, these effects can explain the observed shape of the SFCA supersaturation-flow calibration curve and transients in the outlet droplet sizes. The extent of supersaturation depletion from the presence of CCN during SFCA operation is also examined; we found that depletion effects can be neglected below 4000cm(-3) for CCN number. Copyright 2014 American Association for Aerosol Research C1 [Raatikainen, Tomi; Lin, Jack J.; Lathem, Terry L.; Nenes, Athanasios] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Raatikainen, Tomi] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Cerully, Kate M.; Moore, Richard H.; Nenes, Athanasios] Georgia Inst Technol, Sch Chem & Biomol Engn, Atlanta, GA 30332 USA. [Moore, Richard H.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Nenes, A (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, 311 Ferst Dr, Atlanta, GA 30332 USA. EM nenes@eas.gatech.edu RI Raatikainen, Tomi/C-5410-2014 FU Finnish Cultural Foundation; DOE STTS grant; DOE GCEP Graduate Research Environmental and Global Change Education Fellowships; Electrical Power Research Institute; NSF-CAREER award; NOAA; NSF; Georgia Tech; NASA FX The authors are grateful for the funding from Finnish Cultural Foundation, a DOE STTS grant, DOE GCEP Graduate Research Environmental and Global Change Education Fellowships, the Electrical Power Research Institute, a NSF-CAREER award, and NOAA, NSF, Georgia Tech, and NASA grants is acknowledged. NR 19 TC 3 Z9 3 U1 1 U2 19 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0278-6826 EI 1521-7388 J9 AEROSOL SCI TECH JI Aerosol Sci. Technol. PD MAY 4 PY 2014 VL 48 IS 5 BP 552 EP 561 DI 10.1080/02786826.2014.899429 PG 10 WC Engineering, Chemical; Engineering, Mechanical; Environmental Sciences; Meteorology & Atmospheric Sciences SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AE3MO UT WOS:000333880800010 ER PT J AU Russell, C Ding, J Nunes, A Lawless, K AF Russell, Carolyn Ding, Jeff Nunes, Arthur Lawless, Kirby TI Welding Technology Takes Flight with NASA SO WELDING JOURNAL LA English DT Editorial Material C1 [Russell, Carolyn; Lawless, Kirby] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Ding, Jeff] NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Welding & Mfg Team, Huntsville, AL 35812 USA. [Nunes, Arthur] NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Huntsville, AL 35812 USA. RP Russell, C (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM carolyn.k.russell@nasa.gov; robert.j.ding@nasa.gov; arthurc.nunes@nasa.gov; kirby.g.lawless@nasa.gov NR 3 TC 0 Z9 0 U1 0 U2 0 PU AMER WELDING SOC PI MIAMI PA 550 N W LEJEUNE RD, MIAMI, FL 33126 USA SN 0043-2296 J9 WELD J JI Weld. J. PD MAY PY 2014 VL 93 IS 5 BP 38 EP 43 PG 6 WC Metallurgy & Metallurgical Engineering SC Metallurgy & Metallurgical Engineering GA AW5QR UT WOS:000346329700005 ER PT J AU Miller, RA Kuczmarski, MA AF Miller, Robert A. Kuczmarski, Maria A. TI Burner Rig for Small Particle Erosion Testing of Thermal Barrier Coatings SO JOURNAL OF TESTING AND EVALUATION LA English DT Article DE thermal barrier coatings; erosion; burner rig; computational fluid dynamics ID TEMPERATURE; SIMULATION AB The development of a high-temperature laboratory test to evaluate the erosion resistance of new turbine-blade thermal barrier coatings (TBC) for aircraft gas turbine engines is described. The focus is on improvements to a previously reported design, specifically: (1) larger duct and nozzle diameters leading to a larger and more uniform wear pattern; (2) incorporation of a new auger-style feeder for precise feeding of fine particles at low flow rates; (3) an aperture after the duct to limit the erosive damage at the edges of button specimens; (4) bag filters for particle feed rate measurements. The results of both extensive computational fluid dynamics (CFD) modeling and experiments concentrating on laboratory specimens fabricated from turbine-blade superalloys were used to demonstrate the validity of the test results to meaningfully evaluate the performance of new coating compositions in representative erosive environments, and to help understand damage mechanisms under such conditions. Two specimen geometries were tested in the improved rig using Mach 0.5 jets: "teardrop" burner bar and button specimens. Both types of specimens had electron beam-physical vapor deposition (EB-PVD) prepared ceramic layers of either ZrO2-Y2O3 (7YSZ) or ZrO2-Y2O3-Gd2O3-Yb2O3 (ZYGdYb) applied over PtAl bond coats using various processing parameters or interface treatments. Specimen temperatures for this study were either 980 degrees C (1800 degrees F) or 1090 degrees C (2000 degrees F). C1 [Miller, Robert A.; Kuczmarski, Maria A.] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA. RP Miller, RA (reprint author), NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA. FU NASA Fundamental Aeronautics Program, Subsonic Rotary Wing Project FX This work is sponsored by the NASA Fundamental Aeronautics Program, Subsonic Rotary Wing Project. NR 36 TC 0 Z9 0 U1 5 U2 16 PU AMER SOC TESTING MATERIALS PI W CONSHOHOCKEN PA 100 BARR HARBOR DR, W CONSHOHOCKEN, PA 19428-2959 USA SN 0090-3973 EI 1945-7553 J9 J TEST EVAL JI J. Test. Eval. PD MAY PY 2014 VL 42 IS 3 BP 648 EP 658 DI 10.1520/JTE20120303 PG 11 WC Materials Science, Characterization & Testing SC Materials Science GA AU5JU UT WOS:000345643800007 ER PT J AU Fish, CS Swenson, CM Crowley, G Barjatya, A Neilsen, T Gunther, J Azeem, I Pilinski, M Wilder, R Allen, D Anderson, M Bingham, B Bradford, K Burr, S Burt, R Byers, B Cook, J Davis, K Frazier, C Grover, S Hansen, G Jensen, S LeBaron, R Martineau, J Miller, J Nelsen, J Nelson, W Patterson, P Stromberg, E Tran, J Wassom, S Weston, C Whiteley, M Young, Q Petersen, J Schaire, S Davis, CR Bokaie, M Fullmer, R Baktur, R Sojka, J Cousins, M AF Fish, C. S. Swenson, C. M. Crowley, G. Barjatya, A. Neilsen, T. Gunther, J. Azeem, I. Pilinski, M. Wilder, R. Allen, D. Anderson, M. Bingham, B. Bradford, K. Burr, S. Burt, R. Byers, B. Cook, J. Davis, K. Frazier, C. Grover, S. Hansen, G. Jensen, S. LeBaron, R. Martineau, J. Miller, J. Nelsen, J. Nelson, W. Patterson, P. Stromberg, E. Tran, J. Wassom, S. Weston, C. Whiteley, M. Young, Q. Petersen, J. Schaire, S. Davis, C. R. Bokaie, M. Fullmer, R. Baktur, R. Sojka, J. Cousins, M. TI Design, Development, Implementation, and On-orbit Performance of the Dynamic Ionosphere CubeSat Experiment Mission SO SPACE SCIENCE REVIEWS LA English DT Review DE DICE; CubeSats; Ionospheric diagnostics; DC and AC electric fields; Plasma density; IDA4D; AIME; Constellation; Magnetometer; Langmuir probe ID TOTAL ELECTRON-CONTENT; LATITUDES AB Funded by the NSF CubeSat and NASA ELaNa programs, the Dynamic Ionosphere CubeSat Experiment (DICE) mission consists of two 1.5U CubeSats which were launched into an eccentric low Earth orbit on October 28, 2011. Each identical spacecraft carries two Langmuir probes to measure ionospheric in-situ plasma densities, electric field probes to measure in-situ DC and AC electric fields, and a science grade magnetometer to measure in-situ DC and AC magnetic fields. Given the tight integration of these multiple sensors with the CubeSat platforms, each of the DICE spacecraft is effectively a "sensor-sat" capable of comprehensive ionospheric diagnostics. The use of two identical sensor-sats at slightly different orbiting velocities in nearly identical orbits permits the de-convolution of spatial and temporal ambiguities in the observations of the ionosphere from a moving platform. In addition to demonstrating nanosat-based constellation science, the DICE mission is advancing a number of groundbreaking CubeSat technologies including miniaturized mechanisms and high-speed downlink communications. C1 [Fish, C. S.] Utah State Univ, Res Fdn, Space Dynam Lab, North Logan, UT 84341 USA. [Fish, C. S.] Utah State Univ, Ctr Space Engn, Logan, UT 84322 USA. [Fish, C. S.] Virginia Tech, Elect & Comp Engn Dept, Blacksburg, VA USA. [Swenson, C. M.; Gunther, J.; Fullmer, R.; Baktur, R.; Sojka, J.] Utah State Univ, Logan, UT 84322 USA. [Crowley, G.; Azeem, I.; Pilinski, M.; Wilder, R.] Atmospher & Space Technol Res Associates LLC, Boulder, CO USA. [Barjatya, A.] Embry Riddle Aeronaut Univ, Daytona Beach, FL USA. [Neilsen, T.; Allen, D.; Anderson, M.; Bingham, B.; Bradford, K.; Burr, S.; Burt, R.; Byers, B.; Cook, J.; Davis, K.; Frazier, C.; Grover, S.; Hansen, G.; Jensen, S.; LeBaron, R.; Martineau, J.; Miller, J.; Nelsen, J.; Nelson, W.; Patterson, P.; Stromberg, E.; Tran, J.; Wassom, S.; Weston, C.; Whiteley, M.; Young, Q.] Space Dynam Lab, N Logan, UT USA. [Petersen, J.] L 3 Commun, Salt Lake City, UT USA. [Schaire, S.] NASA, Wallops Flight Facil, Wallops Isl, VA USA. [Davis, C. R.] LJT & Associates, Columbia, MD USA. [Bokaie, M.] TiNi Aerosp, San Rafael, CA USA. [Cousins, M.] SRI Int, Menlo Pk, CA 94025 USA. RP Fish, CS (reprint author), Utah State Univ, Res Fdn, Space Dynam Lab, 1695 North Res Pk Way, North Logan, UT 84341 USA. EM chad.fish@sdl.usu.edu FU NSF [ATM-0838059, AGS-1212381, AGS-1255782] FX The authors gratefully acknowledge funding provided by NSF (grant numbers# ATM-0838059, AGS-1212381, AGS-1255782) and to the NASA ELaNa III group for launch services. The team would also like to gratefully acknowledge the countless hours of dedicated and passionate effort from the students on the DICE program. They indeed rose to the challenge. Without their energy and consistency, DICE would not have become a reality. NR 27 TC 5 Z9 5 U1 0 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD MAY PY 2014 VL 181 IS 1-4 BP 61 EP 120 DI 10.1007/s11214-014-0034-x PG 60 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2CT UT WOS:000335929000002 ER PT J AU Domingue, DL Chapman, CR Killen, RM Zurbuchen, TH Gilbert, JA Sarantos, M Benna, M Slavin, JA Schriver, D Travnicek, PM Orlando, TM Sprague, AL Blewett, DT Gillis-Davis, JJ Feldman, WC Lawrence, DJ Ho, GC Ebel, DS Nittler, LR Vilas, F Pieters, CM Solomon, SC Johnson, CL Winslow, RM Helbert, J Peplowski, PN Weider, SZ Mouawad, N Izenberg, NR McClintock, WE AF Domingue, Deborah L. Chapman, Clark R. Killen, Rosemary M. Zurbuchen, Thomas H. Gilbert, Jason A. Sarantos, Menelaos Benna, Mehdi Slavin, James A. Schriver, David Travnicek, Pavel M. Orlando, Thomas M. Sprague, Ann L. Blewett, David T. Gillis-Davis, Jeffrey J. Feldman, William C. Lawrence, David J. Ho, George C. Ebel, Denton S. Nittler, Larry R. Vilas, Faith Pieters, Carle M. Solomon, Sean C. Johnson, Catherine L. Winslow, Reka M. Helbert, Joern Peplowski, Patrick N. Weider, Shoshana Z. Mouawad, Nelly Izenberg, Noam R. McClintock, William E. TI Mercury's Weather-Beaten Surface: Understanding Mercury in the Context of Lunar and Asteroidal Space Weathering Studies SO SPACE SCIENCE REVIEWS LA English DT Review DE Mercury (planet); Space weathering; Surface processes; Exosphere; Surface composition; Space environment ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; LATE HEAVY BOMBARDMENT; 1ST MESSENGER FLYBY; ELECTRON-STIMULATED DESORPTION; IRON-SILICATE FRACTIONATION; MINERAL ABSORPTION FEATURES; ION IRRADIATION EXPERIMENTS; GAMMA-RAY SPECTROMETER; SOLAR-WIND BOMBARDMENT; NEAR-EARTH ASTEROIDS AB Mercury's regolith, derived from the crustal bedrock, has been altered by a set of space weathering processes. Before we can interpret crustal composition, it is necessary to understand the nature of these surface alterations. The processes that space weather the surface are the same as those that form Mercury's exosphere (micrometeoroid flux and solar wind interactions) and are moderated by the local space environment and the presence of a global magnetic field. To comprehend how space weathering acts on Mercury's regolith, an understanding is needed of how contributing processes act as an interactive system. As no direct information (e.g., from returned samples) is available about how the system of space weathering affects Mercury's regolith, we use as a basis for comparison the current understanding of these same processes on lunar and asteroidal regoliths as well as laboratory simulations. These comparisons suggest that Mercury's regolith is overturned more frequently (though the characteristic surface time for a grain is unknown even relative to the lunar case), more than an order of magnitude more melt and vapor per unit time and unit area is produced by impact processes than on the Moon (creating a higher glass content via grain coatings and agglutinates), the degree of surface irradiation is comparable to or greater than that on the Moon, and photon irradiation is up to an order of magnitude greater (creating amorphous grain rims, chemically reducing the upper layers of grains to produce nanometer-scale particles of metallic iron, and depleting surface grains in volatile elements and alkali metals). The processes that chemically reduce the surface and produce nanometer-scale particles on Mercury are suggested to be more effective than similar processes on the Moon. Estimated abundances of nanometer-scale particles can account for Mercury's dark surface relative to that of the Moon without requiring macroscopic grains of opaque minerals. The presence of nanometer-scale particles may also account for Mercury's relatively featureless visible-near-infrared reflectance spectra. Characteristics of material returned from asteroid 25143 Itokawa demonstrate that this nanometer-scale material need not be pure iron, raising the possibility that the nanometer-scale material on Mercury may have a composition different from iron metal [such as (Fe,Mg)S]. The expected depletion of volatiles and particularly alkali metals from solar-wind interaction processes are inconsistent with the detection of sodium, potassium, and sulfur within the regolith. One plausible explanation invokes a larger fine fraction (grain size < 45 mu m) and more radiation-damaged grains than in the lunar surface material to create a regolith that is a more efficient reservoir for these volatiles. By this view the volatile elements detected are present not only within the grain structures, but also as adsorbates within the regolith and deposits on the surfaces of the regolith grains. The comparisons with findings from the Moon and asteroids provide a basis for predicting how compositional modifications induced by space weathering have affected Mercury's surface composition. C1 [Domingue, Deborah L.; Feldman, William C.; Vilas, Faith; Johnson, Catherine L.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Chapman, Clark R.] Southwest Res Inst, Boulder, CO 80302 USA. [Killen, Rosemary M.; Benna, Mehdi] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Zurbuchen, Thomas H.; Gilbert, Jason A.; Slavin, James A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Sarantos, Menelaos] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Schriver, David] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Travnicek, Pavel M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 90704 USA. [Orlando, Thomas M.] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA. [Orlando, Thomas M.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Sprague, Ann L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Blewett, David T.; Lawrence, David J.; Ho, George C.; Peplowski, Patrick N.; Izenberg, Noam R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Gillis-Davis, Jeffrey J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Ebel, Denton S.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, Div Phys Sci, York, NY 10023 USA. [Nittler, Larry R.; Solomon, Sean C.; Weider, Shoshana Z.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Pieters, Carle M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Johnson, Catherine L.; Winslow, Reka M.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V6T 1Z4, Canada. [Helbert, Joern] DLR, Inst Planetary Res, D-12489 Berlin, Germany. [Mouawad, Nelly] Lebanese Amer Univ, Dept Nat Sci, Beirut, Lebanon. [McClintock, William E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. RP Domingue, DL (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA. EM domingue@psi.edu RI Slavin, James/H-3170-2012; Blewett, David/I-4904-2012; Izenberg, Noam/F-3952-2015; Travnicek, Pavel/G-8608-2014; Ho, George/G-3650-2015; Peplowski, Patrick/I-7254-2012; Lawrence, David/E-7463-2015; Benna, Mehdi/F-3489-2012; Gilbert, Jason/I-9020-2012; OI Slavin, James/0000-0002-9206-724X; Blewett, David/0000-0002-9241-6358; Izenberg, Noam/0000-0003-1629-6478; Ho, George/0000-0003-1093-2066; Peplowski, Patrick/0000-0001-7154-8143; Lawrence, David/0000-0002-7696-6667; Gilbert, Jason/0000-0002-3182-7014; Weider, Shoshana/0000-0003-1034-909X; Helbert, Jorn/0000-0001-5346-9505 FU NASA [NASW-00002, NAS5-97271]; NASA MESSENGER [NNX08AN29G, NNX07AR62GO, NNX07AR61G, NNX07AR78G] FX The authors deeply appreciate the efforts and dedication of the MESSENGER mission operations, engineering, and instrument teams, without whom the scientific successes of the MESSENGER mission would not have been possible. The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory. Contributions by D. T. B., D. S., M. B, and R. K. are made possible by grants from the NASA MESSENGER Participating Scientist Program (NNX08AN29G, NNX07AR62GO, NNX07AR61G, and NNX07AR78G, respectively). The authors also thank T. B. McCord and an anonymous reviewer for their comments on an earlier version of this manuscript. NR 454 TC 23 Z9 23 U1 4 U2 27 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD MAY PY 2014 VL 181 IS 1-4 BP 121 EP 214 DI 10.1007/s11214-014-0039-5 PG 94 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2CT UT WOS:000335929000003 ER PT J AU Anderson, GE Gaensler, BM Kaplan, DL Slane, PO Muno, MP Posselt, B Hong, J Murray, SS Steeghs, DTH Brogan, CL Drake, JJ Farrell, SA Benjamin, RA Chakrabarty, D Drew, JE Finley, JP Grindlay, JE Lazio, TJW Lee, JC Mauerhan, JC van Kerkwijk, MH AF Anderson, Gemma E. Gaensler, B. M. Kaplan, David L. Slane, Patrick O. Muno, Michael P. Posselt, Bettina Hong, Jaesub Murray, Stephen S. Steeghs, Danny T. H. Brogan, Crystal L. Drake, Jeremy J. Farrell, Sean A. Benjamin, Robert A. Chakrabarty, Deepto Drew, Janet E. Finley, John P. Grindlay, Jonathan E. Lazio, T. Joseph W. Lee, Julia C. Mauerhan, Jon C. van Kerkwijk, Marten H. TI CHASING THE IDENTIFICATION OF ASCA GALACTIC OBJECTS (ChIcAGO): AN X-RAY SURVEY OF UNIDENTIFIED SOURCES IN THE GALACTIC PLANE. I. SOURCE SAMPLE AND INITIAL RESULTS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE surveys; X-rays: binaries; X-rays: galaxies; X-rays: general; X-rays: stars ID XMM-NEWTON OBSERVATIONS; H-II-REGIONS; PULSAR WIND NEBULA; ALL-SKY SURVEY; SUPERNOVA REMNANT G349.7+0.2; MASSIVE STAR-FORMATION; MAIN-SEQUENCE STARS; M IR-EXCESS; SOURCE CATALOG; INFRARED COUNTERPART AB We present the Chasing the Identification of ASCA Galactic Objects (ChIcAGO) survey, which is designed to identify the unknown X-ray sources discovered during the ASCA Galactic Plane Survey (AGPS). Little is known about most of the AGPS sources, especially those that emit primarily in hard X-rays (2-10 keV) within the F-x similar to 10(-13) to 10(-11) erg cm(-2) s(-1) X-ray flux range. In ChIcAGO, the subarcsecond localization capabilities of Chandra have been combined with a detailed multiwavelength follow-up program, with the ultimate goal of classifying the >100 unidentified sources in the AGPS. Overall to date, 93 unidentified AGPS sources have been observed with Chandra as part of the ChIcAGO survey. A total of 253 X-ray point sources have been detected in these Chandra observations within 3' of the original ASCA positions. We have identified infrared and optical counterparts to the majority of these sources, using both new observations and catalogs from existing Galactic plane surveys. X-ray and infrared population statistics for the X-ray point sources detected in the Chandra observations reveal that the primary populations of Galactic plane X-ray sources that emit in the F-x similar to 10(-13) to 10(-11) erg cm(-2) s(-1) flux range are active stellar coronae, massive stars with strong stellar winds that are possibly in colliding wind binaries, X-ray binaries, and magnetars. There is also another primary population that is still unidentified but, on the basis of its X-ray and infrared properties, likely comprises partly Galactic sources and partly active galactic nuclei. C1 [Anderson, Gemma E.; Gaensler, B. M.; Farrell, Sean A.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Kaplan, David L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Slane, Patrick O.; Hong, Jaesub; Drake, Jeremy J.; Grindlay, Jonathan E.; Lee, Julia C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Muno, Michael P.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Posselt, Bettina] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Steeghs, Danny T. H.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Brogan, Crystal L.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Benjamin, Robert A.] Univ Wisconsin, Dept Phys, Whitewater, WI 53190 USA. [Chakrabarty, Deepto] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Chakrabarty, Deepto] MIT, Dept Phys, Cambridge, MA 02139 USA. [Drew, Janet E.] Univ Hertfordshire, STRI, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Finley, John P.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Lazio, T. Joseph W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mauerhan, Jon C.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [van Kerkwijk, Marten H.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Anderson, GE (reprint author), Univ Oxford, Dept Phys, Denys Wilkinson Bldg, Oxford OX1 3RH, England. EM gemma.anderson@astro.ox.ac.uk RI Lee, Julia/G-2381-2015; OI Lee, Julia/0000-0002-7336-3588; Anderson, Gemma/0000-0001-6544-8007; Posselt, Bettina/0000-0003-2317-9747; Gaensler, Bryan/0000-0002-3382-9558; Drew, Janet/0000-0003-1192-7082; Kaplan, David/0000-0001-6295-2881 FU Australian Postgraduate Award; Australian Laureate Fellowship through ARC [FL100100114]; NASA [NAS8-03060, NAS8-39073, GO90155X]; STFC Advanced Fellowship; Commonwealth of Australia under the International Science Linkages program; Commonwealth of Australia; Australian Research Council; Science Foundation for Physics within the University of Sydney; NFS FX G.E.A. acknowledges the support of an Australian Postgraduate Award. B.M.G. acknowledges the support of an Australian Laureate Fellowship through ARC grant FL100100114. P.O.S. acknowledges partial support from NASA contract NAS8-03060. D.T.H.S. acknowledges a STFC Advanced Fellowship. J.J.D. was supported by NASA contract NAS8-39073 to the Chandra X-ray Center (CXC). Support for this work was also provided by NASA through Chandra award number GO90155X issued by the CXC, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA. The access to major research facilities program is supported by the Commonwealth of Australia under the International Science Linkages program. This research makes use of data obtained with the Chandra X-ray Observatory and software provided by the CXC in the application packages CIAO. The ATCA is part of the Australia Telescope, funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The MOST is operated with the support of the Australian Research Council and the Science Foundation for Physics within the University of Sydney. Observing time on the 6.5 m Baade Magellan Telescope, located at Las Campanas Observatory, was allocated through the Harvard-Smithsonian Center for Astrophysics and the Massachusetts Institute of Technology. 2MASS is a joint project of the University of Massachusetts and the IPAC/Caltech, funded by NASA and the NFS. GLIMPSE survey data are part of the Spitzer Legacy Program. The Spitzer Space Telescope is operated by JPL/Caltech under a contract with NASA. This research has made use of NASA's Astrophysics Data System. NR 189 TC 2 Z9 2 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2014 VL 212 IS 1 DI 10.1088/0067-0049/212/1/13 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL6HG UT WOS:000339232600013 ER PT J AU Ashby, MLN Stanford, SA Brodwin, M Gonzalez, AH Martinez-Manso, J Bartlett, JG Benson, BA Bleem, LE Crawford, TM Dey, A Dressler, A Eisenhardt, PRM Galametz, A Jannuzi, BT Marrone, DP Mei, S Muzzin, A Pacaud, F Pierre, M Stern, D Vieira, JD AF Ashby, M. L. N. Stanford, S. A. Brodwin, M. Gonzalez, A. H. Martinez-Manso, J. Bartlett, J. G. Benson, B. A. Bleem, L. E. Crawford, T. M. Dey, A. Dressler, A. Eisenhardt, P. R. M. Galametz, A. Jannuzi, B. T. Marrone, D. P. Mei, S. Muzzin, A. Pacaud, F. Pierre, M. Stern, D. Vieira, J. D. TI THE SPITZER SOUTH POLE TELESCOPE DEEP FIELD: SURVEY DESIGN AND INFRARED ARRAY CAMERA CATALOGS (vol 209, 16, 2013) SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Correction C1 [Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Gonzalez, A. H.; Martinez-Manso, J.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Bartlett, J. G.] Univ Paris Diderot, CEA IRFU, Observ Paris, Sorbonne Paris Cite,CNRS IN2P3, F-75205 Paris 13, France. [Benson, B. A.; Bleem, L. E.; Crawford, T. M.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Crawford, T. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Dey, A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Dressler, A.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Eisenhardt, P. R. M.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Galametz, A.] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Jannuzi, B. T.; Marrone, D. P.] Univ Arizona, Dept Astron, Tucson, AZ 85719 USA. [Jannuzi, B. T.; Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA. [Mei, S.] Observ Paris, GEPI, Sect Meudon, F-92190 Meudon, France. [Mei, S.] Univ Paris Denis Diderot, F-75205 Paris 13, France. [Mei, S.] Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Muzzin, A.] Leiden Univ, Leiden Observ, NL-9513 RA Leiden, Netherlands. [Pacaud, F.] Argelander Inst Astron, D-53121 Bonn, Germany. [Pierre, M.] AIM IRFU DSM CEA, Serv Astrophys, F-91190 Gif Sur Yvette, France. [Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. RP Ashby, MLN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mashby@cfa.harvard.edu NR 1 TC 2 Z9 2 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2014 VL 212 IS 1 AR 16 DI 10.1088/0067-0049/212/1/16 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL6HG UT WOS:000339232600016 ER PT J AU Mandelbaum, R Rowe, B Bosch, J Chang, C Courbin, F Gill, M Jarvis, M Kannawadi, A Kacprzak, T Lackner, C Leauthaud, A Miyatake, H Nakajima, R Rhodes, J Simet, M Zuntz, J Armstrong, B Bridle, S Coupon, J Dietrich, JP Gentile, M Heymans, C Jurling, AS Kent, SM Kirkby, D Margala, D Massey, R Melchior, P Peterson, J Roodman, A Schrabback, T AF Mandelbaum, Rachel Rowe, Barnaby Bosch, James Chang, Chihway Courbin, Frederic Gill, Mandeep Jarvis, Mike Kannawadi, Arun Kacprzak, Tomasz Lackner, Claire Leauthaud, Alexie Miyatake, Hironao Nakajima, Reiko Rhodes, Jason Simet, Melanie Zuntz, Joe Armstrong, Bob Bridle, Sarah Coupon, Jean Dietrich, Jorg P. Gentile, Marc Heymans, Catherine Jurling, Alden S. Kent, Stephen M. Kirkby, David Margala, Daniel Massey, Richard Melchior, Peter Peterson, John Roodman, Aaron Schrabback, Tim TI THE THIRD GRAVITATIONAL LENSING ACCURACY TESTING (GREAT3) CHALLENGE HANDBOOK SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE gravitational lensing: weak; methods: data analysis; methods: statistical; techniques: image processing ID HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; IMAGE-ANALYSIS COMPETITION; COSMIC SHEAR MEASUREMENT; POINT-SPREAD FUNCTION; ATMOSPHERIC-TURBULENCE; ADVANCED CAMERA; DARK-MATTER; SHAPE MEASUREMENTS; POLAR SHAPELETS AB The GRavitational lEnsing Accuracy Testing 3 (GREAT3) challenge is the third in a series of image analysis challenges, with a goal of testing and facilitating the development of methods for analyzing astronomical images that will be used to measure weak gravitational lensing. This measurement requires extremely precise estimation of very small galaxy shape distortions, in the presence of far larger intrinsic galaxy shapes and distortions due to the blurring kernel caused by the atmosphere, telescope optics, and instrumental effects. The GREAT3 challenge is posed to the astronomy, machine learning, and statistics communities, and includes tests of three specific effects that are of immediate relevance to upcoming weak lensing surveys, two of which have never been tested in a community challenge before. These effects include many novel aspects including realistically complex galaxy models based on high-resolution imaging from space; a spatially varying, physically motivated blurring kernel; and a combination of multiple different exposures. To facilitate entry by people new to the field, and for use as a diagnostic tool, the simulation software for the challenge is publicly available, though the exact parameters used for the challenge are blinded. Sample scripts to analyze the challenge data using existing methods will also be provided. C1 [Mandelbaum, Rachel; Kannawadi, Arun; Simet, Melanie] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Rowe, Barnaby; Kacprzak, Tomasz] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Rowe, Barnaby; Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bosch, James; Miyatake, Hironao] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Chang, Chihway; Gill, Mandeep; Roodman, Aaron] Stanford Univ, KIPAC, Stanford, CA 94309 USA. [Courbin, Frederic; Gentile, Marc] EPFL, Astrophys Lab, Observ Sauverny, CH-1290 Versoix, Switzerland. [Jarvis, Mike; Armstrong, Bob] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Lackner, Claire; Leauthaud, Alexie] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba, Japan. [Nakajima, Reiko; Schrabback, Tim] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Rhodes, Jason] CALTECH, Pasadena, CA 91125 USA. [Zuntz, Joe; Bridle, Sarah] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Coupon, Jean] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Dietrich, Jorg P.] Univ Sternwarte Munchen, D-81679 Munich, Germany. [Dietrich, Jorg P.] Excellence Cluster Universe, D-85748 Munich, Germany. [Heymans, Catherine] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Jurling, Alden S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jurling, Alden S.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14618 USA. [Kent, Stephen M.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Kirkby, David; Margala, Daniel] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Massey, Richard] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Melchior, Peter] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Melchior, Peter] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Peterson, John] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. RP Mandelbaum, R (reprint author), Carnegie Mellon Univ, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA. RI Mandelbaum, Rachel/N-8955-2014; Simet, Melanie/A-3415-2016; EPFL, Physics/O-6514-2016; OI Mandelbaum, Rachel/0000-0003-2271-1527; Simet, Melanie/0000-0001-8823-8926; Kirkby, David/0000-0002-8828-5463; Dietrich, Jorg/0000-0002-8134-9591; Rowe, Barnaby/0000-0002-7042-9174 FU National Science Foundation [PHYS-1066293]; NASA via the Strategic University Research Partnership (SURP) Program of the Jet Propulsion Laboratory, California Institute of Technology; IST Programme of the European Community under the PASCAL2 Network of Excellence [IST-2007-216886]; NASA through Space Telescope Science Institute; NASA [NAS5-26555]; European Research Council [240672, 240185]; JSPS Postdoctoral Fellowships for Research Abroad; Swiss National Science Foundation (SNSF); LLC [De-AC02-07CH11359]; United States Department of Energy; [HST-AR-12857.01-A] FX The authors of this work benefited greatly from discussions with Christopher Hirata, Gary Bernstein, Lance Miller, and Erin Sheldon; the WFIRST project office, including David Content; the Euclid Consortium; and the LSST imSim team, including En-Hsin Peng; and Peter Freeman. We thank the PASCAL-2 network for its sponsorship of the challenge. This work was supported in part by the National Science Foundation under grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics.; This project was supported in part by NASA via the Strategic University Research Partnership (SURP) Program of the Jet Propulsion Laboratory, California Institute of Technology; and by the IST Programme of the European Community, under the PASCAL2 Network of Excellence, IST-2007-216886. This article only reflects the authors' views.; R.M. was supported in part by program HST-AR-12857.01-A, 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. B.R. and S.B. acknowledge support from the European Research Council in the form of a Starting Grant with number 240672. H.M. acknowledges support from JSPS Postdoctoral Fellowships for Research Abroad. C.H. acknowledges support from the European Research Council under the EC FP7 grant number 240185. F.C. and M.G. are supported by the Swiss National Science Foundation (SNSF).; Center for Particle Astrophysics, Fermi National Accelerator Laboratory is operated by Fermi Research Alliance, LLC under contract No. De-AC02-07CH11359 with the United States Department of Energy. NR 100 TC 37 Z9 37 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2014 VL 212 IS 1 AR 5 DI 10.1088/0067-0049/212/1/5 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL6HG UT WOS:000339232600005 ER PT J AU Downs, ME Buxton, R Moore, A Ploutz-Snyder, R Ploutz-Snyder, L AF Downs, Meghan E. Buxton, Roxanne Moore, Alan, Jr. Ploutz-Snyder, Robert Ploutz-Snyder, Lori TI Contributions Of Astronauts Aerobic Exercise Intensity And Time On Change In Vo(2)Peak During Spaceflight SO MEDICINE AND SCIENCE IN SPORTS AND EXERCISE LA English DT Meeting Abstract CT 61st Annual Meeting of the American-College-of-Sports-Medicine CY APR 01-04, 2014 CL Atlanta, GA SP Amer Coll Sports Med C1 [Downs, Meghan E.; Buxton, Roxanne; Moore, Alan, Jr.; Ploutz-Snyder, Robert; Ploutz-Snyder, Lori] NASA JSC, Houston, TX USA. NR 0 TC 0 Z9 0 U1 1 U2 4 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0195-9131 EI 1530-0315 J9 MED SCI SPORT EXER JI Med. Sci. Sports Exerc. PD MAY PY 2014 VL 46 IS 5 SU 1 MA 1578 BP 429 EP 430 PG 3 WC Sport Sciences SC Sport Sciences GA AL4PW UT WOS:000339115903023 ER PT J AU Moore, AD Downs, ME Lee, SMC Feiveson, AH Knudsen, P Evetts, SE Ploutz-Snyder, L AF Moore, Alan D., Jr. Downs, Meghan E. Lee, Stuart M. C. Feiveson, Alan H. Knudsen, Poul Evetts, Simon E. Ploutz-Snyder, Lori TI Peak Oxygen Uptake During And After Long-duration Space Flight SO MEDICINE AND SCIENCE IN SPORTS AND EXERCISE LA English DT Meeting Abstract CT 61st Annual Meeting of the American-College-of-Sports-Medicine CY APR 01-04, 2014 CL Atlanta, GA SP Amer Coll Sports Med C1 [Moore, Alan D., Jr.; Lee, Stuart M. C.] Wyle Sci Technol & Engn, Houston, TX USA. [Downs, Meghan E.] Univ Houston, Houston, TX USA. [Feiveson, Alan H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Knudsen, Poul] Danish Aerosp Co, Odense, Denmark. [Evetts, Simon E.] Wyle GmbH, Cologne, Germany. [Ploutz-Snyder, Lori] Univ Space Res Assoc, Houston, TX USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0195-9131 EI 1530-0315 J9 MED SCI SPORT EXER JI Med. Sci. Sports Exerc. PD MAY PY 2014 VL 46 IS 5 SU 1 MA 1577 BP 429 EP 429 PG 1 WC Sport Sciences SC Sport Sciences GA AL4PW UT WOS:000339115903022 ER PT J AU Hou, AY Kakar, RK Neeck, S Azarbarzin, AA Kummerow, CD Kojima, M Oki, R Nakamura, K Iguchi, T AF Hou, Arthur Y. Kakar, Ramesh K. Neeck, Steven Azarbarzin, Ardeshir A. Kummerow, Christian D. Kojima, Masahiro Oki, Riko Nakamura, Kenji Iguchi, Toshio TI THE GLOBAL PRECIPITATION MEASUREMENT MISSION SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID DATA ASSIMILATION SYSTEM; PASSIVE MICROWAVE OBSERVATIONS; RAIN-PROFILING ALGORITHM; DUAL-WAVELENGTH RADAR; TROPICAL RAINFALL; RETRIEVAL ALGORITHM; BAYESIAN-ESTIMATION; TRMM SATELLITE; RADIOMETER; IMPACT AB Precipitation affects many aspects of our everyday life. It is the primary source of freshwater and has significant socioeconomic impacts resulting from natural hazards such as hurricanes, floods, droughts, and landslides. Fundamentally, precipitation is a critical component of the global water and energy cycle that governs the weather, climate, and ecological systems. Accurate and timely knowledge of when, where, and how much it rains or snows is essential for understanding how the Earth system functions and for improving the prediction of weather, climate, freshwater resources, and natural hazard events. The Global Precipitation Measurement (GPM) mission is an international satellite mission specifically designed to set a new standard for the measurement of precipitation from space and to provide a new generation of global rainfall and snowfall observations in all parts of the world every 3 h. The National Aeronautics and Space Administration (NASA) and the Japan Aerospace and Exploration Agency (JAXA) successfully launched the Core Observatory satellite on 28 February 2014 carrying advanced radar and radiometer systems to serve as a precipitation physics observatory. This will serve as a transfer standard for improving the accuracy and consistency of precipitation measurements from a constellation of research and operational satellites provided by a consortium of international partners. GPM will provide key measurements for understanding the global water and energy cycle in a changing climate as well as timely information useful for a range of regional and global societal applications such as numerical weather prediction, natural hazard monitoring, freshwater resource management, and crop forecasting. C1 [Hou, Arthur Y.; Azarbarzin, Ardeshir A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kakar, Ramesh K.; Neeck, Steven] Natl Aeronaut & Space Adm Headquarters, Washington, DC USA. [Kummerow, Christian D.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Kojima, Masahiro] Japan Aerosp Explorat Agcy, Tsukuba Space Ctr, Tsukuba, Ibaraki 3058505, Japan. [Oki, Riko] Japan Aerosp Explorat Agcy, Earth Observat Res Ctr, Tsukuba, Ibaraki, Japan. [Nakamura, Kenji] Dokkyo Univ, Dept Econ Sustainabil, Saitama, Japan. [Iguchi, Toshio] Natl Inst Informat & Commun Technol, Tokyo, Japan. RP Kummerow, CD (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. EM kummerow@atmos.colostate.edu RI Measurement, Global/C-4698-2015; PMM, JAXA/K-8537-2016 FU NASA Earth Science Division Flight Programs FX The authors thank Christopher Kidd, Eric Wood, and Gail Skofronick-Jackson for valuable comments on the manuscript. It is also a pleasure to acknowledge contributions to this article by members of the NASA PMM Science Team, the JAXA PMM Science Team, the NASA GPM Advisory Panel on Ground Validation, the GMI Calibration Task Force, the GMI High-Frequency Channels Advisory Group, the U.S.-Japan CEOS Precipitation Constellation Study Team, and the GPM Flight Project at NASA Goddard Space Flight Center in particular, Robert Adler, Emmanouil Anagnostou, Ana Barros, Peter Bauer, Rafael Bras, Scott Braun, Candace Carlisle, V. Chandrasekar, John Durning, Ralph Ferraro, Kinji Furukawa, Efi Foufoula-Georgiou, Ziad Haddad, Steve Horowitz, Robert Houze, David Hudak, George Huffman, Paul Joe, Linwood Jones, Dalia Kirschbaum, Jarkko Koskinen, Sergey Krimchansky, William Lau, Dennis Lettenmaier, Vincenzo Levizzani, Xin Lin, Guosheng Liu, Robert Meneghini, Joe Munchak, William Olson, Christa Peters-Lidard, Walter Petersen, Fritz Policelli, Didier Renaut, Remy Roca, Christopher Ruf, Steven Rutledge, Mathew Schwaller, Marshall Shepherd, James Shiue, Eric Smith, Soroosh Sorooshian, Erich Stocker, Wei-Kuo Tao, Joe Turk, Fuzhong Weng, Thomas Wilheit, and Edward Zipser. This work is supported by NASA Earth Science Division Flight Programs. NR 89 TC 221 Z9 223 U1 20 U2 111 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD MAY PY 2014 VL 95 IS 5 BP 701 EP + DI 10.1175/BAMS-D-13-00164.1 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AL4GS UT WOS:000339091500008 ER PT J AU Ploutz-Snyder, RJ Fiedler, J Feiveson, AH AF Ploutz-Snyder, Robert J. Fiedler, James Feiveson, Alan H. TI Justifying small-n research in scientifically amazing settings: challenging the notion that only "big-n" studies are worthwhile SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Editorial Material ID CONFIDENCE-INTERVALS; SAMPLE-SIZE; INFORMATION; DESIGN C1 [Ploutz-Snyder, Robert J.; Fiedler, James; Feiveson, Alan H.] NASA Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA. RP Ploutz-Snyder, RJ (reprint author), NASA Johnson Space Ctr, Univ Space Res Assoc, 2101 NASA Pkwy,Mail Code SK3, Houston, TX 77058 USA. EM Robert.ploutz-snyder-1@nasa.gov NR 10 TC 5 Z9 6 U1 0 U2 7 PU AMER PHYSIOLOGICAL SOC PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA SN 8750-7587 EI 1522-1601 J9 J APPL PHYSIOL JI J. Appl. Physiol. PD MAY PY 2014 VL 116 IS 9 BP 1251 EP 1252 DI 10.1152/japplphysiol.01335.2013 PG 2 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA AL5IO UT WOS:000339167300017 PM 24408991 ER PT J AU Ploutz-Snyder, RJ Fiedler, J Feiveson, AH AF Ploutz-Snyder, Robert J. Fiedler, James Feiveson, Alan H. TI Last Word on Viewpoint: Justifying small-n research in scientifically amazing settings: Challenging the notion that only "big-n" studies are worthwhile SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Letter C1 [Ploutz-Snyder, Robert J.; Fiedler, James; Feiveson, Alan H.] NASA Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA. RP Ploutz-Snyder, RJ (reprint author), NASA Johnson Space Ctr, Univ Space Res Assoc, 2101 NASA Pkwy,Mail Code SK3, Houston, TX 77058 USA. EM Robert.ploutz-snyder-1@nasa.gov NR 2 TC 0 Z9 0 U1 0 U2 3 PU AMER PHYSIOLOGICAL SOC PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA SN 8750-7587 EI 1522-1601 J9 J APPL PHYSIOL JI J. Appl. Physiol. PD MAY PY 2014 VL 116 IS 9 BP 1254 EP 1254 DI 10.1152/japplphysiol.00214.2014 PG 1 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA AL5IO UT WOS:000339167300020 PM 24789885 ER PT J AU Garrison, JL Cardellach, E Gleason, S Katzberg, S AF Garrison, James L. Cardellach, Estel Gleason, Scott Katzberg, Steve TI Foreword to Special Issue on Reflectometry using Global Navigation Satellite Systems and Other Signals of Opportunity (GNSS+R) SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Editorial Material ID REFLECTED GPS SIGNALS; OCEAN ALTIMETRY; WIND-SPEED C1 [Garrison, James L.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. [Cardellach, Estel] Inst Ciencies Espai CSIC IEEC, Barcelona 08193, Spain. [Gleason, Scott] Southwest Res Inst, Boulder, CO 80302 USA. [Katzberg, Steve] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Garrison, JL (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. RI Cardellach, Estel/C-9418-2012 OI Cardellach, Estel/0000-0001-8908-0972 NR 40 TC 3 Z9 3 U1 0 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD MAY PY 2014 VL 7 IS 5 SI SI BP 1412 EP 1415 DI 10.1109/JSTARS.2014.2325996 PG 4 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA AJ7TQ UT WOS:000337900700001 ER PT J AU Lowe, ST Meehan, T Young, L AF Lowe, Stephen T. Meehan, Thomas Young, Larry TI Direct Signal Enhanced Semicodeless Processing of GNSS Surface-Reflected Signals SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Altimetry; bistatic radar; global navigation satellite systems (GNSS) reflectometry; global positioning system (GPS) reflectometry; scatterometry; semicodeless signal processing ID SEA-SURFACE; OCEAN; REFLECTOMETRY; ALTIMETRY; PARIS AB This paper presents an aircraft demonstration of direct-signal enhanced semicodeless processing of global navigation satellite systems (GNSS) signals reflected from the Earth's surface. Comparisons are made between this new method and an interferometric approach to GNSS reflectometry. Results show that this technique produces waveforms with greater signal-to-noise compared with the interferometric approach for all GNSS signals currently in use or planned for the near future. Alternatively, the semicodeless technique can have similar performance with smaller antennas for lower hardware costs. The semicodeless approach also has the advantage that different signals along with their different surface spatial resolutions are processed separately, each signal's coherent integration time can be optimized, and ground/aircraft experiments and tests are free of spurious signals. The signal processing demands of the semicodeless approach are shown to be proportional to the number of signal components processed when integrated with a GNSS precise orbit determination (POD) receiver. C1 [Lowe, Stephen T.; Meehan, Thomas; Young, Larry] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lowe, ST (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM steve.lowe@jpl.nasa.gov; tomas.meehan@jpl.nasa.gov; larry.young-@jpl.nasa.gov FU National Aeronautics and Space Administration; NASA's Physical Oceanography Program FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, CA, USA, under a contract with the National Aeronautics and Space Administration. This work was supported in part by John LaBrecque, Lead, Earth Surface and Interior Focus Area, NASA's Science Mission Directorate. The Monterey Bay aircraft experiments were originally funded under NASA's Physical Oceanography Program. Government sponsorship acknowledged. NR 15 TC 9 Z9 9 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD MAY PY 2014 VL 7 IS 5 SI SI BP 1469 EP 1472 DI 10.1109/JSTARS.2014.2313061 PG 4 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA AJ7TQ UT WOS:000337900700007 ER PT J AU Przekop, A Jegley, DC AF Przekop, Adam Jegley, Dawn C. TI Evaluation of a Metallic Repair on a Rod-Stiffened Composite Panel SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT 54th AIAA/ASME/ASCE/AHS/ASC Structures, Structural Dynamics, and Materials Conference CY APR 08-11, 2013 CL Boston, MA SP AIAA, ASME, ASCE, AHS, ASC AB A design and analysis of a repair concept applicable to a stiffened composite panel based on the pultruded rod stitched efficient unitized structure was recently completed. The damage scenario considered was a midbay-to-midbay saw-cut with a severed stiffener, flange, and skin. Advanced modeling techniques such as mesh-independent definition of compliant fasteners and elastic-plastic material properties for metal parts were used in the finite-element analysis supporting the design effort. A bolted metallic repair was selected so that it could be easily applied in the operational environment. The present work describes results obtained from a tension panel test conducted to validate both the repair concept and finite-element analysis techniques used in the design effort. The test proved that the proposed repair concept is capable of sustaining load levels that are higher than those resulting from the current working stress allowables. This conclusion enables upward revision of the stress allowables that had been kept at an overly conservative level due to concerns associated with repairability of the panels. Correlation of test data with finite-element analysis results is also presented and assessed. C1 [Przekop, Adam] Analyt Mech Associates Inc, NASA Langley Res Ctr, Hampton, VA 23666 USA. [Jegley, Dawn C.] NASA Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA. RP Przekop, A (reprint author), Analyt Mech Associates Inc, NASA Langley Res Ctr, Mail Stop 190, Hampton, VA 23666 USA. NR 16 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD MAY-JUN PY 2014 VL 51 IS 3 BP 792 EP 804 DI 10.2514/1.C032461 PG 13 WC Engineering, Aerospace SC Engineering GA AJ8UT UT WOS:000337984100008 ER PT J AU Arntzen, M Rizzi, SA Visser, HG Simon, DG AF Arntzen, Michael Rizzi, Stephen A. Visser, Hendrikus G. Simon, Dick G. TI Framework for Simulating Aircraft Flyover Noise Through Nonstandard Atmospheres SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT 18th AIAA/CEAS Aeroacoustics Conference / 33rd AIAA Aeroacoustics Conference CY JUN 04-06, 2012 CL Colorado Springs, CO SP AIAA, CEAS AB This paper describes a new framework for the synthesis of aircraft flyover noise through a nonstandard atmosphere. Central to the framework is a ray-tracing algorithm that defines multiple curved propagation paths, if the atmosphere allows, between the moving source and listener. Because each path has a different emission angle, synthesis of the sound at the source must be performed independently for each path. The time delay, spreading loss, and absorption (ground and atmosphere) are integrated along each path and applied to each synthesized aircraft noise source to simulate a flyover. A final step assigns each resulting signal to its corresponding receiver angle for the simulation of a flyover in a virtual reality environment. Spectrograms of the results from a straight path and a curved path modeling assumption are shown. When the aircraft is at close range, the straight path results are valid. Differences appear especially when the source is relatively far away at shallow elevation angles. These differences, however, are not significant in common sound metrics. Although the framework used in this work performs off-line processing, it is conducive to real-time implementation. C1 [Arntzen, Michael] Natl Aerosp Lab, NL-1059 CM Amsterdam, Netherlands. [Rizzi, Stephen A.] NASA Langley Res Ctr, Struct Acoust Branch, MS 463, Hampton, VA 23681 USA. [Visser, Hendrikus G.; Simon, Dick G.] Delft Univ Technol, NL-2600 AA Delft, Netherlands. RP Arntzen, M (reprint author), Natl Aerosp Lab, Anthony Fokkerweg 2, NL-1059 CM Amsterdam, Netherlands. OI Visser, Hendrikus/0000-0002-5644-0430 NR 30 TC 4 Z9 4 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD MAY-JUN PY 2014 VL 51 IS 3 BP 956 EP 966 DI 10.2514/1.C032049 PG 11 WC Engineering, Aerospace SC Engineering GA AJ8UT UT WOS:000337984100024 ER PT J AU Park, MA Aftosmis, MJ Campbell, RL Carter, MB Cliff, SE Bangert, LS AF Park, Michael A. Aftosmis, Michael J. Campbell, Richard L. Carter, Melissa B. Cliff, Susan E. Bangert, Linda S. TI Summary of the 2008 NASA Fundamental Aeronautics Program Sonic Boom Prediction Workshop SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT 51st AIAA Aerospace Sciences Meeting and Exhibit Including the New Horizons Forum and Aerospace Exposition CY JAN 06-10, 2013 CL Grapevine, TX SP AIAA ID COMPUTATIONAL FLUID-DYNAMICS; POSTERIORI ERROR ESTIMATION; FINITE-ELEMENT METHODS; GRID ADAPTATION; FUNCTIONAL OUTPUTS; MESH GENERATION; FLOWS AB The Supersonics Project of the NASA Fundamental Aeronautics Program organized an internal sonic boom workshop to evaluate near-field sonic-boom prediction capability at the Fundamental Aeronautics Annual Meeting in Atlanta, Georgia, on 8 October 2008. Workshop participants computed sonic-boom signatures for three nonlifting bodies and two lifting configurations. Cone cylinder, parabolic, and quartic bodies of revolution comprised the nonlifting cases. The lifting configurations were a simple 69 deg delta-wing body and a complete low-boom transport configuration designed during the High Speed Research Project in the 1990s with wing, body, tail, nacelle, and boundary-layer diverter components. The AIRPLANE, Cart3D, FUN3D, and USM3D flow solvers were employed with the ANET signature propagation tool, output-based adaptation, and a priori adaptation based on freestream Mach number and angle of attack. Results were presented orally at the workshop. This article documents the workshop and results and provides context on previously available and recently developed methods. C1 [Park, Michael A.] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. [Aftosmis, Michael J.] NASA, Ames Res Ctr, Appl Modeling & Simulat Branch, Moffett Field, CA 94035 USA. [Campbell, Richard L.; Carter, Melissa B.; Bangert, Linda S.] NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA. RP Park, MA (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. NR 72 TC 3 Z9 3 U1 0 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD MAY-JUN PY 2014 VL 51 IS 3 BP 987 EP 1001 DI 10.2514/1.C032589 PG 15 WC Engineering, Aerospace SC Engineering GA AJ8UT UT WOS:000337984100027 ER PT J AU Duan, HY Xu, R Li, JC Yuan, YG Wang, QX Hadi, NI AF Duan Huanyun Xu Rui Li Jianchang Yuan Yage Wang Qiuxia Hadi, Nomana Intekhab TI Analysis on sustainable development countermeasures and barriers of rural household biogas in China (vol 5, 043116, 2013) SO JOURNAL OF RENEWABLE AND SUSTAINABLE ENERGY LA English DT Correction C1 [Duan Huanyun; Xu Rui; Li Jianchang; Yuan Yage; Wang Qiuxia] Yannan Normal Univ, Coll Energy & Environm Sci, Solar Energy Inst, Kunming 650092, Peoples R China. [Hadi, Nomana Intekhab] NASA, Ames Res Ctr, SETI Inst Affiliat, Moffett Field, CA 94035 USA. RP Duan, HY (reprint author), Yannan Normal Univ, Coll Energy & Environm Sci, Solar Energy Inst, Kunming 650092, Peoples R China. EM duanhuanyun@gmail.com; ecowatch.xr@gmail.com; jclee94213@yahoo.com.cn; yuanyage@sina.cn; 798606608@qq.com; nomana.i.hadi@gmail.com NR 1 TC 0 Z9 0 U1 1 U2 11 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1941-7012 J9 J RENEW SUSTAIN ENER JI J. Renew. Sustain. Energy PD MAY PY 2014 VL 6 IS 3 AR 039901 DI 10.1063/1.4880535 PG 1 WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Energy & Fuels SC Science & Technology - Other Topics; Energy & Fuels GA AJ9ZS UT WOS:000338072800048 ER PT J AU Abdo, AA Abeysekara, AU Allen, BT Aune, T Barber, AS Berley, D Braun, J Chen, C Christopher, GE DeYoung, T Dingus, BL Ellsworth, RW Gonzalez, MM Goodman, JA Hays, E Hoffman, CM Huntemeyer, PH Imran, A Kolterman, BE Linnemann, JT McEnery, JE Morgan, T Mincer, AI Nemethy, P Pretz, J Ryan, JM Parkinson, PMS Schneider, M Shoup, A Sinnis, G Smith, AJ Vasileiou, V Walker, GP Williams, DA Yodh, GB AF Abdo, A. A. Abeysekara, A. U. Allen, B. T. Aune, T. Barber, A. S. Berley, D. Braun, J. Chen, C. Christopher, G. E. DeYoung, T. Dingus, B. L. Ellsworth, R. W. Gonzalez, M. M. Goodman, J. A. Hays, E. Hoffman, C. M. Huentemeyer, P. H. Imran, A. Kolterman, B. E. Linnemann, J. T. McEnery, J. E. Morgan, T. Mincer, A. I. Nemethy, P. Pretz, J. Ryan, J. M. Parkinson, P. M. Saz Schneider, M. Shoup, A. Sinnis, G. Smith, A. J. Vasileiou, V. Walker, G. P. Williams, D. A. Yodh, G. B. TI Milagro observations of potential TeV emitters SO ASTROPARTICLE PHYSICS LA English DT Article DE Astroparticle physics; Pulsars; Galaxies; Active galactic nuclei; Gamma-rays ID CYGNUS REGION; SPECTRUM; MARKARIAN-421; DISCOVERY; EMISSION; AREA AB This paper reports the results from three targeted searches of Milagro TeV sky maps: two extragalactic point source lists and one pulsar source list. The first extragalactic candidate list consists of 709 candidates selected from the Fermi-LAT 2FGL catalog. The second extragalactic candidate list contains 31 candidates selected from the TeVCat source catalog that have been detected by imaging atmospheric Cherenkov telescopes (IACTs). In both extragalactic candidate lists Mkn 421 was the only source detected by Milagro. This paper presents the Milagro TeV flux for Mkn 421 and flux limits for the brighter Fermi-LAT extragalactic sources and for all TeVCat candidates. The pulsar list extends a previously published Milagro targeted search for Galactic sources. With the 32 new gamma-ray pulsars identified in 2FGL, the number of pulsars that are studied by both Fermi-LAT and Milagro is increased to 52. In this sample, we find that the probability of Milagro detecting a TeV emission coincident with a pulsar increases with the GeV flux observed by the Fermi-LAT in the energy range from 0.1 GeV to 100 GeV. (C) 2014 Elsevier B.V. All rights reserved. C1 [Abdo, A. A.; Abeysekara, A. U.; Barber, A. S.; Linnemann, J. T.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Allen, B. T.; Chen, C.; Yodh, G. B.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Aune, T.; Parkinson, P. M. Saz; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Berley, D.; Braun, J.; Goodman, J. A.; Smith, A. J.; Vasileiou, V.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Christopher, G. E.; Kolterman, B. E.; Mincer, A. I.; Nemethy, P.] NYU, Dept Phys, New York, NY 10003 USA. [DeYoung, T.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Dingus, B. L.; Hoffman, C. M.; Imran, A.; Pretz, J.; Sinnis, G.; Walker, G. P.] Los Alamos Natl Lab, Grp P 23, Los Alamos, NM 87545 USA. [Ellsworth, R. W.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Gonzalez, M. M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Hays, E.; McEnery, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Huentemeyer, P. H.] Michigan Technol Univ, Dept Phys, Houghton, MI 49931 USA. [Morgan, T.; Ryan, J. M.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Schneider, M.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Shoup, A.] Ohio State Univ, Lima, OH 45804 USA. [Parkinson, P. M. Saz] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. RP Abeysekara, AU (reprint author), Michigan State Univ, Dept Phys & Astron, BioMed Phys Sci Bldg, E Lansing, MI 48824 USA. EM udaraabeysekara@yahoo.com OI Mincer, Allen/0000-0002-6307-1418; Dingus, Brenda/0000-0001-8451-7450 NR 20 TC 1 Z9 1 U1 0 U2 3 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 MAY-JUN PY 2014 VL 57-58 BP 16 EP 25 DI 10.1016/j.astropartphys.2014.03.001 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AJ4MY UT WOS:000337651700004 ER PT J AU Golding, J Steer, CD Lowery, T Jones, R Hibbeln, JR AF Golding, Jean Steer, Colin D. Lowery, Tony Jones, Robert Hibbeln, Joseph R. TI Fish Consumption and Blood Mercury Levels: Golding et al. Respond SO ENVIRONMENTAL HEALTH PERSPECTIVES LA English DT Letter ID UK TOTAL DIET C1 [Golding, Jean; Steer, Colin D.] Univ Bristol, Ctr Child & Adolescent Hlth, Bristol, RI 02809 USA. [Lowery, Tony] Natl Ocean & Atmospher Adm, Natl Marine Fisheries Serv, Natl Seafood Inspect Lab, Pascagoula, MS USA. [Jones, Robert] Ctr Dis Control & Prevent, Inorgan & Radiat Analyt Toxicol Branch, Atlanta, GA USA. [Hibbeln, Joseph R.] NIAAA, NIH, Dept Hlth & Human Serv, Bethesda, MD USA. RP Golding, J (reprint author), Univ Bristol, Ctr Child & Adolescent Hlth, Bristol, RI 02809 USA. EM Jean.Golding@bristol.ac.uk OI Golding, Jean/0000-0003-2826-3307 NR 3 TC 0 Z9 0 U1 0 U2 10 PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE PI RES TRIANGLE PK PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233, RES TRIANGLE PK, NC 27709-2233 USA SN 0091-6765 EI 1552-9924 J9 ENVIRON HEALTH PERSP JI Environ. Health Perspect. PD MAY PY 2014 VL 122 IS 5 BP A120 EP A121 DI 10.1289/ehp.1307997R PG 2 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA AJ3ZC UT WOS:000337606300004 PM 24787643 ER PT J AU Nichols, JE Isles, PDF Peteet, DM AF Nichols, Jonathan E. Isles, Peter D. F. Peteet, Dorothy M. TI A novel framework for quantifying past methane recycling by Sphagnum-methanotroph symbiosis using carbon and hydrogen isotope ratios of leaf wax biomarkers SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Article ID N-ALKANE DISTRIBUTIONS; DELTA-D VALUES; ATMOSPHERIC CH4 GRADIENT; NORTHERN PEATLAND; TESTATE AMEBAS; PLANTS; RECORD; HOLOCENE; BOG; PHOTOSYNTHESIS AB The concentration of atmospheric methane is strongly linked to variations in Earth's climate. Currently, we can directly reconstruct the total atmospheric concentration of methane, but not individual terms of the methane cycle. Northern wetlands, dominated by Sphagnum, are an important contributor of atmospheric methane, and we seek to understand the methane cycle in these systems. We present a novel method for quantifying the proportion of carbon Sphagnum assimilates from its methanotrophic symbionts using stable isotope ratios of leaf-wax biomarkers. Carbon isotope ratios of Sphagnum compounds are determined by two competing influences, water content and the isotope ratio of source carbon. We disentangled these effects using a combined hydrogen and carbon isotope approach. We constrained Sphagnum water content using the contrast between the hydrogen isotope ratios of Sphagnum and vascular plant biomarkers. We then used Sphagnum water content to calculate the carbon isotope ratio of Sphagnum's carbon pool. Using a mass balance equation, we calculated the proportion of recycled methane contributed to the Sphagnum carbon pool, "PRM." We quantified PRM in peat monoliths from three microhabitats in the Mer Bleue peatland complex. Modern studies have shown that water table depth and vegetation have strong influences on the peatland methane cycle on instrumental time scales. With this new approach, delta C-13 of Sphagnum compounds are now a useful tool for investigating the relationships among hydrology, vegetation, and methanotrophy in Sphagnum peatlands over the time scales of entire peatland sediment records, vital to our understanding of the global carbon cycle through the Late Glacial and Holocene. C1 [Nichols, Jonathan E.; Peteet, Dorothy M.] Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Isles, Peter D. F.] Univ Vermont, Rubenstein Sch Environm & Nat Resources, Burlington, VT USA. [Peteet, Dorothy M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Nichols, JE (reprint author), Lamont Doherty Earth Observ, Palisades, NY 10964 USA. EM jnichols@ldeo.columbia.edu OI Nichols, Jonathan/0000-0003-3913-2206 FU National Science Foundation [ARC-1022979]; NASA Postdoctoral Program FX The authors would like to thank Tim Moore and Nigel Roulet for assistance in sample collection and for sharing methane flux data, Carl Johnson for assistance with carbon isotope ratio measurements, and Francesca McInerney and an anonymous reviewer for their helpful comments. This research is supported by the National Science Foundation, ARC-1022979. For part of this research, J. Nichols was supported by the NASA Postdoctoral Program. NR 45 TC 0 Z9 0 U1 1 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1525-2027 J9 GEOCHEM GEOPHY GEOSY JI Geochem. Geophys. Geosyst. PD MAY PY 2014 VL 15 IS 5 BP 1827 EP 1836 DI 10.1002/2014GC005242 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AJ4EQ UT WOS:000337625100009 ER PT J AU Cabrol, NA Herkenhoff, K Knoll, AH Farmer, J Arvidson, R Grin, E Li, RX Fenton, L Cohen, B Bell, JF Yingst, RA AF Cabrol, Nathalie A. Herkenhoff, Kenneth Knoll, Andrew H. Farmer, Jack Arvidson, Raymond Grin, Edmond Li, Ronxing Fenton, Lori Cohen, Barbara Bell, James F., III Yingst, R. Aileen TI Sands at Gusev Crater, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; Gusev; Spirit; Sand; Texture; Sedimentology ID GRAIN-SIZE DISTRIBUTIONS; SEDIMENT TREND ANALYSIS; SPIRIT ROVER; IMAGE-ANALYSIS; PARTICLE-SIZE; MAADIM-VALLIS; ROCKS; EXPLORATION; PARAMETERS; IDENTIFICATION AB Processes, environments, and the energy associated with the transport and deposition of sand at Gusev Crater are characterized at the microscopic scale through the comparison of statistical moments for particle size and shape distributions. Bivariate and factor analyses define distinct textural groups at 51 sites along the traverse completed by the Spirit rover as it crossed the plains and went into the Columbia Hills. Fine-to-medium sand is ubiquitous in ripples and wind drifts. Most distributions show excess fine material, consistent with a predominance of wind erosion over the last 3.8 billion years. Negative skewness at West Valley is explained by the removal of fine sand during active erosion, or alternatively, by excess accumulation of coarse sand from a local source. The coarse to very coarse sand particles of ripple armors in the basaltic plains have a unique combination of size and shape. Their distribution display significant changes in their statistical moments within the similar to 400 m that separate the Columbia Memorial Station from Bonneville Crater. Results are consistent with aeolian and/or impact deposition, while the elongated and rounded shape of the grains forming the ripples, as well as their direction of origin, could point to Ma'adim Vallis as a possible source. For smaller particles on the traverse, our findings confirm that aeolian processes have dominated over impact and other processes to produce sands with the observed size and shape patterns across a spectrum of geologic (e.g., ripples and plains soils) and aerographic settings (e.g., wind shadows). C1 [Cabrol, Nathalie A.; Grin, Edmond; Fenton, Lori] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. [Cabrol, Nathalie A.; Grin, Edmond] NASA Ames Res Ctr, Div Space Sci, Moffett Field, CA USA. [Herkenhoff, Kenneth] US Geol Survey Astrogeol Team, Flagstaff, AZ USA. [Knoll, Andrew H.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Farmer, Jack; Bell, James F., III] Arizona State Univ, Sch Earth & Planetary Explorat, Tempe, AZ USA. [Arvidson, Raymond] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Li, Ronxing] Ohio State Univ, CEGE, Mapping & GIS Lab, Columbus, OH 43210 USA. [Cohen, Barbara] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Yingst, R. Aileen] Planetary Sci Inst, Tucson, AZ USA. RP Cabrol, NA (reprint author), Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. EM Nathalie.A.Cabrol@nasa.gov FU National Aeronautics and Space Administration Mars Exploration Rover mission FX This work was performed for the Jet Propulsion Laboratory, California Institute of Technology, sponsored by the National Aeronautics and Space Administration Mars Exploration Rover mission. The authors want to especially thank Steve Ostrowski (GIS & Mapping Lab Undergraduate Research Assistant, The Ohio State University) for generating the map of Spirit's traverse used in Figure 6. We are also extremely thankful to Robert Craddock and an anonymous reviewer for their thorough reviews and constructive remarks and suggestions. NR 141 TC 2 Z9 2 U1 3 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAY PY 2014 VL 119 IS 5 BP 941 EP 967 DI 10.1002/2013JE004535 PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AJ5AX UT WOS:000337693900003 ER PT J AU Hathaway, DH Upton, L AF Hathaway, D. H. Upton, L. TI The solar meridional circulation and sunspot cycle variability SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Sunspot Cycle ID MAGNETIC-FIELD; TORSIONAL OSCILLATION; FLUX TRANSPORT; FLOW; SUN; ROTATION; SURFACE; HELIOSEISMOLOGY; PHOTOSPHERE; EVOLUTION AB We have measured the meridional motions of the magnetic elements in the Sun's surface layers since 1996 and find systematic and substantial variations. In general the meridional flow speed is fast at cycle minima and slow at cycle maxima. We find that these systematic variations are characterized by a weakening of the meridional flow on the poleward sides of the active (sunspot) latitudes. This can be interpreted as an inflow toward the sunspot zones superimposed on a more general poleward meridional flow profile. We also find variations in the meridional flow which vary from cycle to cycle. The meridional flow was slower at both the minimum and maximum of cycle 23 compared to similar phases of cycles 21, 22, and 24. Models of the magnetic flux transport by a variable meridional flow suggest that it can significantly modulate the size and timing of the following sunspot cycle through its impact on the Sun's polar magnetic fields. We suggest that the meridional flow variations observed in cycle 23 contributed to the weak polar fields at the end of the cycle which then produced a weak cycle 24 and the extraordinary cycle 23/24 minimum. C1 [Hathaway, D. H.] NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Upton, L.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Upton, L.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. RP Hathaway, DH (reprint author), NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. EM david.hathaway@nasa.gov FU NASA [NAG5-10483] FX The authors were supported by a grant from the NASA Living with a Star Program to Marshall Space Flight Center. The HMI data used are courtesy of the NASA/SDO and the HMI science team. The SOHO/MDI project was supported by NASA grant NAG5-10483 to Stanford University. SOHO is a project of international cooperation between ESA and NASA. NR 46 TC 5 Z9 5 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2014 VL 119 IS 5 BP 3316 EP 3324 DI 10.1002/2013JA019432 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ4DS UT WOS:000337622100008 ER PT J AU Elfritz, JG Keesee, AM Buzulukova, N Fok, MC Scime, EE AF Elfritz, J. G. Keesee, A. M. Buzulukova, N. Fok, M. -C. Scime, E. E. TI First results using TWINS-derived ion temperature boundary conditions in CRCM SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE magnetosphere; simulation; temperature ID INTERPLANETARY MAGNETIC-FIELD; CENTRAL PLASMA SHEET; SOLAR-WIND CONTROL; RING CURRENT; EARTHS MAGNETOSPHERE; GEOMAGNETIC STORMS; CURRENT SYSTEMS; MODEL; SUBSTORM; IMAGES AB We have integrated dynamic, spatiotemporally resolved ion temperature boundary conditions into the Comprehensive Ring Current Model (CRCM), which are based on 2-D equatorial maps derived from the Two Wide-Angle Imaging Neutral-Atom Spectrometers (TWINS) energetic neutral atom (ENA) data. The high-speed stream-driven event on 22 July 2009 is simulated and compared against an identical simulation using a statistically derived boundary condition model. ENA-derived temperatures allow users to include event-specific observations associated with a dynamic plasma sheet. This method also provides temperatures in the important region between geosynchronous orbit and the plasma sheet, a region which existing empirical models exclude. We find that the spatial and energy distributions of ring current flux and pressure have sensitive dependence on boundary conditions during this event. The coupling of boundary conditions to the time history of the convection field strength also plays an important role by throttling the influence of the boundary plasma on the inner magnetosphere. Simulated moments and spectra from our simulations are compared with remotely imaged ion temperatures from TWINS and also in situ energy spectra and temperature moments from Time History of Events and Macroscale Interactions during Substorms-D. Storm time dusk-dawn asymmetries consistent with observational data, such as Zhang et al. (2006), are reproduced well when CRCM is provided with the event-specific boundary model. A hot localized structure observed by TWINS at geosynchronous midnight during a strong northward interplanetary magnetic field interval is also reproduced with this boundary model, whereas the empirical boundary model fails to yield this feature. C1 [Elfritz, J. G.; Keesee, A. M.; Scime, E. E.] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA. [Buzulukova, N.; Fok, M. -C.] NASA, Geospace Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD USA. [Buzulukova, N.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Elfritz, JG (reprint author), W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA. EM jelfritz@mix.wvu.edu RI Keesee, Amy/J-8194-2014 OI Keesee, Amy/0000-0002-9719-3229 FU Southwest Research Institute, NSF [AGS- 1113478]; NASA EPSCoR [NNX10AN08A]; NASA [NAS5-02099] FX This work was carried out as a part of the TWINS NASA Explorer mission; work at WVU was supported under subcontract to the Southwest Research Institute, NSF grant AGS- 1113478 and NASA EPSCoR grant NNX10AN08A. The authors would like to thank the members of the TWINS science team for helpful discussions regarding the TWINS ENA data. The authors also acknowledge the use of ACE solar wind data provided through Omni-Web. We acknowledge NASA contract NAS5-02099 and V. Angelopoulos for use of data from the THEMIS Mission. Specifically D. Larson and R. P. Lin for use of SST data as well as C. W. Carlson and J. P. McFadden for use of ESA data. NR 55 TC 3 Z9 3 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2014 VL 119 IS 5 BP 3345 EP 3361 DI 10.1002/2013JA019555 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ4DS UT WOS:000337622100011 ER PT J AU Connor, HK Zesta, E Ober, DM Raeder, J AF Connor, H. K. Zesta, E. Ober, D. M. Raeder, J. TI The relation between transpolar potential and reconnection rates during sudden enhancement of solar wind dynamic pressure: OpenGGCM-CTIM results SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE MI coupling system; Magnetic reconnection; Cross Polar Cap Potential; MHD modeling ID IONOSPHERIC CONDUCTIVITY; MHD SIMULATIONS; AURORAL OVAL; JANUARY 10; IMAGE FUV; POLAR; SATURATION; MAGNETOSPHERE; MAGNETOTAIL; MODEL AB This study investigates how solar wind energy is deposited into the magnetosphere-ionosphere system during sudden enhancements of solar wind dynamic pressure (Psw), using the coupled Open Geospace General Circulation Model-Coupled Ionosphere Thermosphere Model (OpenGGCM-CTIM) 3-D global magnetosphere-ionosphere-thermosphere model. We simulate three unique events of solar wind pressure enhancements that occurred during negative, near-zero, and positive interplanetary magnetic field (IMF) Bz. Then, we examine the behavior of the dayside and nightside reconnection rates and quantify their respective contributions to cross polar cap potential (CPCP), a proxy of ionospheric plasma convection strength. The modeled CPCP increases after a Psw enhancement in all three cases, which agrees well with observations from the Defense Meteorological Satellite Program spacecraft and predictions from the assimilative mapping of ionospheric electrodynamics technique. In the OpenGGCM-CTIM model, dayside reconnection increases within 9-13min of the pressure impact, while nightside reconnection intensifies about 13-25min after the pressure increase. As the strong Psw compresses the dayside magnetosheath and, subsequently, the magnetotail, their magnetic fields intensify and activate stronger antiparallel reconnection on the dayside magnetopause first and near the central plasma sheet second. For southward IMF, dayside reconnection contributes to the CPCP enhancement 2-4 times more than nightside reconnection. For northward IMF, the dayside contribution weakens, and nightside reconnection contributes more to the CPCP enhancement. We find that high-latitude magnetopause reconnection during northward IMF produces sunward ionospheric plasma convection, which decreases the typical dawn-to-dusk ionosphere electric field. This results in a weaker dayside reconnection contribution to the CPCP during northward IMF. C1 [Connor, H. K.] Univ New Mexico, Configurable Space Microsyst Innovat & Applicat, Albuquerque, NM 87131 USA. [Zesta, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Connor, H. K.; Ober, D. M.] Air Force Res Lab, Kirtland AFB, NM USA. [Raeder, J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. RP Connor, HK (reprint author), Univ New Mexico, Configurable Space Microsyst Innovat & Applicat, Albuquerque, NM 87131 USA. EM hyunju.connor@cosmiac.org FU Air Force Office of Scientific Research [11RV09COR] FX The simulation data of this paper are available upon request. This work was supported by a grant LBIR# 11RV09COR from the Air Force Office of Scientific Research. We thank C. Y. Huang and Y.-J. Su for useful discussions. NR 50 TC 2 Z9 2 U1 3 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2014 VL 119 IS 5 BP 3411 EP 3429 DI 10.1002/2013JA019728 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ4DS UT WOS:000337622100016 ER PT J AU Birn, J Hesse, M AF Birn, J. Hesse, M. TI The substorm current wedge: Further insights from MHD simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE substorm current wedge ID MAGNETOTAIL; ASSOCIATION; FLOWS; FIELD AB Using a recent magnetohydrodynamic simulation of magnetotail dynamics, we further investigate the buildup and evolution of the substorm current wedge (SCW), resulting from flow bursts generated by near-tail reconnection. Each flow burst generates an individual current wedge, which includes the reduction of cross-tail current and the diversion to region 1 (R1)-type field-aligned currents (earthward on the dawn and tailward on the duskside), connecting the tail with the ionosphere. Multiple flow bursts generate initially multiple SCW patterns, which at later times combine to a wider single SCW pattern. The standard SCW model is modified by the addition of several current loops, related to particular magnetic field changes: the increase of Bz in a local equatorial region (dipolarization), the decrease of |Bx|away from the equator (current disruption), and increases in |By|resulting from azimuthally deflected flows. The associated loop currents are found to be of similar magnitude, 0.1-0.3 MA. The combined effect requires the addition of region 2 (R2)-type currents closing in the near tail through dawnward currents but also connecting radially with the R1 currents. The current closure at the inner boundary, taken as a crude proxy of an idealized ionosphere, demonstrates westward currents as postulated in the original SCW picture as well as North-South currents connecting R1- and R2-type currents, which were larger than the westward currents by a factor of almost 2. However, this result should be applied with caution to the ionosphere because of our neglect of finite resistance and Hall effects. C1 [Birn, J.] Space Sci Inst, Boulder, CO 80301 USA. [Birn, J.] Los Alamos Natl Lab, Los Alamos, NM USA. [Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Birn, J (reprint author), Space Sci Inst, Boulder, CO 80301 USA. EM jbirn@spacescience.org RI NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 FU NASA [NNX13AD10G, NNX13AD21G]; NSF [1203711] FX This work was performed mostly at Los Alamos National Laboratory under a Guest Scientist agreement, supported by NASA grants NNX13AD10G and NNX13AD21G and NSF grant 1203711. J.B. also acknowledges the hospitality and support of the International Space Science Institute, Bern, Switzerland, and fruitful discussions with Wolfgang Baumjohann and members of the ISSI team on the substorm current wedge. Data necessary to understand, evaluate, replicate, and build upon the reported research will be made available upon request. NR 23 TC 15 Z9 15 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 MAY PY 2014 VL 119 IS 5 BP 3503 EP 3513 DI 10.1002/2014JA019863 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ4DS UT WOS:000337622100022 ER PT J AU Birn, J Runov, A Hesse, M AF Birn, J. Runov, A. Hesse, M. TI Energetic electrons in dipolarization events: Spatial properties and anisotropy SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE electron acceleration; dipolarization fronts; injections ID TEST PARTICLE ORBITS; GEOSYNCHRONOUS OBSERVATIONS; MAGNETOTAIL; ACCELERATION; SUBSTORMS; SIMULATIONS; INJECTIONS; TRANSPORT; DISTRIBUTIONS; ENERGIZATION AB Using the electromagnetic fields of an MHD simulation of magnetotail reconnection, flow bursts, and dipolarization, we further investigate the acceleration of electrons to suprathermal energies. Particular emphasis is on spatial properties and anisotropies as functions of energy and time. The simulation results are compared with Time History of Events and Macroscale Interactions during Substorms observations. The test particle approach successfully reproduces several observed injection features and puts them into a context of spatial maps of the injection region(s): a dominance of perpendicular anisotropies farther down the tail and closer to the equatorial plane, an increasing importance of parallel anisotropy closer to Earth and at higher latitudes, a drop in energy fluxes at energies below approximate to 10keV, coinciding with the plasma density drop, together with increases at higher energy, a triple peak structure of flux increases near 0 degrees, 90 degrees, and 180 degrees, and a tendency of flux increases to extend to higher energy closer to Earth and at lower latitudes. We identified the plasma sheet boundary layers and adjacent lobes as a main source region for both increased and decreased energetic electron fluxes, related to the different effects of adiabatic acceleration at high and low energies. The simulated anisotropies tend to exceed the observed ones, particularly for perpendicular fluxes at high energies. The most plausible reason is that the MHD simulation lacks the effects of anisotropy-driven microinstabilities and waves, which would reduce anisotropies. C1 [Birn, J.] Space Sci Inst, Boulder, CO 80301 USA. [Birn, J.] Los Alamos Natl Lab, Los Alamos, NM USA. [Runov, A.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA. [Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Birn, J (reprint author), Space Sci Inst, Boulder, CO 80301 USA. EM jbirn@spacescience.org RI NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 FU U.S. Department of Energy; NASA [NNX13AD10G, NNX13AD21G, NAS5-0299, NNX13AF81G]; NSF [1203711]; DLR [50 OC 0302]; International Space Science Institute Bern, Switzerland FX The simulation work was performed at Los Alamos under the auspices of the U.S. Department of Energy, supported by NASA grants NNX13AD10G and NNX13AD21G and NSF grant 1203711. THEMIS data analysis was supported by NASA grants NAS5-0299 and NNX13AF81G. We thank V. Angelopoulos for use of data from the THEMIS Mission, C. W. Carlson and J.P. McFadden for use of ESA data, D. Larson and R. P. Lin for use of SST data, D. L. Turner and P. Cruce for help with SST data calibration, and K.-H. Glassmeier, U. Auster, and W. Baumjohann for the use of FGM data provided with financial support through the DLR contract 50 OC 0302. We are grateful to the hospitality and support by the International Space Science Institute Bern, Switzerland, and the fruitful discussions with members of the ISSI working group. NR 37 TC 12 Z9 12 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2014 VL 119 IS 5 BP 3604 EP 3616 DI 10.1002/2013JA019738 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ4DS UT WOS:000337622100029 ER PT J AU Nakano, S Fok, MC Brandt, PC Higuchi, T AF Nakano, S. Fok, M-C. Brandt, P. C. Higuchi, T. TI Estimation of temporal evolution of the helium plasmasphere based on a sequence of IMAGE/EUV images SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE plasmasphere; electric field; data assimilation; magnetospheric convection ID 17 APRIL 2002; SQUARE-ROOT FILTERS; DATA ASSIMILATION; ELECTRIC-FIELD; INNER MAGNETOSPHERE; KALMAN SMOOTHER; CLUSTER DATA; RING CURRENT; ENSEMBLE; DYNAMICS AB We have developed a technique for estimating the temporal evolution of the plasmaspheric helium ion density based on a sequence of extreme ultraviolet (EUV) data obtained from the IMAGE satellite. In the proposed technique, the estimation is obtained by incorporating EUV images from IMAGE into a two-dimensional fluid model of the plasmasphere using a data assimilation approach based on the ensemble transform Kalman filter. Since the motion and the spatial structure of the helium plasmasphere is strongly controlled by the electric field in the inner magnetosphere, the electric field around the plasmapause can also be estimated using the ensemble transform Kalman filter. We performed an experiment using synthetic images that were generated from the same numerical model under a certain condition. It was confirmed that the condition that generated the synthetic images was successfully reproduced. We also present some results obtained using real EUV imaging data. Finally, we discuss the possibility of estimating the density profile along a magnetic field line. Since each EUV image was taken from a different direction due to the motion of the IMAGE satellite, we could obtain the information on the density profile along a field line by combining multiple images. C1 [Nakano, S.; Higuchi, T.] Res Org Informat & Syst, Inst Stat Math, Tachikawa, Tokyo, Japan. [Nakano, S.; Higuchi, T.] Grad Univ Adv Studies, Sch Multidisciplinary Sci, Hayama, Kanagawa, Japan. [Nakano, S.] Univ Reading, Dept Meteorol, Reading, Berks, England. [Fok, M-C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brandt, P. C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Nakano, S (reprint author), Res Org Informat & Syst, Inst Stat Math, Tachikawa, Tokyo, Japan. EM shiny@ism.ac.jp RI Brandt, Pontus/N-1218-2016; OI Brandt, Pontus/0000-0002-4644-0306; Nakano, Shin'ya/0000-0003-0772-4610 FU Japan Society for the Promotion of Science [24740334]; Young Researcher Overseas Visit Program of the Graduate University for Advanced Studies FX The authors would like to thank B. R. Sandel and the University of Arizona for providing the IMAGE/EUV data. The SOHO/SEM data were provided by the Space Science Center of University of Southern California. The authors would also like to thank N. Ness and the ACE Science Center for providing the ACE data. The SYM-H and Dst indices were provided by the World Data Center for Geomagnetism, Kyoto University. The present study was supported by the Japan Society for the Promotion of Science through a Grant-in-Aid for Young Scientists (B), 24740334, and was partially supported by Young Researcher Overseas Visit Program of the Graduate University for Advanced Studies. NR 48 TC 2 Z9 2 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2014 VL 119 IS 5 BP 3708 EP 3723 DI 10.1002/2013JA019734 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ4DS UT WOS:000337622100035 ER PT J AU Nakano, S Fok, MC Brandt, PC Higuchi, T AF Nakano, S. Fok, M. -C. Brandt, P. C. Higuchi, T. TI Estimation of the helium ion density distribution in the plasmasphere based on a single IMAGE/EUV image SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE plasmasphere; inner magnetosphere; inverse problem; magnetospheric convection ID 17 APRIL 2002; ELECTRON-DENSITY; RING CURRENT; PLASMAPAUSE; MODEL; MAGNETOSPHERE AB We have developed a technique by which to estimate the spatial distribution of plasmaspheric helium ions based on extreme ultraviolet (EUV) data obtained from the IMAGE satellite. The estimation is performed using a linear inversion method based on the Bayesian approach. The global imaging data from the IMAGE satellite enable us to estimate a global two-dimensional distribution of the helium ions in the plasmasphere. We applied this technique to a synthetic EUV image generated from a numerical model. This technique was confirmed to successfully reproduce the helium ion density that generated the synthetic EUV data. We also demonstrate how the proposed technique works for real data using two real EUV images. C1 [Nakano, S.; Higuchi, T.] Res Org Informat & Syst, Inst Stat Math, Tachikawa, Tokyo, Japan. [Nakano, S.; Higuchi, T.] Grad Univ Adv Studies, Sch Multidisciplinary Sci, Hayama, Kanagawa, Japan. [Nakano, S.] Univ Reading, Dept Meteorol, Reading, Berks, England. [Fok, M. -C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brandt, P. C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Nakano, S (reprint author), Res Org Informat & Syst, Inst Stat Math, Tachikawa, Tokyo, Japan. EM shiny@ism.ac.jp RI Brandt, Pontus/N-1218-2016; OI Brandt, Pontus/0000-0002-4644-0306; Nakano, Shin'ya/0000-0003-0772-4610 FU Japan Society for the Promotion of Science [24740334] FX The authors would like to thank B. R. Sandel and the University of Arizona for providing the IMAGE/EUV data. The SOHO/SEM data were provided by the Space Science Center of the University of Southern California. The SYM-H and Dst indices were provided by the World Data Center for Geomagnetism, Kyoto University. This research was supported by the Japan Society for the Promotion of Science through a Grant-in-Aid for Young Scientists (B), 24740334. NR 30 TC 1 Z9 1 U1 2 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2014 VL 119 IS 5 BP 3724 EP 3740 DI 10.1002/2013JA019733 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ4DS UT WOS:000337622100036 ER PT J AU Edquist, KT Korzun, AM Dyakonov, AA Studak, JW Kipp, DM Dupzyk, IC AF Edquist, Karl T. Korzun, Ashley M. Dyakonov, Artem A. Studak, Joseph W. Kipp, Devin M. Dupzyk, Ian C. TI Development of Supersonic Retropropulsion for Future Mars Entry, Descent, and Landing Systems SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID PERFORMANCE AB Recent studies have concluded that Viking-era entry system deceleration technologies are extremely difficult to scale for progressively larger payloads (tens of metric tons) required for human Mars exploration. Supersonic retropropulsion is one of a few developing technologies that may enable future human-scale Mars entry systems. However, in order to be considered as a viable technology for future missions, supersonic retropropulsion will require significant maturation beyond its current state. This paper proposes major milestones for advancing the component technologies of supersonic retropropulsion such that it can be reliably used on Mars technology demonstration missions to land larger payloads than are currently possible using Viking-based systems. The development roadmap includes technology gates that are achieved through ground-based testing and high-fidelity analysis, culminating with subscale flight testing in Earth's atmosphere that demonstrates stable and controlled flight. The component technologies requiring advancement include large engines (100s of kilonewtons of thrust) capable of throttling and gimbaling, entry vehicle aerodynamics and aerothermodynamics modeling, entry vehicle stability and control methods, reference vehicle systems engineering and analyses, and high-fidelity models for entry trajectory simulations. Finally, a notional schedule is proposed for advancing the technology from suborbital free-flight tests at Earth through larger and more complex system-level technology demonstrations and precursor missions at Mars. C1 [Edquist, Karl T.; Korzun, Ashley M.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA. [Dyakonov, Artem A.] Blue Origin LLC, Kent, WA 98032 USA. [Studak, Joseph W.] NASA, Lyndon B Johnson Space Ctr, Prop Syst Branch, Houston, TX 77058 USA. [Kipp, Devin M.] CALTECH, Jet Prop Lab, Entry Descent & Landing Syst & Adv Technol Grp, Pasadena, CA 91109 USA. [Dupzyk, Ian C.] Lunexa LLC, San Francisco, CA 94105 USA. RP Edquist, KT (reprint author), NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, MS 489, Hampton, VA 23681 USA. EM Karl.T.Exiquist@nasa.gov FU Exploration Technology Development and Demonstration Program; NASA Ames Research Center; NASA Johnson Space Center; Jet Propulsion Laboratory FX The authors would like to acknowledge the support of the Exploration Technology Development and Demonstration Program, which was managed at NASA John H. Glenn Research Center at Lewis Field. The work documented herein was performed as part of the program's Entry, Descent, and Landing Technology Development Project, which was managed at NASA Langley Research Center and supported by NASA Ames Research Center, NASA Johnson Space Center, and the Jet Propulsion Laboratory. The authors also wish to acknowledge the support of the Entry, Descent, and Landing Systems Analysis team. Finally, the authors wish to acknowledge the valuable contributions of Jeremy Shidner from Analytical Mechanics Associates, Inc., in Hampton, Virginia; Ravi Prakash from the Jet Propulsion Laboratory, California Institute of Technology in Pasadena, California; and Kerry Zarchi from the NASA Ames Research Center in Mountain View, California. NR 28 TC 3 Z9 4 U1 0 U2 8 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2014 VL 51 IS 3 BP 650 EP 663 DI 10.2514/1.A32715 PG 14 WC Engineering, Aerospace SC Engineering GA AJ2NV UT WOS:000337495500002 ER PT J AU Berry, SA Rhode, MN Edquist, K AF Berry, Scott A. Rhode, Matthew N. Edquist, Karl TI Supersonic Retropropulsion Validation Experiment in the NASA Langley Unitary Plan Wind Tunnel SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID COMPUTATIONAL FLUID-DYNAMICS; MARS ENTRY; DESCENT AB The development of supersonic retropropulsion, an enabling technology for heavy payload exploration missions to Mars, is the focus of the present paper. A new experimental model, intended to provide computational fluid dynamics model validation data, was recently designed for the Langley Research Center Unitary Plan Wind Tunnel test section 2. Pretest analyses using modern computational fluid and thermal analysis tools were instrumental for sizing., and refining the model, over the Mach number range of 2.4-4.6, such that tunnel blockage and internal flow separation issues would be minimized. A 5-in.-diam 70 deg sphere-cone forebody, which accommodates up to four 4 : 1 area ratio nozzles, followed by a 9.55-in.-long cylindrical aftbody, was developed for this study based on the computational results. The model was designed to allow for a large number of surface pressure measurements on the forebody and aftbody. Supplemental data included high-speed schlieren video and internal pressures and temperatures. The run matrix was developed to allow for the quantification of various sources of experimental uncertainty, such as random errors due to run-to-run variations and bias errors due to flowfield or model misalignments Observations and trends from this initial test in the Unitary Plan Wind Tunnel are presented. C1 [Berry, Scott A.; Rhode, Matthew N.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. [Edquist, Karl] NASA, Langley Res Ctr, Atmospher Hight & Entry Syst Branch, Hampton, VA 23681 USA. RP Berry, SA (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, M-S 408A, Hampton, VA 23681 USA. FU NASA's Exploration Technology Development and Demonstration (ETDD) Program; NASA's Fundamental Aeronautics Program (FAP); ETDD's Entry, Descent, and Landing Technology Development Project; FAP's Hypersonics Project FX The authors would like to acknowledge the support of NASA's Exploration Technology Development and Demonstration (ETDD) Program and Fundamental Aeronautics Program (FAP). ETDD's Entry, Descent, and Landing Technology Development Project and FAP's Hypersonics Project, both managed at NASA Langley Research Center, supported the work documented herein. Furthermore, the following individuals were instrumental in this experimental endeavor: Chris Laws, Courtney Spells, Andrew McCrea, Bil Kleb, Guy Schauerhamer, Kerry Trumble, Bill Oberkampf, Ashley Korzun, Ruth Amundsen, Aaron Fuchs, Bryan Falman, Ricky Hall, Paul Bagby, and Steve Jones. NR 24 TC 4 Z9 4 U1 2 U2 5 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2014 VL 51 IS 3 BP 664 EP 679 DI 10.2514/1.A32649 PG 16 WC Engineering, Aerospace SC Engineering GA AJ2NV UT WOS:000337495500003 ER PT J AU Zarchi, KA Schauerhamert, DG Kleb, WL Carlson, JR Edquist, KT AF Zarchi, Kerry A. Schauerhamert, Daniel G. Kleb, William L. Carlson, Jan-Renee Edquist, Karl T. TI Analysis of Navier-Stokes Codes Applied to Supersonic Retropropulsion Wind-Tunnel Test SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID MARS ENTRY; DESCENT AB Advancement of supersonic retropropulsion as a technology will rely heavily on the ability of computational methods to accurately predict vehicle aerodynamics during atmospheric descent, where supersonic retropropulsion will be employed. A wind-tunnel test at the NASA Langley Unitary Plan Wind Tunnel was specifically designed to aid in the support of Navier-Stokes codes for supersonic retropropulsion applications. Three computational fluid dynamics codes [data parallel line relaxation, fully unstructured Navier-Stokes three-dimensional, and overset grid flow solver] were exercised for multiple nozzle configurations for a range of freestream Mach numbers and nozzle thrust coefficients. The computational fluid dynamics pretest analysis of this wind-tunnel test aided in the test model design process by identifying the potential for tunnel blockage or unstart, of liquefaction within the plume, and of separation occurring at the internal fingers of the nozzles. This analysis led to a reduced model diameter, heating of the plenum, and reducing the nozzle area ratio, and the requirement to radius the corners at the fingers, to counter these potentials, respectively. Comparisons to test data were used to determine the existing capability of the codes to accurately model this complex flow, identify modeling shortcomings, and gain insight into the computational requirements necessary for correctly computing these flows. All three codes predict similar surface pressure coefficients and flowfield structures, such as jet termination shock, interface, bow shocks, and recirculation regions. However, the codes differ on the level of unsteadiness predicted. C1 [Zarchi, Kerry A.] NASA, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA. [Schauerhamert, Daniel G.] Jacobs Technol Inc, Appl Aerosci & Computat Fluid Dynam Branch, Houston, TX 77058 USA. [Kleb, William L.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. [Carlson, Jan-Renee] NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA. [Edquist, Karl T.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA. RP Zarchi, KA (reprint author), NASA, Ames Res Ctr, Aerothermodynam Branch, Mail Stop 230-2, Moffett Field, CA 94035 USA. NR 37 TC 3 Z9 3 U1 1 U2 4 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2014 VL 51 IS 3 BP 680 EP 692 DI 10.2514/1.A32744 PG 13 WC Engineering, Aerospace SC Engineering GA AJ2NV UT WOS:000337495500004 ER PT J AU Schauerhamer, DG Zarchi, KA Kleb, WL Carlson, JR Edquist, KT AF Schauerhamer, Daniel Guy Zarchi, Kerry A. Kleb, William L. Carlson, Jan-Renee Edquist, Karl. T. TI Supersonic Retropropulsion Computational Fluid Dynamics Validation with Langley 4 x 4 Foot Test Data SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID UNSTRUCTURED GRIDS; TURBULENT FLOWS; MARS ENTRY; DESCENT AB Validation of computational fluid dynamics for supersonic retropropulsion is shown through the comparison of three Navier-Stokes solvers and wind-tunnel test results. The test was designed specifically for computational fluid dynamics validation and was conducted in the NASA Langley Research Center supersonic 4 x 4 foot Unitary Plan Wind Tunnel. The test includes variations in the number of nozzles, Mach and Reynolds numbers, thrust coefficient, and angles of orientation. Code-to-code and code-to-test comparisons are encouraging, and possible error sources are discussed. C1 [Schauerhamer, Daniel Guy] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Zarchi, Kerry A.] NASA, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA. [Kleb, William L.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. [Carlson, Jan-Renee] NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA. [Edquist, Karl. T.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA. RP Schauerhamer, DG (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. FU Exploration Technology Development and Demonstration (ETDD) Program; NASA Ames Research Center; NASA Johnson Space Center; Jet Propulsion Laboratory FX Pieter G. Buning of NASA Langley Research Center, Hampton, Virginia; Phillip C. Stuart and Darby J. Vicker of NASA Johnson Space Center, Houston, Texas; and Thomas M. Booth of Jacobs Technology, Houston, Texas, provided valuable guidance on gridding and solver best practices for OVERFLOW. William T. Jones of NASA Langley Research Center, Hampton, Virginia, provided the GridEx/batchEx unstructured grid generation framework and helped with its application to generate FUN3D grids. Todd R. White and Andrew J. Hyatt of ERC Inc., Moffett Field, California, helped develop DPLR best practices and provided overset gridding assistance for DPLR cases. David A. Saunders of ERC Inc., Moffett Field, California, developed the code used for OVERFLOW and DPLR simulated Schlieren/shadowgraph visualizations. The authors would like to acknowledge the support of the Exploration Technology Development and Demonstration (ETDD) Program, which was managed at NASA Glenn Research Center. The work documented herein was performed as part of ETDD's Entry, Descent, and Landing Technology Development Project, which was managed at NASA Langley Research Center and supported by NASA Ames Research Center, NASA Johnson Space Center, and the Jet Propulsion Laboratory. NR 32 TC 3 Z9 3 U1 0 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2014 VL 51 IS 3 BP 693 EP 714 DI 10.2514/1.A32693 PG 22 WC Engineering, Aerospace SC Engineering GA AJ2NV UT WOS:000337495500005 ER PT J AU Codoni, JR Berry, SA AF Codoni, Joshua R. Berry, Scott A. TI Supersonic Retropropulsion Dynamic Data Analysis from NASA Langley Unitary Plan Wind Tunnel SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID ENTRY AB A supersonic retropropulsion experiment was recently conducted at NASA Langley Research Center's Unitary Plan Wind Tunnel, test section 2, for a range of Mach numbers from 2.4 to 4.6. A 5-in.-diam 70 deg sphere-cone forebody with a 9.55 in. cylindrical aftbody section was the experimental model used, which is capable of multiple retrorocket configurations. These configurations include a single central nozzle on the center point of the forebody, three nozzles at the forebody half-radius, and a combination of the first two configurations. A series of measurements were achieved through various instrumentation, including forebody and aftbody surface pressures, internal pressures and temperatures, and high-speed schlieren visualization. Several high-speed pressure transducers on the forebody and in the plenum were implemented to look at unsteady flow effects. The following work focuses on analyzing frequency traits due to the unsteady flow for a range of thrust coefficients for single-, tri-, and quadnozzle test cases at a freestream Mach number of 4.6 and an angle of attack ranging from 0 to +20 deg. This analysis uses MATLAB (R)'s fast Fourier transform, Welch's method (modified average of a periodogram), to create a power spectral density and analyze any high-speed pressure transducer frequency traits due to the unsteady flow. C1 [Codoni, Joshua R.] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22903 USA. [Berry, Scott A.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. RP Codoni, JR (reprint author), Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22903 USA. NR 19 TC 0 Z9 0 U1 2 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2014 VL 51 IS 3 BP 715 EP 723 DI 10.2514/1.A32619 PG 9 WC Engineering, Aerospace SC Engineering GA AJ2NV UT WOS:000337495500006 ER PT J AU Berry, SA Rhode, MN Edquist, KT AF Berry, Scott A. Rhode, Matthew N. Edquist, Karl T. TI Supersonic Retropropulsion Experimental Results from NASA Ames 9 x 7 Foot Supersonic Wind Tunnel SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID FOURIER-TRANSFORM; MARS ENTRY; DESCENT AB Supersonic retropropulsion was experimentally examined in the Ames Research Center 9 x 7 Foot Supersonic Wind Tunnel at Mach 1.8 and 2.4. The model, previously designed for and tested in the Langley Research Center Unitary Plan Wind Tunnel at Mach 2.4, 3.5, and 4.6, was a 5-in.-diam 70 deg sphere-cone forebody with a 9.55-in.-long cylindrical aftbody. The forebody was designed to accommodate up to four 4:1 area ratio nozzles, one on the model centerline and the other three on the half-radius spaced 120 deg apart. Surface pressure and flow visualization were the primary measurements, including high-speed data to investigate the dynamics of the interactions between the bow and nozzle shocks. Three blowing configurations were tested with thrust coefficients up to 10 and angles of attack up to 20 deg. Results and observations from the test are provided. C1 [Berry, Scott A.; Rhode, Matthew N.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. [Edquist, Karl T.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA. RP Berry, SA (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, Mail Stop 408a, Hampton, VA 23681 USA. FU NASA's Exploration Technology Development and Demonstration (ETDD) Program; NASA's Fundamental Aeronautics Program (FAP) FX The authors would like to acknowledge the support of NASA's Exploration Technology Development and Demonstration (ETDD) Program and Fundamental Aeronautics Program (FAP). The work documented herein was performed jointly by both ETDD's Entry, Descent, and Landing Technology Development Project and FAP's Hypersonics Project, both managed at NASA Langley Research Center. Furthermore, the following individuals were instrumental to this experimental effort: Joe Giuliana, Paul Tucker, Kerry Trumble, Artem Dyakonov, Josh Codoni, Chris Cordell, Guy Schauerhamer, Ashley Korzun, Jennifer Everett, Max Amaya, Tom Bridge, James Brown, Bill Browning, Jay Carolino, Maureen Delgado, Joel Hoffman, John Holmberg, Rudy Jaklitsch, Matt Krakenburg, David Lam, Pam Pfohl, Scott Richey, Tom Romer, Nestor Rostran, Art Silva, Robin Townsend, Dale Tuttle, Jonathan VanHorn, Bill VanZuylen, and Tom Volden. NR 24 TC 1 Z9 1 U1 2 U2 4 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2014 VL 51 IS 3 BP 724 EP 734 DI 10.2514/1.A32650 PG 11 WC Engineering, Aerospace SC Engineering GA AJ2NV UT WOS:000337495500007 ER PT J AU Schauerhamer, DG Zarchi, KA Kleb, WL Edquist, KT AF Schauerhamer, Daniel Guy Zarchi, Kerry A. Kleb, William L. Edquist, Karl T. TI Supersonic Retropropulsion Computational-Fluid-Dynamics Validation with Ames 9 x 7 Foot Test Data SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID UNSTRUCTURED GRIDS; TURBULENT FLOWS; MARS ENTRY; DESCENT AB A validation study of computational fluid dynamics for supersonic retropropulsion was conducted using three Navier-Stokes flow solvers. The study compared results from the computational-fluid-dynamics codes to each other and to wind-tunnel test data obtained in the NASA Ames Research Center 9 x 7 ft Unitary Plan Wind Tunnel. Comparisons include surface pressure coefficient as well as unsteady plume effects and cover a range of Mach numbers, levels of thrust, and angles of orientation for zero-, one-, three-, and four-nozzle configurations. Flow-structure behavior changed with thrust and angle of orientation for all nozzle configurations. In general, the solvers compared best with the test data for the steadier cases of the one-nozzle and high-thrust three-nozzle configurations. Deviation in surface pressure was noted for the more unsteady cases and near transitions in behavioral modes. Strengths and weaknesses of the solvers are identified, and possible error sources are discussed. C1 [Schauerhamer, Daniel Guy] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Zarchi, Kerry A.] NASA, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA. [Kleb, William L.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. [Edquist, Karl T.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA. RP Schauerhamer, DG (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. FU Exploration Technology Development and Demonstration (ETDD) Program; NASA Ames Research Center; NASA Johnson Space Center; Jet Propulsion Laboratory FX Pieter G. Burling of NASA Langley Research Center, Hampton, Virginia, and Phillip C. Stuart, Thomas M. Booth, and Darby J. Vicker of NASA Johnson Space Center, Houston, Texas provided valuable guidance on gridding and solver best practices for OVERFLOW. William T. Jones of NASA Langley Research Center, Hampton, Virginia, provided the GridEx/batchEx unstructured grid-generation framework and helped with its application to generate FUN3D grids. Todd R. White and Andrew J. Hyatt of ERC Inc., Moffett Field, California, helped develop DPLR best practices and provided overset gridding assistance for DPLR cases. David A. Saunders of ERC Inc., Moffett Field, California, developed the code used for OVERFLOW and DPLR simulated Schlieren/shadowgraph visualizations. The authors would like to acknowledge the support of the Exploration Technology Development and Demonstration (ETDD) Program, which was managed at NASA Glenn Research Center. The work documented herein was performed as part of ETDD's Entry, Descent, and Landing Technology Development Project, which was managed at NASA Langley Research Center and supported by NASA Ames Research Center, NASA Johnson Space Center, and the Jet Propulsion Laboratory. NR 22 TC 2 Z9 2 U1 1 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2014 VL 51 IS 3 BP 735 EP 749 DI 10.2514/1.A32694 PG 15 WC Engineering, Aerospace SC Engineering GA AJ2NV UT WOS:000337495500008 ER PT J AU Chen, YK Gokcen, T AF Chen, Yih-Kanq Goekcen, Tahir TI Implicit Coupling Approach for Simulation of Charring Carbon Ablators SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID THERMAL RESPONSE; SHAPE CHANGE; ABLATION; PROGRAM; MODEL AB This study demonstrates that coupling of a material thermal response code and a flow solver with nonequilibrium gas surface interaction for simulation of charring carbon ablators can be performed using an implicit approach. The material thermal response code used in this study, is the three-dimensional version of fully implicit ablation and thermal response program, which predicts charring material thermal response and shape change on hypersonic space vehicles. The flow code solves the reacting Navier-Stokes equations using data-parallel line relaxation method. Coupling between the material response and flow codes is performed by solving the surface mass balance in the flow solver and the surface energy balance in the material response code. Thus, the material surface recession is predicted in the flow code, and the surface temperature and pyrolysis gas injection rate are computed in the material response code. It is demonstrated that the time-lagged explicit approach is sufficient for simulations at low surface heating conditions, in which the surface ablation rate is not a strong function of the surface temperature. At elevated surface heating conditions, the implicit approach has to be taken because the carbon ablation rate becomes a stiff function of the surface temperature, and thus the explicit approach appears to be inappropriate, resulting in severe numerical oscillations of predicted surface temperature. Implicit coupling for simulation of arc-jet models is performed, and the predictions are compared with measured data. Implicit coupling for trajectory-based simulation of Stardust forebody heat shield is also conducted. The predicted stagnation point total recession is compared with that predicted using the chemical equilibrium surface assumption. C1 [Chen, Yih-Kanq] NASA, Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA. [Goekcen, Tahir] ERC Inc, Aerothermodynam Branch, Moffett Field, CA 94035 USA. RP Chen, YK (reprint author), NASA, Ames Res Ctr, Thermal Protect Mat Branch, MS 234-1, Moffett Field, CA 94035 USA. FU NASA Fundamental Aeronautics Program under Hypersonics Entry, Descending, and Landing (EDL) Project FX This work is funded by the NASA Fundamental Aeronautics Program under the Hypersonics Entry, Descending, and Landing (EDL) Project. NR 24 TC 2 Z9 2 U1 0 U2 4 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2014 VL 51 IS 3 BP 779 EP 788 DI 10.2514/1.A32753 PG 10 WC Engineering, Aerospace SC Engineering GA AJ2NV UT WOS:000337495500011 ER PT J AU Mazaheri, A Bruce, WE Mesick, NJ Sutton, K AF Mazaheri, Alireza Bruce, Walter E., III Mesick, Nathaniel J. Sutton, Kenneth TI Methodology for Flight-Relevant Arc-Jet Testing of Flexible Thermal Protection Systems SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article AB A methodology to correlate flight aeroheating environments to the arc-jet environment is presented. For a desired hot-wall flight heating rate, the methodology provides the arc-jet bulk enthalpy for the corresponding cold-wall heating rate. A series of analyses were conducted to examine the effects of the test sample model holder geometry to the overall performance of the test sample. The analyses were compared with arc-jet test samples, and challenges and issues are presented. The transient flight environment was calculated for the Hypersonic Inflatable Aerodynamic Decelerator Earth Atmospheric Reentry Test vehicle, which is a planned demonstration vehicle using a large inflatable, flexible thermal protection system to reenter the Earth's atmosphere from the International Space Station. A series of correlations were developed to define the relevant arc-jet test environment to properly approximate the vehicle flight environment. The computed arc-jet environments were compared with the measured arc-jet values to define the uncertainty of the correlated environment. The results show that, for a given flight surface heat flux and a fully catalytic thermal protection system, the flight-relevant arc-jet heat flux increases with the arc-jet bulk enthalpy, while for a noncatalytic thermal protection system, the arc-jet heat flux decreases with the bulk enthalpy. C1 [Mazaheri, Alireza] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. [Bruce, Walter E., III] NASA, Langley Res Ctr, Struct & Thermal Syst Branch, Hampton, VA 23681 USA. [Mesick, Nathaniel J.] Sci Syst & Applicat Inc, Mech Syst Branch, Hampton, VA 23666 USA. [Sutton, Kenneth] Natl Inst Aerosp, Aerothermodynam Branch, Hampton, VA 23666 USA. RP Mazaheri, A (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, M-S 408A, Hampton, VA 23681 USA. EM Ali.R.Mazatieri@nasa.gov FU Hypersonic Inflatable Aerodynamic Decelerator (HIAD) project; HIAD Earth Atmospheric Reentry Test project FX The present work was supported by the Hypersonic Inflatable Aerodynamic Decelerator (HIAD) and the HIAD Earth Atmospheric Reentry Test projects. The authors would also like to thank John R. Simms and Matthew P. Kardell at the Boeing Large Core Arc Tunnel facility who successfully programmed the arc heater controller to match the arc-jet heat flux and flight surface pressure from the presented correlations. Thanks also go to the reviewers for their thorough review of the paper and constructive comments. NR 18 TC 1 Z9 1 U1 2 U2 7 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2014 VL 51 IS 3 BP 789 EP 800 DI 10.2514/1.A32721 PG 12 WC Engineering, Aerospace SC Engineering GA AJ2NV UT WOS:000337495500012 ER PT J AU Palmer, G Prabhu, D Cruden, BA AF Palmer, Grant Prabhu, Dinesh Cruden, Brett A. TI Aeroheating Uncertainties in Uranus and Saturn Entries by the Monte Carlo Method SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID TRANSPORT PROPERTY COMPUTATIONS; RECOMMENDED COLLISION INTEGRALS; VIBRATIONAL-RELAXATION; VOYAGER MEASUREMENTS; ELASTIC-SCATTERING; HELIUM ABUNDANCE; CHARGE-TRANSFER; HYDROGEN; MARS; HE AB The 2013-2022 decadal survey ("Vision and Voyages for Planetary Science in the Decade 2013-2022," National Research Council Rept., National Academy Press, Washington, D.C., 2011) for planetary exploration has identified probe missions to Uranus and Saturn as high priorities. This work endeavors to examine the uncertainty for determining aeroheating in such entry environments. Representative entry trajectories are constructed using the TRAJ software. Flowfields at selected points on the trajectories are then computed using the data parallel line relaxation computational fluid dynamics code. A Monte Carlo study is performed on the data parallel line relaxation input parameters to determine the uncertainty in the predicted aeroheating, and correlation coefficients are examined to identify which input parameters show the most influence on the uncertainty. A review of the present best practices for input parameters (for example, transport coefficient and vibrational relaxation time) is also conducted. It is found that the 2 sigma-uncertainty for heating on the Uranus entry is no more than 2.1%, assuming an equilibrium catalytic wall, with the uncertainty being determined primarily by diffusion and an H-2 recombination rate within the boundary layer. However, if the wall is assumed to be partially catalytic or noncatalytic, this uncertainty may increase to as large as 18%. The catalytic wall model can contribute over three times the change in heat flux and a 20% variation in film coefficient. Therefore, coupled material response/fluid dynamic models are recommended for this problem. It was also found that much of this variability is artificially suppressed when a constant Schmidt number approach is implemented. Because the boundary layer is reacting, it is necessary to employ self-consistent effective binary diffusion to obtain a correct thermal transport solution. For Saturn entries, the 2 sigma uncertainty for convective heating was less than 3.7%. The major uncertainty driver was dependent on shock temperature/velocity, changing from boundary-layer thermal conductivity to diffusivity and then to shock-layer ionization rate as velocity increases. While radiative heating for Uranus entry was negligible, the nominal solution for Saturn computed up to 20% radiative heating at the highest velocity examined. The radiative heating followed a nonnormal distribution, with up to a three-time variation in magnitude. This uncertainty is driven by the H-2 dissociation rate, as H-2 that persists in the hot nonequilibrium zone contributes significantly to radiation. C1 [Palmer, Grant; Prabhu, Dinesh; Cruden, Brett A.] ERC Inc, Moffett Field, CA 94035 USA. RP Palmer, G (reprint author), NASA, Ames Res Ctr, Washington, DC 20546 USA. FU NASA [NNA10DE12C] FX The authors are supported by NASA contract NNA10DE12C to ERC, Inc. The authors would like to thank Helen Hwang, Suman Muppidi, and Aaron Brandis for useful discussions. Michael Barnhardt is acknowledged for assistance with updating the data parallel line relaxation databases and running test case comparisons. NR 43 TC 0 Z9 0 U1 0 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2014 VL 51 IS 3 BP 801 EP 814 DI 10.2514/1.A32768 PG 14 WC Engineering, Aerospace SC Engineering GA AJ2NV UT WOS:000337495500013 ER PT J AU Yang, HQ Peugeot, J AF Yang, H. Q. Peugeot, John TI Propellant Sloshing Parameter Extraction from Computational-Fluid-Dynamics Analysis SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID BEHAVIOR AB Propellant slosh is a potential source of disturbance critical to the stability of space vehicles. The sloshing dynamics are typically represented by a mechanical model of a spring-mass-damper system. This mechanical model is then included in the equation of motion of the entire vehicle for guidance, navigation and control analysis. The typical parameters required by the mechanical model include the natural frequency of the sloshing, sloshing mass, sloshing mass center coordinates, and critical damping coefficient. During the 1960s in the U.S. space program, these parameters were computed either from analytical solutions for simple geometries or by experimental testing for the subscale configurations. The purpose of this work is to demonstrate the soundness of a computational-fluid-dynamics approach in modeling the detailed fluid dynamics of tank sloshing and the excellent accuracy in extracting mechanical properties for different tank configurations and at different fill levels. As the first attempt, the work focuses mainly on the identification of the natural frequency and the equivalent slosh mass from the simulations. The paper presents verification against the analytical solution of natural frequency for two- and three-dimensional straight cylinders, and validation against experimental results for subscale Centaur Liquid Oxygen and Liquid Hydrogen tanks with and without baffles. The results show that computational-fluid-dynamics technology can provide accurate mechanical parameters for any tank configuration, and is especially valuable to the future design of propellant tanks. C1 [Yang, H. Q.] CFD Res Corp, Huntsville, AL 35805 USA. [Peugeot, John] NASA, George C Marshall Space Flight Ctr, Fluid Dynam Branch ER42, Huntsville, AL 35812 USA. RP Yang, HQ (reprint author), CFD Res Corp, 215 Wynn Dr, Huntsville, AL 35805 USA. EM hqy@cfdrc.com; John.W.Peugeot@nasa.gov FU Jacobs Engineering NASA Marshall Space Flight Center (MSFC) Engineering, Science, and Technical Services (ESTS) [NNM05AB50C] FX This study was performed under a task order of the Jacobs Engineering NASA Marshall Space Flight Center (MSFC) Engineering, Science, and Technical Services (ESTS) contract NNM05AB50C. Ram Ramachandran was the Jacobs ESTS Task Lead, and Jeff West (MSFC Fluid Dynamics Branch, ER42) was the NASA MSFC Task Monitor. NR 15 TC 0 Z9 0 U1 1 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2014 VL 51 IS 3 BP 908 EP 916 DI 10.2514/1.A32608 PG 9 WC Engineering, Aerospace SC Engineering GA AJ2NV UT WOS:000337495500023 ER PT J AU Yang, YM Komjathy, A Langley, RB Vergados, P Butala, MD Mannucci, AJ AF Yang, Yu-Ming Komjathy, Attila Langley, Richard B. Vergados, Panagiotis Butala, Mark D. Mannucci, Anthony J. TI The 2013 Chelyabinsk meteor ionospheric impact studied using GPS measurements SO RADIO SCIENCE LA English DT Article DE remote sensing; GPS; total electron content; ionospheric disturbance; asteriod impact; natural hazards AB On 15 February 2013, the Chelyabinsk meteor event (the largest in size since 1908) provided a unique opportunity to observe ionospheric perturbations associated with the ablation and ionospheric impact of the meteor using GPS measurements. The hypersonic bolide generated powerful shock waves while acoustic perturbations in the atmosphere led to the upward propagation of acoustic and gravity waves into the ionosphere. In our research, we applied two different techniques to detect ionospheric disturbances in dual-frequency global positioning system (GPS) measurements during the meteor impact event. The data were collected from near-field GPS networks in Russia, GPS Earth Observation Network (GEONET) in Japan, and Plate Boundary Observatory (PBO) stations in the coterminous U.S. Using a novel wavelet coherence detection technique, we were able to identify three different wave trains in the measurements collected from the nearest GPS station to the meteor impact site, with frequencies of approximately 4.0-7.8 mHz, 1.0 -2.5 mHz, and 2.7-11 mHz at 03:30 UTC. We estimated the speed and direction of arrival of the total electron content (TEC) disturbances by cross-correlating TEC time series for every pair of stations in several areas of the GEONET and PBO networks. The results may be characterized as three different types of traveling ionospheric disturbances (TIDs). First, the higher-frequency (4.0-7.8 mHz) disturbances were observed around the station ARTU in Arti, Russia (56.43 degrees N, 58.56 degrees E), with an estimated mean propagation speed of about 862 +/- 65m/s (with 95% confidence interval). Another type of TID disturbance related to the wave trains was identified in the lower frequency band (1.0-2.5 mHz), propagating with a mean speed of 362 +/- 23m/s. The lower frequency ionospheric perturbations were observed at distances of 300-1500km away from Chelyabinsk. The third type of TID wave train was identified using the PBO stations in the relative short-period range of 1.5-6min (2.7-11 mHz) with a mean propagation speed of 733 +/- 36m/s. The observed short-period ionospheric perturbations in the U.S. region is, to the best of our knowledge, the first observational evidence of the coincident the long-range meteor-generated infrasound signals propagating in the ionosphere. C1 [Yang, Yu-Ming; Komjathy, Attila; Vergados, Panagiotis; Butala, Mark D.; Mannucci, Anthony J.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. [Komjathy, Attila; Langley, Richard B.] Univ New Brunswick, Dept Geodesy & Geomat Engn, Fredericton, NB, Canada. RP Yang, YM (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. EM oscar.yang@jpl.nasa.gov NR 23 TC 7 Z9 7 U1 2 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 EI 1944-799X J9 RADIO SCI JI Radio Sci. PD MAY PY 2014 VL 49 IS 5 BP 341 EP 350 DI 10.1002/2013RS005344 PG 10 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA AJ4EN UT WOS:000337624700004 ER PT J AU Manney, GL Hegglin, MI Daffer, WH Schwartz, MJ Santee, ML Pawson, S AF Manney, Gloria L. Hegglin, Michaela I. Daffer, William H. Schwartz, Michael J. Santee, Michelle L. Pawson, Steven TI Climatology of Upper Tropospheric-Lower Stratospheric (UTLS) Jets and Tropopauses in MERRA SO JOURNAL OF CLIMATE LA English DT Article DE Atmospheric circulation; Jets; Stratophere-troposphere coupling; Tropopause; Upper troposphere; Data assimilation ID EDDY-DRIVEN JET; NORTHERN-HEMISPHERE WINTER; BREAKING ROSSBY WAVES; POLAR VORTEX; SOUTHERN-HEMISPHERE; TROPICAL PACIFIC; DECADAL CHANGES; WESTERLY JET; WATER-VAPOR; OZONE LOSS AB A global climatology (1979-2012) from the Modern-Era Retrospective Analysis for Research and Applications (MERRA) shows distributions and seasonal evolution of upper tropospheric jets and their relationships to the stratospheric subvortex and multiple tropopauses. The overall climatological patterns of upper tropospheric jets confirm those seen in previous studies, indicating accurate representation of jet stream dynamics in MERRA. The analysis shows a Northern Hemisphere (NH) upper tropospheric jet stretching nearly zonally from the mid-Atlantic across Africa and Asia. In winter-spring, this jet splits over the eastern Pacific, merges again over eastern North America, and then shifts poleward over the North Atlantic. The jets associated with tropical circulations are also captured, with upper tropospheric westerlies demarking cyclonic flow downstream from the Australian and Asian monsoon anticyclones and associated easterly jets. Multiple tropopauses associated with the thermal tropopause break commonly extend poleward from the subtropical upper tropospheric jet. In Southern Hemisphere (SH) summer, the tropopause break, along with a poleward-stretching secondary tropopause, often occurs across the tropical westerly jet downstream of the Australian monsoon region. SH high-latitude multiple tropopauses, nearly ubiquitous in June-July, are associated with the unique polar winter thermal structure. High-latitude multiple tropopauses in NH fall-winter are, however, sometimes associated with poleward-shifted upper tropospheric jets. The SH subvortex jet extends down near the level of the subtropical jet core in winter and spring. Most SH subvortex jets merge with an upper tropospheric jet between May and December; although much less persistent than in the SH, merged NH subvortex jets are common between November and April. C1 [Manney, Gloria L.] NorthWest Res Associates, Socorro, NM USA. [Manney, Gloria L.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA. [Hegglin, Michaela I.] Univ Reading, Reading, Berks, England. [Daffer, William H.; Schwartz, Michael J.; Santee, Michelle L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Pawson, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Manney, GL (reprint author), New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. EM manney@nwra.com RI Pawson, Steven/I-1865-2014; Hegglin, Michaela/D-7528-2017 OI Pawson, Steven/0000-0003-0200-717X; Hegglin, Michaela/0000-0003-2820-9044 FU National Aeronautics and Space Administration FX Thanks to the MLS team at JPL, especially Nathaniel Livesey, Brian Knosp, Ryan Fuller, Vince Perun, and Robert Thurstans, for scientific, data management/processing, and computational support. Thanks to NASA's High-End Computing Program for computational resources used for MERRA, to Michele Rienecker and other colleagues at NASA's GMAO for their advice on using MERRA, and to the Goddard DAAC for distributing the data. Thanks to Dennis Hartmann, Brian Hoskins, Kirstin Kruger, Ken Minschwaner, Dave Raymond, Ted Shepherd, and Gui-Ying Yang for helpful discussions. Thanks to the three anonymous reviewers for very helpful comments. Work at the Jet Propulsion Laboratory, California Institute of Technology, was done under contract with the National Aeronautics and Space Administration. NR 100 TC 8 Z9 8 U1 3 U2 19 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD MAY PY 2014 VL 27 IS 9 BP 3248 EP 3271 DI 10.1175/JCLI-D-13-00243.1 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AI9RU UT WOS:000337272700007 ER PT J AU Phojanamongkolkij, N Kato, S Wielicki, BA Taylor, PC Mlynczak, MG AF Phojanamongkolkij, Nipa Kato, Seiji Wielicki, Bruce A. Taylor, Patrick C. Mlynczak, Martin G. TI A Comparison of Climate Signal Trend Detection Uncertainty Analysis Methods SO JOURNAL OF CLIMATE LA English DT Article DE Climate records; Forecasting techniques; Statistical forecasting; Model comparison ID ENERGY SYSTEM INSTRUMENT; RADIATION BUDGET; CLOUDS; MODELS; OZONE AB Two climate signal trend analysis methods are the focus of this paper. The uncertainty of trend estimate from these two methods is investigated using Monte Carlo simulation. Several theoretically and randomly generated series of white noise, first-order autoregressive and second-order autoregressive, are explored. The choice of method that is most appropriate for the time series of interest depends upon the autocorrelation structure of the series. If the structure has its autocorrelation coefficients decreased with increasing lags (i.e., an exponential decay pattern), then the method of Weatherhead et al. is adequate. If the structure exhibits a decreasing sinusoid pattern of coefficient with lags (or a damped sinusoid pattern) or a mixture of both exponential decay and damped sinusoid patterns, then the method of Leroy et al. is recommended. The two methods are then applied to the time series of monthly and globally averaged top-of-the-atmosphere (TOA) irradiances for the reflected solar shortwave and emitted longwave regions, using radiance observations made by Clouds and the Earth's Radiant Energy System (CERES) instruments during March 2000 through June 2011. Examination of the autocorrelation structures indicates that the reflected shortwave region has an exponential decay pattern, while the longwave region has a mixture of exponential decay and damped sinusoid patterns. Therefore, it is recommended that the method of Weatherhead et al. is used for the series of reflected shortwave irradiances and that the method of Leroy et al. is used for the series of emitted longwave irradiances. C1 [Phojanamongkolkij, Nipa] NASA, Langley Res Ctr, Syst Engn & Engn Methods Branch, Hampton, VA 23681 USA. [Kato, Seiji; Wielicki, Bruce A.; Taylor, Patrick C.; Mlynczak, Martin G.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. RP Phojanamongkolkij, N (reprint author), NASA, Langley Res Ctr, MS 131, Hampton, VA 23681 USA. EM nipa.phojanamongkolkij@nasa.gov RI Taylor, Patrick/D-8696-2015; Richards, Amber/K-8203-2015 OI Taylor, Patrick/0000-0002-8098-8447; FU NASA CLARREO project FX We thank Dr. Stephen Leroy for useful discussions and all reviewers' comments for valuable insights. We also thank Ms. Amber Richards and Dr. Joe A. Walker for proof reading the manuscript. This work is supported by the NASA CLARREO project. NR 18 TC 0 Z9 0 U1 0 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD MAY PY 2014 VL 27 IS 9 BP 3363 EP 3376 DI 10.1175/JCLI-D-13-00400.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AI9RU UT WOS:000337272700013 ER PT J AU Iizumi, T Luo, JJ Challinor, AJ Sakurai, G Yokozawa, M Sakuma, H Brown, ME Yamagata, T AF Iizumi, Toshichika Luo, Jing-Jia Challinor, Andrew J. Sakurai, Gen Yokozawa, Masayuki Sakuma, Hirofumi Brown, Molly E. Yamagata, Toshio TI Impacts of El Nino Southern Oscillation on the global yields of major crops SO NATURE COMMUNICATIONS LA English DT Article ID SEA-SURFACE TEMPERATURE; INDIAN-OCEAN; DIPOLE MODE; CLIMATE; PREDICTION; PATTERNS; AGRICULTURE AB The monitoring and prediction of climate-induced variations in crop yields, production and export prices in major food-producing regions have become important to enable national governments in import-dependent countries to ensure supplies of affordable food for consumers. Although the El Nino/Southern Oscillation (ENSO) often affects seasonal temperature and precipitation, and thus crop yields in many regions, the overall impacts of ENSO on global yields are uncertain. Here we present a global map of the impacts of ENSO on the yields of major crops and quantify its impacts on their global-mean yield anomalies. Results show that El Nino likely improves the global-mean soybean yield by 2.1-5.4% but appears to change the yields of maize, rice and wheat by - 4.3 to +0.8%. The global-mean yields of all four crops during La Nina years tend to be below normal (- 4.5 to 0.0%). Our findings highlight the importance of ENSO to global crop production. C1 [Iizumi, Toshichika; Sakurai, Gen] Natl Inst Agroenvironm Sci, Tsukuba, Ibaraki 3058604, Japan. [Luo, Jing-Jia] Bur Meteorol, Ctr Australian Weather & Climate Res, Melbourne, Vic 3008, Australia. [Challinor, Andrew J.] Univ Leeds, Inst Climate & Atmospher Sci, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. [Challinor, Andrew J.] Univ Copenhagen, CGIAR ESSP Program Climate Change, Agr & Food Secur CCAFS, Dept Plant & Environm Sci,Fac Sci, DK-1958 Frederiksberg, Denmark. [Yokozawa, Masayuki] Shizuoka Univ, Grad Sch Engn, Hamamatsu, Shizuoka 4328561, Japan. [Sakuma, Hirofumi] JAMSTEC, Yokohama Inst Earth Sci, Res Inst Global Change, Yokohama, Kanagawa 2360001, Japan. [Sakuma, Hirofumi; Yamagata, Toshio] JAMSTEC, Yokohama Inst Earth Sci, Applicat Lab, Yokohama, Kanagawa 2360001, Japan. [Brown, Molly E.] NASA Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. RP Iizumi, T (reprint author), Natl Inst Agroenvironm Sci, Tsukuba, Ibaraki 3058604, Japan. EM iizumit@affrc.go.jp RI Brown, Molly/M-5146-2013; Yamagata, Toshio/A-1807-2009; Luo, Jing-Jia/B-2481-2008; Yokozawa, Masayuki/O-2829-2014; Challinor, Andrew/C-4992-2008; Brown, Molly/E-2724-2010 OI Brown, Molly/0000-0001-7384-3314; Luo, Jing-Jia/0000-0003-2181-0638; Yokozawa, Masayuki/0000-0001-7053-2465; Challinor, Andrew/0000-0002-8551-6617; Brown, Molly/0000-0001-7384-3314 FU Environment Research and Technology Development Fund of the Ministry of the Environment, Japan [S-10-2] FX We thank P. McIntosh and T. Beer for their comments. T.I and G.S. were supported by the Environment Research and Technology Development Fund (S-10-2) of the Ministry of the Environment, Japan. NR 44 TC 22 Z9 22 U1 4 U2 61 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD MAY PY 2014 VL 5 AR 3712 DI 10.1038/ncomms4712 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AJ0SB UT WOS:000337365100001 PM 24827075 ER PT J AU Datta, DP Sen, S AF Datta, Dhurjati Prasad Sen, Sudip TI Excitation of flow instabilities due to nonlinear scale invariance SO PHYSICS OF PLASMAS LA English DT Article ID MULTIFRACTAL ANALYSIS; PLASMA; INTERMITTENCY; TURBULENCE; DYNAMICS; TIME AB A novel route to instabilities and turbulence in fluid and plasma flows is presented in kinetic Vlasov-Maxwell model. New kind of flow instabilities is shown to arise due to the availability of new kinetic energy sources which are absent in conventional treatments. The present approach is based on a scale invariant nonlinear analytic formalism developed to address irregular motions on a chaotic attractor or in turbulence in a more coherent manner. We have studied two specific applications of this turbulence generating mechanism. The warm plasma Langmuir wave dispersion relation is shown to become unstable in the presence of these multifractal measures. In the second application, these multifractal measures are shown to induce naturally non-Gaussian, i.e., a stretched, Gaussian distribution and anomalous transport for tracer particles from the turbulent advection-diffusion transport equation in a Vlasov plasma flow. (C) 2014 AIP Publishing LLC. C1 [Datta, Dhurjati Prasad] Univ N Bengal, Dept Math, Siliguri 734013, W Bengal, India. [Sen, Sudip] NASA, Natl Inst Aerosp, LaRC, Hampton, VA 23666 USA. [Sen, Sudip] Coll William & Mary, Williamsburg, VA 23187 USA. RP Datta, DP (reprint author), Univ N Bengal, Dept Math, Siliguri 734013, W Bengal, India. EM dp_datta@yahoo.com NR 22 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD MAY PY 2014 VL 21 IS 5 AR 052311 DI 10.1063/1.4880103 PG 10 WC Physics, Fluids & Plasmas SC Physics GA AI7UY UT WOS:000337107200027 ER PT J AU Jorns, BA Hofer, RR AF Jorns, Benjamin A. Hofer, Richard R. TI Plasma oscillations in a 6-kW magnetically shielded Hall thruster SO PHYSICS OF PLASMAS LA English DT Article ID HOLLOW-CATHODE; DISCHARGE; INSTABILITY; DRIFT AB Plasma oscillations from 0-100 kHz in a 6-kW magnetically shielded Hall thruster are experimentally characterized with a high-speed, optical camera. Two modes are identified at 7-12 kHz and 70-90 kHz. The low frequency mode is found to be azimuthally uniform across the thruster face, while the high frequency oscillation is peaked close to the centerline-mounted cathode with an m 1 azimuthal dependence. An analysis of these results in the context of wave-based theory suggests that the low frequency wave is the breathing mode oscillation, while the higher frequency mode is gradient-driven. The effect of these oscillations on thruster operation is examined through an analysis of thruster discharge current and a comparison with published observations from an unshielded variant of the thruster. Most notably, it is found that although the oscillation spectra of the two thrusters are different, they exhibit nearly identical steady-state behavior. (C) 2014 AIP Publishing LLC. C1 [Jorns, Benjamin A.; Hofer, Richard R.] CALTECH, Jet Prop Lab, Elect Prop Grp, Pasadena, CA 91109 USA. RP Jorns, BA (reprint author), CALTECH, Jet Prop Lab, Elect Prop Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM benjamin.a.jorns@jpl.nasa.gov FU In-Space Propulsion Technologies program FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and funded through the In-Space Propulsion Technologies program. The authors would like to acknowledge Ray Swindlehurst and Nowell Niblitt for their assistance in running the experimental facility. We are also grateful to Dr. Dan Goebel and Dr. Ioannis Mikellides for providing data on the H6MS and to Michael Sekerak for his assistance in understanding the FASTCAM algorithms developed at the University of Michigan. NR 54 TC 4 Z9 4 U1 0 U2 9 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD MAY PY 2014 VL 21 IS 5 AR 053512 DI 10.1063/1.4879819 PG 11 WC Physics, Fluids & Plasmas SC Physics GA AI7UY UT WOS:000337107200072 ER PT J AU Ni, XL Park, T Choi, SH Shi, YL Cao, CX Wang, XJ Lefsky, MA Simard, M Myneni, RB AF Ni, Xiliang Park, Taejin Choi, Sungho Shi, Yuli Cao, Chunxiang Wang, Xuejun Lefsky, Michael A. Simard, Marc Myneni, Ranga B. TI Allometric Scaling and Resource Limitations Model of Tree Heights: Part 3. Model Optimization and Testing over Continental China SO REMOTE SENSING LA English DT Article DE tree height; allometric scaling law; resource limitation; model optimization; geoscience laser altimeter system (GLAS); national forest inventory (NFI) ID SPATIAL INTERPOLATION; VEGETATION STRUCTURE; SURFACE-TOPOGRAPHY; TROPICAL FORESTS; DIAMETER MODELS; WATER RELATIONS; CANOPY HEIGHT; WAVE-FORMS; CLIMATE; LIDAR AB The ultimate goal of our multi-article series is to demonstrate the Allometric Scaling and Resource Limitation (ASRL) approach for mapping tree heights and biomass. This third article tests the feasibility of the optimized ASRL model over China at both site (14 meteorological stations) and continental scales. Tree heights from the Geoscience Laser Altimeter System (GLAS) waveform data are used for the model optimizations. Three selected ASRL parameters (area of single leaf, a; exponent for canopy radius, eta; and root absorption efficiency, gamma) are iteratively adjusted to minimize differences between the references and predicted tree heights. Key climatic variables (e.g., temperature, precipitation, and solar radiation) are needed for the model simulations. We also exploit the independent GLAS and in situ tree heights to examine the model performance. The predicted tree heights at the site scale are evaluated against the GLAS tree heights using a two-fold cross validation (RMSE = 1.72 m; R-2 = 0.97) and bootstrapping (RMSE = 4.39 m; R-2 = 0.81). The modeled tree heights at the continental scale (1 km spatial resolution) are compared to both GLAS (RMSE = 6.63 m; R-2 = 0.63) and in situ (RMSE = 6.70 m; R-2 = 0.52) measurements. Further, inter-comparisons against the existing satellite-based forest height maps have resulted in a moderate degree of agreements. Our results show that the optimized ASRL model is capable of satisfactorily retrieving tree heights over continental China at both scales. Subsequent studies will focus on the estimation of woody biomass after alleviating the discussed limitations. C1 [Ni, Xiliang; Cao, Chunxiang] Chinese Acad Sci, Inst Remote Sensing & Digital Earth, State Key Lab Remote Sensing Sci, Beijing 100101, Peoples R China. [Ni, Xiliang; Park, Taejin; Choi, Sungho; Shi, Yuli; Myneni, Ranga B.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. [Shi, Yuli] Nanjing Univ Informat Sci & Technol, Sch Remote Sensing, Nanjing 210044, Jiangsu, Peoples R China. [Wang, Xuejun] State Forest Adm China, Survey Planning & Design Inst, Beijing 100714, Peoples R China. [Lefsky, Michael A.] Colorado State Univ, Nat Resource Ecol Lab, Ctr Ecol Anal Lidar, Ft Collins, CO 80523 USA. [Simard, Marc] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Park, T (reprint author), Boston Univ, Dept Earth & Environm, 675 Commonwealth Ave, Boston, MA 02215 USA. EM nixl@irsa.ac.cn; partj@bu.edu; schoi@bu.edu; ylshi.nuist@gmail.com; cao413@irsa.ac.cn; wangxuejun320@126.com; lefsky@cnr.colostate.edu; marc.simard@jpl.nasa.gov; ranga.myneni@gmail.com RI Myneni, Ranga/F-5129-2012; Simard, Marc/H-3516-2013 OI Simard, Marc/0000-0002-9442-4562 FU National high Technology Research and Development Program of China (863 Program) [2013AA12A302]; Fulbright Program for graduate studies; NASA Headquarters under the NASA Earth and Space Science Fellowship Program-Grant [NNX13AP55H] FX The authors would like to thank Joshua Mantooth for his helpful review of this paper. Thanks also to the three anonymous reviewers whose comments significantly improved this manuscript. This study was partially funded by the National high Technology Research and Development Program of China (863 Program) (Grand No. 2013AA12A302). This work was also supported by the Fulbright Program for graduate studies and NASA Headquarters under the NASA Earth and Space Science Fellowship Program-Grant "NNX13AP55H". NR 56 TC 4 Z9 4 U1 2 U2 21 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD MAY PY 2014 VL 6 IS 5 BP 3533 EP 3553 DI 10.3390/rs6053533 PG 21 WC Remote Sensing SC Remote Sensing GA AI8JW UT WOS:000337160700001 ER PT J AU Wentz, EA Anderson, S Fragkias, M Netzband, M Mesev, V Myint, SW Quattrochi, D Rahman, A Seto, KC AF Wentz, Elizabeth A. Anderson, Sharolyn Fragkias, Michail Netzband, Maik Mesev, Victor Myint, Soe W. Quattrochi, Dale Rahman, Atiqur Seto, Karen C. TI Supporting Global Environmental Change Research: A Review of Trends and Knowledge Gaps in Urban Remote Sensing SO REMOTE SENSING LA English DT Review DE urban mapping; environmental indices; social indices; climate modeling; socioeconomic modeling ID LAND-SURFACE TEMPERATURE; NIGHTTIME SATELLITE IMAGERY; HIGH-RESOLUTION SATELLITE; SPECTRAL MIXTURE ANALYSIS; BUILT-UP INDEX; IMPERVIOUS SURFACE; HEAT-ISLAND; UNITED-STATES; COVER CLASSIFICATION; POPULATION-DENSITY AB This paper reviews how remotely sensed data have been used to understand the impact of urbanization on global environmental change. We describe how these studies can support the policy and science communities' increasing need for detailed and up-to-date information on the multiple dimensions of cities, including their social, biological, physical, and infrastructural characteristics. Because the interactions between urban and surrounding areas are complex, a synoptic and spatial view offered from remote sensing is integral to measuring, modeling, and understanding these relationships. Here we focus on three themes in urban remote sensing science: mapping, indices, and modeling. For mapping we describe the data sources, methods, and limitations of mapping urban boundaries, land use and land cover, population, temperature, and air quality. Second, we described how spectral information is manipulated to create comparative biophysical, social, and spatial indices of the urban environment. Finally, we focus how the mapped information and indices are used as inputs or parameters in models that measure changes in climate, hydrology, land use, and economics. C1 [Wentz, Elizabeth A.; Myint, Soe W.] Arizona State Univ, Sch Geog Sci & Urban Planning, Tempe, AZ 85287 USA. [Anderson, Sharolyn] Univ S Australia, Sch Nat & Built Environm, Adelaide, SA 5001, Australia. [Fragkias, Michail] Boise State Univ, COBE, Dept Econ, Boise, ID 83725 USA. [Netzband, Maik] Ruhr Univ Bochum, Dept Geog, D-44801 Bochum, Germany. [Mesev, Victor] Florida State Univ, Dept Geog, Tallahassee, FL 32306 USA. [Quattrochi, Dale] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35812 USA. [Rahman, Atiqur] Jamia Millia Islamia, Dept Geog, New Delhi 110025, India. [Seto, Karen C.] Yale Univ, Yale Sch Forestry & Environm Studies, New Haven, CT 06511 USA. RP Wentz, EA (reprint author), Arizona State Univ, Sch Geog Sci & Urban Planning, Coor Hall,5th Floor,975 S Myrtle Ave, Tempe, AZ 85287 USA. EM wentz@asu.edu; Sharolyn.Anderson@unisa.edu.au; michailfragkias@boisestate.edu; maik.netzband@rub.de; vmesev@fsu.edu; dale.quattrochi@nasa.gov; ateeqgeog@yahoo.co.in; karen.seto@yale.edu RI Seto, Karen/C-2722-2008; Anderson, Sharolyn/F-4653-2013 OI Anderson, Sharolyn/0000-0002-9456-0193 FU NASA [NNX10AN11G]; National Science Foundation [GSS-023907] FX This material is based upon work supported by NASA Grant No. NNX10AN11G and the National Science Foundation Grant No. GSS-023907. Any opinions, findings and conclusions, or recommendation expressed here are those of the authors and do not necessarily reflect the views of the funding agencies. The authors also acknowledge contributions from the Forecasting Urban Land-use Change Workshop (NASA) and the Urban Remote Sensing Workshop (NSF) participants: Rimjhim Aggarwal, Shlomo (Solly) Angel, Philip Christensen, Keith Clarke, Richard Dawson, Fabio Dell'Aqua, Xiangzheng Deng, Peter Omu Elias, Jonathan Fink, Tyler Frazier, Arjit Guha, Subhro Guhathakurta, Burak Guneralp, Geoffrey Henebry, Clair Jantz, Shai Kaplan, Donghwan Kim, Jose Lobo, Miguel Luengo-Oroz, Jacqueline Lu, Darle Monroe, David Nelson, Robert (Gil) Pontius, Milap Punia, Lela Preshad, Ray Quay, Charles Redman, Qing Shen, Christopher Small, William Solecki, Tod Swanson, Scott Weisman, and Sainan Zhang. We also acknowledge Cary Simmons and Qian Zhang for help with graphics. NR 162 TC 11 Z9 12 U1 9 U2 116 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD MAY PY 2014 VL 6 IS 5 BP 3879 EP 3905 DI 10.3390/rs6053879 PG 27 WC Remote Sensing SC Remote Sensing GA AI8JW UT WOS:000337160700017 ER PT J AU Lee, BC Huang, W Tao, L Yamamoto, N Gallimore, AD Yalin, AP AF Lee, B. C. Huang, W. Tao, L. Yamamoto, N. Gallimore, A. D. Yalin, A. P. TI A cavity ring-down spectroscopy sensor for real-time Hall thruster erosion measurements SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article AB A continuous-wave cavity ring-down spectroscopy sensor for real-time measurements of sputtered boron from Hall thrusters has been developed. The sensor uses a continuous-wave frequency-quadrupled diode laser at 250 nm to probe ground state atomic boron sputtered from the boron nitride insulating channel. Validation results from a controlled setup using an ion beam and target showed good agreement with a simple finite-element model. Application of the sensor for measurements of two Hall thrusters, the H6 and SPT-70, is described. The H6 was tested at power levels ranging from 1.5 to 10 kW. Peak boron densities of 10 +/- 2 x 10(14) m (3) were measured in the thruster plume, and the estimated eroded channel volume agreed within a factor of 2 of profilometry. The SPT-70 was tested at 600 and 660 W, yielding peak boron densities of 7.2 +/- 1.1 x 10(14) m (3), and the estimated erosion rate agreed within similar to 20% of profilometry. Technical challenges associated with operating a high-finesse cavity in the presence of energetic plasma are also discussed. (C) 2014 AIP Publishing LLC. C1 [Lee, B. C.] Colorado State Univ, Dept Phys, Ft Collins, CO 80521 USA. [Huang, W.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Tao, L.; Yamamoto, N.; Yalin, A. P.] Colorado State Univ, Dept Mech Engn, Ft Collins, CO 80521 USA. [Gallimore, A. D.] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA. RP Yalin, AP (reprint author), Colorado State Univ, Dept Mech Engn, Ft Collins, CO 80521 USA. EM ayalin@engr.colostate.edu RI Tao, Lei/F-6793-2012 FU National Aeronautics and Space Administration (NASA) Space Technology Research Fellowship [NX11AN30H] FX The authors would like to acknowledge support from the National Aeronautics and Space Administration (NASA) Space Technology Research Fellowship Grant No. NX11AN30H. NR 41 TC 3 Z9 3 U1 2 U2 17 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 MAY PY 2014 VL 85 IS 5 AR 053111 DI 10.1063/1.4879135 PG 11 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA AI7UD UT WOS:000337104600011 PM 24880357 ER PT J AU Tobiska, WK Gersey, B Wilkins, R Mertens, C Atwell, W Bailey, J AF Tobiska, W. Kent Gersey, Brad Wilkins, Richard Mertens, Chris Atwell, William Bailey, Justin TI Reply to comment by Rainer Facius et al. on "US Government shutdown degrades aviation radiation monitoring during solar radiation storm" SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID INITIAL VALIDATION; MODEL DEVELOPMENT; DOSE CLIMATOLOGY AB The premise of this comment perpetuates an unfortunate trend among some radiation researchers to minimize potential risks to human tissue from low-radiation sources. In fact, this discussion on the risk uncertainties of low-dose radiation further illustrates the need for more measurements and a program of active monitoring, especially when solar eruptive events can substantially elevate the radiation environment. This debate also highlights the context of a bigger problem; i.e., how do we as professionals act with due diligence to take the immense body of knowledge of space weather radiation effects on human tissue and distil it into ideas that regulatory agencies can use to maximize the safety of a population at risk. The focus of our article on radiation risks due to solar energetic particle events starts with our best assessment of risks and is based on the body of scientific knowledge while, at the same time, erring on the side of public safety. The uncertainty inherent in our assessment is accepted and described with this same philosophy in mind. C1 [Tobiska, W. Kent; Bailey, Justin] Space Environm Technol, Pacific Palisades, CA 90272 USA. [Gersey, Brad; Wilkins, Richard] Prairie View A&M Univ, Prairie View, TX USA. [Mertens, Chris] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Atwell, William] Boeing Co, Houston, TX USA. RP Tobiska, WK (reprint author), Space Environm Technol, Pacific Palisades, CA 90272 USA. EM ktobiska@spacenvironment.net NR 11 TC 1 Z9 1 U1 1 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 MAY PY 2014 VL 12 IS 5 BP 320 EP 321 DI 10.1002/2014SW001074 PG 2 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AJ3BW UT WOS:000337541100005 ER PT J AU Ade, PAR Aghanim, N Alves, MIR Arnaud, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Battaner, E Benabed, K Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bonaldi, A Bond, IR Borrill, J Bouchet, FR Boulanger, E Burigana, C Cardoso, JF Casassus, S Catalano, A Chamballu, A Chen, X Chiang, HC Chiang, LY Christensen, PR Clements, DL Colombi, S Colombo, LPL Couchot, F Crill, BP Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Desert, FX Dickinson, C Diego, JM Donzelli, S Dore, O Dupac, X Ensslin, TA Eriksen, HK Finelli, F Forni, O Franceschi, E Galeotta, S Ganga, K Genova-Santos, RT Ghosh, T Giard, M Gonzalez-Nuevo, J Gorski, KM Gregorio, A Gruppuso, A Hansen, EK Harrison, DL Helou, G Hernandez-Monteagudo, C Hildebrandt, SR Hivon, E Hobson, M Hornstrup, A Jaffe, AH Jaffe, TR Jones, WC Keihanen, E Keskitalo, R Kneissl, R Knoche, I Kunz, M Kurki-Suonio, H Lahteenmaki, A Lamarre, JM Lasenby, A Lawrence, CR Leonardi, R Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Mazzotta, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Migliaccio, M Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Naselsky, P Nati, F Natoli, P Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Oxborrow, CA Pagano, L Pajot, F Paladini, R Paoletti, D Patanchon, G Pearson, TJ Peel, M Perdereau, O Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Pratt, GW Prunet, S Puget, JL Rachen, JP Rebolo, R Reich, W Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Savini, G Scott, D Spencer, D Stolyarov, V Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Tibbs, CT Toffolatti, L Tomasi, M Tristram, M Tucci, M Valenziano, L Valiviita, J Van Tent, B Varis, J Verstraete, L Vielva, P Villa, F Wandelt, BD Watson, R Wilkinson, A Ysard, N Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Alves, M. I. R. Arnaud, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Battaner, E. Benabed, K. Benoit-Levy, A. Bernard, J-P Bersanelli, M. Bielewicz, P. Bobin, J. Bonaldi, A. Bond, I. R. Borrill, J. Bouchet, F. R. Boulanger, E. Burigana, C. Cardoso, J-F Casassus, S. Catalano, A. Chamballu, A. Chen, X. Chiang, H. C. Chiang, L-Y Christensen, P. R. Clements, D. L. Colombi, S. Colombo, L. P. L. Couchot, F. Crill, B. P. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Desert, F-X Dickinson, C. Diego, J. M. Donzelli, S. Dore, O. Dupac, X. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Franceschi, E. Galeotta, S. Ganga, K. Genova-Santos, R. T. Ghosh, T. Giard, M. Gonzalez-Nuevo, J. Gorski, K. M. Gregorio, A. Gruppuso, A. Hansen, E. K. Harrison, D. L. Helou, G. Hernandez-Monteagudo, C. Hildebrandt, S. R. Hivon, E. Hobson, M. Hornstrup, A. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Keihanen, E. Keskitalo, R. Kneissl, R. Knoche, I. Kunz, M. Kurki-Suonio, H. Lahteenmaki, A. Lamarre, J-M Lasenby, A. Lawrence, C. R. Leonardi, R. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Mazzotta, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Miville-Deschenes, M-A Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Naselsky, P. Nati, F. Natoli, P. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Pagano, L. Pajot, F. Paladini, R. Paoletti, D. Patanchon, G. Pearson, T. J. Peel, M. Perdereau, O. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Pratt, G. W. Prunet, S. Puget, J-L Rachen, J. P. Rebolo, R. Reich, W. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Savini, G. Scott, D. Spencer, D. Stolyarov, V. Sutton, D. Suur-Uski, A-S Sygnet, J-F Tauber, J. A. Tavagnacco, D. Terenzi, L. Tibbs, C. T. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Valenziano, L. Valiviita, J. Van Tent, B. Varis, J. Verstraete, L. Vielva, P. Villa, F. Wandelt, B. D. Watson, R. Wilkinson, A. Ysard, N. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck intermediate results. XV. A study of anomalous microwave emission in Galactic clouds SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE HII regions; radiation mechanisms: general; radio continuum: ISM; submillimeter: ISM ID SPINNING DUST EMISSION; PROBE WMAP OBSERVATIONS; H-II REGIONS; PRE-LAUNCH STATUS; CENTIMETER-WAVE CONTINUUM; GHZ SKY SURVEY; ANISOTROPY-PROBE; MOLECULAR CLOUDS; FOREGROUND EMISSION; STAR-FORMATION AB Anomalous microwave emission (AME) is believed to be due to electric dipole radiation from small spinning dust grains. The aim of this paper is a statistical study of the basic properties of AME regions and the environment in which they emit. We used WMAP and Planck maps, combined with ancillary radio and IR data, to construct a sample of 98 candidate AME sources, assembling SEDs for each source using aperture photometry on 1 degrees-smoothed maps from 0.408 GHz up to 3000 GHz. Each spectrum is fitted with a simple model of free-free, synchrotron (where necessary), cosmic microwave background (CMB), thermal dust, and spinning dust components. We find that 42 of the 98 sources have significant (>5 sigma) excess emission at frequencies between 20 and 60 GHz. An analysis of the potential contribution of optically thick free-free emission from ultra-compact H II regions, using IR colour criteria, reduces the significant AME sample to 27 regions. The spectrum of the AME is consistent with model spectra of spinning dust. Peak frequencies are in the range 20-35 GHz except for the California nebula (NGC1499), which appears to have a high spinning dust peak frequency of (50 +/- 17) GHz. The AME regions tend to be more spatially extended than regions with little or no AME. The AME intensity is strongly correlated with the sub-millimetre/IR flux densities and comparable to previous AME detections in the literature. AME emissivity, defined as the ratio of AME to dust optical depth, varies by an order of magnitude for the AME regions. The AME regions tend to be associated with cooler dust in the range 14-20K and an average emissivity index, beta(d), of + 1.8, while the non-AME regions are typically warmer, at 20-27 K. In agreement with previous studies, the AME emissivity appears to decrease with increasing column density. This supports the idea of AME originating from small grains that are known to be depleted in dense regions, probably due to coagulation onto larger grains. We also find a correlation between the AME emissivity (and to a lesser degree the spinning dust peak frequency) and the intensity of the interstellar radiation field, G(0). Modelling of this trend suggests that both radiative and collisional excitation are important for the spinning dust emission. The most significant AME regions tend to have relatively less ionized gas (free-free emission), although this could be a selection effect. The infrared excess, a measure of the heating of dust associated with H II regions, is typically >4 for AME sources, indicating that the dust is not primarily heated by hot OB stars. The AME regions are associated with known dark nebulae and have higher 12 mu m/25 mu m ratios. The emerging picture is that the bulk of the AME is coming from the polycyclic aromatic hydrocarbons and small dust grains from the colder neutral interstellar medium phase. C1 [Cardoso, J-F; Delabrouille, J.; Ganga, K.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.] Univ Paris Diderot, APC, Sorbonne Paris Cite, CNRS,IN2P3,CEA,Irfu,Observ Paris, F-75205 Paris 13, France. [Lahteenmaki, A.] Aalto Univ, Metsahovi Radio Observ, Aalto 00076, Finland. [Lahteenmaki, A.] Aalto Univ, Dept Radio Sci & Engn, Aalto 00076, Finland. [Kunz, M.] African Inst Math Sci, ZA-7950 Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, Rome, Italy. [Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Astrophys Grp, Cavendish Lab, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa. [Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile. [Bond, I. R.; Martin, P. G.; Miville-Deschenes, M-A] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J-P; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse 4, France. [Crill, B. P.; Dore, O.; Helou, G.; Hildebrandt, S. R.; Pearson, T. J.; Rocha, G.] CALTECH, Pasadena, CA 91125 USA. [Hernandez-Monteagudo, C.] CEFCA, Teruel 44001, Spain. [Borrill, J.; Keskitalo, R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Rebolo, R.] CSIC, Madrid, Spain. [Chamballu, A.; Yvon, D.] CEA Saclay, DSM, Irfu, SPP, F-91191 Gif Sur Yvette, France. [Hornstrup, A.; Linden-Vornle, M.; Norgaard-Nielsen, H. U.; Oxborrow, C. A.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark. [Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland. [Atrio-Barandela, F.] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Rachen, J. P.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Keskitalo, R.] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, Los Angeles, CA 90089 USA. [Benoit-Levy, A.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Keihanen, E.; Kurki-Suonio, H.; Suur-Uski, A-S; Valiviita, J.; Ysard, N.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Chiang, H. C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Meinhold, P. R.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA. [Liguori, M.; Matarrese, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Burigana, C.; Mandolesi, N.; Natoli, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Nati, F.; Pagano, L.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Gregorio, A.; Tavagnacco, D.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Mazzotta, P.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Kneissl, R.] European So Observ, ESO Vitacura, Santiago 19, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid 28692, Spain. [Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands. [Kurki-Suonio, H.; Lahteenmaki, A.; Suur-Uski, A-S; Valiviita, J.] Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland. [de Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Galeotta, S.; Gregorio, A.; Tavagnacco, D.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Massardi, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Paoletti, D.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] IASF Bologna, INAF, I-40129 Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Maino, D.; Mennella, A.; Tomasi, M.] IASF Milano, INAF, Milan, Italy. [Finelli, F.; Paoletti, D.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy. [Melchiorri, A.; Pagano, L.] Univ Roma La Sapienza, Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy. [Gregorio, A.] INFN Natl Inst Nucl Phys, I-34127 Trieste, Italy. [Desert, F-X; Ponthieu, N.] Univ Grenoble 1, IPAG, Grenoble CNRS INSU 1, UMR 5274, F-38041 Grenoble, France. [Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Chen, X.; Paladini, R.; Pearson, T. J.; Rusholme, B.; Tibbs, C. T.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Aghanim, N.; Alves, M. I. R.; Aumont, J.; Boulanger, E.; Chamballu, A.; Ghosh, T.; Kunz, M.; Miville-Deschenes, M-A; Pajot, F.; Ponthieu, N.; Puget, J-L; Remazeilles, M.; Verstraete, L.] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR8617, F-91405 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J-F; Colombi, S.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J-F; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. [Popa, L.] Inst Space Sci, Bucharest, Romania. [Chiang, L-Y] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Harrison, D. L.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Eriksen, H. K.; Hansen, E. K.; Lilje, P. B.; Valiviita, J.] Univ Oslo, Inst Theoret Astrophys, N-0313 Oslo, Norway. [Genova-Santos, R. T.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Barreiro, R. B.; Diego, J. M.; Gonzalez-Nuevo, J.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gorski, K. M.; Lawrence, C. R.; Pietrobon, D.; Rocha, G.; Roudier, G.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Bonaldi, A.; Davies, R. D.; Davis, R. J.; Dickinson, C.; Maffei, B.; Noviello, F.; Peel, M.; Remazeilles, M.; Watson, R.; Wilkinson, A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Harrison, D. L.; Lasenby, A.; Migliaccio, M.; Stolyarov, V.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Couchot, F.; Perdereau, O.; Plaszczynski, S.; Tristram, M.; Tucci, M.] Univ Paris 11, CNRS, IN2P3, LAL, F-91405 Orsay, France. [Catalano, A.; Lamarre, J-M; Roudier, G.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Arnaud, M.; Bobin, J.; Chamballu, A.; Marshall, D. J.; Pratt, G. W.] Univ Paris Diderot, CEA Saclay, Lab AIM, IRFU,Serv Astrophys,CEA,DSM,CNRS, F-91191 Gif Sur Yvette, France. [Cardoso, J-F] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris, France. [Cardoso, J-F] Telecom ParisTech, F-75634 Paris, France. [Catalano, A.; Macias-Perez, J. F.; Renault, C.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, Inst Natl Polytech Grenoble, CNRS,IN2P3, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France. [Van Tent, B.] CNRS, F-91405 Orsay, France. [Ensslin, T. A.; Hernandez-Monteagudo, C.; Knoche, I.; Rachen, J. P.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Reich, W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo 02044, Finland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Savini, G.] UCL, Opt Sci Lab, London WC1E 6BT, England. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Arkhyz 369167, Zelenchukskiy R, Russia. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR 7095, F-75014 Paris, France. [Casassus, S.] Univ Santiago Chile, Santiago, Chile. [Banday, A. J.; Bernard, J-P; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Dickinson, C (reprint author), Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. EM clive.dickinson@manchester.ac.uk RI Remazeilles, Mathieu/N-1793-2015; Bobin, Jerome/P-3729-2014; Stolyarov, Vladislav/C-5656-2017; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Ghosh, Tuhin/E-6899-2016; Tomasi, Maurizio/I-1234-2016; Casassus, Simon/I-8609-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Lopez-Caniego, Marcos/M-4695-2013; Battaner, Eduardo/P-7019-2014; Vielva, Patricio/F-6745-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Pearson, Timothy/N-2376-2015; OI de Bernardis, Paolo/0000-0001-6547-6446; Remazeilles, Mathieu/0000-0001-9126-6266; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Lopez-Caniego, Marcos/0000-0003-1016-9283; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Watson, Robert/0000-0002-5873-0124; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Bobin, Jerome/0000-0003-1457-7890; Stolyarov, Vladislav/0000-0001-8151-828X; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Sandri, Maura/0000-0003-4806-5375; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Morgante, Gianluca/0000-0001-9234-7412; Peel, Mike/0000-0003-3412-2586; Masi, Silvia/0000-0001-5105-1439; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Gruppuso, Alessandro/0000-0001-9272-5292; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Pearson, Timothy/0000-0001-5213-6231; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Cuttaia, Francesco/0000-0001-6608-5017; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043 FU NASA Office of Space Science; National Aeronautics and Space Administration; STFC Advanced Fellowship; EU; ERC [307209]; ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MICINN (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); PRACE (EU) FX We thank the anonymous referee for providing useful comments. We thank Justin Jonas for providing the 2326 MHz HartRAO map. We acknowledge the use of the MPIfR Survey Sampler website at http://www.mpifr-bonn.mpg.de/survey.html and the Legacy Archive for Microwave Background Data Analysis (LAMBDA); support for LAMBDA is provided by the NASA Office of Space Science. 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 also makes use of the SIMBAD database, operated at the CDS, Strasbourg, France. We acknowledge the use of NASA's SkyView facility (http://skyview.gsfc.nasa.gov) located at NASA Goddard Space Flight Center. C. D. acknowledges an STFC Advanced Fellowship, an EU Marie-Curie IRG grant under the FP7, and an ERC Starting Grant (No. 307209). The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collabora tion NR 153 TC 21 Z9 21 U1 4 U2 19 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2014 VL 565 AR A103 DI 10.1051/0004-6361/201322612 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900103 ER PT J AU Bitsakis, T Charmandaris, V Appleton, PN Diaz-Santos, T Le Floc'h, E da Cunha, E Alatalo, K Cluver, M AF Bitsakis, T. Charmandaris, V. Appleton, P. N. Diaz-Santos, T. Le Floc'h, E. da Cunha, E. Alatalo, K. Cluver, M. TI Herschel observations of Hickson compact groups of galaxies: Unveiling the properties of cold dust SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; galaxies: interactions; galaxies: groups: general; infrared: galaxies ID STEPHANS QUINTET; STAR-FORMATION; NEARBY GALAXIES; MOLECULAR GAS; SUBMILLIMETER PHOTOMETRY; INFRARED PROPERTIES; NEUTRAL HYDROGEN; NUCLEAR ACTIVITY; VIRGO CLUSTER; GREEN VALLEY AB We present a Herschel far-infrared and sub-millimetre (sub-mm) study of a sample of 120 galaxies in 28 tlickson compact groups (HCGs). Fitting their UV to sub-mm spectral energy distributions with the model of da Cunha et al. (2008), we accurately estimate the dust masses, luminosities, and temperatures of the individual galaxies. We find that nearly half of the late-type galaxies in dynamically "old" groups, those with more than 25% of early-type members and redder UV-optical colours, also have significantly lower dust-to-stellar mass ratios compared to those of actively star-forming galaxies of the same mass found both in HCGs and in the field. Examining their dust-to-gas mass ratios, we conclude that dust was stripped out of these systems as a result of the gravitational and hydrodynamic interactions, experienced owing to previous encounters with other group members. About 40% of the early-type galaxies (mostly lenticulars), in dynamically "old" groups, display dust properties similar to those of the UV-optical red late-type galaxies. Given their stellar masses, star formation rates, and UV-optical colours, we suggest that red late-type and dusty lenticular galaxies represent transition populations between blue star-forming disk galaxies and quiescent early-type ellipticals. On the other hand, both the complete absence of any correlation between the dust and stellar masses of the dusty ellipticals and their enhanced star formation activity, suggest the increase in their gas and dust content due to accretion and merging. Our deep Herschel observations also allow us to detect the presence of diffuse cold intragroup dust in 4 HCGs. We also find that the fraction of 250 mu m emission that is located outside of the main bodies of both the red late-type galaxies and the dusty lenticulars is 15-20% of their integrated emission at this band. All these findings are consistent with an evolutionary scenario in which gas dissipation, shocks, and turbulence, in addition to tidal interactions, shape the evolution of galaxies in compact groups. C1 [Bitsakis, T.; Charmandaris, V.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Bitsakis, T.; Appleton, P. N.; Alatalo, K.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Bitsakis, T.] Fdn Res & Technol Hellas, IESL, Iraklion 71110, Greece. [Charmandaris, V.] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, Penteli 15236, Greece. [Charmandaris, V.] Observ Paris, F-75014 Paris, France. [Diaz-Santos, T.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Le Floc'h, E.] CEA Saclay, F-91191 Gif Sur Yvette, France. [da Cunha, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Cluver, M.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. RP Bitsakis, T (reprint author), Univ Crete, Dept Phys, Iraklion 71003, Greece. EM bitsakis@physics.uoc.gr RI Charmandaris, Vassilis/A-7196-2008; Bitsakis, Theodoros/O-2766-2013; OI Charmandaris, Vassilis/0000-0002-2688-1956; Bitsakis, Theodoros/0000-0001-5787-8242; Appleton, Philip/0000-0002-7607-8766; da Cunha, Elisabete/0000-0001-9759-4797 FU EU [PIRSES-GA-2012-316788]; NASA FX T.B. and V.C. would like to acknowledge partial support from the EU FP7 Grant PIRSES-GA-2012-316788. This work is based, in part, on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was also provided by NASA through an award issued by JPL/Caltech. We also appreciate the very useful comments of the referee, A. Boseili, which helped improve this paper. Finally, we are grateful to L. Verdes-Montenegro for providing the HI moment-0 maps of 4 HCGs. NR 82 TC 16 Z9 16 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 MAY PY 2014 VL 565 AR A25 DI 10.1051/0004-6361/201323349 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900025 ER PT J AU Fremling, C Sollerman, J Taddia, F Ergon, M Valenti, S Arcavi, I Ben-Ami, S Cao, Y Cenko, SB Filippenko, AV Gal-Yam, A Howell, DA AF Fremling, C. Sollerman, J. Taddia, F. Ergon, M. Valenti, S. Arcavi, I. Ben-Ami, S. Cao, Y. Cenko, S. B. Filippenko, A. V. Gal-Yam, A. Howell, D. A. TI The rise and fall of the Type Ib supernova iPTF13bvn Not a massive Wolf-Rayet star SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE supernovae: general; supernovae: individual: iPTF13bvn ID CORE-COLLAPSE SUPERNOVA; LIGHT CURVES; LOW-RESOLUTION; X-RAY; EVOLUTION; PROGENITOR; TELESCOPE; SPECTRA; I.; NUCLEOSYNTHESIS AB Context. We investigate iPTF13bvn, a core-collapse (CC) supernova (SN) in the nearby spiral galaxy NGC 5806. This object was discovered by the intermediate Palomar Transient Factory (iPTF) very close to the estimated explosion date and was classified as a stripped-envelope CC SN, likely of Type Ib. Furthermore, a possible progenitor detection in pre-explosion Hubble Space Telescope (HST) images was reported, making this the only SN Ib with such an identification. Based on the luminosity and color of the progenitor candidate, as well as on early-time spectra and photometry of the SN, it was argued that the progenitor candidate is consistent with a single, massive Wolf-Rayet (WR) star. Aims. We aim to confirm the progenitor detection, to robustly classify the SN using additional spectroscopy, and to investigate if our follow-up photometric and spectroscopic data on iPTF13bvn are consistent with a single-star WR progenitor scenario. Methods. We present a large set of observational data, consisting of multi-band light curves (UBVRI, g' r' i' z') and optical spectra. We perform standard spectral line analysis to track the evolution of the SN ejecta. We also construct a bolometric light curve and perform hydrodynamical calculations to model this light curve to constrain the synthesized radioactive nickel mass and the total ejecta mass of the SN. Late-time photometry is analyzed to constrain the amount of oxygen. Furthermore, image registration of pre- and post-explosion HST images is performed. Results. Our HST astrometry confirms the location of the progenitor candidate of iPTF13bvn, and follow-up spectra securely classify this as a SN Ib. We use our hydrodynamical model to fit the observed bolometric light curve, estimating the total ejecta mass to be 1.9 M-circle dot and the radioactive nickel mass to be 0.05 M-circle dot. The model fit requires the nickel synthesized in the explosion to be highly mixed out in the ejecta. We also find that the late-time nebular r'-band luminosity is not consistent with predictions based on the expected oxygen nucleosynthesis in very massive stars. Conclusions. We find that our bolometric light curve of iPTF13bvn is not consistent with the previously proposed single massive WR-star progenitor scenario. The total ejecta mass and, in particular, the late-time oxygen emission are both significantly lower than what would be expected from a single WR progenitor with a main-sequence mass of at least 30 M-circle dot. C1 [Fremling, C.; Sollerman, J.; Taddia, F.; Ergon, M.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, S-10691 Stockholm, Sweden. [Valenti, S.; Arcavi, I.; Howell, D. A.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Valenti, S.; Howell, D. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Arcavi, I.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Ben-Ami, S.; Gal-Yam, A.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Cao, Y.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Fremling, C (reprint author), Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, S-10691 Stockholm, Sweden. EM christoffer.fremling@astro.su.se OI Sollerman, Jesper/0000-0003-1546-6615 FU Swedish Research Council; W. M. Keck Foundation; EU/FP7 via ERC [307260]; Israeli Committee for planning and budgeting; ISF grant; GIF grant; Minerva grant; Kimmel award; Christopher R. Redlich Fund; TABASGO Foundation; NSF [AST-1211916]; NASA from the Space Telescope Science Institute [AR-12623, AR-12850]; NASA [NAS 5-26555] FX The Oskar Klein Centre is funded by the Swedish Research Council. This work is partially based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. 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. A. G.-Y. is supported by the EU/FP7 via ERC grant 307260, "The Quantum Universe" I-Core program by the Israeli Committee for planning and budgeting, by ISF, GIF, and Minerva grants, and by the Kimmel award. A. V. F.'s group at UC Berkeley has received generous financial assistance from the Christopher R. Redlich Fund, the TABASGO Foundation, NSF grant AST-1211916, and NASA grants AR-12623 and AR-12850 from the Space Telescope Science Institute (which is operated by AURA, Inc., under NASA contract NAS 5-26555). We extend our thanks to the following people for their various contributions to this work: Shri Kulkarni, Mansi M. Kasliwal, Ofer Yaron, Paul Vreeswijk, Daniel Perley, Joel Johansson, Anders Jerkstrand, Kelsey Clubb, Ori Fox, Patrick Kelly, Barak Zackay, Adam Waszczak, Donald O'Sullivan, and Thomas Augusteijn. NR 43 TC 24 Z9 24 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 MAY PY 2014 VL 565 AR A114 DI 10.1051/0004-6361/201423884 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900114 ER PT J AU Grinberg, V Pottschmidt, K Bock, M Schmid, C Nowak, MA Uttley, P Tomsick, JA Rodriguez, J Hell, N Markowitz, A Bodaghee, A Bel, MC Rothschild, RE Wilms, J AF Grinberg, V. Pottschmidt, K. Boeck, M. Schmid, C. Nowak, M. A. Uttley, P. Tomsick, J. A. Rodriguez, J. Hell, N. Markowitz, A. Bodaghee, A. Bel, M. Cadolle Rothschild, R. E. Wilms, J. TI Long term variability of Cygnus X-1 VI. Energy-resolved X-ray variability 1999-2011 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: binaries; stars: individual: Cygnus X-1; binaries: close ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE CANDIDATES; ACCRETION-EJECTION INSTABILITY; QUASI-PERIODIC OSCILLATIONS; TIMING-EXPLORER OBSERVATION; POWER SPECTRAL COMPONENTS; DEPENDENT TIME LAGS; HARD STATE; XMM-NEWTON; SOFT STATE AB We present the most extensive analysis of Fourier-based X-ray timing properties of the black hole binary Cygnus X-1 to date, based on 12 years of bi-weekly monitoring with RXTE from 1999 to 2011. Our aim is a comprehensive study of timing behavior across all spectral states, including the elusive transitions and extreme hard and soft states. We discuss the dependence of the timing properties on spectral shape and photon energy, and study correlations between Fourier-frequency dependent coherence and time lags with features in the power spectra. Our main results are: (a) The fractional rms in the 0.125-256 Hz range in different spectral states shows complex behavior that depends on the energy range considered. It reaches its maximum not in the hard state, but in the soft state in the Comptonized tail above 10 keV. (b) The shape of power spectra in hard and intermediate states and the normalization in the soft state are strongly energy dependent in the 2.1-15 keV range. This emphasizes the need for an energy-dependent treatment of power spectra and a careful consideration of energy- and mass-scaling when comparing the variability of different source types, e.g., black hole binaries and AGN. PSDs during extremely hard and extremely soft states can be easily confused for energies above similar to 5 keV in the 0.125-256 Hz range. (c) The coherence between energy bands drops during transitions from the intermediate into the soft state but recovers in the soft state. (d) The time lag spectra in soft and intermediate states show distinct features at frequencies related to the frequencies of the main variability components seen in the power spectra and show the same shift to higher frequencies as the source softens. Our results constitute a template for other sources and for physical models for the origin of the X-ray variability. In particular, we discuss how the timing properties of Cyg X-1 can be used to assess the evolution of variability with spectral shape in other black hole binaries. Our results suggest that none of the available theoretical models can explain the full complexity of X-ray timing behavior of Cyg X-1, although several ansatzes with different physical assumptions are promising. C1 [Grinberg, V.; Schmid, C.; Markowitz, A.; Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany. [Grinberg, V.; Nowak, M. A.] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA. [Pottschmidt, K.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA. [Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Boeck, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Uttley, P.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Tomsick, J. A.; Bodaghee, A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Rodriguez, J.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,UMR 7158,IRFU SAp, F-91191 Gif Sur Yvette, France. [Hell, N.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Markowitz, A.; Rothschild, R. E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Bel, M. Cadolle] Univ Munich, D-85748 Garching, Germany. RP Grinberg, V (reprint author), Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, Sternwartstr 7, D-96049 Bamberg, Germany. EM victoria.grinberg@fau.de RI Wilms, Joern/C-8116-2013; OI Wilms, Joern/0000-0003-2065-5410; Rodriguez, Jerome/0000-0002-4151-4468 FU Bundesministerium fur Wirtschaft und Technologie under Deutsches Zentrum fur Luft- und Raumfahrt grants [50 OR 1007, 50 OR 1113]; European Commission [ITN 215212]; LLNL [DE-AC52-07NA27344]; NASA [SV3-73016, NAS8-03060]; NASA/GSFC FX This work has been partially funded by the Bundesministerium fur Wirtschaft und Technologie under Deutsches Zentrum fur Luft- und Raumfahrt grants 50 OR 1007 and 50 OR 1113 and by the European Commission through ITN 215212 "Black Hole Universe". It was partially completed by LLNL under contract DE-AC52-07NA27344, and is supported by NASA grants to LLNL and NASA/GSFC. Support for this work was also provided by NASA through the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to MIT for Support of the Chandra X-Ray Center (CXC) and Science Instruments; CXC is operated by SAO for and on behalf of NASA under contract NAS8-03060. We further acknowledge support from the DFG Cluster of Excellence "Origin and Structure of the Universe" and are grateful for the support by MCB through the Computational Center for Particle and Astrophysics (C2PAP). This research has made use of NASA's Astrophysics Data System Bibliographic Services. We thank John E. Davis for the development of the slxfig module used to prepare all figures in this work and Fritz-Walter Schwarm and Ingo Kreykenbohm for their work on the Remeis computing cluster. This research made use of ISIS functions (isisscripts) provided by ECAP/Remeis observatory and MIT9. Without the hard work by Evan Smith to schedule the Cyg X-1 so uniformly for more than a decade, this paper would not have been possible. V.G. is grateful for the support through the ESAC faculty grant program to support student attendance at the workshop "Spectral/timing properties of accreting objects: from X-ray binaries to AGN" that proved pivotal for the basic idea behind this research. NR 125 TC 14 Z9 14 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2014 VL 565 AR A1 DI 10.1051/0004-6361/201322969 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900001 ER PT J AU Marshall, JP Moro-Martin, A Eiroa, C Kennedy, G Mora, A Sibthorpe, B Lestrade, JE Maldonado, J Sanz-Forcada, J Wyatt, MC Matthews, B Horner, J Montesinos, B Bryden, G del Burgo, C Greaves, JS Ivison, RJ Meeus, G Olofsson, G Pilbratt, GL White, GJ AF Marshall, J. P. Moro-Martin, A. Eiroa, C. Kennedy, G. Mora, A. Sibthorpe, B. Lestrade, J-E Maldonado, J. Sanz-Forcada, J. Wyatt, M. C. Matthews, B. Horner, J. Montesinos, B. Bryden, G. del Burgo, C. Greaves, J. S. Ivison, R. J. Meeus, G. Olofsson, G. Pilbratt, G. L. White, G. J. TI Correlations between the stellar, planetary, and debris components of exoplanet systems observed by Herschel SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE infrared: stars; infrared: planetary systems; circumstellar matter; planet-disk interactions ID EXTRA-SOLAR PLANETS; ANGLO-AUSTRALIAN PLANET; EARTH-LIKE PLANETS; 47 URSAE-MAJORIS; M-CIRCLE-PLUS; HIGH-RESOLUTION SIMULATIONS; HOBBY-EBERLY TELESCOPE; NEPTUNE-MASS PLANET; SUN-LIKE STARS; HARPS SEARCH AB Context. Stars form surrounded by gas- and dust-rich protoplanetary discs. Generally, these discs dissipate over a few (3-10) Myr, leaving a faint tenuous debris disc composed of second-generation dust produced by the attrition of larger bodies formed in the protoplanetary disc. Giant planets detected in radial velocity and transit surveys of main-sequence stars also form within the protoplanetary disc, whilst super-Earths now detectable may form once the gas has dissipated. Our own solar system, with its eight planets and two debris belts, is a prime example of an end state of this process. Aims. The Herschel DEBRIS, DUNES, and GI' programmes observed 37 exoplanet host stars within 25 pc at 70, 100, and 160 mu m with the sensitivity to detect far-infrared excess emission at flux density levels only an order of magnitude greater than that of the solar system's Edgeworth-Kuiper belt. Here we present an analysis of that sample, using it to more accurately determine the (possible) level of dust emission from these exoplanet host stars and thereafter determine the links between the various components of these exoplanetary systems through statistical analysis. Methods. We have fitted the flux densities measured from recent Herschel observations with a simple two parameter (T-d, L-IR/L-*) black-body model (or to the 3 sigma upper limits at 100 mu m). From this uniform approach we calculated the fractional luminosity, radial extent and dust temperature. We then plotted the calculated dust luminosity or upper limits against the stellar properties, e.g. effective temperature, metallicity, and age, and identified correlations between these parameters. Results. A total of eleven debris discs are identified around the 37 stars in the sample. An incidence of ten cool debris discs around the Sun-like exoplanet host stars (29 +/- 9%) is consistent with the detection rate found by DUNES (20.2 +/- 2.0%). For the debris disc systems, the dust temperatures range from 20 to 80 K, and fractional luminosities (L-IR/L-*) between 2.4 x10(-6) and 4.1 x10(-4). In the case of non-detections, we calculated typical 3 sigma upper limits to the dust fractional luminosities of a few x10(-6). Conclusions. We recover the previously identified correlation between stellar metallicity and hot-Jupiter planets in our data set. We find a correlation between the increased presence of dust, lower planet masses, and lower stellar metallicities. This confirms the recently identified correlation between cold debris discs and low-mass planets in the context of planet formation by core accretion. C1 [Marshall, J. P.; Eiroa, C.; Maldonado, J.; Meeus, G.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. [Marshall, J. P.; Horner, J.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Moro-Martin, A.] Ctr Astrobiol, Dept Astrophys, Madrid 28850, Spain. [Moro-Martin, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kennedy, G.; Wyatt, M. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain. [Sibthorpe, B.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Lestrade, J-E] CNRS, Observ Paris, F-75014 Paris, France. [Maldonado, J.] INAF Observ Astron Palermo, I-90134 Palermo, Italy. [Sanz-Forcada, J.; Montesinos, B.] CSIC, INTA, Ctr Astrobiol CAB, Dept Astrophys, Madrid 28691, Spain. [Matthews, B.] Natl Res Council Canada, Herzberg Astron & Astrophys, Victoria, BC V9E 2E7, Canada. [Matthews, B.] Univ Victoria, Victoria, BC V8W 3P6, Canada. [Horner, J.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Horner, J.] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. [Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [del Burgo, C.] Inst Nacl Astrofis Opt & Electr, Puebla, Mexico. [Greaves, J. S.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Olofsson, G.] Stockholm Univ, Dept Astron, AlbaNova linivers Ctr, S-10691 Stockholm, Sweden. [Pilbratt, G. L.] ESTEC SRE SA, ESA Astrophys & Fundamental Phys Missions Div, NL-2201 AZ Noordwijk, Netherlands. [White, G. J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [White, G. J.] Rutherford Appleton Lab, Chilton OX11 0QX, Oxon, England. RP Marshall, JP (reprint author), Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. EM jonathan.marshall@uam.es RI Ivison, R./G-4450-2011; Sanz-Forcada, Jorge/C-3176-2017; Montesinos, Benjamin/C-3493-2017; OI Ivison, R./0000-0001-5118-1313; Sanz-Forcada, Jorge/0000-0002-1600-7835; Montesinos, Benjamin/0000-0002-7982-2095; Marshall, Jonathan/0000-0001-6208-1801; Horner, Jonti/0000-0002-1160-7970; Kennedy, Grant/0000-0001-6831-7547 FU Spanish grant [AYA 2011-26202]; European Union through ERC [279973]; Spitzer grant OT1_amoromar_1 FX This research has made use of NASA's Astrophysics Data System Bibliographic Services. This research has made use of the SIMBAD database, operated at CDS; Strasbourg, France. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org, and the Extrasolar Planets Encyclopedia at exoplanets.eu. J.P.M., CE., J.M. and B.M. are partially supported by Spanish grant AYA 2011-26202. This work was supported by the European Union through ERC grant number no. 279973 (GMK and MCW) and has been partially supported by Spitzer grant OT1_amoromar_1 (AMM). NR 170 TC 20 Z9 20 U1 1 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2014 VL 565 AR A15 DI 10.1051/0004-6361/201323058 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900015 ER PT J AU Moehler, S Dreizler, S LeBlanc, F Khalack, V Michaud, G Richer, J Sweigart, AV Grundahl, F AF Moehler, S. Dreizler, S. LeBlanc, F. Khalack, V. Michaud, G. Richer, J. Sweigart, A. V. Grundahl, F. TI Hot horizontal branch stars in NGC288-effects of diffusion and stratification on their atmospheric parameters SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: horizontal-branch; stars: atmospheres; techniques: spectroscopic; globular clusters: individual: NGC 288 ID GLOBULAR-CLUSTER M13; ABUNDANCE ANOMALIES; PHYSICAL PARAMETERS; MULTIPLE POPULATIONS; HB STARS; VERTICAL STRATIFICATION; RADIATIVE LEVITATION; B-STARS; NGC 288; CONSEQUENCES AB Context. NGC288 is a globular cluster with a well-developed blue horizontal branch (HB) covering the u-jump that indicates the onset of diffusion. It is therefore well suited to study the effects of diffusion in blue HB stars. Aims. We compare observed abundances with predictions from stellar evolution models calculated with diffusion and from stratified atmospheric models. We verify the effect of using stratified model spectra to derive atmospheric parameters. In addition, we investigate the nature of the overluminous blue HB stars around the u-jump. Methods. We defined a new photometric index sz from uvby measurements that is gravity-sensitive between 8000 K and 12 000 K. Using medium-resolution spectra and Stromgren photometry, we determined atmospheric parameters (T-eff, log g) and abundances for the blue HB stars. We used both homogeneous and stratified model spectra for our spectroscopic analyses. Results. The atmospheric parameters and masses of the hot HB stars in NGC288 show a behaviour seen also in other clusters for temperatures between 9000 K and 14 000 K. Outside this temperature range, however, they instead follow the results found for such stars in.Cen. The abundances derived from our observations are for most elements (except He and P) within the abundance range expected from evolutionary models that include the effects of atomic diffusion and assume a surface mixed mass of 10(-7) M-circle dot. The abundances predicted by stratified model atmospheres are generally significantly more extreme than observed, except for Mg. When effective temperatures, surface gravities, and masses are determined with stratified model spectra, the hotter stars agree better with canonical evolutionary predictions. Conclusions. Our results show definite promise towards solving the long-standing problem of surface gravity and mass discrepancies for hot HB stars, but much work is still needed to arrive at a self-consistent solution. C1 [Moehler, S.] European So Observ, D-85748 Garching, Germany. [Moehler, S.] Inst Theoret Phys & Astrophys, D-24118 Kiel, Germany. [Dreizler, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [LeBlanc, F.; Khalack, V.] Univ Moncton, Dept Phys & Astron, Moncton, NB E1A 3E9, Canada. [Michaud, G.; Richer, J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Sweigart, A. V.] NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. [Grundahl, F.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. RP Moehler, S (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM smoehler@eso.org; dreizler@astro.physik.uni-goettingen.de; francis.leblanc@umoncton.ca; viktor.khalak@umoncton.ca; michaudg@umontreal.ca; jacques.richer@umontreal.ca; allen.sweigart@gmail.com; fgj@phys.au.dk OI Moehler, Sabine/0000-0002-4152-9643 NR 52 TC 5 Z9 5 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 MAY PY 2014 VL 565 AR A100 DI 10.1051/0004-6361/201322953 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900100 ER PT J AU Presotto, V Girardi, M Nonino, M Mercurio, A Grillo, C Rosati, P Biviano, A Annunziatella, M Balestra, I Cui, W Sartoris, B Lemze, D Ascaso, B Moustakas, J Ford, H Fritz, A Czoske, O Ettori, S Kuchner, U Lombardi, M Maier, C Medezinski, E Molino, A Scodeggio, M Strazzullo, V Tozzi, P Ziegler, B Bartelmann, M Benitez, N Bradley, L Brescia, M Broadhurst, T Coe, D Donahue, M Gobat, R Graves, G Kelson, D Koekemoer, A Melchior, P Meneghetti, M Merten, J Moustakas, LA Munari, E Postman, M Regos, E Seitz, S Umetsu, K Zheng, W Zitrin, A AF Presotto, V. Girardi, M. Nonino, M. Mercurio, A. Grillo, C. Rosati, P. Biviano, A. Annunziatella, M. Balestra, I. Cui, W. Sartoris, B. Lemze, D. Ascaso, B. Moustakas, J. Ford, H. Fritz, A. Czoske, O. Ettori, S. Kuchner, U. Lombardi, M. Maier, C. Medezinski, E. Molino, A. Scodeggio, M. Strazzullo, V. Tozzi, P. Ziegler, B. Bartelmann, M. Benitez, N. Bradley, L. Brescia, M. Broadhurst, T. Coe, D. Donahue, M. Gobat, R. Graves, G. Kelson, D. Koekemoer, A. Melchior, P. Meneghetti, M. Merten, J. Moustakas, L. A. Munari, E. Postman, M. Regos, E. Seitz, S. Umetsu, K. Zheng, W. Zitrin, A. TI Intracluster light properties in the CLASH-VLT cluster MACS J1206.2-0847 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: individual: MACS J1206.2-0847; cosmology: observations ID DIFFUSE OPTICAL LIGHT; SIMULATED GALAXY CLUSTERS; STAR-FORMATION EFFICIENCY; RAY BRIGHTEST CLUSTERS; X-RAY; SURFACE PHOTOMETRY; MASSIVE GALAXIES; CD-GALAXIES; COSMOLOGICAL SIMULATIONS; DYNAMICAL FRICTION AB Aims. We aim constrain the assembly history of clusters by studying the intracluster light (ICL) properties, estimating its contribution to the fraction of baryons in stars, f(*), and understanding possible systematics or bias using different ICL detection techniques. Methods. We developed an automated method, GALtoICL, based on the software GALAPAGOS, to obtain a refined version of typical BCG+ICL maps. We applied this method to our test case MACS J1206.2-0847, a massive cluster located at z similar to 0 : 44, which is part of the CLASH sample. Using deep multiband Subaru images, we extracted the surface brightness (SB) profile of the BCG+ICL and studied the ICL morphology, color, and contribution to f(*) out to R500. We repeated the same analysis using a different definition of the ICL, SBlimit method, i.e., a SB cut-off level, to compare the results. Results. The most peculiar feature of the ICL in MACS1206 is its asymmetric radial distribution, with an excess in the SE direction and extending toward the second brightest cluster galaxy, which is a post starburst galaxy. This suggests an interaction between the BCG and this galaxy that dates back to tau <= 1.5 Gyr. The BCG+ICL stellar content is similar to 8% of M-*, (500), and the (de-) projected baryon fraction in stars is f(*) = 0.0177(0.0116), in excellent agreement with recent results. The SBlimit method provides systematically higher ICL fractions and this effect is stronger at lower SB limits. This is due to the light from the outer envelopes of member galaxies that contaminate the ICL. Though more time consuming, the GALtoICL method provides safer ICL detections that are almost free of this contamination. This is one of the few ICL study at redshift z > 0.3. At completion, the CLASH/VLT program will allow us to extend this analysis to a statistically significant cluster sample spanning a wide redshift range: 0.2 less than or similar to z.0 less than or similar to 6. C1 [Presotto, V.; Girardi, M.; Annunziatella, M.; Cui, W.; Sartoris, B.] Univ Trieste, Dipartimento Fis, I-34143 Trieste, Italy. [Presotto, V.; Girardi, M.; Nonino, M.; Biviano, A.; Annunziatella, M.; Balestra, I.; Cui, W.; Sartoris, B.; Munari, E.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Mercurio, A.; Balestra, I.; Brescia, M.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Grillo, C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Rosati, P.] Univ Ferrara, Dipartimento Fis Sci Terra, I-44122 Ferrara, Italy. [Cui, W.] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia. [Sartoris, B.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Lemze, D.; Ford, H.; Zheng, W.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ascaso, B.; Molino, A.; Benitez, N.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Moustakas, J.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Fritz, A.; Scodeggio, M.] IASF Milano, INAF, I-20133 Milan, Italy. [Czoske, O.; Kuchner, U.; Maier, C.; Ziegler, B.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Ettori, S.; Meneghetti, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Ettori, S.; Meneghetti, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Lombardi, M.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Medezinski, E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Strazzullo, V.] CEA Saclay, F-91191 Gif Sur Yvette, France. [Tozzi, P.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Bartelmann, M.] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany. [Bradley, L.; Coe, D.; Koekemoer, A.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Broadhurst, T.] Univ Basque Country, Dept Theoret Phys, Bilbao 48080, Spain. [Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Gobat, R.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM Paris Saclay,CEA,DSM,CNRS,Irfu, F-91191 Gif Sur Yvette, France. [Graves, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Graves, G.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Kelson, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Melchior, P.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Merten, J.; Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Regos, E.] CERN, European Lab Particle Phys, CH-1211 Geneva 23, Switzerland. [Seitz, S.] Univ Observ Munich, D-81679 Munich, Germany. [Seitz, S.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Zitrin, A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RP Presotto, V (reprint author), Univ Trieste, Dipartimento Fis, Via Tiepolo 11, I-34143 Trieste, Italy. RI Ettori, Stefano/N-5004-2015; Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015; Cui, Weiguang/P-4953-2014; OI Biviano, Andrea/0000-0002-0857-0732; LOMBARDI, MARCO/0000-0002-3336-4965; Moustakas, Leonidas/0000-0003-3030-2360; Koekemoer, Anton/0000-0002-6610-2048; Benitez, Narciso/0000-0002-0403-7455; Tozzi, Paolo/0000-0003-3096-9966; Ettori, Stefano/0000-0003-4117-8617; Grillo, Claudio/0000-0002-5926-7143; Meneghetti, Massimo/0000-0003-1225-7084; Cui, Weiguang/0000-0002-2113-4863; Maier, Christian/0000-0001-6405-2182; Nonino, Mario/0000-0001-6342-9662; Balestra, Italo/0000-0001-9660-894X; Scodeggio, Marco/0000-0002-2282-5850; Brescia, Massimo/0000-0001-9506-5680; Umetsu, Keiichi/0000-0002-7196-4822 FU PRIN-INAF2010; MIUR [J91J12000450001]; European Commission's Framework Programme 7, through the Marie Curie Initial Training Network CosmoComp [PITN-GA-2009-238356]; ARC [DP130100117]; Survey Simulation Pipeline (SSimPL); INAF through VIPERS; NASA [HST-HF-51334.01-A]; STScI FX We thank the anonymous referee for constructive comments that helped us to improve the manuscript. V.P. is grateful to Monaco, P., Murante, G., and De Grandi, S. for useful discussion and comments. V.P. acknowledges the grant "Cofinanziamento di Ateneo 2010" and financial support from PRIN-INAF2010 and MIUR PRIN2010-2011 (J91J12000450001). W.C. acknowledges a fellowship from the European Commission's Framework Programme 7, through the Marie Curie Initial Training Network CosmoComp (PITN-GA-2009-238356), supports from ARC DP130100117 and from the Survey Simulation Pipeline (SSimPL; http://ssimpl-universe.tk/). A.F. acknowledges the support by INAF through VIPERS grants PRIN 2008 and PRIN 2010. The work of LAM was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for A.Z. is provided by NASA through Hubble Fellowship grant #HST-HF-51334.01-A awarded by STScI. NR 94 TC 17 Z9 17 U1 1 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 MAY PY 2014 VL 565 AR A126 DI 10.1051/0004-6361/201323251 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900126 ER PT J AU Reindl, N Rauch, T Parthasarathy, M Werner, K Kruk, JW Hamann, WR Sander, A Todt, H AF Reindl, N. Rauch, T. Parthasarathy, M. Werner, K. Kruk, J. W. Hamann, W-R Sander, A. Todt, H. TI The rapid evolution of the exciting star of the Stingray nebula SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: abundances; stars: evolution; stars: AGB and post-AGB; stars: individual: SAO 244567; stars: fundamental parameters; planetary nebulae: individual: Stingray nebula (Henize 3-1357) ID INTERMEDIATE-MASS STARS; POST-AGB STARS; PLANETARY-NEBULA; STELLAR EVOLUTION; SAKURAIS OBJECT; FG SAGITTAE; SAO-244567; TEMPERATURE; ATMOSPHERES; EXTINCTION AB Context. SAO 244567, the exciting star of the Stingray nebula, is rapidly evolving. Previous analyses suggested that it has heated up from an effective temperature of about 21 kK in 1971 to over 50 kK in the 1990s. Canonical post-asymptotic giant branch evolution suggests a relatively high mass while previous analyses indicate a low-mass star. Aims. A comprehensive model-atmosphere analysis of UV and optical spectra taken during 1988-2006 should reveal the detailed temporal evolution of its atmospheric parameters and provide explanations for the unusually fast evolution. Methods. Fitting line profiles from static and expanding non-LTE model atmospheres to the observed spectra allowed us to study the temporal change of effective temperature, surface gravity, mass-loss rate, and terminal wind velocity. In addition, we determined the chemical composition of the atmosphere. Results. We find that the central star has steadily increased its effective temperature from 38 kK in 1988 to a peak value of 60 kK in 2002. During the same time, the star was contracting, as concluded from an increase in surface gravity from log g = 4.8 to 6.0 and a drop in luminosity. Simultaneously, the mass-loss rate declined from log(M/M-circle dot yr(-1)) = -9.0 to -11.6 and the terminal wind velocity increased from v(infinity) = 1800 km s(-1) to 2800 km s(-1). Since around 2002, the star stopped heating and has cooled down again to 55 kK by 2006. It has a largely solar surface composition with the exception of slightly subsolar carbon, phosphorus, and sulfur. The results are discussed by considering different evolutionary scenarios. Conclusions. The position of SAO 244567 in the log T-eff-log g plane places the star in the region of sdO stars. By comparison with stellar-evolution calculations, we confirm that SAO 244567 must be a low-mass star (M < 0.55 M-circle dot). However, the slow evolution of the respective stellar evolutionary models is in strong contrast to the observed fast evolution and the young planetary nebula with a kinematical age of only about 1000 years. We speculate that the star could be a late He-shell flash object. Alternatively, it could be the outcome of close-binary evolution. Then SAD 244567 would be a low-mass (0.354 M-circle dot) helium pre-white dwarf after the common-envelope phase, during which the planetary nebula was ejected. C1 [Reindl, N.; Rauch, T.; Werner, K.] Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany. [Parthasarathy, M.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hamann, W-R; Sander, A.; Todt, H.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. RP Reindl, N (reprint author), Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, Sand 1, D-72076 Tubingen, Germany. EM reindl@astro.uni-tuebingen.de FU German Research Foundation (DFG) [WE 1312/41-1]; German Aerospace Center (DLR) [05 OR 0806]; NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G] FX N.R. is supported by the German Research Foundation (DFG, grant WE 1312/41-1), TR by the German Aerospace Center (DLR, grant 05 OR 0806). We thank Marcelo Miguel Miller Bertolami and Philip Hall for helpful discussions and comments. M.P. is grateful to Profs. Ajit K. Kembhavi, Kandaswamy Subramanian and T. Padmanabhan for their kind encouragement, support, and hospitality. This research has made use of the SIMBAD database, operated at the CDS, Strasbourg, France. This research made use of NASA's Astrophysics Data System. This work used the profile-fitting procedure OWENS developed by M. Lemoine and the French FUSE Team. 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 49 TC 5 Z9 5 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2014 VL 565 AR A40 DI 10.1051/0004-6361/201323189 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900040 ER PT J AU Sanna, A Cesaroni, R Moscadelli, L Zhang, Q Menten, KM Molinari, S Garatti, ACO De Buizer, JM AF Sanna, A. Cesaroni, R. Moscadelli, L. Zhang, Q. Menten, K. M. Molinari, S. Garatti, A. Caratti O. De Buizer, J. M. TI A subarcsecond study of the hot molecular core in G023.01-00.41 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: kinematics and dynamics; instrumentation: high angular resolution; stars individual: G23.01-0.41; stars: formation ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; GALACTIC PLANE; MASSIVE STARS; HI-GAL; OUTFLOWS; EMISSION; G23.01-0.41; PROTOSTARS; ACCRETION AB Context. Searching for disk-outflow systems in massive star-forming regions is a key to assessing the main physical processes in the recipe of massive star formation. Aims. We have selected a hot molecular core (HMC) in the high-mass star-forming region G023.011-00.41, where VLBI multi-epoch observations of water and methanol masers have suggested the existence of rotation and expansion within 2000 AU of its center. Our piu-pose is to image the thermal line and continuum emission at millimeter was to establish the physical parameters and velocity field of the gas in the region. Methods. We performed SMA observations at 1.3 mm with both the most extended and compact array configurations, providing subarcsecond and high sensitivity maps of various molecular lines, including both hot-core and outflow tracers. We also reconstructed the spectral energy distribution of the region from millimeter to near infrared wavelengths, using the Herschel/Hi-GAL maps, as well as archival data. Results. From the spectral energy distribution, we derive a bolometric luminosity of similar to 4 x 10(4) L-circle dot. Our interferometric observations reveal that the distribution of dense gas and dust in the HMC is significantly flattened and extends up to a radius of 8000 AU from the center of radio continuum and maser emission in the region. The equatorial plane of this HMC is strictly perpendicular to the elongation of the collimated bipolar outflow, as imaged on scales of similar to 0.1-0.5 pc in the main CO isotopomers, as well as in the SiO(5-4) line. In the innermost LIMC regions (less than or similar to 1000 AU), the velocity.field traced by the CH3CN (12(K)-11(K)) line emission shows that molecular gas is both expanding along the outflow direction following a Hubble law and rotating about the outflow axis, in agreement with the (3D) velocity field traced by methanol masers. The velocity field associated with rotation indicates a dynamical mass of similar to 19 M-circle dot at the center of the core. The latter is likely to be concentrated in a single O9.5 ZAMS star, consistent with the estimated bolometric luminosity of G023.01-00.41. The physical properties of the CO (2-1) outflow emission, such as its momentum rate 6 x 10(-3) M-circle dot km s(-1) yr(-1) and its outflow rate 2 x 10(-4) M circle dot yr(-1), support our estimates of the luminosity (and mass) of the embedded young stellar object. C1 [Sanna, A.; Menten, K. M.; Garatti, A. Caratti O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Cesaroni, R.; Moscadelli, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Molinari, S.] INAF IFSI, I-00133 Rome, Italy. [De Buizer, J. M.] NASA, Stratospher Observ Infrared Astron USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Sanna, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM asanna@mpifr-bonn.mpg.de RI Molinari, Sergio/O-4095-2016; OI Molinari, Sergio/0000-0002-9826-7525; Moscadelli, Luca/0000-0002-8517-8881; Cesaroni, Riccardo/0000-0002-2430-5103; Caratti o Garatti, Alessio/0000-0001-8876-6614; Zhang, Qizhou/0000-0003-2384-6589 FU European Research Council for the ERC Advanced [247078]; National Aeronautics and Space Administration FX Comments from the anonymous referee, which helped improving our paper, are gratefully acknowledged. Financial support by the European Research Council for the ERC Advanced Grant GLOSTAR (ERC-2009-AdG, Grant Agreement no. 247078) is gratefully acknowledged. This research made use of the myXCLASS program (https//www.astro.uni-koeln.de/projects/schilke/XCLASS), which accesses the CDMS (http//www.cdms.de) and JPL (http://spec.jpl.nasa.gov) molecular databases. This publication makes use of data products from the Widefield Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 37 TC 9 Z9 9 U1 1 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2014 VL 565 AR A34 DI 10.1051/0004-6361/201323129 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900034 ER PT J AU Sokolovsky, KV Schinzel, FK Tanaka, YT Abolmasov, PK Angelakis, E Bulgarelli, A Carrasco, L Cenko, SB Cheung, CC Clubb, KI D'Ammando, F Escande, L Fegan, SJ Filippenko, AV Finke, JD Fuhrmann, L Fukazawa, Y Hays, E Healey, SE Ikejiri, Y Itoh, R Kawabata, KS Komatsu, T Kovalev, YA Kovalev, YY Krichbaum, TP Larsson, S Lister, ML Lott, B Max-Moerbeck, W Nestoras, I Pittori, C Pursimo, T Pushkarev, AB Readhead, ACS Recillas, E Richards, JL Riquelme, D Romani, RW Sakimoto, K Sasada, M Schmidt, R Shaw, MS Sievers, A Thompson, DJ Uemura, M Ungerechts, H Vercellone, S Verrecchia, F Yamanaka, M Yoshida, M Zensus, JA AF Sokolovsky, K. V. Schinzel, F. K. Tanaka, Y. T. Abolmasov, P. K. Angelakis, E. Bulgarelli, A. Carrasco, L. Cenko, S. B. Cheung, C. C. Clubb, K. I. D'Ammando, F. Escande, L. Fegan, S. J. Filippenko, A. V. Finke, J. D. Fuhrmann, L. Fukazawa, Y. Hays, E. Healey, S. E. Ikejiri, Y. Itoh, R. Kawabata, K. S. Komatsu, T. Kovalev, Yu A. Kovalev, Y. Y. Krichbaum, T. P. Larsson, S. Lister, M. L. Lott, B. Max-Moerbeck, W. Nestoras, I. Pittori, C. Pursimo, T. Pushkarev, A. B. Readhead, A. C. S. Recillas, E. Richards, J. L. Riquelme, D. Romani, R. W. Sakimoto, K. Sasada, M. Schmidt, R. Shaw, M. S. Sievers, A. Thompson, D. J. Uemura, M. Ungerechts, H. Vercellone, S. Verrecchia, F. Yamanaka, M. Yoshida, M. Zensus, J. A. TI Two active states of the narrow-line gamma-ray-loud AGN GB 1310+487 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE quasars: individual: GB 1310+487; galaxies: jets; gamma rays: galaxies; radiation mechanisms: non-thermal; galaxies: active ID LARGE-AREA TELESCOPE; BL-LACERTAE OBJECTS; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; ALL-SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; INVERSE-COMPTON CATASTROPHE; COMPACT NONTHERMAL SOURCES; FERMI-DETECTED BLAZARS; RAPID TEV VARIABILITY; AGILE SPACE MISSION AB Context. Previously unremarkable, the extragalactic radio source GB 1310+487 showed gamma-ray flare on 2009 November 18, reaching a daily flux of similar to 10(-6) photons cm(-2) s(-1) at energies E > 100 MeV and became one of the brightest GeV sources for about two weeks. Its optical spectrum shows strong forbidden-line emission while lacking broad permitted lines, which is not typical for a blazar. Instead, the spectrum resembles those of narrow emission-line galaxies. Aims. We investigate changes in the object's radio-to-GeV spectral energy distribution (SED) during and after the prominent gamma-ray flare with the aim of determining the nature of the object and of constraining the origin of the variable high-energy emission. Methods. The data collected by the Fermi and AGILE satellites at gamma-ray energies; Swift at X-ray and ultraviolet (UV); the Kanata, NOT, and Keck telescopes at optical; OAGH and WISE at infrared (IR); and IRAM 30m, OVRO 40m, Effelsberg 100 m, RATAN-600, and VLBA at radio are analyzed together to trace the SED evolution on timescales of months. Results. The gamma-ray/ radio-loud narrow-line active galactic nucleus (AGN) is located at redshift z = 0.638. It shines through an unrelated foreground galaxy at z = 0.500. The AGN light is probably amplified by gravitational lensing. The AGN SED shows a two-humped structure typical of blazars and gamma-ray-loud narrow-line Seyfert 1 galaxies, with the high-energy (inverse-Compton) emission dominating by more than an order of magnitude over the low-energy (synchrotron) emission during gamma-ray flares. The difference between the two SED humps is smaller during the low-activity state. Fermi observations reveal a strong correlation between the gamma-ray flux and spectral index, with the hardest spectrum observed during the brightest gamma-ray state. The gamma-ray flares occurred before and during a slow rising trend in the radio, but no direct association between gamma-ray and radio flares could be established. Conclusions. If the gamma-ray flux is a mixture of synchrotron self-Compton and external Compton emission, the observed GeV spectral variability may result from varying relative contributions of these two emission components. This explanation fits the observed changes in the overall IR to gamma-ray SED. C1 [Sokolovsky, K. V.; Schinzel, F. K.; Angelakis, E.; Fuhrmann, L.; Kovalev, Y. Y.; Krichbaum, T. P.; Nestoras, I.; Pushkarev, A. B.; Schmidt, R.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Sokolovsky, K. V.; Kovalev, Yu A.; Kovalev, Y. Y.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Sokolovsky, K. V.; Abolmasov, P. K.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Schinzel, F. K.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Tanaka, Y. T.; Kawabata, K. S.; Uemura, M.; Yoshida, M.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Bulgarelli, A.] INAF IASF Bologna, I-40129 Bologna, Italy. [Carrasco, L.; Recillas, E.] Inst Nacl Astrofis Opt & Electr, Mexico City 72860, DF, Mexico. [Cenko, S. B.; Clubb, K. I.; Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cenko, S. B.; Hays, E.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Cheung, C. C.] Naval Res Lab, Washington, DC 20375 USA. [D'Ammando, F.] Univ Perugia, Dipartimento Fis, I-060123 Perugia, Italy. [D'Ammando, F.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [D'Ammando, F.] INAF IRA Bologna, I-40129 Bologna, Italy. [Escande, L.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France. [Fegan, S. J.] Ecole Polytech, Lab Leprince Ringuet, CNRS, IN2P3, F-91120 Palaiseau, France. [Finke, J. D.] US Naval Res Lab, Washington, DC 20375 USA. [Fukazawa, Y.; Ikejiri, Y.; Itoh, R.; Komatsu, T.; Sakimoto, K.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Healey, S. E.; Romani, R. W.; Shaw, M. S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Larsson, S.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Larsson, S.] AlbaNova, Oskar Klein Ctr Cosmoparticie Phys, S-10691 Stockholm, Sweden. [Larsson, S.] Stockholm Univ, Dept Phys, AlbaNova, S-10691 Stockholm, Sweden. [Lister, M. L.; Richards, J. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Lott, B.] Univ Bordeaux, CENBG, UMR 5797, F-33170 Gradignan, France. [Lott, B.] CNRS, CENBG, IN2P3, UMR 5797, F-33170 Gradignan, France. [Max-Moerbeck, W.; Readhead, A. C. S.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91101 USA. [Pittori, C.; Verrecchia, F.] ASI ASDC, I-00044 Rome, Italy. [Pursimo, T.] Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain. [Pushkarev, A. B.] Pulkovo Observ, St Petersburg 196140, Russia. [Pushkarev, A. B.] Crimean Astrophys Observ, UA-98409 Nauchnyi, Crimea, Ukraine. [Riquelme, D.; Sievers, A.; Ungerechts, H.] Inst Radioastron Milimetr, Granada 18012, Spain. [Sasada, M.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Vercellone, S.] INAF IASF Palermo, I-90146 Palermo, Italy. [Yamanaka, M.] Kyoto Univ, Kwasan Observ, Yamashina Ku, Kyoto 6078471, Japan. RP Sokolovsky, KV (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM kirx@scan.sai.msu.ru RI Kovalev, Yuri/J-5671-2013; Sokolovsky, Kirill/D-2246-2015; Kovalev, Yuri/N-1053-2015; Pushkarev, Alexander/M-9997-2015; Pittori, Carlotta/C-7710-2016 OI Kovalev, Yuri/0000-0001-9303-3263; Sokolovsky, Kirill/0000-0001-5991-6863; Pittori, Carlotta/0000-0001-6661-9779 FU INSU/CNRS (France); MPG (Germany); IGN (Spain); NASA [NNX08AW31G, NNG06GG1G]; NSF [AST-0808050, AST-1211916]; NASA-Fermi [NNX08AV67G]; W. M. Keck Foundation; NASA Fermi Guest Investigator program [NXX12A075G]; Russian Foundation for Basic Research [11-02-00368, 13-02-12103]; Physical Sciences Division of the Russian Academy of Sciences; Ministry of Education and Science of the Russian Federation [8405, 14.518.11.7054]; Dynasty Foundation; Science Education Complex of the Lebedev Physical Inst. (UNK-FIAN); Presidium of the Russian Academy of Sciences; NASA/Fermi [NNX12AF12GA]; Christopher R. Redlich Fund; NASA FX We thank Sara Cutini, Marco Ajello, Denis Bastieri, Boris Komberg, Seth Digel, Luca Latronico and the anonymous referee for discussions and comments that helped improve this paper. The Fermi/LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration (NASA) and the Department of Energy in the United States, the Commissariat l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, and the Swedish Research Council as well as the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d' Etudes Spatiales in France. We acknowledge the use of public data from the Swift data archive at the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. Based in part on observations with the 100m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) and the IRAM 30m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). The OVRO 40m monitoring program is supported in part by NASA grants NNX08AW31G and NNG06GG1G, and by NSF grant AST-0808050. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2009a). The data presented herein were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. The MOJAVE project is supported under NASA-Fermi grant NNX08AV67G. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We thank O. Fox, P. Kelly, I. Shivvers, and W. Zheng for assistance with some of the Keck observations. The near-IR observations were carried out with the 2.1m telescope of the Guillermo Haro Observatory, INAOE, Mexico. F. K. S. and K. V. S. were partly supported for this research. F. K. S. acknowledges support by the NASA Fermi Guest Investigator program, grant NXX12A075G. I.N. and R. S. are members of the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. K. V. S., Y. A. K., and Y. Y. K. were supported in part by the Russian Foundation for Basic Research (Projects 11-02-00368 and 13-02-12103), the basic research program "Active processes in galactic and extragalactic objects" of the Physical Sciences Division of the Russian Academy of Sciences, and the Ministry of Education and Science of the Russian Federation (agreement No. 8405). Y. Y. K. was also supported by the Dynasty Foundation.; RATAN-600 operations were carried out with the financial support of the Ministry of Education and Science of the Russian Federation (contract 14.518.11.7054). K. V. S. was supported by the Science Education Complex of the Lebedev Physical Inst. (UNK-FIAN). A. B. P. was supported by the "Non-stationary processes in the Universe" Program of the Presidium of the Russian Academy of Sciences. A. V. F. and S. B. C. are grateful for the support of NASA/Fermi grant NNX12AF12GA, NSF grant AST-1211916, the Christopher R. Redlich Fund, and Gary and Cynthia Bengier. 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 NASA. We also used NASA's Astrophysics Data System. K. V. S. thanks Maria Mogilen for her help in preparing this manuscript. NR 204 TC 1 Z9 1 U1 0 U2 9 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2014 VL 565 AR A26 DI 10.1051/0000-6361/201220703 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900026 ER PT J AU Ueta, T Ladjal, D Exter, KM Otsuka, M Szczerba, R Siodmiak, N Aleman, I van Hoof, PAM Kastner, JH Montez, R McDonald, I Wittkowski, M Sandin, C Ramstedt, S De Marco, O Villaver, E Chu, YH Vlemmings, W Izumiura, H Sahai, R Lopez, JA Balick, B Zijlstra, A Tielens, AGGM Rattray, RE Behar, E Blackman, EG Hebden, K Hora, JL Murakawa, K Nordhaus, J Nordon, R Yamamura, I AF Ueta, T. Ladjal, D. Exter, K. M. Otsuka, M. Szczerba, R. Siodmiak, N. Aleman, I. van Hoof, P. A. M. Kastner, J. H. Montez, R., Jr. McDonald, I. Wittkowski, M. Sandin, C. Ramstedt, S. De Marco, O. Villaver, E. Chu, Y-H Vlemmings, W. Izumiura, H. Sahai, R. Lopez, J. A. Balick, B. Zijlstra, A. Tielens, A. G. G. M. Rattray, R. E. Behar, E. Blackman, E. G. Hebden, K. Hora, J. L. Murakawa, K. Nordhaus, J. Nordon, R. Yamamura, I. TI The Herschel Planetary Nebula Survey (HerPlaNS) I. Data overview and analysis demonstration with NGC 6781 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE infrared: stars; planetary nebulae: general; stars: winds, outflows; stars: mass-loss; planetary nebulae: individual: NGC 6781; circumstellar matter ID GIANT BRANCH STARS; OPTICAL RECOMBINATION LINES; FAR-INFRARED SPECTROSCOPY; INTERMEDIATE-MASS STARS; EXCITATION ATOMIC GAS; HELIX-NEBULA; EVOLVED STARS; CHEMICAL ABUNDANCES; INTERSTELLAR-MEDIUM; MAGELLANIC-CLOUD AB Context. This is the first of a series of investigations into far-IR characteristics of 11 planetary nebulae (PNe) under the Herschel Space Observatory open time 1 program, Herschel Planetary Nebula Survey (HerPlaNS). Aims. Using the HerPlaNS data set, we look into the PN energetics and variations of the physical conditions within the target nebulae. In the present work, we provide an overview of the survey, data acquisition and processing, and resulting data products. Methods. We performed (1) PACS/SPIRE broadband imaging to determine the spatial distribution of the cold dust component in the target PNe and (2) PACS/SPIRE spectral-energy-distribution and line spectroscopy to determine the spatial distribution of the gas component in the target PNe. Results. For the case of NGC 6781, the broadband maps confirm the nearly pole-on barrel structure of the amorphous carbon-rich dust shell and the surrounding halo having temperatures of 26-40 K. The PACS/SPIRE multiposition spectra show spatial variations of far-.IR lines that reflect the physical stratification of the nebula. We demonstrate that spatially resolved far-IR line diagnostics yield the (T-e, n(e)) profiles, from which distributions of ionized, atomic, and molecular gases can be determined. Direct comparison of the dust and gas column mass maps constrained by the HerPlaNS data allows to construct an empirical gas-to-dust mass ratio map, which shows a range of ratios with the median of 195 +/- 110. The present analysis yields estimates of the total mass of the shell to be 0.86 M-circle dot, consisting of 0.54 M-circle dot of ionized gas, 0.12 M-circle dot of atomic gas, 0.2 M-circle dot of molecular gas, and 4 x 10(-3) M-circle dot of dust grains. These estimates' also suggest that the central star of about 1.5 M-circle dot initial mass is terminating its PN evolution onto the white dwarf cooling track. Conclusions. The HerPlaNS data provide various diagnostics for both the dust and gas components in a spatially resolved manner. In the forthcoming papers of the HerPlaNS series we will explore the HerPlaNS data set fully for the entire sample of 11 PNe. C1 [Ueta, T.; Ladjal, D.; Rattray, R. E.] Univ Denver, Dept Phys & Astron, Denver, CO 80210 USA. [Ueta, T.; Yamamura, I.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Exter, K. M.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Otsuka, M.] Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. [Szczerba, R.; Siodmiak, N.] N Copernicus Astron Ctr, PL-87100 Torun, Poland. [Aleman, I.; Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Hoof, P. A. M.] Royal Observ Belgium, B-1180 Brussels, Belgium. [Kastner, J. H.] Rochester Inst Technol, Rochester, NY 14623 USA. [Montez, R., Jr.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [McDonald, I.; Zijlstra, A.; Hebden, K.] Jodrell Batik Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Wittkowski, M.] ESO, D-85748 Garching, Germany. [Sandin, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Ramstedt, S.] Uppsala Univ, Div Astron & Space Phys, Dept Phys & Astron, S-75120 Uppsala, Sweden. [De Marco, O.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Villaver, E.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. [Chu, Y-H] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Vlemmings, W.] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. [Izumiura, H.] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan. [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lopez, J. A.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 22800, Baja California, Mexico. [Balick, B.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Behar, E.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Blackman, E. G.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14618 USA. [Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murakawa, K.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Nordhaus, J.] Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 USA. [Nordon, R.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. RP Ueta, T (reprint author), Univ Denver, Dept Phys & Astron, 2112 E Wesley Ave, Denver, CO 80210 USA. EM tueta@du.edu RI Aleman, Isabel/F-3251-2012; OI /0000-0002-2700-9916; Wittkowski, Markus/0000-0002-7952-9550 FU NASA by jet Propulsion Laboratory, Caltech; NASA by jet Propulsion Laboratory, Ladjal; NASA by jet Propulsion Laboratory, Kastner; NASA by jet Propulsion Laboratory, Sahai; Japan Society for the Promotion of Science (JSPS); Belgian Federal Science Policy Office via the PRODEX Programme of ESA; Polish NCN [2011/01/B/ST9/02031]; European Research Council via the advanced-ERC [246976]; Dutch Science Agency (NWO) via the Dutch Astrochemistry Network; NASA FX This work is based on observations made with the Herschel Space Observatory, a European Space Agency (ESA) Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by jet Propulsion Laboratory, Caltech Ladjal, Kastner, Sahai), the Japan Society for the Promotion of Science (JSPS) through a FY2013 long-term invitation fellowship program (Ueta), the Belgian Federal Science Policy Office via the PRODEX Programme of ESA (Exter, van Hoof), the Polish NCN through a grant 2011/01/B/ST9/02031 (Szczerba, Siodmiak), and the European Research Council via the advanced-ERC grant 246976 and the Dutch Science Agency (NWO) via the Dutch Astrochemistry Network and the Spinoza prize (Aleman, Tielens). The authors thank M. A. Guerrero for sharing the NOT optical images of NGC 6781 with us. Also, H. Monteiro's generosity is appreciated for the reproduction of one of his figures (Fig. 3 of Schwarz & Monteiro 2006). Sahai acknowledges that his contribution to the research described here was carried out at the JPE/Caltech, under a contract with NASA. Finally, Ueta also acknowledges the hospitality of the members of the Laboratory of Infrared Astrophysics at ISAS/JAXA during his sabbatical stay as a JSPS invitation fellow. NR 84 TC 7 Z9 7 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 MAY PY 2014 VL 565 AR A36 DI 10.1051/0004-6361/201423395 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900036 ER PT J AU Waizmann, JC Redlich, M Meneghetti, M Bartelmann, M AF Waizmann, J-C Redlich, M. Meneghetti, M. Bartelmann, M. TI The strongest gravitational lenses Ill. The order statistics of the largest Einstein radii SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gravitational lensing: strong; methods: statistical; galaxies: clusters: general; cosmology: miscellaneous ID STRONG-LENSING ANALYSIS; MACS J0717.5+3745; GALAXY CLUSTERS; LAMBDA-CDM; MASS-DISTRIBUTION; COMPLETE SAMPLE; ARC STATISTICS; UNIVERSE; IMAGES; A1689 AB Context. The Einstein radius of a gravitational lens is a key characteristic. It encodes information about decisive quantities such as halo mass, concentration, triaxiality, and orientation with respect to the observer. Therefore, the largest Einstein radii can potentially be utilised to test the predictions of the ACDM model. Aims. Hitherto, studies have focussed on the single largest observed Einstein radius. We extend those studies by employing order statistics to formulate exclusion criteria based on the n largest Einstein radii and apply these criteria to the strong lensing analysis of 12 MACS clusters at z > 0.5. Methods. We obtain the order statistics of Einstein radii by a Monte Carlo approach, based on the semi-analytic modelling of the halo population on the past lightcone. After sampling the order statistics, we fit a general extreme value distribution to the first-order distribution, which allows us to derive analytic relations for the order statistics of the Einstein radii. Results. We find that the Einstein radii of the 12 MACS clusters are not in conflict with the ACDM expectations. Our exclusion criteria indicate that, in order to exhibit tension with the concordance model, one would need to observe approximately twenty Einstein radii with theta(eff) greater than or similar to 30 '', ten with theta(eff) greater than or similar to 35 '', five with theta(eff) greater than or similar to 42 '', or one with theta(eff) greater than or similar to 74 '' in the redshift range 0.5 <= z <= 1.0 on the full sky (assuming a source redshift of z(s) = 2). Furthermore, we find that, with increasing order, the haloes with the largest Einstein radii are on average less aligned along the line-of-sight and less triaxial. In general, the ctunulative distribution functions steepen for higher orders, giving them better constraining power. Conclusions. A framework that allows the individual and joint order distributions of the n-largest Einstein radii to be derived is presented. From a statistical point of view, we do not see any evidence of an Einstein ring problem even for the largest Einstein radii of the studied MACS sample. This conclusion is consolidated by the large uncertainties that enter the lens modelling and to which the largest Einstein radii are particularly sensitive. C1 [Waizmann, J-C] Blue Yonder GmbH, D-76139 Karlsruhe, Germany. [Waizmann, J-C] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Waizmann, J-C; Meneghetti, M.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Waizmann, J-C; Meneghetti, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Redlich, M.; Bartelmann, M.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Meneghetti, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Waizmann, JC (reprint author), Blue Yonder GmbH, Karlsruher Str 88, D-76139 Karlsruhe, Germany. EM jean-claude.waizmann@blue-yonder.com RI Meneghetti, Massimo/O-8139-2015 OI Meneghetti, Massimo/0000-0003-1225-7084 FU ASI-INAF [I/023/05/0, I/088/06/0]; ASI [I/016/07/0 COFIS]; ASI Euclid-DUNE [I/064/08/0]; ASI-Uni Bologna-Astronomy Dept. Euclid-NIS [I/039/10/0]; PRIN MIUR; German Academic Exchange Service (DAAD); Internationale Spitzenforschung II-1 of the Baden-Wurttemberg Stiftung; Dark Universe of the German Science Foundation [Transregio-Sonderforschungsbereich TR 33] FX J.C.W. acknowledges financial contributions from the contracts ASI-INAF I/023/05/0, ASI-INAF I/088/06/0, ASI I/016/07/0 COFIS, ASI Euclid-DUNE I/064/08/0, ASI-Uni Bologna-Astronomy Dept. Euclid-NIS I/039/10/0, and PRIN MIUR 2008 Dark energy and cosmology with large galaxy surveys. M.R. thanks the Sydney Institute for Astronomy for the hospitality and the German Academic Exchange Service (DAAD) for their financial support. Furthermore, M.R.'s work was supported in part by contract research Internationale Spitzenforschung II-1 of the Baden-Wurttemberg Stiftung. M.B. is supported in part by the Transregio-Sonderforschungsbereich TR 33 The Dark Universe of the German Science Foundation. NR 33 TC 3 Z9 3 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2014 VL 565 AR A28 DI 10.1051/0004-6361/201323022 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900028 ER PT J AU Li, C Su, CH Lehoczky, SL Scripa, RN Ban, H Lin, B AF Li, C. Su, Ching-Hua Lehoczky, S. L. Scripa, R. N. Ban, H. Lin, B. TI Thermophysical properties of HgTe and Hg0.9Cd0.1Te melts SO JOURNAL OF NON-CRYSTALLINE SOLIDS LA English DT Article DE II-VI semiconductor melt; Density; Electrical conductivity; Viscosity ID ELECTRICAL-CONDUCTIVITY; DISORDERED MATERIALS; LIQUID TE; VISCOSITY; HG1-XCDXTE; DENSITY; HG0.8CD0.2TE; TRANSPORT; MERCURY; PHASE AB Thermophysical properties, namely, density, viscosity, and electrical conductivity of HgTe and Hg0.9Cd0.1Te melts were measured as a function of temperature. A pycnometric method was used to measure the melt density in the temperature range of 948 to 1073 K for the HgTe melt and 1011 to 1131 K for the Hg0.9Cd0.1Te melt. The density results show a maximum at 1023 and 1020 K, respectively, for the HgTe and Hg0.9Cd0.1Te melts. The viscosity and electrical conductivity were simultaneously determined using a transient torque method from 944 to 1098 K for the HgTe melt and from 1016 to 1127 K for the Hg0.9Cd0.1Te melt. The measured electrical conductivity decreases as the mole fraction of CdTe, x, increases at a specific temperature, and increases as a function of temperature, which shows a semiconductor-like behavior. The measured viscosity decreases as the mole fraction of CdTe, x, increases at a specific temperature and decreases as the temperature increased. The analysis of the electrical conductivity of the melts and the relationship between the kinematic viscosity and density implied a structural transition in these melts. No relaxation phenomena were observed in the density, electrical conductivity, and viscosity of the HgTe and Hg0.9Cd0.1Te melts. Published by Elsevier B.V. C1 [Li, C.; Scripa, R. N.] Univ Alabama Birmingham, Dept Mat Sci & Engn, Birmingham, AL 35294 USA. [Su, Ching-Hua; Lehoczky, S. L.] NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Huntsville, AL 35812 USA. [Ban, H.; Lin, B.] Univ Alabama Birmingham, Dept Mech Engn, Birmingham, AL 35294 USA. RP Su, CH (reprint author), NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Huntsville, AL 35812 USA. EM ching.h.su@nasa.gov FU Advanced Capabilities Division, Exploration Systems Mission Directorate, NASA Headquarter FX The author would like to acknowledge the supports of the Advanced Capabilities Division, Exploration Systems Mission Directorate, NASA Headquarter. NR 26 TC 0 Z9 0 U1 1 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-3093 EI 1873-4812 J9 J NON-CRYST SOLIDS JI J. Non-Cryst. Solids PD MAY 1 PY 2014 VL 391 BP 54 EP 60 DI 10.1016/j.jnoncrysol.2014.03.012 PG 7 WC Materials Science, Ceramics; Materials Science, Multidisciplinary SC Materials Science GA AI5AA UT WOS:000336876600010 ER PT J AU Agu, NC Redwine, KM Bell, C Garcia, KM Martin, DS Poffenbarger, TS Bricker, JT Portman, RJ Gupta-Malhotra, M AF Agu, Ngozi C. Redwine, Karen McNiece Bell, Cynthia Garcia, Kathleen Marie Martin, David S. Poffenbarger, Tim S. Bricker, John T. Portman, Ronald J. Gupta-Malhotra, Monesha TI Detection of early diastolic alterations by Tissue Doppler Imaging in untreated childhood-onset essential hypertension SO JOURNAL OF THE AMERICAN SOCIETY OF HYPERTENSION LA English DT Article DE Echocardiography; hypertension; pediatrics; insulin; diastole ID LEFT-VENTRICULAR MASS; ALTERED MYOCARDIAL-METABOLISM; MITRAL ANNULUS VELOCITY; BLOOD-PRESSURE; CARDIOVASCULAR-DISEASE; DIABETES-MELLITUS; AMERICAN-SOCIETY; HEART-FAILURE; BODY-SIZE; CHILDREN AB The aim of the study was to determine the presence of preclinical diastolic dysfunction in hypertensive children relative to normotensive children by Tissue Doppler Imaging (TDI). We prospectively enrolled children with untreated essential hypertension in absence of any other disease and a matched healthy control group with normal blood pressure (BP); both groups confirmed by clinic BP and a 24-hour ambulatory BP monitoring. Echocardiographic diastolic parameters were determined using spectral transmitral inflow Doppler, flow propagation velocity, TDI, and systolic parameters were determined via midwall shortening fraction and ejection fraction. A total of 80 multiethnic children were prospectively enrolled for the study: 46 hypertensive (median age, 13 years; 72% males) and 34 control (median age, 14 years; 65% males). The only echocardiography parameters that had a statistically significant change compared with the control children, were regional mitral Ea, Aa, and the E/Ea ratio by TDI. In comparison with controls, hypertensive children had lower Ea and Aa velocities of anterior and posterior walls and higher lateral wall E/Ea ratio. The decrease in posterior wall Ea and Aa remained significant after adjustment for gender, age, body mass index, ethnicity, and left ventricular hypertrophy on multivariate analysis. The lateral and septal wall E/Ea ratios correlated significantly with fasting serum insulin levels on similar multivariate analysis. Decreased regional TDI velocities were seen with preserved left ventricular systolic function even when other measures of diastolic dysfunction remained unchanged in untreated hypertensive children. Hypertension and serum insulin levels had strong associations with preclinical diastolic alterations in children. (C) 2014 American Society of Hypertension. All rights reserved. C1 [Agu, Ngozi C.; Bricker, John T.; Gupta-Malhotra, Monesha] Univ Texas Houston, Childrens Mem Hermann Hosp, Sch Med, Dept Pediat,Div Pediat Cardiol, Houston, TX 77030 USA. [Redwine, Karen McNiece; Gupta-Malhotra, Monesha] Univ Arkansas Med Sci, Arkansas Childrens Hosp, Dept Pediat, Div Pediat Nephrol, Little Rock, AR 72205 USA. [Redwine, Karen McNiece; Bell, Cynthia; Poffenbarger, Tim S.; Portman, Ronald J.] Univ Texas Houston, Childrens Mem Hermann Hosp, Sch Med, Dept Pediat,Div Pediat Nephrol, Houston, TX 77030 USA. [Garcia, Kathleen Marie; Martin, David S.] Wyle Sci Technol & Engn, Natl Aeronaut & Space Adm, Johnson Space Ctr, Cardiovasc Lab, Houston, TX USA. RP Gupta-Malhotra, M (reprint author), Univ Texas Houston, Childrens Mem Hermann Hosp, Houston Med Sch, Div Pediat Cardiol, 6410 Fannin St,UTPB Ste 425, Houston, TX 77030 USA. EM Monesha.gupta@uth.tmc.edu RI Bell, Cynthia/B-1634-2009 OI Bell, Cynthia/0000-0002-2366-1843 FU National Heart, Lung, and Blood Institute [K23HL089391]; Dr Gupta's Faculty Development Grant - University of Texas Health Science Center at Houston; Dr Redwine's Ruth L. Kirschstein National Research Service Individual Fellowship Award [F32 HL079813]; University of Texas Health Science Center at Houston General Clinical Research Center [M01-RR 0255] FX The project described was partially supported by Grant Number K23HL089391 (PI Monesha Gupta) from the National Heart, Lung, and Blood Institute. The content is solely the responsibility of the authors and does not necessarily represent the official views of the National Heart, Lung, and Blood Institute or the National Institutes of Health. A portion of the study was funded by Dr Gupta's Faculty Development Grant from the University of Texas Health Science Center at Houston. A portion of the study was funded by Dr Redwine's Ruth L. Kirschstein National Research Service Individual Fellowship Award (F32 HL079813) and the University of Texas Health Science Center at Houston General Clinical Research Center (M01-RR 0255). NR 51 TC 6 Z9 6 U1 0 U2 1 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1933-1711 EI 1878-7436 J9 J AM SOC HYPERTENS JI J. Am. Soc. Hypertens. PD MAY PY 2014 VL 8 IS 5 BP 303 EP 311 DI 10.1016/j.jash.2014.02.008 PG 9 WC Peripheral Vascular Disease SC Cardiovascular System & Cardiology GA AI5DS UT WOS:000336886200005 PM 24685005 ER PT J AU Davarian, F AF Davarian, Faramaz TI In Search of Earth-Like Planets SO PROCEEDINGS OF THE IEEE LA English DT Editorial Material C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Davarian, F (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9219 EI 1558-2256 J9 P IEEE JI Proc. IEEE PD MAY PY 2014 VL 102 IS 5 SI SI BP 643 EP 645 DI 10.1109/JPROC.2014.2314771 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA AI5NR UT WOS:000336915700001 ER PT J AU Hartwig, J Darr, S AF Hartwig, Jason Darr, Samuel TI Influential factors for liquid acquisition device screen selection for cryogenic propulsion systems SO APPLIED THERMAL ENGINEERING LA English DT Article DE Cryogenics; Liquid acquisition device; Porous screen; Surface tension; Fuel depot ID SURFACE-TENSION; POINT; MIXTURES; FLOW AB This paper presents the influential factors which govern screen selection for liquid acquisition devices (LADS) operating in microgravity conditions for future in-space cryogenic propulsion engines and cryogenic propellant depots. Space flight requirements, which include mass flow rate, acceleration level and direction, and thermal environment, dictate screen selection for a particular mission. The five influential factors include bubble point pressure, flow-through-screen pressure drop, wicking rate, screen compliance, and material compatibility. Governing equations and analytical models for these parameters are developed from first principles. A comprehensive survey of the historical data on coarser LAD meshes over four decades of work is conducted, and liquid hydrogen data for finer Dutch Twill meshes (325 x 2300, 450 x 2750, 510 x 3600) from recently concluded experiments is also presented to validate analytical models. Each of these parameters is measurable from ground based tests, making it facile to predict flight system performance. Therefore analytical models in this paper will be valuable for future LAD designs for both cryogenic and storable propulsion systems. Additionally, analysis will be given on the impact of the factors on liquid hydrogen systems. Published by Elsevier Ltd. C1 [Hartwig, Jason] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Darr, Samuel] Univ Florida, Gainesville, FL 32611 USA. RP Hartwig, J (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM Jason.W.Hartwig@nasa.gov OI Darr, Samuel/0000-0002-1891-405X NR 55 TC 12 Z9 13 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-4311 J9 APPL THERM ENG JI Appl. Therm. Eng. PD MAY PY 2014 VL 66 IS 1-2 BP 548 EP 562 DI 10.1016/j.applthermaleng.2014.02.022 PG 15 WC Thermodynamics; Energy & Fuels; Engineering, Mechanical; Mechanics SC Thermodynamics; Energy & Fuels; Engineering; Mechanics GA AH7YT UT WOS:000336352000057 ER PT J AU Kolli, KK Arif, I Peelukhana, SV Succop, P Back, LH Helmy, TA Leesar, MA Effat, MA Banerjee, RK AF Kolli, Kranthi K. Arif, Imran Peelukhana, Srikara V. Succop, Paul Back, Lloyd H. Helmy, Tarek A. Leesar, Massoud A. Effat, Mohamed A. Banerjee, Rupak K. TI Diagnostic Performance of Pressure Drop Coefficient in Relation to Fractional Flow Reserve and Coronary Flow Reserve SO JOURNAL OF INVASIVE CARDIOLOGY LA English DT Article DE coronary disease; FFR; CFR; catheterization; meta-analysis ID CONCOMITANT MICROVASCULAR DISEASE; HEMODYNAMIC END-POINTS; PORCINE MODEL; VELOCITY RESERVE; BLOOD-FLOW; CARDIAC-CATHETERIZATION; ARTERY-DISEASE; HEART-RATE; STENOSIS; INDEX AB Objectives and Background. Functional assessment of coronary lesion severity during cardiac catheterization is conducted using diagnostic parameters like fractional flow reserve (FFR; pressure derived) and coronary flow reserve (CFR; flow derived). However, the complex hemodynamics of stenosis might not be sufficiently explained by either pressure or flow alone, particularly in the case of intermediate stenosis. CDP (ratio of pressure drop across a stenosis to distal dynamic pressure), a non-dimensional index derived from fundamental fluid dynamic principles based on a combination of intracoronary pressure and flow, may improve the functional assessment of coronary lesion severity. Methods. We performed a meta-analysis of seven studies, retrieved from MEDLINE and PubMed, comparing the results of FFR and CFR of the same lesions. Two studies reported functional measurements (pressure and flow) obtained in individual patients. Five studies reported two-dimensional plots of FFR vs CFR. The FFR and CFR data were digitized and corresponding funetional measurements were extracted using the reported mean values of hemodynamic data from each of the five studies. The receiver operating characteristic (ROC) curve was used to identify the optimal cut-off point of CDP, which corresponds to the clinically used cut-off values (FFR = 0.80, FFR = 0.75, and CFR = 2.0). Results. CDP correlated significantly with FFR (r = 0.78; P<.001) and had significant diagnostic efficiency (area under the ROC curve = 89%), specificity (83% and 85%), and sensitivity (81% and 76%) at FFR <0.8 and FFR <0.75, respectively. The corresponding cut-off value for CDP to detect FFR <0.80 and FFR <0.75 was at CDP >27.1 and CDP >27.9, respectively. Conclusions. CDP, a functional parameter based on both intracoronary pressure and flow measurements, has close agreement (area under the ROC curve = 89%) with FFR, the most frequently used method for evaluation of coronary stenosis severity. C1 [Kolli, Kranthi K.; Peelukhana, Srikara V.; Banerjee, Rupak K.] Univ Cincinnati, Dept Mech & Mat Engn, Cincinnati, OH USA. [Arif, Imran; Helmy, Tarek A.; Effat, Mohamed A.] Univ Cincinnati, Div Cardiovasc Dis, Cincinnati, OH USA. [Succop, Paul] Univ Cincinnati, Dept Environm Hlth, Cincinnati, OH USA. [Kolli, Kranthi K.; Arif, Imran; Peelukhana, Srikara V.; Helmy, Tarek A.; Effat, Mohamed A.; Banerjee, Rupak K.] Vet Affairs Med Ctr, Cincinnati, OH 45267 USA. [Back, Lloyd H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Leesar, Massoud A.] Univ Alabama Birmingham, Div Cardiovasc Dis, Birmingham, AL USA. RP Banerjee, RK (reprint author), Dept Mech & Mat Engn, 598 Rhodes Hall,POB 210072, Cincinnati, OH 45221 USA. EM Rupak.Banerjee@UC.edu FU Department of Veteran Affairs through VA Merit Review Grant [I01CX000342-01] FX This work is supported by financial support from Department of Veteran Affairs through VA Merit Review Grant (I01CX000342-01). NR 36 TC 3 Z9 3 U1 1 U2 4 PU H M P COMMUNICATIONS PI MALVERN PA 83 GENERAL WARREN BLVD, STE 100, MALVERN, PA 19355 USA SN 1042-3931 EI 1557-2501 J9 J INVASIVE CARDIOL JI J. Invasive Cardiol. PD MAY PY 2014 VL 26 IS 5 BP 188 EP 195 PG 8 WC Cardiac & Cardiovascular Systems SC Cardiovascular System & Cardiology GA AI0BM UT WOS:000336511200001 PM 24791716 ER PT J AU Fulton, JA Edwards, JR Hassan, HA McDaniel, JC Goyne, CP Rockwell, RD Cutler, AD Johansen, CT Danehy, PM AF Fulton, Jesse A. Edwards, Jack R. Hassan, Hassan A. McDaniel, James C. Goyne, Christopher P. Rockwell, Robert D. Cutler, Andrew D. Johansen, Craig T. Danehy, Paul M. TI Large-Eddy/Reynolds-Averaged Navier-Stokes Simulations of Reactive Flow in Dual-Mode Scramjet Combustor SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID LARGE-EDDY SIMULATION; SUPERSONIC COMBUSTION; HYDROGEN-AIR AB Numerical simulations of the turbulent reactive flow within a model scramjet combustor configuration, experimentally mapped at the University of Virginia's Scramjet Combustion Facility at an equivalence ratio of 0.17, are described in this paper. A hybrid large-eddy simulation/Reynolds-averaged Navier-Stokes method is used, with special attention focused on capturing facility-specific effects, such as asymmetric inflow temperature distributions, on flow development within the combustor. Predictions obtained using two nine-species hydrogen oxidation models are compared with experimental data obtained using coherent anti-Stokes Raman spectroscopy, hydroxyl radical planar laser-induced fluorescence, stereoscopic particle image velocimetry, and focusing schlieren techniques. The large-eddy simulation/Reynolds-averaged Navier-Stokes models accurately capture the mean structure of the fully developed flame but tend to overpredict fluctuation levels toward the outer edge of the reactive plume. Model predictions worsen in the flame-anchoring region just downstream of the fuel injector. Here, turbulence/chemistry interactions are more pronounced, and the flame is more influenced by the inflow conditions. Comparisons with hydroxyl radical planar laser-induced fluorescence imagery indicate that the large-eddy simulation/Reynolds-averaged Navier-Stokes model can capture the effects of larger turbulent scales in deforming the flame structure but does not capture the effects of small turbulent structures in broadening the OH profiles. C1 [Fulton, Jesse A.; Edwards, Jack R.; Hassan, Hassan A.] N Carolina State Univ, Raleigh, NC 27695 USA. [McDaniel, James C.; Goyne, Christopher P.; Rockwell, Robert D.] Univ Virginia, Charlottesville, VA 22904 USA. [Cutler, Andrew D.] George Washington Univ, Newport News, VA 23602 USA. [Johansen, Craig T.] Univ Calgary, Calgary, AB T2N 1N4, Canada. [Danehy, Paul M.] NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA. RP Fulton, JA (reprint author), N Carolina State Univ, Raleigh, NC 27695 USA. FU National Center for Hypersonic Combined Cycle Propulsion [FA 9550-09-1-0611] FX This work was sponsored by the National Center for Hypersonic Combined Cycle Propulsion (grant FA 9550-09-1-0611), with technical monitors Chiping Li (U.S. Air Force Office of Scientific Research) and Rick Gaffney (NASA). The authors would like to thank Chad Smith at the University of Virginia; Gaetano Magnotti, Luca Cantu, and Emanuela Gallo at George Washington University; Ron Hanson, Jay Jeffries, Ian Schultz, and Chris Goldenstein at Stanford University; and Toshinori Kouchi at Tohoku University for providing experimental data and for many helpful discussions. Computing time was obtained from NASA's National Academy of Science supercomputing resource and by the Department,of Defense's High-Performance Computing modernization program. NR 40 TC 8 Z9 8 U1 2 U2 22 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 EI 1533-3876 J9 J PROPUL POWER JI J. Propul. Power PD MAY-JUN PY 2014 VL 30 IS 3 BP 558 EP 575 DI 10.2514/1.B34929 PG 18 WC Engineering, Aerospace SC Engineering GA AH7ZI UT WOS:000336353500005 ER PT J AU Mao, HS Wirz, RE Goebel, DM AF Mao, Hann-Shin Wirz, Richard E. Goebel, Dan M. TI Plasma Structure of Miniature Ring-Cusp Ion Thruster Discharges SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID PERFORMANCE AB Previous miniature ion thruster studies have demonstrated impressive performance using ring-cusp discharges. These studies suggest that the magnetic field must be sufficiently strong to increase primary electron confinement times for ionization, but weak enough to allow plasma electrons to escape and maintain the plasma potential necessary for ionization. To investigate these phenomena, an experiment was developed to allow detailed measurements of the internal structure and characteristics of a miniature ring-cusp discharge. These measurements provide spatially resolved values for plasma density, electron temperature, and plasma potential along a meridian plane. The magnetic field configuration is arranged as a quasi-periodic domain in order to generalize the findings to all multipole discharges. The results show that the magnetic field strength drives the plasma structure, and the dependence on discharge power can be removed with proper scaling of the plasma parameters. The stronger magnetic field results in a higher peak plasma density, but relatively low discharge utilization efficiency. In addition, the potential measurements indicate the likely onset of discharge instability. In contrast, the weaker magnetic field, or baseline. configuration, better uses the volume of the chamber. This leads to a higher and more uniform density near the downstream end of the discharge where ion extraction would occur, implying superior discharge utilization. C1 [Mao, Hann-Shin; Wirz, Richard E.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Goebel, Dan M.] CALTECH, Jet Prop Lab, Prop & Mat Engn Sect, Pasadena, CA 91109 USA. RP Mao, HS (reprint author), Univ Calif Los Angeles, Los Angeles, CA 90095 USA. NR 20 TC 0 Z9 0 U1 5 U2 13 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 EI 1533-3876 J9 J PROPUL POWER JI J. Propul. Power PD MAY-JUN PY 2014 VL 30 IS 3 BP 628 EP 636 DI 10.2514/1.B34759 PG 9 WC Engineering, Aerospace SC Engineering GA AH7ZI UT WOS:000336353500010 ER PT J AU Talukder, A Panangadan, A AF Talukder, Ashit Panangadan, Anand TI Extreme event detection and assimilation from multimedia sources SO MULTIMEDIA TOOLS AND APPLICATIONS LA English DT Article DE Event detection; Information retrieval; Matching; Multimedia; Representation; Search; Spatio-temporal trajectory; Tracking ID VIDEO; MODEL AB A new event-based multimedia processing framework for detection, retrieval, and cross-media content assimilation of geo-spatiotemporal phenomena is described. Multimedia information relevant to geo-spatiotemporal events are available from sources such as remote satellites, in-situ sensors as image streams, and other outlets such as news articles, weather bulletins as text documents and in various formats, each with widely varying properties. We pose an event-based framework to automatically detect geo-spatiotemporal phenomena from raw untagged remote-sensing satellite image streams, extract attributes for such events, match the spatiotemporal properties of the detected phenomenon with events in a database to automatically derive a media-independent event description, and subsequently use the media-independent event descriptions to assimilate relevant information of the same event across other media sources from the web using a mashup. A virtual globe interface enables simultaneous visualization of the assimilated spatiotemporal information annotated with Internet sources. This framework is demonstrated for the automatic detection of tropical cyclones from satellite imagery followed by the retrieval and assimilation of related information from government-run weather sites and commercial news portals. C1 [Talukder, Ashit] NIST, Gaithersburg, MD 20899 USA. [Panangadan, Anand] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Talukder, A (reprint author), NIST, 100 Bur Dr,Mail Stop 8940, Gaithersburg, MD 20899 USA. EM ashit.talukder@nist.gov; Anand.V.Panangadan@jpl.nasa.gov FU National Aeronautics and Space Administration (NASA) Applied Information Systems Research (AISR) Program FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology with funding from the National Aeronautics and Space Administration (NASA) Applied Information Systems Research (AISR) Program. The authors acknowledge the contributions of Eric Rigor, Andrew Bingham, and Shen-shyang Ho. NR 38 TC 1 Z9 1 U1 0 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1380-7501 EI 1573-7721 J9 MULTIMED TOOLS APPL JI Multimed. Tools Appl. PD MAY PY 2014 VL 70 IS 1 BP 237 EP 261 DI 10.1007/s11042-012-1088-y PG 25 WC Computer Science, Information Systems; Computer Science, Software Engineering; Computer Science, Theory & Methods; Engineering, Electrical & Electronic SC Computer Science; Engineering GA AI4AK UT WOS:000336807300010 ER PT J AU Freeman, JC AF Freeman, Jon C. TI Self-heating in semiconductors: A comparative study SO SOLID-STATE ELECTRONICS LA English DT Article DE Heat generation; Bipolar semiconductor; Numerical simulation; Thermoelectric ID DEVICES; GENERATION; CONDUCTION; SIMULATION; DIODES; MODEL; SI AB A new expression for the source term H, in the heat flow equation is developed for bipolar semiconductors. This term consists of heat generated by carrier-lattice collisions, recombination of electrons and holes, and other processes. The expression allows self-consistent calculations of self-heating in any device. The derivation is based on thermoelectric concepts. There exists several expressions for H in the general literature for calculating the temperature field, and the presently developed one is compared with the older ones. Discrepancies exist between all of the formulas and reasons for them are given. (C) 2014 Published by Elsevier Ltd. C1 Natl Aeronaut & Space Adm, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Freeman, JC (reprint author), Natl Aeronaut & Space Adm, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM freem231@umn.edu NR 43 TC 1 Z9 1 U1 3 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-1101 EI 1879-2405 J9 SOLID STATE ELECTRON JI Solid-State Electron. PD MAY PY 2014 VL 95 BP 8 EP 14 DI 10.1016/j.sse.2014.02.005 PG 7 WC Engineering, Electrical & Electronic; Physics, Applied; Physics, Condensed Matter SC Engineering; Physics GA AI3QI UT WOS:000336776600002 ER PT J AU Yamamoto, N Gdoutos, E Toda, R White, V Manohara, H Daraio, C AF Yamamoto, Namiko Gdoutos, Eleftherios Toda, Risaku White, Victor Manohara, Harish Daraio, Chiara TI Thin Films with Ultra-low Thermal Expansion SO ADVANCED MATERIALS LA English DT Article DE ultra-low thermal expansion; thermal stability; thin films; metals; microstructures ID DIGITAL-IMAGE-CORRELATION; HIGH STIFFNESS; OPTIMIZATION; COEFFICIENT; SYSTEMS; DESIGN C1 [Yamamoto, Namiko; Gdoutos, Eleftherios; Daraio, Chiara] CALTECH, Grad Aerosp Labs, Pasadena, CA 91125 USA. [Toda, Risaku; White, Victor; Manohara, Harish] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Daraio, Chiara] Swiss Fed Inst Technol, Dept Mech & Proc Engn, CH-8092 Zurich, Switzerland. RP Yamamoto, N (reprint author), CALTECH, Grad Aerosp Labs, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM namikoy@caltech.edu RI Daraio, Chiara/N-2170-2015 OI Daraio, Chiara/0000-0001-5296-4440 FU Keck Institute for Space Studies, Center Innovation Funds (CIF) from Jet Propulsion Laboratory; Government sponsorship FX The authors acknowledge Prof. Craig A. Steeves from University of Toronto, Mr. Keith Patterson from California Institute of Technology, Dr. Andrew A. Shapiro and Dr. James Breckinridge from Jet Propulsion Laboratory, and Ms. Elisha Byrne from the Correlated Solutions, Inc. for helpful discussions and technical assistance. This work was supported by the Keck Institute for Space Studies, Center Innovation Funds (CIF) from Jet Propulsion Laboratory. A part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. (c) 2010 California Institute of Technology. Government sponsorship acknowledged. NR 23 TC 11 Z9 11 U1 3 U2 25 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0935-9648 EI 1521-4095 J9 ADV MATER JI Adv. Mater. PD MAY PY 2014 VL 26 IS 19 BP 3076 EP 3080 DI 10.1002/adma.201304997 PG 5 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA AH1GW UT WOS:000335869100017 PM 24677188 ER PT J AU Han, JW Oh, JS Meyyappan, M AF Han, Jin-Woo Oh, Jae Sub Meyyappan, M. TI Cofabrication of Vacuum Field Emission Transistor (VFET) and MOSFET SO IEEE TRANSACTIONS ON NANOTECHNOLOGY LA English DT Article DE Beyond CMOS; field emission; insulated-gate; monolithic integration; more than Moore; vacuum field emission transistor (VFET) ID TRIODE; FABRICATION; AMPLIFIER AB Co-fabrication of a nanoscale vacuum field emission transistor (VFET) and a metal-oxide-semiconductor field effect transistor (MOSFET) is demonstrated on a silicon-on-insulator wafer. The insulated-gate VFET with a gap distance of 100 nm is achieved by using a conventional 0.18-mu m process technology and subsequent photoresist ashing process. The VFET shows a turn-on voltage of 2 V at a cell current of 2 nA and a cell current of 3 mu A at the operation voltage of 10 V with an ON/OFF current ratio of 10(4). The gap distance between the cathode and anode in the VFET is defined to be less than the mean free path of electrons in air, and consequently, the operation voltage is reduced to be less than the ionization potential of air molecules. This allows the relaxation of the vacuum requirement. The present integration scheme can be useful as it combines the advantages of both structures on the same chip. C1 [Han, Jin-Woo; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. [Oh, Jae Sub] Natl Nanofab Ctr, Taejon 305701, South Korea. RP Han, JW (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. EM jin-woo.han@nasa.gov; jsoh@nnfc.re.kr; m.meyyappan@nasa.gov FU Center Innovation Fund at NASA Ames Research Center FX This work was supported by the Center Innovation Fund at NASA Ames Research Center. The review of this paper was arranged by Associate Editor M. M. De Souza. NR 13 TC 8 Z9 8 U1 3 U2 26 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1536-125X EI 1941-0085 J9 IEEE T NANOTECHNOL JI IEEE Trans. Nanotechnol. PD MAY PY 2014 VL 13 IS 3 BP 464 EP 468 DI 10.1109/TNANO.2014.2310774 PG 5 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Science & Technology - Other Topics; Materials Science; Physics GA AH4IQ UT WOS:000336091000011 ER PT J AU Siegel, PH AF Siegel, Peter H. TI Untitled SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Editorial Material C1 [Siegel, Peter H.] CALTECH, Pasadena, CA 91125 USA. [Siegel, Peter H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Siegel, PH (reprint author), CALTECH, Pasadena, CA 91125 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD MAY PY 2014 VL 4 IS 3 BP 293 EP 293 DI 10.1109/TTHZ.2014.2315757 PG 1 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA AH6EH UT WOS:000336223000001 ER PT J AU Zhang, XY Tan, B Yu, YY AF Zhang, Xiaoyang Tan, Bin Yu, Yunyue TI Interannual variations and trends in global land surface phenology derived from enhanced vegetation index during 1982-2010 SO INTERNATIONAL JOURNAL OF BIOMETEOROLOGY LA English DT Article DE Long-term global phenology; Interannual variation; Trend; Remote sensing ID CONTERMINOUS UNITED-STATES; HIGH-RESOLUTION RADIOMETER; NET PRIMARY PRODUCTION; TIME-SERIES; CANOPY PHENOLOGY; GROWING-SEASON; SATELLITE DATA; TEMPORAL VARIATION; AVHRR DATA; DATA SET AB Land surface phenology is widely retrieved from satellite observations at regional and global scales, and its long-term record has been demonstrated to be a valuable tool for reconstructing past climate variations, monitoring the dynamics of terrestrial ecosystems in response to climate impacts, and predicting biological responses to future climate scenarios. This study detected global land surface phenology from the advanced very high resolution radiometer (AVHRR) and the Moderate Resolution Imaging Spectroradiometer (MODIS) data from 1982 to 2010. Based on daily enhanced vegetation index at a spatial resolution of 0.05 degrees, we simulated the seasonal vegetative trajectory for each individual pixel using piecewise logistic models, which was then used to detect the onset of greenness increase (OGI) and the length of vegetation growing season (GSL). Further, both overall interannual variations and pixel-based trends were examined across Koeppen's climate regions for the periods of 1982-1999 and 2000-2010, respectively. The results show that OGI and GSL varied considerably during 1982-2010 across the globe. Generally, the interannual variation could be more than a month in precipitation-controlled tropical and dry climates while it was mainly less than 15 days in temperature-controlled temperate, cold, and polar climates. OGI, overall, shifted early, and GSL was prolonged from 1982 to 2010 in most climate regions in North America and Asia while the consistently significant trends only occurred in cold climate and polar climate in North America. The overall trends in Europe were generally insignificant. Over South America, late OGI was consistent (particularly from 1982 to 1999) while either positive or negative GSL trends in a climate region were mostly reversed between the periods of 1982-1999 and 2000-2010. In the Northern Hemisphere of Africa, OGI trends were mostly insignificant, but prolonged GSL was evident over individual climate regions during the last 3 decades. OGI mainly showed late trends in the Southern Hemisphere of Africa while GSL was reversed from reduced GSL trends (1982-1999) to prolonged trends (2000-2010). In Australia, GSL exhibited considerable interannual variation, but the consistent trend lacked presence in most regions. Finally, the proportion of pixels with significant trends was less than 1 % in most of climate regions although it could be as large as 10 %. C1 [Zhang, Xiaoyang] S Dakota State Univ, GSCE, Brookings, SD 57007 USA. [Tan, Bin] NASA Goddard Space Flight Ctr, Earth Resources Technol Inc, Greenbelt, MD 20771 USA. [Yu, Yunyue] NOAA NESDIS STAR, College Pk, MD 20740 USA. RP Zhang, XY (reprint author), S Dakota State Univ, GSCE, 1021 Medary Ave,Wecota Hall 506B, Brookings, SD 57007 USA. EM xiaoyang.zhang@sdstate.edu RI Yu, Yunyue/F-5636-2010 FU NASA MEaSUREs [NNX08AT05A] FX This work was partially supported by NASA MEaSUREs contract NNX08AT05A. We wish to thank Kamel Didan and Armando Barreto Munoz at the University of Arizona for providing long-term EVI2 detest. NR 67 TC 21 Z9 21 U1 4 U2 53 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0020-7128 EI 1432-1254 J9 INT J BIOMETEOROL JI Int. J. Biometeorol. PD MAY PY 2014 VL 58 IS 4 BP 547 EP 564 DI 10.1007/s00484-014-0802-z PG 18 WC Biophysics; Environmental Sciences; Meteorology & Atmospheric Sciences; Physiology SC Biophysics; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences; Physiology GA AH7QU UT WOS:000336329300013 PM 24639008 ER PT J AU Dubey, A Antypas, K Calder, AC Daley, C Fryxell, B Gallagher, JB Lamb, DQ Lee, D Olson, K Reid, LB Rich, P Ricker, PM Riley, KM Rosner, R Siegel, A Taylor, NT Weide, K Timmes, FX Vladimirova, N ZuHone, J AF Dubey, Anshu Antypas, Katie Calder, Alan C. Daley, Chris Fryxell, Bruce Gallagher, J. Brad Lamb, Donald Q. Lee, Dongwook Olson, Kevin Reid, Lynn B. Rich, Paul Ricker, Paul M. Riley, Katherine M. Rosner, Robert Siegel, Andrew Taylor, Noel T. Weide, Klaus Timmes, Francis X. Vladimirova, Natasha ZuHone, John TI Evolution of FLASH, a multi-physics scientific simulation code for high-performance computing SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS LA English DT Article DE FLASH; scientific application code; multi-physics; multi-scale; community code; software evolution ID STAGGERED MESH SCHEME; RAYLEIGH-TAYLOR; MAGNETOHYDRODYNAMICS; HYDRODYNAMICS; ASTROPHYSICS; DIMENSIONS; PLUTO; FLOWS AB The FLASH code has evolved into a modular and extensible scientific simulation software system over the decade of its existence. During this time it has been cumulatively used by over a thousand researchers to investigate problems in astrophysics, cosmology, and in some areas of basic physics, such as turbulence. Recently, many new capabilities have been added to the code to enable it to simulate problems in high-energy density physics. Enhancements to these capabilities continue, along with enhancements enabling simulations of problems in fluid-structure interactions. The code started its life as an amalgamation of already existing software packages and sections of codes developed independently by various participating members of the team for other purposes. The code has evolved through a mixture of incremental and deep infrastructural changes. In the process, it has undergone four major revisions, three of which involved a significant architectural advancement. Along the way, a software process evolved that addresses the issues of code verification, maintainability, and support for the expanding user base. The software process also resolves the conflicts arising out of being in development and production simultaneously with multiple research projects, and between performance and portability. This paper describes the process of code evolution with emphasis on the design decisions and software management policies that have been instrumental in the success of the code. The paper also makes the case for a symbiotic relationship between scientific research and good software engineering of the simulation software. C1 [Dubey, Anshu; Daley, Chris; Gallagher, J. Brad; Lamb, Donald Q.; Lee, Dongwook; Taylor, Noel T.; Weide, Klaus] Univ Chicago, Flash Ctr Computat Sci, Chicago, IL 60637 USA. [Dubey, Anshu] Lawrence Berkeley Natl Lab, Computat Res Div, Berkeley, CA USA. [Antypas, Katie; Daley, Chris] Lawrence Berkeley Natl Lab, Natl Energy Res Sci Comp Ctr, Berkeley, CA USA. [Calder, Alan C.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY USA. [Calder, Alan C.] SUNY Stony Brook, Inst Adv Computat Sci, Stony Brook, NY USA. [Gallagher, J. Brad; Lamb, Donald Q.; Lee, Dongwook; Rosner, Robert; Weide, Klaus] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Lamb, Donald Q.; Lee, Dongwook; Rosner, Robert; Siegel, Andrew] Argonne Natl Lab, Math & Comp Sci Div, Argonne, IL 60439 USA. [Fryxell, Bruce] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Lamb, Donald Q.; Lee, Dongwook; Rosner, Robert] Univ Chicago, Computat Inst, Chicago, IL 60637 USA. [Lamb, Donald Q.; Lee, Dongwook; Rosner, Robert] Argonne Natl Lab, Argonne, IL 60439 USA. [Olson, Kevin] Drexel Univ, Dept Phys, Philadelphia, PA USA. [Reid, Lynn B.] Univ Western Australia, Nedlands, WA 6009, Australia. [Reid, Lynn B.] CDM Smith, Brisbane, Qld, Australia. [Rich, Paul; Riley, Katherine M.] Argonne Natl Lab, Argonne Leadership Comp Facil, Argonne, IL 60439 USA. [Ricker, Paul M.] Univ Illinois, Dept Astron, Chicago, IL 60680 USA. [Timmes, Francis X.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Timmes, Francis X.] Univ Notre Dame, Joint Inst Nucl Astrophys, Notre Dame, IN 46556 USA. [Vladimirova, Natasha] Univ New Mexico, Dept Math & Stat, Albuquerque, NM 87131 USA. [ZuHone, John] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD USA. RP Dubey, A (reprint author), Univ Chicago, 5747 S Ellis Ave, Chicago, IL 60637 USA. EM adubey@lbl.gov OI Weide, Klaus/0000-0001-9869-9750 FU DOE [B523820]; US DOE NNSA ASC through the Argonne Institute for Computing in Science [57789]; NSF [5-27429] FX The FLASH code was in part developed by the DOE-supported ASC/Alliance Center for Astrophysical Thermonuclear Flashes at the University of Chicago (grant number B523820). The continued development has been supported in part by the US DOE NNSA ASC through the Argonne Institute for Computing in Science (field work proposal 57789) and by a NSF Peta-apps grant (grant number 5-27429). NR 33 TC 2 Z9 2 U1 0 U2 8 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1094-3420 EI 1741-2846 J9 INT J HIGH PERFORM C JI Int. J. High Perform. Comput. Appl. PD MAY PY 2014 VL 28 IS 2 SI SI BP 225 EP 237 DI 10.1177/1094342013505656 PG 13 WC Computer Science, Hardware & Architecture; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA AH6EE UT WOS:000336222700006 ER PT J AU Williams, CR Bringi, VN Carey, LD Chandrasekar, V Gatlin, PN Haddad, ZS Meneghini, R Munchak, SJ Nesbitt, SW Petersen, WA Tanelli, S Tokay, A Wilson, A Wolff, DB AF Williams, Christopher R. Bringi, V. N. Carey, Lawrence D. Chandrasekar, V. Gatlin, Patrick N. Haddad, Ziad S. Meneghini, Robert Munchak, S. Joseph Nesbitt, Stephen W. Petersen, Walter A. Tanelli, Simone Tokay, Ali Wilson, Anna Wolff, David B. TI Describing the Shape of Raindrop Size Distributions Using Uncorrelated Raindrop Mass Spectrum Parameters SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article DE Precipitation; Rainfall; Algorithms; Radars; Radar observations; Satellite observations ID FREQUENCY RADAR MEASUREMENTS; TRMM PRECIPITATION RADAR; GAMMA-DISTRIBUTIONS; RETRIEVAL ALGORITHM; PROFILING ALGORITHM; MOMENT ESTIMATORS; VIDEO DISDROMETER; MICROPHYSICS; ERRORS; BIAS AB Rainfall retrieval algorithms often assume a gamma-shaped raindrop size distribution (DSD) with three mathematical parameters N-w, D-m, and . If only two independent measurements are available, as with the dual-frequency precipitation radar on the Global Precipitation Measurement (GPM) mission core satellite, then retrieval algorithms are underconstrained and require assumptions about DSD parameters. To reduce the number of free parameters, algorithms can assume that is either a constant or a function of D-m. Previous studies have suggested - constraints [where = (4 + )/D-m], but controversies exist over whether - constraints result from physical processes or mathematical artifacts due to high correlations between gamma DSD parameters. This study avoids mathematical artifacts by developing joint probability distribution functions (joint PDFs) of statistically independent DSD attributes derived from the raindrop mass spectrum. These joint PDFs are then mapped into gamma-shaped DSD parameter joint PDFs that can be used in probabilistic rainfall retrieval algorithms as proposed for the GPM satellite program. Surface disdrometer data show a high correlation coefficient between the mass spectrum mean diameter D-m and mass spectrum standard deviation sigma(m). To remove correlations between DSD attributes, a normalized mass spectrum standard deviation is constructed to be statistically independent of D-m, with representing the most likely value and std representing its dispersion. Joint PDFs of D-m and are created from D-m and . A simple algorithm shows that rain-rate estimates had smaller biases when assuming the DSD breadth of than when assuming a constant . C1 [Williams, Christopher R.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Williams, Christopher R.] NOAA, ESRL Phys Sci Div, Boulder, CO USA. [Bringi, V. N.; Chandrasekar, V.] Colorado State Univ, Ft Collins, CO 80523 USA. [Carey, Lawrence D.] Univ Alabama, Huntsville, AL 35899 USA. [Gatlin, Patrick N.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Haddad, Ziad S.; Tanelli, Simone] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Meneghini, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Munchak, S. Joseph] Univ Maryland, College Pk, MD 20742 USA. [Nesbitt, Stephen W.] Univ Illinois, Urbana, IL USA. [Petersen, Walter A.; Wolff, David B.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. [Tokay, Ali] Univ Maryland Baltimore Cty, Greenbelt, MD USA. [Wilson, Anna] Duke Univ, Durham, NC USA. RP Williams, CR (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, 216 UCB, Boulder, CO 80309 USA. EM christopher.williams@colorado.edu RI Williams, Christopher/A-2723-2015; Measurement, Global/C-4698-2015; OI Williams, Christopher/0000-0001-9394-8850; Gatlin, Patrick/0000-0001-9345-1457 FU NASA Global Precipitation Measurement (GPM) mission [NNX13AI94G, NNX10AM54G, NNX13AF89G, NNX12AD03A, NNX10AP84G, NNX13AF86G, NNX13AJ55G, NNX13AI89G, NNX10AH66G]; NASA Precipitation Measurement Missions (PMM) FX Support for this work was provided by Ramesh Kakar under the NASA Precipitation Measurement Missions (PMM) and NASA Global Precipitation Measurement (GPM) mission, including Grants NNX13AI94G, NNX10AM54G, NNX13AF89G, NNX12AD03A, NNX10AP84G, NNX13AF86G, NNX13AJ55G, NNX13AI89G, and NNX10AH66G. The authors thank Dr. Merhala Thurai for her insightful discussions. NR 37 TC 17 Z9 17 U1 5 U2 20 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 MAY PY 2014 VL 53 IS 5 BP 1282 EP 1296 DI 10.1175/JAMC-D-13-076.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AG6ZF UT WOS:000335567000010 ER PT J AU Dong, XQ Xi, BK Kennedy, A Minnis, P Wood, R AF Dong, Xiquan Xi, Baike Kennedy, Aaron Minnis, Patrick Wood, Robert TI A 19-Month Record of Marine Aerosol- Cloud-Radiation Properties Derived from DOE ARM Mobile Facility Deployment at the Azores. Part I: Cloud Fraction and Single-Layered MBL Cloud Properties SO JOURNAL OF CLIMATE LA English DT Article DE Boundary layer; Cloud cover; Diurnal effects; Subsidence; Aerosols; Cloud microphysics ID GROUND-BASED MEASUREMENTS; LIQUID WATER PATH; GENERAL-CIRCULATION MODELS; WARM STRATOCUMULUS CLOUDS; BOUNDARY-LAYER; STRATIFORM CLOUDS; MICROPHYSICAL CONTRASTS; STRATUS; CLIMATE; ASTEX AB A 19-month record of total and single-layered low (<3 km), middle (3-6 km), and high (>6 km) cloud fractions (CFs) and the single-layered marine boundary layer (MBL) cloud macrophysical and microphysical properties was generated from ground-based measurements at the Atmospheric Radiation Measurement Program (ARM) Azores site between June 2009 and December 2010. This is the most comprehensive dataset of marine cloud fraction and MBL cloud properties. The annual means of total CF and single-layered low, middle, and high CFs derived from ARM radar and lidar observations are 0.702, 0.271, 0.01, and 0.106, respectively. Greater total and single-layered high (>6 km) CFs occurred during the winter, whereas single-layered low (<3 km) CFs were more prominent during summer. Diurnal cycles for both total and low CFs were stronger during summer than during winter. The CFs are bimodally distributed in the vertical with a lower peak at similar to 1 km and a higher peak between 8 and 11 km during all seasons, except summer when only the low peak occurs. Persistent high pressure and dry conditions produce more single-layered MBL clouds and fewer total clouds during summer, whereas the low pressure and moist air masses during winter generate more total and multilayered clouds, and deep frontal clouds associated with midlatitude cyclones.The seasonal variations of cloud heights and thickness are also associated with the seasonal synoptic patterns. The MBL cloud layer is low, warm, and thin with large liquid water path (LWP) and liquid water content (LWC) during summer, whereas during winter it is higher, colder, and thicker with reduced LWP and LWC. The cloud LWP and LWC values are greater at night than during daytime. The monthly mean daytime cloud droplet effective radius r(e) values are nearly constant, while the daytime droplet number concentration N-d basically follows the LWC variation. There is a strong correlation between cloud condensation nuclei (CCN) concentration N-CCN and N-d during January-May, probably due to the frequent low pressure systems because upward motion brings more surface CCN to cloud base (well-mixed boundary layer). During summer and autumn, the correlation between N-d and N-CCN is not as strong as that during January-May because downward motion from high pressure systems is predominant. Compared to the compiled aircraft in situ measurements during the Atlantic Stratocumulus Transition Experiment (ASTEX), the cloud microphysical retrievals in this study agree well with historical aircraft data. Different air mass sources over the ARM Azores site have significant impacts on the cloud microphysical properties and surface CCN as demonstrated by great variability in N-CCN and cloud microphysical properties during some months. C1 [Dong, Xiquan; Xi, Baike; Kennedy, Aaron] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA. [Minnis, Patrick] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA USA. [Wood, Robert] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. RP Dong, XQ (reprint author), Univ N Dakota, Dept Atmospher Sci, 4149 Campus Rd,Box 9006, Grand Forks, ND 58202 USA. EM dong@aero.und.edu RI Wood, Robert/A-2989-2008; Minnis, Patrick/G-1902-2010; OI Wood, Robert/0000-0002-1401-3828; Minnis, Patrick/0000-0002-4733-6148; Dong, Xiquan/0000-0002-3359-6117 FU U.S. Department of Energy (DOE) Office of Energy Research, Office of Health and Environmental Research, Environmental Sciences Division; NASA CERES project at the University of North Dakota project [NNX10AI05G]; DOE ASR project at the University of North Dakota [DE-SC0008468]; DOE ASR project at the University of Washington [DE-SC0006865MOD0002]; DOE ASR program under Interagency Grant [DE-SC0000991/003] FX The data were obtained from the Atmospheric Radiation Measurement (ARM) Program sponsored by the U.S. Department of Energy (DOE) Office of Energy Research, Office of Health and Environmental Research, Environmental Sciences Division. This study was primarily supported by the NASA CERES project at the University of North Dakota project under Grant NNX10AI05G and by the DOE ASR project at the University of North Dakota under a grant with Award DE-SC0008468. Dr. Robert Wood was supported by the DOE ASR project at the University of Washington with Award DE-SC0006865MOD0002. Patrick Minnis was supported by the DOE ASR program under Interagency Grant DE-SC0000991/003. Special thanks to Dr. Long, who provided the clear-sky SW fluxes over the ARM Azores site. NR 51 TC 15 Z9 15 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 MAY PY 2014 VL 27 IS 10 BP 3665 EP 3682 DI 10.1175/JCLI-D-13-00553.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AG6PO UT WOS:000335541100012 ER PT J AU Baker, NC Huang, HP AF Baker, Noel C. Huang, Huei-Ping TI A Comparative Study of Precipitation and Evaporation between CMIP3 and CMIP5 Climate Model Ensembles in Semiarid Regions SO JOURNAL OF CLIMATE LA English DT Article DE Europe; North America; Rainfall; Water budget; Ensembles; Ensembles ID GLOBAL PRECIPITATION; VARIABILITY; REANALYSES; MONSOON; GPCP; ERA AB The twentieth-century climatology and twenty-first-century trend in precipitation P, evaporation E, and P - E for selected semiarid U.S. Southwest and Mediterranean regions are compared between ensembles from phases 3 and 5 of the Coupled Model Intercomparison Project (CMIP3 and CMIP5). The twentieth-century simulations are validated with precipitation from observation and evaporation from reanalysis. It is found that the Special Report on Emissions Scenarios (SRES) A1B simulations in CMIP3 and the simulations with representative concentration pathways (RCPs) 4.5 and 8.5 in CMIP5 produce qualitatively similar seasonal cycles of the twenty-first-century trend in P - E for both semiarid regions. For the southwestern United States, it is characterized by a strong drying trend in spring, a weak moistening trend in summer, a weak drying trend in winter, and an overall drying trend for the annual mean. For the Mediterranean region, a drying trend is simulated for all seasons with an October maximum and July minimum. The consistency between CMIP3 and CMIP5 scenarios indicates that the simulated trend is robust; however, while the trend in P - E is negative in spring for the southwestern United States for all CMIP ensembles, CMIP3 predicts a strongly negative trend in P and minor negative trend in E whereas both CMIP5 scenarios predict a nearly zero trend in P and positive trend in E. For the twentieth-century simulations, the P, E, and P - E of the two model ensembles are statistically indistinguishable for most seasons. This stagnation of the simulated climatology from CMIP3 to CMIP5 implies that the hydroclimatic variable biases have not decreased in the newer generation of models. Notably, over the southwestern United States the CMIP3 models produce too much precipitation in the cold season. This bias remains almost unchanged in CMIP5. C1 [Baker, Noel C.; Huang, Huei-Ping] Arizona State Univ, Sch Engn Matter Transport & Energy, Tempe, AZ USA. RP Baker, NC (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd,Mail Stop 420, Hampton, VA 23681 USA. EM noel.c.baker@nasa.gov FU Office of Science (BER), U.S. Department of Energy FX This study is supported by the Office of Science (BER), U.S. Department of Energy. The NCEP R2 data were obtained from the NOAA ESRL/PSDdata portal (http://www.esrl.noaa.gov/psd). ECMWF ERA-Interim data have been obtained from the ECMWF data server (http://apps.ecmwf.int/datasets/). NR 25 TC 12 Z9 12 U1 2 U2 25 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD MAY PY 2014 VL 27 IS 10 BP 3731 EP 3749 DI 10.1175/JCLI-D-13-00398.1 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AG6PO UT WOS:000335541100016 ER PT J AU Holland, PR Bruneau, N Enright, C Losch, M Kurtz, NT Kwok, R AF Holland, Paul R. Bruneau, Nicolas Enright, Clare Losch, Martin Kurtz, Nathan T. Kwok, Ron TI Modeled Trends in Antarctic Sea Ice Thickness SO JOURNAL OF CLIMATE LA English DT Article DE Antarctica; Sea ice; Southern Ocean; Climate variability; Interannual variability; Trends ID OCEAN MODEL; DATA ASSIMILATION; SOUTHERN-OCEAN; CMIP5 MODELS; MASS-BALANCE; WEDDELL SEA; SNOW DEPTH; MAUD RISE; VARIABILITY; SIMULATIONS AB Unlike the rapid sea ice losses reported in the Arctic, satellite observations show an overall increase in Antarctic sea ice concentration over recent decades. However, observations of decadal trends in Antarctic ice thickness, and hence ice volume, do not currently exist. In this study a model of the Southern Ocean and its sea ice, forced by atmospheric reanalyses, is used to assess 1992-2010 trends in ice thickness and volume. The model successfully reproduces observations of mean ice concentration, thickness, and drift, and decadal trends in ice concentration and drift, imparting some confidence in the hindcasted trends in ice thickness. The model suggests that overall Antarctic sea ice volume has increased by approximately 30 km(3) yr(-1) (0.4% yr(-1)) as an equal result of areal expansion (20 x 10(3) km(2) yr(-1) or 0.2% yr(-1)) and thickening (1.5 mm yr(-1) or 0.2% yr(-1)). This ice volume increase is an order of magnitude smaller than the Arctic decrease, and about half the size of the increased freshwater supply from the Antarctic Ice Sheet. Similarly to the observed ice concentration trends, the small overall increase in modeled ice volume is actually the residual of much larger opposing regional trends. Thickness changes near the ice edge follow observed concentration changes, with increasing concentration corresponding to increased thickness. Ice thickness increases are also found in the inner pack in the Amundsen and Weddell Seas, where the model suggests that observed ice-drift trends directed toward the coast have caused dynamical thickening in autumn and winter. Modeled changes are predominantly dynamic in origin in the Pacific sector and thermodynamic elsewhere. C1 [Holland, Paul R.; Bruneau, Nicolas] British Antarctic Survey, Cambridge CB3 0ET, England. [Enright, Clare] Univ E Anglia, Tyndall Ctr Climate Change Res, Norwich NR4 7TJ, Norfolk, England. [Losch, Martin] Alfred Wegener Inst Polar & Marine Res, Bremerhaven, Germany. [Kurtz, Nathan T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kwok, Ron] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Holland, PR (reprint author), British Antarctic Survey, Madingley Rd, Cambridge CB3 0ET, England. EM p.holland@bas.ac.uk RI Holland, Paul/G-2796-2012; Kwok, Ron/A-9762-2008; Losch, Martin/S-5896-2016; OI Kwok, Ron/0000-0003-4051-5896; Losch, Martin/0000-0002-3824-5244; Bruneau, Nicolas/0000-0002-9017-1000 NR 78 TC 22 Z9 22 U1 2 U2 36 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD MAY PY 2014 VL 27 IS 10 BP 3784 EP 3801 DI 10.1175/JCLI-D-13-00301.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AG6PO UT WOS:000335541100019 ER PT J AU Eingorn, M Zhuk, A AF Eingorn, Maxim Zhuk, Alexander TI Remarks on mechanical approach to observable Universe SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE cosmological perturbation theory; gravity; dark energy theory; cosmic flows ID DARK ENERGY AB We consider the Universe deep inside the cell of uniformity. At these scales, the Universe is filled with inhomogeneously distributed discrete structures (galaxies, groups and clusters of galaxies), which perturb the background Friedmann model. Here, the mechanical approach (Eingorn & Zhuk, 2012) is the most appropriate to describe the dynamics of the inhomogeneities which is defined, on the one hand, by gravitational potentials of inhomogeneities and, on the other hand, by the cosmological expansion of the Universe. In this paper, we present additional arguments in favor of this approach. First, we estimate the size of the cell of uniformity. With the help of the standard methods of statistical physics and for the galaxies of the type of the Milky Way and Andromeda, we get that it is of the order of 190 Mpc which is rather close to observations. Then, we show that the nonrelativistic approximation (with respect to the peculiar velocities) is valid for z less than or similar to 10, i.e. approximately for 13 billion years from the present moment. We consider scalar perturbations and, within the ACDM model, justify the main equations. Moreover, we demonstrate that radiation can be naturally incorporated into our scheme. This emphasizes the viability of our approach. This approach gives a possibility to analyze different cosmological models and compare them with the observable Universe. For example, we indicate some problematic aspects of the spatially flat models. Such models require a rather specific distribution of the inhomogeneities to get a finite potential at any points outside gravitating masses. We also criticize the application of the Schwarzschild-de Sitter solution to the description of the motion of test bodies on the cosmological background. C1 [Eingorn, Maxim] N Carolina Cent Univ, CREST, Durham, NC 27707 USA. [Eingorn, Maxim] N Carolina Cent Univ, NASA, Res Ctr, Durham, NC 27707 USA. [Zhuk, Alexander] Odessa Natl Univ, Astron Observ, UA-65082 Odessa, Ukraine. RP Eingorn, M (reprint author), N Carolina Cent Univ, CREST, Fayetteville St 1801, Durham, NC 27707 USA. EM maxim.eingorn@gmail.com; ai.zhuk2@gmail.com RI Eingorn, Maxim/L-1543-2014 OI Eingorn, Maxim/0000-0002-1545-7818 FU NSF CREST award [HRD-1345219]; NASA grant [NNX09AV07A] FX The work of M. Eingorn was supported by NSF CREST award HRD-1345219 and NASA grant NNX09AV07A. NR 21 TC 17 Z9 17 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD MAY PY 2014 IS 5 AR 024 DI 10.1088/1475-7516/2014/05/024 PG 19 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AH4JC UT WOS:000336092200026 ER PT J AU DeGuzman, V Vercoutere, W Shenasa, H Deamer, D AF DeGuzman, Veronica Vercoutere, Wenonah Shenasa, Hossein Deamer, David TI Generation of Oligonucleotides Under Hydrothermal Conditions by Non-enzymatic Polymerization SO JOURNAL OF MOLECULAR EVOLUTION LA English DT Article DE RNA; Condensation reactions; Hydrolysis; Organizing matrix; Prebiotic chemistry ID POLYNUCLEOTIDE MOLECULES; RNA MOLECULES; ORIGIN; LIFE; DISCRIMINATION; EVOLUTION; ACID; RIBOZYME; CHANNEL; VENTS AB We previously reported that 5'-mononucleotides organized within a multilamellar lipid matrix can produce oligomers in the anhydrous phase of hydration-dehydration (HD) cycles. However, hydrolysis of oligomers can occur during hydration, and it is important to better understand the steady state in which ester bond synthesis is balanced by hydrolysis. In order to study condensation products of mononucleotides and hydrolysis of their polymers, we established a simulation of HD cycles that would occur on the early Earth when volcanic land masses emerged from the ocean over 4 billion years ago. At this stage on early Earth, precipitation produced hydrothermal fields characterized by small aqueous pools undergoing evaporation and refilling at elevated temperatures. Here, we confirm that under these conditions, the chemical potential made available by cycles of hydration and dehydration is sufficient to drive synthesis of ester bonds. If 5'-mononucleotides are in solution at millimolar concentrations, then oligomers resembling RNA are synthesized and exist in a steady state with their monomers. Furthermore, if the mononucleotides can form complementary base pairs, then some of the products have properties suggesting that secondary structures are present, including duplex species stabilized by hydrogen bonds. C1 [DeGuzman, Veronica; Vercoutere, Wenonah] NASA, Ames Res Ctr, Adv Studies Lab, Moffett Field, CA 94035 USA. [Shenasa, Hossein; Deamer, David] Univ Calif Santa Cruz, Dept Biomol Engn, Santa Cruz, CA 95064 USA. RP Deamer, D (reprint author), Univ Calif Santa Cruz, Dept Biomol Engn, Santa Cruz, CA 95064 USA. EM deamer@soe.ucsc.edu FU Lonsdale Research Award FX This investigation was supported by a Lonsdale Research Award, funded by a generous gift from Harry Lonsdale. NR 31 TC 10 Z9 18 U1 1 U2 38 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2844 EI 1432-1432 J9 J MOL EVOL JI J. Mol. Evol. PD MAY PY 2014 VL 78 IS 5 BP 251 EP 262 DI 10.1007/s00239-014-9623-2 PG 12 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA AI1IE UT WOS:000336603400003 PM 24821106 ER PT J AU Law, J Van Baalen, M Foy, M Mason, SS Mendez, C Wear, ML Meyers, VE Alexander, D AF Law, Jennifer Van Baalen, Mary Foy, Millennia Mason, Sara S. Mendez, Claudia Wear, Mary L. Meyers, Valerie E. Alexander, David TI Relationship Between Carbon Dioxide Levels and Reported Headaches on the International Space Station SO JOURNAL OF OCCUPATIONAL AND ENVIRONMENTAL MEDICINE LA English DT Article ID CEREBRAL-BLOOD-FLOW; AIR SUPPLY RATE; CO2 CONCENTRATIONS; PERFORMANCE; VENTILATION; RESPONSES; SYMPTOMS AB Objective: Because of anecdotal reports of CO2-related symptoms onboard the International Space Station (ISS), the relationship between CO2 and in-flight headaches was analyzed. Methods: Headache reports and CO2 measurements were obtained, and arithmetic means and single-point maxima were determined for 24-hour and 7-day periods. Multiple imputation addressed missing data, and logistic regression modeled the relationship between CO2, headache probability, and covariates. Results: CO2 level, age at launch, time in-flight, and data source were significantly associated with headache. For each 1-mm Hg increase in CO2, the odds of a crew member reporting a headache doubled. To keep the risk of headache below 1%, average 7-day CO2 would need to be maintained below 2.5 mm Hg (current ISS range: 1 to 9 mm Hg). Conclusions: Although headache incidence was not high, results suggest an increased susceptibility to physiological effects of CO2 in-flight. C1 [Law, Jennifer; Van Baalen, Mary; Meyers, Valerie E.; Alexander, David] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Foy, Millennia; Wear, Mary L.] Wyle Sci Technol & Engn, Houston, TX USA. [Mason, Sara S.; Mendez, Claudia] MEI Technol, Houston, TX USA. RP Law, J (reprint author), 2101 NASA Pkwy,Mail Code SD2, Houston, TX 77058 USA. EM jennifer.t.law@nasa.gov NR 27 TC 7 Z9 7 U1 5 U2 11 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 1076-2752 EI 1536-5948 J9 J OCCUP ENVIRON MED JI J. Occup. Environ. Med. PD MAY PY 2014 VL 56 IS 5 BP 477 EP 483 DI 10.1097/JOM.0000000000000158 PG 7 WC Public, Environmental & Occupational Health SC Public, Environmental & Occupational Health GA AH1FZ UT WOS:000335866500005 PM 24806559 ER PT J AU Love, SG Pettit, DR Messenger, SR AF Love, Stanley G. Pettit, Donald R. Messenger, Scott R. TI Particle aggregation in microgravity: Informal experiments on the International Space Station SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID PLANETESIMAL FORMATION; DUST AGGREGATION; SOLAR NEBULA; CHONDRULES; STICKING; GROWTH; COAGULATION; MECHANISMS; COLLISIONS; DYNAMICS AB We conducted experiments in space to investigate the aggregation of millimeter- and submillimeter-sized particles in microgravity, an important early step in planet formation. Particulate materials included salt (NaCl), sugar (sucrose), coffee, mica, ice, Bjurbole chondrules, ordinary and carbonaceous chondrite meteorite fragments, and acrylic and glass beads, all triply confined in clear plastic containers. Angular submillimeter particles rapidly and spontaneously formed clusters strong enough to survive turbulence in a protoplanetary nebula. Smaller particles generally aggregated more strongly and quickly than larger ones. We observed only a weak dependence of aggregation time on particle number density. We observed no strong dependence on composition. Round, smooth particles aggregated weakly or not at all. In a mixture of particle types, some phases aggregated more readily than others, creating selection effects that controlled the composition of the growing clumps. The physical process of aggregation appears to be electrostatic in nature. C1 [Love, Stanley G.; Pettit, Donald R.] NASA, Lyndon B Johnson Space Ctr, Mail Code CB, Houston, TX 77058 USA. [Messenger, Scott R.] NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, Mail Code KR,Astromat Res & Explorat Sci Director, Houston, TX 77058 USA. RP Love, SG (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code CB, 2101 NASA Pkwy, Houston, TX 77058 USA. EM stanley.g.love@nasa.gov NR 41 TC 3 Z9 3 U1 0 U2 9 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 MAY PY 2014 VL 49 IS 5 BP 732 EP 739 DI 10.1111/maps.12286 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AH9TE UT WOS:000336484500002 ER PT J AU Veres, P Farnocchia, D Jedicke, R Spoto, F AF Veres, Peter Farnocchia, Davide Jedicke, Robert Spoto, Federica TI The Effect of Parallax and Cadence on Asteroid Impact Probabilities and Warning Times SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID EARTH-APPROACHING ASTEROIDS; OBJECT PROCESSING SYSTEM; PAN-STARRS; ORBIT DETERMINATION; CHELYABINSK; ASTROMETRY; EFFICIENCY; ORIGIN AB We study the time evolution of the impact probability for synthetic, but realistic, impacting and close-approaching asteroids detected in a simulated all-sky survey. We use the impact probability to calculate the impact warning time (t(w)) as the time interval between when an object reaches a Palermo Scale value of -2 and when it impacts Earth. A simple argument shows that t(w) proportional to D-x, with the exponent in the range [1.0,1.5], and our derived value was x = 1.3 +/- 0.1. The low-precision astrometry from the single simulated all-sky survey could require many days or weeks to establish an imminent impact for asteroids larger than 100 m in diameter that are discovered far from Earth. Most close-approaching asteroids are quickly identified as not being impactors, but a size-dependent percentage, even for those larger than 50 m diameter, have a persistent impact probability of greater than 10(-6) on the day of closest approach. Thus, a single all-sky survey can be of tremendous value in identifying Earth-impacting and close-approaching asteroids in advance of their closest approach, but it can not solve the problem on its own: high-precision astrometry from other optical or radar systems is necessary to rapidly establish an object as an impactor or close approacher. We show that the parallax afforded by surveying the sky from two sites is only of benefit for a small fraction of the smallest objects detected within a couple days before impact: probably not enough to justify the increased operating costs of a two-site survey. Finally, the survey cadence within a fixed time span is relatively unimportant to the impact probability calculation. We tested three different reasonable cadences and found that one provided similar to 10 times higher (better) value for the impact probability on the discovery night for the smallest (10 m diameter) objects, but the consequences on the overall impact probability calculation are negligible. C1 [Veres, Peter; Jedicke, Robert] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Farnocchia, Davide] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. [Spoto, Federica] Univ Pisa, Dept Math, I-56127 Pisa, Italy. RP Veres, P (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM veres@ifa.hawaii.edu FU NASA; NASA NEOO [NNX12AR65G] FX We thank J. Tonry and L. Denneau of the ATLAS survey for assistance in characterizing and designing a representative ATLAS survey. D. Farnocchia was supported for this research by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. Peter Veres's Pan-STARRS MOPS Postdoctoral Fellowship was sponsored by NASA NEOO grant No. NNX12AR65G. NR 40 TC 0 Z9 0 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD MAY PY 2014 VL 126 IS 939 BP 433 EP 444 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI1VJ UT WOS:000336643000001 ER PT J AU Tse, LA Ganapathi, GB Wirz, RE Lavine, AS AF Tse, Louis A. Ganapathi, Gani B. Wirz, Richard E. Lavine, Adrienne S. TI Spatial and temporal modeling of sub- and supercritical thermal energy storage SO SOLAR ENERGY LA English DT Article DE Energy storage; Thermodynamic model; Transient behavior; Concentrating solar power ID PLANTS AB This paper describes a thermodynamic model that simulates the discharge cycle of a single-tank thermal energy storage (TES) system that can operate from the two-phase (liquid-vapor) to supercritical regimes for storage fluid temperatures typical of concentrating solar power plants. State-of-the-art TES design utilizes a two-tank system with molten nitrate salts; one major problem is the high capital cost of the salts (International Renewable Energy Agency, 2012). The alternate approach explored here opens up the use of low-cost fluids by considering operation at higher pressures associated with the two-phase and supercritical regimes. The main challenge to such a system is its high pressures and temperatures which necessitate a relatively high-cost containment vessel that represents a large fraction of the system capital cost. To mitigate this cost, the proposed design utilizes a single-tank TES system, effectively halving the required wall material. A single-tank approach also significantly reduces the complexity of the system in comparison to the two-tank systems, which require expensive pumps and external heat exchangers. A thermodynamic model is used to evaluate system performance; in particular it predicts the volume of tank wall material needed to encapsulate the storage fluid. The transient temperature of the tank is observed to remain hottest at the storage tank exit, which is beneficial to system operation. It is also shown that there is an optimum storage fluid loading that generates a given turbine energy output while minimizing the required tank wall material. Overall, this study explores opportunities to further improve current solar thermal technologies. The proposed single-tank system shows promise for decreasing the cost of thermal energy storage. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Tse, Louis A.; Wirz, Richard E.; Lavine, Adrienne S.] Univ Calif Los Angeles, Dept Mech & Aerosp Engn, Los Angeles, CA 90095 USA. [Ganapathi, Gani B.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Tse, LA (reprint author), Univ Calif Los Angeles, Dept Mech & Aerosp Engn, Los Angeles, CA 90095 USA. EM ltse1@ucla.edu FU ARPA-E [DE-AR0000140]; Southern California Gas Company [5660021607]; National Science Foundation [DGE-0707424] FX This effort was supported by ARPA-E Award DE-AR0000140, Grant No. 5660021607 from the Southern California Gas Company, and Grant No. DGE-0707424 from the National Science Foundation. NR 20 TC 5 Z9 5 U1 1 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-092X J9 SOL ENERGY JI Sol. Energy PD MAY PY 2014 VL 103 BP 402 EP 410 DI 10.1016/j.solener.2014.02.040 PG 9 WC Energy & Fuels SC Energy & Fuels GA AH7YR UT WOS:000336351800036 ER PT J AU Nguyen, H Katzfuss, M Cressie, N Braverman, A AF Hai Nguyen Katzfuss, Matthias Cressie, Noel Braverman, Amy TI Spatio-Temporal Data Fusion for Very Large Remote Sensing Datasets SO TECHNOMETRICS LA English DT Article DE EM algorithm; Fixed rank smoothing; Kalman filter; Multivariate geostatistics; Spatial random effects model ID HIERARCHICAL-MODELS; CARBON-DIOXIDE; DATA SETS; SCIENCE AB Developing global maps of carbon dioxide (CO2) mole fraction (in units of parts per million) near the Earth's surface can help identify locations where major amounts of CO2 are entering and exiting the atmosphere, thus providing valuable insights into the carbon cycle and mitigating the greenhouse effect of atmospheric CO2. Existing satellite remote sensing data do not provide measurements of the CO2 mole fraction near the surface. Japan's Greenhouse gases Observing SATellite (GOSAT) is sensitive to average CO2 over the entire column, and NASA's Atmospheric InfraRed Sounder (AIRS) is sensitive to CO2 in the middle troposphere. One might expect that lower-atmospheric CO2 could be inferred by differencing GOSAT column-average and AIRS mid-tropospheric data. However, the two instruments have different footprints, measurement-error characteristics, and data coverages. In addition, the spatio-temporal domains are large, and the AIRS dataset is massive. In this article, we describe a spatio-temporal data-fusion (STDF) methodology based on reduced-dimensional Kalman smoothing. Our STDF is able to combine the complementary GOSAT and AIRS datasets to optimally estimate lower-atmospheric CO2 mole fraction over the whole globe. Further, it is designed for massive remote sensing datasets and accounts for differences in instrument footprint, measurement-error characteristics, and data coverages. This article has supplementary material online. C1 [Hai Nguyen; Braverman, Amy] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Katzfuss, Matthias] Heidelberg Univ, Inst Angew Math, D-69117 Heidelberg, Germany. [Cressie, Noel] Univ Wollongong, Sch Math & Appl Stat, Wollongong, NSW 2522, Australia. RP Nguyen, H (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM hai.nguyen@jpl.nasa.gov; katzfuss@gmail.com; ncressie@uow.edu.au; amy.braverman@jpl.nasa.gov FU NASA's Earth Science Technology Office through its Advanced Information Systems Technology program; Mathematics Center Heidelberg; Naval Surface Warfare Center, Dahlgren Division FX The research described in this article was carried out in part by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. It is supported by NASA's Earth Science Technology Office through its Advanced Information Systems Technology program. Katzfuss' research was partially supported by the Mathematics Center Heidelberg. Cressie's research was partially supported by the Naval Surface Warfare Center, Dahlgren Division. NR 41 TC 3 Z9 3 U1 0 U2 19 PU AMER STATISTICAL ASSOC PI ALEXANDRIA PA 732 N WASHINGTON ST, ALEXANDRIA, VA 22314-1943 USA SN 0040-1706 EI 1537-2723 J9 TECHNOMETRICS JI Technometrics PD MAY PY 2014 VL 56 IS 2 BP 174 EP 185 DI 10.1080/00401706.2013.831774 PG 12 WC Statistics & Probability SC Mathematics GA AH2NG UT WOS:000335957600005 ER PT J AU Doarn, CR Pruitt, S Jacobs, J Harris, Y Bott, DM Riley, W Lamer, C Oliver, AL AF Doarn, Charles R. Pruitt, Sherilyn Jacobs, Jessica Harris, Yael Bott, David M. Riley, William Lamer, Christopher Oliver, Anthony L. TI Original Research Federal Efforts to Define and Advance Telehealth-A Work in Progress SO TELEMEDICINE AND E-HEALTH LA English DT Article DE telemedicine; telehealth; U; S; Government; healthcare reform ID ARMY TELEMEDICINE; MOBILE HEALTH; TECHNOLOGY; FUTURE; CARE; IMPLEMENTATION; PERSPECTIVES; MANAGEMENT; SUPPORT; HOME AB Background:The integration of telecommunications and information systems in healthcare is not new or novel; indeed, it is the current practice of medicine and has been an integral part of medicine in remote locations for several decades. The U.S. Government has made a significant investment, measured in hundreds of millions of dollars, and therefore has a strong presence in the integration of telehealth/telemedicine in healthcare. However, the terminologies and definitions in the lexicon vary across agencies and departments of the U.S. Government. The objective of our survey was to identify and evaluate the definitions of telehealth/telemedicine across the U.S. Government to provide a better understanding of what each agency or department means when it uses these terms.Methodology:The U.S. Government, under the leadership of the Health Resources and Services Administration in the U.S. Department of Health and Human Services, established the Federal Telemedicine (FedTel) Working Group, through which all members responded to a survey on each agency or department's definition and use of terms associated with telehealth.Results and Conclusions:Twenty-six agencies represented by more than 100 individuals participating in the FedTel Working Group identified seven unique definitions of telehealth in current use across the U.S. Government. Although many definitions are similar, there are nuanced differences that reflect each organization's legislative intent and the population they serve. These definitions affect how telemedicine has been or is being applied across the healthcare landscape, reflecting the U.S. Government's widespread and influential role in healthcare access and service delivery. The evidence base suggests that a common nomenclature for defining telemedicine may benefit efforts to advance the use of this technology to address the changing nature of healthcare and new demands for services expected as a result of health reform. C1 [Doarn, Charles R.] NASA Headquarters, Washington, DC USA. [Doarn, Charles R.] Univ Cincinnati, Coll Med, Dept Family & Community Med, Cincinnati, OH 45267 USA. [Pruitt, Sherilyn; Oliver, Anthony L.] US Dept HHS, Off Adv Telehlth, Rockville, MD USA. [Jacobs, Jessica] Aetna, Washington, DC USA. [Harris, Yael] US Dept HHS, Div Healthcare Qual, Off Dis Prevent & Hlth Promot, Rockville, MD USA. [Bott, David M.] US Dept HHS, Ctr Medicare & Medicaid Serv, Baltimore, MD USA. [Riley, William] NCI, Div Canc Control & Populat Sci, Bethesda, MD 20892 USA. [Lamer, Christopher] Indian Hlth Serv, Rockville, MD USA. RP Doarn, CR (reprint author), Univ Cincinnati, Coll Med, Dept Family & Community Med, Cincinnati, OH 45267 USA. EM charles.doarn@uc.edu NR 36 TC 9 Z9 9 U1 0 U2 5 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1530-5627 EI 1556-3669 J9 TELEMED E-HEALTH JI Telemed. e-Health PD MAY 1 PY 2014 VL 20 IS 5 BP 409 EP 418 DI 10.1089/tmj.2013.0336 PG 10 WC Health Care Sciences & Services SC Health Care Sciences & Services GA AG4MG UT WOS:000335393400004 PM 24502793 ER PT J AU Comiso, JC Hall, DK AF Comiso, Josefino C. Hall, Dorothy K. TI Climate trends in the Arctic as observed from space SO WILEY INTERDISCIPLINARY REVIEWS-CLIMATE CHANGE LA English DT Review ID GREENLAND ICE-SHEET; INTERACTIVE MULTISENSOR SNOW; SEA-SURFACE TEMPERATURE; NORTHERN-HEMISPHERE; AIR-TEMPERATURE; MASS-LOSS; SATELLITE-OBSERVATIONS; RADIATION PROPERTIES; MAPPING SYSTEM; LEVEL RISE AB The Arctic is a region in transformation. Warming in the region has been amplified, as expected from ice-albedo feedback effects, with the rate of warming observed to be approximate to 0.600.07 degrees C/decade in the Arctic (>64 degrees N) compared to approximate to 0.17 degrees C/decade globally during the last three decades. This increase in surface temperature is manifested in all components of the cryosphere. In particular, the sea ice extent has been declining at the rate of approximate to 3.8%/decade, whereas the perennial ice (represented by summer ice minimum) is declining at a much greater rate of approximate to 11.5%/decade. Spring snow cover has also been observed to be declining by -2.12%/decade for the period 1967-2012. The Greenland ice sheet has been losing mass at the rate of approximate to 34.0Gt/year (sea level equivalence of 0.09mm/year) during the period from 1992 to 2011, but for the period 2002-2011, a higher rate of mass loss of approximate to 215Gt/year has been observed. Also, the mass of glaciers worldwide declined at the rate of 226 Gt/year from 1971 to 2009 and 275 Gt/year from 1993 to 2009. Increases in permafrost temperature have also been measured in many parts of the Northern Hemisphere while a thickening of the active layer that overlies permafrost and a thinning of seasonally frozen ground has also been reported. To gain insight into these changes, comparative analysis with trends in clouds, albedo, and the Arctic Oscillation is also presented. For further resources related to this article, please visit the .

Conflict of interest: The authors have declared no conflicts of interest for this article. C1 [Comiso, Josefino C.; Hall, Dorothy K.] NASA, Goddard Space Flight Ctr, Code Earth Sci Div 615, Cryospher Sci Lab, Greenbelt, MD 20771 USA. RP Comiso, JC (reprint author), NASA, Goddard Space Flight Ctr, Code Earth Sci Div 615, Cryospher Sci Lab, Greenbelt, MD 20771 USA. EM josefino.c.comiso@nasa.gov NR 122 TC 47 Z9 50 U1 12 U2 75 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1757-7780 EI 1757-7799 J9 WIRES CLIM CHANGE JI Wiley Interdiscip. Rev.-Clim. Chang. PD MAY PY 2014 VL 5 IS 3 BP 389 EP 409 DI 10.1002/wcc.277 PG 21 WC Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AF3CQ UT WOS:000334589500007 ER PT J AU Arendt, RG Dwek, E Kober, G Rho, J Hwang, U AF Arendt, Richard G. Dwek, Eli Kober, Gladys Rho, Jeonghee Hwang, Una TI INTERSTELLAR AND EJECTA DUST IN THE CAS A SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust,extinction; infrared: ISM; ISM: individual objects: (Cassiopeia A); ISM: supernova remnants ID CASSIOPEIA-A SUPERNOVA; OPTICAL-PROPERTIES; SILICATE MINERALOGY; INFRARED-EMISSION; 3-DIMENSIONAL STRUCTURE; EARLY UNIVERSE; SPITZER; CARBON; ORIGIN; GRAINS AB Infrared continuum observations provide a means of investigating the physical composition of the dust in the ejecta and swept up medium of the Cas A supernova remnant (SNR). Using low-resolution Spitzer IRS spectra (5-35 mu m), and broad-band Herschel PACS imaging (70, 100, and 160 mu m), we identify characteristic dust spectra, associated with ejecta layers that underwent distinct nuclear burning histories. The most luminous spectrum exhibits strong emission features at similar to 9 and 21 mu m and is closely associated with ejecta knots with strong Ar emission lines. The dust features can be reproduced by magnesium silicate grains with relatively low Mg to Si ratios. Another dust spectrum is associated with ejecta having strong Ne emission lines. It has no indication of any silicate features and is best fit by Al2O3 dust. A third characteristic dust spectrum shows features that are best matched by magnesium silicates with a relatively high Mg to Si ratio. This dust is primarily associated with the X-ray-emitting shocked ejecta, but it is also evident in regions where shocked interstellar or circumstellar material is expected. However, the identification of dust composition is not unique, and each spectrum includes an additional featureless dust component of unknown composition. Colder dust of indeterminate composition is associated with emission from the interior of the SNR, where the reverse shock has not yet swept up and heated the ejecta. Most of the dust mass in Cas A is associated with this unidentified cold component, which is less than or similar to 0.1M(circle dot). The mass of warmer dust is only similar to 0.04M(circle dot). C1 [Arendt, Richard G.] Univ Maryland, CRESST, Baltimore, MD 21250 USA. [Arendt, Richard G.; Dwek, Eli; Kober, Gladys; Hwang, Una] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kober, Gladys] Catholic Univ Amer, Dept Phys, IACS, Washington, DC 20064 USA. [Rho, Jeonghee] SETI Inst, Mountain View, CA 94043 USA. [Rho, Jeonghee] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Hwang, Una] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. RP Arendt, RG (reprint author), Univ Maryland, CRESST, Baltimore, MD 21250 USA. EM Richard.G.Arendt@nasa.gov OI Arendt, Richard/0000-0001-8403-8548 FU NASA [NNH09ZDA001N-ADP-0032] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA Program NNH09ZDA001N-ADP-0032. This research made use of Tiny Tim/Spitzer, developed by John Krist for the Spitzer Science Center. The Center is managed by the California Institute of Technology under a contract with NASA. This research has made use of NASA ' s Astrophysics Data System Bibliographic Services. We thank T. Kozasa for providing digitized (and extrapolated and interpolated) versions of the optical constants for several dust species as noted in Table 3. We also thank the referee for constructive comments on the manuscript. NR 71 TC 17 Z9 17 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 55 DI 10.1088/0004-637X/786/1/55 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700055 ER PT J AU Barriere, NM Tomsick, JA Baganoff, FK Boggs, SE Christensen, FE Craig, WW Dexter, J Grefenstette, B Hailey, CJ Harrison, FA Madsen, KK Mori, K Stern, D Zhang, WW Zhang, S Zoglauer, A AF Barriere, Nicolas M. Tomsick, John A. Baganoff, Frederick K. Boggs, Steven E. Christensen, Finn E. Craig, William W. Dexter, Jason Grefenstette, Brian Hailey, Charles J. Harrison, Fiona A. Madsen, Kristin K. Mori, Kaya Stern, Daniel Zhang, William W. Zhang, Shuo Zoglauer, Andreas TI NuSTAR DETECTION OF HIGH-ENERGY X-RAY EMISSION AND RAPID VARIABILITY FROM SAGITTARIUS A(star) FLARES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; Galaxy: center; stars: black holes; stars: flare; stars: individual (Sgr A*); X-rays: general ID SGR-A-ASTERISK; SUPERMASSIVE BLACK-HOLE; NEAR-INFRARED FLARES; EXTRAGALACTIC RADIO-SOURCES; GALACTIC-CENTER; FLARING ACTIVITY; XMM-NEWTON; BRIGHTEST FLARE; ACCRETION FLOW; STELLAR ORBITS AB Sagittarius A(star) harbors the supermassive black hole that lies at the dynamical center of our Galaxy. Sagittarius A(star) spends most of its time in a low luminosity emission state but flares frequently in the infrared and X-ray, increasing up to a few hundred fold in brightness for up to a few hours at a time. The physical processes giving rise to the X-ray flares are uncertain. Here we report the detection with the NuSTAR observatory in Summer and Fall 2012 of four low to medium amplitude X-ray flares to energies up to 79 keV. For the first time, we clearly see that the power-law spectrum of Sagittarius A(star) X-ray flares extends to high energy, with no evidence for a cutoff. Although the photon index of the absorbed power-law fits are in agreement with past observations, we find a difference between the photon index of two of the flares (significant at the 95% confidence level). The spectra of the two brightest flares (similar to 55 times quiescence in the 2-10 keV band) are compared to simple physical models in an attempt to identify the main X-ray emission mechanism, but the data do not allow us to significantly discriminate between them. However, we confirm the previous finding that the parameters obtained with synchrotron models are, for the X-ray emission, physically more reasonable than those obtained with inverse Compton models. One flare exhibits large and rapid (< 100 s) variability, which, considering the total energy radiated, constrains the location of the flaring region to be within similar to 10 Schwarzschild radii of the black hole. C1 [Barriere, Nicolas M.; Tomsick, John A.; Boggs, Steven E.; Craig, William W.; Zoglauer, Andreas] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Baganoff, Frederick K.] 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. [Dexter, Jason] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Dexter, Jason] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Grefenstette, Brian; Harrison, Fiona A.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Hailey, Charles J.; Mori, Kaya; Zhang, Shuo] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. RP Barriere, NM (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RI Boggs, Steven/E-4170-2015 OI Boggs, Steven/0000-0001-9567-4224 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration FX This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The authors thank S. Nayakshin, S. Markoff, A. Eckart, G. Trap, M. Wardle, and F. Yusef-Zadeh for useful discussions. We also thank the Chandra Sgr Astar XVP collaboration for information on absence of X-ray transients before and after the flares reported here. NR 55 TC 27 Z9 27 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 MAY 1 PY 2014 VL 786 IS 1 AR 46 DI 10.1088/0004-637X/786/1/46 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700046 ER PT J AU Brandt, TD Kuzuhara, M McElwain, MW Schlieder, JE Wisniewski, JP Turner, EL Carson, J Matsuo, T Biller, B Bonnefoy, M Dressing, C Janson, M Knapp, GR Moro-Martin, A Thalmann, C Kudo, T Kusakabe, N Hashimoto, J Abe, L Brandner, W Currie, T Egner, S Feldt, M Golota, T Goto, M Grady, CA Guyon, O Hayano, Y Hayashi, M Hayashi, S Henning, T Hodapp, KW Ishii, M Iye, M Kandori, R Kwon, J Mede, K Miyama, S Morino, JI Nishimura, T Pyo, TS Serabyn, E Suenaga, T Suto, H Suzuki, R Takami, M Takahashi, Y Takato, N Terada, H Tomono, D Watanabe, M Yamada, T Takami, H Usuda, T Tamura, M AF Brandt, Timothy D. Kuzuhara, Masayuki McElwain, Michael W. Schlieder, Joshua E. Wisniewski, John P. Turner, Edwin L. Carson, J. Matsuo, T. Biller, B. Bonnefoy, M. Dressing, C. Janson, M. Knapp, G. R. Moro-Martin, A. Thalmann, C. Kudo, T. Kusakabe, N. Hashimoto, J. Abe, L. Brandner, W. Currie, T. Egner, S. Feldt, M. Golota, T. Goto, M. Grady, C. A. Guyon, O. Hayano, Y. Hayashi, M. Hayashi, S. Henning, T. Hodapp, K. W. Ishii, M. Iye, M. Kandori, R. Kwon, J. Mede, K. Miyama, S. Morino, J. -I. Nishimura, T. Pyo, T. -S. Serabyn, E. Suenaga, T. Suto, H. Suzuki, R. Takami, M. Takahashi, Y. Takato, N. Terada, H. Tomono, D. Watanabe, M. Yamada, T. Takami, H. Usuda, T. Tamura, M. TI THE MOVING GROUP TARGETS OF THE SEEDS HIGH-CONTRAST IMAGING SURVEY OF EXOPLANETS AND DISKS: RESULTS AND OBSERVATIONS FROM THE FIRST THREE YEARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; brown dwarfs; open clusters and associations: general; stars: activity; stars: imaging; stars: low-mass; stars: planetary systems ID TW-HYDRAE ASSOCIATION; LATE-TYPE STARS; LOW-MASS STARS; MAIN-SEQUENCE STARS; STELLAR KINEMATIC GROUPS; YOUNG SOLAR ANALOGS; ALL-SKY SURVEY; EXTRASOLAR GIANT PLANETS; GENEVA-COPENHAGEN SURVEY; ADAPTIVE OPTICS SURVEY AB We present results from the first three years of observations of moving group (MG) targets in the Strategic Exploration of Exoplanets and Disks with Subaru (SEEDS) high-contrast imaging survey of exoplanets and disks using the Subaru telescope. We achieve typical contrasts of similar to 10(5) at 1 '' and similar to 10(6) beyond 2 '' around 63 proposed members of nearby kinematic MGs. We review each of the kinematic associations to which our targets belong, concluding that five, beta Pictoris (similar to 20 Myr), AB Doradus (similar to 100 Myr), Columba (similar to 30 Myr), Tucana-Horogium (similar to 30 Myr), and TW Hydrae (similar to 10 Myr), are sufficiently well-defined to constrain the ages of individual targets. Somewhat less than half of our targets are high-probability members of one of these MGs. For all of our targets, we combine proposed MG membership with other age indicators where available, including Ca II HK emission, X-ray activity, and rotation period, to produce a posterior probability distribution of age. SEEDS observations discovered a substellar companion to one of our targets,. And, a late B star. We do not detect any other substellar companions, but do find seven new close binary systems, of which one still needs to be confirmed. A detailed analysis of the statistics of this sample, and of the companion mass constraints given our age probability distributions and exoplanet cooling models, will be presented in a forthcoming paper. C1 [Brandt, Timothy D.; Turner, Edwin L.; Janson, M.; Knapp, G. R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Kuzuhara, Masayuki] Tokyo Inst Technol, Tokyo 152, Japan. [McElwain, Michael W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Schlieder, Joshua E.; Carson, J.; Biller, B.; Bonnefoy, M.; Brandner, W.; Feldt, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Matsuo, T.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Univ WPI, Tokyo 1138654, Japan. [Carson, J.] Coll Charleston, Charleston, SC 29401 USA. [Matsuo, T.] Kyoto Univ, Dept Astron, Kyoto, Japan. [Dressing, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Moro-Martin, A.] CAB CSIC INTA, Dept Astrophys, Madrid, Spain. [Thalmann, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Kudo, T.; Egner, S.; Golota, T.; Guyon, O.; Hayano, Y.; Hayashi, S.; Ishii, M.; Nishimura, T.; Pyo, T. -S.; Takato, N.; Terada, H.; Tomono, D.; Takami, H.; Usuda, T.] Subaru Telescope, Hilo, HI USA. [Kusakabe, N.; Hashimoto, J.; Iye, M.; Kandori, R.; Kwon, J.; Morino, J. -I.; Suto, H.; Suzuki, R.; Tamura, M.] Natl Astron Observ Japan, Tokyo, Japan. [Abe, L.] Lab Hippolyte Fizeau, Nice, France. [Currie, T.] Univ Toronto, Toronto, ON, Canada. [Goto, M.] Univ Sternwarte, Munich, Germany. [Grady, C. A.] Eureka Sci, Oakland, CA USA. [Hayashi, M.; Takahashi, Y.; Tamura, M.] Univ Tokyo, Tokyo, Japan. [Hodapp, K. W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Kwon, J.; Suenaga, T.] Grad Univ Adv Studies, Dept Astron Sci, Tokyo, Japan. [Miyama, S.] Hiroshima Univ, Higashihiroshima 724, Japan. [Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido, Japan. [Yamada, T.] Tohoku Univ, Astron Inst, Sendai, Miyagi 980, Japan. RP Brandt, TD (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016 OI Watanabe, Makoto/0000-0002-3656-4081 NR 237 TC 27 Z9 27 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 1 DI 10.1088/0004-637X/786/1/1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700001 ER PT J AU Broekhoven-Fiene, H Matthews, BC Harvey, PM Gutermuth, RA Huard, TL Tothill, NFH Nutter, D Bourke, TL DiFrancesco, J Jorgensen, JK Allen, LE Chapman, NL Dunham, MM Merin, B Miller, JF Terebey, S Peterson, DE Stapelfeldt, KR AF Broekhoven-Fiene, Hannah Matthews, Brenda C. Harvey, Paul M. Gutermuth, Robert A. Huard, Tracy L. Tothill, Nicholas F. H. Nutter, David Bourke, Tyler L. DiFrancesco, James Jorgensen, Jes K. Allen, Lori E. Chapman, Nicholas L. Dunham, Michael M. Merin, Bruno Miller, Jennifer F. Terebey, Susan Peterson, Dawn E. Stapelfeldt, Karl R. TI THE Spitzer SURVEY OF INTERSTELLAR CLOUDS IN THE GOULD BELT. VI. THE AURIGA-CALIFORNIA MOLECULAR CLOUD OBSERVED WITH IRAC AND MIPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: general; ISM: clouds; stars: formation ID YOUNG STELLAR OBJECTS; ARRAY CAMERA IRAC; T-TAURI STARS; C2D SURVEY; SPACE-TELESCOPE; NEARBY; PERSEUS; POPULATION; DISTRIBUTIONS; LUMINOSITIES AB We present observations of the Auriga-California Molecular Cloud (AMC) at 3.6, 4.5, 5.8, 8.0, 24, 70, and 160 mu m observed with the IRAC and MIPS detectors as part of the Spitzer Gould Belt Legacy Survey. The total mapped areas are 2.5 deg(2) with IRAC and 10.47 deg(2) with MIPS. This giant molecular cloud is one of two in the nearby Gould Belt of star-forming regions, the other being the Orion A Molecular Cloud (OMC). We compare source counts, colors, and magnitudes in our observed region to a subset of the SWIRE data that was processed through our pipeline. Using color-magnitude and color-color diagrams, we find evidence for a substantial population of 166 young stellar objects (YSOs) in the cloud, many of which were previously unknown. Most of this population is concentrated around the LkH alpha 101 cluster and the filament extending from it. We present a quantitative description of the degree of clustering and discuss the relative fraction of YSOs in earlier (Class I and F) and later (Class II) classes compared to other clouds. We perform simple SED modeling of the YSOs with disks to compare the mid-IR properties to disks in other clouds and identify 14 classical transition disk candidates. Although the AMC is similar in mass, size, and distance to the OMC, it is forming about 15-20 times fewer stars. C1 [Broekhoven-Fiene, Hannah; Matthews, Brenda C.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Matthews, Brenda C.; DiFrancesco, James] Natl Res Council Herzberg Astron Astrophys, Victoria, BC V9E 2E7, Canada. [Harvey, Paul M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Gutermuth, Robert A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Huard, Tracy L.; Miller, Jennifer F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Huard, Tracy L.] Univ Western Sydney, Sch Comp Engn & Math, Penrith, NSW 2751, Australia. [Tothill, Nicholas F. H.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Nutter, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bourke, Tyler L.; Miller, Jennifer F.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Jorgensen, Jes K.] Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Jorgensen, Jes K.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Allen, Lori E.] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Chapman, Nicholas L.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Chapman, Nicholas L.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Dunham, Michael M.] ESAC ESA, Herschel Sci Ctr, E-28691 Madrid, Spain. [Merin, Bruno] Space Sci Inst, Boulder, CO 80301 USA. [Terebey, Susan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Broekhoven-Fiene, H (reprint author), Univ Victoria, Dept Phys & Astron, POB 3055, Victoria, BC V8W 3P6, Canada. RI Tothill, Nicholas/M-6379-2016 OI Tothill, Nicholas/0000-0002-9931-5162 FU NSERC Discovery Grant; NASA - California Institute of Technology [NCC5-626] FX We thank the referee whose comments and suggestions greatly helped improve the paper and its clarity. H.B.F. gratefully acknowledges research support from an NSERC Discovery Grant. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy. github. com. This research also made use of Montage, funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology. Montage is maintained by the NASA/IPAC Infrared Science Archive. NR 39 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 37 DI 10.1088/0004-637X/786/1/37 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700037 ER PT J AU Del Moro, A Mullaney, JR Alexander, DM Comastri, A Bauer, FE Treister, E Stern, D Civano, F Ranalli, P Vignali, C Aird, JA Ballantyne, DR Balokovic, M Boggs, SE Brandt, WN Christensen, FE Craig, WW Gandhi, P Gilli, R Hailey, CJ Harrison, FA Hickox, RC LaMassa, SM Lansbury, GB Luo, B Puccetti, S Urry, M Zhang, WW AF Del Moro, A. Mullaney, J. R. Alexander, D. M. Comastri, A. Bauer, F. E. Treister, E. Stern, D. Civano, F. Ranalli, P. Vignali, C. Aird, J. A. Ballantyne, D. R. Balokovic, M. Boggs, S. E. Brandt, W. N. Christensen, F. E. Craig, W. W. Gandhi, P. Gilli, R. Hailey, C. J. Harrison, F. A. Hickox, R. C. LaMassa, S. M. Lansbury, G. B. Luo, B. Puccetti, S. Urry, M. Zhang, W. W. TI NuSTAR J033202-2746.8: DIRECT CONSTRAINTS ON THE COMPTON REFLECTION IN A HEAVILY OBSCURED QUASAR AT z approximate to 2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; infrared: galaxies; quasars: general; quasars: individual (NuSTAR J033202-2746.8); X-rays: galaxies ID DEEP FIELD-SOUTH; ACTIVE GALACTIC NUCLEI; RAY SPECTRAL PROPERTIES; HARD X-RAYS; XMM-NEWTON OBSERVATIONS; STAR-FORMING GALAXIES; POINT-SOURCE CATALOGS; LINE RADIO GALAXIES; MS SOURCE CATALOGS; SWIFT-BAT SURVEY AB We report Nuclear Spectroscopic Telescope Array (NuSTAR) observations of NuSTAR J033202-2746.8, a heavily obscured, radio-loud quasar detected in the Extended Chandra Deep Field-South, the deepest layer of the NuSTAR extragalactic survey (similar to 400 ks, at its deepest). NuSTAR J033202-2746.8 is reliably detected by NuSTAR only at E > 8 keV and has a very flat spectral slope in the NuSTAR energy band (Gamma = 0.55(-0.64)(+0.62); 3-30 keV). Combining the NuSTAR data with extremely deep observations by Chandra and XMM-Newton (4 Ms and 3 Ms, respectively), we constrain the broad-band X-ray spectrum of NuSTAR J033202-2746.8, indicating that this source is a heavily obscured quasar (N-H = 5.6(-0.8)(+0.9) x 10(23) cm(-2)) with luminosity L10-40 keV approximate to 6.4 x 10(44) erg s(-1). Although existing optical and near-infrared (near-IR) data, as well as follow-up spectroscopy with the Keck and VLT telescopes, failed to provide a secure redshift identification for NuSTAR J033202-2746.8, we reliably constrain the redshift z = 2.00 +/- 0.04 from the X-ray spectral features (primarily from the iron K edge). The NuSTAR spectrum shows a significant reflection component (R = 0.55(-0.37)(+0.44)), which was not constrained by previous analyses of Chandra and XMM-Newton data alone. The measured reflection fraction is higher than the R similar to 0 typically observed in bright radio-loud quasars such as NuSTAR J033202-2746.8, which has L-1.4 GHz approximate to 10(27) W Hz(-1). Constraining the spectral shape of active galactic nuclei (AGNs), including bright quasars, is very important for understanding the AGN population, and can have a strong impact on the modeling of the X-ray background. Our results show the importance of NuSTAR in investigating the broad-band spectral properties of quasars out to high redshift. C1 [Del Moro, A.; Mullaney, J. R.; Alexander, D. M.; Aird, J. A.; Gandhi, P.; Lansbury, G. B.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Mullaney, J. R.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Comastri, A.; Vignali, C.; Gilli, R.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Civano, F.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ranalli, P.] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, Inst Astron, Penteli 15236, Greece. [Vignali, C.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Balokovic, M.; Harrison, F. A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 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. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [LaMassa, S. M.; Urry, M.] Yale Univ, Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA. [Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Puccetti, S.] INAF Osservatorio Astronomico Roma, I-00040 Monte Porzio Catone, Italy. [Zhang, W. W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Del Moro, A (reprint author), Univ Durham, Dept Phys, S Rd, Durham DH1 3LE, England. EM agnese.del-moro@durham.ac.uk RI Ranalli, Piero/K-6363-2013; Vignali, Cristian/J-4974-2012; Boggs, Steven/E-4170-2015; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Ranalli, Piero/0000-0003-3956-755X; Vignali, Cristian/0000-0002-8853-9611; Boggs, Steven/0000-0001-9567-4224; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Alexander, David/0000-0002-5896-6313 FU UK Science and Technology Facilities Council (STFC) [ST/I001573/I, ST/K501979/1, ST/J003697/1]; Leverhulme Trust; ASI/INAF [I/037/12/0-011/13]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024]; Anillo [ACT1101]; FONDECYT [1120061]; Caltech NuSTAR [44A-1092750]; NASA ADP [NNX10AC99G]; NASA [NNG08FD60C]; National Aeronautics and Space Administration; ESO Telescopes at the La Silla Paranal Observatory under the program [ID 092.A-0452] FX We thank the anonymous referee for careful reading and for the helpful comments, which helped improving this manuscript. We gratefully acknowledge financial support from the UK Science and Technology Facilities Council (STFC, ST/I001573/I, ADM and DMA; ST/K501979/1, GBL; ST/J003697/1, PG) and the Leverhulme Trust (D.M.A. and J.R.M.). A.C., C.V., R.G., and P.R. thank the ASI/INAF grant I/037/12/0-011/13. F.E.B. acknowledges support from Basal-CATA (PFB-06/2007) and CONICYT-Chile (FONDECYT 1101024 and Anillo grant ACT1101) and E.T. acknowledges the FONDECYT grant 1120061. W.N.B. and B.L. thank Caltech NuSTAR subcontract 44A-1092750 and NASA ADP grant NNX10AC99G. M.B. acknowledges the International Fulbright Science and Technology Award. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work also used observations made with ESO Telescopes at the La Silla Paranal Observatory under the program ID 092.A-0452. NR 111 TC 19 Z9 19 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 16 DI 10.1088/0004-637X/786/1/16 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700016 ER PT J AU Grillo, C Gobat, R Presotto, V Balestra, I Mercurio, A Rosati, P Nonino, M Vanzella, E Christensen, L Graves, G Biviano, A Lemze, D Bartelmann, M Benitez, N Bouwens, R Bradley, L Broadhurst, T Coe, D Donahue, M Ford, H Infante, L Jouvel, S Kelson, D Koekemoer, A Lahav, O Medezinski, E Melchior, P Meneghetti, M Merten, J Molino, A Monna, A Moustakas, J Moustakas, LA Postman, M Seitz, S Umetsu, K Zheng, W Zitrin, A AF Grillo, C. Gobat, R. Presotto, V. Balestra, I. Mercurio, A. Rosati, P. Nonino, M. Vanzella, E. Christensen, L. Graves, G. Biviano, A. Lemze, D. Bartelmann, M. Benitez, N. Bouwens, R. Bradley, L. Broadhurst, T. Coe, D. Donahue, M. Ford, H. Infante, L. Jouvel, S. Kelson, D. Koekemoer, A. Lahav, O. Medezinski, E. Melchior, P. Meneghetti, M. Merten, J. Molino, A. Monna, A. Moustakas, J. Moustakas, L. A. Postman, M. Seitz, S. Umetsu, K. Zheng, W. Zitrin, A. TI CLASH: EXTENDING GALAXY STRONG LENSING TO SMALL PHYSICAL SCALES WITH DISTANT SOURCES HIGHLY MAGNIFIED BY GALAXY CLUSTER MEMBERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: clusters: individual (MACS J1206.2-0847); galaxies: high-redshift; galaxies: stellar content; galaxies: structure; gravitational lensing: strong ID INITIAL MASS FUNCTION; SPECTROSCOPICALLY SELECTED SAMPLE; DARK-MATTER HALOS; ACS SURVEY; GRAVITATIONAL LENSES; ADVANCED CAMERA; 2-DIMENSIONAL KINEMATICS; INTERNAL STRUCTURE; MACS J1206.2-0847; RXC J2248.7-4431 AB We present a complex strong lensing system in which a double source is imaged five times by two early-type galaxies. We take advantage in this target of the extraordinary multi-band photometric data set obtained as part of the Cluster Lensing And Supernova survey with Hubble (CLASH) program, complemented by the spectroscopic measurements of the VLT/VIMOS and FORS2 follow-up campaign. We use a photometric redshift value of 3.7 for the source and confirm spectroscopically the membership of the two lenses to the galaxy cluster MACS J1206.2-0847 at redshift 0.44. We exploit the excellent angular resolution of the HST/ACS images to model the two lenses in terms of singular isothermal sphere profiles and derive robust effective velocity dispersion values of 97 +/- 3 and 240 +/- 6 km s(-1). Interestingly, the total mass distribution of the cluster is also well characterized by using only the local information contained in this lensing system, which is located at a projected distance of more than 300 kpc from the cluster luminosity center. According to our best-fitting lensing and composite stellar population models, the source is magnified by a total factor of 50 and has a luminous mass of approximately (1.0 +/- 0.5) x10(9) M circle dot (assuming a Salpeter stellar initial mass function). By combining the total and luminous mass estimates of the two lenses, we measure luminous over total mass fractions projected within the effective radii of 0.51 +/- 0.21 and 0.80 +/- 0.32. Remarkably, with these lenses we can extend the analysis of the mass properties of lens early-type galaxies by factors that are approximately two and three times smaller than previously done with regard to, respectively, velocity dispersion and luminous mass. The comparison of the total and luminous quantities of our lenses with those of astrophysical objects with different physical scales, like massive early-type galaxies and dwarf spheroidals, reveals the potential of studies of this kind for improving our knowledge about the internal structure of galaxies. These studies, made possible thanks to the CLASH survey, will allow us to go beyond the current limits posed by the available lens samples in the field. C1 [Grillo, C.; Christensen, L.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Gobat, R.] Univ Paris Diderot, CEA Saclay, CEA DSM CNRS, Irfu Serv Astrophys,Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Presotto, V.] Univ Trieste, Dipartimento Fis, I-34143 Trieste, Italy. [Balestra, I.; Nonino, M.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Balestra, I.; Mercurio, A.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Rosati, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [Vanzella, E.; Meneghetti, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Graves, G.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Lemze, D.; Medezinski, E.; Zheng, W.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Bartelmann, M.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Benitez, N.; Molino, A.] CSIC, Inst Astrofis Andalucia, Granada 18008, Spain. [Bouwens, R.] Leiden Univ, Leiden Observ, NL-2333 Leiden, Netherlands. [Bradley, L.; Coe, D.; Koekemoer, A.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21208 USA. [Broadhurst, T.] Univ Basque Country, Dept Theoret Phys, E-48080 Bilbao, Spain. [Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Infante, L.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Jouvel, S.] CSIC, IEE, Inst Cincies Espai, Bellaterra 08193, Barcelona, Spain. [Jouvel, S.; Lahav, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Kelson, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Melchior, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Merten, J.; Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Monna, A.; Seitz, S.] Univ Sternwarte, Inst Astron & Astrophys, D-81679 Munich, Germany. [Moustakas, J.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Zitrin, A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RP Grillo, C (reprint author), Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. EM grillo@dark-cosmology.dk RI Christensen, Lise/M-5301-2014; Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015; OI Koekemoer, Anton/0000-0002-6610-2048; Benitez, Narciso/0000-0002-0403-7455; Christensen, Lise/0000-0001-8415-7547; Grillo, Claudio/0000-0002-5926-7143; Meneghetti, Massimo/0000-0003-1225-7084; Nonino, Mario/0000-0001-6342-9662; Moustakas, Leonidas/0000-0003-3030-2360; Balestra, Italo/0000-0001-9660-894X; Vanzella, Eros/0000-0002-5057-135X; Umetsu, Keiichi/0000-0002-7196-4822; Biviano, Andrea/0000-0002-0857-0732 FU Association of Universities for Research in Astronomy, Inc., under NASA [NAS 5-26555]; NASA [NAS 5-32864, HST-GO-12065.01-A]; DNRF; DFG Cluster of Excellence Origin Structure of the Universe; PRIN INAF; Cofinanziamento di Ateneo; NASA through Hubble Fellowship [HST-HF-51334.01-A]; STScI; "Internationale Spitzenforschung II/2-6" of the Baden Wurttemberg Stiftung FX The CLASH Multi-Cycle Treasury Program is based on observations made with the NASA/ESA Hubble Space Telescope. The Space Telescope Science Institute is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. ACS was developed under NASA Contract NAS 5-32864. This research is supported in part by NASA grant HST-GO-12065.01-A. We thank ESO for the continuous support of the Large Programme 186.A-0798. The Dark Cosmology Centre is funded by the DNRF. We acknowledge partial support by the DFG Cluster of Excellence Origin Structure of the Universe. V.P. acknowledges the grant PRIN INAF 2010 and "Cofinanziamento di Ateneo 2010." The work of L.A.M. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for A.Z. is provided by NASA through Hubble Fellowship grant HST-HF-51334.01-A awarded by STScI. Part of this work was also supported by contract research "Internationale Spitzenforschung II/2-6" of the Baden Wurttemberg Stiftung. NR 94 TC 5 Z9 5 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 11 DI 10.1088/0004-637X/786/1/11 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700011 ER PT J AU Hagen, A Ciardullo, R Gronwall, C Acquaviva, V Bridge, J Zeimann, GR Blanc, GA Bond, NA Finkelstein, SL Song, M Gawiser, E Fox, DB Gebhardt, H Malz, AI Schneider, DP Drory, N Gebhardt, K Hill, GJ AF Hagen, Alex Ciardullo, Robin Gronwall, Caryl Acquaviva, Viviana Bridge, Joanna Zeimann, Gregory R. Blanc, Guillermo A. Bond, Nicholas A. Finkelstein, Steven L. Song, Mimi Gawiser, Eric Fox, Derek B. Gebhardt, Henry Malz, A. I. Schneider, Donald P. Drory, Niv Gebhardt, Karl Hill, Gary J. TI SPECTRAL ENERGY DISTRIBUTION FITTING OF HETDEX PILOT SURVEY Ly alpha EMITTERS IN COSMOS AND GOODS-N SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: high-redshift; galaxies: starburst ID LYMAN BREAK GALAXIES; STAR-FORMATION HISTORIES; EMISSION-LINE GALAXIES; HIGH-REDSHIFT GALAXIES; EXTRAGALACTIC LEGACY SURVEY; INITIAL MASS FUNCTION; EMITTING GALAXIES; STELLAR MASS; MORPHOLOGICAL PROPERTIES; SUBMILLIMETER GALAXIES AB We use broadband photometry extending from the rest-frame UV to the near-IR to fit the individual spectral energy distributions of 63 bright (L(Ly alpha) > 10(43) erg s(-1)) Ly alpha emitting galaxies (LAEs) in the redshift range 1.9 < z < 3.6. We find that these LAEs are quite heterogeneous, with stellar masses that span over three orders of magnitude, from 7.5 < log M/M-circle dot < 10.5. Moreover, although most LAEs have small amounts of extinction, some high-mass objects have stellar reddenings as large as E(B - V) similar to 0.4. Interestingly, in dusty objects the optical depths for Ly alpha and the UV continuum are always similar, indicating that Ly alpha photons are not undergoing many scatters before escaping their galaxy. In contrast, the ratio of optical depths in low-reddening systems can vary widely, illustrating the diverse nature of the systems. Finally, we show that in the star-formation-rate-log-mass diagram, our LAEs fall above the "main-sequence" defined by z similar to 3 continuum selected star-forming galaxies. In this respect, they are similar to submillimeter-selected galaxies, although most LAEs have much lower mass. C1 [Hagen, Alex; Ciardullo, Robin; Gronwall, Caryl; Bridge, Joanna; Zeimann, Gregory R.; Fox, Derek B.; Gebhardt, Henry; Malz, A. I.; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Acquaviva, Viviana] CUNY, New York City Coll Technol, Dept Phys, Brooklyn, NY 11201 USA. [Blanc, Guillermo A.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Bond, Nicholas A.] NASA, Goddard Space Flight Ctr, Cosmol Lab, Greenbelt, MD 20771 USA. [Finkelstein, Steven L.; Song, Mimi; Drory, Niv; Gebhardt, Karl; Hill, Gary J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Hagen, Alex; Ciardullo, Robin; Gronwall, Caryl; Bridge, Joanna; Zeimann, Gregory R.; Fox, Derek B.; Gebhardt, Henry; Malz, A. I.; Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. RP Hagen, A (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM hagen@psu.edu; rbc@astro.psu.edu; caryl@astro.psu.edu; vacquaviva@citytech.cuny.edu; jsbridge@psu.edu; grzeimann@psu.edu; gblancm@obs.carnegiescience.edu; nicholas.bond@nasa.gov; stevenf@astro.as.utexas.edu; mmsong@astro.as.utexas.edu; drory@astro.as.utexas.edu; dfox@astro.psu.edu; gebhardt@psu.edu; malz@psu.edu; dps@astro.psu.edu; drory@astro.as.utexas.edu; gebhardt@astro.as.utexas.edu; hill@astro.as.utexas.edu RI Blanc, Guillermo/I-5260-2016; OI Hagen, Alex/0000-0003-2031-7737 FU NASA [NAS5-26555]; NSF [AST 09-26641, AST 10-55919]; Eberly College of Science; Office of the Senior Vice President for Research at the Pennsylvania State University FX We thank the referee for helpful comments. We also thank Joshua Adams for the use of his photometry from the HET-DEX Pilot Survey. We acknowledge the Research Computer and Cyberinfrastructure Unit of Information Technology Services, and in particular W. Brouwer at The Pennsylvania State University for providing computational support and resources for this project. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. The work was also partially supported by NSF grants AST 09-26641 and AST 10-55919. The Institute for Gravitation and the Cosmos is supported by the Eberly College of Science and the Office of the Senior Vice President for Research at the Pennsylvania State University. NR 87 TC 22 Z9 22 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 59 DI 10.1088/0004-637X/786/1/59 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700059 ER PT J AU Hoard, DW Long, KS Howell, SB Wachter, S Brinkworth, CS Knigge, C Drew, JE Szkody, P Kafka, S Belle, K Ciardi, DR Froning, CS van Belle, GT Pretorius, ML AF Hoard, D. W. Long, Knox S. Howell, Steve B. Wachter, Stefanie Brinkworth, Carolyn S. Knigge, Christian Drew, J. E. Szkody, Paula Kafka, S. Belle, Kunegunda Ciardi, David R. Froning, Cynthia S. van Belle, Gerard T. Pretorius, M. L. TI NOVA-LIKE CATACLYSMIC VARIABLES IN THE INFRARED SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; circumstellar matter; infrared: stars; novae, cataclysmic variables; stars: individual (TT Ari, WX Ari, QU Car, V592 Cas, V442 Oph, V347 Pup, V3885 Sgr, VY Scl, RW Sex, RW Tri, UX UMa, IX Vel) ID UX URSAE MAJORIS; SW SEXTANTIS STAR; SPITZER-SPACE-TELESCOPE; CIRCUMBINARY ENVELOPE FORMATION; AQUARII PLANETARY SYSTEM; VY SCL STARS; ACCRETION DISK; TT-ARIETIS; WHITE-DWARF; X-RAY AB Nova-like (NL) cataclysmic variables have persistently high mass transfer rates and prominent steady state accretion disks. We present an analysis of infrared observations of 12 NLs obtained from the Two Micron All Sky Survey, the Spitzer Space Telescope, and the Wide-field Infrared Survey Explorer All Sky Survey. The presence of an infrared excess at lambda greater than or similar to 3-5 mu m over the expectation of a theoretical steady state accretion disk is ubiquitous in our sample. The strength of the infrared excess is not correlated with orbital period, but shows a statistically significant correlation (but shallow trend) with system inclination that might be partially (but not completely) linked to the increasing view of the cooler outer accretion disk and disk rim at higher inclinations. We discuss the possible origin of the infrared excess in terms of emission from bremsstrahlung or circumbinary dust, with either mechanism facilitated by the mass outflows (e.g., disk wind/corona, accretion stream overflow, and so on) present in NLs. Our comparison of the relative advantages and disadvantages of either mechanism for explaining the observations suggests that the situation is rather ambiguous, largely circumstantial, and in need of stricter observational constraints. C1 [Hoard, D. W.] Eureka Sci Inc, Oakland, CA 94602 USA. [Hoard, D. W.; Wachter, Stefanie] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Brinkworth, Carolyn S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Brinkworth, Carolyn S.; Ciardi, David R.] CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Knigge, Christian] Univ Southampton, Southampton, Hants, England. [Drew, J. E.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Szkody, Paula] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Kafka, S.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Belle, Kunegunda] Los Alamos Natl Lab, Los Alamos, NM USA. [Froning, Cynthia S.] Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [van Belle, Gerard T.] Lowell Observ, Flagstaff, AZ 86001 USA. [Pretorius, M. L.] Univ Oxford, Dept Phys, Oxford, England. RP Hoard, DW (reprint author), Eureka Sci Inc, Oakland, CA 94602 USA. EM hoard@mpia.de OI Ciardi, David/0000-0002-5741-3047; Drew, Janet/0000-0003-1192-7082; Long, Knox/0000-0002-4134-864X FU NASA; National Science Foundation (NSF) FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech), under a contract with the National Aeronautics and Space Administration (NASA). Support for this work was provided by NASA. We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. This work is also based on data, data products, and other resources obtained from: (1) The Two Micron All Sky Survey (2MASS), a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center (IPAC)/Caltech, funded by NASA and the National Science Foundation (NSF). (2) NASA's Astrophysics Data System. (3) The NASA/IPAC Infrared Science Archive (IRSA), which is operated by JPL/Caltech, under a contract with NASA. (4) The SIMBAD database, operated at CDS, Strasbourg, France. (5) The Wide-field Infrared Survey Explorer (WISE), which is a joint project of the University of California, Los Angeles, and JPL/Caltech, funded by NASA. NR 201 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 68 DI 10.1088/0004-637X/786/1/68 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700068 ER PT J AU Patel, B McCully, C Jha, SW Rodney, SA Jones, DO Graur, OR Merten, J Zitrin, A Riess, AG Matheson, T Sako, M Holoien, TWS Postman, M Coe, D Bartelmann, M Balestra, I Benitez, N Bouwens, R Bradley, L Broadhurst, T Cenko, SB Donahue, M Filippenko, AV Ford, H Garnavich, P Grillo, C Infante, L Jouvel, S Kelson, D Koekemoer, A Lahav, O Lemze, D Maoz, D Medezinski, E Melchior, P Meneghetti, M Molino, A Moustakas, J Moustakas, LA Nonino, M Rosati, P Seitz, S Strolger, LG Umetsu, K Zheng, W AF Patel, Brandon McCully, Curtis Jha, Saurabh W. Rodney, Steven A. Jones, David O. Graur, O. R. Merten, Julian Zitrin, Adi Riess, Adam G. Matheson, Thomas Sako, Masao Holoien, Thomas W. -S. Postman, Marc Coe, Dan Bartelmann, Matthias Balestra, Italo Benitez, Narciso Bouwens, Rychard Bradley, Larry Broadhurst, Tom Cenko, S. Bradley Donahue, Megan Filippenko, Alexei V. Ford, Holland Garnavich, Peter Grillo, Claudio Infante, Leopoldo Jouvel, Stephanie Kelson, Daniel Koekemoer, Anton Lahav, Ofer Lemze, Doron Maoz, Dan Medezinski, Elinor Melchior, Peter Meneghetti, Massimo Molino, Alberto Moustakas, John Moustakas, Leonidas A. Nonino, Mario Rosati, Piero Seitz, Stella Strolger, Louis G. Umetsu, Keiichi Zheng, Wei TI THREE GRAVITATIONALLY LENSED SUPERNOVAE BEHIND CLASH GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: general; gravitational lensing: weak; supernovae: general ID DIGITAL SKY SURVEY; HIGH-REDSHIFT SUPERNOVAE; HUBBLE-SPACE-TELESCOPE; IA LIGHT CURVES; FARTHEST KNOWN SUPERNOVA; DARK-ENERGY CONSTRAINTS; LEGACY SURVEY; DISTANT SUPERNOVAE; COSMOLOGICAL PARAMETERS; ACCELERATING UNIVERSE AB We report observations of three gravitationally lensed supernovae (SNe) in the Cluster Lensing And Supernova survey with Hubble (CLASH) Multi-Cycle Treasury program. These objects, SN CLO12Car (z = 1.28), SN CLN12Did (z = 0.85), and SN CLA11Tib (z = 1.14), are located behind three different clusters, MACSJ1720.2+3536 (z = 0.391), RXJ1532.9+3021 (z = 0.345), and A383 (z = 0.187), respectively. Each SN was detected in Hubble Space Telescope optical and infrared images. Based on photometric classification, we find that SNe CLO12Car and CLN12Did are likely to be Type Ia supernovae (SNe Ia), while the classification of SN CLA11Tib is inconclusive. Using multi-color light-curve fits to determine a standardized SN Ia luminosity distance, we infer that SN CLO12Car was similar to 1.0 +/- 0.2 mag brighter than field SNe Ia at a similar redshift and ascribe this to gravitational lens magnification. Similarly, SN CLN12Did is similar to 0.2 +/- 0.2 mag brighter than field SNe Ia. We derive independent estimates of the predicted magnification from CLASH strong+weak-lensing maps of the clusters (in magnitude units, 2.5 log(10) mu): 0.83 +/- 0.16 mag for SN CLO12Car, 0.28 +/- 0.08 mag for SN CLN12Did, and 0.43 +/- 0.11 mag for SN CLA11Tib. The two SNe Ia provide a new test of the cluster lens model predictions: we find that the magnifications based on the SN Ia brightness and those predicted by the lens maps are consistent. Our results herald the promise of future observations of samples of cluster-lensed SNe Ia (from the ground or space) to help illuminate the dark-matter distribution in clusters of galaxies, through the direct determination of absolute magnifications. C1 [Patel, Brandon; McCully, Curtis; Jha, Saurabh W.; Holoien, Thomas W. -S.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Rodney, Steven A.; Jones, David O.; Graur, O. R.; Riess, Adam G.; Ford, Holland; Lemze, Doron; Medezinski, Elinor; Zheng, Wei] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Graur, O. R.; Maoz, Dan] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Graur, O. R.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Graur, O. R.] NYU, CCPP 4, New York, NY 10003 USA. [Merten, Julian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zitrin, Adi] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Riess, Adam G.; Koekemoer, Anton; Strolger, Louis G.] Space Telescope Sci Inst, Baltimore, MD 21208 USA. [Matheson, Thomas] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Sako, Masao] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bartelmann, Matthias] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Balestra, Italo; Nonino, Mario] INAF Osservatorio Astron Trieste, I-34131 Trieste, Italy. [Balestra, Italo] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy. [Benitez, Narciso; Molino, Alberto] Inst Astrofis Andalucia CSIC, E-18008 Granada, Spain. [Bouwens, Rychard] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Broadhurst, Tom] Univ Basque Country, Dept Theoret Phys, E-48080 Bilbao, Spain. [Cenko, S. Bradley] NASA GSFC, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. Bradley; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Garnavich, Peter] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Grillo, Claudio] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Infante, Leopoldo] Pontificia Univ Catolica Chile, Inst Astrophys, Santiago, Chile. [Jouvel, Stephanie] Inst Ciencias Espai IEEC CSIC, E-08913 Bellaterra, Barcelona, Spain. [Kelson, Daniel] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Lahav, Ofer] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Melchior, Peter] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Melchior, Peter] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Meneghetti, Massimo] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Meneghetti, Massimo] INFN, I-40127 Bologna, Italy. [Meneghetti, Massimo] INFN, Sez Bologna, I-40127 Bologna, Italy. [Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Rosati, Piero] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [Rosati, Piero] ESO European So Observ, D-85748 Garching, Germany. [Seitz, Stella] Univ Sternwarte, D-81679 Munich, Germany. [Umetsu, Keiichi] Acad Sin, Inst Astron & Astrophys, Taipei 10617, Taiwan. RP Patel, B (reprint author), Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. EM bpatel02@physics.rutgers.edu RI Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015; OI Grillo, Claudio/0000-0002-5926-7143; Meneghetti, Massimo/0000-0003-1225-7084; Nonino, Mario/0000-0001-6342-9662; Koekemoer, Anton/0000-0002-6610-2048; Benitez, Narciso/0000-0002-0403-7455; Balestra, Italo/0000-0001-9660-894X; Graur, Or/0000-0002-4391-6137; Umetsu, Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360 FU [GN-2012A-Q-32]; [GN-2013A-Q-25] FX Additional data were obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). The data were taken as part of programs GN-2012A-Q-32 and GN-2013A-Q-25. NR 93 TC 23 Z9 23 U1 1 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 9 DI 10.1088/0004-637X/786/1/9 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700009 ER PT J AU Quintana, EV Lissauer, JJ AF Quintana, Elisa V. Lissauer, Jack J. TI THE EFFECT OF PLANETS BEYOND THE ICE LINE ON THE ACCRETION OF VOLATILES BY HABITABLE-ZONE ROCKY PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; planets and satellites: composition; planets and satellites: dynamical evolution and stability; planets and satellites: formation; planets and satellites: terrestrial planets ID HIGH-RESOLUTION SIMULATIONS; BINARY STAR SYSTEMS; EARTH-LIKE PLANETS; TERRESTRIAL PLANETS; WATER DELIVERY; COLLISIONS; ASTEROIDS; RATIO; TIMESCALES; DIVERSITY AB Models of planet formation have shown that giant planets have a large impact on the number, masses, and orbits of terrestrial planets that form. In addition, they play an important role in delivering volatiles from material that formed exterior to the snow line (the region in the disk beyond which water ice can condense) to the inner region of the disk where terrestrial planets can maintain liquid water on their surfaces. We present simulations of the late stages of terrestrial planet formation from a disk of protoplanets around a solar-type star and we include a massive planet (from 1M(circle plus) to 1 M-J) in Jupiter's orbit at similar to 5.2 AU in all but one set of simulations. Two initial disk models are examined with the same mass distribution and total initial water content, but with different distributions of water content. We compare the accretion rates and final watermass fraction of the planets that form. Remarkably, all of the planets that formed in our simulations without giant planets were water-rich, showing that giant planet companions are not required to deliver volatiles to terrestrial planets in the habitable zone. In contrast, an outer planet at least several times the mass of Earth may be needed to clear distant regions of debris truncating the epoch of frequent large impacts. Observations of exoplanets from radial velocity surveys suggest that outer Jupiter-like planets may be scarce, therefore, the results presented here suggest that there may be more habitable planets residing in our galaxy than previously thought. C1 [Quintana, Elisa V.] SETI Inst, Mountain View, CA 94043 USA. [Quintana, Elisa V.; Lissauer, Jack J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div 245 3, Moffett Field, CA 94035 USA. RP Quintana, EV (reprint author), SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA. EM elisa.quintana@nasa.gov FU NASA Ames Team of the NASA Astrobiology Institute FX This work was funded in part by the NASA Ames Team of the NASA Astrobiology Institute. E.V.Q. thanks Tom Barclay for useful discussions and assistance with the figures. NR 42 TC 7 Z9 7 U1 2 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 33 DI 10.1088/0004-637X/786/1/33 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700033 ER PT J AU Tang, SM Bildsten, L Wolf, WM Li, KL Kong, AKH Cao, Y Cenko, SB De Cia, A Kasliwal, MM Kulkarni, SR Laher, RR Masci, F Nugent, PE Perley, DA Prince, TA Surace, J AF Tang, Sumin Bildsten, Lars Wolf, William M. Li, K. L. Kong, Albert K. H. Cao, Yi Cenko, S. Bradley De Cia, Annalisa Kasliwal, Mansi M. Kulkarni, Shrinivas R. Laher, Russ R. Masci, Frank Nugent, Peter E. Perley, Daniel A. Prince, Thomas A. Surace, Jason TI AN ACCRETING WHITE DWARF NEAR THE CHANDRASEKHAR LIMIT IN THE ANDROMEDA GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M31); novae, cataclysmic variables; supernovae : general; white dwarfs; X-rays : binaries ID REMARKABLE RECURRENT NOVA; STELLAR ASTROPHYSICS MESA; X-RAY SOURCES; CLASSICAL NOVAE; PHOTOMETRIC CALIBRATION; CENTRAL REGION; LIGHT CURVES; U SCORPII; TELESCOPE; M31 AB The intermediate Palomar Transient Factory (iPTF) detection of the most recent outburst of the recurrent nova (RN) system RX J0045.4+4154 in the Andromeda galaxy has enabled the unprecedented study of a massive (M > 1.3 M (circle dot)) accreting white dwarf (WD). We detected this nova as part of the near-daily iPTF monitoring of M31 to a depth of R approximate to 21 mag and triggered optical photometry, spectroscopy and soft X-ray monitoring of the outburst. Peaking at an absolute magnitude of M-R = -6.6 mag, and with a decay time of 1 mag per day, it is a faint and very fast nova. It shows optical emission lines of He/N and expansion velocities of 1900-2600 km s(-1) 1-4 days after the optical peak. The Swift monitoring of the X-ray evolution revealed a supersoft source (SSS) with kT(eff) approximate to 90-110 eV that appeared within 5 days after the optical peak, and lasted only 12 days. Most remarkably, this is not the first event from this system, rather it is an RN with a time between outbursts of approximately 1 yr, the shortest known. Recurrent X-ray emission from this binary was detected by ROSAT in 1992 and 1993, and the source was well characterized as a M > 1.3 M (circle dot) WD SSS. Based on the observed recurrence time between different outbursts, the duration and effective temperature of the SS phase, MESA models of accreting WDs allow us to constrain the accretion rate to M > 1.7 Chi 10(-7) M-circle dot yr(-1) and WD mass > 1.30 M-circle dot. If the WD keeps 30% of the accreted material, it will take less than a Myr to reach core densities high enough for carbon ignition (if made of C/O) or electron capture (if made of O/Ne) to end the binary evolution. C1 [Tang, Sumin; Bildsten, Lars] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Tang, Sumin; Cao, Yi; Kulkarni, Shrinivas R.; Perley, Daniel A.; Prince, Thomas A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Bildsten, Lars; Wolf, William M.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Li, K. L.; Kong, Albert K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Li, K. L.; Kong, Albert K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. [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. [De Cia, Annalisa] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Kasliwal, Mansi M.] Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. [Laher, Russ R.; Surace, Jason] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Masci, Frank] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Nugent, Peter E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Tang, SM (reprint author), Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. OI Wolf, William/0000-0002-6828-0630 FU National Science Foundation [PHY 11-25915, AST 11-09174, AST 12-05574]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; National Science Council of the Republic of China (Taiwan) [NSC101-2119-M-008-007-MY3]; Hubble Fellowship; Carnegie-Princeton Fellowship FX This work was supported by the National Science Foundation under grants PHY 11-25915, AST 11-09174, and AST 12-05574. Most of the MESA simulations for this work were made possible by the Triton Resource. The Triton Resource is a high-performance research computing system operated by the San Diego Supercomputer Center at UC San Diego. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. A.K.H.K. is supported by the National Science Council of the Republic of China (Taiwan) through grant NSC101-2119-M-008-007-MY3. M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. We are grateful to the Swift Team for the superb timely scheduling of the observations and providing data and analysis tools, and to Bill Paxton for his development of MESA. NR 59 TC 25 Z9 25 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 61 DI 10.1088/0004-637X/786/1/61 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700061 ER PT J AU Wylezalek, D Vernet, J De Breuck, C Stern, D Brodwin, M Galametz, A Gonzalez, AH Jarvis, M Hatch, N Seymour, N Stanford, SA AF Wylezalek, Dominika Vernet, Joel De Breuck, Carlos Stern, Daniel Brodwin, Mark Galametz, Audrey Gonzalez, Anthony H. Jarvis, Matt Hatch, Nina Seymour, Nick Stanford, Spencer A. TI THE GALAXY CLUSTER MID-INFRARED LUMINOSITY FUNCTION AT 1.3 < z < 3.2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: luminosity function, mass function; techniques: photometric ID STELLAR POPULATION SYNTHESIS; COLOR-MAGNITUDE RELATION; REDSHIFT RADIO GALAXIES; ACTIVE GALACTIC NUCLEI; SOUTH-POLE TELESCOPE; IRAC SHALLOW SURVEY; H-ALPHA EMITTERS; STAR-FORMATION; FUNDAMENTAL-PLANE; HOST GALAXIES AB We present 4.5 mu m luminosity functions for galaxies identified in 178 candidate galaxy clusters at 1.3 < z < 3.2. The clusters were identified as Spitzer/Infrared Array Camera (IRAC) color-selected overdensities in the Clusters Around Radio-Loud AGN project, which imaged 420 powerful radio-loud active galactic nuclei (RLAGNs) at z > 1.3. The luminosity functions are derived for different redshift and richness bins, and the IRAC imaging reaches depths of m* + 2, allowing us to measure the faint end slopes of the luminosity functions. We find that alpha = -1 describes the luminosity function very well in all redshift bins and does not evolve significantly. This provides evidence that the rate at which the low mass galaxy population grows through star formation gets quenched and is replenished by in-falling field galaxies does not have a major net effect on the shape of the luminosity function. Our measurements for m* are consistent with passive evolution models and high formation redshifts (z(f) similar to 3). We find a slight trend toward fainter m* for the richest clusters, implying that the most massive clusters in our sample could contain older stellar populations, yet another example of cosmic downsizing. Modeling shows that a contribution of a star-forming population of up to 40% cannot be ruled out. This value, found from our targeted survey, is significantly lower than the values found for slightly lower redshift, z similar to 1, clusters found in wide-field surveys. The results are consistent with cosmic downsizing, as the clusters studied here were all found in the vicinity of RLAGNs-which have proven to be preferentially located in massive dark matter halos in the richest environments at high redshift-and they may therefore be older and more evolved systems than the general protocluster population. C1 [Wylezalek, Dominika; Vernet, Joel; De Breuck, Carlos] European So Observ, D-85748 Garching, Germany. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Galametz, Audrey] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Jarvis, Matt] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Jarvis, Matt] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Hatch, Nina] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Seymour, Nick] CASS, Epping, NSW 1710, Australia. [Stanford, Spencer A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, Spencer A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. RP Wylezalek, D (reprint author), European So Observ, Karl Schwarzschildstr 2, D-85748 Garching, Germany. OI Hatch, Nina/0000-0001-5600-0534; Vernet, Joel/0000-0002-8639-8560; Seymour, Nicholas/0000-0003-3506-5536; De Breuck, Carlos/0000-0002-6637-3315 FU ARC Future Fellowship; NASA FX We thank the referee for helpful comments that have improved the manuscript. We gratefully thank Mark Lacy for allowing us to access SERVS images and catalogs and Roberto Assef and Conor Mancone for helpful discussions and advice. N. Seymour is the recipient of an ARC Future Fellowship. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 61 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 MAY 1 PY 2014 VL 786 IS 1 AR 17 DI 10.1088/0004-637X/786/1/17 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700017 ER PT J AU Turner, DD Ferrare, RA Wulfmeyer, V Scarino, AJ AF Turner, D. D. Ferrare, R. A. Wulfmeyer, V. Scarino, A. J. TI Aircraft Evaluation of Ground-Based Raman Lidar Water Vapor Turbulence Profiles in Convective Mixed Layers SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Boundary layer; Mass fluxes/transport; Water vapor; Lidars/Lidar observations ID SOUTHERN GREAT-PLAINS; ATMOSPHERIC BOUNDARY-LAYER; LARGE-EDDY SIMULATION; AEROSOL EXTINCTION; DOPPLER LIDAR; VERTICAL VELOCITY; RADAR-RASS; WRF MODEL; CLOUDS; STATISTICS AB High temporal and vertical resolution water vapor measurements by Raman and differential absorption lidar systems have been used to characterize the turbulent fluctuations in the water vapor mixing ratio field in convective mixed layers. Since daytime Raman lidar measurements are inherently noisy (due to solar background and weak signal strengths), the analysis approach needs to quantify and remove the contribution of the instrument noise in order to derive the desired atmospheric water vapor mixing ratio variance and skewness profiles. This is done using the approach outlined by Lenschow et al.; however, an intercomparison with in situ observations was not performed. Water vapor measurements were made by a diode laser hygrometer flown on a Twin Otter aircraft during the Routine Atmospheric Radiation Measurement (ARM) Program Aerial Facility Clouds with Low Optical Water Depths Optical Radiative Observations (RACORO) field campaign over the ARM Southern Great Plains (SGP) site in 2009. Two days with Twin Otter flights were identified where the convective mixed layer was quasi stationary, and hence the 10-s, 75-m data from the SGP Raman lidar could be analyzed to provide profiles of water vapor mixing ratio variance and skewness. Airborne water vapor observations measured during level flight legs were compared to the Raman lidar data, demonstrating good agreement in both variance and skewness. The results also illustrate the challenges of comparing a point sensor making measurements over time to a moving platform making similar measurements horizontally. C1 [Turner, D. D.] NOAA, Natl Severe Storms Lab, Norman, OK 73072 USA. [Ferrare, R. A.] NASA Langley Res Ctr, Hampton, VA USA. [Wulfmeyer, V.] Univ Hohenheim, Stuttgart, Germany. [Scarino, A. J.] Sci Syst & Applicat Inc, Hampton, VA USA. RP Turner, DD (reprint author), NOAA, Natl Severe Storms Lab, 120 David L Boren Blvd, Norman, OK 73072 USA. EM dave.turner@noaa.gov FU NOAA's National Severe Storms Laboratory; Department of Energy (DOE) Atmospheric System Research (ASR); NASA Science Mission Directorate; ASR program [DE-AI02-05ER63985]; DOE Office of Science, Office of Biological and Environmental Research (OBER); NASA CALIPSO project FX NOAA's National Severe Storms Laboratory and the Department of Energy (DOE) Atmospheric System Research (ASR) program supported this work. We thank the Raman lidar mentor team of Chris Martin, John Goldsmith, and Rob Newsom for their efforts in maintaining the Raman lidar. We would also like to thank the entire RACORO team: Andy Vogelmann for his leadership before, during, and after the experiment; the RACORO scientific steering committee; Haf Jonsson for the analysis and processing of the Twin Otter flight data; Glen Diskin for the DLH processing; and the AAF for its coordination of the RACORO flight activities. The data used in this paper were collected as part of ARM, and are available via its online data archive (http://www.archive.arm.gov). HSRL operations were supported by the NASA Science Mission Directorate, the ASR program (Interagency Agreement DE-AI02-05ER63985), the DOE Office of Science, Office of Biological and Environmental Research (OBER), and the NASA CALIPSO project. The authors thank the NASA Langley King Air B-200 flight crew for its outstanding work supporting these flights and measurements. Finally, we thank Mike Coniglio, Andy Vogelmann, Glenn Diskin, and Haf Jonsson for providing comments on an earlier draft of this manuscript, and especially the two anonymous reviewers for their excellent input, which improved this manuscript. NR 38 TC 11 Z9 11 U1 0 U2 17 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 MAY PY 2014 VL 31 IS 5 BP 1078 EP 1088 DI 10.1175/JTECH-D-13-00075.1 PG 11 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AH1LF UT WOS:000335881600004 ER PT J AU Kwok, R Markus, T Morison, J Palm, SP Neumann, TA Brunt, KM Cook, WB Hancock, DW Cunningham, GF AF Kwok, R. Markus, T. Morison, J. Palm, S. P. Neumann, T. A. Brunt, K. M. Cook, W. B. Hancock, D. W. Cunningham, G. F. TI Profiling Sea Ice with a Multiple Altimeter Beam Experimental Lidar (MABEL) SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Remote sensing; Altimetry; Satellite observations; Sea ice; Lidars/Lidar observations; Ice thickness ID MISSION; SHEET AB The sole instrument on the upcoming Ice, Cloud, and Land Elevation Satellite (ICESat-2) altimetry mission is a micropulse lidar that measures the time of flight of individual photons from laser pulses transmitted at 532 nm. Prior to launch, the Multiple Altimeter Beam Experimental Lidar (MABEL) serves as an airborne implementation for testing and development. This paper provides a first examination of MABEL data acquired on two flights over sea ice in April 2012: one north of the Arctic coast of Greenland and the other in the east Greenland Sea. The phenomenology of photon distributions in the sea ice returns is investigated. An approach to locate the surface and estimate its elevation in the distributions is described, and its achievable precision is assessed. Retrieved surface elevations over relatively flat leads in the ice cover suggest that precisions of several centimeters are attainable. Restricting the width of the elevation window used in the surface analysis can mitigate potential biases in the elevation estimates due to subsurface returns at 532 nm. Comparisons of nearly coincident elevation profiles from MABEL with those acquired by an analog lidar show good agreement. Discrimination of ice and open water, a crucial step in the determination of sea ice freeboard and the estimation of ice thickness, is facilitated by contrasts in the observed signal-background photon statistics. Future flight paths will sample a broader range of seasonal ice conditions for further evaluation of the year-round profiling capabilities and limitations of the MABEL instrument. C1 [Kwok, R.; Cunningham, G. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Markus, T.; Neumann, T. A.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Morison, J.] Univ Washington, Polar Sci Ctr, Seattle, WA 98195 USA. [Palm, S. P.] Sci Syst & Applicat Inc, Lanham, MD USA. [Brunt, K. M.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Brunt, K. M.] NASA, Goddard Space Flight Ctr, GESTAR, Greenbelt, MD 20771 USA. [Cook, W. B.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Processes Lab, Greenbelt, MD 20771 USA. [Hancock, D. W.] NASA, Wallops Flight Facil, Wallops Isl, VA USA. RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ron.kwok@jpl.nasa.gov RI Kwok, Ron/A-9762-2008; Neumann, Thomas/D-5264-2012 OI Kwok, Ron/0000-0003-4051-5896; FU NASA's Airborne Science Program; National Aeronautics and Space Administration FX The digital camera system (DCS) on the ER-2 is operated and maintained by the Airborne Sensor Facility under the auspices of NASA's Airborne Science Program. RK and GFC carried out this work at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 14 TC 7 Z9 9 U1 3 U2 13 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 MAY PY 2014 VL 31 IS 5 BP 1151 EP 1168 DI 10.1175/JTECH-D-13-00120.1 PG 18 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AH1LF UT WOS:000335881600009 ER PT J AU Schubert, SD Wang, HL Koster, RD Suarez, MJ Groisman, PY AF Schubert, Siegfried D. Wang, Hailan Koster, Randal D. Suarez, Max J. Groisman, Pavel Ya. TI Northern Eurasian Heat Waves and Droughts SO JOURNAL OF CLIMATE LA English DT Review DE Hydrologic cycle; Anticyclones; Waves, atmospheric; Climate variability; Drought; Atmosphere-land interaction ID SOIL-MOISTURE; ATMOSPHERIC BLOCKING; SURFACE-TEMPERATURE; CLIMATE EXTREMES; EUROPEAN SUMMER; ANNULAR MODE; SEA-ICE; PRECIPITATION; HEMISPHERE; TELECONNECTION AB This article reviews the understanding of the characteristics and causes of northern Eurasian summertime heat waves and droughts. Additional insights into the nature of temperature and precipitation variability in Eurasia on monthly to decadal time scales and into the causes and predictability of the most extreme events are gained from the latest generation of reanalyses and from supplemental simulations with the NASA Goddard Earth Observing System model, version 5 (GEOS-5). Key new results are 1) the identification of the important role of summertime stationary Rossby waves in the development of the leading patterns of monthly Eurasian surface temperature and precipitation variability (including the development of extreme events such as the 2010 Russian heat wave); 2) an assessment of the mean temperature and precipitation changes that have occurred over northern Eurasia in the last three decades and their connections to decadal variability and global trends in SST; and 3) the quantification (via a case study) of the predictability of the most extreme simulated heat wave/drought events, with some focus on the role of soil moisture in the development and maintenance of such events. A literature survey indicates a general consensus that the future holds an enhanced probability of heat waves across northern Eurasia, while there is less agreement regarding future drought, reflecting a greater uncertainty in soil moisture and precipitation projections. Substantial uncertainties remain in the understanding of heat waves and drought, including the nature of the interactions between the short-term atmospheric variability associated with such extremes and the longer-term variability and trends associated with soil moisture feedbacks, SST anomalies, and an overall warming world. C1 [Schubert, Siegfried D.; Wang, Hailan; Koster, Randal D.; Suarez, Max J.] NASA, GSFC, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Groisman, Pavel Ya.] Natl Climat Ctr, Asheville, NC USA. RP Schubert, SD (reprint author), NASA, GSFC, Global Modeling & Assimilat Off, NASA GSFC Code 610-1, Greenbelt, MD 20771 USA. EM siegfried.d.schubert@nasa.gov RI Koster, Randal/F-5881-2012 OI Koster, Randal/0000-0001-6418-6383 FU NASA Modeling, Analysis, and Prediction (MAP) Program; NOAA/NASA [NNX13AJ02G]; Ministry of Education and Science of the Russian Federation [14.B25.31.0026]; WCRP; ESA-ESRIN; NASA; NIDIS; NSF; GEO; USCLIVAR; NOAA FX Support for this project was provided by the NASA Modeling, Analysis, and Prediction (MAP) Program. Research of Pavel Groisman was supported by NOAA/NASA (Grant NNX13AJ02G) and Grant 14.B25.31.0026 of the Ministry of Education and Science of the Russian Federation. The lead author would like to thank Anna Borovikov for helping to translate some of the Russian language literature. We also wish to thank two anonymous reviewers for their helpful comments and suggestions for improving the manuscript. The NOAA GHCN gridded V2 data, the NOAA Merged Air Land and SST Anomalies data, the NASA GPCP precipitation, and the NOAA PRECL precipitation data were obtained from NOAA/OAR/ESRL PSD from their website at http://www.esrl.noaa.gov/psd/. This paper is part of a special collection devoted to our understanding of drought throughout the world. The idea for this collection came about as a recommendation of a 2012 international workshop on the development of a Global Drought Information System (GDIS) sponsored by WCRP and various partner organizations (ESA-ESRIN, NASA, NIDIS, NSF, GEO, USCLIVAR, and NOAA). NR 134 TC 27 Z9 28 U1 6 U2 56 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD MAY PY 2014 VL 27 IS 9 BP 3169 EP 3207 DI 10.1175/JCLI-D-13-00360.1 PG 39 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AG9EI UT WOS:000335721800002 ER PT J AU Som, SM AF Som, Sanjoy M. TI PLANETARY SCIENCE Into thin martian air SO NATURE GEOSCIENCE LA English DT News Item ID EARLY MARS; CLIMATE AB A dense early atmosphere has been invoked to explain the strong greenhouse effect inferred for early Mars. Yet an analysis of the smallest impact craters suggests that the atmospheric pressure on Mars 3.6 billion years ago was surprisingly low. C1 [Som, Sanjoy M.] NASA, Ames Res Ctr, Blue Marble Space Inst Sci, Exobiol Branch, Moffett Field, CA 94035 USA. [Som, Sanjoy M.] NASA, Ames Res Ctr, Flight Syst Implementat Branch, Moffett Field, CA 94035 USA. RP Som, SM (reprint author), NASA, Ames Res Ctr, Blue Marble Space Inst Sci, Exobiol Branch, Moffett Field, CA 94035 USA. EM sanjoy@bmsis.org NR 11 TC 0 Z9 0 U1 1 U2 12 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 MAY PY 2014 VL 7 IS 5 BP 329 EP 330 DI 10.1038/ngeo2145 PG 2 WC Geosciences, Multidisciplinary SC Geology GA AH2JZ UT WOS:000335948600005 ER PT J AU Neu, JL Flury, T Manney, GL Santee, ML Livesey, NJ Worden, J AF Neu, Jessica L. Flury, Thomas Manney, Gloria L. Santee, Michelle L. Livesey, Nathaniel J. Worden, John TI Tropospheric ozone variations governed by changes in stratospheric circulation SO NATURE GEOSCIENCE LA English DT Article ID QUASI-BIENNIAL OSCILLATION; TRENDS; MODEL; VARIABILITY; CHEMISTRY; EXCHANGE; ENSO AB The downward transport of stratospheric ozone is an important natural source of tropospheric ozone, particularly in the upper troposphere, where changes in ozone have their largest radiative effect(1). Stratospheric circulation is projected to intensify over the coming century, which could lead to an increase in the flux of ozone from the stratosphere to the troposphere(2-4). However, large uncertainties in the stratospheric contribution to trends and variability in tropospheric ozone levels(5-7) make it difficult to reliably project future changes in tropospheric ozone(8). Here, we use satellite measurements of stratospheric water vapour and tropospheric ozone levels collected between 2005 and 2010 to assess the effect of changes in stratospheric circulation, driven by El Nino/Southern Oscillation and the stratospheric Quasi-Biennial Oscillation, on tropospheric ozone levels. Wefindthat interannual variations in the strength of the stratospheric circulation of around 40%-comparable to the mean change in stratospheric circulation projected this century(2)-lead to changes in tropospheric ozone levels in the northern mid-latitudes of around 2%, approximately half of the interannual variability. Assuming that the observed response of tropospheric ozone levels to interannual variations in circulation is a good predictor of its equilibrium response, we suggest that the projected intensification of the stratospheric circulation over the coming century could lead to small but important increases in tropospheric ozone levels. C1 [Neu, Jessica L.; Flury, Thomas; Santee, Michelle L.; Livesey, Nathaniel J.; Worden, John] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Manney, Gloria L.] NorthWest Res Associates, Socorro, NM 87801 USA. [Manney, Gloria L.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA. RP Neu, JL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jessica.l.neu@jpl.nasa.gov FU National Aeronautics and Space Administration FX We thank the MLS and TES science teams and the Aura project for their support. We also thank J-F. Lamarque and D. Kinnison of the National Center for Atmospheric Research for providing CAM-Chem and WACCM modelling results, respectively, H. Nguyen of the Jet Propulsion Laboratory for help with the statistical analysis, T. Shepherd of the University of Reading for allowing us to include results from the CMAM model, and S. Hardiman of the UK Meterological Office for providing model residual vertical velocities. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 30 TC 31 Z9 31 U1 1 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 MAY PY 2014 VL 7 IS 5 BP 340 EP 344 DI 10.1038/ngeo2138 PG 5 WC Geosciences, Multidisciplinary SC Geology GA AH2JZ UT WOS:000335948600010 ER PT J AU Xu, HF Shen, ZZ Konishi, H Fu, PQ Szlufarska, I AF Xu, Huifang Shen, Zhizhang Konishi, Hiromi Fu, Pingqiu Szlufarska, Izabela TI Crystal structures of laihunite and intermediate phases between laihunite-1M and fayalite: Z-contrast imaging and ab initio study SO AMERICAN MINERALOGIST LA English DT Article DE Laihunite; vacancy ordering; Z-contrast imaging; DFT; HRTEM; superstructure; olivine; oxidation ID OLIVINE; OXIDATION; MICROSCOPY; SERPENTINE AB Crystals of laihunite from Xiaolaihe of Liaoning Province, northeast China, were studied using selected-area electron diffraction (SAED), high-resolution transmission electron microscopy (HRTEM), and Z-contrast imaging. Z-contrast images directly reveal ordered vacancies in M1 sites. The results confirm early structural models for 1-layer laihunite (or laihunite-1M) with ideal stoichiometry of square 0 5Fe0.52+Fe3+SiO4. 2-layer laihunite and 3-layer laihunite are found to be chemically different from laihunite-1M. The 2-layer laihunite can be viewed as a periodic intergrowth of laihunite and fayalite in the 1:1 ratio. The 3-layer laihunite can be considered to be a periodic intergrowth of laihunite and fayalite in the 1:0.5 ratio along the c-axis. Ideal stoichiometries for the 2-layer structure and the 3-layer structure are square 0.5Fe2.52+Fe3+[SiO4](2) and square 1.0Fe3.02+Fe2.03+[SiO4](3), respectively. The structural intergrowth of the 3-layer laihunite and the 1-layer lahunite results in chemical compositions falling within the range between the two aforementioned structures, such as the chemical formula of square 0.4Fe0.82+Fe0.83+SiO4, reported earlier in the literature. The crystal structures of the 1-layer laihunite (1M), the 2-layer laihunite (2M), and the 3-layer laihunite (3Or) determined from Z-contrast images and ab initio calculations using the density functional theory (DFT) have space groups of P2(1)/b, P2(1)/b, and Pbnm, respectively. The previously reported monoclinic symmetry for the 3-layer laihunite may be an artifact due to overlapping diffraction spots from both, the laihunite-3 Or and the laihunite-1M. Our study demonstrates that the method of combining Z-contrast imaging and ab initio calculation can be effectively used for identifying structures of nano-phases in host crystals. Perhaps more importantly, Z-contrast imaging provides a powerful means for direct observation of vacancies and other defects, and may be utilized to map vacancies in Fe3+-bearing olivines, the alignments of which can greatly affect anisotropic diffusion in such structures. C1 [Xu, Huifang; Shen, Zhizhang; Konishi, Hiromi] Univ Wisconsin, NASA Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA. [Fu, Pingqiu] Chinese Acad Sci, Inst Geochem, Guiyang 550002, Guizhou, Peoples R China. [Szlufarska, Izabela] Univ Wisconsin, Dept Mat Sci & Engn, Madison, WI 53706 USA. RP Xu, HF (reprint author), Univ Wisconsin, NASA Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA. EM hfxu@geology.wisc.edu FU NASA Astrobiology Institute [N07-5489]; NSF [EAR-095800]; Major Research Instrumentation (MRI) program of NSF; K. C. Wong Education Foundation (Hong Kong) FX This work is supported by NASA Astrobiology Institute (N07-5489) and NSF (EAR-095800). Authors thank Alex Kivit for optimizing instrument condition. Author also thank Major Research Instrumentation (MRI) program of NSF for funding the aberration corretced STEM. Xu thanks David Veblen for supporting his early TEM works at Johns Hopkins University. Xu and Fu acknowledge K. C. Wong Education Foundation (Hong Kong) for supporting early stage of this collaborative research. NR 34 TC 7 Z9 7 U1 1 U2 14 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD MAY-JUN PY 2014 VL 99 IS 5-6 BP 881 EP 889 DI 10.2138/am.2014.4691 PG 9 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AG7YE UT WOS:000335633900003 ER PT J AU Dyar, MD Jawin, ER Breves, E Marchand, G Nelms, M Lane, MD Mertzman, SA Bish, DL Bishop, JL AF Dyar, M. Darby Jawin, Erica R. Breves, Elly Marchand, Gerard Nelms, Melissa Lane, Melissa D. Mertzman, Stanley A. Bish, David L. Bishop, Janice L. TI Mossbauer parameters of iron in phosphate minerals: Implications for interpretation of martian data SO AMERICAN MINERALOGIST LA English DT Article DE Mossbauer; Mars; phosphates; alluaudite; arrojadite; vivianite; triphylite ID SOLID-SOLUTION SERIES; X-RAY SPECTROMETER; QUADRUPOLE SPLITTING DISTRIBUTIONS; CRYSTAL-STRUCTURE DETERMINATION; TRIPLITE-TRIPLOIDITE GROUP; ALLUAUDITE STRUCTURE TYPE; SAPUCAIA-PEGMATITE MINE; MERIDIANI-PLANUM; SNC METEORITES; SYNTHETIC LIPSCOMBITE AB Phosphate minerals, while relatively rare, show a broad range of crystal structure types with linkages among PO4 tetrahedra mimicking the hierarchy of polymerization of SiO4 tetrahedra seen in silicate minerals. To augment previous Mossbauer studies of individual phosphate species and groups of species, this paper presents new Mossbauer data on 63 different phosphate samples, and integrates them with data on more than 37 phosphate species in 62 other studies from the literature. Variations in Mossbauer parameters of different sites in each mineral are then related to both the local polyhedral environment around the Fe cations and the overall structural characteristics of each species. The entire aggregated Mossbauer data set on phosphate minerals is juxtaposed against parameters obtained for spectra from the MIMOS spectrometers on Mars. This comparison demonstrates that signatures from many different phosphate or sulfate mineral species could also be contributing to Mars Mossbauer spectra. Results underscore the conclusion that unique mineral identifications are generally not possible from Mossbauer data alone, particularly for paramagnetic phases, although combining Mossbauer results with other data sets enables a greater level of confidence in constraining mineralogy. This study provides a wealth of new data on Fe-bearing phosphate minerals to bolster future analyses of Mossbauer spectra acquired on Mars. C1 [Dyar, M. Darby; Jawin, Erica R.; Breves, Elly; Marchand, Gerard; Nelms, Melissa] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. [Lane, Melissa D.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Mertzman, Stanley A.] Franklin & Marshall Coll, Dept Earth & Environm, Lancaster, PA 17603 USA. [Bish, David L.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. [Bishop, Janice L.] NASA, SETI Inst, Ames Res Ctr, Mountain View, CA 94043 USA. RP Dyar, MD (reprint author), Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. EM mdyar@mtholyoke.edu FU NASA [NNX08AP42G]; NSF [MRI-0923224] FX We are grateful to Ed Cloutis, the Harvard Mineralogical Museum, and the NMNH for the loan of samples, and for support from NASA Grant NNX08AP42G. Student support for this project was provided by the Massachusetts Space Grant Consortium. We thank David Palmer for help with the CrystalMaker models. Mertzman salutes the NSF for award MRI-0923224, which enabled the purchase of PANalytical XRD system X'Pert PRO equipped with a 15 position sample changer used in this study. This is PSI Contribution Number 608. NR 257 TC 8 Z9 8 U1 5 U2 28 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD MAY-JUN PY 2014 VL 99 IS 5-6 BP 914 EP 942 DI 10.2138/am.2014.4701 PG 29 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AG7YE UT WOS:000335633900007 ER PT J AU McCollom, TM Ehlmann, BL Wang, A Hynek, BM Moskowitz, B Berquo, TS AF McCollom, Thomas M. Ehlmann, Bethany L. Wang, Alian Hynek, Brian M. Moskowitz, Bruce Berquo, Thelma S. TI Detection of iron substitution in natroalunite-natrojarosite solid solutions and potential implications for Mars SO AMERICAN MINERALOGIST LA English DT Article DE Mars; alunite group; visible/near infrared spectra; Raman spectra; hydrothermal; acid-sulfate alteration ID ACID-SULFATE ALTERATION; JAROSITE-GROUP; RAMAN-SPECTROSCOPY; CRYSTAL-CHEMISTRY; MERIDIANI-PLANUM; ALUNITE; MOSSBAUER; SPECTROMETER; MINERALS; HEMATITE AB Natroalunite containing substantial amounts of Fe occurs as a prominent secondary phase during acid-sulfate alteration of pyroclastic basalts in volcanic fumaroles in Nicaragua and elsewhere, and has been observed in laboratory simulations of acid-sulfate alteration as well. Reaction path models constrained by field and experimental observations predict that Fe-rich natroalunite should also form as a major secondary phase during alteration of martian basalt under similar circumstances. Here, we evaluate the potential to use spectroscopic methods to identify minerals from the alunite group with chemical compositions intermediate between natroalunite and natrojarosite on the surface of Mars, and to remotely infer their Fe contents. X-ray diffraction and spectroscopic measurements (Raman, visible/near infrared, mid-infrared, Mossbauer) were obtained for a suite of synthetic solid solutions with a range of Fe contents ranging from natroalunite to natrojarosite. In the visible/near infrared, minerals with intermediate compositions display several spectral features not evident in end-member spectra that could be used to remotely identify these minerals and infer their composition. In addition, Raman spectra, mid-infrared spectra, and X-ray diffraction peaks all show systematic variation with changing Fe content, indicating that these methods could potentially be used to infer mineral compositions as well. The results suggest that alunite group minerals with intermediate Fe compositions may be able to account for some visible/near-infrared and Mossbauer spectral features from Mars that had previously been unidentified or attributed to other phases. Overall, our findings indicate that consideration of solid solutions may lead to new identifications of alunite group minerals on the surface of Mars, and raise the possibility that minerals with compositions intermediate between natroalunite and natrojarosite may be widely distributed on the planet. C1 [McCollom, Thomas M.; Hynek, Brian M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Hynek, Brian M.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Ehlmann, Bethany L.] CALTECH, Pasadena, CA 91125 USA. [Ehlmann, Bethany L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wang, Alian] Washington Univ, Deptartment Earth & Planetary Sci, St Louis, MO 63130 USA. [Wang, Alian] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Moskowitz, Bruce] Univ Minnesota, Dept Earth Sci, Minneapolis, MN 55455 USA. [Moskowitz, Bruce] Univ Minnesota, Inst Rock Magnetism, Minneapolis, MN 55455 USA. [Berquo, Thelma S.] Concordia Coll, Dept Phys, Moorhead, MN 56562 USA. RP McCollom, TM (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. EM mccollom@lasp.colorado.edu RI Berquo, Thelma/D-6359-2013 FU NASA Mars Fundamental Research Program [NNX12AI02G, NNX10AM89G]; NASA Exobiology Award [NNX08AQ11G]; NASA Early Career Award [NNX12AF20G]; Instruments and Facilities Program, Division of Earth Science, National Science Foundation FX This research was supported by funds from NASA Mars Fundamental Research Program grants NNX12AI02G (T.M.M.) and NNX10AM89G (A.W.), NASA Exobiology Award NNX08AQ11G (T.M.M. and B.M.H.), and NASA Early Career Award NNX12AF20G (B.M.H.). Thanks to George Rossman for assistance and use of his FTIR spectrometer and to Frieder Klein for help with the Raman analysis of natural samples. The authors are grateful for reviews by Gregg Swayze and Stuart Mills, whose thoughtful comments helped to improve the manuscript. The Institute for Rock Magnetism is supported by grants from the Instruments and Facilities Program, Division of Earth Science, National Science Foundation. NR 53 TC 15 Z9 15 U1 3 U2 20 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD MAY-JUN PY 2014 VL 99 IS 5-6 BP 948 EP 964 DI 10.2138/am.2014.4617 PG 17 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AG7YE UT WOS:000335633900009 ER PT J AU Papike, JJ Burger, PV Bell, AS Shearer, CK Le, LA Jones, J Provencio, P AF Papike, James J. Burger, Paul V. Bell, Aaron S. Shearer, Charles K. Le, Loan Jones, John Provencio, Paula TI Valence state partitioning of V between pyroxene and melt for martian melt compositions Y 980459 and QUE 94201: The effect of pyroxene composition and crystal structure SO AMERICAN MINERALOGIST LA English DT Article DE Vanadium; partitioning; pyroxene; orthopyroxene; augite; pigeonite; EBSD; valence ID OXYGEN FUGACITY; UPPER-MANTLE; OLIVINE; BASALTS; MARS; PETROGENESIS; CONSTRAINTS; SILICATES; VANADIUM; SPINEL AB A martian basalt (Yamato 980459) composition was used to synthesize olivine, spinel, and pyroxene at 1200 degrees C at five oxygen fugacities: IW-1, IW, IW+1, IW+2, and QFM. The goal of this study is to examine the significant variation in the value of D-V(pyroxene/melt) with changing Wo content in pyroxene. While most literature on this subject relies on electron microprobe data that assumes that if the Wo component (CaSiO3) is <4 mol%, the pyroxene is in fact orthopyroxene, we've made a more robust identification of orthopyroxene using appropriate Kikuchi diffraction lines collected during electron backscatter diffraction analysis. We compare augite (Wo similar to 33), pigeonite (Wo similar to 13), orthopyroxene (Wo <4), and olivine. In augite (Wo similar to 33), the M2 site is 8-coordinated, while in pigeonite (Wo similar to 13), the site is 6-coordinated. The larger (8-coordinated) M2 site in augite requires structural expansion along the chain direction. The longer chain is enabled by the substitution of the larger Al for Si. The Al3+ substitution for Si4+ causes a charge deficiency that is made up, in part, by the substitution of V4+ and V3+ in the pyroxene M1 site. This rationale does not fully explain the dramatic decrease in D-V(orthopyroxene/melt). In monoclinic pyroxenes, the TOT stacking is characterized by + + + + (indicating the direction), a stacking pattern that produces a monoclinic offset. In orthopyroxene, the stacking is + + - -, which produces an orthorhombic structure. The M2 site is located between the reversed TOT units and is highly constrained to 6-coordination and thus cannot contain significant Ca that requires 8-coordination. Because the M2 site in orthopyroxene is small and constrained, it accommodates less Al in the tetrahedral chains and thus less V in the pyroxene M1 site. C1 [Papike, James J.; Burger, Paul V.; Bell, Aaron S.; Shearer, Charles K.; Provencio, Paula] Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Le, Loan] NASA Johnson Space Ctr, JSC Engn Technol & Sci JETS, Houston, TX 77058 USA. [Jones, John] NASA Johnson Space Ctr, Houston, TX 77058 USA. RP Papike, JJ (reprint author), Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. EM pvburger@unm.edu FU NASA Cosmochemistry program FX We acknowledge support for this research from the NASA Cosmochemistry program to Charles Shearer and John Jones. NR 19 TC 2 Z9 3 U1 0 U2 6 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD MAY-JUN PY 2014 VL 99 IS 5-6 BP 1175 EP 1178 DI 10.2138/am.2014.4788 PG 4 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AG7YE UT WOS:000335633900030 ER PT J AU Boening, C AF Boening, Carmen TI Detecting sea-level rise SO NATURE CLIMATE CHANGE LA English DT Editorial Material C1 CALTECH, Jet Prop Lab, Pasadena, CA 91104 USA. RP Boening, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91104 USA. EM carmen.boening@jpl.nasa.gov NR 8 TC 0 Z9 0 U1 2 U2 9 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X EI 1758-6798 J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD MAY PY 2014 VL 4 IS 5 BP 327 EP 328 PG 2 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AG4PV UT WOS:000335403500014 ER PT J AU Wang, Y Lee, KH Lin, Y Levy, M Zhang, RY AF Wang, Yuan Lee, Keun-Hee Lin, Yun Levy, Misti Zhang, Renyi TI Distinct effects of anthropogenic aerosols on tropical cyclones SO NATURE CLIMATE CHANGE LA English DT Article ID HURRICANES; ATLANTIC; INTENSITY; IMPACTS; MODEL AB Long-term observations have revealed large amplitude fluctuations in the frequency and intensity of tropical cyclones (TCs; refs 1-4), but the anthropogenic impacts, including greenhouse gases and particulate matter pollution(4,5), remain to be elucidated. Here, we show distinct aerosol effects on the development of TCs: the coupled microphysical and radiative effects of anthropogenic aerosols result in delayed development, weakened intensity and early dissipation, but an enlarged rainband and increased precipitation under polluted conditions. Our results imply that anthropogenic aerosols probably exhibit an opposite effect to that of greenhouse gases, highlighting the necessity of incorporating a realistic microphysical-radiative interaction of aerosols for accurate forecasting and climatic prediction of TCs in atmospheric models. C1 [Wang, Yuan; Lee, Keun-Hee; Lin, Yun; Levy, Misti; Zhang, Renyi] Texas A&M Univ, Dept Atmospher Sci, Ctr Atmospher Chem & Environm, College Stn, TX 77843 USA. [Wang, Yuan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lee, Keun-Hee] Korean Meteorol Adm, Seoul 156720, South Korea. [Zhang, Renyi] Peking Univ, Coll Environm Sci & Engn, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100871, Peoples R China. RP Wang, Y (reprint author), Texas A&M Univ, Dept Atmospher Sci, Ctr Atmospher Chem & Environm, College Stn, TX 77843 USA. EM Yuan.Wang@jpl.nasa.gov; renyi-zhang@geos.tamu.edu RI Levy, Misti/G-8660-2014; Lin, Yun/B-1906-2013; Zhang, Renyi/A-2942-2011; OI Levy, Misti/0000-0002-4832-7753; Lin, Yun/0000-0001-8222-0346 FU NASA; Ministry of Science and Technology of China [2013CB955800] FX Y.W. was supported by a NASA graduate fellowship in Earth Sciences. R.Z. acknowledges support from the Ministry of Science and Technology of China under award number 2013CB955800. We thank K.. Emanuel, P. Liss, C. Schumacher and F. Zhang for helpful discussions. Supercomputing computational facilities were provided by the Texas A&M University. Y.W. acknowledges additional support by the NASA ROSES COUND program at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 33 TC 17 Z9 17 U1 4 U2 36 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X EI 1758-6798 J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD MAY PY 2014 VL 4 IS 5 BP 368 EP 373 DI 10.1038/NCLIMATE2144 PG 6 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AG4PV UT WOS:000335403500025 ER PT J AU Keppenne, CL AF Keppenne, Christian L. TI An ensemble recentering Kalman filter with an application to Argo temperature data assimilation into the NASA GEOS-5 coupled model SO OCEAN MODELLING LA English DT Article DE Data assimilation; Kalman filter; Ensemble Kalman filter; Particle filter; Coupled data assimilation ID QUASI-GEOSTROPHIC MODEL; ALTIMETER DATA AB A two-step ensemble recentering Kalman filter (ERKF) analysis scheme is introduced. The algorithm consists of a recentering step followed by an ensemble Kalman filter (EnKF) analysis step. The recentering step is formulated such as to adjust the prior distribution of an ensemble of model states so that the deviations of individual samples from the sample mean are unchanged but the original sample mean is shifted to the prior position of the most likely particle, where the likelihood of each particle is measured in terms of closeness to the assimilated observations. The computational cost of the ERKF is essentially the same as that of a same size EnKF. The ERKF is applied to the assimilation of Argo temperature profiles into the OGCM component of an ensemble of NASA GEOS-5 coupled models. Unassimilated Argo salt data are used for validation. These data serve as a proxy to assess the potential of the ERKF to improve estimates of unobserved model variables. A surprisingly small number (16) of model trajectories is sufficient to significantly improve model estimates of salinity over estimates from an ensemble run without assimilation. The two-step algorithm also performs better than the EnKF although its performance is degraded in poorly observed regions. The efficacy of the recentering is attributed to its ability to preserve balance relationships between observed and unobserved variables, even when the ensemble size is too small for the EnKF to accurately estimate cross-field error covariances. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Keppenne, Christian L.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Keppenne, Christian L.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. RP Keppenne, CL (reprint author), NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA. EM christian.keppenne@nasa.gov FU NASA's Modeling Analysis and Prediction Program [WBS 802678.02.17.01.25] FX This work is supported by NASA's Modeling Analysis and Prediction Program under WBS 802678.02.17.01.25. The infrastructure for the runs is provided by the NASA Center for Climate Simulation (NCCS). Yuri Vikhliaev, Max Suarez and Bin Zhao helped configure the GEOS-5 modeling system. Guillaume Vernieres helped configure the data assimilation system and Robin Kovach assisted with the observation preprocessing and with plotting the results. Eugenia Kalnay, Michele Rienecker and two insightful anonymous reviewers helped interpreting the results and improve the initial draft manuscript. NR 14 TC 2 Z9 2 U1 0 U2 6 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1463-5003 EI 1463-5011 J9 OCEAN MODEL JI Ocean Model. PD MAY PY 2014 VL 77 BP 50 EP 55 DI 10.1016/j.ocemod.2014.03.001 PG 6 WC Meteorology & Atmospheric Sciences; Oceanography SC Meteorology & Atmospheric Sciences; Oceanography GA AG9MT UT WOS:000335744100004 ER PT J AU Mishchenko, MI Liu, L Cairns, B Mackowski, DW AF Mishchenko, Michael I. Liu, Li Cairns, Brian Mackowski, Daniel W. TI Optics of water cloud droplets mixed with black-carbon aerosols SO OPTICS LETTERS LA English DT Article ID T-MATRIX; SOLAR-RADIATION; SCATTERING; ABSORPTION; INCLUSIONS; PARTICLES AB We use the recently extended superposition T-matrix method to calculate scattering and absorption properties of micrometer-sized water droplets contaminated by black carbon. Our numerically exact results reveal that, depending on the mode of soot-water mixing, the soot specific absorption can vary by a factor exceeding 6.5. The specific absorption is maximized when the soot material is quasi-uniformly distributed throughout the droplet interior in the form of numerous small monomers. The range of mixing scenarios captured by our computations implies a wide range of remote sensing and radiation budget implications of the presence of black carbon in liquid-water clouds. We show that the popular Maxwell-Garnett effective-medium approximation can be used to calculate the optical cross sections, single-scattering albedo, and asymmetry parameter for the quasi-uniform mixing scenario, but is likely to fail in application to other mixing scenarios and in computations of the elements of the scattering matrix. (C) 2014 Optical Society of America C1 [Mishchenko, Michael I.; Liu, Li; Cairns, Brian] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Liu, Li] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. [Mackowski, Daniel W.] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA. RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM michael.i.mishchenko@nasa.gov RI Mishchenko, Michael/D-4426-2012; Mackowski, Daniel/K-1917-2013; OI Cairns, Brian/0000-0002-1980-1022 NR 21 TC 17 Z9 17 U1 4 U2 19 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 EI 1539-4794 J9 OPT LETT JI Opt. Lett. PD MAY 1 PY 2014 VL 39 IS 9 BP 2607 EP 2610 DI 10.1364/OL.39.002607 PG 4 WC Optics SC Optics GA AG5YX UT WOS:000335496400020 PM 24784057 ER PT J AU Aartsen, MG Abbasi, R Ackermann, M Adams, J Aguilar, JA Ahlers, M Altmann, D Arguelles, C Arlen, TC Auffenberg, J Bai, X Baker, M Barwick, SW Baum, V Bay, R Beatty, JJ Tjus, JB Becker, KH BenZvi, S Berghaus, P Berley, D Bernardini, E Bernhard, A Besson, DZ Binder, G Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bose, D Boser, S Botner, O Brayeur, L Bretz, HP Brown, AM Bruijn, R Casey, J Casier, M Chirkin, D Christov, A Christy, B Clark, K Classen, L Clevermann, F Coenders, S Cohen, S Cowen, DF Silva, AHC Danninger, M Daughhetee, J Davis, JC Day, M de Andre, JPAM De Clercq, C De Ridder, S Desiati, P de Vries, KD de With, M DeYoung, T Diaz-Velez, JC Dunkman, M Eagan, R Eberhardt, B Eichmann, B Eisch, J Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feintzeig, J Feusels, T Filimonov, K Finley, C Fischer-Wasels, T Flis, S Franckowiak, A Frantzen, K Fuchs, T Gaisser, TK Gallagher, J Gerhardt, L Gladstone, L Glusenkamp, T Goldschmidt, A Golup, G Gonzalez, JG Goodman, JA Gora, D Grandmont, DT Grant, D Gretskov, P Groh, JC Gross, A Ha, C Ismail, AH Hallen, P Hallgren, A Halzen, F Hanson, K Hebecker, D Heereman, D Heinen, D Helbing, K Hellauer, R Hickford, S Hill, GC Hoffman, KD Hoffmann, R Homeier, A Hoshina, K Huang, F Huelsnitz, W Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobi, E Jacobsen, J Jagielski, K Japaridze, GS Jero, K Jlelati, O Kaminsky, B Kappes, A Karg, T Karle, A Kauer, M Kelley, JL Kiryluk, J Klas, J Klein, SR Kohne, JH Kohnen, G Kolanoski, H Kopke, L Kopper, C Kopper, S Koskinen, DJ Kowalski, M Krasberg, M Kriesten, A Krings, K Kroll, G Kunnen, J Kurahashi, N Kuwabara, T Labare, M Landsman, H Larson, MJ Lesiak-Bzdak, M Leuermann, M Leute, J Lunemann, J Macias, O Madsen, J Maggi, G Maruyama, R Mase, K Matis, HS McNally, F Meagher, K Merck, M Meures, T Miarecki, S Middell, E Milke, N Miller, J Mohrmann, L Montaruli, T Morse, R Nahnhauer, R Naumann, U Niederhausen, H Nowicki, SC Nygren, DR Obertacke, A Odrowski, S Olivas, A Omairat, A O'Murchadha, A Palczewski, T Paul, L Pepper, JA de los Heros, CP Pfendner, C Pieloth, D Pinat, E Posselt, J Price, PB Przybylski, GT Quinnan, M Radel, L Rameez, M Rawlins, K Redl, P Reimann, R Resconi, E Rhode, W Ribordy, M Richman, M Riedel, B Robertson, S Rodrigues, JP Rott, C Ruhe, T Ruzybayev, B Ryckbosch, D Saba, SM Sander, HG Santander, M Sarkar, S Schatto, K Scheriau, F Schmidt, T Schmitz, M Schoenen, S Schoneberg, S Schonwald, A Schukraft, A Schulte, L Schulz, O Seckel, D Sestayo, Y Seunarine, S Shanidze, R Sheremata, C Smith, MWE Soldin, D Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stanisha, NA Stasik, A Stezelberger, T Stokstad, RG Stossl, A Strahler, EA Strom, R Strotjohann, NL Sullivan, GW Taavola, H Taboada, I Tamburro, A Tepe, A Ter-Antonyan, S Tesic, G Tilav, S Toale, PA Tobin, MN Toscano, S Tselengidou, M Unger, E Usner, M Vallecorsa, S van Eijndhoven, N Van Overloop, A van Santen, J Vehring, M Voge, M Vraeghe, M Walck, C Waldenmaier, T Wallraff, M Weaver, C Wellons, M Wendt, C Westerhoff, S Whelan, B Whitehorn, N Wiebe, K Wiebusch, CH Williams, DR Wissing, H Wolf, M Wood, TR Woschnagg, K Xu, DL Xu, XW Yanez, JP Yodh, G Yoshida, S Zarzhitsky, P Ziemann, J Zierke, S Zoll, M AF Aartsen, M. G. Abbasi, R. Ackermann, M. Adams, J. Aguilar, J. A. Ahlers, M. Altmann, D. Arguelles, C. Arlen, T. C. Auffenberg, J. Bai, X. Baker, M. Barwick, S. W. Baum, V. Bay, R. Beatty, J. J. Tjus, J. Becker Becker, K. -H. BenZvi, S. Berghaus, P. Berley, D. Bernardini, E. Bernhard, A. Besson, D. Z. Binder, G. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bose, D. Boeser, S. Botner, O. Brayeur, L. Bretz, H. -P. Brown, A. M. Bruijn, R. Casey, J. Casier, M. Chirkin, D. Christov, A. Christy, B. Clark, K. Classen, L. Clevermann, F. Coenders, S. Cohen, S. Cowen, D. F. Silva, A. H. Cruz Danninger, M. Daughhetee, J. Davis, J. C. Day, M. de Andre, J. P. A. M. De Clercq, C. De Ridder, S. Desiati, P. de Vries, K. D. de With, M. DeYoung, T. Diaz-Velez, J. C. Dunkman, M. Eagan, R. Eberhardt, B. Eichmann, B. Eisch, J. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feintzeig, J. Feusels, T. Filimonov, K. Finley, C. Fischer-Wasels, T. Flis, S. Franckowiak, A. Frantzen, K. Fuchs, T. Gaisser, T. K. Gallagher, J. Gerhardt, L. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Golup, G. Gonzalez, J. G. Goodman, J. A. Gora, D. Grandmont, D. T. Grant, D. Gretskov, P. Groh, J. C. Gross, A. Ha, C. Ismail, A. Haj Hallen, P. Hallgren, A. Halzen, F. Hanson, K. Hebecker, D. Heereman, D. Heinen, D. Helbing, K. Hellauer, R. Hickford, S. Hill, G. C. Hoffman, K. D. Hoffmann, R. Homeier, A. Hoshina, K. Huang, F. Huelsnitz, W. Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jacobi, E. Jacobsen, J. Jagielski, K. Japaridze, G. S. Jero, K. Jlelati, O. Kaminsky, B. Kappes, A. Karg, T. Karle, A. Kauer, M. Kelley, J. L. Kiryluk, J. Klaes, J. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koepke, L. Kopper, C. Kopper, S. Koskinen, D. J. Kowalski, M. Krasberg, M. Kriesten, A. Krings, K. Kroll, G. Kunnen, J. Kurahashi, N. Kuwabara, T. Labare, M. Landsman, H. Larson, M. J. Lesiak-Bzdak, M. Leuermann, M. Leute, J. Luenemann, J. Macias, O. Madsen, J. Maggi, G. Maruyama, R. Mase, K. Matis, H. S. McNally, F. Meagher, K. Merck, M. Meures, T. Miarecki, S. Middell, E. Milke, N. Miller, J. Mohrmann, L. Montaruli, T. Morse, R. Nahnhauer, R. Naumann, U. Niederhausen, H. Nowicki, S. C. Nygren, D. R. Obertacke, A. Odrowski, S. Olivas, A. Omairat, A. O'Murchadha, A. Palczewski, T. Paul, L. Pepper, J. A. Perez de los Heros, C. Pfendner, C. Pieloth, D. Pinat, E. Posselt, J. Price, P. B. Przybylski, G. T. Quinnan, M. Raedel, L. Rameez, M. Rawlins, K. Redl, P. Reimann, R. Resconi, E. Rhode, W. Ribordy, M. Richman, M. Riedel, B. Robertson, S. Rodrigues, J. P. Rott, C. Ruhe, T. Ruzybayev, B. Ryckbosch, D. Saba, S. M. Sander, H. -G. Santander, M. Sarkar, S. Schatto, K. Scheriau, F. Schmidt, T. Schmitz, M. Schoenen, S. Schoeneberg, S. Schoenwald, A. Schukraft, A. Schulte, L. Schulz, O. Seckel, D. Sestayo, Y. Seunarine, S. Shanidze, R. Sheremata, C. Smith, M. W. E. Soldin, D. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stanisha, N. A. Stasik, A. Stezelberger, T. Stokstad, R. G. Stossl, A. Strahler, E. A. Strom, R. Strotjohann, N. L. Sullivan, G. W. Taavola, H. Taboada, I. Tamburro, A. Tepe, A. Ter-Antonyan, S. Tesic, G. Tilav, S. Toale, P. A. Tobin, M. N. Toscano, S. Tselengidou, M. Unger, E. Usner, M. Vallecorsa, S. van Eijndhoven, N. Van Overloop, A. van Santen, J. Vehring, M. Voge, M. Vraeghe, M. Walck, C. Waldenmaier, T. Wallraff, M. Weaver, Ch Wellons, M. Wendt, C. Westerhoff, S. Whelan, B. Whitehorn, N. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wissing, H. Wolf, M. Wood, T. R. Woschnagg, K. Xu, D. L. Xu, X. W. Yanez, J. P. Yodh, G. Yoshida, S. Zarzhitsky, P. Ziemann, J. Zierke, S. Zoll, M. CA IceCube Collaboration TI Search for neutrino-induced particle showers with IceCube-40 SO PHYSICAL REVIEW D LA English DT Article ID SCATTERING; SELECTION; CASCADES; SPECTRUM; AMANDA; SYSTEM; MODEL; ICE AB We report on the search for neutrino-induced particle showers, so-called cascades, in the IceCube-40 detector. The data for this search were collected between April 2008 and May 2009 when the first 40 IceCube strings were deployed and operational. Three complementary searches were performed, each optimized for different energy regimes. The analysis with the lowest energy threshold (2 TeV) targeted atmospheric neutrinos. A total of 67 events were found, consistent with the expectation of 41 atmospheric muons and 30 atmospheric neutrino events. The two other analyses targeted a harder, astrophysical neutrino flux. The analysis with an intermediate threshold of 25 TeV leads to the observation of 14 cascadelike events, again consistent with the prediction of 3.0 atmospheric neutrino and 7.7 atmospheric muon events. We hence set an upper limit of E-2 Phi(lim) <= 7.46 x 10(-8) GeV sr(-1) s(-1) cm(-2) (90% C.L.) on the diffuse flux from astrophysical neutrinos of all neutrino flavors, applicable to the energy range 25 TeV to 5 PeV, assuming an E-nu(-2) spectrum and a neutrino flavor ratio of 1: 1: 1 at the Earth. The third analysis utilized a larger and optimized sample of atmospheric muon background simulation, leading to a higher energy threshold of 100 TeV. Three events were found over a background prediction of 0.04 atmospheric muon events and 0.21 events from the flux of conventional and prompt atmospheric neutrinos. Including systematic errors this corresponds to a 2.7 sigma excess with respect to the background-only hypothesis. Our observation of neutrino event candidates above 100 TeV complements IceCube's recently observed evidence for high-energy astrophysical neutrinos. C1 [Bissok, M.; Blumenthal, J.; Coenders, S.; Euler, S.; Gretskov, P.; Hallen, P.; Heinen, D.; Jagielski, K.; Kriesten, A.; Krings, K.; Leuermann, M.; Paul, L.; Raedel, L.; Reimann, R.; Schoenen, S.; Schukraft, A.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.; Zierke, S.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Aartsen, M. G.; Hill, G. C.; Robertson, S.; Whelan, B.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Bay, R.; Binder, G.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Binder, G.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [de With, M.; Kolanoski, H.; Waldenmaier, T.] Univ Berlin, Inst Phys, D-12489 Berlin, Germany. [Tjus, J. Becker; Eichmann, B.; Fedynitch, A.; Saba, S. M.; Schoeneberg, S.; Unger, E.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany. [Boeser, S.; Franckowiak, A.; Hebecker, D.; Homeier, A.; Kowalski, M.; Schulte, L.; Stasik, A.; Strotjohann, N. L.; Usner, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.; Pinat, E.] Univ Libre Brussels, Sci Fac CP230, B-1050 Brussels, Belgium. [Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; Golup, G.; Kunnen, J.; Maggi, G.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Adams, J.; Brown, A. M.; Hickford, S.; Macias, O.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Berley, D.; Blaufuss, E.; Christy, B.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Koskinen, D. J.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Clevermann, F.; Frantzen, K.; Fuchs, T.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.; Scheriau, F.; Schmitz, M.; Ziemann, J.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany. [Grandmont, D. T.; Grant, D.; Nowicki, S. C.; Odrowski, S.; Sheremata, C.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Altmann, D.; Classen, L.; Gora, D.; Kappes, A.; Tselengidou, M.] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91054 Erlangen, Germany. [Aguilar, J. A.; Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland. [De Ridder, S.; Feusels, T.; Ismail, A. Haj; Jlelati, O.; Labare, M.; Ryckbosch, D.; Van Overloop, A.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium. [Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bruijn, R.; Cohen, S.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Abbasi, R.; Ahlers, M.; Arguelles, C.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Tobin, M. N.; Toscano, S.; van Santen, J.; Weaver, Ch; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Abbasi, R.; Ahlers, M.; Arguelles, C.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Tobin, M. N.; Toscano, S.; van Santen, J.; Weaver, Ch; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA. [Baum, V.; Eberhardt, B.; Koepke, L.; Kroll, G.; Luenemann, J.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Bernhard, A.; Gross, A.; Leute, J.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany. [Bai, X.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bai, X.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Bose, D.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea. [Clark, K.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Larson, M. J.; Palczewski, T.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Arlen, T. C.; Boersma, D. J.; Cowen, D. F.; de Andre, J. P. A. M.; DeYoung, T.; Dunkman, M.; Eagan, R.; Groh, J. C.; Huang, F.; Quinnan, M.; Smith, M. W. E.; Stanisha, N. A.; Tesic, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Botner, O.; Hallgren, A.; Perez de los Heros, C.; Strom, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Helbing, K.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Omairat, A.; Posselt, J.; Soldin, D.; Tepe, A.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Ackermann, M.; Berghaus, P.; Bernardini, E.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Jacobi, E.; Kaminsky, B.; Karg, T.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Shanidze, R.; Spiering, C.; Stossl, A.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany. [Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hickford, S (reprint author), Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch 1, New Zealand. EM stephanie.v.hickford@gmail.com; eike.middell@desy.de RI Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011; Wiebusch, Christopher/G-6490-2012; Tjus, Julia/G-8145-2012; Koskinen, David/G-3236-2014; Auffenberg, Jan/D-3954-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015; Taavola, Henric/B-4497-2011; OI Maruyama, Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Wiebusch, Christopher/0000-0002-6418-3008; Rott, Carsten/0000-0002-6958-6033; Ter-Antonyan, Samvel/0000-0002-5788-1369; Schukraft, Anne/0000-0002-9112-5479; Groh, John/0000-0001-9880-3634; Koskinen, David/0000-0002-0514-5917; Auffenberg, Jan/0000-0002-1185-9094; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Taavola, Henric/0000-0002-2604-2810; Perez de los Heros, Carlos/0000-0002-2084-5866; Strotjohann, Nora Linn/0000-0002-4667-6730; Arguelles Delgado, Carlos/0000-0003-4186-4182 FU U.S. National Science Foundation-Office of Polar Programs; U.S. National Science Foundation-Physics Division; University of Wisconsin Alumni Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison; Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy; National Energy Research Scientific Computing Center; Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada; WestGrid and Compute/Calcul Canada; Swedish Research Council; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC),; Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Helmholtz Alliance for Astroparticle Physics (HAP); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute to encourage scientific and technological research in industry (IWT); Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Danish National Research Foundation, Denmark (DNRF) FX We acknowledge the support from the following agencies: U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada, WestGrid and Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Danish National Research Foundation, Denmark (DNRF) NR 58 TC 17 Z9 17 U1 0 U2 8 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 MAY 1 PY 2014 VL 89 IS 10 AR 102001 DI 10.1103/PhysRevD.89.102001 PG 20 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AG6LZ UT WOS:000335531400002 ER PT J AU de Putter, R Linder, EV Mishra, A AF de Putter, Roland Linder, Eric V. Mishra, Abhilash TI Inflationary freedom and cosmological neutrino constraints SO PHYSICAL REVIEW D LA English DT Article ID PRIMORDIAL POWER SPECTRUM; OSCILLATION SPECTROSCOPIC SURVEY; MICROWAVE-ANISOTROPY-PROBE; COSMIC INVERSION METHOD; SOUTH-POLE TELESCOPE; DIGITAL SKY SURVEY; SDSS-III; BACKGROUND ANISOTROPIES; WMAP OBSERVATIONS; DATA RELEASE AB The most stringent bounds on the absolute neutrino mass scale come from cosmological data. These bounds are made possible because massive relic neutrinos affect the expansion history of the universe and lead to a suppression of matter clustering on scales smaller than the associated free streaming length. However, the resulting effect on cosmological perturbations is relative to the primordial power spectrum of density perturbations from inflation, so freedom in the primordial power spectrum affects neutrino mass constraints. Using measurements of the cosmic microwave background (CMB), the galaxy power spectrum and the Hubble constant, we constrain neutrino mass and number of species for a model-independent primordial power spectrum. Describing the primordial power spectrum by a 20-node spline, we find that the neutrino mass upper limit is a factor 3 weaker than when a power law form is imposed, if only CMB data are used. The primordial power spectrum itself is constrained to better than 10% in the wave vector range k approximate to 0.01 - 0.25 Mpc(-1). Galaxy clustering data and a determination of the Hubble constant play a key role in reining in the effects of inflationary freedom on neutrino constraints. The inclusion of both eliminates the inflationary freedom degradation of the neutrino mass bound, giving for the sum of neutrino masses Sigma m(nu) < 0.18 eV (at 95% confidence level, Planck + BOSS + H-0), approximately independent of the assumed primordial power spectrum model. When allowing for a free effective number of species, N-eff, the joint constraints on Sigma m(nu) and N-eff are loosened by a factor 1.7 when the power law form of the primordial power spectrum is abandoned in favor of the spline parametrization. C1 [de Putter, Roland] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [de Putter, Roland; Mishra, Abhilash] CALTECH, Pasadena, CA 91125 USA. [Linder, Eric V.] Univ Calif Berkeley, Berkeley Lab, Berkeley, CA 94720 USA. [Linder, Eric V.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Linder, Eric V.] Ewha Womans Univ, Inst Early Universe WCU, Seoul 120750, South Korea. RP de Putter, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU NASA ATP [11-ATP090]; DOE Grant [DE-SC-0007867]; Director, Office of Science, Office of High Energy Physics; U.S. Department of Energy [DE-AC02-05CH11231]; Korea World Class University [R32-2009-000-10130-0] FX We thank Olga Mena for her assistance with the galaxy power spectrum likelihood code and Jan Hamann for useful discussion regarding Appendix B. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This work is supported by NASA ATP Grant No. 11-ATP090, DOE Grant No. DE-SC-0007867, and the Director, Office of Science, Office of High Energy Physics, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, and by Korea World Class University Grant No. R32-2009-000-10130-0. R. d. P. thanks the Institute for the Early Universe at Ewha University, Seoul, where part of this work was performed, for its hospitality. NR 68 TC 14 Z9 14 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD MAY 1 PY 2014 VL 89 IS 10 AR 103502 DI 10.1103/PhysRevD.89.103502 PG 17 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AG6LZ UT WOS:000335531400005 ER PT J AU Min, JB Xue, D Shi, Y AF Min, J. B. Xue, D. Shi, Y. TI Micromechanics modeling for fatigue damage analysis designed for fabric reinforced ceramic matrix composites SO COMPOSITE STRUCTURES LA English DT Article DE Three-phase micromechanics; Shear-lag; Fracture mechanics; Damage progression; Fatigue failure; Fabric reinforced composite structures ID FIBER; FRACTURE; FAILURE AB A micromechanics analysis modeling method was developed to analyze the damage progression and fatigue failure of fabric reinforced composite structures, especially for the brittle ceramic matrix material composites. A repeating unit cell concept of fabric reinforced composites was used to represent the global composite structure. The thermal and mechanical properties of the repeating unit cell were considered as the same as those of the global composite structure. The three-phase micromechanics, the shear-lag, and the continuum fracture mechanics models were integrated with a statistical model in the repeating unit cell to predict the progressive damages and fatigue life of the composite structures. The global structure failure was defined as the loss of loading capability of the repeating unit cell, which depends on the stiffness reduction due to material slice failures and nonlinear material properties in the repeating unit cell. The present methodology is demonstrated with the analysis results evaluated through the experimental test performed with carbon fiber reinforced silicon carbide matrix plain weave composite specimens. Published by Elsevier Ltd. C1 [Min, J. B.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Xue, D.; Shi, Y.] Analyt Serv & Mat Inc, Hampton, VA 23666 USA. RP Min, JB (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA. EM James.B.Min@nasa.gov FU NASA Fundamental Aeronautics Research Fixed Wing Project FX The first author gratefully acknowledges the support by NASA Fundamental Aeronautics Research Fixed Wing Project to prepare this paper. NR 25 TC 4 Z9 6 U1 2 U2 19 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 MAY PY 2014 VL 111 BP 213 EP 223 DI 10.1016/j.compstruct.2013.12.025 PG 11 WC Materials Science, Composites SC Materials Science GA AG5VN UT WOS:000335486900021 ER PT J AU Liu, Z Ostrenga, D Teng, W Kempler, S Milich, L AF Liu, Zhong Ostrenga, Dana Teng, William Kempler, Steven Milich, Lenard TI Developing GIOVANNI-based online prototypes to intercompare TRMM-related global gridded-precipitation products SO COMPUTERS & GEOSCIENCES LA English DT Article DE Precipitation; Satellite remote sensing; Intercomparison; Uncertainty; TRMM; Online tools ID TROPICAL RAINFALL; PASSIVE MICROWAVE; ORBIT BOOST; SATELLITE; SYSTEM; VISUALIZATION; VALIDATION; RESOLUTION; ALGORITHM; INFORMATION AB New online prototypes have been developed to extend and enhance the previous effort by facilitating investigation of product characteristics and intercomparison of precipitation products in different algorithms as well as in different versions at different spatial scales ranging from local to global without downloading data and software. Several popular Tropical Rainfall Measuring Mission (TRMM) products and the TRMM Composite Climatology are included. In addition, users can download customized data in several popular formats for further analysis. Examples show product quality problems and differences in several monthly precipitation products. It is seen that differences in daily and monthly precipitation products are distributed unevenly in space and it is necessary to have tools such as those presented here for customized and detailed investigations. A simple time series and two area maps allow the discovery of abnormal values of 3A25 in one of the months. An example shows a V-shaped valley issue in the Version 6 3B43 time series and another example shows a sudden drop in 3A25 monthly rain rate, all of which provide important information when the products are used for long-term trend studies. Future plans include adding more products and statistical functionality in the prototypes. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Liu, Zhong; Ostrenga, Dana; Teng, William; Kempler, Steven] NASA Goddard Space Flight Ctr, Goddard Earth Sci Data & Informat Serv Ctr GES DI, Greenbelt, MD 20771 USA. [Liu, Zhong] George Mason Univ, CSISS, Fairfax, VA 22030 USA. [Ostrenga, Dana; Teng, William] ADNET Syst Inc, Rockville, MD USA. [Milich, Lenard] Univ Arizona, Tucson, AZ 85721 USA. RP Liu, Z (reprint author), NASA Goddard Space Flight Ctr, Goddard Earth Sci Data & Informat Serv Ctr GES DI, Code 610-2, Greenbelt, MD 20771 USA. EM Zhong.Liu@nasa.gov FU NASA Research Opportunities in Space and Earth Science (ROSES); NASA GES DISC; Earth System Data Records Uncertainty Analysis; [NNH10ZDA001N-ESDRERR] FX This project is supported by NASA Research Opportunities in Space and Earth Science-2010 (ROSES-2010), NNH10ZDA001N-ESDRERR, Appendix A32: "Earth System Data Records Uncertainty Analysis" and the NASA GES DISC. Special thanks to the GIOVANNI development team and Dr. Jianfu Pan for providing the details about the Giovanni infrastructure. Thanks extend to Drs. Robert Adler and Jian-Jian Wang for providing the TCC products and the description and participating in the tool development The authors would like to thank three anonymous reviewers for their constructive comments, which have much improved the manuscript NR 29 TC 7 Z9 7 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0098-3004 EI 1873-7803 J9 COMPUT GEOSCI-UK JI Comput. Geosci. PD MAY PY 2014 VL 66 BP 168 EP 181 DI 10.1016/j.cageo.2013.12.012 PG 14 WC Computer Science, Interdisciplinary Applications; Geosciences, Multidisciplinary SC Computer Science; Geology GA AG3CP UT WOS:000335293700016 ER PT J AU Duan, L Choudhari, MM Wu, MW AF Duan, Lian Choudhari, Meelan M. Wu, Minwei TI Numerical study of acoustic radiation due to a supersonic turbulent boundary layer SO JOURNAL OF FLUID MECHANICS LA English DT Article DE aeroacoustics; turbulent boundary layers; turbulence simulation ID WALL-PRESSURE-FLUCTUATIONS; CHANNEL FLOW; REYNOLDS-NUMBER; SHEAR FLOWS; SIMULATION; TRANSITION; FIELD; BENEATH; NOISE; RECEPTIVITY AB Direct numerical simulations are used to examine the pressure fluctuations generated by fully developed turbulence in a Mach 2.5 turbulent boundary layer, with an emphasis on the acoustic fluctuations radiated into the free stream. Single-and multi-point statistics of computed surface pressure fluctuations show good agreement with measurements and numerical simulations at similar flow conditions. Consistent with spark shadowgraphs obtained in free flight, the quasi-homogeneous acoustic near field in the free-stream region consists of randomly spaced wavepackets with a finite spatial coherence. The free-stream pressure fluctuations exhibit important differences from the surface pressure fluctuations in amplitude, frequency content and convection speeds. Such information can be applied towards improved modelling of boundary layer receptivity in conventional supersonic facilities and, hence, enable a better utilization of transition data acquired in such wind tunnels. The predicted acoustic characteristics are compared with the limited available measurements. Finally, the numerical database is used to understand the acoustic source mechanisms, with the finding that the supersonically convecting eddies that can directly radiate to the free stream are confined to the buffer zone within the boundary layer. C1 [Duan, Lian] Missouri Univ Sci & Technol, Rolla, MO 65409 USA. [Choudhari, Meelan M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Wu, Minwei] Natl Inst Aerosp, Hampton, VA 23666 USA. RP Duan, L (reprint author), Missouri Univ Sci & Technol, Rolla, MO 65409 USA. EM duanl@mst.edu RI Choudhari, Meelan/F-6080-2017 OI Choudhari, Meelan/0000-0001-9120-7362 NR 62 TC 2 Z9 2 U1 1 U2 23 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-1120 EI 1469-7645 J9 J FLUID MECH JI J. Fluid Mech. PD MAY PY 2014 VL 746 BP 165 EP 192 DI 10.1017/jfm.2014.116 PG 28 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA AG4IW UT WOS:000335384200012 ER PT J AU Joshi, SM Gonzalez, OR Upchurch, JM AF Joshi, Suresh M. Gonzalez, Oscar R. Upchurch, Jason M. TI Identifiability of Additive Actuator and Sensor Faults by State Augmentation SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article C1 [Joshi, Suresh M.; Upchurch, Jason M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Gonzalez, Oscar R.] Old Dominion Univ, Dept Elect & Comp Engn, Norfolk, VA 23529 USA. RP Joshi, SM (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM suresh.m.joshi@nasa.gov; ogonzale@odu.edu; jason.m.upchurch@nasa.gov FU Copyright Clearance Center, Inc. FX This material is declared a work of the U.S. Government and is not subject to copyright protection in the United States. Copies of this paper may be made for personal or internal use, on condition that the copier pay the $ 10.00 per-copy fee to the Copyright Clearance Center, Inc., 222 Rosewood Drive, Danvers, MA 01923; include the code 1533-3884/14 and $ 10.00 in correspondence with the CCC. NR 11 TC 1 Z9 1 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD MAY-JUN PY 2014 VL 37 IS 3 BP 941 EP 946 DI 10.2514/1.62523 PG 6 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA AG4NT UT WOS:000335397700021 ER PT J AU Neichel, B Rigaut, F Vidal, F van Dam, MA Garrel, V Carrasco, ER Pessev, P Winge, C Boccas, M d'Orgeville, C Arriagada, G Serio, A Fesquet, V Rambold, WN Luhrs, J Moreno, C Gausachs, G Galvez, RL Montes, V Vucina, TB Marin, E Urrutia, C Lopez, A Diggs, SJ Marchant, C Ebbers, AW Trujillo, C Bec, M Trancho, G McGregor, P Young, PJ Colazo, F Edwards, ML AF Neichel, Benoit Rigaut, Francois Vidal, Fabrice van Dam, Marcos A. Garrel, Vincent Rodrigo Carrasco, Eleazar Pessev, Peter Winge, Claudia Boccas, Maxime d'Orgeville, Celine Arriagada, Gustavo Serio, Andrew Fesquet, Vincent Rambold, William N. Luehrs, Javier Moreno, Cristian Gausachs, Gaston Galvez, Ramon L. Montes, Vanessa Vucina, Tomislav B. Marin, Eduardo Urrutia, Cristian Lopez, Ariel Diggs, Sarah J. Marchant, Claudio Ebbers, Angelic W. Trujillo, Chadwick Bec, Matthieu Trancho, Gelys McGregor, Peter Young, Peter J. Colazo, Felipe Edwards, Michelle L. TI Gemini multiconjugate adaptive optics system review - II. Commissioning, operation and overall performance SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: adaptive optics; instrumentation: high angular resolution; telescopes ID LASER-GUIDE-STAR; CENTROID GAIN; BLACK-HOLE; FIELD; GALAXIES; SOUTH; COMPENSATION; MITIGATION; TELESCOPES; DYNAMICS AB The Gemini multiconjugate adaptive optics system - GeMS, a facility instrument mounted on the Gemini South telescope, delivers a uniform, near diffraction limited images at near-infrared wavelengths (0.95-2.5 mu m) over a field of view of 120 arcsec. GeMS is the first sodium layer based multilaser guide star adaptive optics system used in astronomy. It uses five laser guide stars distributed on a 60 arcsec square constellation to measure for atmospheric distortions and two deformable mirrors to compensate for it. In this paper, the second one devoted to describe the GeMS project, we present the commissioning, overall performance and operational scheme of GeMS. Performance of each subsystem is derived from the commissioning results. The typical image quality, expressed in full with at half-maximum, Strehl ratios and variations over the field delivered by the system are then described. A discussion of the main contributor to performance limitation is carried out. Finally, overheads and future system upgrades are described. C1 [Neichel, Benoit; Vidal, Fabrice; van Dam, Marcos A.; Garrel, Vincent; Rodrigo Carrasco, Eleazar; Pessev, Peter; Winge, Claudia; Boccas, Maxime; Arriagada, Gustavo; Serio, Andrew; Fesquet, Vincent; Rambold, William N.; Luehrs, Javier; Moreno, Cristian; Gausachs, Gaston; Galvez, Ramon L.; Montes, Vanessa; Vucina, Tomislav B.; Marin, Eduardo; Urrutia, Cristian; Lopez, Ariel; Diggs, Sarah J.; Marchant, Claudio; Ebbers, Angelic W.; Trujillo, Chadwick] AURA, Gemini Observ, La Serena, Chile. [Neichel, Benoit] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Rigaut, Francois; d'Orgeville, Celine; McGregor, Peter; Young, Peter J.] Australian Natl Univ, RSAA, Mt Stromlo Observ, Weston, ACT 2611, Australia. [van Dam, Marcos A.] Flat Wavefronts, Christchurch 8140, New Zealand. [Bec, Matthieu; Trancho, Gelys] Giant Magellan Telescope Org Corp, Pasadena, CA 91109 USA. [Colazo, Felipe] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Edwards, Michelle L.] Univ Arizona, LBT Observ, Tucson, AZ 85721 USA. RP Neichel, B (reprint author), AURA, Gemini Observ, Casilla 603, La Serena, Chile. EM benoit.neichel@lam.fr FU French ANR programme WASABI [ANR-13-PDOC-0006-01] FX Part of this work has been funded by the French ANR programme WASABI - ANR-13-PDOC-0006-01. NR 63 TC 39 Z9 39 U1 2 U2 15 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2014 VL 440 IS 2 BP 1002 EP 1019 DI 10.1093/mnras/stu403 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5GO UT WOS:000334742200005 ER PT J AU Komarov, SV Churazov, EM Schekochihin, AA ZuHone, JA AF Komarov, S. V. Churazov, E. M. Schekochihin, A. A. ZuHone, J. A. TI Suppression of local heat flux in a turbulent magnetized intracluster medium SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE conduction; magnetic fields; plasmas; turbulence; galaxies: clusters: intracluster medium ID ANISOTROPIC THERMAL CONDUCTION; GALAXY CLUSTERS; COLD FRONTS; BUOYANCY INSTABILITIES; X-RAY; MAGNETOHYDRODYNAMIC SIMULATIONS; GAS MOTIONS; FIELDS; TRANSPORT; PROFILES AB X-ray observations of hot gas in galaxy clusters often show steeper temperature gradients across cold fronts - contact discontinuities, driven by the differential gas motions. These sharp (a few kpc wide) surface brightness/temperature discontinuities would be quickly smeared out by the electron thermal conduction in unmagnetized plasma, suggesting significant suppression of the heat flow across the discontinuities. In fact, the character of the gas flow near cold fronts is favourable for suppression of conduction by aligning magnetic field lines along the discontinuities. We argue that a similar mechanism is operating in the bulk of the gas. Generic 3D random isotropic and incompressible motions increase the temperature gradients (in some places) and at the same time suppress the local conduction by aligning the magnetic field lines perpendicular to the local temperature gradient. We show that the suppression of the effective conductivity in the bulk of the gas can be linked to the increase of the frozen magnetic field energy density. On average the rate of decay of the temperature fluctuations d <>/dt decreases as << B-2 >>(-1/5). C1 [Komarov, S. V.; Churazov, E. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Komarov, S. V.; Churazov, E. M.] Space Res Inst IKI, Moscow 117997, Russia. [Komarov, S. V.] MIPT, Inst Pereulok 9, Dolgoprudnyi 141700, Moscow Region, Russia. [Schekochihin, A. A.] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England. [ZuHone, J. A.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Komarov, SV (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM komarov@mpa-garching.mpg.de RI Churazov, Eugene/A-7783-2013 FU Leverhulme Trust Network on Magnetized Plasma Turbulence FX This work was supported in part by the Leverhulme Trust Network on Magnetized Plasma Turbulence. NR 51 TC 4 Z9 4 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 MAY PY 2014 VL 440 IS 2 BP 1153 EP 1164 DI 10.1093/mnras/stu281 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5GO UT WOS:000334742200016 ER PT J AU Agliozzo, C Noriega-Crespo, A Umana, G Flagey, N Buemi, C Ingallinera, A Trigilio, C Leto, P AF Agliozzo, C. Noriega-Crespo, A. Umana, G. Flagey, N. Buemi, C. Ingallinera, A. Trigilio, C. Leto, P. TI The candidate luminous blue variable G79.29+0.46: a comprehensive study of its ejecta through a multiwavelength analysis SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: early-type; stars: evolution; stars: mass-loss; ISM: bubbles; infrared: ISM; radio continuum: ISM ID LARGE ARRAY OBSERVATIONS; RING NEBULA G79.29+0.46; LARGE-MAGELLANIC-CLOUD; H-II REGIONS; ETA-CARINAE; CYGNUS-X; GALACTIC-CENTER; MU-M; SPITZER; DUST AB We present a multiwavelength analysis of the nebula around the candidate luminous blue variable G79.29+0.46. The study is based on our radio observations performed at the Expanded Very Large Array and at the Green Bank Telescope and on archival infrared data sets, including recent images obtained by the Herschel Space Observatory. We confirm that the radio central object is characterized by a stellar wind and we derive a current mass-loss rate of about 1.4 x 10(-6) M-circle dot yr(-1). We find the presence of a dusty compact envelope close to the star, with a temperature between similar to 40 and 1200 K. We estimate for the outer ejecta an ionized gas mass of 1.51 M-circle dot and a warm (60-85 K) dust mass of 0.02 M-circle dot. Diagnostics of the far-infrared spectra indicate the presence of a photodissociation region around the ionized gas. Finally, we model the nebula with the photoionization code cloudy, using as input parameters those estimated from our analysis. We find for the central star a luminosity of 10(5.4) L-circle dot and an effective temperature of 20.4 kK. C1 [Agliozzo, C.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Agliozzo, C.] Univ Catania, Sez Astrofis, Dipartimento Fis & Astron, I-95123 Catania, Italy. [Noriega-Crespo, A.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Umana, G.; Buemi, C.; Ingallinera, A.; Trigilio, C.; Leto, P.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Flagey, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Agliozzo, C (reprint author), Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. EM agliozzo@oact.inaf.it OI Buemi, Carla Simona/0000-0002-7288-4613; Umana, Grazia/0000-0002-6972-8388; Leto, Paolo/0000-0003-4864-2806 FU NASA; ESA Member States; National Science Foundation FX This work is based on observations performed at the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Herschel is a European Space Agency (ESA) space observatory with science instruments provided by the European-led Principal Investigator consortia and with important participation from the National Aeronautics and Space Administration (NASA). This research has also made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. The ISO was an ESA project with instruments funded by ESA Member States (especially the PI countries, France, Germany, the Netherlands and the UK) and with the participation of ISAS and NASA. Finally, this publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the National Science Foundation. NR 70 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 MAY PY 2014 VL 440 IS 2 BP 1391 EP 1409 DI 10.1093/mnras/stu296 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5GO UT WOS:000334742200034 ER PT J AU Vigeland, SJ Vallisneri, M AF Vigeland, Sarah J. Vallisneri, Michele TI Bayesian inference for pulsar-timing models SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational waves ID GRAVITATIONAL-RADIATION; MILLISECOND PULSARS; LIMITS; PACKAGE; BINARY; TEMPO2; ASTROMETRY; SYSTEM; WAVES; NOISE AB The extremely regular, periodic radio emission from millisecond pulsars makes them useful tools for studying neutron star astrophysics, general relativity, and low-frequency gravitational waves. These studies require that the observed pulse times of arrival be fitted to complex timing models that describe numerous effects such as the astrometry of the source, the evolution of the pulsar's spin, the presence of a binary companion, and the propagation of the pulses through the interstellar medium. In this paper, we discuss the benefits of using Bayesian inference to obtain pulsar-timing solutions. These benefits include the validation of linearized least-squares model fits when they are correct, and the proper characterization of parameter uncertainties when they are not; the incorporation of prior parameter information and of models of correlated noise; and the Bayesian comparison of alternative timing models. We describe our computational setup, which combines the timing models of tempo2 with the nested-sampling integrator multinest. We compare the timing solutions generated using Bayesian inference and linearized least-squares for three pulsars: B1953+29, J2317+1439, and J1640+2224, which demonstrate a variety of the benefits that we posit. C1 [Vigeland, Sarah J.; Vallisneri, Michele] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Vigeland, SJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Sarah.J.Vigeland@jpl.nasa.gov; Michele.Vallisneri@jpl.nasa.gov FU National Aeronautics and Space Administration (NASA) Postdoctoral Programme at the Jet Propulsion Laboratory; NASA; Jet Propulsion Laboratory RTD Programme FX We are grateful to Paul Demorest, Joe Lazio, Sarah Burke-Spolaor, Rutger van Haasteren, Lindley Lentati, Tom Prince, and to all NANOGrav colleagues for helpful discussions. SV was supported by an appointment to the National Aeronautics and Space Administration (NASA) Postdoctoral Programme at the Jet Propulsion Laboratory administered by Oak Ridge Associated Universities through a contract with NASA. MV was supported by the Jet Propulsion Laboratory RTD Programme. This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract to the NASA. Copyright 2014 California Institute of Technology. NR 48 TC 8 Z9 8 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 MAY PY 2014 VL 440 IS 2 BP 1446 EP 1457 DI 10.1093/mnras/stu312 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5GO UT WOS:000334742200038 ER PT J AU Giocoli, C Meneghetti, M Metcalf, RB Ettori, S Moscardini, L AF Giocoli, Carlo Meneghetti, Massimo Metcalf, R. Benton Ettori, Stefano Moscardini, Lauro TI Mass and concentration estimates from weak and strong gravitational lensing: a systematic study SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: strong; gravitational lensing: weak; methods: analytical; galaxies: haloes; cosmology: theory; dark matter ID DARK-MATTER HALOS; HIERARCHICAL SATELLITE ACCRETION; SIMULATED GALAXY CLUSTERS; X-RAY-CLUSTERS; MARENOSTRUM UNIVERSE; DENSITY PROFILE; ARC STATISTICS; SUBSTRUCTURE; SHAPES; MODELS AB We study how well halo properties of galaxy clusters, such as mass and concentration, are recovered using lensing data. In order to generate a large sample of systems at different redshifts, we use the code moka. We measure halo mass and concentration using weak lensing data alone (WL), fitting to a Navarro, Frenk & White (NFW) profile the reduced tangential shear profile, or by combining weak and strong lensing data, by adding information about the size of the Einstein radius (WL+SL). For different redshifts, we measure the mass and the concentration biases and find that these are mainly caused by the random orientation of the halo ellipsoid with respect to the line of sight. Since our simulations account for the presence of a bright central galaxy, we perform mass and concentration measurements using a generalized NFW profile which allows for a free inner slope. This reduces both the mass and the concentration biases. We discuss how the mass function and the concentration-mass relation change when using WL and WL+SL estimates. We investigate how selection effects impact the measured concentration-mass relation showing that strong lens clusters may have a concentration 20-30 per cent higher than the average, at fixed mass, considering also the particular case of strong lensing selected samples of relaxed clusters. Finally, we notice that selecting a sample of relaxed galaxy clusters, as is done in some cluster surveys, explains the concentration-mass relation biases. C1 [Giocoli, Carlo; Metcalf, R. Benton; Moscardini, Lauro] Alma Mater Studiorum Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Giocoli, Carlo; Meneghetti, Massimo; Ettori, Stefano; Moscardini, Lauro] INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Giocoli, Carlo; Meneghetti, Massimo; Ettori, Stefano; Moscardini, Lauro] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Meneghetti, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Giocoli, C (reprint author), Alma Mater Studiorum Univ Bologna, Dipartimento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy. EM carlo.giocoli@unibo.it RI Ettori, Stefano/N-5004-2015; Meneghetti, Massimo/O-8139-2015; OI Ettori, Stefano/0000-0003-4117-8617; Meneghetti, Massimo/0000-0003-1225-7084; METCALF, ROBERT BENTON/0000-0003-3167-2574 FU project GLENCO under European Seventh Framework Programme, Ideas [259349]; PRIN MIUR; PRIN-INAF; MOKALEN3 [HP10CMXLBH]; [ASI/INAFI/023/12/0]; [ASI-INAF I/088/06/0] FX CG and RBM's research is part of the project GLENCO, funded under the European Seventh Framework Programme, Ideas, Grant Agreement no. 259349. We acknowledge financial contributions from contracts ASI/INAFI/023/12/0 and by the PRIN MIUR 2010-2011 'The dark Universe and the cosmic evolution of baryons: from current surveys to Euclid'. CG and LM also acknowledge the financial contribution by the PRIN INAF 2012 'The Universe in the box: multiscale simulations of cosmic structure'. SE acknowledges the financial contribution from contracts ASI-INAF I/088/06/0 and PRIN-INAF 2012. CG would like to thank Giuseppe Tormen and Vincenzo Mezzalira to have host part of the computer jobs run to produce the simulated galaxy cluster sample. Part of the simulations of this project have been run during the Class C Project-HP10CMXLBH (MOKALEN3). CG would also like to particularly thank Matthias Bartelmann for useful and stimulating discussions. We are also grateful to Marusa Bradac Anja Von der Linden, Stefano Borgani, Stefano Andreon and Mauro Sereno for the conversations they had during the conference in Madonna di Campiglio in 2013 March. We are grateful to the anonymous referee for his/her comments and suggestions that helped to improve the presentation of our results. NR 86 TC 15 Z9 15 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2014 VL 440 IS 2 BP 1899 EP 1915 DI 10.1093/mnras/stu303 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5GO UT WOS:000334742200071 ER PT J AU Prive, NC Errico, RM Tai, KS AF Prive, N. C. Errico, R. M. Tai, K. -S. TI The Impact of Increased Frequency of Rawinsonde Observations on Forecast Skill Investigated with an Observing System Simulation Experiment SO MONTHLY WEATHER REVIEW LA English DT Article DE Radiosonde observations; Numerical weather prediction/forecasting; Forecast verification/skill ID DATA ASSIMILATION SYSTEM; MOIST PHYSICS; VALIDATION; OFFICE AB Most rawinsondes are launched once or twice daily, at 0000 and/or 1200 UTC; only a small number of the total rawinsonde observations are taken at 0600 and 1800 UTC ("off hour" cycle times). In this study, the variations of forecast and analysis quality between cycle times and the potential improvement of skill due to supplemental rawinsonde measurements at 0600 and 1800 UTC are tested in the framework of an observing system simulation experiment (OSSE). The National Aeronautics and Space Administration Global Modeling and Assimilation Office (NASA GMAO) Goddard Earth Observing System Model, version 5 (GEOS-5), is used with the GMAO OSSE setup for an experiment emulating the months of July and August with the 2011 observational network. The OSSE is run with and without supplemental rawinsonde observations at 0600 and 1800 UTC, and the differences in analysis error and forecast skill are quantified. The addition of supplemental rawinsonde observations results in significant improvement of analysis quality in the Northern Hemisphere for both the 0000/1200 and 0600/1800 UTC cycle times, with greater improvement for the off-hour times. Reduction of root-mean-square errors on the order of 1%-3% for wind and temperature is found at the 24- and 48-h forecast times. There is a slight improvement in Northern Hemisphere anomaly correlations at the 120-h forecast time. C1 [Prive, N. C.; Errico, R. M.] Morgan State Univ, Goddard Earth Sci Technol & Res Ctr, Greenbelt, MD USA. [Tai, K. -S.] Sci Syst & Applicat Inc, Greenbelt, MD USA. RP Prive, NC (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA. EM nikki.prive@nasa.gov OI Prive, Nikki/0000-0001-8309-8741 FU GMAO FX The ECMWF nature run was provided by Erik Andersson through arrangements made by Michiko Masutani. Support for this project was encouraged by Michele Rienecker and provided by GMAO core funding. Helpful comments from three anonymous reviewers led to significant improvements in this manuscript. NR 12 TC 2 Z9 2 U1 1 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 EI 1520-0493 J9 MON WEATHER REV JI Mon. Weather Rev. PD MAY PY 2014 VL 142 IS 5 BP 1823 EP 1834 DI 10.1175/MWR-D-13-00237.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AG0OS UT WOS:000335115400008 ER PT J AU Zhou, LM Tian, YH Myneni, RB Ciais, P Saatchi, S Liu, YY Piao, SL Chen, HS Vermote, EF Song, CH Hwang, TH AF Zhou, Liming Tian, Yuhong Myneni, Ranga B. Ciais, Philippe Saatchi, Sassan Liu, Yi Y. Piao, Shilong Chen, Haishan Vermote, Eric F. Song, Conghe Hwang, Taehee TI Widespread decline of Congo rainforest greenness in the past decade SO NATURE LA English DT Article ID VEGETATION INDEXES; MICROWAVE EMISSION; TROPICAL FORESTS; DRY SEASON; MODIS; DROUGHT; CLIMATE; AMAZON; RETRIEVALS; PRODUCTS AB Tropical forests are global epicentres of biodiversity and important modulators of climate change(1), and are mainly constrained by rainfall patterns(1-3). The severe short-term droughts that occurred recently in Amazonia have drawn attention to the vulnerability of tropical forests to climatic disturbances(4-9). The central African rainforests, the second-largest on Earth, have experienced a long-term drying trend(10,11) whose impacts on vegetation dynamics remain mostly unknown because in situ observations are very limited. The Congolese forest, with its drier conditions and higher percentage of semi-evergreen trees(12,13), may be more tolerant to short-term rainfall reduction than are wetter tropical forests(11), but for a long-term drought there may be critical thresholds of water availability below which higher-biomass, closed-canopy forests transition to more open, lower-biomass forests(1,2,14). Here we present observational evidence for a widespread decline in forest greenness over the past decade based on analyses of satellite data (optical, thermal, microwave and gravity) from several independent sensors over the Congo basin. This decline in vegetation greenness, particularly in the northern Congolese forest, is generally consistent with decreases in rainfall, terrestrial water storage, water content in aboveground woody and leaf biomass, and the canopy backscatter anomaly caused by changes in structure and moisture in upper forest layers. It is also consistent with increases in photosynthetically active radiation and land surface temperature. These multiple lines of evidence indicate that this large-scale vegetation browning, or loss of photosynthetic capacity, may be partially attributable to the long-term drying trend. Our results suggest that a continued gradual decline of photosynthetic capacity and moisture content driven by the persistent drying trend could alter the composition and structure of the Congolese forest to favour the spread of drought-tolerant species(1,2,14). C1 [Zhou, Liming] SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY 12222 USA. [Tian, Yuhong] NOAA, IMSG, NESDIS, Ctr Satellite Applicat & Res,STAR, College Pk, MD 20740 USA. [Myneni, Ranga B.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. [Ciais, Philippe] UVSQ, CEA, CNRS, LSCE, F-91191 Gif Sur Yvette, France. [Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Liu, Yi Y.] Univ New S Wales, ARC Ctr Excellence Climate Syst Sci, Sydney, NSW 2052, Australia. [Liu, Yi Y.] Univ New S Wales, Climate Change Res Ctr, Sydney, NSW 2052, Australia. [Piao, Shilong] Peking Univ, Dept Ecol, Coll Urban & Environm Sci, Beijing 100871, Peoples R China. [Chen, Haishan] Nanjing Univ Informat Sci & Technol, Minist Educ, Key Lab Meteorol Disaster, Nanjing 210044, Jiangsu, Peoples R China. [Vermote, Eric F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Song, Conghe] Univ N Carolina, Dept Geog, Chapel Hill, NC 29599 USA. [Song, Conghe] Anhui Agr Univ, Sch Forestry & Landscape Architecture, Hefei 230036, Anhui, Peoples R China. [Hwang, Taehee] Univ N Carolina, Inst Environm, Chapel Hill, NC 29599 USA. RP Zhou, LM (reprint author), SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY 12222 USA. EM lzhou@albany.edu RI Myneni, Ranga/F-5129-2012; Young, Kristina/M-3069-2014; Liu, Yi/H-9226-2013; Song, Conghe/E-3087-2016; Liu, Yi/M-7169-2015; Zhou, Liming/A-2688-2012; OI Song, Conghe/0000-0002-4099-4906; Liu, Yi/0000-0001-9059-8269; Chen, Haishan/0000-0002-2403-3187 FU NOAA NESDIS [NA11NES4400010]; University at Albany, State University of New York; NASA's Earth Science Division; National Natural Science Foundation of China [41230422] FX This study was supported by the NOAA NESDIS project (NA11NES4400010) and by the startup funds provided by the University at Albany, State University of New York. R. B. M. was funded by NASA's Earth Science Division. The views, opinions, and findings contained in this report are those of the authors and should not be construed as an official NOAA or US Government position, policy, or decision. H. C. is supported by the National Natural Science Foundation of China (grant number 41230422). NR 51 TC 60 Z9 62 U1 17 U2 249 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAY 1 PY 2014 VL 509 IS 7498 BP 86 EP + DI 10.1038/nature13265 PG 18 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AG1TM UT WOS:000335199100044 PM 24759324 ER PT J AU Oviatt, CG Chan, MA Jewell, PW Bills, BG Madsen, DB Miller, DM AF Oviatt, Charles G. Chan, Marjorie A. Jewell, Paul W. Bills, Bruce G. Madsen, David B. Miller, David M. TI Interpretations of evidence for large Pleistocene paleolakes in the Bonneville basin, western North America COMMENT on: Bonneville basin shoreline records of large lake intervals during marine isotope stage 3 and the last glacial maximum, by Nishizawa et al. (2013) SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Pleistocene; Great Basin; Radiocarbon; Lake Bonneville; MIS 3 ID UTAH AB Nishizawa et al. (2013) argue in support of three large paleolakes in the Bonneville basin during Marine Oxygen Isotope Stage 3 (MIS 3). If true, that would be an important contribution to paleoclimate investigations. However, the key evidence in support of their argument consists of four radiocarbon ages that are out of stratigraphic order and near the practical and theoretical limit of the dating method. The interpretation of three large MIS 3 lakes conflicts with some of their own data, as well as with independently derived stratigraphic information from the basin. Nishizawa et al. (2013) also interpret a series of radiocarbon ages of mollusk samples as indicating previously undocumented lake transgressions a few thousand years older than basal radiocarbon ages of wood samples. We believe that these interpretations are in error, and arise largely from reliance on radiocarbon ages from carbonate material. Lake records constrained by ages of non-carbonate organic materials, along with compelling stratigraphic information from unconformities and buried soils, argue for not changing interpretations of Lake Bonneville history until more supporting information for older lakes at relatively high altitudes is found. (C) 2014 Elsevier B.V. All rights reserved. C1 [Oviatt, Charles G.] Kansas State Univ, Dept Geol, Manhattan, KS 66506 USA. [Chan, Marjorie A.; Jewell, Paul W.] Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA. [Bills, Bruce G.] CALTECH, Jet Prop Lab, Asteroids Comets & Satellites Grp, Pasadena, CA 91109 USA. [Madsen, David B.] Lanzhou Univ, Res Sch Arid Environm & Climate Change, Lanzhou 730000, Peoples R China. [Miller, David M.] US Geol Survey, Menlo Pk, CA 94025 USA. RP Oviatt, CG (reprint author), Kansas State Univ, Dept Geol, Manhattan, KS 66506 USA. EM joviatt@ksu.edu NR 16 TC 2 Z9 2 U1 0 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD MAY 1 PY 2014 VL 401 BP 173 EP 176 DI 10.1016/j.palaeo.2014.03.003 PG 4 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA AG2YK UT WOS:000335282800014 ER PT J AU Ray, FA Robinson, E McKenna, M Hada, M George, K Cucinotta, F Goodwin, EH Bedford, JS Bailey, SM Cornforth, MN AF Ray, F. Andrew Robinson, Erin McKenna, Miles Hada, Megumi George, Kerry Cucinotta, Francis Goodwin, Edwin H. Bedford, Joel S. Bailey, Susan M. Cornforth, Michael N. TI Directional genomic hybridization: inversions as a potential biodosimeter for retrospective radiation exposure SO RADIATION AND ENVIRONMENTAL BIOPHYSICS LA English DT Article DE Chromosome inversions; Biodosimetry; Ionizing radiation; FISH; DGH; Directional genomic hybridization; Strand-specific hybridization ID IN-SITU HYBRIDIZATION; COMPLEX CHROMOSOME-ABERRATIONS; IONIZING-RADIATION; HUMAN-LYMPHOCYTES; ALPHA-PARTICLES; GAMMA-RAYS; HEAVY-IONS; BIOLOGICAL DOSIMETRY; EXCHANGE ABERRATIONS; CYTOGENETIC METHODS AB Chromosome aberrations in blood lymphocytes provide a useful measure of past exposure to ionizing radiation. Despite the widespread and successful use of the dicentric assay for retrospective biodosimetry, the approach suffers substantial drawbacks, including the fact that dicentrics in circulating blood have a rather short half-life (roughly 1-2 years by most estimates). So-called symmetrical aberrations such as translocations are far more stable in that regard, but their high background frequency, which increases with age, also makes them less than ideal for biodosimetry. We developed a cytogenetic assay for potential use in retrospective biodosimetry that is based on the detection of chromosomal inversions, another symmetrical aberration whose transmissibility (stability) is also ostensibly high. Many of the well-known difficulties associated with inversion detection were circumvented through the use of directional genomic hybridization, a method of molecular cytogenetics that is less labor intensive and better able to detect small chromosomal inversions than other currently available approaches. Here, we report the dose-dependent induction of inversions following exposure to radiations with vastly different ionization densities [i.e., linear energy transfer (LET)]. Our results show a dramatic dose-dependent difference in the yields of inversions induced by low-LET gamma rays, as compared to more damaging high-LET charged particles similar to those encountered in deep space. C1 [Ray, F. Andrew; Bedford, Joel S.; Bailey, Susan M.] Colorado State Univ, Dept Environm & Radiol Hlth Sci, Ft Collins, CO 80523 USA. [Robinson, Erin; McKenna, Miles; Goodwin, Edwin H.] KromaTiD Inc, Ft Collins, CO 80524 USA. [Hada, Megumi] Univ Space Res Assoc, Houston, TX 77058 USA. [George, Kerry] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. [Cucinotta, Francis] Natl Aeronaut & Space Adm, Houston, TX 77058 USA. [Cornforth, Michael N.] Univ Texas Med Branch, Dept Radiat Oncol, Galveston, TX 77555 USA. RP Ray, FA (reprint author), Colorado State Univ, Dept Environm & Radiol Hlth Sci, Ft Collins, CO 80523 USA. EM fa.ray@colostate.edu FU NASA [NNX08AB65G, NNX09CE42P, NNX10CB05C, NNJ06HA29A]; NIH/NIAID [R01AI080486-02] FX Funding for this work from NASA (NNX08AB65G; NNX09CE42P; NNX10CB05C; NNJ06HA29A) and NIH/NIAID (R01AI080486-02) is gratefully acknowledged. NR 49 TC 4 Z9 4 U1 2 U2 9 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0301-634X EI 1432-2099 J9 RADIAT ENVIRON BIOPH JI Radiat. Environ. Biophys. PD MAY PY 2014 VL 53 IS 2 BP 255 EP 263 DI 10.1007/s00411-014-0513-1 PG 9 WC Biology; Biophysics; Environmental Sciences; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Biophysics; Environmental Sciences & Ecology; Radiology, Nuclear Medicine & Medical Imaging GA AF8XF UT WOS:000334998200005 PM 24477407 ER PT J AU Pate, DJ Gray, J German, BJ AF Pate, David J. Gray, Justin German, Brian J. TI A graph theoretic approach to problem formulation for multidisciplinary design analysis and optimization SO STRUCTURAL AND MULTIDISCIPLINARY OPTIMIZATION LA English DT Article DE Graph theory; Multidisciplinary design optimization; Problem formulation ID DECOMPOSITION; SYSTEMS AB The formulation of multidisciplinary design, analysis, and optimization (MDAO) problems has become increasingly complex as the number of analysis tools and design variables included in typical studies has grown. This growth in the scale and scope of MDAO problems has been motivated by the need to incorporate additional disciplines and to expand the parametric design space to enable the exploration of unconventional design concepts. In this context, given a large set of disciplinary analysis tools, the problem of determining a feasible data flow between tools to produce a specified set of system-level outputs is combinatorially challenging. The difficulty is compounded in multi-fidelity problems, which are of increasing interest to the MDAO community. In this paper, we propose an approach for addressing this problem based on the formalism of graph theory. The approach begins by constructing the maximal connectivity graph (MCG) describing all possible interconnections between a set of analysis tools. Graph operations are then conducted to reduce the MCG to a fundamental problem graph (FPG) that describes the connectivity of analysis tools needed to solve a specified system-level design problem. The FPG does not predispose a particular solution procedure; any relevant MDO solution architecture could be selected to implement the optimization. Finally, the solution architecture can be represented in a problem solution graph (PSG). The graph approach is applied to an example problem based on a commercial aircraft MDAO study. C1 [Pate, David J.; German, Brian J.] Georgia Inst Technol, Sch Aerosp Engn, Atlanta, GA 30332 USA. [Gray, Justin] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP German, BJ (reprint author), Georgia Inst Technol, Sch Aerosp Engn, 270 Ferst Dr, Atlanta, GA 30332 USA. EM brian.german@aerospace.gatech.edu NR 31 TC 0 Z9 0 U1 3 U2 22 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1615-147X EI 1615-1488 J9 STRUCT MULTIDISCIP O JI Struct. Multidiscip. Optim. PD MAY PY 2014 VL 49 IS 5 BP 743 EP 760 DI 10.1007/s00158-013-1006-6 PG 18 WC Computer Science, Interdisciplinary Applications; Engineering, Multidisciplinary; Mechanics SC Computer Science; Engineering; Mechanics GA AG6EC UT WOS:000335510400004 ER PT J AU Duda, BM Menter, FR Hansen, T Esteve, MJ Deck, S Bezard, H AF Duda, Benjamin M. Menter, Florian R. Hansen, Thorsten Esteve, Marie-Josephe Deck, Sebastien Bezard, Herve TI Aerothermal Prediction of Multiple Hot Jets in Crossflow for Aircraft Applications SO AIAA JOURNAL LA English DT Article ID LARGE-EDDY-SIMULATION; SCALE-ADAPTIVE SIMULATION; MODEL AB Even though many technical applications feature multiple jets in crossflow, little attention has been paid so far to their simultaneous numerical simulation as a system. A special challenge in this context is the simulation of exhausts of air systems on aircraft since they feature multiple hot jets in crossflow at high Reynolds numbers. As standard statistical turbulence models are not capable of correctly predicting thermal mixing between the jet and crossflow as well as interjet mixing, the scale-adaptive simulation is employed. In a first step, a simplified configuration comprising five laterally aligned jets is investigated, and numerical results are compared to wind tunnel data with good agreement. The establishing flowfield is analyzed, and its dynamics are compared to a single jet in the crossflow reference case. In a second step, the exhaust of an existing antiicing system is considered on an aircraft under realistic flight conditions. To take into account the local flow topology and to reduce computational costs, a sequential simulation methodology is applied, which relies on a Reynolds-Averaged Navier-Stokes simulation of the aircraft to provide boundary conditions for a subsequent scale-adaptive simulation calculation in a truncated subdomain. Results are compared to flight test data with good agreement, which highlights the applicability of the proposed approach. C1 [Duda, Benjamin M.] Airbus Ind, Aerodynam Tools & Simulat, F-31060 Toulouse, France. [Duda, Benjamin M.] NASA, Langley Res Center, Hampton, VA USA. [Menter, Florian R.] ANSYS Germany GmbH, Core Dev, D-83624 Otterfing, Germany. [Hansen, Thorsten] ANSYS Germany GmbH, Customer & Sales Support, D-83624 Otterfing, Germany. [Esteve, Marie-Josephe] Airbus Ind, Aerodynam Tools & Simulat, F-31060 Toulouse, France. [Deck, Sebastien] Off Natl Etud & Rech Aerosp, Appl Aerodynam Dept, F-92190 Meudon, France. [Bezard, Herve] Off Natl Etud & Rech Aerosp, Aerodynam & Energet Modeling Dept, F-31055 Toulouse, France. RP Duda, BM (reprint author), Airbus Ind, Aerodynam Tools & Simulat, F-31060 Toulouse, France. OI Deck, Sebastien/0000-0003-1020-0965 NR 28 TC 0 Z9 1 U1 1 U2 8 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 MAY PY 2014 VL 52 IS 5 BP 1035 EP 1046 DI 10.2514/1.J052370 PG 12 WC Engineering, Aerospace SC Engineering GA AF7AE UT WOS:000334864900012 ER PT J AU Bregon, A Daigle, M Roychoudhury, I Biswas, G Koutsoukos, X Pulido, B AF Bregon, Anibal Daigle, Matthew Roychoudhury, Indranil Biswas, Gautam Koutsoukos, Xenofon Pulido, Belarmino TI An event-based distributed diagnosis framework using structural model decomposition SO ARTIFICIAL INTELLIGENCE LA English DT Article DE Distributed diagnosis; Structural model decomposition; Discrete event systems; Possible Conflicts ID ANALYTICAL REDUNDANCY RELATIONS; FAULT-DIAGNOSIS; FAILURE DIAGNOSIS; SYSTEMS; DIAGNOSABILITY; ALGORITHM; CONFLICTS; NETWORKS AB Complex engineering systems require efficient on-line fault diagnosis methodologies to improve safety and reduce maintenance costs. Traditionally, diagnosis approaches are centralized, but these solutions do not scale well. Also, centralized diagnosis solutions are difficult to implement on increasingly prevalent distributed, networked embedded systems. This paper presents a distributed diagnosis framework for physical systems with continuous behavior. Using Possible Conflicts, a structural model decomposition method from the Artificial Intelligence model-based diagnosis (DX) community, we develop a distributed diagnoser design algorithm to build local event-based diagnosers. These diagnosers are constructed based on global diagnosability analysis of the system, enabling them to generate local diagnosis results that are globally correct without the use of a centralized coordinator. We also use Possible Conflicts to design local parameter estimators that are integrated with the local diagnosers to form a comprehensive distributed diagnosis framework. Hence, this is a fully distributed approach to fault detection, isolation, and identification. We evaluate the developed scheme on a four-wheeled rover for different design scenarios to show the advantages of using Possible Conflicts, and generate on-line diagnosis results in simulation to demonstrate the approach. (C) 2014 Elsevier B.V. All rights reserved. C1 [Bregon, Anibal; Pulido, Belarmino] Univ Valladolid, Dept Comp Sci, E-47011 Valladolid, Spain. [Daigle, Matthew] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Roychoudhury, Indranil] NASA, Ames Res Ctr, SGT Inc, Moffett Field, CA 94035 USA. [Biswas, Gautam; Koutsoukos, Xenofon] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Inst Software Integrated Syst, Nashville, TN 37235 USA. RP Bregon, A (reprint author), Univ Valladolid, Dept Comp Sci, E-47011 Valladolid, Spain. EM anibal@infor.uva.es; matthew.j.daigle@nasa.gov; indranil.roychoudhury@nasa.gov; gautam.biswas@vanderbilt.edu; xenofon.koutsoukos@vanderbilt.edu; belar@infor.uva.es RI Pulido Junquera, Belarmino/I-2506-2015; OI Pulido Junquera, Belarmino/0000-0003-2340-684X; Daigle, Matthew/0000-0002-4616-3302 FU Spanish MCI grant [TIN2009-11326]; NASA System-wide Safety and Assurance Technologies (SSAT) project; National Science Foundation [CNS-1238959] FX A. Bregon and B. Pulido's work has been partially supported by the Spanish MCI TIN2009-11326 grant.; M. Daigle and I. Roychoudhury's work has been partially supported by the NASA System-wide Safety and Assurance Technologies (SSAT) project.; Xenofon Koutsoukos' work was supported in part by the National Science Foundation (CNS-1238959). NR 58 TC 8 Z9 8 U1 0 U2 21 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0004-3702 EI 1872-7921 J9 ARTIF INTELL JI Artif. Intell. PD MAY PY 2014 VL 210 BP 1 EP 35 DI 10.1016/j.artint.2014.01.003 PG 35 WC Computer Science, Artificial Intelligence SC Computer Science GA AF8OF UT WOS:000334974800001 ER PT J AU Coughlin, JL Thompson, SE Bryson, ST Burke, CJ Caldwell, DA Christiansen, JL Haas, MR Howell, SB Jenkins, JM Kolodziejczak, JJ Mullally, FR Rowe, JF AF Coughlin, Jeffrey L. Thompson, Susan E. Bryson, Stephen T. Burke, Christopher J. Caldwell, Douglas A. Christiansen, Jessie L. Haas, Michael R. Howell, Steve B. Jenkins, Jon M. Kolodziejczak, Jeffery J. Mullally, Fergal R. Rowe, Jason F. TI CONTAMINATION IN THE KEPLER FIELD. IDENTIFICATION OF 685 KOIs AS FALSE POSITIVES VIA EPHEMERIS MATCHING BASED ON Q1-Q12 DATA SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; instrumentation: detectors; planetary systems; planets and satellites: detection; stars: statistics; techniques: photometric ID ECLIPSING BINARIES; PLANET HUNTERS; DATA RELEASE; VALIDATION; CATALOG; SYSTEMS AB The Kepler mission has to date found almost 6000 planetary transit-like signals, utilizing three years of data for over 170,000 stars at extremely high photometric precision. Due to its design, contamination from eclipsing binaries, variable stars, and other transiting planets results in a significant number of these signals being false positives (FPs). This directly affects the determination of the occurrence rate of Earth-like planets in our Galaxy, as well as other planet population statistics. In order to detect as many of these FPs as possible, we perform ephemeris matching among all transiting planet, eclipsing binary, and variable star sources. We find that 685 Kepler Objects of Interest (KOIs)-12% of all those analyzed-are FPs as a result of contamination, due to 409 unique parent sources. Of these, 118 have not previously been identified by other methods. We estimate that similar to 35% of KOIs are FPs due to contamination, when performing a first-order correction for observational bias. Comparing single-planet candidate KOIs to multi-planet candidate KOIs, we find an observed FP fraction due to contamination of 16% and 2.4% respectively, bolstering the existing evidence that multi-planet KOIs are significantly less likely to be FPs. We also analyze the parameter distributions of the ephemeris matches and derive a simple model for the most common type of contamination in the Kepler field. We find that the ephemeris matching technique is able to identify low signal-to-noise FPs that are difficult to identify with other vetting techniques. We expect FP KOIs to become more frequent when analyzing more quarters of Kepler data, and note that many of them will not be able to be identified based on Kepler data alone. C1 [Coughlin, Jeffrey L.; Thompson, Susan E.; Burke, Christopher J.; Caldwell, Douglas A.; Jenkins, Jon M.; Mullally, Fergal R.; Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA. [Coughlin, Jeffrey L.; Thompson, Susan E.; Bryson, Stephen T.; Burke, Christopher J.; Caldwell, Douglas A.; Haas, Michael R.; Howell, Steve B.; Jenkins, Jon M.; Mullally, Fergal R.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Christiansen, Jessie L.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Kolodziejczak, Jeffery J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Coughlin, JL (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA. EM jeffrey.l.coughlin@nasa.gov RI Caldwell, Douglas/L-7911-2014 OI Caldwell, Douglas/0000-0003-1963-9616 FU NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; NASA Science Mission directorate FX We thank the anonymous referee for his or her very helpful comments, which especially helped to improve the clarity of the paper. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research has made use of NASA's Astrophysics Data System. 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 paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. NR 24 TC 32 Z9 32 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2014 VL 147 IS 5 AR 119 DI 10.1088/0004-6256/147/5/119 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3DO UT WOS:000334591900026 ER PT J AU O'Dea, JA Jenet, FA Cheng, TH Buu, CM Beroiz, M Asmar, SW Armstrong, JW AF O'Dea, J. Andrew Jenet, F. A. Cheng, Tsan-Huei Buu, Chau M. Beroiz, Martin Asmar, Sami W. Armstrong, J. W. TI BRIGHT MICROWAVE PULSES FROM PSR B0531+21 OBSERVED WITH A PROTOTYPE TRANSIENT SURVEY RECEIVER SO ASTRONOMICAL JOURNAL LA English DT Article DE instrumentation: detectors; pulsars: individual (B0531+21) ID ANISOTROPIC MAGNETOGASDYNAMIC TURBULENCE; CRAB PULSAR; INTERSTELLAR-MEDIUM; DENSITY-FLUCTUATIONS; RADIO TRANSIENT; GIANT PULSES; SCINTILLATION; SCATTERING; EMISSION; SPECTRUM AB Recent discoveries of transient radio events have renewed interest in time-variable astrophysical phenomena. Many radio transient events are rare, requiring long observing times for reliable statistical study. The National Aeronautics and Space Administration/Jet Propulsion Laboratory's Deep Space Network (DSN) tracks spacecraft nearly continuously with 13 large-aperture, low system temperature radio antennas. During normal spacecraft operations, the DSN processes only a small fraction of the pre-detection bandwidth available from these antennas; any information in the remaining bandwidth, e.g., from an astronomical source in the same antenna beam as the spacecraft, is currently ignored. As a firmware modification to the standard DSN tracking receiver, we built a prototype receiver that could be used for astronomical transient surveys. Here, we demonstrate the receiver's utility through observations of bright pulses from the Crab pulsar and describe attributes of potential transient survey observations piggybacking on operational DSN tracks. C1 [O'Dea, J. Andrew; Cheng, Tsan-Huei; Buu, Chau M.; Asmar, Sami W.; Armstrong, J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Jenet, F. A.; Beroiz, Martin] Univ Texas Brownsville, Dept Phys & Astron, Brownsville, TX 78520 USA. RP O'Dea, JA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. FU JPL; National Aeronautics and Space Administration FX The authors thank Ron Creech and Larry Bracamonte of ITT and the Goldstone team for supporting the test passes at DSS15. We benefited from discussions with W. A. Coles and Richard Woo. Development of the RRAT TRAP prototype was supported under the Director's Research and Development Fund at JPL. For the JPL authors, the research described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 31 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2014 VL 147 IS 5 AR 100 DI 10.1088/0004-6256/147/5/100 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3DO UT WOS:000334591900007 ER PT J AU Kourdis, PD Bellan, J AF Kourdis, Panayotis D. Bellan, Josette TI Heavy-alkane oxidation kinetic-mechanism reduction using dominant dynamic variables, self similarity and chemistry tabulation SO COMBUSTION AND FLAME LA English DT Article DE Reduced kinetics for n-heptane; Iso-octane; n-Decane and n-dodecane; Self-similarity; Dominant variable ID EQUATION-OF-STATE; SENSITIVITY FUNCTIONS; COMBUSTION; MODELS; JET AB A model of local and full or partial self similarity is developed for situations in which a phenomenon exhibits a dominant variable, with the goal of applying the model to obtain reduced oxidation kinetics from detailed kinetics for n-heptane, iso-octane, n-decane and n-dodecane. Upon appropriate normalization, it is shown that the state vector for all four alkanes indeed obeys local full self similarity with respect to the dominant variable which is here a normalized temperature. Further, the vector of species mass fractions is partitioned into major species which are those of interest to calculate, and thus for which equations are solved, and minor species which are those of no interest to calculate and are therefore modeled. The goal of the chemical kinetic reduction is to provide a model which expresses the influence of the minor species on the major species. The identification of major species with the light species, and of the minor species with the heavy species leads to partitioning the energetics into computed and modeled parts. This partition of the species set is shown to lead to local full self similarity of the reaction rates between the modeled and calculated species; the local full self similarity also prevails for the energy of the modeled species and for the average heat capacity at constant volume of the heavy species. A methodology is developed to take advantage of this self similarity by considering the initial condition as a point in the three-dimensional space of the initial pressure, initial temperature and equivalence ratio, choosing eight points surrounding the initial condition in this space, developing the self similarity graphs at these eight points using the LLNL detailed mechanism in conjunction with CHEMKIN II, and calculating at each time step the modeled contributions at the surrounded point by interpolating from those known at the eight points. Once the modeled contributions are known, the conservation equations for the species and the energy, coupled with a real-gas equation of state, are solved. With a focus on the high-pressure conditions in automotive engines, extensive results are shown for the four alkanes over a wide range of initial temperatures (650-1000 K) and equivalence ratios (0.35-3.00) at 20 bar and 40 bar. The results consist of timewise profiles of the temperature and species, allowing the calculation of the ignition time and the equilibrium or maximum temperature. Comparisons between the reduced mechanism and the detailed mechanism show excellent to very good agreement for all alkanes when only 20 progress-variable light species are used in the reduced mechanism; the 20 species are the same for all fuels, and for n-decane and n-dodecane this represents a reduction in the species progress variables by factor of more than 100. As an example, calculations that excellently duplicate the elemental mechanism are also shown for n-dodecane using only 15 or 6 progress-variable light species, indicating the potential for further progress-variable reduction beyond the 20 species. (C) 2013 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, Pasadena, CA 91125 USA. EM Josette.Bellan@jpl.nasa.gov FU Army Research Office FX This study was conducted at the California Institute of Technology, Jet Propulsion Laboratory (JPL), and was sponsored by the 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 JPL/NASA Supercomputing facilities. NR 15 TC 2 Z9 2 U1 7 U2 22 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0010-2180 EI 1556-2921 J9 COMBUST FLAME JI Combust. Flame PD MAY PY 2014 VL 161 IS 5 BP 1196 EP 1223 DI 10.1016/j.combustflame.2013.11.012 PG 28 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA AF4AO UT WOS:000334654000006 ER PT J AU Tonui, E Zolensky, M Hiroi, T Nakamura, T Lipschutz, ME Wang, MS Okudaira, K AF Tonui, Eric Zolensky, Mike Hiroi, Takahiro Nakamura, Tomoki Lipschutz, Michael E. Wang, Ming-Sheng Okudaira, Kyoko TI Petrographic, chemical and spectroscopic evidence for thermal metamorphism in carbonaceous chondrites I: CI and CM chondrites (vol 126, pg 284, 2014) SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Correction C1 [Tonui, Eric] BP Upstream Res & Technol, Houston, TX 77079 USA. [Zolensky, Mike] NASA, Johnson Space Ctr, ARES, Houston, TX 77058 USA. [Hiroi, Takahiro] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Nakamura, Tomoki] Tohoku Univ Aramaki, Dept Earth & Planetary Mat Sci, Fac Sci, Sendai, Miyagi 9808578, Japan. [Lipschutz, Michael E.; Wang, Ming-Sheng] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA. [Okudaira, Kyoko] Univ Aizu, Aizu Wakamatsu, Fukushima 9658580, Japan. RP Tonui, E (reprint author), BP Upstream Res & Technol, 501 Westlake Blvd, Houston, TX 77079 USA. NR 1 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 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY 1 PY 2014 VL 132 BP 458 EP 458 DI 10.1016/j.gca.2014.02.022 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AF6NP UT WOS:000334832100025 ER PT J AU Olsen, N Luhr, H Finlay, CC Sabaka, TJ Michaelis, I Rauberg, J Toffner-Clausen, L AF Olsen, Nils Luehr, Hermann Finlay, Christopher C. Sabaka, Terence J. Michaelis, Ingo Rauberg, Jan Toffner-Clausen, Lars TI The CHAOS-4 geomagnetic field model SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE Inverse theory; Magnetic anomalies: modelling and interpretation; Rapid time variations; Satellite magnetics ID EARTHS MAGNETIC-FIELD; SECULAR VARIATION; OBSERVATORY DATA; SATELLITE DATA; POLAR VORTEX; CORE; CHAMP AB We present CHAOS-4, a new version in the CHAOS model series, which aims to describe the Earth's magnetic field with high spatial and temporal resolution. Terms up to spherical degree of at least n = 85 for the lithospheric field, and up to n = 16 for the time-varying core field are robustly determined. More than 14 yr of data from the satellites circle divide rsted, CHAMP and SAC-C, augmented with magnetic observatory monthly mean values have been used for this model. Maximum spherical harmonic degree of the static (lithospheric) field is n = 100. The core field is expressed by spherical harmonic expansion coefficients up to n = 20; its time-evolution is described by order six splines, with 6-month knot spacing, spanning the time interval 1997.0-2013.5. The third time derivative of the squared radial magnetic field component is regularized at the core-mantle boundary. No spatial regularization is applied to the core field, but the high-degree lithospheric field is regularized for n > 85. CHAOS-4 model is derived by merging two submodels: its low-degree part has been derived using similar model parametrization and data sets as used for previous CHAOS models (but of course including more recent data), while its high-degree lithospheric field part is solely determined from low-altitude CHAMP satellite observations taken during the last 2 yr (2008 September-2010 September) of the mission. We obtain a good agreement with other recent lithospheric field models like MF7 for degrees up to n = 85, confirming that lithospheric field structures down to a horizontal wavelength of 500 km are currently robustly determined. C1 [Olsen, Nils; Finlay, Christopher C.; Toffner-Clausen, Lars] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Luehr, Hermann; Michaelis, Ingo; Rauberg, Jan] Deutsch GeoForschungsZentrum GFZ, Helmholtz Zentrum Potsdam, D-14473 Potsdam, Germany. [Sabaka, Terence J.] NASA, Goddard Space Flight Ctr, Geodynam Branch, Greenbelt, MD 20771 USA. RP Olsen, N (reprint author), Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JW, Midlothian, Scotland. RI Finlay, Christopher/B-5062-2014; Olsen, Nils/H-1822-2011; OI Finlay, Christopher/0000-0002-4592-2290; Olsen, Nils/0000-0003-1132-6113; Toffner-Clausen, Lars/0000-0003-4314-3776 FU CHAMP mission by the German Aerospace Center (DLR); Federal Ministry of Education and Research FX This paper has been finalised while N.O. was visiting Professor at University of Edinburgh, kindly supported by The Leverhulme Trust. We would like to thank the staff of the geomagnetic observatories and INTERMAGNET for supplying high-quality observatory data, and Susan Macmillan for providing us with checked and corrected observatory hourly mean values. The support of the CHAMP mission by the German Aerospace Center (DLR) and the Federal Ministry of Education and Research is gratefully acknowledged. The Orsted Project was made possible by extensive support from the Danish Government, NASA, ESA, CNES, DARA and the Thomas B. Thriges Foundation. NR 49 TC 52 Z9 54 U1 1 U2 19 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 MAY PY 2014 VL 197 IS 2 BP 815 EP 827 DI 10.1093/gji/ggu033 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AF5EK UT WOS:000334736600010 ER PT J AU Casner, SM Schooler, JW AF Casner, Stephen M. Schooler, Jonathan W. TI Thoughts in Flight Automation Use and Pilots' Task-Related and Task-Unrelated Thought SO HUMAN FACTORS LA English DT Article DE awareness; mind wandering; attention; cockpit automation ID TIME-ESTIMATION; MIND; PERFORMANCE AB Objective: The objective was to examine the relationship between cockpit automation use and task-related and task-unrelated thought among airline pilots. Background: Studies find that cockpit automation can sometimes relieve pilots of tedious control tasks and afford them more time to think ahead. Paradoxically, automation has also been shown to lead to lesser awareness. These results prompt the question of what pilots think about while using automation. Method: A total of 18 airline pilots flew a Boeing 747-400 simulator while we recorded which of two levels of automation they used. As they worked, pilots were verbally probed about what they were thinking. Pilots were asked to categorize their thoughts as pertaining to (a) a specific task at hand, (b) higher-level flight-related thoughts (e.g., planning ahead), or (c) thoughts unrelated to the flight. Pilots' performance was also measured. Results: Pilots reported a smaller percentage of task-at-hand thoughts (27% vs. 50%) and a greater percentage of higher-level flight-related thoughts (56% vs. 29%) when using the higher level of automation. However, when all was going according to plan, using either level of automation, pilots also reported a higher percentage of task-unrelated thoughts (21%) than they did when in the midst of an unsuccessful performance (7%). Task-unrelated thoughts peaked at 25% when pilots were not interacting with the automation. Conclusion: Although cockpit automation may provide pilots with more time to think, it may encourage pilots to reinvest only some of this mental free time in thinking flight-related thoughts. Application: This research informs the design of human-automation systems that more meaningfully engage the human operator. C1 [Casner, Stephen M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Schooler, Jonathan W.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. RP Casner, SM (reprint author), NASA, Ames Res Ctr, Mail Stop 262-4, Moffett Field, CA 94035 USA. EM stephen.casner@nasa.gov FU Aviation Safety Program at the National Aeronautics and Space Administration FX This work was supported by the Aviation Safety Program at the National Aeronautics and Space Administration. NR 27 TC 7 Z9 7 U1 1 U2 16 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 MAY PY 2014 VL 56 IS 3 BP 433 EP 442 DI 10.1177/0018720813501550 PG 10 WC Behavioral Sciences; Engineering, Industrial; Ergonomics; Psychology, Applied; Psychology SC Behavioral Sciences; Engineering; Psychology GA AF3SJ UT WOS:000334632200001 PM 24930166 ER PT J AU Davis, CA Ahijevych, DA Haggerty, JA Mahoney, MJ AF Davis, Christopher A. Ahijevych, David A. Haggerty, Julie A. Mahoney, Michael J. TI Observations of Temperature in the Upper Troposphere and Lower Stratosphere of Tropical Weather Disturbances SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article DE Tropopause; Aircraft observations; Microwave observations; Convective clouds; Tropical cyclones ID TROPOPAUSE REGION; CLOUDS; WAVES; CONVECTION; EVOLUTION; ATLANTIC; CLIMATE; PREDICT; LAYER; CYCLOGENESIS AB Microwave temperature profiler (MTP) data are analyzed to document temperature signatures in the upper troposphere and lower stratosphere that accompany Atlantic tropical weather disturbances. The MTP was deployed on the National Science Foundation-National Center for Atmospheric Research Gulfstream V (GV) aircraft during the Pre-Depression Investigation of Cloud-Systems in the Tropics (PREDICT) in August and September 2010. Temporal variations in cold-point temperature compared with infrared cloud-top temperature reveal that organized deep convection penetrated to near or beyond the cold point for each of the four disturbances that developed into a tropical cyclone. Relative to the lower-tropospheric circulation center, MTP and dropsonde data confirmed a stronger negative radial gradient of temperature in the upper troposphere (10-13 km) of developing disturbances prior to genesis compared with nondeveloping disturbances. The MTP data revealed a somewhat higher and shallower area of relative warmth near the center when compared with dropsonde data. MTP profiles through anvil cloud depicted cooling near 15 km and warming in the lower stratosphere near the time of maximum coverage of anvil clouds shortly after sunrise. Warming occurred through a deep layer of the upper troposphere toward local noon, presumably associated with radiative heating in cloud. The temperature signatures of anvil cloud above 10-km altitude contributed to the radial gradient of temperature because of the clustering of deep convection near the center of circulation. However, it is concluded that these signatures may be more a result of properties of convection than a direct distinguishing factor of genesis. C1 [Davis, Christopher A.; Ahijevych, David A.; Haggerty, Julie A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Mahoney, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Davis, CA (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM cdavis@ucar.edu FU National Science Foundation FX The National Center for Atmospheric Research is sponsored by the National Science Foundation. NR 50 TC 4 Z9 4 U1 2 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 EI 1520-0469 J9 J ATMOS SCI JI J. Atmos. Sci. PD MAY PY 2014 VL 71 IS 5 BP 1593 EP 1608 DI 10.1175/JAS-D-13-0278.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF8UQ UT WOS:000334991500005 ER PT J AU Shen, BW AF Shen, Bo-Wen TI Nonlinear Feedback in a Five-Dimensional Lorenz Model SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article DE Differential equations; Nonlinear dynamics; Numerical weather prediction/forecasting; Climate prediction; Lyapunov vectors; Numerical analysis/modeling ID GENERAL-CIRCULATION MODEL; LOCAL LYAPUNOV EXPONENTS; OCEAN-ATMOSPHERE MODEL; BENARD CONVECTION; TIME-SERIES; PREDICTABILITY; TRUNCATIONS; ORDER; CHAOS; SYSTEMS AB In this study, based on the number of modes, the original three-dimensional Lorenz model (3DLM) is generalized with two additional modes [five-dimensional Lorenz model (5DLM)] to examine their role in the predictability of the numerical solutions and to understand the underlying processes that increase the solution stability. As a result of the simplicity of the 5DLM with respect to existing generalized Lorenz models (LMs), the author is able to obtain the analytical solutions of its critical points and identify the role of the major nonlinear term in the solution's stability, which have previously not been documented in the literature. The nonlinear Jacobian terms of the governing equations are analyzed to highlight the importance of selecting new modes for extending the nonlinear feedback loop of the 3DLM and thus effectively increasing the degree of nonlinearity (i.e., the nonlinear mode-mode interactions) in the 5DLM. It is then shown that numerical solutions in the 5DLM require a larger normalized Rayleigh number r for the onset of chaos and are more predictable than those in the 3DLM when r is between 25 and 40 and the Prandtl number sigma is 10. The improved predictability is attributable to the negative nonlinear feedback enabled by the new modes. The role of the (negative) nonlinear feedback is further verified using a revised 3DLM with a parameterized nonlinear eddy dissipative term. The finding of the increased stability in the 5DLM and revised 3DLM with respect to the 3DLM is confirmed with the linear stability analysis and the analysis of the Lyapunov exponents using different values of r and sigma. To further understand the impact of an additional heating term, results from the 5DLM and a higher-dimensional LM [e.g., the six-dimensional LM (6DLM)] are analyzed and compared. C1 [Shen, Bo-Wen] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Shen, Bo-Wen] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Shen, BW (reprint author), NASA, Mesoscale Atmospher Proc Lab, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA. EM bo-wen.shen-1@nasa.gov FU NASA Advanced Information System Technology (AIST) program of the Earth Science Technology Office (ESTO); NASA Computational Modeling Algorithms and Cyberinfrastructure (CMAC) program FX We thank anonymous reviewers, Drs. Y.-L. Lin, R. Anthes, X. Zeng, R. Pielke, J. Dutton, A. Molod, H.-M. H. Juang, S. Cheung, C.-L. Shie, and Y.-L. Wu for their valuable comments and encouragement, Professor Z. Wu for providing the code for the calculation of Gaussian white noise, and Ms. J. Dunbar and K. Massaro for proofreading this manuscript. We are grateful for support from the NASA Advanced Information System Technology (AIST) program of the Earth Science Technology Office (ESTO) and from the NASA Computational Modeling Algorithms and Cyberinfrastructure (CMAC) program. Resources supporting this work were provided by the NASA High-End Computing (HEC) program through the NASA Advanced Supercomputing division at Ames Research Center. Special thanks are due to the library personnel of NASA GSFC Library for helping obtain a copy of several classical journal articles. NR 42 TC 7 Z9 7 U1 0 U2 7 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 MAY PY 2014 VL 71 IS 5 BP 1701 EP 1723 DI 10.1175/JAS-D-13-0223.1 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF8UQ UT WOS:000334991500011 ER PT J AU Chung, D Matheou, G AF Chung, Daniel Matheou, Georgios TI Large-Eddy Simulation of Stratified Turbulence. Part I: A Vortex-Based Subgrid-Scale Model SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article DE Large eddy simulations; Subgrid-scale processes ID PLANETARY BOUNDARY-LAYER; STRETCHED SPIRAL VORTICES; ATMOSPHERIC SURFACE-LAYER; ISOTROPIC TURBULENCE; CHANNEL FLOW; NUMERICAL-SIMULATION; CUMULUS CONVECTION; ENERGY-DISSIPATION; STRESS MODEL; VELOCITY AB The stretched-vortex subgrid-scale (SGS) model is extended to enable large-eddy simulation of buoyancy-stratified turbulence. Both stable and unstable stratifications are considered. The extended model retains the anisotropic form of the original stretched-vortex model, but the SGS kinetic energy and the characteristic SGS eddy size are modified by buoyancy subject to two constraints: first, the SGS kinetic energy dynamics is determined by stationary and homogeneous conditions, and second, the SGS eddy size obeys a scaling analogous to the Monin-Obukhov similarity theory. The SGS model construction, comprising an ensemble of subgrid stretched-vortical structures, naturally limits vertical mixing but allows horizontal mixing provided the alignment of the SGS vortex ensemble is favorable, even at high nominal gradient Richardson numbers. In very stable stratification, the model recovers the z-less limit, in which a vortex-based Obukhov length controls the SGS dynamics, while in very unstable stratification, the model recovers the free-convection limit, in which a vortex-based Deardorff velocity controls the SGS dynamics. The efficacy of the present SGS model is demonstrated by simulating the canonical stationary and homogeneous, stratified sheared turbulence at high Reynolds numbers and moderately high Richardson numbers. In the postprocessing, the SGS dynamics of the stretched-vortex model is further interrogated to yield predictions of buoyancy-adjusted one-dimensional SGS spectra and SGS root-mean-square velocity-derivative fluctuations. C1 [Chung, Daniel] Univ Melbourne, Dept Mech Engn, Melbourne, Vic 3010, Australia. [Matheou, Georgios] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Chung, D (reprint author), Univ Melbourne, Dept Mech Engn, Melbourne, Vic 3010, Australia. EM daniel.chung@unimelb.edu.au RI Chung, Daniel/F-4468-2016 OI Chung, Daniel/0000-0003-3732-364X FU Office of Naval Research, Marine Meteorology Program [N0001411IP20087, N0001411IP20069]; NASA MAP Program; NOAA/CPO MAPP Program; National Aeronautics and Space Administration FX Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. We acknowledge the support provided by the Office of Naval Research, Marine Meteorology Program, under Awards N0001411IP20087 and N0001411IP20069, the NASA MAP Program, and the NOAA/CPO MAPP Program. 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 69 TC 11 Z9 11 U1 0 U2 11 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 MAY PY 2014 VL 71 IS 5 BP 1863 EP 1879 DI 10.1175/JAS-D-13-0126.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF8UQ UT WOS:000334991500019 ER PT J AU Johansen, CT Mcrae, CD Danehy, PM Gallo, ECA Cantu, LML Magnotti, G Cutler, AD Rockwell, RD Goyne, CP McDaniel, JC AF Johansen, Craig T. McRae, Colin D. Danehy, Paul M. Gallo, Emanuela C. A. Cantu, Luca M. L. Magnotti, Gaetano Cutler, Andrew D. Rockwell, Robert D., Jr. Goyne, Chris P. McDaniel, James C. TI OH PLIF visualization of the UVa supersonic combustion experiment: configuration A SO JOURNAL OF VISUALIZATION LA English DT Article DE Flow visualization; Planar laser-induced fluorescence; Supersonic combustion ID SCRAMJET ENGINES; TUNNEL AB Hydroxyl radical (OH) planar laser-induced fluorescence (PLIF) visualizations were performed in the University of Virginia supersonic combustion experiment. The test section was set up in configuration A, which includes a Mach 2 nozzle, combustor, and extender section. Hydrogen fuel was injected through an unswept compression ramp at two different equivalence ratios. Through the translation of the optical system and the use of two separate camera views, the entire optically accessible range of the combustor was imaged. Single-shot, average, and standard deviation images of the OH PLIF signal are presented at several streamwise locations. The results show the development of a highly turbulent flame structure and provide an experimental database to be used for numerical model assessment. C1 [Johansen, Craig T.; McRae, Colin D.] Univ Calgary, Calgary, AB, Canada. [Danehy, Paul M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Gallo, Emanuela C. A.; Cantu, Luca M. L.; Magnotti, Gaetano; Cutler, Andrew D.] George Washington Univ, Newport News, VA USA. [Rockwell, Robert D., Jr.; Goyne, Chris P.; McDaniel, James C.] Univ Virginia, Charlottesville, VA USA. RP Mcrae, CD (reprint author), Univ Calgary, Calgary, AB, Canada. EM johansen@ucalgary.ca; mcraec@ucalgary.ca OI Magnotti, Gaetano/0000-0002-1723-5258 FU Natural Sciences and Engineering Research Council of Canada (NSERC); Air Force Office of Scientific Research (AFOSR); NASA National Center for Hypersonic Combined Cycle Propulsion [FA 9550-09-1-0611] FX Dr. Johansen was supported by the Natural Sciences and Engineering Research Council of Canada (NSERC). This work was supported by the Air Force Office of Scientific Research (AFOSR) and NASA National Center for Hypersonic Combined Cycle Propulsion grant FA 9550-09-1-0611. The technical monitors are Chiping Li from the AFOSR and Rick Gaffney from NASA. NR 22 TC 6 Z9 6 U1 3 U2 20 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1343-8875 EI 1875-8975 J9 J VISUAL-JAPAN JI J. Vis. PD MAY PY 2014 VL 17 IS 2 BP 131 EP 141 DI 10.1007/s12650-014-0197-2 PG 11 WC Computer Science, Interdisciplinary Applications; Imaging Science & Photographic Technology SC Computer Science; Imaging Science & Photographic Technology GA AF1XJ UT WOS:000334506900005 ER PT J AU Clarke, GB Wilson, EL Miller, JH Melroy, HR AF Clarke, G. B. Wilson, E. L. Miller, J. H. Melroy, H. R. TI Uncertainty analysis for the miniaturized laser heterodyne radiometer (mini-LHR) for the measurement of carbon dioxide in the atmospheric column SO MEASUREMENT SCIENCE AND TECHNOLOGY LA English DT Article DE laser heterodyne radiometer; carbon dioxide ( CO2); radio frequency ( RF) receiver; column abundance; remote sensing ID AERONET AB Presented here is a sensitivity analysis for the miniaturized laser heterodyne radiometer. This passive, ground-based instrument measures carbon dioxide (CO2) in the atmospheric column and has been under development at NASA/ GSFC since 2009. The goal of this development is to produce a low-cost, easily-deployable instrument that can extend current ground measurement networks in order to (1) validate column satellite observations, (2) provide coverage in regions of limited satellite observations, (3) target regions of interest such as thawing permafrost, and (4) support the continuity of a long-term climate record. In this paper an uncertainty analysis of the instrument performance is presented and compared with results from three sets of field measurements. The signal-to-noise ratio (SNR) and corresponding maximum uncertainty for a single scan are calculated to be 329.4 +/- 1.3 by deploying error propagation through the equation governing the SNR. Reported is an absorbance noise of 0.0024 for six averaged scans of field data, for an instrument precision of 0.14 ppmv for CO2. C1 [Clarke, G. B.] Amer Univ, Washington, DC 20016 USA. [Clarke, G. B.; Wilson, E. L.; Melroy, H. R.] NASA, Goddard Space Flight Ctr, Laser Remote Sensing Lab, Greenbelt, MD 20771 USA. [Miller, J. H.; Melroy, H. R.] George Washington Univ, Dept Chem, Washington, DC 20052 USA. RP Clarke, GB (reprint author), Amer Univ, 4400 Massachusetts Ave, Washington, DC 20016 USA. EM gclarke@american.edu NR 14 TC 2 Z9 2 U1 3 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0957-0233 EI 1361-6501 J9 MEAS SCI TECHNOL JI Meas. Sci. Technol. PD MAY PY 2014 VL 25 IS 5 AR 055204 DI 10.1088/0957-0233/25/5/055204 PG 5 WC Engineering, Multidisciplinary; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA AE9TD UT WOS:000334352000022 ER PT J AU Lane, WM Cotton, WD van Velzen, S Clarke, TE Kassim, NE Helmboldt, JF Lazio, TJW Cohen, AS AF Lane, W. M. Cotton, W. D. van Velzen, S. Clarke, T. E. Kassim, N. E. Helmboldt, J. F. Lazio, T. J. W. Cohen, A. S. TI The Very Large Array Low-frequency Sky Survey Redux (VLSSr) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: image processing; catalogues; surveys; radio continuum: general ID STAR-FORMATION HISTORY; RADIO-SOURCES; SOURCE CATALOG; SPECTRUM; EVOLUTION; GALAXIES; UNIVERSE; SCALE; AREA AB We present the results of a recent re-reduction of the data from the Very Large Array (VLA) Low-frequency Sky Survey (VLSS). We used the VLSS catalogue as a sky model to correct the ionospheric distortions in the data and create a new set of sky maps and corresponding catalogue at 73.8 MHz. The VLSS Redux (VLSSr) has a resolution of 75 arcsec, and an average map rms noise level of Sigma similar to 0.1 Jy beam(-1). The clean bias is 0.66 x Sigma and the theoretical largest angular size is 36 arcmin. Six previously unimaged fields are included in the VLSSr, which has an unbroken sky coverage over 9.3 sr above an irregular southern boundary. The final catalogue includes 92 964 sources. The VLSSr improves upon the original VLSS in a number of areas including imaging of large sources, image sensitivity, and clean bias; however the most critical improvement is the replacement of an inaccurate primary beam correction which caused source flux errors which vary as a function of radius to nearest pointing centre in the VLSS. C1 [Lane, W. M.; Clarke, T. E.; Kassim, N. E.; Helmboldt, J. F.] Naval Res Lab, Washington, DC 20375 USA. [Cotton, W. D.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [van Velzen, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cohen, A. S.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Lane, WM (reprint author), Naval Res Lab, Code 7213,4555 Overlook Ave SW, Washington, DC 20375 USA. EM wendy.peters@nrl.navy.mil RI Helmboldt, Joseph/C-8105-2012 FU 6.1 base funds; National Aeronautics and Space Administration FX Basic research at the Naval Research Lab is supported by 6.1 base funds. We thank E. Polisensky for help with the graphics. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 42 TC 59 Z9 59 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2014 VL 440 IS 1 BP 327 EP 338 DI 10.1093/mnras/stu256 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4OD UT WOS:000334691900026 ER PT J AU Negrello, M Hopwood, R Dye, S da Cunha, E Serjeant, S Fritz, J Rowlands, K Fleuren, S Bussmann, RS Cooray, A Dannerbauer, H Gonzalez-Nuevo, J Lapi, A Omont, A Amber, S Auld, R Baes, M Buttiglione, S Cava, A Danese, L Dariush, A De Zotti, G Dunne, L Eales, S Ibar, E Ivison, RJ Kim, S Leeuw, L Maddox, S Michalowski, MJ Massardi, M Pascale, E Pohlen, M Rigby, E Smith, DJB Sutherland, W Temi, P Wardlow, J AF Negrello, M. Hopwood, R. Dye, S. da Cunha, E. Serjeant, S. Fritz, J. Rowlands, K. Fleuren, S. Bussmann, R. S. Cooray, A. Dannerbauer, H. Gonzalez-Nuevo, J. Lapi, A. Omont, A. Amber, S. Auld, R. Baes, M. Buttiglione, S. Cava, A. Danese, L. Dariush, A. De Zotti, G. Dunne, L. Eales, S. Ibar, E. Ivison, R. J. Kim, S. Leeuw, L. Maddox, S. Michalowski, M. J. Massardi, M. Pascale, E. Pohlen, M. Rigby, E. Smith, D. J. B. Sutherland, W. Temi, P. Wardlow, J. TI Herschel-ATLAS: deep HST/WFC3 imaging of strongly lensed submillimetre galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: strong; galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation; infrared: galaxies; submillimetre: galaxies ID SCIENCE DEMONSTRATION PHASE; EXTRAGALACTIC SURVEY; LUMINOSITY FUNCTIONS; INFRARED-EMISSION; HIGH-REDSHIFT; SIMPLE-MODEL; BLACK-HOLES; DUST; EVOLUTION; STELLAR AB We report on deep near-infrared observations obtained with the Wide Field Camera-3 (WFC3) onboard the Hubble Space Telescope (HST) of the first five confirmed gravitational lensing events discovered by the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). We succeed in disentangling the background galaxy from the lens to gain separate photometry of the two components. The HST data allow us to significantly improve on previous constraints of the mass in stars of the lensed galaxy and to perform accurate lens modelling of these systems, as described in the accompanying paper by Dye et al. We fit the spectral energy distributions of the background sources from near-IR to millimetre wavelengths and use the magnification factors estimated by Dye et al. to derive the intrinsic properties of the lensed galaxies. We find these galaxies to have star-formations rates (SFR) similar to 400-2000 M-circle dot yr(-1), with similar to(6-25) x 10(10) M-circle dot of their baryonic mass already turned into stars. At these rates of star formation, all remaining molecular gas will be exhausted in less than similar to 100 Myr, reaching a final mass in stars of a few 10(11) M-circle dot. These galaxies are thus proto-ellipticals caught during their major episode of star formation, and observed at the peak epoch (z similar to 1.5-3) of the cosmic star formation history of the Universe. C1 [Negrello, M.; Buttiglione, S.; De Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. [Dye, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [da Cunha, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Serjeant, S.; Amber, S.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Fritz, J.; Baes, M.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Rowlands, K.] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Fleuren, S.; Sutherland, W.] Univ London, Sch Math Sci, London E1 4NS, England. [Bussmann, R. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bussmann, R. S.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Cooray, A.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dannerbauer, H.] Univ Vienna, Inst Astron, A-1160 Vienna, Austria. [Gonzalez-Nuevo, J.] Inst Fis Cantabria CSIC UC, E-39005 Santander, Spain. [Lapi, A.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Lapi, A.; Danese, L.; De Zotti, G.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Omont, A.] Univ Paris 06, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Omont, A.] CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Auld, R.; Dariush, A.; Eales, S.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Cava, A.] Univ Geneva, Observ Geneve, CH-1290 Versoix, Switzerland. [Dunne, L.; Maddox, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Ibar, E.] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile. [Ivison, R. J.] European So Observ, D-85748 Garching, Germany. [Ivison, R. J.; Michalowski, M. J.] Univ Edinburgh, Inst Astron, Scottish Univ Phys Alliance, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Kim, S.] Catholic Univ Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Leeuw, L.] UNISA, Coll Grad Studies, ZA-0003 Unisa, South Africa. [Massardi, M.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [Rigby, E.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Smith, D. J. B.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. RP Negrello, M (reprint author), Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. EM mattia.negrello@oapd.inaf.it RI Wardlow, Julie/C-9903-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Ivison, R./G-4450-2011; Cava, Antonio/C-5274-2017; OI Baes, Maarten/0000-0002-3930-2757; Maddox, Stephen/0000-0001-5549-195X; Dye, Simon/0000-0002-1318-8343; Wardlow, Julie/0000-0003-2376-8971; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Smith, Daniel/0000-0001-9708-253X; Ivison, R./0000-0001-5118-1313; Cava, Antonio/0000-0002-4821-1275; De Zotti, Gianfranco/0000-0003-2868-2595 FU STFC [PP/D002400/1, ST/G002533/1]; ASI/INAF [I/072/09/0]; PRIN-INAF; Spanish Ministerio de Ciencia e Innovacion [AYA2010-21766-C03-01]; Spanish CSIC; European Social Fund; National Aeronautics and Space Administration FX This work was supported by STFC (grants PP/D002400/1 and ST/G002533/1), by ASI/INAF agreement I/072/09/0, by PRIN-INAF 2012 project 'Looking into the dust-obscured phase of galaxy formation through cosmic zoom lenses in the Herschel Astrophysical Large Area Survey' and, in part, by the Spanish Ministerio de Ciencia e Innovacion (project AYA2010-21766-C03-01). JGN acknowledges financial support from the Spanish CSIC for a JAE-DOC fellowship, co-funded by the European Social Fund. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The Herschel-ATLAS is a project with Herschel, which is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS website is http://www.h-atlas.org/. This publication makes use of data products from the WISE, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 61 TC 26 Z9 26 U1 0 U2 15 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2014 VL 440 IS 3 BP 1999 EP 2012 DI 10.1093/mnras/stu413 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5HG UT WOS:000334744000009 ER PT J AU Marinucci, A Matt, G Kara, E Miniutti, G Elvis, M Arevalo, P Ballantyne, DR Balokovic, M Bauer, F Brenneman, L Boggs, SE Cappi, M Christensen, FE Craig, WW Fabian, AC Fuerst, F Hailey, CJ Harrison, FA Risaliti, G Reynolds, CS Stern, DK Walton, DJ Zhang, W AF Marinucci, A. Matt, G. Kara, E. Miniutti, G. Elvis, M. Arevalo, P. Ballantyne, D. R. Balokovic, M. Bauer, F. Brenneman, L. Boggs, S. E. Cappi, M. Christensen, F. E. Craig, W. W. Fabian, A. C. Fuerst, F. Hailey, C. J. Harrison, F. A. Risaliti, G. Reynolds, C. S. Stern, D. K. Walton, D. J. Zhang, W. TI Simultaneous NuSTAR and XMM-Newton 0.5-80 keV spectroscopy of the narrow-line Seyfert 1 galaxy SWIFT J2127.4+5654 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; galaxies: active; galaxies: individual: SWIFT J2127.4+5654; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; HIGH-ENERGY OBSERVATIONS; PHOTON IMAGING CAMERA; RAY-EMITTING REGION; X-RAY; IRON K; BEPPOSAX OBSERVATIONS; REVERBERATION LAGS; COSMIC EVOLUTION AB We present a broad-band spectral analysis of the joint XMM-Newton and Nuclear Spectroscopic Telescope Array observational campaign of the narrow-line Seyfert 1 SWIFT J2127.4+5654, consisting of 300 ks performed during three XMM-Newton orbits. We detect a relativistic broadened iron K alpha line originating from the innermost regions of the accretion disc surrounding the central black hole, from which we infer an intermediate spin of a = 0.58(-0.17)(+0.11). The intrinsic spectrum is steep (Gamma = 2.08 +/- 0.01) as commonly found in narrow-line Seyfert 1 galaxies, while the cutoff energy (Ec = 108(-10)(+11)kev) falls within the range observed in broad-line Seyfert 1 galaxies. We measure a low-frequency lag that increases steadily with energy, while at high frequencies, there is a clear lag following the shape of the broad Fe K emission line. Interestingly, the observed Fe K lag in SWIFT J2127.4+5654 is not as broad as in other sources that have maximally spinning black holes. The lag amplitude suggests a continuum-to-reprocessor distance of about 10-20 r(g). These timing results independently support an intermediate black hole spin and a compact corona. C1 [Marinucci, A.; Matt, G.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. [Kara, E.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Miniutti, G.] Ctr Astrobiol CSIC INTA, Dep Astrofis, E-28691 Madrid, Spain. [Miniutti, G.] ESAC, E-28691 Madrid, Spain. [Elvis, M.; Brenneman, L.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Arevalo, P.; Bauer, F.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 22, Chile. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Balokovic, M.; Fuerst, F.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Cappi, M.] IASF Bologna, INAF, I-40129 Bologna, Italy. [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. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Risaliti, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Stern, D. K.] 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 Roma Tre, Dipartimento Fis, Via Vasca Navale 84, I-00146 Rome, Italy. EM marinucci@fis.uniroma3.it RI Miniutti, Giovanni/L-2721-2014; Boggs, Steven/E-4170-2015; Cappi, Massimo/F-4813-2015; OI Miniutti, Giovanni/0000-0003-0707-4531; Boggs, Steven/0000-0001-9567-4224; Cappi, Massimo/0000-0001-6966-8920; Risaliti, Guido/0000-0002-3556-977X FU Italian Space Agency [ASI/INAFI/037/12/0-011/13]; European Union [312789]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024]; Anillo ACT1101; International Fulbright Science and Technology Award; NASA [NNG08FD60C]; National Aeronautics and Space Administration FX We thank the referee for her/his comments and suggestions that greatly improved the paper. AM thanks Javier Garcia and Thomas Dauser for the efforts in producing XILLVER and RELXILL tables to use in this paper. AM and GM acknowledge financial support from Italian Space Agency under grant ASI/INAFI/037/12/0-011/13 and from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789. PA and FB acknowledge support from Basal-CATA PFB-06/2007 (FEB), CONICYT-Chile FONDECYT 1101024 (FEB) and Anillo ACT1101 (FEB, PA). MB acknowledges support from the International Fulbright Science and Technology Award. This work was supported under NASA Contract no. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). NR 69 TC 47 Z9 47 U1 1 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2014 VL 440 IS 3 BP 2347 EP 2356 DI 10.1093/mnras/stu404 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5HG UT WOS:000334744000033 ER PT J AU Schultz, MR Rose, CA Guzman, JC McCarville, D Hilburger, MW AF Schultz, Marc R. Rose, Cheryl A. Guzman, J. Carlos McCarville, Douglas Hilburger, Mark W. TI An experimental study of the compression response of fluted-core composite panels with joints SO COMPOSITES PART B-ENGINEERING LA English DT Article DE Polymer matrix composites (PMCs); Mechanical testing; Joints/joining; Fluted-core sandwich composites AB Fluted-core sandwich composites consist of integral angled web members spaced between laminate facesheets, and may have the potential to provide benefits over traditional sandwich composites for certain aerospace applications. However, fabrication of large autoclave-cured fluted-core cylindrical shells with existing autoclaves will require that the shells be fabricated in segments, and joined longitudinally to form a complete barrel. Experiments on two different fluted-core longitudinal joint designs were considered in this study. In particular, jointed fluted-core-composite panels were tested in longitudinal compression because this is the primary loading condition in dry launch-vehicle barrel sections. One of the joint designs performed well in comparison with unjointed test articles, and the other joint design failed at loads approximately 14% lower than unjointed test articles. The compression-after-impact (CAI) performance of jointed fluted-core composites was also investigated with test articles that had been subjected to 6 ft-lb impacts from a 1/2-in, hemispherical indenter. It was found that such impacts reduced the load-carrying capability by 9 similar to 40%. This reduction was dependent on the joint concept. (C) 2014 Published by Elsevier Ltd. C1 [Schultz, Marc R.; Rose, Cheryl A.; Hilburger, Mark W.] NASA, Struct Mech & Concepts Branch, Langley Res Ctr, Hampton, VA 23681 USA. [Guzman, J. Carlos; McCarville, Douglas] Boeing Co, Boeing Res & Technol, Seattle, WA 98124 USA. RP Schultz, MR (reprint author), NASA, Struct Mech & Concepts Branch, Langley Res Ctr, Mail Stop 190, Hampton, VA 23681 USA. EM marc.r.schultz@nasa.gov FU NASA Engineering and Safety Center (NESC) Shell Buckling Knockdown Factor Project, NESC [07-010-E] FX This work was conducted as part of the NASA Engineering and Safety Center (NESC) Shell Buckling Knockdown Factor Project, NESC assessment number 07-010-E. All of the panels used to make the test articles discussed herein were produced and provided by The Boeing Company. Jeffrey Seebo of Analytical Mechanics Associates, Inc. at NASA Langley developed the system used for the ultrasonic scans and was instrumental in interpreting the data. The ultrasonic scans were performed by Richard Churray of NASA Langley. NR 7 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1359-8368 EI 1879-1069 J9 COMPOS PART B-ENG JI Compos. Pt. B-Eng. PD MAY PY 2014 VL 61 BP 229 EP 237 DI 10.1016/j.compositesb.2013.12.029 PG 9 WC Engineering, Multidisciplinary; Materials Science, Composites SC Engineering; Materials Science GA AE6UQ UT WOS:000334133900027 ER PT J AU Burow, LC Woebken, D Marshall, IPG Singer, SW Pett-Ridge, J Prufert-Bebout, L Spormann, AM Bebout, BM Weber, PK Hoehler, TM AF Burow, L. C. Woebken, D. Marshall, I. P. G. Singer, S. W. Pett-Ridge, J. Prufert-Bebout, L. Spormann, A. M. Bebout, B. M. Weber, P. K. Hoehler, T. M. TI Identification of Desulfobacterales as primary hydrogenotrophs in a complex microbial mat community SO GEOBIOLOGY LA English DT Article ID SULFATE-REDUCING BACTERIA; SP-NOV; GEN. NOV.; DIVERSITY; SEDIMENTS; ECOLOGY; BIOGEOCHEMISTRY; METHANOGENESIS; SEQUENCES; REDUCTION AB Hypersaline microbial mats have been shown to produce significant quantities of H-2 under dark, anoxic conditions via cyanobacterial fermentation. This flux of a widely accessible microbial substrate has potential to significantly influence the ecology of the mat, and any consumption will affect the net efflux of H-2 that might otherwise be captured as a resource. Here, we focus on H-2 consumption in a microbial mat from Elkhorn Slough, California, USA, for which H-2 production has been previously characterized. Active biologic H-2 consumption in this mat is indicated by a significant time-dependent decrease in added H-2 compared with a killed control. Inhibition of sulfate reduction, as indicated by a decrease in hydrogen sulfide production relative to controls, resulted in a significant increase in H-2 efflux, suggesting that sulfate-reducing bacteria (SRB) are important hydrogenotrophs. Low methane efflux under these same conditions indicated that methanogens are likely not important hydrogenotrophs. Analyses of genes and transcripts that encode for rRNA or dissimilatory sulfite reductase, using both PCR-dependent and PCR-independent metatranscriptomic sequencing methods, demonstrated that Desulfobacterales are the dominant, active SRB in the upper, H-2-producing layer of the mat (0-2mm). This hypothesis was further supported by the identification of transcripts encoding hydrogenases derived from Desulfobacterales capable of H-2 oxidation. Analysis of molecular data provided no evidence for the activity of hydrogenotrophic methanogens. The combined biogeochemical and molecular data strongly indicate that SRB belonging to the Desulfobacterales are the quantitatively important hydrogenotrophs in the Elkhorn Slough mat. C1 [Burow, L. C.; Woebken, D.; Marshall, I. P. G.; Spormann, A. M.] Stanford Univ, Dept Chem Engn, Stanford, CA 94305 USA. [Burow, L. C.; Woebken, D.; Marshall, I. P. G.; Spormann, A. M.] Stanford Univ, Dept Civil Engn, Stanford, CA 94305 USA. [Burow, L. C.; Woebken, D.; Marshall, I. P. G.; Spormann, A. M.] Stanford Univ, Dept Environm Engn, Stanford, CA 94305 USA. [Burow, L. C.; Woebken, D.; Prufert-Bebout, L.; Bebout, B. M.; Hoehler, T. M.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Singer, S. W.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA 94720 USA. [Pett-Ridge, J.; Weber, P. K.] Lawrence Livermore Natl Lab, Div Chem Sci, Livermore, CA USA. RP Burow, LC (reprint author), IP Australia, Appl Chem & Biotechnol Sect, Dept Ind, Canberra, ACT, Australia. EM tori.m.hoehler@nasa.gov; tori.m.hoehler@nasa.gov RI Woebken, Dagmar/A-4447-2013; OI Woebken, Dagmar/0000-0002-1314-9926 FU US Department of Energy at Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; US Department of Energy at Lawrence Berkeley National Laboratory [DE-AC02-05CH11231]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; German Research Foundation (Deutsche Forschungsgemeinschaft); US. Department of Energy (DOE) Genomic Science Program [SCW1039] FX We thank Angela Detweiler and Adrienne Frisbee at the NASA Ames Research Center for technical support and Tijana Glavina del Rio, Susannah Tringe, Erika Lindquist and Stephanie Malfatti at the Joint Genome Institute for assistance obtaining rRNA pyrotag and metatranscriptomic sequences. We thank Jeff Cann, Associate Wildlife Biologist, Central Region, California Department of Fish and Game for coordinating our access to the Elkhorn Slough Wildlife Area. Work at LLNL was performed under the auspices of the US Department of Energy at Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. Work at LBNL was performed under the auspices of the US Department of Energy at Lawrence Berkeley National Laboratory under Contract DE-AC02-05CH11231. Pyrotag and metatranscriptomic sequencing were conducted by the Joint Genome Institute, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. DW was partially funded by the German Research Foundation (Deutsche Forschungsgemeinschaft). Funding was provided by the US. Department of Energy (DOE) Genomic Science Program under contract SCW1039. NR 47 TC 8 Z9 8 U1 6 U2 35 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 MAY PY 2014 VL 12 IS 3 BP 221 EP 230 DI 10.1111/gbi.12080 PG 10 WC Biology; Environmental Sciences; Geosciences, Multidisciplinary SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Geology GA AE9WI UT WOS:000334361800004 PM 24730641 ER PT J AU Russell, JA Brady, AL Cardman, Z Slater, GF Lim, DSS Biddle, JF AF Russell, J. A. Brady, A. L. Cardman, Z. Slater, G. F. Lim, D. S. S. Biddle, J. F. TI Prokaryote populations of extant microbialites along a depth gradient in Pavilion Lake, British Columbia, Canada SO GEOBIOLOGY LA English DT Article ID MODERN MARINE STROMATOLITES; FRESH-WATER MICROBIALITES; CANDIDATUS CHLORACIDOBACTERIUM THERMOPHILUM; LITHIFIED MICRITIC LAMINAE; SULFATE-REDUCING BACTERIA; DRY VALLEY LAKES; CUATRO CIENEGAS; SHARK BAY; COMPARATIVE METAGENOMICS; WESTERN-AUSTRALIA AB Pavilion Lake in British Columbia, Canada, is home to modern-day microbialites that are actively growing at multiple depths within the lake. While microbialite morphology changes with depth and previous isotopic investigations suggested a biological role in the formation of these carbonate structures, little is known about their microbial communities. Microbialite samples acquired through the Pavilion Lake Research Project (PLRP) were first investigated for phototrophic populations using Cyanobacteria-specific primers and 16S rRNA gene cloning. These data were expounded on by high-throughput tagged sequencing analyses of the general bacteria population. These molecular analyses show that the microbial communities of Pavilion Lake microbialites are diverse compared to non-lithifying microbial mats also found in the lake. Phototrophs and heterotrophs were detected, including species from the recently described Chloroacidobacteria genus, a photoheterotroph that has not been previously observed in microbialite systems. Phototrophs were shown as the most influential contributors to community differences above and below 25 meters, and corresponding shifts in heterotrophic populations were observed at this interface as well. The isotopic composition of carbonate also mirrored this shift in community states. Comparisons to previous studies indicated this population shift may be a consequence of changes in lake chemistry at this depth. Microbial community composition did not correlate with changing microbialite morphology with depth, suggesting something other than community changes may be a key to observed variations in microbialite structure. C1 [Russell, J. A.; Biddle, J. F.] Univ Delaware, Sch Marine Sci & Policy, Lewes, DE 19958 USA. [Brady, A. L.] Univ Calgary, Dept Biol Sci, Calgary, AB T2N 1N4, Canada. [Cardman, Z.] Univ N Carolina, Chapel Hill, NC USA. [Slater, G. F.] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON, Canada. [Lim, D. S. S.] NASA Ames Res Ctr, Moffett Field, CA USA. [Lim, D. S. S.] SETI Inst, Mountain View, CA USA. RP Biddle, JF (reprint author), Univ Calgary, Dept Biol Sci, 2500 Univ Dr 1 NW, Calgary, AB T2N 1N4, Canada. EM jfbiddle@udel.edu RI Biddle, Jennifer/F-8323-2010; OI Biddle, Jennifer/0000-0002-4344-8724; Russell, Joseph/0000-0002-0623-5519 FU NASA Moon and Mars Analog Mission Activities (MMAMA) grant; Canadian Space Agency's (CSA) Canadian Analogue Research Network (CARN); Analogue Missions programs, Nuytco Research, the Delaware Space Grant Consortium; NASA CAN [NNX10AN63H]; Marian R. Okie Fellowship; National Science Foundation EPSCoR Grant [EPS-0814251]; State of Delaware FX Special thanks to Donnie Reid and all members of the PLRP field team, especially the science divers and deep worker pilots who collected the samples. We thank Jennifer Hansen for laboratory assistance with carbonate measurements. This work was supported by the NASA Moon and Mars Analog Mission Activities (MMAMA) grant to D. Lim, the Canadian Space Agency's (CSA) Canadian Analogue Research Network (CARN), and Analogue Missions programs, Nuytco Research, the Delaware Space Grant Consortium funded by NASA CAN NNX10AN63H to D. Mullan and by the UD College of Earth, Ocean, and Environment. J. Russell was supported by a Marian R. Okie Fellowship. This publication was made possible by the National Science Foundation EPSCoR Grant No. EPS-0814251 and the State of Delaware. We are also grateful to Linda and Mickey Macri for hosting the PLRP project from 2004 to present and to the Ts'Kw'aylaxw First Nation and British Columbia Parks for their continued support of our research. This is Pavilion Lake Research Project publication # 13-02. NR 63 TC 7 Z9 7 U1 0 U2 23 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 MAY PY 2014 VL 12 IS 3 BP 250 EP 264 DI 10.1111/gbi.12082 PG 15 WC Biology; Environmental Sciences; Geosciences, Multidisciplinary SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Geology GA AE9WI UT WOS:000334361800006 PM 24636451 ER PT J AU Benafan, O Noebe, RD Padula, SA Brown, DW Vogel, S Vaidyanathan, R AF Benafan, O. Noebe, R. D. Padula, S. A., II Brown, D. W. Vogel, S. Vaidyanathan, R. TI Thermomechanical cycling of a NiTi shape memory alloy-macroscopic response and microstructural evolution SO INTERNATIONAL JOURNAL OF PLASTICITY LA English DT Article DE Phase transformation; Microstructures; Twinning; Polycrystalline material; Mechanical testing ID REVERSIBLE MARTENSITIC-TRANSFORMATION; LOW-TEMPERATURE CREEP; TI-NI; TEXTURE ANALYSIS; NEUTRON-DIFFRACTION; ELECTRICAL-RESISTIVITY; PHASE-TRANSFORMATIONS; CONSTITUTIVE MODEL; BINARY NITI; R-PHASE AB Thermomechanical cycling of a Ni49.9Ti50.1 (at.%) shape memory alloy was investigated. Combined ex situ macroscopic experiments and in situ neutron diffraction measurements were performed to relate the macroscopic evolution in behavior (e.g., dimensional instabilities) observed during thermal cycling to the responsible microscopic mechanism(s) through texture, internal strain, peak shape, and phase evolution from the neutron data. Pre-deformation in the austenite or martensite phases affected the macroscopic cyclic behavior (e.g., actuation strain), depending on the level of pre-strain and the associated microstructural changes. However, the pre-deformation did not completely stabilize the cyclic response. Subsequent thermomechanical cycling revealed that the martensite texture changed with continued thermal cycling, while the austenite texture did not. For the conditions investigated, stagnation of the martensite texture occurred around the eighth cycle, consistent with asymptotic saturation of the macroscopic transformation strains. Moreover, diffraction spectra peak shapes (broadening) were found to vary with cycling indicative of the accumulation of lattice defects, consistent with the constant increase in residual strain. Published by Elsevier Ltd. C1 [Benafan, O.; Vaidyanathan, R.] Univ Cent Florida, Adv Mat Proc & Anal Ctr, Mech Mat & Aerosp Engn Dept, Orlando, FL 32816 USA. [Benafan, O.; Noebe, R. D.; Padula, S. A., II] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. [Brown, D. W.; Vogel, S.] Los Alamos Natl Lab, Lujan Ctr, Los Alamos, NM 87545 USA. RP Benafan, O (reprint author), NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. EM othmane.benafan@nasa.gov OI Vogel, Sven C./0000-0003-2049-0361 FU NASA Fundamental Aeronautics Program, Aeronautical Sciences Project; Office of Basic Energy Sciences DOE; DOE [DE-AC52-06NA25396]; [NNX08AB51A] FX Funding from the NASA Fundamental Aeronautics Program, Aeronautical Sciences Project is gratefully acknowledged. Grant NNX08AB51A to UCF is gratefully acknowledged. The authors thank B. Clausen, T. Sisneros and M. Helmut at LANL and D. Gaydosh, A. Garg and G. Bigelow at NASA GRC for technical support and helpful discussions. D.E. Nicholson's help in performing the neutron diffraction experiments is gratefully acknowledged. This work has benefited from the use of the Lujan Neutron Scattering Center at LANSCE, which is funded by the Office of Basic Energy Sciences DOE. LANL is operated by Los Alamos National Security LLC under DOE Contract No. DE-AC52-06NA25396. NR 89 TC 20 Z9 21 U1 4 U2 41 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0749-6419 EI 1879-2154 J9 INT J PLASTICITY JI Int. J. Plast. PD MAY PY 2014 VL 56 BP 99 EP 118 DI 10.1016/j.ijplas.2014.01.006 PG 20 WC Engineering, Mechanical; Materials Science, Multidisciplinary; Mechanics SC Engineering; Materials Science; Mechanics GA AE6EI UT WOS:000334083000005 ER PT J AU Goldberg, RK Binienda, WK AF Goldberg, Robert K. Binienda, Wieslaw K. TI Special Section on Advances in Ballistic Impact and Crashworthiness Response of Aerospace Structures SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Editorial Material C1 [Goldberg, Robert K.] NASA, Res Aerosp Engn, Glenn Res Ctr, Cleveland, OH 44135 USA. [Binienda, Wieslaw K.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA. RP Goldberg, RK (reprint author), NASA, Res Aerosp Engn, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Robert.K.Goldberg@nasa.gov; wbinienda@uakron.edu NR 0 TC 0 Z9 0 U1 2 U2 18 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 MAY 1 PY 2014 VL 27 IS 3 BP 423 EP 423 DI 10.1061/(ASCE)AS.1943-5525.0000414 PG 1 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA AE9RU UT WOS:000334347400001 ER PT J AU Jackson, KE Fasanella, EL Polanco, MA AF Jackson, K. E. Fasanella, E. L. Polanco, M. A. TI Simulating the Response of a Composite Honeycomb Energy Absorber. I: Dynamic Crushing of Components and Multiterrain Impacts SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE LS-DYNA; Composite materials; Structural impact; Multiterrain impact; Explicit simulation; Energy absorption; Crushing ID FUSELAGE SECTION AB This paper describes the experimental and analytical evaluation of an externally deployable composite honeycomb structure that is designed to attenuate impact energy during helicopter crashes. The concept, designated the deployable energy absorber (DEA), uses an expandable Kevlar honeycomb to dissipate kinetic energy through crushing. The DEA incorporates a unique flexible-hinge design that enables the honeycomb to be packaged and stowed efficiently until needed for deployment. Experimental evaluation of the DEA included dynamic crush tests of multicell components and vertical drop tests of a composite fuselage section retrofitted with DEA blocks onto multiterrain. Finite-element models of the test articles were developed and simulations were performed using the transient dynamic code LS-DYNA. In each simulation, the DEA was represented using shell elements assigned two different material properties: Mat 24, an isotropic piecewise linear plasticity model, and Mat 58, a continuum damage mechanics model used to represent laminated composite fabrics. DEA model development and test analysis comparisons are presented. C1 [Jackson, K. E.] NASA, Struct Dynam Branch, Langley Res Ctr, Hampton, VA 23681 USA. [Fasanella, E. L.] NASA, Natl Inst Aerosp, Langley Res Ctr, Hampton, VA 23681 USA. [Polanco, M. A.] Eagle Technol LLC, Hampton, VA 23666 USA. RP Jackson, KE (reprint author), NASA, Struct Dynam Branch, Langley Res Ctr, 12 West Bush Rd, Hampton, VA 23681 USA. EM karen.e.jackson-1@nasa.gov; edwin.l.fasanella@nasa.gov; mpolanco@eagleaviationtech.com NR 31 TC 1 Z9 1 U1 4 U2 31 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 MAY 1 PY 2014 VL 27 IS 3 BP 424 EP 436 DI 10.1061/(ASCE)AS.1943-5525.0000357 PG 13 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA AE9RU UT WOS:000334347400002 ER PT J AU Fasanella, EL Annett, MS Jackson, KE Polanco, MA AF Fasanella, E. L. Annett, M. S. Jackson, K. E. Polanco, M. A. TI Simulating the Response of a Composite Honeycomb Energy Absorber. II: Full-Scale Impact Testing SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE Explicit transient dynamic finite-element simulation; Energy absorption; Composite materials; Full-scale crash testing AB The National Aeronautics and Space Administration (NASA) has sponsored research to evaluate an externally deployable composite honeycomb designed to attenuate loads in the event of a helicopter crash. The concept, designated the deployable energy absorber (DEA), is an expandable Kevlar honeycomb. The DEA incorporates a flexible hinge that allows the honeycomb to be stowed collapsed until needed during an emergency. Evaluation of the DEA began with material characterization of the Kevlar-129 fabric/epoxy and ended with a full-scale crash test of a retrofitted MD-500 helicopter. During each evaluation phase, finite-element (FE) models of the test articles were developed, and simulations were performed using the dynamic FE code LS-DYNA. This paper focuses on simulations of two full-scale impact tests involving the DEA: a mass simulator and a DEA-retrofitted MD-500 helicopter. Isotropic (Mat 24) and composite (Mat 58) material models that were assigned to DEA shell elements were compared. Based on simulation results, the Mat 58 model showed better agreement with the test results. C1 [Fasanella, E. L.] NASA, Natl Inst Aerosp, Langley Res Ctr, Hampton, VA 23681 USA. [Annett, M. S.] NASA, Struct Dynam Branch, Langley Res Ctr, Hampton, VA USA. [Jackson, K. E.] NASA, Struct Dynam Branch, Langley Res Ctr, Hampton, VA 23681 USA. [Polanco, M. A.] Eagle Technol LLC, Hampton, VA 23666 USA. RP Fasanella, EL (reprint author), NASA, Natl Inst Aerosp, Langley Res Ctr, 12 West Bush Rd, Hampton, VA 23681 USA. EM edwin.l.fasanella@nasa.gov; martin.s.annett@nasa.gov; karen.e.jackson-1@nasa.gov; mpolanco@eagleaviationtech.com NR 20 TC 2 Z9 2 U1 0 U2 17 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 MAY 1 PY 2014 VL 27 IS 3 BP 437 EP 441 DI 10.1061/(ASCE)AS.1943-5525.0000358 PG 5 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA AE9RU UT WOS:000334347400003 ER PT J AU Vassilakos, GJ Hardy, RC AF Vassilakos, Gregory J. Hardy, Robin C. TI Sand Impact Tests of a Half-Scale Crew Module Test Article SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE Sand (material); Simulation models; Spacecraft; Impact tests AB Although the Orion Multi-Purpose Crew Vehicle (MPCV) is being designed primarily for water landings, the possibility exists of an onshore landing at Kennedy Space Center (KSC) following a launch abort. To obtain data to evaluate the adequacy of sand material models used in beach landing simulations, sand impact tests were conducted at National Aeronautics and Space Administration (NASA) Langley Research Center (LRC). Both vertical drop tests and swing tests with combined vertical and horizontal velocity were performed onto beds of common construction-grade sand using a geometrically scaled crew module test article. The tests were simulated using the explicit, nonlinear, transient dynamic finite-element code LS-DYNA. The shape of the test article was similar to a scaled crew module, but the structure was much heavier and was sufficiently robust to survive multiple impacts without permanent deformation. The focus was the sand model, not the structural response of the test article. The sand material models utilized in the simulations were based on tests of sand specimens. Although the LS-DYNA models provided reasonable predictions for peak accelerations, they were not always able to track the response through the duration of the impact. Further improvements to the material model used for the sand were identified based on results from the sand specimen tests. C1 [Vassilakos, Gregory J.] Analyt Mech Associates Inc, Hampton, VA 23666 USA. [Vassilakos, Gregory J.; Hardy, Robin C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Vassilakos, GJ (reprint author), Analyt Mech Associates Inc, 21 Enterprise Pkwy,Ste 300, Hampton, VA 23666 USA. EM gregory.j.vassilakos@nasa.gov; robin.c.hardy@nasa.gov FU NASA Orion Program Office via the Landing and Descent Deceleration Earth Recovery System (LADDERS); Structural Passive Landing Attenuation for Survivability of Human Crew (SPLASH) projects FX This paper describes work funded by the NASA Orion Program Office via the Landing and Descent Deceleration Earth Recovery System (LADDERS) and Structural Passive Landing Attenuation for Survivability of Human Crew (SPLASH) projects. NR 11 TC 1 Z9 1 U1 0 U2 6 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 MAY 1 PY 2014 VL 27 IS 3 BP 442 EP 455 DI 10.1061/(ASCE)AS.1943-5525.0000365 PG 14 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA AE9RU UT WOS:000334347400004 ER PT J AU Pereira, JM Revilock, DM Ruggeri, CR Emmerling, WC Altobelli, DJ AF Pereira, J. Michael Revilock, Duane M. Ruggeri, Charles R. Emmerling, William C. Altobelli, Donald J. TI Ballistic Impact Testing of Aluminum 2024 and Titanium 6Al-4V for Material Model Development SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE Material tests; Metals (materials); Material modeling; Impact tests AB Ballistic impact testing was conducted on aluminum (Al) 2024 and titanium (Ti) 6Al-4Vanadium (V) sheet and plate samples of different thicknesses. The tests were conducted on flat panels with two different areal dimensions: 61x61 cm (24x24 in.) (large panel) and 38x38 cm (15x15 in.) (small panel), with projectile velocities between 150 and 300 m/s (500 and 1,000 ft/s). The smaller panels were impacted in a normal direction with cylindrical projectiles ranging in diameter from 1.27 cm to 1.91 cm (0.5 to 0.75 in.). The larger panels involved a more complex projectile, with some features representing those of real turbine engine fan blades, impacting the panel in an oblique orientation. For the large panels, data are reported on the impact velocity and whether the projectile penetrated the panel; for the small panels, data are reported on the residual velocities. For thick panels, friction between the projectile and the panel as the projectile translated through the panel appear to play a large role in penetration. Projectile hardness affects the penetration velocity. The data presented here provide a useful tool for developing and validating impact models. C1 [Pereira, J. Michael; Revilock, Duane M.; Ruggeri, Charles R.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Emmerling, William C.] Atlantic City Int Airport, Struct & Mat Sect ANG E231, Fed Aviat Adm William J Hughes Tech Ctr, Atlantic City, NJ 08405 USA. [Altobelli, Donald J.] Atlantic City Int Airport, Fed Aviat Adm William J Hughes Tech Ctr, Atlantic City, NJ 08405 USA. RP Pereira, JM (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM J.M.Pereira@nasa.gov; revilock@nasa.gov; charles.r.ruggeri@nasa.gov; william.emmerling@faa.gov NR 5 TC 1 Z9 1 U1 0 U2 2 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 MAY 1 PY 2014 VL 27 IS 3 BP 456 EP 465 DI 10.1061/(ASCE)AS.1943-5525.0000356 PG 10 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA AE9RU UT WOS:000334347400005 ER PT J AU Zhang, C Binienda, WK Kohlman, LW AF Zhang, Chao Binienda, Wieslaw K. Kohlman, Lee W. TI Analytical Model and Numerical Analysis of the Elastic Behavior of Triaxial Braided Composites SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE Finite-element analysis; Elastic behavior; Braided composite; Undulation; Analytical model ID WOVEN FABRIC COMPOSITES; TEXTILE COMPOSITES; STRENGTH; PREDICTION; FAILURE AB This paper is concerned with elastic behavior of a triaxial braided composite by using a three-dimensional analytical model and mesoscale finite-element (FE) analysis, in conjunction with experimental observations. The analytical method and FEM take into account the actual fabric structure by considering the fiber undulation and actual architecture parameters. A representative unit cell model of the triaxial braided architecture is first identified based on fiber volume ratio, specimen thickness, and microscopic image analysis. Detailed geometric parameters for axial and bias fiber bundles are obtained, which provide precise information to enable the development of analytical and FE models. A general three-dimensional analytical model based on realistic architecture is developed with consideration of axial and bias fiber undulation. A typical study on the effect of axial fiber undulation is presented through the analytical model and axial tensile test. The prediction of effective elastic constants of the composite are presented and are compared with the experimental data. Edge damage, which is identified through FE simulation and experiments, is found to occur periodically along the free edge and to result in reduced transverse properties. The edge effect on the elastic modulus is studied through FE simulation with various numbers of unit cells. The axial fiber undulation and edge effect explains the discrepancy between the analytical and computational predictions and the experimental results. C1 [Zhang, Chao; Binienda, Wieslaw K.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA. [Kohlman, Lee W.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Zhang, C (reprint author), Univ Akron, Dept Civil Engn, Akron, OH 44325 USA. EM cz14@zips.uakron.edu; wbinienda@uakron.edu; lee.w.kohlman@nasa.gov RI Zhang, Chao/H-3397-2013 NR 36 TC 9 Z9 9 U1 4 U2 29 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 MAY 1 PY 2014 VL 27 IS 3 BP 473 EP 483 DI 10.1061/(ASCE)AS.1943-5525.0000369 PG 11 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA AE9RU UT WOS:000334347400007 ER PT J AU Wang, CX Yang, P Dessler, A Baum, BA Hu, YX AF Wang, Chenxi Yang, Ping Dessler, Andrew Baum, Bryan A. Hu, Yongxiang TI Estimation of the cirrus cloud scattering phase function from satellite observations SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Thin cirrus clouds; Optical properties; Cloud phase function; Satellite observations ID TROPICAL THIN CIRRUS; ATMOSPHERIC INFRARED SOUNDER; LAND-SURFACE TEMPERATURE; RADIATIVE-TRANSFER MODEL; OPTICAL-THICKNESS; MICROPHYSICAL PROPERTIES; LIDAR MEASUREMENTS; WATER-VAPOR; ICE CLOUDS; PART II AB Optical and microphysical properties for optically thin ice clouds are retrieved from one year of collocated Aqua/MODIS and CALIPSO/CALIOP measurements in 2008. The values of optical thickness tau and effective particle size D-eff are inferred from MODIS measurements at three infrared (IR) bands located at 8.5, 11, and 12 mu m in conjunction with collocated CALIOP cloud boundary altitudes and the MERRA atmospheric profile datasets. The values inferred from MODIS IR window measurements are insensitive to the pre-assumed particle and habit distributions. Based on near-IR measurements at 1.38 mu m and the IR-based tau, a new method is developed to infer the scattering phase functions over both ocean and land. A comparison between theoretically calculated phase functions and the retrieved counterparts demonstrates that roughened solid columns provide the best match for cirrus clouds over ocean, whereas droxtals may exist in optically thin cirrus clouds. The best-fitted phase functions are generated using appropriate habit mixtures to match the inferred phase functions. The phase function resulting from a mixture of 55% severely roughened solid columns, 35% severely roughened droxtals, and 10% smooth aggregates almost perfectly matches the mean phase function value retrieved over ocean. The asymmetry factor based on the oceanic best-fitted phase functions is 0.778 at a wavelength of 0.65 mu m. However, it is difficult to find an appropriate habit recipe to fit the inferred phase function over land. This may be caused by the relatively large uncertainties associated with tau retrievals over land. The retrieval of Deff shows that optically thin cirrus clouds consist of smaller ice particles in comparison with optically thicker ice clouds. The mean D-eff values of optically thin ice clouds over land and ocean are 41 mu m and 48 mu m, respectively. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Wang, Chenxi; Yang, Ping; Dessler, Andrew] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Baum, Bryan A.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA. [Hu, Yongxiang] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA USA. RP Yang, P (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM pyang@tamu.edu RI Baum, Bryan/B-7670-2011; Yang, Ping/B-4590-2011; Hu, Yongxiang/K-4426-2012; Dessler, Andrew/G-8852-2012 OI Baum, Bryan/0000-0002-7193-2767; Dessler, Andrew/0000-0003-3939-4820 FU NASA grants [NNX10AM27G, NNX11AK37G, NNX11AF40G]; Texas A&M University through the University of Wisconsin-Madison [301K630] FX This study is supported by NASA grants NNX10AM27G, NNX11AK37G, and NNX11AF40G (the associated subcontract to Texas A&M University through the University of Wisconsin-Madison, 301K630). Bryan Baum and Ping Yang thank Drs. Ramesh Kakar and Hal Maring for their encouragement and support over the years. NR 68 TC 6 Z9 6 U1 1 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD MAY PY 2014 VL 138 BP 36 EP 49 DI 10.1016/j.jqsrt.2014.02.001 PG 14 WC Optics; Spectroscopy SC Optics; Spectroscopy GA AE6DR UT WOS:000334081300003 ER PT J AU Nikitin, AV Thomas, X Regalia, L Daumont, L Rey, M Tashkun, SA Tyuterev, VG Brown, LR AF Nikitin, A. V. Thomas, X. Regalia, L. Daumont, L. Rey, M. Tashkun, S. A. Tyuterev, Vl. G. Brown, L. R. TI Measurements and modeling of long-path (CH4)-C-12 spectra in the 4800-5300 cm(-1) region SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Near infrared methane; Tetradecad; Long path FTIR; Transparency window; Titan; Outer planets ID M TRANSPARENCY WINDOW; HIGH-RESOLUTION SPECTROSCOPY; EMPIRICAL LINE PARAMETERS; MIRS COMPUTER PACKAGE; MU-M; GLOBAL ANALYSIS; ROVIBRATIONAL SPECTRA; INFRARED-SPECTROSCOPY; POLYATOMIC-MOLECULES; METHANE (CH4)-C-12 AB new study of (CH4)-C-12 line positions and intensities was performed for the lower portion of the Tetradecad region between 4800 and 5300 cm(-1) using long path (1603 m) spectra of normal sample CH4 at three pressures recorded with the Fourier transform spectrometer in Reims, France. Line positions and intensities were retrieved by least square curve-fitting procedures and analyzed using the effective Hamiltonian and the effective Dipole moment expressed in terms of irreducible tensor operators adapted to spherical top molecules. An existing spectrum of enriched (CH4)-C-13 was used to discern the isotopic lines. A new measured linelist produced positions and intensities for 5851 features (a factor of two more than prior work). Assignments were made for 46% of these; 2725 experimental line positions and 1764 selected line intensities were fitted with RMS standard deviations of 0.004 cm(-1) and 7.3%, respectively. The RMS of prior intensity fits of the lower Tetradecad was previously a factor of two worse. The sum of observed intensities between 4800 and 5300 cm(-1) fell within 5% of the predicted value from variational calculations. (c) 2014 Elsevier Ltd. All rights reserved. C1 [Nikitin, A. V.; Tashkun, S. A.] SB RAS, VE Zuev Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634021, Russia. [Thomas, X.; Regalia, L.; Daumont, L.; Rey, M.; Tyuterev, Vl. G.] Univ Reims, CNRS, UMR 7331, Grp Spectrometrie Mol & Atmospher, F-51687 Reims 2, France. [Brown, L. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nikitin, A. V.] Tomsk State Univ, Tomsk 634050, Russia. RP Nikitin, AV (reprint author), SB RAS, VE Zuev Inst Atmospher Opt, Lab Theoret Spect, 1 Acad Zuev Sq, Tomsk 634021, Russia. EM avn@lts.iao.ru RI Nikitin, Andrei/K-2624-2013; Tashkun, Sergey/E-8682-2014 OI Nikitin, Andrei/0000-0002-4280-4096; FU Groupement de Recherche International SAMIA; CNRS (France); RFBR (Russia); CAS (China); IDRIS\CINES computer centers of CNRS France; computer center Reims-Champagne-Ardenne; PNP CNRS France FX This work is part of the ANR project "CH4@Titan" (ref.: BLAN08-2_321467). The support of the Groupement de Recherche International SAMIA between CNRS (France), RFBR (Russia) and CAS (China) is acknowledged. We acknowledge the support from IDRIS\CINES computer centers of CNRS France and of the computer center Reims-Champagne-Ardenne. The support of PNP CNRS France in frame of the project "Study of isotopic methane bands in the 2 micron window for the interpretation of space mission data" is acknowledged. A.N. thanks computer centers of ICM@MG SB RAS (Novosibirsk) and SKIF Siberia (Tomsk). Part of the research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contracts with the National Aeronautics and Space Administration. NR 58 TC 8 Z9 8 U1 0 U2 5 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 MAY PY 2014 VL 138 BP 116 EP 123 DI 10.1016/j.jqsrt.2014.02.005 PG 8 WC Optics; Spectroscopy SC Optics; Spectroscopy GA AE6DR UT WOS:000334081300010 ER PT J AU Feldman, PD Glenar, DA Stubbs, TJ Retherford, KD Gladstone, GR Miles, PF Greathouse, TK Kaufmann, DE Parker, JW Stern, SA AF Feldman, Paul D. Glenar, David A. Stubbs, Timothy J. Retherford, Kurt D. Gladstone, G. Randall Miles, Paul F. Greathouse, Thomas K. Kaufmann, David E. Parker, Joel Wm. Stern, S. Alan TI Upper limits for a lunar dust exosphere from far-ultraviolet spectroscopy by LRO/LAMP SO ICARUS LA English DT Article DE Moon; Atmospheres, evolution; Ultraviolet observations ID ZODIACAL LIGHT; SCATTERING; MOON; LAMP AB Since early 2012, the Lyman-Alpha Mapping Project (LAMP) far-ultraviolet spectrograph on the Lunar Reconnaissance Orbiter (LRO) spacecraft has carried out a series of limb observations from within lunar shadow to search for the presence of a high altitude dust exosphere via forward-scattering of sunlight from dust grains. Bright "horizon-glow" was observed from orbit during several Apollo missions and interpreted in terms of dust at altitudes of several km and higher. However, no confirmation of such an exosphere has been made since that time. This raises basic questions about the source(s) of excess brightness in the early measurements and also the conditions for producing observable dust concentrations at km altitudes and higher. Far-ultraviolet measurements between 170 and 190 nm, near the LAMP long wavelength cutoff, are especially sensitive to scattering by small (0.1-0.2 mu m radius) dust grains, since the scattering cross-section is near-maximum, and the solar flux is rising rapidly with wavelength. An additional advantage of ultraviolet measurements is the lack of interference by background zodiacal light which must be taken into account at longer wavelengths. As of July 2013, LAMP has completed several limb-observing sequences dedicated to the search for horizon glow, but no clear evidence of dust scattering has yet been obtained. Upper limits for vertical dust column abundance have been estimated at less than 10 grains cm(-2) (0.1 mu m grain radius), by comparing the measured noise-equivalent brightness with the results of Mie scattering simulations for the same observing geometries. These results indicate that Lunar Atmosphere Dust Environment Explorer (LADEE) UVS lunar dust observations will be considerably more challenging than planned. (C) 2014 Elsevier Inc. All rights reserved. C1 [Feldman, Paul D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Glenar, David A.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Stubbs, Timothy J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Retherford, Kurt D.; Gladstone, G. Randall; Miles, Paul F.; Greathouse, Thomas K.] SW Res Inst, San Antonio, TX 78228 USA. [Kaufmann, David E.; Parker, Joel Wm.; Stern, S. Alan] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Glenar, David A.; Stubbs, Timothy J.] NASA, Ames Res Ctr, Lunar Sci Inst, Moffett Field, CA 94035 USA. RP Feldman, PD (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM pdf@pha.jhu.edu RI Stubbs, Timothy/I-5139-2013; OI Stubbs, Timothy/0000-0002-5524-645X; Greathouse, Thomas/0000-0001-6613-5731 FU NASA [NNG05EC87C]; Southwest Research Institute; NASA LASER Grant [NNX09AO79G]; NASA Lunar Science Institute (NLSI/DREAM) [NNX09AG78A] FX We thank the Lunar Reconnaissance Orbiter project team at NASA's Goddard Space Flight Center for their continuous support. This work was financially supported under contract NNG05EC87C from NASA to the Southwest Research Institute. The work at Johns Hopkins University was supported by a sub-contract from Southwest Research Institute. D. Glenar and T. Stubbs were supported by NASA LASER Grant NNX09AO79G and by the NASA Lunar Science Institute (NLSI/DREAM) under Grant NNX09AG78A. NR 24 TC 13 Z9 13 U1 0 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 MAY 1 PY 2014 VL 233 BP 106 EP 113 DI 10.1016/j.icarus.2014.01.039 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE1KX UT WOS:000333729300010 ER PT J AU Cruikshank, DP Ore, CMD Clark, RN Pendleton, YJ AF Cruikshank, Dale P. Ore, Cristina M. Dalle Clark, Roger N. Pendleton, Yvonne J. TI Aromatic and aliphatic organic materials on Iapetus: Analysis of Cassini VIMS data SO ICARUS LA English DT Article DE Iapetus; Organic chemistry; Satellites, composition; Saturn, satellites ID DIFFUSE INTERSTELLAR-MEDIUM; INFRARED MAPPING SPECTROMETER; SATURNS MOON PHOEBE; 3.4 MU-M; EMISSION FEATURES; IRREGULAR SATELLITES; INTERPLANETARY DUST; SURFACE-COMPOSITION; HYDROCARBONS PAHS; ION IRRADIATION AB We present a quantitative analysis of the hydrocarbon and other organic molecular inventory as a component of the low-albedo material of Saturn's satellite Iapetus, based on a revision of the calibration of the Cassini VIMS instrument. Our study uses hyperspectral data from a mosaic of Iapetus' surface (Pinilla-Alonso, N., Roush, T.L., Marzo, G.A., Cruikshank, D.P., Dalle Ore, C.M. [2011]. Icarus 215, 75-82) constructed from VIMS data on a close fly-by of the satellite. We extracted 2235 individual spectra of the low-albedo regions, and with a clustering analysis tool (Dalle Ore, C.M., Cruikshank, D.P., Clark, R.N. 120121 Icarus 221, 735-743), separated them into two spectrally distinct groups, one concentrated on the leading hemisphere of Iapetus, and the other group on the trailing. This distribution is broadly consistent with that found from Cassini ISS data analyzed by Denk et al. (Denk, T. et al. [2010]. Science 327, 435-439). We modeled the average spectra of the two geographic regions using the materials and techniques described by Clark et al. (Clark, R.N., Cruikshank, D.P., Jaumann, R., Brown, R.H., Stephan, K, Dalle Ore, C.M., Livio, K.E., Pearson, N., Curchin, J.M., Hoefen, T.M., Buratti, B.J., Filacchione, G., Baines, ICH., Nicholson, P.D. [2012]. Icarus 218, 831-860), and after dividing the Iapetus spectrum by the model for each case, we extracted the resulting spectra in the interval 2.7-4.0 mu m for analysis of the organic molecular bands. The spectra reveal the C H stretching modes of aromatic hydrocarbons at similar to 3.28 mu m (similar to 3050 cm(-1)), plus four blended bands of aliphatic -CH2_- and -CH3 in the range similar to 3.36-3.52 mu m (similar to 2980-2840 cm(-1)). In these data, the aromatic band, probably indicating the presence of polycyclic aromatic hydrocarbons (PAR), is unusually strong in comparison to the aliphatic bands, as was found for Hyperion (Dalton, J.B., Cruikshank, D.P., Clark, R.N. [2012]. Icarus 220, 752-776; Dalle Ore, C.M., Cruikshank, D.P., Clark, R.N. [2012], op. cit.) and Phoebe (Dalle Ore, C.M., Cruikshank, D.P., Clark, R.N. [2012], op. cit.). Our Gaussian decomposition of the organic band region suggests the presence of molecular bands in addition to those noted above, specifically bands attributable to cycloalkanes, olefinic compounds, CH3OH, and N-substituted PAHs, as well as possible H-n-PAHs (PAHs with excess peripheral H atoms). In a minimalist interpretation of the Gaussian band fitting, we find the ratio of aromatic CH to aliphatic CH2 + CH3 functional groups for both the leading and trailing hemispheres of Iapetus is 10, with no clear difference between them. In the aliphatic component of the surface material, the ratio CH2/CH3 is 4.0 on the leading hemisphere and 3.0 on the trailing; both values are higher than those found in interstellar dust and other Solar System materials and the difference between the two hemispheres may be statistically significant. The superficial layer of low-albedo material on Iapetus originated in the interior of Phoebe and is being transported to and deposited on Iapetus (and Hyperion) in the current epoch via the Phoebe dust ring (Tosi, F., Turrini, D., Coradini, A., Filacchione, G., and the VIMS Team [2010]. Mon. Not. 1 Astron. Soc. 403, 1113-1130; Tamayo, D., Burns, J.A., Hamilton, D.P., Hedman, M.M. [2011]. Icarus 215, 260-278). The PAHs on Iapetus exist in a H2O-rich environment, and consequently are subject to UV destruction by hydrogenation on short time-scales. The occurrence of this material is therefore consistent with the assertion that the deposition of the PAH-bearing dust is occurring at the present time. If the organic inventory we observe represents the interior composition of Phoebe, we may be sampling the original material from a region of the solar nebula beyond Neptune where Phoebe formed prior to its capture by Saturn (Johnson, T.V., Lunine, J.I. [2005]. Nature 435, 69-71). Published by Elsevier Inc. C1 [Cruikshank, Dale P.; Ore, Cristina M. Dalle; Pendleton, Yvonne J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ore, Cristina M. Dalle] SETI Inst, Mountain View, CA 94043 USA. [Clark, Roger N.] US Geol Survey, Denver, CO 80225 USA. RP Cruikshank, DP (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM dale.p.cruikshank@nasa.gov FU NASA Cassini project; VIMS team; Cassini Data Analysis program FX We thank Drs. Hiroshi Imanaka, U. Allamandola, M.P. Bernstein, A.G.G.M. Tielens, Diane H. Wooden, and especially S.A. Sandford for helpful conversations as this work progressed. This work is supported in part by the NASA Cassini project, the VIMS team, and Cassini Data Analysis program (R. Clark and C.M. Dalle Ore, Principal Investigators). NR 65 TC 6 Z9 7 U1 0 U2 15 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAY 1 PY 2014 VL 233 BP 306 EP 315 DI 10.1016/j.icarus.2014.02.011 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE1KX UT WOS:000333729300026 ER PT J AU Reichle, RH De Lannoy, GJM Forman, BA Draper, CS Liu, Q AF Reichle, Rolf H. De Lannoy, Gabrielle J. M. Forman, Barton A. Draper, Clara S. Liu, Qing TI Connecting Satellite Observations with Water Cycle Variables Through Land Data Assimilation: Examples Using the NASA GEOS-5 LDAS SO SURVEYS IN GEOPHYSICS LA English DT Review DE Land data assimilation; Land surface modeling; Satellite remote sensing; Soil moisture; Snow; Terrestrial water storage; Ensemble Kalman filter ID ENSEMBLE KALMAN FILTER; SURFACE DATA ASSIMILATION; CATCHMENT-BASED APPROACH; 1997 FIELD EXPERIMENT; SOIL-MOISTURE; PASSIVE MICROWAVE; SNOW DEPTH; MODEL; SYSTEM; EQUIVALENT AB A land data assimilation system (LDAS) can merge satellite observations (or retrievals) of land surface hydrological conditions, including soil moisture, snow, and terrestrial water storage (TWS), into a numerical model of land surface processes. In theory, the output from such a system is superior to estimates based on the observations or the model alone, thereby enhancing our ability to understand, monitor, and predict key elements of the terrestrial water cycle. In practice, however, satellite observations do not correspond directly to the water cycle variables of interest. The present paper addresses various aspects of this seeming mismatch using examples drawn from recent research with the ensemble-based NASA GEOS-5 LDAS. These aspects include (1) the assimilation of coarse-scale observations into higher-resolution land surface models, (2) the partitioning of satellite observations (such as TWS retrievals) into their constituent water cycle components, (3) the forward modeling of microwave brightness temperatures over land for radiance-based soil moisture and snow assimilation, and (4) the selection of the most relevant types of observations for the analysis of a specific water cycle variable that is not observed (such as root zone soil moisture). The solution to these challenges involves the careful construction of an observation operator that maps from the land surface model variables of interest to the space of the assimilated observations. C1 [Reichle, Rolf H.; De Lannoy, Gabrielle J. M.; Draper, Clara S.; Liu, Qing] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [De Lannoy, Gabrielle J. M.; Draper, Clara S.] Univ Space Res Assoc, Columbia, MD USA. [Forman, Barton A.] Univ Maryland, Dept Civil & Environm Engn, College Pk, MD 20742 USA. [Liu, Qing] Sci Syst & Applicat Inc, Lanham, MD USA. RP Reichle, RH (reprint author), NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Code 610-1,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM rolf.reichle@nasa.gov RI Reichle, Rolf/E-1419-2012; Draper, Clara/P-6097-2016 OI Draper, Clara/0000-0002-8299-4939 FU NASA program on The Science of Terra and Aqua; NASA Soil Moisture Active Passive mission; NASA Postdoctoral Program; NASA High-End Computing program FX The authors thank the organizers of the ISSI Workshop on "The Earth's Hydrological Cycle" held February 6-10, 2012 and two anonymous reviewers for their efforts. The research was supported by the NASA program on The Science of Terra and Aqua, the NASA Soil Moisture Active Passive mission, the NASA Postdoctoral Program, and the NASA High-End Computing program. NR 104 TC 19 Z9 19 U1 3 U2 42 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-3298 EI 1573-0956 J9 SURV GEOPHYS JI Surv. Geophys. PD MAY PY 2014 VL 35 IS 3 BP 577 EP 606 DI 10.1007/s10712-013-9220-8 PG 30 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AE1BN UT WOS:000333700700006 ER PT J AU Lahoz, WA De Lannoy, GJM AF Lahoz, William A. De Lannoy, Gabrielle J. M. TI Closing the Gaps in Our Knowledge of the Hydrological Cycle over Land: Conceptual Problems SO SURVEYS IN GEOPHYSICS LA English DT Review DE Hydrological cycle; Earth observation; Land surface models; Data assimilation ID SURFACE SOIL-MOISTURE; DATA ASSIMILATION SYSTEM; ENSEMBLE KALMAN FILTER; VARIATIONAL DATA ASSIMILATION; NUMERICAL WEATHER-PREDICTION; SNOW-COVERED AREA; MICROWAVE BRIGHTNESS TEMPERATURE; ERROR COVARIANCE STATISTICS; ENVIRONMENT SIMULATOR JULES; INTEGRATED FORECAST SYSTEM AB This paper reviews the conceptual problems limiting our current knowledge of the hydrological cycle over land. We start from the premise that to understand the hydrological cycle we need to make observations and develop dynamic models that encapsulate our understanding. Yet, neither the observations nor the models could give a complete picture of the hydrological cycle. Data assimilation combines observational and model information and adds value to both the model and the observations, yielding increasingly consistent and complete estimates of hydrological components. In this review paper we provide a historical perspective of conceptual problems and discuss state-of-the-art hydrological observing, modelling and data assimilation systems. C1 [Lahoz, William A.] NILU, N-2027 Kjeller, Norway. [Lahoz, William A.] Meteo France, CNRM GMGEC CARMA, F-31100 Toulouse, France. [De Lannoy, Gabrielle J. M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Lahoz, WA (reprint author), NILU, Inst Veien 18,POB 100, N-2027 Kjeller, Norway. EM wal@nilu.no; Gabrielle.Delannoy@nasa.gov FU NILU internal project FX This paper arose from the International Space Science Institute (ISSI) workshop "The Earth's Hydrological Cycle", held at ISSI, Bern, Switzerland, on 6-10 February 2012. A NILU internal project supported WAL. Thanks to Alexandra Griesfeller for providing Fig. 2. NR 292 TC 14 Z9 14 U1 4 U2 43 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-3298 EI 1573-0956 J9 SURV GEOPHYS JI Surv. Geophys. PD MAY PY 2014 VL 35 IS 3 BP 623 EP 660 DI 10.1007/s10712-013-9221-7 PG 38 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AE1BN UT WOS:000333700700008 ER PT J AU Foufoula-Georgiou, E Ebtehaj, AM Zhang, SQ Hou, AY AF Foufoula-Georgiou, E. Ebtehaj, A. M. Zhang, S. Q. Hou, A. Y. TI Downscaling Satellite Precipitation with Emphasis on Extremes: A Variational l(1)-Norm Regularization in the Derivative Domain SO SURVEYS IN GEOPHYSICS LA English DT Review DE Sparsity; Inverse problems; l(1)-norm regularization; Non-smooth convex optimization; Generalized Gaussian density; Extremes; Hurricanes ID RESOLUTION TEMPORAL RAINFALL; MULTICOMPONENT DECOMPOSITION; ATOMIC DECOMPOSITION; INVERSE PROBLEMS; BASIS PURSUIT; LARGE-SCALE; WAVELET; SHRINKAGE; FIELDS; MODEL AB The increasing availability of precipitation observations from space, e.g., from the Tropical Rainfall Measuring Mission (TRMM) and the forthcoming Global Precipitation Measuring (GPM) Mission, has fueled renewed interest in developing frameworks for downscaling and multi-sensor data fusion that can handle large data sets in computationally efficient ways while optimally reproducing desired properties of the underlying rainfall fields. Of special interest is the reproduction of extreme precipitation intensities and gradients, as these are directly relevant to hazard prediction. In this paper, we present a new formalism for downscaling satellite precipitation observations, which explicitly allows for the preservation of some key geometrical and statistical properties of spatial precipitation. These include sharp intensity gradients (due to high-intensity regions embedded within lower-intensity areas), coherent spatial structures (due to regions of slowly varying rainfall), and thicker-than-Gaussian tails of precipitation gradients and intensities. Specifically, we pose the downscaling problem as a discrete inverse problem and solve it via a regularized variational approach (variational downscaling) where the regularization term is selected to impose the desired smoothness in the solution while allowing for some steep gradients (called a""(1)-norm or total variation regularization). We demonstrate the duality between this geometrically inspired solution and its Bayesian statistical interpretation, which is equivalent to assuming a Laplace prior distribution for the precipitation intensities in the derivative (wavelet) space. When the observation operator is not known, we discuss the effect of its misspecification and explore a previously proposed dictionary-based sparse inverse downscaling methodology to indirectly learn the observation operator from a data base of coincidental high- and low-resolution observations. The proposed method and ideas are illustrated in case studies featuring the downscaling of a hurricane precipitation field. C1 [Foufoula-Georgiou, E.] Univ Minnesota, Dept Civil Engn, St Anthony Falls Lab, Minneapolis, MN 55455 USA. [Ebtehaj, A. M.] Univ Minnesota, Sch Math, Dept Civil Engn, St Anthony Falls Lab, Minneapolis, MN 55455 USA. [Zhang, S. Q.; Hou, A. Y.] NASA, Goddard Space Flight Ctr, Greenbelt, MA USA. RP Foufoula-Georgiou, E (reprint author), Univ Minnesota, Dept Civil Engn, St Anthony Falls Lab, Minneapolis, MN 55455 USA. EM efi@umn.edu; ebteh001@umn.edu; sara.q.zhang@nasa.gov; arthur.y.hou@nasa.gov RI Measurement, Global/C-4698-2015 FU NASA-GPM award [NNX10AO12G]; NASA Earth and Space Science Fellowship [NNX12AN45H]; Doctoral Dissertation Fellowship of the University of Minnesota FX This work has been mainly supported by a NASA-GPM award (NNX10AO12G), a NASA Earth and Space Science Fellowship (NNX12AN45H), and a Doctoral Dissertation Fellowship of the University of Minnesota to the second author. The insightful comments of one anonymous referee are also gratefully acknowledged. NR 31 TC 5 Z9 5 U1 5 U2 22 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-3298 EI 1573-0956 J9 SURV GEOPHYS JI Surv. Geophys. PD MAY PY 2014 VL 35 IS 3 BP 765 EP 783 DI 10.1007/s10712-013-9264-9 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AE1BN UT WOS:000333700700013 ER PT J AU Bates, PD Neal, JC Alsdorf, D Schumann, GJP AF Bates, Paul D. Neal, Jefferey C. Alsdorf, Douglas Schumann, Guy J-P TI Observing Global Surface Water Flood Dynamics SO SURVEYS IN GEOPHYSICS LA English DT Review DE Floods; Surface water; Floodplains; Rivers; Wetlands; Remote sensing; Surface water ocean topography (SWOT) mission ID RADAR INTERFEROMETRY; SATELLITE RADAR; LEVEL CHANGES; DIGITAL PHOTOGRAMMETRY; RIVER DISCHARGE; AMAZON RIVER; INUNDATION; ASSIMILATION; ALTIMETRY; HYDROLOGY AB Flood waves moving along river systems are both a key determinant of globally important biogeochemical and ecological processes and, at particular times and particular places, a major environmental hazard. In developed countries, sophisticated observing networks and ancillary data, such as channel bathymetry and floodplain terrain, exist with which to understand and model floods. However, at global scales, satellite data currently provide the only means of undertaking such studies. At present, there is no satellite mission dedicated to observing surface water dynamics and, therefore, surface water scientists make use of a range of sensors developed for other purposes that are distinctly sub-optimal for the task in hand. Nevertheless, by careful combination of the data available from topographic mapping, oceanographic, cryospheric and geodetic satellites, progress in understanding some of the world's major river, floodplain and wetland systems can be made. This paper reviews the surface water data sets available to hydrologists on a global scale and the recent progress made in the field. Further, the paper looks forward to the proposed NASA/CNES Surface Water Ocean Topography satellite mission that may for the first time provide an instrument that meets the needs of the hydrology community. C1 [Bates, Paul D.; Neal, Jefferey C.] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England. [Alsdorf, Douglas] Ohio State Univ, Sch Earth Sci, Byrd Polar Res Ctr, Columbus, OH 43210 USA. [Schumann, Guy J-P] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bates, PD (reprint author), Univ Bristol, Sch Geog Sci, Univ Rd, Bristol BS8 1SS, Avon, England. EM paul.bates@bristol.ac.uk RI Bates, Paul/C-8026-2012; Neal, Jeffrey/C-8723-2009; Schumann, Guy/F-9760-2011 OI Bates, Paul/0000-0001-9192-9963; Neal, Jeffrey/0000-0001-5793-9594; FU National Aeronautics and Space Administration FX Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 82 TC 15 Z9 15 U1 10 U2 55 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-3298 EI 1573-0956 J9 SURV GEOPHYS JI Surv. Geophys. PD MAY PY 2014 VL 35 IS 3 BP 839 EP 852 DI 10.1007/s10712-013-9269-4 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AE1BN UT WOS:000333700700016 ER PT J AU McGillivray, DA Cravey, RL Dudley, KL Vedeler, E Gupta, MC AF McGillivray, Duncan A. Cravey, Robin L. Dudley, Kenneth L. Vedeler, Erik Gupta, Mool C. TI POLARIZATION PROPERTIES OF A ONE DIMENSIONAL METAMATERIAL LENS SO MICROWAVE AND OPTICAL TECHNOLOGY LETTERS LA English DT Article DE metamaterials; split ring resonators; polarization; transmission; sensors ID NEGATIVE REFRACTION AB The control of microwave (MW) radiation transmission through the polarization state of the incident beam is the basis for many applications in sensors and optics. Altering the polarization state of electromagnetic radiation by transmission through a metamaterial (MTM) lens could lead to novel devices and sensors. The polarization properties of 1D split ring resonator and rod type MTM structures were investigated and compared to a previously reported corresponding 2D MTM lens. Unlike the 2D lens, the 1D MTM did not contribute to a change in polarization state of transmitted MWs. The transmission response, however, was found to be determined by the coupling mechanisms between the MTMs constituent elements and orientation of the incident MW polarization. For the 1D lens, changing incident polarization from alignment parallel to the MTMs rod elements to alignment perpendicular to the rods, at resonance frequency, changes the effective index of refraction from net negative to positive. For a MTM structure, facing perpendicular to the incident radiation, the effective electromagnetic properties change from negative permittivity and positive permeability (for polarization parallel to the rod elements) to positive permittivity and negative permeability (for polarization perpendicular to the rod elements). (c) 2014 Wiley Periodicals, Inc. Microwave Opt Technol Lett 56:1218-1222, 2014 C1 [McGillivray, Duncan A.; Gupta, Mool C.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. [Cravey, Robin L.; Dudley, Kenneth L.; Vedeler, Erik] NASA, Langley Res Ctr, Electromagnet & Sensors Branch, Hampton, VA 23681 USA. RP Gupta, MC (reprint author), Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. EM mgupta@virginia.edu NR 16 TC 0 Z9 0 U1 2 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0895-2477 EI 1098-2760 J9 MICROW OPT TECHN LET JI Microw. Opt. Technol. Lett. PD MAY PY 2014 VL 56 IS 5 BP 1218 EP 1222 DI 10.1002/mop.28309 PG 5 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA AC4VP UT WOS:000332519500049 ER PT J AU Ghisellini, G Sbarrato, T Tagliaferri, G Foschini, L Tavecchio, F Ghirlanda, G Braito, V Gehrels, N AF Ghisellini, G. Sbarrato, T. Tagliaferri, G. Foschini, L. Tavecchio, F. Ghirlanda, G. Braito, V. Gehrels, N. TI SDSS J114657.79+403708.6: the third most distant blazar at z=5.0 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; quasars: general; X-rays: general ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; DATA RELEASE; BLACK-HOLES; X-RAY; FERMI BLAZARS; LINE REGION; SWIFT; TELESCOPE; MISSION AB The radio-loud quasar SDSS J114657.79+403708.6 at a redshift z = 5.0 is one of the most distant radio-loud objects. The IR-optical luminosity and spectrum suggest that its black hole has a very large mass: M = (5 +/- 1) x 10(9) M-circle dot. The radio-loudness (ratio of the radio to optical flux) of the source is large (around 100), suggesting that the source is viewed at small angles from the jet axis, and could be a blazar. The X-ray observations fully confirm this hypothesis, due to the high level and hardness of the flux. This makes SDSS J114657.79+403708.6 the third most distant blazar known, after Q0906+693 (z = 5.47) and B2 1023+25 (z = 5.3). Among those, SDSS J114657.79+403708.6 has the largest black holemass, setting interesting constraints on the mass function of heavy (>10(9)M(circle dot)) black holes at high redshifts. C1 [Ghisellini, G.; Sbarrato, T.; Tagliaferri, G.; Foschini, L.; Tavecchio, F.; Ghirlanda, G.; Braito, V.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Sbarrato, T.] Univ Insubria, Dipartimento Fis & Matemat, I-22100 Como, Italy. [Sbarrato, T.] ESO European Southern Observ, D-8578 Garching, Germany. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ghisellini, G (reprint author), INAF Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy. EM gabriele.ghisellini@brera.inaf.it OI Braito, Valentina/0000-0002-2629-4989; Ghirlanda, Giancarlo/0000-0001-5876-9259; Ghisellini, Gabriele/0000-0002-0037-1974; Sbarrato, Tullia/0000-0002-3069-9399; Foschini, Luigi/0000-0001-8678-0324; Tagliaferri, Gianpiero/0000-0003-0121-0723; Tavecchio, Fabrizio/0000-0003-0256-0995 FU NASA FX We thank the anonymous referee for useful comments. 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 NASA. Part of this work is based on archival data and online service provided by the ASI Science Data Center (ASDC). NR 38 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 MAY 1 PY 2014 VL 440 IS 1 BP L111 EP L115 DI 10.1093/mnrasl/slu032 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM8DM UT WOS:000357927000023 ER PT J AU Ringerud, S Kummerow, C Peters-Lidard, C Tian, YD Harrison, K AF Ringerud, Sarah Kummerow, Christian Peters-Lidard, Christa Tian, Yudong Harrison, Kenneth TI A Comparison of Microwave Window Channel Retrieved and Forward-Modeled Emissivities Over the US Southern Great Plains SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Emissivity; land surface; passive microwave remote sensing; precipitation ID LAND-SURFACE EMISSIVITIES; SOIL-MOISTURE; SATELLITE-OBSERVATIONS; DATA ASSIMILATION; CLOUD DETECTION; UNITED-STATES; WATER-CONTENT; MODIS; TEMPERATURE; RAINFALL AB An accurate understanding of land surface emissivity in terms of associated surface properties is necessary for improved passive microwave remote sensing of the atmosphere, including water vapor, clouds, and precipitation, over land. In an effort to advance this understanding, emissivities are calculated for a 5 degrees latitude by 5 degrees longitude region in the U. S. Southern Great Plains using a combination of land surface model and physical emissivity model. Results are compared to retrieved values from the Advanced Microwave Scanning Radiometer-Earth Observing System passive microwave observations for cloud-free scenes over a six-year period. The resulting emissivities are compared in the context of surface properties including surface temperature, leaf area index (LAI), soil moisture, and precipitation. The comparison confirms that lower frequency channels respond most directly to the surface soil and its dielectric properties. Differences between retrieved and modeled emissivities are generally lower than 2%-3% and appear to be a function of soil moisture and LAI at frequencies less than 37 GHz. Agreement is better for the vertical polarization channels. At 89 GHz, a large difference is present between retrieved and modeled emissivities in both mean and magnitude of variability, particularly in the summer months. Problems are likely present at higher microwave frequencies in both the retrieved and modeled products, including the inability of the emissivity model to represent liquid water in the form of dew or precipitation interception on the vegetation canopy. C1 [Ringerud, Sarah; Kummerow, Christian] Colorado State Univ, Ft Collins, CO 80523 USA. [Peters-Lidard, Christa; Tian, Yudong; Harrison, Kenneth] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ringerud, S (reprint author), Colorado State Univ, Ft Collins, CO 80523 USA. EM sarah@atmos.colostate.edu; kummerow@atmos.colostate.edu; christa.d.peters-lidard@nasa.gov; yudong.tian-1@nasa.gov; Kenneth.Harrison@nasa.gov RI Peters-Lidard, Christa/E-1429-2012; Measurement, Global/C-4698-2015 OI Peters-Lidard, Christa/0000-0003-1255-2876; FU Office of Science, Office of Biological and Environmental Research, Climate and Environmental Sciences Division, U.S. Department of Energy FX Data were obtained from the ARS Micronet program, operated and maintained by the USDA Agricultural Research Service's Grazinglands Research Laboratory, and from the Atmospheric Radiation Measurement Program sponsored by the Office of Science, Office of Biological and Environmental Research, Climate and Environmental Sciences Division, U.S. Department of Energy. NR 42 TC 10 Z9 10 U1 0 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 MAY PY 2014 VL 52 IS 5 BP 2395 EP 2412 DI 10.1109/TGRS.2013.2260759 PG 18 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AC4IN UT WOS:000332484700010 ER PT J AU Fore, AG Yueh, SH Tang, WQ Hayashi, AK Lagerloef, GSE AF Fore, Alexander G. Yueh, Simon H. Tang, Wenqing Hayashi, Akiko K. Lagerloef, Gary S. E. TI Aquarius Wind Speed Products: Algorithms and Validation SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Aquarius; ocean winds; radar; remote sensing; scatterometery ID BAND MICROWAVE OBSERVATIONS; SEA-SURFACE SALINITY; DIELECTRIC-CONSTANT; TRIPLE COLLOCATION; SCATTEROMETER; SATELLITE; OCEAN; RETRIEVAL; INSTRUMENT; STABILITY AB This paper introduces and validates the Aquarius scatterometer-only wind speed algorithm and the combined active passive (CAP) wind speed products. The scatterometer-only algorithm uses the co-polarized radar cross-section to determine the ocean surface wind speed with a maximum-likelihood estimator approach while the CAP algorithm uses both the scatterometer and radiometer channels to achieve a simultaneous ocean vector wind and sea surface salinity retrieval. We discuss complications in the speed retrieval due to the shape of the scatterometer model function at L-band and develop mitigation strategies. We find the performance of the Aquarius scatterometer-only wind speed is better than 1.00 ms(-1), with best performance for low wind speeds and increasing noise levels as the wind speed increases. The CAP wind speed product is significantly better than the scatterometer-only due to the inclusion of passive measurements and achieves 0.70 ms(-1) root-mean-square error. C1 [Fore, Alexander G.; Yueh, Simon H.; Tang, Wenqing; Hayashi, Akiko K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lagerloef, Gary S. E.] Earth & Space Res, Seattle, WA 98121 USA. RP Fore, AG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Alexander.Fore@jpl.nasa.gov FU National Aeronautics and Space Administration FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 26 TC 8 Z9 8 U1 0 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAY PY 2014 VL 52 IS 5 BP 2920 EP 2927 DI 10.1109/TGRS.2013.2267616 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 AC4IN UT WOS:000332484700052 ER PT J AU Wei, J Savtchenko, A Vollmer, B Hearty, T Albayrak, A Crisp, D Eldering, A AF Wei, J. Savtchenko, A. Vollmer, B. Hearty, T. Albayrak, A. Crisp, D. Eldering, A. TI Advances in CO2 Observations From AIRS and ACOS SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Carbon dioxide; infrared measurements; orbiting carbon observatory-2 (OCO-2); satellite application ID ATMOSPHERIC CO2; RETRIEVAL ALGORITHM; SURFACE AB NASA Goddard Earth Sciences Data and Information Services Center (GES DISC) archives and distributes pioneering collections of data on atmospheric greenhouse gases. In September of 2012, the Atmospheric Infrared Sounder (AIRS) marked a decade of tropospheric observations of carbon dioxide (CO2). Most recently, the Atmospheric CO2 Observations from Space (ACOS) project and GES DISC released CO2 retrievals derived from radiances observed by the Japanese Greenhouse gases Observing SATellite (GOSAT) satellite, launched in 2009. In this letter, we present the most recent estimates of decadal mid-tropospheric trends of CO2 from AIRS, as well as the most recent status of the total column-average distribution of CO2 from ACOS. We also demonstrate that significant discrepancies still exist in the global distribution of observed and modeled column amounts of CO2 using the CO2 retrievals from the ACOS project. C1 [Wei, J.; Savtchenko, A.; Albayrak, A.] ADNET Syst Inc, Greenbelt, MD 20771 USA. [Vollmer, B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hearty, T.] Wyle Informat Syst, Greenbelt, MD 20771 USA. [Crisp, D.; Eldering, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA. RP Wei, J (reprint author), ADNET Syst Inc, Greenbelt, MD 20771 USA. EM jennifer.c.wei@nasa.gov FU NASA Earth Science Data and Information System (ESDIS) Project; National Aeronautics and Space Administration FX This work was supported by the NASA Earth Science Data and Information System (ESDIS) Project. Part of the work described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 21 TC 3 Z9 3 U1 2 U2 42 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 MAY PY 2014 VL 11 IS 5 BP 891 EP 895 DI 10.1109/LGRS.2013.2281147 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 275WC UT WOS:000328708000001 ER PT J AU Brunt, KM Neumann, TA Walsh, KM Markus, T AF Brunt, Kelly M. Neumann, Thomas A. Walsh, Kaitlin M. Markus, Thorsten TI Determination of Local Slope on the Greenland Ice Sheet Using a Multibeam Photon-Counting Lidar in Preparation for the ICESat-2 Mission SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Airborne lidar; laser altimetry; photon counting ID ELEVATION; ACCURACY AB The greatest changes in elevation in Greenland and Antarctica are happening along the margins of the ice sheets where the surface frequently has significant slopes. For this reason, the upcoming Ice, Cloud, and land Elevation Satellite-2 (ICESat-2) mission utilizes pairs of laser altimeter beams that are perpendicular to the flight direction in order to extract slope information in addition to elevation. The Multiple Altimeter Beam Experimental Lidar (MABEL) is a high-altitude airborne laser altimeter designed as a simulator for ICESat-2. The MABEL design uses multiple beams at fixed angles and allows for local slope determination. Here, we present local slopes as determined by MABEL and compare them to those determined by the Airborne Topographic Mapper (ATM) over the same flight lines in Greenland. We make these comparisons with consideration for the planned ICESat-2 beam geometry. Results indicate that the mean slope residuals between MABEL and ATM remain small (< 0.05 degrees) through a wide range of localized slopes using ICESat-2 beam geometry. Furthermore, when MABEL data are subsampled by a factor of 4 to mimic the planned ICESat-2 transmit-energy configuration, the results are indistinguishable from the full-data-rate analysis. Results from MABEL suggest that ICESat-2 beam geometry and transmit-energy configuration are appropriate for the determination of slope on similar to 90-m spatial scales, a measurement that will be fundamental to deconvolving the effects of surface slope from the ice-sheet surface change derived from ICESat-2. C1 [Brunt, Kelly M.] NASA, Goddard Space Flight Ctr, GESTAR, Greenbelt, MD 20771 USA. [Neumann, Thomas A.; Markus, Thorsten] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Walsh, Kaitlin M.] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA. RP Brunt, KM (reprint author), NASA, Goddard Space Flight Ctr, GESTAR, Greenbelt, MD 20771 USA. EM kelly.m.brunt@nasa.gov RI Neumann, Thomas/D-5264-2012 NR 18 TC 9 Z9 10 U1 4 U2 34 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 MAY PY 2014 VL 11 IS 5 BP 935 EP 939 DI 10.1109/LGRS.2013.2282217 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 275WC UT WOS:000328708000010 ER PT J AU Makishima, K Enoto, T Hiraga, JS Nakano, T Nakazawa, K Sakurai, S Sasano, M Murakami, H AF Makishima, K. Enoto, T. Hiraga, J. S. Nakano, T. Nakazawa, K. Sakurai, S. Sasano, M. Murakami, H. TI Possible Evidence for Free Precession of a Strongly Magnetized Neutron Star in the Magnetar 4U 0142+61 SO PHYSICAL REVIEW LETTERS LA English DT Article ID X-RAY PULSARS; BOARD SUZAKU; FIELDS; SOFT; 4U-0142+61; EVOLUTION; REPEATERS; RXTE AB Magnetars are a special type of neutron stars, considered to have extreme dipole magnetic fields reaching similar to 10(11) T. The magnetar 4U 0142 + 61, one of the prototypes of this class, was studied in broadband x rays (0.5-70 keV) with the Suzaku observatory. In hard x rays (15-40 keV), its 8.69 sec pulsations suffered slow phase modulations by +/- 0.7 sec, with a period of similar to 15 h. When this effect is interpreted as free precession of the neutron star, the object is inferred to deviate from spherical symmetry by similar to 1.6 x 10(-4) in its moments of inertia. This deformation, when ascribed to magnetic pressure, suggests a strong toroidal magnetic field, similar to 10(12) T, residing inside the object. This provides one of the first observational approaches towards toroidal magnetic fields of magnetars. C1 [Makishima, K.; Nakano, T.; Nakazawa, K.; Sakurai, S.; Sasano, M.; Murakami, H.] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Makishima, K.; Hiraga, J. S.] Univ Tokyo, Grad Sch Sci, Res Ctr Early Univ, Bunkyo Ku, Tokyo 1130033, Japan. [Makishima, K.] RIKEN, MAXI Team, Wako, Saitama 3510198, Japan. [Enoto, T.] RIKEN, Nishina Ctr, High Energy Astrophys Lab, Wako, Saitama 3510198, Japan. [Enoto, T.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Makishima, K (reprint author), Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. RI XRAY, SUZAKU/A-1808-2009 FU MEXT [25105507] FX This work was supported partially by the MEXT Grant-in-Aid for Scientific Research on Innovative Areas, Area No. 2404, Grant No. 25105507. NR 38 TC 22 Z9 22 U1 0 U2 0 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 APR 30 PY 2014 VL 112 IS 17 AR 171102 DI 10.1103/PhysRevLett.112.171102 PG 5 WC Physics, Multidisciplinary SC Physics GA AH0NM UT WOS:000335816700002 PM 24836230 ER PT J AU Brando, PM Balch, JK Nepstad, DC Morton, DC Putz, FE Coe, MT Silverio, D Macedo, MN Davidson, EA Nobrega, CC Alencar, A Soares, BS AF Brando, Paulo Monteiro Balch, Jennifer K. Nepstad, Daniel C. Morton, Douglas C. Putz, Francis E. Coe, Michael T. Silverio, Divino Macedo, Marcia N. Davidson, Eric A. Nobrega, Caroline C. Alencar, Ane Soares-Filho, Britaldo S. TI Abrupt increases in Amazonian tree mortality due to drought-fire interactions SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE forest dieback; fireline intensity; stable states; MODIS; fire mapping ID CLIMATE-CHANGE; RAIN-FORESTS; SAVANNA; SUSCEPTIBILITY; DEFORESTATION; RESILIENCE; FEEDBACKS; BEHAVIOR; DIEBACK; TRAITS AB Interactions between climate and land-use change may drive widespread degradation of Amazonian forests. High-intensity fires associated with extreme weather events could accelerate this degradation by abruptly increasing tree mortality, but this process remains poorly understood. Here we present, to our knowledge, the first field-based evidence of a tipping point in Amazon forests due to altered fire regimes. Based on results of a large-scale, longterm experiment with annual and triennial burn regimes (B1yr and B3yr, respectively) in the Amazon, we found abrupt increases in fire-induced tree mortality (226 and 462%) during a severe drought event, when fuel loads and air temperatures were substantially higher and relative humidity was lower than long-term averages. This threshold mortality response had a cascading effect, causing sharp declines in canopy cover (23 and 31%) and aboveground live biomass (12 and 30%) and favoring widespread invasion by flammable grasses across the forest edge area (80 and 63%), where fires were most intense (e. g., 220 and 820 kW.m(-1)). During the droughts of 2007 and 2010, regional forest fires burned 12 and 5% of southeastern Amazon forests, respectively, compared with < 1% in nondrought years. These results show that a few extreme drought events, coupled with forest fragmentation and anthropogenic ignition sources, are already causing widespread fire-induced tree mortality and forest degradation across southeastern Amazon forests. Future projections of vegetation responses to climate change across drier portions of the Amazon require more than simulation of global climate forcing alone and must also include interactions of extreme weather events, fire, and land-use change. C1 [Brando, Paulo Monteiro; Silverio, Divino; Nobrega, Caroline C.; Alencar, Ane] Inst Pesquisa Ambiental Amazonia, BR-66035170 Belem, Para, Brazil. [Brando, Paulo Monteiro; Coe, Michael T.; Macedo, Marcia N.; Davidson, Eric A.] Woods Hole Res Ctr, Falmouth, MA 02450 USA. [Brando, Paulo Monteiro] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Balch, Jennifer K.] Penn State Univ, Dept Geog, University Pk, PA 16802 USA. [Nepstad, Daniel C.] Earth Innovat Inst, San Francisco, CA 94110 USA. [Morton, Douglas C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Putz, Francis E.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Silverio, Divino] Univ Brasilia, Dept Ecol, BR-70910900 Brasilia, DF, Brazil. [Nobrega, Caroline C.] Univ Fed Goias, Inst Ciencias Biol, BR-74001970 Goiania, Go, Brazil. [Soares-Filho, Britaldo S.] Univ Fed Minas Gerais, Inst Geociencias, BR-6627 Belo Horizonte, MG, Brazil. RP Brando, PM (reprint author), Inst Pesquisa Ambiental Amazonia, BR-66035170 Belem, Para, Brazil. EM pmbrando@ipam.org.br RI Morton, Douglas/D-5044-2012; Silverio, Divino Vicente/G-1154-2012; Davidson, Eric/K-4984-2013; Brando, Paulo/C-4302-2012 OI Silverio, Divino Vicente/0000-0003-1642-9496; Davidson, Eric/0000-0002-8525-8697; Brando, Paulo/0000-0001-8952-7025 FU Gordon and Betty Moore Foundation; National Science Foundation (Division of Environmental Biology) [0410315, 0743703]; Packard Foundation; National Aeronautics and Space Administration; Max Planck Institute for Biogeochemistry FX We thank S. Trumbore, Y. Malhi, C. A. Baldeck, and P. Cox for comments; L. Curran and O. Carvalho for help with the experimental design; and Instituto de Pesquisa Ambiental da Amazonia's field crew for taking measurements. Grupo A. Maggi provided access to the field site and logistical support. This study was supported by the Gordon and Betty Moore Foundation, the National Science Foundation (Division of Environmental Biology Grants 0410315 and 0743703), the Packard Foundation, the National Aeronautics and Space Administration, and the Max Planck Institute for Biogeochemistry. NR 43 TC 98 Z9 99 U1 21 U2 137 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 APR 29 PY 2014 VL 111 IS 17 BP 6347 EP 6352 DI 10.1073/pnas.1305499111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AG1TL UT WOS:000335199000061 PM 24733937 ER PT J AU Gopalswamy, N Akiyama, S Yashiro, S Xie, H Makela, P Michalek, G AF Gopalswamy, Nat Akiyama, Sachiko Yashiro, Seiji Xie, Hong Maekelae, Pertti Michalek, Grzegorz TI Anomalous expansion of coronal mass ejections during solar cycle 24 and its space weather implications SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE coronal mass ejections; anomalous expansion; geomagentic storms; solar energetic particle events; space weather; solar cycle 24 ID ENERGETIC PARTICLE; INTENSITY; EVENTS AB The familiar correlation between the speed and angular width of coronal mass ejections (CMEs) is also found in solar cycle 24, but the regression line has a larger slope: for a given CME speed, cycle 24 CMEs are significantly wider than those in cycle 23. The slope change indicates a significant change in the physical state of the heliosphere, due to the weak solar activity. The total pressure in the heliosphere (magnetic+plasma) is reduced by similar to 40%, which leads to the anomalous expansion of CMEs explaining the increased slope. The excess CME expansion contributes to the diminished effectiveness of CMEs in producing magnetic storms during cycle 24, both because the magnetic content of the CMEs is diluted and also because of the weaker ambient fields. The reduced magnetic field in the heliosphere may contribute to the lack of solar energetic particles accelerated to very high energies during this cycle. C1 [Gopalswamy, Nat] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Akiyama, Sachiko; Yashiro, Seiji; Xie, Hong; Maekelae, Pertti] Catholic Univ Amer, Dept Phys, Washington, DE USA. [Michalek, Grzegorz] Jagiellonian Univ, Astron Observ, Krakow, Poland. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM nat.gopalswamy@nasa.gov OI Gopalswamy, Nat/0000-0001-5894-9954 FU NASA LWS TRT program FX SOHO is a project of international cooperation between ESA and NASA. This research was supported by NASA LWS TR&T program. We thank E.W. Cliver and an anonymous referee for their constructive criticism, which improved the presentation of the paper. NR 24 TC 23 Z9 23 U1 0 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 APR 28 PY 2014 VL 41 IS 8 BP 2673 EP 2680 DI 10.1002/2014GL059858 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AH0KW UT WOS:000335809800002 ER PT J AU Guan, B Lee, T Halkides, DJ Waliser, DE AF Guan, Bin Lee, Tong Halkides, Daria J. Waliser, Duane E. TI Aquarius surface salinity and the Madden-Julian Oscillation: The role of salinity in surface layer density and potential energy SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Aquarius; salinity; MJO; satellite ID MOIST THERMODYNAMIC STRUCTURE; INTRASEASONAL OSCILLATIONS; TROPICAL CYCLONES; WESTERN PACIFIC; MJO; OCEAN; TEMPERATURE; CIRCULATION; MODEL; VARIABILITY AB Sea surface salinity (SSS) data from the Aquarius satellite are analyzed along with auxiliary data to investigate the SSS signature of the Madden-Julian Oscillation (MJO) in the equatorial Indian and Pacific Oceans, the effect of evaporation-minus-precipitation (E-P), the implication for the role of ocean dynamics, and the SSS influence on surface density and potential energy. MJO-related SSS changes are consistent with E-P forcing in the western Indian Ocean throughout the MJO cycle and in the central Indian Ocean during the wet phase of the MJO cycle. However, SSS changes cannot be explained by E-P in the central Indian Ocean during the dry phase and in the eastern Indian and western Pacific Oceans throughout the MJO cycle, implying the importance of ocean dynamics. SSS has an overall larger contribution to MJO-related surface density and potential energy anomalies than SST. It partially offsets the SST effect in the western-to-central Indian Ocean and reinforces the SST effect in the eastern Indian and western Pacific Oceans. Ocean modeling and assimilation need to properly account for salinity effects in order to correctly represent mixed layer variability associated with the MJO. Our results also clarify some discrepancy in previous studies about the E-P effect on MJO-related SSS variations. Key Points Clarifies role of E-P on MJO-related salinity and implication for ocean dynamics Corrects misinterpretation in a recent study about the role of E-P on salinity Reveals the important effects of salinity in surface layer density and energy C1 [Guan, Bin; Halkides, Daria J.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Guan, Bin; Lee, Tong; Halkides, Daria J.; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Lee, T (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Tong.Lee@jpl.nasa.gov RI Guan, Bin/F-6735-2010 FU National Aeronautics and Space Administration (NASA) FX The research described in this paper was in part carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). NR 60 TC 8 Z9 8 U1 0 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD APR 28 PY 2014 VL 41 IS 8 BP 2858 EP 2869 DI 10.1002/2014GL059704 PG 12 WC Geosciences, Multidisciplinary SC Geology GA AH0KW UT WOS:000335809800026 ER PT J AU Ye, HC Fetzer, EJ Wong, S Behrangi, A Olsen, ET Cohen, J Lambrigtsen, BH Chen, LK AF Ye, Hengchun Fetzer, Eric J. Wong, Sun Behrangi, Ali Olsen, Edward T. Cohen, Judah Lambrigtsen, Bjorn H. Chen, Luke TI Impact of increased water vapor on precipitation efficiency over northern Eurasia SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE atmospheric precipitable water; precipitation; relative humidity; northern Eurasia; High latitudes; water vapor ID HYDROLOGICAL CYCLE; TEMPERATURE; VARIABILITY; FREQUENCY; HUMIDITY; TRENDS; MODEL; GCM AB This study investigates the relationships among water vapor, precipitation efficiency, precipitation amount, and air temperature anomalies on monthly time scales over northern Eurasia for winter and summer 2003-2010. Daily precipitation and temperature records at 505 historical stations, and atmospheric total precipitable water vapor and relative humidity data from Atmospheric Infrared Sounders, are used for analysis. Results show that higher atmospheric precipitable water associated with warmer temperature directly contributes to winter precipitation amount but has little impact on winter precipitation efficiency. However, accelerated decreasing relative humidity associated with higher temperature is the primary factor in the reduction of precipitation efficiency and precipitation amount regardless of higher precipitable water in summer. This study suggests that there are evident seasonal differences in precipitation trend associated with air temperature changes over the study region. Air temperature modifies a key atmospheric water variable that directly controls precipitation for that particular season. Key Points Increasing water vapor directly contributes to winter precipitation Reduced summer precipitation is related to accelerated decreasing RH C1 [Ye, Hengchun] Calif State Univ Los Angeles, Dept Geosci & Environm, Los Angeles, CA 90032 USA. [Fetzer, Eric J.; Wong, Sun; Behrangi, Ali; Olsen, Edward T.; Lambrigtsen, Bjorn H.; Chen, Luke] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Cohen, Judah] Atmospher & Environm Res Inc, Lexington, MA USA. RP Ye, HC (reprint author), Calif State Univ Los Angeles, Dept Geosci & Environm, Los Angeles, CA 90032 USA. EM hye2@calstatela.edu FU NSF [BCS-1060788]; JPL's Summer Faculty Fellow [BCS-1060323] FX 5This research is supported by NSF grant BCS-1060788 and JPL's Summer Faculty Fellow for HY; BCS-1060323 for JC. The authors wish to express our gratitude toward the Carbon Dioxide Information Analysis Center for providing the historical station precipitation data. We appreciate the supportive comments and valuable suggestions from the three anonymous reviewers that have improved the quality of this research. NR 43 TC 7 Z9 8 U1 0 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 APR 28 PY 2014 VL 41 IS 8 BP 2941 EP 2947 DI 10.1002/2014GL059830 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AH0KW UT WOS:000335809800037 ER PT J AU Zhao, YD Chen, XM Park, C Fay, CC Stupkiewicz, S Ke, CH AF Zhao, Yadong Chen, Xiaoming Park, Cheol Fay, Catharine C. Stupkiewicz, Stanislaw Ke, Changhong TI Mechanical deformations of boron nitride nanotubes in crossed junctions SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID INDIVIDUAL CARBON NANOTUBES; ELASTIC-MODULUS; WALLED CARBON; FORCE; OXIDATION AB We present a study of the mechanical deformations of boron nitride nanotubes (BNNTs) in crossed junctions. The structure and deformation of the crossed tubes in the junction are characterized by using atomic force microscopy. Our results show that the total tube heights are reduced by 20%-33% at the crossed junctions formed by double-walled BNNTs with outer diameters in the range of 2.21-4.67 nm. The measured tube height reduction is found to be in a nearly linear relationship with the summation of the outer diameters of the two tubes forming the junction. The contact force between the two tubes in the junction is estimated based on contact mechanics theories and found to be within the range of 4.2-7.6 nN. The Young's modulus of BNNTs and their binding strengths with the substrate are quantified, based on the deformation profile of the upper tube in the junction, and are found to be 1.07 +/- 0.11 TPa and 0.18-0.29 nJ/m, respectively. Finally, we perform finite element simulations on the mechanical deformations of the crossed BNNT junctions. The numerical simulation results are consistent with both the experimental measurements and the analytical analysis. The results reported in this paper contribute to a better understanding of the structural and mechanical properties of BNNTs and to the pursuit of their applications. (C) 2014 AIP Publishing LLC. C1 [Zhao, Yadong; Chen, Xiaoming; Ke, Changhong] SUNY Binghamton, Dept Mech Engn, Binghamton, NY 13902 USA. [Park, Cheol; Fay, Catharine C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Park, Cheol] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA. [Stupkiewicz, Stanislaw] Inst Fundamental Technol Res, PL-00049 Warsaw, Poland. RP Ke, CH (reprint author), SUNY Binghamton, Dept Mech Engn, Binghamton, NY 13902 USA. EM cke@binghamton.edu RI Ke, Changhong/C-4064-2008; Stupkiewicz, Stanislaw/J-8417-2012; CHEN, XIAOMING/A-1377-2016 OI Stupkiewicz, Stanislaw/0000-0002-4592-3576; FU U.S. Air Force Office of Scientific Research-Low Density Materials program [FA9550-11-1-0042, FA9550-10-1-0451]; National Science Center (NCN) in Poland [2011/01/B/ST8/07434] FX This work was funded by U.S. Air Force Office of Scientific Research-Low Density Materials program under Grant Nos. FA9550-11-1-0042 and FA9550-10-1-0451. S.S. acknowledges the financial support of the National Science Center (NCN) in Poland under Grant No. 2011/01/B/ST8/07434. The authors thank Dr. In-tae Bae for his assistance with the TEM characterization. The TEM characterizations were performed using the facilities in the Analytical and Diagnostics Laboratory at Binghamton University's Small Scale Systems Integration and Packaging Center (S3IP). NR 46 TC 7 Z9 7 U1 2 U2 17 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD APR 28 PY 2014 VL 115 IS 16 AR 164305 DI 10.1063/1.4872238 PG 9 WC Physics, Applied SC Physics GA AG2EH UT WOS:000335228400060 ER PT J AU Mocquet, A Grasset, O Sotin, C AF Mocquet, A. Grasset, O. Sotin, C. TI Very high-density planets: a possible remnant of gas giants SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE exoplanets; internal structures; naked cores; gas giants; icy giants ID MASS-RADIUS RELATIONSHIPS; SUPER-EARTHS; SOLID EXOPLANETS; OCEAN-PLANETS; HIGH-PRESSURE; HOT JUPITERS; ATMOSPHERE; VISCOSITY AB Data extracted from the Extrasolar Planets Encyclopaedia (see http://exoplanet.eu) show the existence of planets that are more massive than iron cores that would have the same size. After meticulous verification of the data, we conclude that the mass of the smallest of these planets is actually not known. However, the three largest planets, Kepler-52b, Kepler-52c and Kepler-57b, which are between 30 and 100 times the mass of the Earth, have indeed density larger than an iron planet of the same size. This observation triggers this study that investigates under which conditions these planets could represent the naked cores of gas giants that would have lost their atmospheres during their migration towards the star. This study shows that for moderate viscosity values (10(25) Pa s or lower), large values of escape rate and associated unloading stress rate during the atmospheric loss process lead to the explosion of extremely massive planets. However, for moderate escape rate, the bulk viscosity and finite-strain incompressibility of the cores of giant planets can be large enough to retain a very high density during geological time scales. This would make those a new kind of planet, which would help in understanding the interior structure of the gas giants. However, this new family of exoplanets adds some degeneracy for characterizing terrestrial exoplanets. C1 [Mocquet, A.; Grasset, O.] Univ Nantes, CNRS, UMR 6112, LPG Nantes, F-44322 Nantes 03, France. [Sotin, C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Grasset, O (reprint author), Univ Nantes, CNRS, UMR 6112, LPG Nantes, 2 Rue Houssiniere, F-44322 Nantes 03, France. EM olivier.grasset@univ-nantes.fr NR 36 TC 2 Z9 2 U1 3 U2 11 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-503X EI 1471-2962 J9 PHILOS T R SOC A JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci. PD APR 28 PY 2014 VL 372 IS 2014 AR 20130164 DI 10.1098/rsta.2013.0164 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AD6XM UT WOS:000333404700016 PM 24664925 ER PT J AU Jin, ZH Lukachin, C Roberts, Y Wielicki, B Feldman, D Collins, W AF Jin, Zhonghai Lukachin, Constantin Roberts, Yolanda Wielicki, Bruce Feldman, Daniel Collins, William TI Interannual variability of the Earth's spectral solar reflectance from measurements and simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE interannual variability; spectral solar reflectance; climate benchmark ID MODELS; SYSTEM AB The mean solar spectral reflectance averaged over large spatiotemporal scales is an important climate benchmark data product proposed for the Climate Absolute Radiance and Refractivity Observatory mission. The interannual variability of these reflectances over the ocean is examined through satellite-measured hyperspectral data and through satellite instrument emulation based on model simulation. Such large domain-averaged reflectances show small interannual variation, usually under few percent, depending on the latitude region and spatiotemporal scale used for averaging. Although the interannual variation is usually less than the absolute accuracy of model calculation, the model simulated interannual variations are consistent with the measurements because most of the modeling errors in the reflectance averaged in large climate domains are systematic and are canceled out in the interannual difference spectra. The interannual variability is also shown to decrease as the temporal and spatial scales increase. Both the observational data and the model simulations show that the natural variability in the annual mean reflectance is about 50% lower than that in the monthly mean over all spectra. The interannual variability determined from observations in large climate domains also compares favorably with that from the climate Observing System Simulation Experiment based on climate model simulations; both show a standard deviation of less than 1% of the mean reflectance across all spectra for global and annual average over the ocean. Key Points Interannual variation of solar reflectance in large climate domains is small Simulated variation is consistent with hyperspectral satellite measurements Variance decreases as time/space scales increase, under 1% for global average C1 [Jin, Zhonghai] Sci Syst & Applicat, Hampton, VA 23666 USA. [Jin, Zhonghai; Lukachin, Constantin; Roberts, Yolanda; Wielicki, Bruce] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23665 USA. [Feldman, Daniel; Collins, William] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Collins, William] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Climate Sci Dept, Berkeley, CA 94720 USA. RP Jin, ZH (reprint author), Sci Syst & Applicat, Hampton, VA 23666 USA. EM zhonghai.jin@nasa.gov RI Collins, William/J-3147-2014; Richards, Amber/K-8203-2015; Feldman, Daniel/N-8703-2013 OI Collins, William/0000-0002-4463-9848; Feldman, Daniel/0000-0003-3365-5233 FU CLARREO project of NASA FX We thank the SCIAMACHY team for the solar radiance data, the NASA CERES group for the SSF data, and Sky Yang for the ozone data. The CERES SSF data are available at the Atmospheric Science Data Center (ASDC) at NASA Langley Research Center (https://eosweb.larc.nasa.gov/project/ceres/ssf_table). The SCIAMACHY data are provided through ESA by DLR (http://atmos.caf.dlr.de/projects/scops/). The SMOBA ozone data are provided by Sky Yang (Sk.Yang@noaa.gov) at NOAA. Amber Richards and Rosemary Baize helped with the English editing. This research is supported by the CLARREO project of NASA. NR 19 TC 3 Z9 3 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 27 PY 2014 VL 119 IS 8 BP 4458 EP 4470 DI 10.1002/2013JD021056 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH0KP UT WOS:000335809100002 ER PT J AU Yao, YJ Liang, SL Li, XL Hong, Y Fisher, JB Zhang, NN Chen, JQ Cheng, J Zhao, SH Zhang, XT Jiang, B Sun, L Jia, K Wang, KC Chen, Y Mu, QZ Feng, F AF Yao, Yunjun Liang, Shunlin Li, Xianglan Hong, Yang Fisher, Joshua B. Zhang, Nannan Chen, Jiquan Cheng, Jie Zhao, Shaohua Zhang, Xiaotong Jiang, Bo Sun, Liang Jia, Kun Wang, Kaicun Chen, Yang Mu, Qiaozhen Feng, Fei TI Bayesian multimodel estimation of global terrestrial latent heat flux from eddy covariance, meteorological, and satellite observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Review DE latent heat flux; evapotranspiration; Bayesian model averaging method; simple model averaging method ID REFLECTANCE DISTRIBUTION FUNCTION; LAND-SURFACE EVAPORATION; ENERGY-BALANCE CLOSURE; NET PRIMARY PRODUCTION; SOUTHERN GREAT-PLAINS; REMOTELY-SENSED DATA; CARBON-DIOXIDE; EVAPOTRANSPIRATION ALGORITHM; ALBEDO RETRIEVALS; BOREAL FOREST AB Accurate estimation of the satellite-based global terrestrial latent heat flux (LE) at high spatial and temporal scales remains a major challenge. In this study, we introduce a Bayesian model averaging (BMA) method to improve satellite-based global terrestrial LE estimation by merging five process-based algorithms. These are the Moderate Resolution Imaging Spectroradiometer (MODIS) LE product algorithm, the revised remote-sensing-based Penman-Monteith LE algorithm, the Priestley-Taylor-based LE algorithm, the modified satellite-based Priestley-Taylor LE algorithm, and the semi-empirical Penman LE algorithm. We validated the BMA method using data for 2000-2009 and by comparison with a simple model averaging (SA) method and five process-based algorithms. Validation data were collected for 240 globally distributed eddy covariance tower sites provided by FLUXNET projects. The validation results demonstrate that the five process-based algorithms used have variable uncertainty and the BMA method enhances the daily LE estimates, with smaller root mean square errors (RMSEs) than the SA method and the individual algorithms driven by tower-specific meteorology and Modern Era Retrospective Analysis for Research and Applications (MERRA) meteorological data provided by the NASA Global Modeling and Assimilation Office (GMAO), respectively. The average RMSE for the BMA method driven by daily tower-specific meteorology decreased by more than 5 W/m(2) for crop and grass sites, and by more than 6 W/m(2) for forest, shrub, and savanna sites. The average coefficients of determination (R-2) increased by approximately 0.05 for most sites. To test the BMA method for regional mapping, we applied it for MODIS data and GMAO-MERRA meteorology to map annual global terrestrial LE averaged over 2001-2004 for spatial resolution of 0.05 degrees. The BMA method provides a basis for generating a long-term global terrestrial LE product for characterizing global energy, hydrological, and carbon cycles. Key Points BMA-based latent heat flux estimation Global terrestrial LE estimation Integrating five process-based algorithms C1 [Yao, Yunjun; Liang, Shunlin; Li, Xianglan; Cheng, Jie; Zhang, Xiaotong; Jiang, Bo; Jia, Kun; Feng, Fei] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, State Key Lab Remote Sensing Sci, Beijing 100875, Peoples R China. [Liang, Shunlin] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Hong, Yang] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA. [Hong, Yang] Tsinghua Univ, Dept Hydraul Engn, Beijing 100084, Peoples R China. [Hong, Yang] Tsinghua Univ, State Key Lab Hydrosci & Engn, Beijing 100084, Peoples R China. [Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Zhang, Nannan] Hohai Univ, Sch Earth Sci & Engn, Nanjing, Jiangsu, Peoples R China. [Chen, Jiquan] Univ Toledo, Dept Environm Sci, Toledo, OH 43606 USA. [Zhao, Shaohua] Minist Environm Protect, Environm Satellite Ctr, Beijing, Peoples R China. [Sun, Liang] Chinese Acad Agr Sci, Inst Agr Resources & Reg Planning, Beijing 100193, Peoples R China. [Wang, Kaicun; Chen, Yang] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, State Key Lab Earth Surface Proc & Resource Ecol, Beijing 100875, Peoples R China. [Mu, Qiaozhen] Univ Montana, Dept Ecosyst & Conservat Sci, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. RP Yao, YJ (reprint author), Beijing Normal Univ, Coll Global Change & Earth Syst Sci, State Key Lab Remote Sensing Sci, Beijing 100875, Peoples R China. EM boyyunjun@163.com; xlli@bnu.edu.cn RI rslab, water/O-7043-2015; Wang, Kaicun/F-7813-2012; Cheng, Jie/G-2039-2011; Chen, Jiquan/D-1955-2009; Hong, Yang/D-5132-2009; Mu, Qiaozhen/G-5695-2010; liang, shunlin/C-2809-2015; rslab, hiwater/O-7037-2015 OI Wang, Kaicun/0000-0002-7414-5400; Fisher, Joshua/0000-0003-4734-9085; Hong, Yang/0000-0001-8720-242X; FU U.S. Department of Energy, Biological and Environmental Research, Terrestrial Carbon Program [DE-FG02-04ER63917, DE-FG02-04ER63911]; CFCAS; NSERC; BIOCAP; Environment Canada; NRCan; CarboEuropeIP; FAO-GTOS-TCO; iLEAPS; Max Planck Institute for Biogeochemistry; National Science Foundation; University of Tuscia; Universite Laval; U.S. Department of Energy; High-Tech Research and Development Program of China [2013AA122801]; Natural Science Fund of China [41201331, 41101310, 41101313, 41301353, 41205104]; National Basic Research Program of China [2012CB955302]; Fundamental Research Funds for the Central Universities [2013YB34]; High Resolution Earth Observation Systems of National Science and Technology Major Projects [05-Y30B02-9001-13/15-9]; National Aeronautics and Space Administration FX Authors thank the three anonymous reviewers for their critical and helpful comments and suggestions. Authors also thank Shaomin Liu, Wenping Yuan, and Ziwei Xu from Beijing Normal University, China; Guangsheng Zhou from the Institute of Botany, CAS; Yan Li and Ran Liu from Xinjiang Institute of Ecology and Geography, CAS; Guoyi Zhou and Yuelin Li from South China Botanic Garden, CAS; and Bin Zhao from Fudan University, China, for providing ground-measured data. This work used eddy covariance data acquired by the FLUXNET community and, in particular, by the following networks: AmeriFlux (U.S. Department of Energy, Biological and Environmental Research, Terrestrial Carbon Program (DE-FG02-04ER63917 and DE-FG02-04ER63911)), AfriFlux, AsiaFlux, CarboAfrica, CarboEuropeIP, CarboItaly, CarboMont, ChinaFlux, Fluxnet-Canada (supported by CFCAS, NSERC, BIOCAP, Environment Canada, and NRCan), GreenGrass, KoFlux, LBA, NECC, OzFlux, TCOS-Siberia, and USCCC. We acknowledge the financial support to the eddy covariance data harmonization provided by CarboEuropeIP, FAO-GTOS-TCO, iLEAPS, Max Planck Institute for Biogeochemistry, National Science Foundation, University of Tuscia, Universite Laval, Environment Canada, and U.S. Department of Energy, and the database development and technical support from Berkeley Water Center, Lawrence Berkeley National Laboratory, Microsoft Research eScience, Oak Ridge National Laboratory, University of California-Berkeley, and the University of Virginia. Other ground-measured data were obtained from the GAME ANN (http://aan.suiri.tsukuba.ac.jp/), the Coordinated Enhanced Observation Project (CEOP) in arid and semiarid regions of northern China (http://observation.tea.ac.cn/), and the water experiments of Environmental and Ecological Science Data Center for West China (http://westdc.westgis.ac.cn/water). MODIS LAI/FPAR, NDVI, albedo, and land cover satellite products were obtained online (http://reverb.echo.nasa.gov/reverb). This work was partially supported by the High-Tech Research and Development Program of China (2013AA122801), the Natural Science Fund of China (41201331, 41101310, 41101313, 41301353, and 41205104), the National Basic Research Program of China (2012CB955302), the Fundamental Research Funds for the Central Universities (2013YB34), the High Resolution Earth Observation Systems of National Science and Technology Major Projects (05-Y30B02-9001-13/15-9). J.B.F. contributed to this paper from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 105 TC 17 Z9 18 U1 5 U2 67 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 APR 27 PY 2014 VL 119 IS 8 BP 4521 EP 4545 DI 10.1002/2013JD020864 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH0KP UT WOS:000335809100007 ER PT J AU Tang, L Tian, YD Lin, X AF Tang, Ling Tian, Yudong Lin, Xin TI Validation of precipitation retrievals over land from satellite- based passive microwave sensors SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE satellite precipitation; error; passive microwave ID LATENT HEATING DISTRIBUTIONS; CONTINENTAL UNITED-STATES; OCEAN RAIN RATE; PHYSICAL RETRIEVALS; SOUNDING UNIT; ALGORITHMS; RESOLUTION; PRODUCTS; CLOUD; IMAGER/SOUNDER AB Precipitation retrievals from spaceborne passive microwave (PMW) radiometers are the backbone of modern satellite-based global precipitation data sets. The error characteristics in these individual retrievals directly affect the merged end products and applications but have not been systematically studied. This paper focuses on extensive and systematic validation of PMW precipitation retrievals and quantification of their error characteristics. Retrievals from 12 PMW radiometers were evaluated and intercompared at instantaneous scale (5min) over continental United States. These precipitation-sensing radiometers include both imagers (Tropical Rainfall Measuring Mission Microwave Imager, Advanced Microwave Scanning Radiometer for the Earth Observing System, Special Sensor Microwave Imager, and Special Sensor Microwave Imager/Sounder) and sounders (advanced microwave sounding unit-B and Microwave Humidity Sounders). A high-resolution ground radar-based data set over the continental United States was used as the ground reference data. The high spatial and temporal resolution of the reference data allows collocation within 5min and relatively more precise comparison with the satellite overpasses. Our results show that PMW sensor retrievals exhibit fairly systematic biases depending on season and precipitation intensity, with overestimates in summer at moderate to high precipitation rates and underestimates in winter at low and moderate precipitation rates. Retrievals from the microwave imagers have notably better performance than those from the sounders. The latter tend to have a narrower dynamic range, higher biases, and random errors. Key Points Extensive and systematic validation for L2 precipitation retrievals from PMWs Fairly systematic biases Imagers have notably better performance than the sounders C1 [Tang, Ling; Tian, Yudong; Lin, Xin] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Tang, Ling; Tian, Yudong; Lin, Xin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tang, L (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM ltang21@umd.edu RI Measurement, Global/C-4698-2015 FU NASA Earth System Data Records Uncertainty Analysis Program [NNH10ZDA001N-ESDRERR] FX This research was supported by the NASA Earth System Data Records Uncertainty Analysis Program (Martha E. Maiden) under solicitation NNH10ZDA001N-ESDRERR. Computing resources were provided by the NASA Center for Climate Simulation. We appreciate the assistance and advice from Bob Adler, Bob Joyce, Eric Nelkin, Daniel Vila, Huan Meng, Nai-Yu Wang, and Jun Dong. Helpful comments and suggestions from three anonymous reviewers are gratefully acknowledged. NR 51 TC 20 Z9 21 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 27 PY 2014 VL 119 IS 8 BP 4546 EP 4567 DI 10.1002/2013JD020933 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH0KP UT WOS:000335809100008 ER PT J AU Dumka, UC Tripathi, SN Misra, A Giles, DM Eck, TF Sagar, R Holben, BN AF Dumka, U. C. Tripathi, S. N. Misra, Amit Giles, D. M. Eck, T. F. Sagar, Ram Holben, B. N. TI Latitudinal variation of aerosol properties from IndoGangetic Plain to central Himalayan foothills during TIGERZ campaign SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Central Himalayas; heating rate; aerosol radiative forcing; aerosol optical properites; TIGERZ ID INDO-GANGETIC BASIN; SKY RADIANCE MEASUREMENTS; TROPICAL INDIAN-OCEAN; OPTICAL-PROPERTIES; NORTHERN INDIA; ORGANIC-CARBON; DUST STORMS; AERONET; DEPTH; ABSORPTION AB As part of TIGERZ campaign, latitudinal variation of aerosol optical properties was analyzed over Indo-Gangetic Plains (IGP) to central Himalayas during premonsoon of 2008 and 2009. Measurements of aerosol optical depth (AOD) were performed using Aerosol Robotic Network Sun photometer at four sites with different aerosol environments. The AOD increases from Nainital located in central Himalayas to Kanpur located in IGP region. Further, aerosol size varies spatially with dominance of coarse-mode aerosols at Kanpur compared to fine-mode aerosols dominated at Nainital. Spectral variation of single-scattering albedo suggests that during premonsoon, dust is the dominant species in the IGP with exception of Pantnagar, where absorbing aerosols are dominant. The optical properties of aerosols are calculated, and shortwave clear-sky aerosol radiative forcing (ARF) is estimated. An insignificant difference is found in columnar ARF and columnar heating rate (HR) when vertical profiles of aerosols are included in radiative transfer models. Over Nainital, average ARF is estimated to be -7.61, -45.75, and 38.14Wm(-2) at top of atmosphere (TOA), surface (SUR), and in the atmosphere (ATM), respectively. Average ARF is less negative at Kanpur compared to Pantnagar and Bareilly with values -17.63, -73.06, and 55.43Wm(-2) at TOA, SUR, and ATM, respectively. ARF shows positive gradient from the highlands to the IGP sites; larger TOA and SUR cooling were observed at the three sites compared to the highland site. This translates into large columnar HR with estimated average values as 1.07, 1.41, 1.58, and 1.56 Kd(-1) for Nainital, Pantnagar, Bareilly, and Kanpur, respectively. C1 [Dumka, U. C.; Sagar, Ram] Aryabhatta Res Inst Observat Sci, Naini Tal, India. [Tripathi, S. N.; Misra, Amit] Indian Inst Technol, Dept Civil Engn, Kanpur 208016, Uttar Pradesh, India. [Giles, D. M.] Sigma Space Corp, Lanham, MD USA. [Giles, D. M.; Eck, T. F.; Holben, B. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eck, T. F.] Univ Space Res Assoc, Columbia, MD USA. RP Dumka, UC (reprint author), Aryabhatta Res Inst Observat Sci, Naini Tal, India. EM dumka@aries.res.in; snt@iitk.ac.in RI Dumka, Umesh /D-3520-2015; Tripathi, Sachchida/J-4840-2016 OI Dumka, Umesh /0000-0001-9448-1543; FU National Academy of Science; U.S. Agency for International Development FX The authors thank the editor and anonymous reviewers for their valuable comments and suggestions which significantly improved the paper. A part of this work was supported by National Academy of Science and U.S. Agency for International Development. The authors would like to acknowledge Harish Vishwakarma at IIT-Kanpur for field support during TIGERZ. The authors thank the AERONET team for calibrating and maintaining the instrument and processing the data. The NCEP reanalysis data are obtained from http://www.cdc.noaa.gov, and CALIPSO extinction coefficients are obtained from http://www-calipso.larc.nasa.gov/tools/data_avail/. NR 66 TC 15 Z9 15 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 27 PY 2014 VL 119 IS 8 BP 4750 EP 4769 DI 10.1002/2013JD021040 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH0KP UT WOS:000335809100020 ER PT J AU Douglass, AR Strahan, SE Oman, LD Stolarski, RS AF Douglass, A. R. Strahan, S. E. Oman, L. D. Stolarski, R. S. TI Understanding differences in chemistry climate model projections of stratospheric ozone SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE stratospheric ozone; chemistry climate models ID MIDDLE ATMOSPHERE; CHLORINE PERTURBATIONS; INORGANIC CHLORINE; TRANSPORT MODEL; TECHNICAL NOTE; TRENDS; CLONO2; SENSITIVITY; HCL; PHOTOCHEMISTRY AB Chemistry climate models (CCMs) are used to project future evolution of stratospheric ozone as concentrations of ozone-depleting substances (ODSs) decrease and greenhouse gases increase, cooling the stratosphere. CCM projections exhibit not only many common features but also a broad range of values for quantities such as year of ozone return to 1980 and global ozone level at the end of the 21st century. Multiple linear regression is applied to each of 14 CCMs to separate ozone response to ODS concentration change from that due to climate change. We show that the sensitivity of lower stratospheric ozone to chlorine change O-3/Cl-y is a near-linear function of partitioning of total inorganic chlorine (Cl-y) into its reservoirs; both Cl-y and its partitioning are largely controlled by lower stratospheric transport. CCMs with best performance on transport diagnostics agree with observations for chlorine reservoirs and produce similar ozone responses to chlorine change. After 2035, differences in O-3/Cl-y contribute little to the spread in CCM projections as the anthropogenic contribution to Cl-y becomes unimportant. Differences among upper stratospheric ozone increases due to temperature decreases are explained by differences in ozone sensitivity to temperature change O-3/T due to different contributions from various ozone loss processes, each with its own temperature dependence. Ozone decrease in the tropical lower stratosphere caused by a projected speedup in the Brewer-Dobson circulation may or may not be balanced by ozone increases in the middle- and high-latitude lower stratosphere and upper troposphere. This balance, or lack thereof, contributes most to the spread in late 21st century projections. C1 [Douglass, A. R.; Oman, L. D.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Strahan, S. E.] Univ Space Res Assoc, Columbia, MD USA. [Stolarski, R. S.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. RP Douglass, AR (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Anne.R.Douglass@nasa.gov RI Douglass, Anne/D-4655-2012; Stolarski, Richard/B-8499-2013; Oman, Luke/C-2778-2009 OI Stolarski, Richard/0000-0001-8722-4012; Oman, Luke/0000-0002-5487-2598 FU NASA's Atmospheric Chemistry Modeling and Analysis Program (ACMAP); Modeling and Analysis Program (MAP) FX We acknowledge the modeling groups for making their simulations available for this analysis. The Chemistry-Climate Model Validation Activity (CCMVal) for WCRP's (World Climate Research Programme) SPARC (Stratosphere-troposphere Processes and their Role in Climate) project for organizing and coordinating the model data analysis activity and the British Atmospheric Data Center (BADC) for collecting and archiving the CCMVal model output. The data used in this publication were obtained as part of the Network for the Detection of Atmospheric Composition Change (NDACC) and are publicly available (see http://www.ndacc.org). We appreciate helpful comments from three anonymous reviewers. This work is supported by NASA's Atmospheric Chemistry Modeling and Analysis Program (ACMAP) and Modeling and Analysis Program (MAP). NR 58 TC 3 Z9 3 U1 1 U2 19 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 27 PY 2014 VL 119 IS 8 BP 4922 EP 4939 DI 10.1002/2013JD021159 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH0KP UT WOS:000335809100030 ER PT J AU Divakarla, M Barnet, C Liu, X Gu, DG Wilson, M Kizer, S Xiong, XZ Maddy, E Ferraro, R Knuteson, R Hagan, D Ma, XL Tan, CY Nalli, N Reale, A Mollner, AK Yang, WZ Gambacorta, A Feltz, M Iturbide-Sanchez, F Sun, BM Goldberg, M AF Divakarla, Murty Barnet, Christopher Liu, Xu Gu, Degui Wilson, Michael Kizer, Susan Xiong, Xiaozhen Maddy, Eric Ferraro, Ralph Knuteson, Robert Hagan, Denise Ma, Xia-lin Tan, Changyi Nalli, Nicholas Reale, Anthony Mollner, Andrew K. Yang, Wenze Gambacorta, Antonia Feltz, Michelle Iturbide-Sanchez, Flavio Sun, Bomin Goldberg, Mitch TI The CrIMSS EDR Algorithm: Characterization, Optimization, and Validation SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE CrIMSS; CrIS; ATMS; EDR ID INFRARED SOUNDER TEMPERATURE; TERRESTRIAL MATERIALS; ATMOSPHERIC WINDOW; RADIO OCCULTATION; PRODUCTS; WEATHER; AIRS/AMSU/HSB; RETRIEVALS; EMISSIVITY; CLIMATE AB The Cross-track Infrared Sounder (CrIS) and the Advanced Technology Microwave Sounder (ATMS) instruments aboard the Suomi National Polar-orbiting Partnership satellite provide high-quality hyperspectral infrared and microwave observations to retrieve atmospheric vertical temperature and moisture profiles (AVTP and AVMP) and many other environmental data records (EDRs). The official CrIS and ATMS EDR algorithm, together called the Cross-track Infrared and Microwave Sounding Suite (CrIMSS), produces EDR products on an operational basis through the interface data processing segment. The CrIMSS algorithm group is to assess and ensure that operational EDRs meet beta and provisional maturity requirements and are ready for stages 1-3 validations. This paper presents a summary of algorithm optimization efforts, as well as characterization and validation of the AVTP and AVMP products using the European Centre for Medium-Range Weather Forecasts (ECMWF) analysis, the Atmospheric Infrared Sounder (AIRS) retrievals, and conventional and dedicated radiosonde observations. The global root-mean-square (RMS) differences between the CrIMSS products and the ECMWF show that the AVTP is meeting the requirements for layers 30-300hPa (1.53K versus 1.5K) and 300-700hPa (1.28K versus 1.5K). Slightly higher RMS difference for the 700hPa-surface layer (1.78K versus 1.6K) is attributable to land and polar profiles. The AVMP product is within the requirements for 300-600hPa (26.8% versus 35%) and is close in meeting the requirements for 600hPa-surface (25.3% versus 20%). After just one year of maturity, the CrIMSS EDR products are quite comparable to the AIRS heritage algorithm products and show readiness for stages 1-3 validations. C1 [Divakarla, Murty; Wilson, Michael; Xiong, Xiaozhen; Tan, Changyi; Nalli, Nicholas; Gambacorta, Antonia; Iturbide-Sanchez, Flavio; Sun, Bomin] IM Syst Grp Inc, Rockville, MD 20852 USA. [Barnet, Christopher] Sci & Technol Corp, Columbia, MD USA. [Liu, Xu] NASA Langley Res Ctr, Hampton, VA USA. [Gu, Degui; Hagan, Denise; Ma, Xia-lin] Northrop Grumman Aerosp Syst, Redondo Beach, CA USA. [Kizer, Susan] Sci Syst & Applicat Inc, Hampton, VA USA. [Maddy, Eric] Sci & Technol Corp, Hampton, VA 23666 USA. [Ferraro, Ralph; Reale, Anthony; Goldberg, Mitch] NOAA Ctr Satellite Applicat & Res, College Pk, MD USA. [Knuteson, Robert] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA. [Mollner, Andrew K.] Aerosp Corp, El Segundo, CA 90245 USA. [Yang, Wenze] Univ Maryland, ESSIC CICS, College Pk, MD 20742 USA. [Feltz, Michelle] Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI USA. RP Divakarla, M (reprint author), IM Syst Grp Inc, Rockville, MD 20852 USA. EM Murty.Divakarla@noaa.gov RI Reale, Tony/F-5621-2010; Yang, Wenze/B-8356-2012; Sun, Bomin/P-8742-2014; Gambacorta, Antonia/E-7937-2011; Maddy, Eric/G-3683-2010; Ferraro, Ralph/F-5587-2010; Nalli, Nicholas/F-6731-2010; Richards, Amber/K-8203-2015; Divakarla, Murty/E-7936-2011; Iturbide-Sanchez, Flavio/F-9186-2014; Tan, Changyi/F-4786-2010; Xiong, Xiaozhen/F-6591-2010; Wilson, Michael/G-9611-2013 OI Feltz, Michelle/0000-0001-5871-0353; Reale, Tony/0000-0003-2150-5246; Yang, Wenze/0000-0001-8514-2742; Sun, Bomin/0000-0002-4872-9349; Gambacorta, Antonia/0000-0002-2446-9132; Maddy, Eric/0000-0003-1151-339X; Ferraro, Ralph/0000-0002-8393-7135; Nalli, Nicholas/0000-0002-6914-5537; Divakarla, Murty/0000-0002-0399-3381; Iturbide-Sanchez, Flavio/0000-0002-8539-0073; FU JPSS Program Office FX We wish to thank the European Centre for Medium-Range Forecasting group and the National Center for Environmental Prediction for providing the ECMWF and NCEP data used in this paper. We also express our sincere appreciation to the Jet Propulsion Laboratory and the Goddard Earth Sciences Data and Information Services Center for providing the AIRS V6 retrievals for the focus days. The funding for this paper has been provided by the JPSS Program Office and is gratefully acknowledged. The manuscript contents are solely the opinions of the authors and do not constitute a statement of policy, decision, or position on behalf of NOAA, NASA, or the U.S. Government. NR 51 TC 10 Z9 10 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 27 PY 2014 VL 119 IS 8 BP 4953 EP 4977 DI 10.1002/2013JD020438 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH0KP UT WOS:000335809100032 ER PT J AU Waller, RG Stone, RP Johnstone, J Mondragon, J AF Waller, Rhian G. Stone, Robert P. Johnstone, Julia Mondragon, Jennifer TI Sexual Reproduction and Seasonality of the Alaskan Red Tree Coral, Primnoa pacifica SO PLOS ONE LA English DT Article ID DEEP-SEA; FUNGIACYATHUS-MARENZELLERI; POCILLOPORA-DAMICORNIS; FERTILIZATION SUCCESS; MARINE-INVERTEBRATES; WATER CORALS; OCTOCORAL; ECOLOGY; REEF; GROWTH AB The red tree coral Primnoa pacifica is an important habitat forming octocoral in North Pacific waters. Given the prominence of this species in shelf and upper slope areas of the Gulf of Alaska where fishing disturbance can be high, it may be able to sustain healthy populations through adaptive reproductive processes. This study was designed to test this hypothesis, examining reproductive mode, seasonality and fecundity in both undamaged and simulated damaged colonies over the course of 16 months using a deepwater-emerged population in Tracy Arm Fjord. Females within the population developed asynchronously, though males showed trends of synchronicity, with production of immature spermatocysts heightened in December/January and maturation of gametes in the fall months. Periodicity of individuals varied from a single year reproductive event to some individuals taking more than the 16 months sampled to produce viable gametes. Multiple stages of gametes occurred in polyps of the same colony during most sampling periods. Mean oocyte size ranged from 50 to 200 mu m in any season, and maximum oocyte size (802 mu m) suggests a lecithotrophic larva. No brooding larvae were found during this study, though unfertilized oocytes were found adhered to the outside of polyps, where they are presumably fertilized. This species demonstrated size-dependent reproduction, with gametes first forming in colonies over 42-cm length, and steady oocyte sizes being achieved after reaching 80-cm in length. The average fecundity was 86 (+/- 12) total oocytes per polyp, and 17 (+/- 12) potential per polyp fecundity. Sub-lethal injury by removing 21-40% of colony tissue had no significant reproductive response in males or females over the course of this study, except for a corresponding loss in overall colony fecundity. The reproductive patterns and long gamete generation times observed in this study indicate that recruitment events are likely to be highly sporadic in this species increasing its vulnerability to anthropogenic disturbances. C1 [Waller, Rhian G.] Univ Maine, Darling Marine Ctr, Sch Marine Sci, Walpole, ME 04573 USA. [Stone, Robert P.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK USA. [Johnstone, Julia] Univ Maine, Darling Marine Ctr, Walpole, ME 04573 USA. [Mondragon, Jennifer] NOAA, Alaska Reg Off, Natl Marine Fisheries Serv, Juneau, AK USA. RP Waller, RG (reprint author), Univ Maine, Darling Marine Ctr, Sch Marine Sci, Walpole, ME 04573 USA. EM rhian.waller@maine.edu FU National Oceanic and Atmospheric Administration Alaska Fisheries Science Center; National Geographic Society FX This work was funded by the National Oceanic and Atmospheric Administration Alaska Fisheries Science Center, and through the National Geographic Society. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 53 TC 7 Z9 8 U1 5 U2 18 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 25 PY 2014 VL 9 IS 4 AR e90893 DI 10.1371/journal.pone.0090893 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AI3CM UT WOS:000336736600001 PM 24770675 ER PT J AU Van Gorp, B Mouroulis, P Blaney, D Green, RO Ehlmann, BL Rodriguez, JI AF Van Gorp, Byron Mouroulis, Pantazis Blaney, Diana Green, Robert O. Ehlmann, Bethany L. Rodriguez, Jose I. TI Ultra-compact imaging spectrometer for remote, in situ, and microscopic planetary mineralogy SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE imaging spectroscopy; imaging spectrometer; mineralogy; Mars rover; microspectroscopy ID SPECTROSCOPY; SURFACE AB The ultra-compact imaging spectrometer is a miniature imaging spectrometer that has been designed for compatibility with operation in a Martian environment. The spectrometer can be mated to a variety of front optics, both telescopic and microscopic. With a miniature telescope, it can serve as a rover mast instrument that surveys the surrounding area from a distance of similar to 1 m to infinity and produces full spectral data (500 to 2500 nm) of a wide panoramic scene in order to find the most mineralogically promising targets for further analysis and for directing subsequent rover activities. With a microscopic front lens, it can serve as an analytical tool for determining types of minerals in a rock and their spatial relations at a scale of tens of micrometers in order to make detailed interpretations of geological history. A realization of the instrument, adapted for operation in the Earth's atmosphere, has been produced and tested both in the laboratory and in the field. The results prove the ability of the instrument to detect and map minerals of interest in both modes of operation. (C) 2014 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Van Gorp, Byron; Mouroulis, Pantazis; Blaney, Diana; Green, Robert O.; Ehlmann, Bethany L.; Rodriguez, Jose I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ehlmann, Bethany L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Van Gorp, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM byron.e.van.gorp@jpl.nasa.gov NR 21 TC 6 Z9 6 U1 0 U2 5 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 APR 25 PY 2014 VL 8 AR 084988 DI 10.1117/1.JRS.8.084988 PG 16 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AG8BV UT WOS:000335644600001 ER PT J AU Capece, AM Polk, JE Mikellides, IG Shepherd, JE AF Capece, Angela M. Polk, James E. Mikellides, Ioannis G. Shepherd, Joseph E. TI Oxygen transport in the internal xenon plasma of a dispenser hollow cathode SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID IMPREGNATED-CATHODE; ELECTRON-IMPACT; CHARGE-EXCHANGE; CROSS-SECTIONS; BARIUM; MECHANISM; OPERATION; IONIZATION; BA; ATTACHMENT AB Reactive gases such as oxygen and water vapor modify the surface morphology of BaO dispenser cathodes and degrade the electron emission properties. For vacuum cathodes operating at fixed temperature, the emission current drops rapidly when oxygen adsorbs on top of the low work function surface. Previous experiments have shown that plasma cathodes are more resistant to oxygen poisoning and can operate with O-2 partial pressures one to two orders of magnitude higher than vacuum cathodes before the onset of poisoning occurs. Plasma cathodes used for electric thrusters are typically operated with xenon; however, gas phase barium, oxygen, and tungsten species may be found in small concentrations. The densities of these minor species are small compared with the plasma density, and thus, their presence in the discharge does not significantly alter the xenon plasma parameters. It is important, however, to consider the transport of these minor species as they may deposit on the emitter surface and affect the electron emission properties. In this work, we present the results of a material transport model used to predict oxygen fluxes to the cathode surface by solving the species conservation equations in a cathode with a 2.25 mm diameter orifice operated at a discharge current of 15 A, a Xe flow rate of 3.7 sccm, and 100 ppm of O-2. The dominant ionization process for O-2 is resonant charge exchange with xenon ions. Ba is effectively recycled in the plasma; however, BaO and O-2 are not. The model shows that the oxygen flux to the surface is not diffusion-limited; therefore, the high resistance to oxygen poisoning observed in plasma cathodes likely results from surface processes not considered here. (C) 2014 AIP Publishing LLC. C1 [Capece, Angela M.; Shepherd, Joseph E.] CALTECH, Pasadena, CA 91125 USA. [Polk, James E.; Mikellides, Ioannis G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Capece, AM (reprint author), Princeton Plasma Phys Lab, POB 451, Princeton, NJ 08543 USA. EM acapece@pppl.gov RI Shepherd, Joseph/B-5997-2014 OI Shepherd, Joseph/0000-0003-3181-9310 NR 48 TC 1 Z9 1 U1 0 U2 11 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD APR 21 PY 2014 VL 115 IS 15 AR 153302 DI 10.1063/1.4871755 PG 13 WC Physics, Applied SC Physics GA AG2DU UT WOS:000335227100007 ER PT J AU Aasi, J Abadie, J Abbott, BP Abbott, R Abbott, T Abernathy, MR Accadia, T Acernese, F Adams, C Adams, T Adhikari, RX Affeldt, C Agathos, M Aggarwal, N Aguiar, OD Ajith, P Allen, B Allocca, A Ceron, EA Amariutei, D Anderson, RA Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, C Areeda, J Ast, S Aston, SM Astone, P Aufmuth, P Aulbert, C Austin, L Aylott, BE Babak, S Baker, PT Ballardin, G Ballmer, SW Barayoga, JC Barker, D Barnum, SH Barone, F Barr, B Barsotti, L Barsuglia, M Barton, MA Bartos, I Bassiri, R Basti, A Batch, J Bauchrowitz, J Bauer, TS Bebronne, M Behnke, B Bejger, M Beker, MG Bell, AS Bell, C Belopolski, I Bergmann, G Berliner, JM Bersanetti, D Bertolini, A Bessis, D Betzwieser, J Beyersdorf, PT Bhadbhade, T Bilenko, IA Billingsley, G Birch, J Bitossi, M Bizouard, MA Black, E Blackburn, JK Blackburn, L Blair, D Blom, M Bock, O Bodiya, TP Boer, M Bogan, C Bond, C Bondu, F Bonelli, L Bonnand, R Bork, R Born, M Boschi, V Bose, S Bosi, L Bowers, J Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brannen, CA Brau, JE Breyer, J Briant, T Bridges, DO Brillet, A Brinkmann, M Brisson, V Britzger, M Brooks, AF Brown, DA Brown, DD Bruckner, F Bulik, T Bulten, HJ Buonanno, A Buskulic, D Buy, C Byer, RL Cadonati, L Cagnoli, G Bustillo, JC Calloni, E Camp, JB Campsie, P Cannon, KC Canuel, B Cao, J Capano, CD Carbognani, F Carbone, L Caride, S Castiglia, A Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Cella, G Cepeda, C Cesarini, E Chakraborty, R Chalermsongsak, T Chao, S Charlton, P Chassande-Mottin, E Chen, X Chen, Y Chincarini, A Chiummo, A Cho, HS Chow, J Christensen, N Chu, Q Chua, SSY Chung, S Ciani, G Clara, F Clark, DE Clark, JA Cleva, F Coccia, E Cohadon, PF Colla, A Colombini, M Constancio, M Conte, A Conte, R Cook, D Corbitt, TR Cordier, M Cornish, N Corsi, A Costa, CA Coughlin, MW Coulon, JP Countryman, S Couvares, P Coward, DM Cowart, M Coyne, DC Craig, K Creighton, JDE Creighton, TD Crowder, SG Cumming, A Cunningham, L Cuoco, E Dahl, K Dal Canton, T Damjanic, M Danilishin, SL D'Antonio, S Danzmann, K Dattilo, V Daudert, B Daveloza, H Davier, M Davies, GS Daw, EJ Day, R Dayanga, T Debreczeni, G Degallaix, J Deleeuw, E Deleglise, S Del Pozzo, W Denker, T Dent, T Dereli, H Dergachev, V DeRosa, RT De Rosa, R DeSalvo, R Dhurandhar, S Diaz, M Dietz, A Di Fiore, L Di Lieto, A Di Palma, I Di Virgilio, A Dmitry, K Donovan, F Dooley, KL Doravari, S Drago, M Drever, RWP Driggers, JC Du, Z Dumas, JC Dwyer, S Eberle, T Edwards, M Effler, A Ehrens, P Eichholz, J Eikenberry, SS EndrHoczi, G Essick, R Etzel, T Evans, K Evans, M Evans, T Factourovich, M Fafone, V Fairhurst, S Fang, Q Farinon, S Farr, B Farr, W Favata, M Fazi, D Fehrmann, H Feldbaum, D Ferrante, I Ferrini, F Fidecaro, F Finn, LS Fiori, I Fisher, R Flaminio, R Foley, E Foley, S Forsi, E Fotopoulos, N Fournier, JD Franco, S Frasca, S Frasconi, F Frede, M Frei, M Frei, Z Freise, A Frey, R Fricke, TT Fritschel, P Frolov, VV Fujimoto, MK Fulda, P Fyffe, M Gair, J Gammaitoni, L Garcia, J Garufi, F Gehrels, N Gemme, G Genin, E Gennai, A Gergely, L Ghosh, S Giaime, JA Giampanis, S Giardina, KD Giazotto, A Gil-Casanova, S Gill, C Gleason, J Goetz, E Goetz, R Gondan, L Gonzalez, G Gordon, N Gorodetsky, ML Gossan, S Gossler, S Gouaty, R Graef, C Graff, PB Granata, M Grant, A Gras, S Gray, C Greenhalgh, RJS Gretarsson, AM Griffo, C Groot, P Grote, H Grover, K Grunewald, S Guidi, GM Guido, C Gushwa, KE Gustafson, EK Gustafson, R Hall, B Hall, E Hammer, D Hammond, G Hanke, M Hanks, J Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Hartman, MT Haughian, K Hayama, K Heefner, J Heidmann, A Heintze, M Heitmann, H Hello, P Hemming, G Hendry, M Heng, IS Heptonstall, AW Heurs, M Hild, S Hoak, D Hodge, KA Holt, K Hong, T Hooper, S Horrom, T Hosken, DJ Hough, J Howell, EJ Hu, Y Hua, Z Huang, V Huerta, EA Hughey, B Husa, S Huttner, SH Huynh, M Huynh-Dinh, T Iafrate, J Ingram, DR Inta, R Isogai, T Ivanov, A Iyer, BR Izumi, K Jacobson, M James, E Jang, H Jang, YJ Jaranowski, P Jimenez-Forteza, F Johnson, WW Jones, D Jones, DI Jones, R Jonker, RJG Ju, L Haris, K Kalmus, P Kalogera, V Kandhasamy, S Kang, G Kanner, JB Kasprzack, M Kasturi, R Katsavounidis, E Katzman, W Kaufer, H Kaufman, K Kawabe, K Kawamura, S Kawazoe, F Kefelian, F Keitel, D Kelley, DB Kells, W Keppel, DG Khalaidovski, A Khalili, FY Khazanov, EA Kim, BK Kim, C Kim, K Kim, N Kim, W Kim, YM King, EJ King, PJ Kinzel, DL Kissel, JS Klimenko, S Kline, J Koehlenbeck, S Kokeyama, K Kondrashov, V Koranda, S Korth, WZ Kowalska, I Kozak, D Kremin, A Kringel, V Krishnan, B Krolak, A Kucharczyk, C Kudla, S Kuehn, G Kumar, A Kumar, P Kumar, R Kurdyumov, R Kwee, P Landry, M Lantz, B Larson, S Lasky, PD Lawrie, C Leaci, P Lebigot, EO Lee, CH Lee, HK Lee, HM Lee, J Lee, J Leonardi, M Leong, JR Le Roux, A Leroy, N Letendre, N Levine, B Lewis, JB Lhuillier, V Li, TGF Lin, AC Littenberg, TB Litvine, V Liu, F Liu, H Liu, Y Liu, Z Lloyd, D Lockerbie, NA Lockett, V Lodhia, D Loew, K Logue, J Lombardi, AL Lorenzini, M Loriette, V Lormand, M Losurdo, G Lough, J Luan, J Lubinski, MJ Luck, H Lundgren, AP Macarthur, J Macdonald, E Machenschalk, B Maclnnis, M Macleod, DM Magana-Sandoval, F Mageswaran, M Mailand, K Majorana, E Maksimovic, I Malvezzi, V Man, N Manca, M Mandel, I Mandic, V Mangano, V Mantovani, M Marchesoni, F Marion, F Marka, S Marka, Z Markosyan, A Maros, E Marque, J Martelli, F Martin, IW Martin, RM Martinelli, L Martynov, D Marx, JN Mason, K Masserot, A Massinger, TJ Matichard, F Matone, L Matzner, RA Mavalvala, N May, G Mazumder, N Mazzolo, G McCarthy, R McClelland, DE McGuire, SC Mclntyre, G Mclver, J Meacher, D Meadors, GD Mehmet, M Meidam, J Meier, T Melatos, A Mendell, G Mercer, RA Meshkov, S Messenger, C Meyer, MS Miao, H Michel, C Mikhailov, EE Milano, L Miller, J Minenkov, Y Mingarelli, CMF Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Moe, B Mohan, M Mohapatra, SRP Mokler, F Moraru, D Moreno, G Morgado, N Mori, T Morriss, SR Mossavi, K Mours, B Mow-Lowry, CM Mueller, CL Mueller, G Mukherjee, S Mullavey, A Munch, J Murphy, D Murray, PG Mytidis, A Nagy, MF Kumar, DN Nardecchia, I Nash, T Naticchioni, L Nayak, R Necula, V Nelemans, G Neri, I Neri, M Newton, G Nguyen, T Nishida, E Nishizawa, A Nitz, A Nocera, F Nolting, D Normandin, ME Nuttall, LK Ochsner, E O'Dell, J Oelker, E Ogin, GH Oh, JJ Oh, SH Ohme, F Oppermann, P O'Reilly, B Larcher, WO O'Shaughnessy, R Osthelder, C Ott, CD Ottaway, DJ Ottens, RS Ou, J Overmier, H Owen, BJ Padilla, C Pai, A Palomba, C Pan, Y Pankow, C Paoletti, F Paoletti, R Papa, MA Paris, H Pasqualetti, A Passaquieti, R Passuello, D Pedraza, M Peiris, P Penn, S Perreca, A Phelps, M Pichot, M Pickenpack, M Piergiovanni, F Pierro, V Pinard, L Pindor, B Pinto, IM Pitkin, M Poeld, J Poggiani, R Poole, V Poux, C Predoi, V Prestegard, T Price, LR Prijatelj, M Principe, M Privitera, S Prix, R Prodi, GA Prokhorov, L Puncken, O Punturo, M Puppo, P Quetschke, V Quintero, E Quitzow-James, R Raab, FJ Rabeling, DS Racz, I Radkins, H Raffai, P Raja, S Rajalakshmi, G Rakhmanov, M Ramet, C Rapagnani, P Raymond, V Re, V Reed, CM Reed, T Regimbau, T Reid, S Reitze, DH Ricci, F Riesen, R Riles, K Robertson, NA Robinet, F Rocchi, A Roddy, S Rodriguez, C Rodruck, M Roever, C Rolland, L Rollins, JG Romano, R Romanov, G Romie, JH Rosinska, D Rowan, S Rudiger, A Ruggi, P Ryan, K Salemi, F Sammut, L de la Jordana, LS Sandberg, V Sanders, J Sannibale, V Santiago-Prieto, I Saracco, E Sassolas, B Sathyaprakash, BS Saulson, PR Savage, R Schilling, R Schnabel, R Schofield, RMS Schreiber, E Schuette, D Schulz, B Schutz, BF Schwinberg, P Scott, J Scott, SM Seifert, F Sellers, D Sengupta, AS Sentenac, D Sequino, V Sergeev, A Shaddock, D Shah, S Shahriar, MS Shaltev, M Shapiro, B Shawhan, P Shoemaker, DH Sidery, TL Siellez, K Siemens, X Sigg, D Simakov, D Singer, A Singer, L Sintes, AM Skelton, GR Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Smith, RJE Smith-Lefebvre, ND Soden, K Son, EJ Sorazu, B Souradeep, T Sperandio, L Staley, A Steinert, E Steinlechner, J Steinlechner, S Steplewski, S Stevens, D Stochino, A Stone, R Strain, KA Straniero, N Strigin, S Stroeer, AS Sturani, R Stuver, AL Summerscales, TZ Susmithan, S Sutton, PJ Swinkels, B Szeifert, G Tacca, M Talukder, D Tang, L Tanner, DB Tarabrin, SP Taylor, R ter Braack, APM Thirugnanasambandam, MP Thomas, M Thomas, P Thorne, KA Thorne, KS Thrane, E Tiwari, V Tokmakov, KV Tomlinson, C Toncelli, A Tonelli, M Torre, O Torres, CV Torrie, CI Travasso, F Traylor, G Tse, M Ugolini, D Unnikrishnan, CS Vahlbruch, H Vajente, G Vallisneri, M van den Brand, JFJ Van Den Broeck, C van der Putten, S van der Sluys, MV van Heijningen, J van Veggel, AA Vass, S Vasuth, M Vaulin, R Vecchio, A Vedovato, G Veitch, J Veitch, PJ Venkateswara, K Verkindt, D Verma, S Vetrano, F Vicere, A Vincent-Finley, R Vinet, JY Vitale, S 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TI Application of a Hough search for continuous gravitational waves on data from the fifth LIGO science run SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article DE gravitational waves; LIGO; neutron stars ID SPIN-DOWN LIMIT; PERIODIC SOURCES; EMISSION; PULSAR; RADIATION AB We report on an all-sky search for periodic gravitational waves in the frequency range 50-1000 Hz with the first derivative of frequency in the range -8.9 Chi 10(-10) Hz s(-1) to zero in two years of data collected during LIGO's fifth science run. Our results employ a Hough transform technique, introducing a chi(2) test and analysis of coincidences between the signal levels in years 1 and 2 of observations that offers a significant improvement in the product of strain sensitivity with compute cycles per data sample compared to previously published searches. Since our search yields no surviving candidates, we present results taking the form of frequency dependent, 95% confidence upper limits on the strain amplitude h(0). The most stringent upper limit from year 1 is 1.0 Chi 10(-24) in the 158.00-158.25 Hz band. In year 2, the most stringent upper limit is 8.9 Chi 10(-25) in the 146.50-146.75 Hz band. This improved detection pipeline, which is computationally efficient by at least two orders of magnitude better than our flagship Einstein@ Home search, will be important for 'quicklook' searches in the Advanced LIGO and Virgo detector era. C1 [Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Ajith, P.; Anderson, R. A.; Anderson, S. B.; Arai, K.; Araya, M. C.; Austin, L.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chakraborty, R.; Chalermsongsak, T.; Coyne, D. C.; Daudert, B.; Dergachev, V.; Driggers, J. C.; Ehrens, P.; Etzel, T.; Fotopoulos, N.; Gushwa, K. E.; Gustafson, E. K.; Hall, E.; Harms, J.; Heefner, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; James, E.; Kalmus, P.; Kells, W.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D.; Lewis, J. B.; Litvine, V.; Lloyd, D.; Mageswaran, M.; Mailand, K.; Maros, E.; Martynov, D.; Marx, J. N.; Mclntyre, G.; Meshkov, S.; Nash, T.; Ogin, G. H.; Osthelder, C.; Pedraza, M.; Phelps, M.; Poux, C.; Price, L. R.; Privitera, S.; Quintero, E.; Raymond, V.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Seifert, F.; Singer, A.; Singer, L.; Smith, M. R.; Smith-Lefebvre, N. D.; Taylor, R.; Thirugnanasambandam, M. P.; Thrane, E.; Torrie, C. I.; Vass, S.; Wallace, L.; Weinstein, A. J.; Whitcomb, S. E.; Williams, R.; Yamamoto, H.; Yeaton-Massey, D.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Abbott, T.; Bowers, J.; Corbitt, T. R.; DeRosa, R. T.; Effler, A.; Giaime, J. A.; Gonzalez, G.; Iafrate, J.; Johnson, W. W.; Kokeyama, K.; Kudla, S.; May, G.; Mullavey, A.; Walker, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Accadia, T.; Bebronne, M.; Buskulic, D.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Verkindt, D.; Yvert, M.] Univ Savoie, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules LAPP, F-74941 Annecy Le Vieux, France. [Acernese, F.; Barone, F.; Calloni, E.; De Rosa, R.; Di Fiore, L.; Garufi, F.; Milano, L.; Romano, R.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy. [Acernese, F.; Barone, F.; Romano, R.] Univ Salerno, I-84084 Salerno, Italy. [Adams, C.; Aston, S. M.; Betzwieser, J.; Birch, J.; Bridges, D. O.; Cowart, M.; Doravari, S.; Evans, T.; Feldbaum, D.; Forsi, E.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Guido, C.; Hanson, J.; Heintze, M.; Holt, K.; Huynh-Dinh, T.; Katzman, W.; Kinzel, D. L.; Le Roux, A.; Lormand, M.; Meyer, M. S.; Nolting, D.; O'Reilly, B.; Overmier, H.; Ramet, C.; Riesen, R.; Roddy, S.; Romie, J. H.; Sellers, D.; Stuver, A. L.; Thomas, M.; Thorne, K. A.; Traylor, G.; Welborn, T.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA. [Adams, T.; Edwards, M.; Fairhurst, S.; Liu, H.; Macdonald, E.; Macleod, D. M.; Nuttall, L. K.; Ohme, F.; Predoi, V.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales. [Affeldt, C.; Allen, B.; Aulbert, C.; Bauchrowitz, J.; Bergmann, G.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Dahl, K.; Dal Canton, T.; Damjanic, M.; Danzmann, K.; Denker, T.; Dent, T.; Di Palma, I.; Dooley, K. L.; Eberle, T.; Fehrmann, H.; Frede, M.; Fricke, T. T.; Goetz, E.; Gossler, S.; Grote, H.; Hanke, M.; Heurs, M.; Kawazoe, F.; Keitel, D.; Keppel, D. G.; Khalaidovski, A.; Koehlenbeck, S.; Kringel, V.; Krishnan, B.; Kuehn, G.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Manca, M.; Mazzolo, G.; Mehmet, M.; Mokler, F.; Mossavi, K.; Mow-Lowry, C. 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[Boer, M.; Brillet, A.; Cleva, F.; Coulon, J-P; Dereli, H.; Fournier, J-D; Heitmann, H.; Kefelian, F.; Man, N.; Martinelli, L.; Meacher, D.; Pichot, M.; Regimbau, T.; Siellez, K.; Vinet, J-Y; Wei, L-W] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice, France. [Bondu, F.] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France. [Bonnand, R.; Cagnoli, G.; Degallaix, J.; Flaminio, R.; Granata, M.; Michel, C.; Morgado, N.; Pinard, L.; Saracco, E.; Sassolas, B.; Straniero, N.] Univ Lyon, CNRS, IN2P3, Lab Mat Avances, F-69622 Lyon, France. [Bose, S.; Brannen, C. A.; Dayanga, T.; Ghosh, S.; Hall, B.; Poole, V.; Steplewski, S.] Washington State Univ, Pullman, WA 99164 USA. [Bosi, L.; Colombini, M.; Gammaitoni, L.; Marchesoni, F.; Neri, I.; Punturo, M.; Travasso, F.; Vocca, H.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Branchesi, M.; Guidi, G. 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[Williams, T.; Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA. [Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA. RP Aasi, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. EM alicia.sintes@uib.es RI Ward, Robert/I-8032-2014; Ferrante, Isidoro/F-1017-2012; Travasso, Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Cesarini, Elisabetta/C-4507-2017; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Martelli, Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Gehring, Tobias/A-8596-2016; Strain, Kenneth/D-5236-2011; Miao, Haixing/O-1300-2013; Howell, Eric/H-5072-2014; Heidmann, Antoine/G-4295-2016; Ott, Christian/G-2651-2011; Marchesoni, Fabio/A-1920-2008; Zhu, Xingjiang/E-1501-2016; Frasconi, Franco/K-1068-2016; Groot, Paul/K-4391-2016; Pinto, Innocenzo/L-3520-2016; Leonardi, Matteo/G-9694-2015; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Ottaway, David/J-5908-2015; Garufi, Fabio/K-3263-2015; Deleglise, Samuel/B-1599-2015; 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Science and Technology Facilities Council of the United Kingdom; Max-Planck-Society; State of Niedersachsen/Germany; Italian Istituto Nazionale di Fisica Nucleare; French Centre National de la Recherche Scientifique; Australian Research Council; International Science Linkages program of the Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Netherlands Organisation for Scientific Research; Polish Ministry of Science and Higher Education; Foundation for Polish Science; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Alfred P Sloan Foundation FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P Sloan Foundation. This document has been assigned LIGO Laboratory document number LIGO- P1300071. NR 41 TC 9 Z9 9 U1 9 U2 50 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD APR 21 PY 2014 VL 31 IS 8 AR 085014 DI 10.1088/0264-9381/31/8/085014 PG 35 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AF0QK UT WOS:000334418900015 ER PT J AU Aasi, J Abadie, J Abbott, BP Abbott, R Abbott, T Abernathy, MR Accadia, T Acernese, F Adams, C Adams, T Adhikari, RX Affeldt, C Agathos, M Aggarwal, N Aguiar, OD Ajith, P Allen, B Allocca, A Ceron, EA Amariutei, D Anderson, RA Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, C Areeda, J Ast, S Aston, SM Astone, P Aufmuth, P Aulbert, C Austin, L Aylott, BE Babak, S Baker, PT Ballardin, G Ballmer, SW Barayoga, JC Barker, D Barnum, SH Barone, F Barr, B Barsotti, L Barsuglia, M Barton, MA Bartos, I Bassiri, R Basti, A Batch, J Bauchrowitz, J Bauer, TS Bebronne, M Behnke, B Bejger, M Beker, MG Bell, AS Bell, C Belopolski, I Bergmann, G Berliner, JM Bersanetti, D Bertolini, A Bessis, D Betzwieser, J Beyersdorf, PT Bhadbhade, T Bilenko, IA Billingsley, G Birch, J Bitossi, M Bizouard, MA Black, E Blackburn, JK Blackburn, L Blair, D Blom, M Bock, O Bodiya, TP Boer, M Bogan, C Bond, C Bondu, F Bonelli, L Bonnand, R Bork, R Born, M Boschi, V Bose, S Bosi, L Bowers, J Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brannen, CA Brau, JE Breyer, J Briant, T Bridges, DO Brillet, A Brinkmann, M Brisson, V Britzger, M Brooks, AF Brown, DA Brown, DD Brueckner, F Bulik, T Bulten, HJ Buonanno, A Buskulic, D Buy, C Byer, RL Cadonati, L Cagnoli, G Bustillo, JC Calloni, E Camp, JB Campsie, P Cannon, KC Canuel, B Cao, J Capano, CD Carbognani, F Carbone, L Caride, S Castiglia, A Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Cella, G Cepeda, C Cesarini, E Chakraborty, R Chalermsongsak, T Chao, S Charlton, P Chassande-Mottin, E Chen, X Chen, Y Chincarini, A Chiummo, A Cho, HS Chow, J Christensen, N Chu, Q Chua, SSY Chung, S Ciani, G Clara, F Clark, DE Clark, JA Cleva, F Coccia, E Cohadon, PF Colla, A Colombini, M Jr, MC Conte, A Conte, R Cook, D Corbitt, TR Cordier, M Cornish, N Corsi, A Costa, CA Coughlin, MW Coulon, JP Countryman, S Couvares, P Coward, DM Cowart, M Coyne, DC Craig, K Creighton, JDE Creighton, TD Crowder, SG Cumming, A Cunningham, L Cuoco, E Dahl, K Dal Canton, T Damjanic, M Danilishin, SL D'Antonio, S Danzmann, K Dattilo, V Daudert, B Daveloza, H Davier, M Davies, GS Daw, EJ Day, R Dayanga, T De Rosa, R Debreczeni, G Degallaix, J Del Pozzo, W Deleeuw, E Deleglise, S Denker, T Dent, T Dereli, H Dergachev, V DeRosa, R DeSalvo, R Dhurandhar, S Di Fiore, L Di Lieto, A Di Palma, I Di Virgilio, A Diaz, M Dietz, A Dmitry, K Donovan, F Dooley, KL Doravari, S Drago, M Drever, RWP Driggers, JC Du, Z Dumas, JC Dwyer, S Eberle, T Edwards, M Effler, A Ehrens, P Eichholz, J Eikenberry, SS Endroczi, G Essick, R Etzel, T Evans, K Evans, M Evans, T Factourovich, M Fafone, V Fairhurst, S Fang, Q Farinon, S Farr, B Farr, W Favata, M Fazi, D Fehrmann, H Feldbaum, D Ferrante, I Ferrini, F Fidecaro, F Finn, LS Fiori, I Fisher, R Flaminio, R Foley, E Foley, S Forsi, E Fotopoulos, N Fournier, JD Franco, S Frasca, S Frasconi, F Frede, M Frei, M Frei, Z Freise, A Frey, R Fricke, TT Fritschel, P Frolov, VV Fujimoto, MK Fulda, P Fyffe, M Gair, J Gammaitoni, L Garcia, J Garufi, F Gehrels, N Gemme, G Genin, E Gennai, A Gergely, L Ghosh, S Giaime, JA Giampanis, S Giardina, KD Giazotto, A Gil-Casanova, S Gill, C Gleason, J Goetz, E Goetz, R Gondan, L Gonzalez, G Gordon, N Gorodetsky, ML Gossan, S Gossler, S Gouaty, R Graef, C Graff, PB Granata, M Grant, A Gras, S Gray, C Greenhalgh, RJS Gretarsson, AM Griffo, C Groot, P Grote, H Grover, K Grunewald, S Guidi, GM Guido, C Gushwa, KE Gustafson, EK Gustafson, R Hall, B Hall, E Hammer, D Hammond, G Hanke, M Hanks, J Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Hartman, MT Haughian, K Hayama, K Heefner, J Heidmann, A Heintze, M Heitmann, H Hello, P Hemming, G Hendry, M Heng, IS Heptonstall, AW Heurs, M Hild, S Hoak, D Hodge, KA Holt, K Holtrop, M Hong, T Hooper, S Horrom, T Hosken, DJ Hough, J Howell, EJ Hu, Y Hua, Z Huang, V Huerta, EA Hughey, B Husa, S Huttner, SH Huynh, M Huynh-Dinh, T Iafrate, J Ingram, DR Inta, R Isogai, T Ivanov, A Iyer, BR Izumi, K Jacobson, M James, E Jang, H Jang, YJ Jaranowski, P Jimenez-Forteza, F Johnson, WW Jones, D Jones, DI Jones, R Jonker, RJG Ju, L Haris, K Kalmus, P Kalogera, V Kandhasamy, S Kang, G Kanner, JB Kasprzack, M Kasturi, R Katsavounidis, E Katzman, W Kaufer, H Kaufman, K Kawabe, K Kawamura, S Kawazoe, F Kefelian, F Keitel, D Kelley, DB Kells, W Keppel, DG Khalaidovski, A Khalili, FY Khazanov, EA Kim, BK Kim, C Kim, K Kim, N Kim, W Kim, YM King, EJ King, PJ Kinzel, DL Kissel, JS Klimenko, S Kline, J Koehlenbeck, S Kokeyama, K Kondrashov, V Koranda, S Korth, WZ Kowalska, I Kozak, D Kremin, A Kringel, V Krishnan, B Krolak, A Kucharczyk, C Kudla, S Kuehn, G Kumar, A Kumar, P Kumar, R Kurdyumov, R Kwee, P Landry, M Lantz, B Larson, S Lasky, PD Lawrie, C Lazzarini, A Le Roux, 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S Messenger, C Meyer, MS Miao, H Michel, C Mikhailov, EE Milano, L Miller, J Minenkov, Y Mingarelli, CMF Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Moe, B Mohan, M Mohapatra, SRP Mokler, F Moraru, D Moreno, G Morgado, N Mori, T Morriss, SR Mossavi, K Mours, B Mow-Lowry, CM Mueller, CL Mueller, G Mukherjee, S Mullavey, A Munch, J Murphy, D Murray, PG Mytidis, A Nagy, MF Kumar, DN Nardecchia, I Nash, T Naticchioni, L Nayak, R Necula, V Nelemans, G Neri, I Neri, M Newton, G Nguyen, T Nishida, E Nishizawa, A Nitz, A Nocera, F Nolting, D Normandin, ME Nuttall, LK Ochsner, E O'Dell, J Oelker, E Ogin, GH Oh, JJ Oh, SH Ohme, F Oppermann, P O'Reilly, B Larcher, WO O'Shaughnessy, R Osthelder, C Ottaway, DJ Ottens, RS Ou, J Overmier, H Owen, BJ Padilla, C Pai, A Palomba, C Pan, Y Pankow, C Paoletti, F Paoletti, R Papa, MA Paris, H Pasqualetti, A Passaquieti, R Passuello, D Pedraza, M Peiris, P Penn, S Perreca, A Phelps, M Pichot, M Pickenpack, M Piergiovanni, F Pierro, V Pinard, L 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Skelton, G. R. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Smith, R. J. E. Smith-Lefebvre, N. D. Soden, K. Son, E. J. Sorazu, B. Souradeep, T. Sperandio, L. Staley, A. Steinert, E. Steinlechner, J. Steinlechner, S. Steplewski, S. Stevens, D. Stochino, A. Stone, R. Strain, K. A. Straniero, N. Strigin, S. Stroeer, A. S. Sturani, R. Stuver, A. L. Summerscales, T. Z. Susmithan, S. Sutton, P. J. Swinkels, B. Szeifert, G. Tacca, M. Talukder, D. Tang, L. Tanner, D. B. Tarabrin, S. P. Taylor, R. Ter Braack, A. P. M. Thirugnanasambandam, M. P. Thomas, M. Thomas, P. Thorne, K. A. Thorne, K. S. Thrane, E. Tiwari, V. Tokmakov, K. V. Tomlinson, C. Toncelli, A. Tonelli, M. Torre, O. Torres, C. V. Torrie, C. I. Travasso, F. Traylor, G. Tse, M. Ugolini, D. Unnikrishnan, C. S. Vahlbruch, H. Vajente, G. Vallisneri, M. Van den Brand, J. F. J. Van den Broeck, C. Van der Putten, S. Van der Sluys, M. V. Van Heijningen, J. Van Veggel, A. A. Vass, S. Vasuth, M. Vaulin, R. Vecchio, A. Vedovato, G. Veitch, J. Veitch, P. J. Venkateswara, K. Verkindt, D. Verma, S. Vetrano, F. Vicere, A. Vincent-Finley, R. Vinet, J. -Y. Vitale, S. Vlcek, B. Vo, T. Vocca, H. Vorvick, C. Vousden, W. D. Vrinceanu, D. Vyachanin, S. P. Wade, A. Wade, L. Wade, M. Waldman, S. J. Walker, M. Wallace, L. Wan, Y. Wang, J. Wang, M. Wang, X. Wanner, A. Ward, R. L. Was, M. Weaver, B. Wei, L. -W. Weinert, M. Weinstein, A. J. Weiss, R. Welborn, T. Wen, L. Wessels, P. West, M. Westphal, T. Wette, K. Whelan, J. T. Whitcomb, S. E. White, D. J. Whiting, B. F. Wibowo, S. Wiesner, K. Wilkinson, C. Williams, L. Williams, R. Williams, T. Willis, J. L. Willke, B. Wimmer, M. Winkelmann, L. Winkler, W. Wipf, C. C. Wittel, H. Woan, G. Worden, J. Yablon, J. Yakushin, I. Yamamoto, H. Yancey, C. C. Yang, H. Yeaton-Massey, D. Yoshida, S. Yum, H. Yvert, M. Zadrozny, A. Zanolin, M. Zendri, J. -P. Zhang, F. Zhang, L. Zhao, C. Zhu, H. Zhu, X. J. Zotov, N. Zucker, M. E. Zweizig, J. Collaboration, Ligo Sci Collaboration, Virgo Buchner, S. Cognard, I. Corongiu, A. D'Amico, N. Espinoza, C. M. Freire, P. C. C. Gotthelf, E. V. Guillemot, L. Hessels, J. W. T. Hobbs, G. B. Kramer, M. Lyne, A. G. Marshall, F. E. Possenti, A. Ransom, S. M. Ray, P. S. Roy, J. Stappers, B. W. TI GRAVITATIONAL WAVES FROM KNOWN PULSARS: RESULTS FROM THE INITIAL DETECTOR ERA SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational waves; pulsars: general ID GAMMA-RAY PULSARS; SPIN-DOWN LIMIT; NEUTRON-STARS; CRAB PULSAR; GLOBULAR-CLUSTERS; PSR J1734-3333; PROPER MOTION; WIND TORI; EMISSION; DISCOVERY AB We present the results of searches for gravitational waves from a large selection of pulsars using data from the most recent science runs (S6, VSR2 and VSR4) of the initial generation of interferometric gravitational wave detectors LIGO (Laser Interferometric Gravitational-wave Observatory) and Virgo. We do not see evidence for gravitational wave emission from any of the targeted sources but produce upper limits on the emission amplitude. We highlight the results from seven young pulsars with large spin-down luminosities. We reach within a factor of five of the canonical spin-down limit for all seven of these, whilst for the Crab and Vela pulsars we further surpass their spin-down limits. We present new or updated limits for 172 other pulsars (including both young and millisecond pulsars). Now that the detectors are undergoing major upgrades, and, for completeness, we bring together all of the most up-to-date results from all pulsars searched for during the operations of the first-generation LIGO, Virgo and GEO600 detectors. This gives a total of 195 pulsars including the most recent results described in this paper. C1 [Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Ajith, P.; Anderson, R. A.; Anderson, S. B.; Arai, K.; Araya, M. C.; Austin, L.; Barayoga, J. C.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chakraborty, R.; Chalermsongsak, T.; Coyne, D. C.; Daudert, B.; Dergachev, V.; Driggers, J. C.; Etzel, T.; Fotopoulos, N.; Gushwa, K. E.; Gustafson, E. K.; Hall, E.; Harms, J.; Heefner, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; James, E.; Kalmus, P.; Kells, W.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D.; Lazzarini, A.; Lewis, J. B.; Litvine, V.; Lloyd, D.; Mageswaran, M.; Mailand, K.; Maros, E.; Martynov, D.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Nash, T.; Ogin, G. H.; Osthelder, C.; Pedraza, M.; Phelps, M.; Poux, C.; Price, L. R.; Privitera, S.; Quintero, E.; Raymond, V.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Seifert, F.; Singer, A.; Singer, L.; Smith, M. R.; Smith-Lefebvre, N. D.; Taylor, R.; Thirugnanasambandam, M. P.; Thrane, E.; Torrie, C. I.; Vass, S.; Wallace, L.; Weinstein, A. J.; Whitcomb, S. 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RI Ward, Robert/I-8032-2014; Cella, Giancarlo/A-9946-2012; Cesarini, Elisabetta/C-4507-2017; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Strain, Kenneth/D-5236-2011; Miao, Haixing/O-1300-2013; Howell, Eric/H-5072-2014; Heidmann, Antoine/G-4295-2016; Marchesoni, Fabio/A-1920-2008; Zhu, Xingjiang/E-1501-2016; Frasconi, Franco/K-1068-2016; Groot, Paul/K-4391-2016; Pinto, Innocenzo/L-3520-2016; Ferrante, Isidoro/F-1017-2012; Travasso, Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Ottaway, David/J-5908-2015; Garufi, Fabio/K-3263-2015; Deleglise, Samuel/B-1599-2015; Neri, Igor/F-1482-2010; Shaddock, Daniel/A-7534-2011; Vicere, Andrea/J-1742-2012; Rocchi, Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Gehring, Tobias/A-8596-2016; Iyer, Bala R./E-2894-2012; Canuel, Benjamin/C-7459-2014; Prokhorov, Leonid/I-2953-2012; Lee, Chang-Hwan/B-3096-2015; Khalili, Farit/D-8113-2012; Gorodetsky, Michael/C-5938-2008; McClelland, David/E-6765-2010; M, Manjunath/N-4000-2014; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Strigin, Sergey/I-8337-2012; Leonardi, Matteo/G-9694-2015; Sigg, Daniel/I-4308-2015; Salemi, Francesco/F-6988-2014; Gammaitoni, Luca/B-5375-2009; Bell, Angus/E-7312-2011; Nelemans, Gijs/D-3177-2012; Kumar, Prem/B-6691-2009; prodi, giovanni/B-4398-2010; Gemme, Gianluca/C-7233-2008; Costa, Cesar/G-7588-2012; Huerta, Eliu/J-5426-2014; Losurdo, Giovanni/K-1241-2014; Steinlechner, Sebastian/D-5781-2013; Hild, Stefan/A-3864-2010; Danilishin, Stefan/K-7262-2012 OI Boschi, Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418; Husa, Sascha/0000-0002-0445-1971; Papa, M.Alessandra/0000-0002-1007-5298; Vocca, Helios/0000-0002-1200-3917; Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Guidi, Gianluca/0000-0002-3061-9870; Pierro, Vincenzo/0000-0002-6020-5521; Denker, Timo/0000-0003-1259-5315; Drago, Marco/0000-0002-3738-2431; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Whelan, John/0000-0001-5710-6576; Vedovato, Gabriele/0000-0001-7226-1320; Fairhurst, Stephen/0000-0001-8480-1961; Pitkin, Matthew/0000-0003-4548-526X; Veitch, John/0000-0002-6508-0713; Ray, Paul/0000-0002-5297-5278; Davies, Gareth/0000-0002-4289-3439; Principe, Maria/0000-0002-6327-0628; Ransom, Scott/0000-0001-5799-9714; Vitale, Salvatore/0000-0003-2700-0767; Kanner, Jonah/0000-0001-8115-0577; Freise, Andreas/0000-0001-6586-9901; Nitz, Alexander/0000-0002-1850-4587; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Murphy, David/0000-0002-8538-815X; Bondu, Francois/0000-0001-6487-5197; Del Pozzo, Walter/0000-0003-3978-2030; O'Shaughnessy, Richard/0000-0001-5832-8517; Allen, Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Coccia, Eugenio/0000-0002-6669-5787; Vetrano, Flavio/0000-0002-7523-4296; Naticchioni, Luca/0000-0003-2918-0730; calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Sorazu, Borja/0000-0002-6178-3198; Cella, Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Aulbert, Carsten/0000-0002-1481-8319; Corongiu, Alessandro/0000-0002-5924-3141; Swinkels, Bas/0000-0002-3066-3601; Strain, Kenneth/0000-0002-2066-5355; Miao, Haixing/0000-0003-4101-9958; Howell, Eric/0000-0001-7891-2817; Heidmann, Antoine/0000-0002-0784-5175; Marchesoni, Fabio/0000-0001-9240-6793; Zhu, Xingjiang/0000-0001-7049-6468; Frasconi, Franco/0000-0003-4204-6587; Groot, Paul/0000-0002-4488-726X; Ferrante, Isidoro/0000-0002-0083-7228; Travasso, Flavio/0000-0002-4653-6156; Punturo, Michele/0000-0001-8722-4485; Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168; Deleglise, Samuel/0000-0002-8680-5170; Neri, Igor/0000-0002-9047-9822; Shaddock, Daniel/0000-0002-6885-3494; Vicere, Andrea/0000-0003-0624-6231; Rocchi, Alessio/0000-0002-1382-9016; Martelli, Filippo/0000-0003-3761-8616; Gehring, Tobias/0000-0002-4311-2593; Iyer, Bala R./0000-0002-4141-5179; Lee, Chang-Hwan/0000-0003-3221-1171; Gorodetsky, Michael/0000-0002-5159-2742; McClelland, David/0000-0001-6210-5842; M, Manjunath/0000-0001-8710-0730; Vecchio, Alberto/0000-0002-6254-1617; Sigg, Daniel/0000-0003-4606-6526; Gammaitoni, Luca/0000-0002-4972-7062; Bell, Angus/0000-0003-1523-0821; Nelemans, Gijs/0000-0002-0752-2974; prodi, giovanni/0000-0001-5256-915X; Gemme, Gianluca/0000-0002-1127-7406; Losurdo, Giovanni/0000-0003-0452-746X; Steinlechner, Sebastian/0000-0003-4710-8548; Danilishin, Stefan/0000-0001-7758-7493 FU United States National Science Foundation; Science and Technology Facilities Council of the United Kingdom; Max-Planck-Society; State of Niedersachsen/Germany; Australian Research Council; International Science Linkages program of the Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Netherlands Organisation for Scientific Research; Polish Ministry of Science and Higher Education; FOCUS Programme of Foundation for Polish Science; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; OTKA of Hungary; Lyon Institute of Origins (LIO); National Research Foundation of Korea; Industry Canada; Province of Ontario through the Ministry of Economic Development and Innovation; National Science and Engineering Research Council Canada; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P. Sloan Foundation FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the National Aeronautics and Space Administration, OTKA of Hungary, the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the National Science and Engineering Research Council Canada, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. The Nancay Radio Observatory is operated by the Paris Observatory, associated with the French Centre National de la Recherche Scientifique. LIGO Document No. LIGO-P1200104. NR 90 TC 46 Z9 46 U1 6 U2 71 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 APR 20 PY 2014 VL 785 IS 2 AR 119 DI 10.1088/0004-637X/785/2/119 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800038 ER PT J AU Bennett, DP Batista, V Bond, IA Bennett, CS Suzuki, D Beaulieu, JP Udalski, A Donatowicz, J Bozza, V Abe, F Botzler, CS Freeman, M Fukunaga, D Fukui, A Itow, Y Koshimoto, N Ling, CH Masuda, K Matsubara, Y Muraki, Y Namba, S Ohnishi, K Rattenbury, NJ Saito, T Sullivan, DJ Sumi, T Sweatman, WL Tristram, PJ Tsurumi, N Wada, K Yock, PCM Albrow, MD Bachelet, E Brillant, S Caldwell, JAR Cassan, A Cole, AA Corrales, E Coutures, C Dieters, S Prester, DD Fouque, P Greenhill, J Horne, K Koo, JR Kubas, D Marquette, JB Martin, R Menzies, JW Sahu, KC Wambsganss, J Williams, A Zub, M Choi, JY DePoy, DL Dong, SB Gaudi, BS Gould, A Han, C Henderson, CB McGregor, D Lee, CU Pogge, RW Shin, IG Yee, JC Szymanski, MK Skowron, J Poleski, R Kozllowski, S Wyrzykowski, L Kubiak, M Pietrukowicz, P Pietrzynski, G Soszynski, I Ulaczyk, K Tsapras, Y Street, RA Dominik, M Bramich, DM Browne, P Hundertmark, M Kains, N Snodgrass, C Steele, IA Dekany, I Gonzalez, OA Heyrovsky, D Kandori, R Kerins, E Lucas, PW Minniti, D Nagayama, T Rejkuba, M Robin, AC Saito, R AF Bennett, D. P. Batista, V. Bond, I. A. Bennett, C. S. Suzuki, D. Beaulieu, J. -P. Udalski, A. Donatowicz, J. Bozza, V. Abe, F. Botzler, C. S. Freeman, M. Fukunaga, D. Fukui, A. Itow, Y. Koshimoto, N. Ling, C. H. Masuda, K. Matsubara, Y. Muraki, Y. Namba, S. Ohnishi, K. Rattenbury, N. J. Saito, To. Sullivan, D. J. Sumi, T. Sweatman, W. L. Tristram, P. J. Tsurumi, N. Wada, K. Yock, P. C. M. Albrow, M. D. Bachelet, E. Brillant, S. Caldwell, J. A. R. Cassan, A. Cole, A. A. Corrales, E. Coutures, C. Dieters, S. Prester, D. Dominis Fouque, P. Greenhill, J. Horne, K. Koo, J. -R. Kubas, D. Marquette, J. -B. Martin, R. Menzies, J. W. Sahu, K. C. Wambsganss, J. Williams, A. Zub, M. Choi, J. Y. DePoy, D. L. Dong, Subo Gaudi, B. S. Gould, A. Han, C. Henderson, C. B. McGregor, D. Lee, C. -U. Pogge, R. W. Shin, I. -G. Yee, J. C. Szymanski, M. K. Skowron, J. Poleski, R. Kozllowski, S. Wyrzykowski, L. Kubiak, M. Pietrukowicz, P. Pietrzynski, G. Soszynski, I. Ulaczyk, K. Tsapras, Y. Street, R. A. Dominik, M. Bramich, D. M. Browne, P. Hundertmark, M. Kains, N. Snodgrass, C. Steele, I. A. Dekany, I. Gonzalez, O. A. Heyrovsky, D. Kandori, R. Kerins, E. Lucas, P. W. Minniti, D. Nagayama, T. Rejkuba, M. Robin, A. C. Saito, R. CA MOA Collaboration PLANET Collaboration FUN Collaboration OGLE Collaboration RoboNet Collaboration TI MOA-2011-BLG-262Lb: A SUB-EARTH-MASS MOON ORBITING A GAS GIANT PRIMARY OR A HIGH VELOCITY PLANETARY SYSTEM IN THE GALACTIC BULGE SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing: micro; planetary systems ID GRAVITATIONAL LENSING EXPERIMENT; FREE-FLOATING PLANET; MAGNIFICATION MICROLENSING EVENTS; SNOW LINE; EXTRASOLAR PLANETS; MAIN-SEQUENCE; STELLAR-MASS; BROWN DWARF; OGLE-III; JUPITER/SATURN ANALOG AB We present the first microlensing candidate for a free-floating exoplanet-exomoon system, MOA-2011-BLG-262, with a primary lens mass of M-host similar to 4 Jupitermasses hosting a sub-Earthmassmoon. The argument for an exomoon hinges on the system being relatively close to the Sun. The data constrain the product M-L pi(rel) where ML is the lens system mass and prel is the lens-source relative parallax. If the lens system is nearby (large pi(rel)), then ML is small (a few Jupiter masses) and the companion is a sub-Earth-mass exomoon. The best-fit solution has a large lens-source relative proper motion, mu(rel) = 19.6 +/- 1.6 mas yr(-1), which would rule out a distant lens system unless the source star has an unusually high proper motion. However, data from the OGLE collaboration nearly rule out a high source proper motion, so the exoplanet+exomoon model is the favored interpretation for the best fit model. However, there is an alternate solution that has a lower proper motion and fits the data almost as well. This solution is compatible with a distant (so stellar) host. A Bayesian analysis does not favor the exoplanet+exomoon interpretation, so Occam's razor favors a lens system in the bulge with host and companion masses of M-host = 0.12(-0.06)(+0.19) M-circle dot and m(comp) = 18(-10)(+28) M-circle plus, at a projected separation of a(perpendicular to) = 0.84(-0.14)(+0.25) AU. The existence of this degeneracy is an unlucky accident, so current microlensing experiments are in principle sensitive to exomoons. In some circumstances, it will be possible to definitively establish the mass of such lens systems through the microlensing parallax effect. Future experiments will be sensitive to less extreme exomoons. C1 [Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Batista, V.; Gaudi, B. S.; Gould, A.; McGregor, D.; Pogge, R. W.; Yee, J. C.; Poleski, R.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Batista, V.; Beaulieu, J. -P.; Cassan, A.; Corrales, E.; Coutures, C.; Kubas, D.; Marquette, J. -B.] UPMC, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Bond, I. A.; Ling, C. H.; Sweatman, W. L.] Massey Univ, Inst Nat & Math Sci, Auckland 0745, New Zealand. [Bennett, C. S.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Bennett, C. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Suzuki, D.; Koshimoto, N.; Namba, S.; Sumi, T.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Udalski, A.; Szymanski, M. K.; Skowron, J.; Poleski, R.; Kozllowski, S.; Wyrzykowski, L.; Kubiak, M.; Pietrukowicz, P.; Pietrzynski, G.; Soszynski, I.; Ulaczyk, K.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Donatowicz, J.] Vienna Univ Technol, A-1040 Vienna, Austria. [Bozza, V.] Univ Salerno, Dipartimento Fis, I-84084 Fisciano, Italy. [Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy. [Abe, F.; Fukunaga, D.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Tsurumi, N.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Botzler, C. S.; Freeman, M.; Rattenbury, N. J.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1001, New Zealand. [Fukui, A.] Natl Astron Observ, Okayama Astrophys Observ, Okayama 7190232, Japan. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Saito, To.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan. [Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Tristram, P. J.] Mt John Univ Observ, Lake Tekapo 8770, New Zealand. [Albrow, M. D.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand. [Bachelet, E.; Fouque, P.] Univ Toulouse, CNRS, IRAP, F-31400 Toulouse, France. [Brillant, S.; Gonzalez, O. A.; Rejkuba, M.] European So Observ, Santiago 19, Chile. [Caldwell, J. A. R.] McDonald Observ, Fort Davis, TX 79734 USA. [Cole, A. A.; Dieters, S.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Prester, D. Dominis] Univ Rijeka, Dept Phys, Rijeka 51000, Croatia. [Horne, K.; Dominik, M.; Browne, P.; Hundertmark, M.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Koo, J. -R.; Choi, J. Y.; Han, C.; Shin, I. -G.] Chungbuk Natl Univ, Dept Phys, Chongju 371763, South Korea. [Martin, R.; Williams, A.] Perth Observ, Perth, WA 6076, Australia. [Menzies, J. W.] S African Astron Observ, ZA-7925 Cape Town, South Africa. [Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Wambsganss, J.; Zub, M.] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. [DePoy, D. L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Dong, Subo] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Tsapras, Y.; Street, R. A.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Tsapras, Y.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England. [Bramich, D. M.; Kains, N.] ESO Headquarters, D-85748 Munich, Germany. [Bramich, D. M.] Qatar Fdn, Qatar Environm & Energy Res Inst, Doha, Qatar. [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England. [Dekany, I.; Minniti, D.; Saito, R.] Pontificia Univ Catolica Chile, Santiago 22, Chile. [Heyrovsky, D.] Charles Univ Prague, Inst Theoret Phys, Prague 18000, Czech Republic. [Kandori, R.; Nagayama, T.] Nagoya Univ, Grad Sch Sci, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Kerins, E.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Lucas, P. W.] Univ Hertfordshire, Hatfield AL10 9AB, Herts, England. [Robin, A. C.] Univ Franche Comte, UTINAM, CNRS, Observ Besancon Inst,UMR 6213, F-25010 Besancon, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bennett, DP (reprint author), Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. EM bennett@nd.edu RI Skowron, Jan/M-5186-2014; Heyrovsky, David/A-2031-2015; Williams, Andrew/K-2931-2013; Hundertmark, Markus/C-6190-2015; Saito, Roberto/L-6722-2016; OI Skowron, Jan/0000-0002-2335-1730; Heyrovsky, David/0000-0002-5198-5343; Williams, Andrew/0000-0001-9080-0105; Hundertmark, Markus/0000-0003-0961-5231; Dominik, Martin/0000-0002-3202-0343; Cole, Andrew/0000-0003-0303-3855; Rejkuba, Marina/0000-0002-6577-2787; Snodgrass, Colin/0000-0001-9328-2905 FU JSPS [JSPS23340044, JSPS24253004]; NASA Keck PI Data Award; W. M. Keck Foundation; NSF [AST 110347, AST-0807444]; NASA [NNX12AB99G]; Ralph E. and Doris M. Hansmann Membership at the IAS; California Institute of Technology (Caltech); NASA through the Sagan Fellowship Program; European Research Council under the European Community's Seventh Framework Programme (FP7)/ERC [246678]; Czech Science Foundation grant GACR [P209/10/1318]; NPRP grant from the Qatar National Research Fund (a member of the Qatar Foundation) [NPRP-09-476-1-78]; [NASA-NNX12AF54G]; [JPL-RSA 1453175]; [NSF AST-1211875]; [JSPS18253002]; [JSPS20340052] FX D.P.B. was supported by grants NASA-NNX12AF54G, JPL-RSA 1453175 and NSF AST-1211875. This MOA project is supported by the grants JSPS18253002 and JSPS20340052. T. S. acknowledges the financial support from the JSPS, JSPS23340044, JSPS24253004. This work was partially supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. B. S. G. and A. G. were supported by NSF grant AST 110347. B. S. G., A. G., R. P. G. were supported by NASA grant NNX12AB99G. S. D. was partly supported through a Ralph E. and Doris M. Hansmann Membership at the IAS and by NSF grant AST-0807444. Work by J.C.Y. was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 246678 to A. U. D. H. was supported by Czech Science Foundation grant GACR P209/10/1318. D. M. B., M. D., K. H., C. S., R. A. S., M. H. and Y.T. are supported by NPRP grant NPRP-09-476-1-78 from the Qatar National Research Fund (a member of the Qatar Foundation). NR 95 TC 28 Z9 28 U1 1 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2014 VL 785 IS 2 AR 155 DI 10.1088/0004-637X/785/2/155 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800074 ER PT J AU Kane, SR Howell, SB Horch, EP Feng, Y Hinkel, NR Ciardi, DR Everett, ME Howard, AW Wright, JT AF Kane, Stephen R. Howell, Steve B. Horch, Elliott P. Feng, Ying Hinkel, Natalie R. Ciardi, David R. Everett, Mark E. Howard, Andrew W. Wright, Jason T. TI LIMITS ON STELLAR COMPANIONS TO EXOPLANET HOST STARS WITH ECCENTRIC PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HD 4203, HD 168443, HD 1690, HD 137759); techniques: high angular resolution; techniques: radial velocities ID SOLAR-TYPE STARS; GIANT IOTA-DRACONIS; BINARY STARS; STATISTICAL PROPERTIES; REFRACTORY ELEMENTS; EXTRASOLAR PLANETS; HIPPARCOS STARS; MULTIPLICITY; ABUNDANCES; DISCOVERY AB Though there are now many hundreds of confirmed exoplanets known, the binarity of exoplanet host stars is not well understood. This is particularly true of host stars that harbor a giant planet in a highly eccentric orbit since these are more likely to have had a dramatic dynamical history that transferred angular momentum to the planet. Here we present observations of four exoplanet host stars that utilize the excellent resolving power of the Differential Speckle Survey Instrument on the Gemini North telescope. Two of the stars are giants and two are dwarfs. Each star is host to a giant planet with an orbital eccentricity >0.5 and whose radial velocity (RV) data contain a trend in the residuals to the Keplerian orbit fit. These observations rule out stellar companions 4-8 mag fainter than the host star at passbands of 692 nm and 880 nm. The resolution and field of view of the instrument result in exclusion radii of 0.'' 05-1.'' 4, which excludes stellar companions within several AU of the host star in most cases. We further provide new RVs for the HD 4203 system that confirm that the linear trend previously observed in the residuals is due to an additional planet. These results place dynamical constraints on the source of the planet's eccentricities, place constraints on additional planetary companions, and inform the known distribution of multiplicity amongst exoplanet host stars. C1 [Kane, Stephen R.; Hinkel, Natalie R.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Horch, Elliott P.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Feng, Ying; Wright, Jason T.] Penn State Univ, Dept Phys & Astron, University Pk, PA 16802 USA. [Feng, Ying; Wright, Jason T.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Kane, SR (reprint author), San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA. EM skane@sfsu.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Wright, Jason/0000-0001-6160-5888; Ciardi, David/0000-0002-5741-3047 FU National Aeronautics and Space Administration; National Science Foundation [AST-1109662] FX This work is 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). This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. This research has also made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The authors acknowledge financial support from the National Science Foundation through grant AST-1109662. NR 52 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2014 VL 785 IS 2 AR 93 DI 10.1088/0004-637X/785/2/93 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800012 ER PT J AU Kataria, T Showman, AP Fortney, JJ Marley, MS Freedman, RS AF Kataria, T. Showman, A. P. Fortney, J. J. Marley, M. S. Freedman, R. S. TI THE ATMOSPHERIC CIRCULATION OF THE SUPER EARTH GJ 1214b: DEPENDENCE ON COMPOSITION AND METALLICITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; methods: numerical; planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: individual (GJ 1214b) ID HOT JUPITERS; TRANSMISSION SPECTRUM; HD 209458B; EXOPLANET; MODEL; SPECTROSCOPY; DYNAMICS; NEPTUNE; GJ1214B; CLOUDS AB We present three-dimensional atmospheric circulation models of GJ 1214b, a 2.7 Earth-radius, 6.5 Earth-mass super Earth detected by the MEarth survey. Here we explore the planet's circulation as a function of atmospheric metallicity and atmospheric composition, modeling atmospheres with a low mean molecular weight (MMW; i.e., H-2-dominated) and a high MMW (i.e., water-and CO2-dominated). We find that atmospheres with a low MMW have strong day-night temperature variations at pressures above the infrared photosphere that lead to equatorial superrotation. For these atmospheres, the enhancement of atmospheric opacities with increasing metallicity lead to shallower atmospheric heating, larger day-night temperature variations, and hence stronger superrotation. In comparison, atmospheres with a high MMW have larger day-night and equator-to-pole temperature variations than low MMW atmospheres, but differences in opacity structure and energy budget lead to differences in jet structure. The circulation of a water-dominated atmosphere is dominated by equatorial superrotation, while the circulation of a CO2-dominated atmosphere is instead dominated by high-latitude jets. By comparing emergent flux spectra and light curves for 50x solar and water-dominated compositions, we show that observations in emission can break the degeneracy in determining the atmospheric composition of GJ 1214b. The variation in opacity with wavelength for the water-dominated atmosphere leads to large phase variations within water bands and small phase variations outside of water bands. The 50x solar atmosphere, however, yields small variations within water bands and large phase variations at other characteristic wavelengths. These observations would be much less sensitive to clouds, condensates, and hazes than transit observations. C1 [Kataria, T.; Showman, A. P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Kataria, T.; Showman, A. P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Fortney, J. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Marley, M. S.; Freedman, R. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Freedman, R. S.] SETI Inst, Mountain View, CA 94043 USA. RP Kataria, T (reprint author), Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. EM tkataria@lpl.arizona.edu RI Marley, Mark/I-4704-2013; OI Fortney, Jonathan/0000-0002-9843-4354; Marley, Mark/0000-0002-5251-2943 FU Origins grant [NNX12AI79G]; Harriet P. Jenkins Pre-Doctoral Fellowship Program (JPFP); NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center FX This work was supported by Origins grant NNX12AI79G to A.P.S. T.K. also acknowledges support from the Harriet P. Jenkins Pre-Doctoral Fellowship Program (JPFP). Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. We thank Roxana Lupu for comments and for providing opacity tables for CO2-CO2 pressure-induced absorption. We also thank Daniel Apai, Nikole Lewis, and Robert Zellem for insightful discussions. Last, we thank the anonymous referee for helpful comments and suggestions. NR 41 TC 17 Z9 17 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 APR 20 PY 2014 VL 785 IS 2 AR 92 DI 10.1088/0004-637X/785/2/92 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800011 ER PT J AU Lau, RM Herter, TL Morris, MR Adams, JD AF Lau, R. M. Herter, T. L. Morris, M. R. Adams, J. D. TI NATURE VERSUS NURTURE: LUMINOUS BLUE VARIABLE NEBULAE IN AND NEAR MASSIVE STELLAR CLUSTERS AT THE GALACTIC CENTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; Hii regions; Infrared: ISM; stars: evolution ID PASCHEN-ALPHA SURVEY; WOLF-RAYET STARS; QUINTUPLET CLUSTER; TEMPERATURE-FLUCTUATIONS; OPTICAL-PROPERTIES; MAGNETIC-FIELD; SMALL GRAINS; DUST; PISTOL; SPECTROSCOPY AB Three luminous blue variables (LBVs) are located in and near the Quintuplet Cluster at the Galactic center: the Pistol Star, G0.120-0.048, and qF362. We present imaging at 19, 25, 31, and 37 mu m of the region containing these three LBVs, obtained with SOFIA using FORCAST. We argue that Pistol and G0.120-0.048 are identical " twins" that exhibit contrasting nebulae due to the external influence of their different environments. Our images reveal the asymmetric, compressed shell of hot dust surrounding the Pistol Star and provide the first detection of the thermal emission from the symmetric, hot dust envelope surrounding G0.120-0.048. However, no detection of hot dust associated with qF362 is made. Dust and gas composing the Pistol nebula are primarily heated and ionized by the nearby Quintuplet Cluster stars. The northern region of the Pistol nebula is decelerated due to the interactionwith the high-velocity (2000 km s(-1)) winds from adjacent Wolf-Rayet Carbon (WC) stars. From fits to the spectral energy distribution (SED) of the Pistol nebula with the DustEM code we determine that the Pistol nebula is composed of a distribution of very small, transiently heated grains (10 to similar to 35 angstrom) having a total dust mass of 0.03M(circle dot), and that it exhibits a gradient of decreasing grain size from south to north due to differential sputtering by the winds from the WC stars. The total IR luminosity of the Pistol nebula is 5.2 x 10 (5) L-circle dot. Dust in the G0.120-0.048 nebula is primarily heated by the central star; however, the nebular gas is ionized externally by the Arches Cluster. Unlike the Pistol nebula, the G0.120-0.048 nebula is freely expanding into the surrounding medium. A grain size distribution identical to that of the non-sputtered region of the Pistol nebula satisfies the constraints placed on the G0.120-0.048 nebula from DustEM model fits to its SED and implies a total dust mass of 0.021M(circle dot). The total IR luminosity of the G0.120-0.048 nebula is similar to 10(5) L-circle dot. From Paschen-alpha and 6 cm observations we determine a total gas mass of 9.3M(circle dot) and 6.2M(circle dot) for the Pistol and G0.120-0.048 nebulae, respectively. Given the independent dust and gas mass estimates we find that the Pistol and G0.120-0.048 nebulae exhibit similar gas-to-dust mass ratios of 310+ 77 -52 and 293+ 73 -101, respectively. Both nebulae share identical size scales (similar to 0.7 pc) which suggests that they have similar dynamical timescales of similar to 10(4) yr, assuming a shell expansion velocity of vexp = 60 km s(-1). C1 [Lau, R. M.; Herter, T. L.; Adams, J. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Morris, M. R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Adams, J. D.] NASA, Ames Res Ctr, Univ Space Res Assoc, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. RP Lau, RM (reprint author), Cornell Univ, Dept Astron, 202 Space Sci Bldg, Ithaca, NY 14853 USA. FU NASA [NAS2-97001, 8500-98-014]; Deutsches SOFIA Institut (DSI) under DLR [50 OK 0901]; USRA FX We would like to thank the rest of the FORCAST team, George Gull, Justin Schoenwald, Chuck Henderson, and Jason Wang, the USRA Science and Mission Ops teams, and the entire SOFIA staff. This work is based on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA science mission operations are conducted jointly by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901. Financial support for FORCAST was provided by NASA through award 8500-98-014 issued by USRA. NR 38 TC 0 Z9 0 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 APR 20 PY 2014 VL 785 IS 2 AR 120 DI 10.1088/0004-637X/785/2/120 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800039 ER PT J AU Lis, DC Schilke, P Bergin, EA Gerin, M Black, JH Comito, C De Luca, M Godard, B Higgins, R Le Petit, F Pearson, JC Pellegrini, EW Phillips, TG Yu, S AF Lis, D. C. Schilke, P. Bergin, E. A. Gerin, M. Black, J. H. Comito, C. De Luca, M. Godard, B. Higgins, R. Le Petit, F. Pearson, J. C. Pellegrini, E. W. Phillips, T. G. Yu, S. TI WIDESPREAD ROTATIONALLY HOT HYDRONIUM ION IN THE GALACTIC INTERSTELLAR MEDIUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; galaxies: nuclei; ISM: molecules; molecular processes; submillimeter: general; techniques: spectroscopic ID SIGHT-LINE; SGR B2; MOLECULAR-HYDROGEN; H3O+; AMMONIA; CLOUDS; REGIONS; HIFI; H2O+; GAS AB We present new Herschel observations of the (6,6) and (9,9) inversion transitions of the hydronium ion toward Sagittarius B2(N) and W31C. Sensitive observations toward Sagittarius B2(N) show that the high, similar to 500 K, rotational temperatures characterizing the population of the highly excited metastable H3O+ rotational levels are present over a wide range of velocities corresponding to the Sagittarius B2 envelope, as well as the foreground gas clouds between the Sun and the source. Observations of the same lines toward W31C, a line of sight that does not intersect the Central Molecular Zone but instead traces quiescent gas in the Galactic disk, also imply a high rotational temperature of similar to 380 K, well in excess of the kinetic temperature of the diffuse Galactic interstellar medium. While it is plausible that some fraction of the molecular gas may be heated to such high temperatures in the active environment of the Galactic center, characterized by high X-ray and cosmic-ray fluxes, shocks, and high degree of turbulence, this is unlikely in the largely quiescent environment of the Galactic disk clouds. We suggest instead that the highly excited states of the hydronium ion are populated mainly by exoergic chemical formation processes and the temperature describing the rotational level population does not represent the physical temperature of the medium. The same arguments may be applicable to other symmetric top rotors, such as ammonia. This offers a simple explanation of the long-standing puzzle of the presence of a pervasive, hot molecular gas component in the central region of the Milky Way. Moreover, our observations suggest that this is a universal process not limited to the active environments associated with galactic nuclei. C1 [Lis, D. C.; Phillips, T. G.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Lis, D. C.] Univ Paris 06, Sorbonne Univ, CNRS, Observ Paris,LERMA,UMR 8112, Paris, France. [Schilke, P.; Comito, C.; Higgins, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Bergin, E. A.] Univ Michigan, Ann Arbor, MI 48109 USA. [Gerin, M.; De Luca, M.; Godard, B.; Le Petit, F.] Ecole Normale Super, CNRS, Observ Paris, LERMA,UMR 8112, Paris, France. [Black, J. H.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Pearson, J. C.; Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Pellegrini, E. W.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. RP Lis, DC (reprint author), CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. EM dcl@caltech.edu; schilke@ph1.uni-koeln.de; ebergin@umich.edu; maryvonne.gerin@lra.ens.fr; john.black@chalmers.se; ccomito@ph1.uni-koeln.de; deluca@lra.ens.fr; benjamin.godard@lra.ens.fr; higgins@ph1.uni-koeln.de; franck.lepetit@obspm.fr; john.c.pearson@jpl.nasa.gov; eric.pellegrini@utoledo.edu; tgp@submm.caltech.edu; shanshan.yu@jpl.nasa.gov RI Yu, Shanshan/D-8733-2016 FU NASA through JPL/Caltech; Collaborative Research Center 956 - Deutsche Forschungsgemeinschaft (DFG) FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States (NASA) under the leadership of SRON, Netherlands Institute for Space Research, Groningen, The Netherlands, and with major contributions from Germany, France, and the US. Support for this work was provided by NASA (Herschel OT funding) through an award issued by JPL/Caltech. The research of P. S., C. C., and R. H. is supported by the Collaborative Research Center 956 funded by the Deutsche Forschungsgemeinschaft (DFG). NR 46 TC 11 Z9 11 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2014 VL 785 IS 2 AR 135 DI 10.1088/0004-637X/785/2/135 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800054 ER PT J AU Masters, D McCarthy, P Siana, B Malkan, M Mobasher, B Atek, H Henry, A Martin, CL Rafelski, M Hathi, NP Scarlata, C Ross, NR Bunker, AJ Blanc, G Bedregal, AG Dominguez, A Colbert, J Teplitz, H Dressler, A AF Masters, Daniel McCarthy, Patrick Siana, Brian Malkan, Mathew Mobasher, Bahram Atek, Hakim Henry, Alaina Martin, Crystal L. Rafelski, Marc Hathi, Nimish P. Scarlata, Claudia Ross, Nathaniel R. Bunker, Andrew J. Blanc, Guillermo Bedregal, Alejandro G. Dominguez, Alberto Colbert, James Teplitz, Harry Dressler, Alan TI PHYSICAL PROPERTIES OF EMISSION-LINE GALAXIES AT z similar to 2 FROM NEAR-INFRARED SPECTROSCOPY WITH MAGELLAN FIRE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: high-redshift; galaxies: kinematics and dynamics; galaxies: starburst; galaxies: star formation ID STAR-FORMING GALAXIES; MASS-METALLICITY RELATION; H-II REGIONS; DIGITAL SKY SURVEY; INTEGRAL FIELD SPECTROSCOPY; FRAME OPTICAL-SPECTRA; LYMAN BREAK GALAXIES; GREATER-THAN 1; HIGH-REDSHIFT; CHEMICAL ABUNDANCES AB We present results from near-infrared spectroscopy of 26 emission-line galaxies at z similar to 2.2 and z similar to 1.5 obtained with the Folded-port InfraRed Echellette (FIRE) spectrometer on the 6.5 m Magellan Baade telescope. The sample was selected from the WFC3 Infrared Spectroscopic Parallels survey, which uses the near-infrared grism of the Hubble Space Telescope Wide Field Camera 3 (WFC3) to detect emission-line galaxies over 0.3 less than or similar to z less than or similar to 2.3. Our FIRE follow-up spectroscopy (R similar to 5000) over 1.0-2.5 mu m permits detailedmeasurements of the physical properties of the z similar to 2 emission-line galaxies. Dust-corrected star formation rates for the sample range from similar to 5-100 M-circle dot yr(-1) with a mean of 29 M-circle dot yr(-1). We derive a median metallicity for the sample of 12 + log(O/H) = 8.34 or similar to 0.45 Z(circle dot). The estimated stellar masses range from similar to 10(8.5)-10(9.5) M-circle dot, and a clear positive correlation between metallicity and stellar mass is observed. The average ionization parameter measured for the sample, log U approximate to -2.5, is significantly higher than what is found for most star-forming galaxies in the local universe, but similar to the values found for other star-forming galaxies at high redshift. We derive composite spectra from the FIRE sample, from which we measure typical nebular electron densities of similar to 100-400 cm(-3). Based on the location of the galaxies and composite spectra on diagnostic diagrams, we do not find evidence for significant active galactic nucleus activity in the sample. Most of the galaxies, as well as the composites, are offset diagram toward higher [O III]/H beta at a given [N II]/H alpha, in agreement with other observations of z greater than or similar to 1 star-forming galaxies, but composite spectra derived from the sample do not show an appreciable offset from the local star-forming sequence on the [O III]/H beta versus [S II]/H alpha diagram. We infer a high nitrogen-to-oxygen abundance ratio from the composite spectrum, which may contribute to the offset of the high-redshift galaxies from the local star-forming sequence in the [O III]/H beta versus [N II]/H alpha diagram. We speculate that the elevated nitrogen abundance could result from substantial numbers of Wolf-Rayet stars in starbursting galaxies at z similar to 2. C1 [Masters, Daniel; Siana, Brian; Mobasher, Bahram; Dominguez, Alberto] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Masters, Daniel; McCarthy, Patrick; Blanc, Guillermo; Dressler, Alan] Carnegie Observ, Pasadena, CA 91101 USA. [Malkan, Mathew; Ross, Nathaniel R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Atek, Hakim] Ecole Polytech Fed, Astrophys Lab, CH-1290 Sauverny, Switzerland. [Henry, Alaina] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Martin, Crystal L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Rafelski, Marc; Colbert, James] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Hathi, Nimish P.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Scarlata, Claudia] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Bunker, Andrew J.] Univ Oxford, Dept Phys, Oxford OX1 2JD, England. [Bedregal, Alejandro G.] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. [Teplitz, Harry] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. RP Masters, D (reprint author), Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. RI Blanc, Guillermo/I-5260-2016; Hathi, Nimish/J-7092-2014; OI Hathi, Nimish/0000-0001-6145-5090; Dominguez, Alberto/0000-0002-3433-4610 FU Carnegie Observatories graduate research fellowship; NSF [AAG 1109288] FX We thank the anonymous referee for thoughtful comments and suggestions that significantly improved this paper, and Evan Skillman for a careful reading and helpful comments. We are also grateful to Rob Simcoe, Lisa Kewley, Ryan Quadri, Daniel Kelson, and Louis Abramson for discussions regarding the FIRE observations and science. D. C. M. gratefully acknowledges the support provided by the Carnegie Observatories graduate research fellowship, as well as the excellent support provided by the staff of the Las Campanas Observatory. C. L. M. acknowledges support from NSF AAG 1109288. NR 96 TC 59 Z9 59 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 APR 20 PY 2014 VL 785 IS 2 AR 153 DI 10.1088/0004-637X/785/2/153 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800072 ER PT J AU Nakamura, M Meier, DL AF Nakamura, Masanori Meier, David L. TI A MAGNETOHYDRODYNAMIC MODEL OF THE M87 JET. II. SELF-CONSISTENT QUAD-SHOCK JET MODEL FOR OPTICAL RELATIVISTIC MOTIONS AND PARTICLE ACCELERATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (M87); galaxies: jets; magnetohydrodynamics (MHD); methods: numerical ID COSMIC-RAY ACCELERATION; HUBBLE-SPACE-TELESCOPE; MAGNETIC-FIELD AMPLIFICATION; ACTIVE GALACTIC NUCLEI; BASE-LINE ARRAY; ULTRARELATIVISTIC SHOCKS; NUMERICAL SIMULATIONS; ASTROPHYSICAL SHOCKS; FERMI ACCELERATION; INTERNAL SHOCKS AB We describe a new paradigm for understanding both relativistic motions and particle acceleration in the M87 jet: a magnetically dominated relativistic flow that naturally produces four relativistic magnetohydrodynamic (MHD) shocks (forward/reverse fast and slow modes). We apply this model to a set of optical super-and subluminal motions discovered by Biretta and coworkers with the Hubble Space Telescope during 1994-1998. The model concept consists of ejection of a single relativistic Poynting jet, which possesses a coherent helical (poloidal + toroidal) magnetic component, at the remarkably flaring point HST-1. We are able to reproduce quantitatively proper motions of components seen in the optical observations of HST-1 with the same model we used previously to describe similar features in radio very long baseline interferometry observations in 2005-2006. This indicates that the quad relativistic MHD shock model can be applied generally to recurring pairs of super/subluminal knots ejected from the upstream edge of the HST-1 complex as observed from radio to optical wavelengths, with forward/reverse fast-mode MHD shocks then responsible for observed moving features. Moreover, we identify such intrinsic properties as the shock compression ratio, degree of magnetization, and magnetic obliquity and show that they are suitable to mediate diffusive shock acceleration of relativistic particles via the first-order Fermi process. We suggest that relativistic MHD shocks in Poynting-flux-dominated helical jets may play a role in explaining observed emission and proper motions in many active galactic nuclei. C1 [Nakamura, Masanori] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Meier, David L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Nakamura, M (reprint author), Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS-NTU 1, Taipei 10617, Taiwan. EM nakamura@asiaa.sinica.edu.tw; david.l.meier@jpl.nasa.gov FU Allan C. Davis fellowship; Department of Physics and Astronomy at Johns Hopkins University; Space Telescope Science Institute; National Aeronautics and Space Administration FX M.N. acknowledges part of this research was carried out under supported by the Allan C. Davis fellowship jointly awarded by the Department of Physics and Astronomy at Johns Hopkins University and the Space Telescope Science Institute. Part of this research also was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 60 TC 7 Z9 7 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 APR 20 PY 2014 VL 785 IS 2 AR 152 DI 10.1088/0004-637X/785/2/152 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800071 ER PT J AU Ranjan, S Charbonneau, D Desert, JM Madhusudhan, N Deming, D Wilkins, A Mandell, AM AF Ranjan, Sukrit Charbonneau, David Desert, Jean-Michel Madhusudhan, Nikku Deming, Drake Wilkins, Ashlee Mandell, Avi M. TI ATMOSPHERIC CHARACTERIZATION OF FIVE HOT JUPITERS WITH THE WIDE FIELD CAMERA 3 ON THE HUBBLE SPACE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; techniques: photometric; techniques: spectroscopic ID NICMOS TRANSMISSION SPECTROSCOPY; EXTRASOLAR PLANET ATMOSPHERE; COLLISION-INDUCED ABSORPTION; INFRARED-EMISSION SPECTRUM; SECONDARY ECLIPSE; HD 189733B; TEMPERATURE INVERSION; EXOPLANET ATMOSPHERES; MODEL ATMOSPHERES; THERMAL EMISSION AB We probe the structure and composition of the atmospheres of five hot Jupiter exoplanets using the Hubble Space Telescope Wide Field Camera 3 (WFC3) instrument. We use the G141 grism (1.1-1.7 mu m) to study TrES-2b, TrES-4b, and CoRoT-1b in transit; TrES-3b in secondary eclipse; and WASP-4b in both. This wavelength region includes a predicted absorption feature from water at 1.4 mu m, which we expect to be nondegenerate with the other molecules that are likely to be abundant for hydrocarbon-poor (e. g., solar composition) hot Jupiter atmospheres. We divide our wavelength regions into 10 bins. For each bin we produce a spectrophotometric light curve spanning the time of transit or eclipse. We correct these light curves for instrumental systematics without reference to an instrument model. For our transmission spectra, our mean 1 sigma precision per bin corresponds to variations of 2.1, 2.8, and 3.0 atmospheric scale heights for TrES-2b, TrES-4b, and CoRoT-1b, respectively. We find featureless spectra for these three planets. We are unable to extract a robust transmission spectrum for WASP-4b. For our dayside emission spectra, our mean 1 sigma precision per bin corresponds to a planet-to-star flux ratio of 1.5 x 10(-4) and 2.1 x 10(-4) for WASP-4b and TrES-3b, respectively. We combine these estimates with previous broadband measurements and conclude that for both planets isothermal atmospheres are disfavored. We find no signs of features due to water. We confirm that WFC3 is suitable for studies of transiting exoplanets, but in staring mode multivisit campaigns are necessary to place strong constraints on water abundance. C1 [Ranjan, Sukrit; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Desert, Jean-Michel] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Madhusudhan, Nikku] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA. [Deming, Drake; Wilkins, Ashlee] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mandell, Avi M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Desert, Jean-Michel] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Ranjan, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sranjan@cfa.harvard.edu OI Ranjan, Sukrit/0000-0002-5147-9053 FU NASA through Space Telescope Science Institute; NASA [NAS 5-26555]; National Science Foundation Graduate Research Fellowship [DGE-1144152]; California Institute of Technology (Caltech); NASA through the Sagan Fellowship Program grant; Yale University through the YCAA postdoctoral prize fellowship; [HST-GO-12181] FX Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute (STScI). These observations are associated with program HST-GO-12181. Support for this program was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1144152. This work was also performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program grant awarded to J.-M.D. N.M. acknowledges support from Yale University through the YCAA postdoctoral prize fellowship. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org; the SIMBAD database, operated at CDS, Strasbourg, France; NASA's Astrophysics Data System Bibliographic Services; and SAOImage DS9, developed by Smithsonian Astrophysical Observatory. The authors are grateful to Z. Berta-Thompson and J. Carter for many fruitful discussions, to the STScI HST help team for their assistance, and to an anonymous referee whose comments strengthened the paper. NR 69 TC 15 Z9 15 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2014 VL 785 IS 2 AR 148 DI 10.1088/0004-637X/785/2/148 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800067 ER PT J AU Robinson, TD Marley, MS AF Robinson, Tyler D. Marley, Mark S. TI TEMPERATURE FLUCTUATIONS AS A SOURCE OF BROWN DWARF VARIABILITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; convection; radiation mechanisms: thermal; stars: atmospheres ID LOW-MASS STARS; T-DWARFS; EVOLVING WEATHER; ULTRACOOL DWARFS; INFRARED COLORS; GRAVITY-WAVES; GIANT PLANETS; ATMOSPHERES; MODELS; CLOUDS AB A number of brown dwarfs are now known to be variable with observed amplitudes as large as 10%-30% at some wavelengths. While spatial inhomogeneities in cloud coverage and thickness are likely responsible for much of the observed variability, it is possible that some of the variations arise from atmospheric temperature fluctuations instead of, or in addition to, clouds. To better understand the role that thermal variability might play we present a case study of brown dwarf variability using a newly developed one-dimensional, time-stepping model of atmospheric thermal structure. We focus on the effects of thermal perturbations, intentionally simplifying the problem through omission of clouds and atmospheric circulation. Model results demonstrate that thermal perturbations occurring deep in the atmosphere (at pressures greater than 10 bar) of a model T-dwarf can be communicated to the upper atmosphere through radiative heating via the windows in near-infrared water opacity. The response time depends on where in the atmosphere a thermal perturbation is introduced. We show that, for certain periodic perturbations, the emission spectrum can have complex time-and wavelength-dependent behaviors, including phase shifts in times of maximum flux observed at different wavelengths. Since different wavelengths probe different levels in the atmosphere, these variations track a wavelength-dependent set of radiative exchanges happening between different atmospheric levels as a perturbation evolves in time. We conclude that thermal-as well as cloud-fluctuations must be considered as possible contributors to the observed brown dwarf variability. C1 [Robinson, Tyler D.; Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Robinson, Tyler D.] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA. RP Robinson, TD (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM tyler.d.robinson@nasa.gov RI Marley, Mark/I-4704-2013; OI Marley, Mark/0000-0002-5251-2943; Robinson, Tyler/0000-0002-3196-414X FU NASA Astrobiology Institute's Virtual Planetary Laboratory [NNH05ZDA001C]; NASA Planetary Atmospheres and Origins programs FX T.R. gratefully acknowledges support from an appointment to the NASA Postdoctoral Program at NASA Ames Research Center, administered by Oak Ridge Affiliated Universities, and from the NASA Astrobiology Institute's Virtual Planetary Laboratory, under solicitation No. NNH05ZDA001C. M. M. acknowledges support of the NASA Planetary Atmospheres and Origins programs. We thank Jonathan Fortney for sharing tools for computing normalized contribution functions, Jacqueline Radigan for reviewing an early version of this paper, and Caroline Morley for sharing updates to relevant cloud routines in our thermal structure model. NR 35 TC 16 Z9 16 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 APR 20 PY 2014 VL 785 IS 2 AR 158 DI 10.1088/0004-637X/785/2/158 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800077 ER PT J AU Spilker, JS Marrone, DP Aguirre, E Aravena, M Ashby, MLN Bethermin, M Bradford, CM Bothwell, MS Brodwin, M Carlstrom, JE Chapman, SC Crawford, TM de Breuck, C Fassnacht, CD Gonzalez, AH Greve, TR Gullberg, B Hezaveh, Y Holzapfel, WL Husband, K Ma, J Malkan, M Murphy, EJ Reichardt, CL Rotermund, KM Stalder, B Stark, AA Strandet, M Vieira, JD Weiss, A Welikala, N AF Spilker, J. S Marrone, D. P. Aguirre, E. Aravena, M. Ashby, M. L. N. Bethermin, M. Bradford, C. M. Bothwell, M. S. Brodwin, M. Carlstrom, J. E. Chapman, S. C. Crawford, T. M. de Breuck, C. Fassnacht, C. D. Gonzalez, A. H. Greve, T. R. Gullberg, B. Hezaveh, Y. Holzapfel, W. L. Husband, K. Ma, J. Malkan, M. Murphy, E. J. Reichardt, C. L. Rotermund, K. M. Stalder, B. Stark, A. A. Strandet, M. Vieira, J. D. Weiss, A. Welikala, N. TI THE REST-FRAME SUBMILLIMETER SPECTRUM OF HIGH-REDSHIFT, DUSTY, STAR-FORMING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: ISM; galaxies: star formation; ISM: molecules ID DENSE MOLECULAR GAS; SOUTH-POLE TELESCOPE; ULTRALUMINOUS INFRARED GALAXIES; DIFFUSE INTERSTELLAR-MEDIUM; CLOVERLEAF QUASAR; APM 08279+5255; CONVERSION FACTOR; HERSCHEL-SPIRE; LINE EMISSION; ARP 220 AB We present the average rest-frame spectrum of high-redshift dusty, star-forming galaxies from 250 to 770 GHz. This spectrum was constructed by stacking Atacama Large Millimeter/submillimeter Array (ALMA) 3 mm spectra of 22 such sources discovered by the South Pole Telescope and spanning z = 2.0-5.7. In addition to multiple bright spectral features of (CO)-C-12, [C I], and H2O, we also detect several faint transitions of (CO)-C-13, HCN, HNC, HCO+, and CN, and use the observed line strengths to characterize the typical properties of the interstellar medium of these high-redshift starburst galaxies. We find that the (CO)-C-13 brightness in these objects is comparable to that of the only otherz > 2 star-forming galaxy in which (CO)-C-13 has been observed. We show that the emission from the high-critical density molecules HCN, HNC, HCO+, and CN is consistent with a warm, dense medium with T-kin similar to 55K and n(H2) >= 10(5.5) cm(-3). High molecular hydrogen densities are required to reproduce the observed line ratios, and we demonstrate that alternatives to purely collisional excitation are unlikely to be significant for the bulk of these systems. We quantify the average emission from several species with no individually detected transitions, and find emission from the hydride CH and the linear molecule CCH for the first time at high redshift, indicating that these molecules may be powerful probes of interstellar chemistry in high-redshift systems. These observations represent the first constraints on many molecular species with rest-frame transitions from 0.4 to 1.2 mm in star-forming systems at high redshift, and will be invaluable in making effective use of ALMA in full science operations. C1 [Spilker, J. S; Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Aguirre, E.] Univ Penn, Philadelphia, PA 19104 USA. [Aravena, M.] European So Observ, Casilla 19001, Vitacura Santia, Chile. [Aravena, M.] Univ Diego Port, Fac Ingn, Santiago, Chile. [Ashby, M. L. N.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bethermin, M.] Univ Paris Diderot, CEA Saclay, CEA DSM Irfu CNRS, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bothwell, M. S.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HA, England. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Carlstrom, J. E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Chapman, S. C.; Rotermund, K. M.] Dalhousie Univ, Halifax, NS, Canada. [de Breuck, C.; Gullberg, B.] European So Observ, D-85748 Garching, Germany. [Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Gonzalez, A. H.; Husband, K.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Hezaveh, Y.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Holzapfel, W. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Husband, K.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Malkan, M.] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Murphy, E. J.] Carnegie Inst Sci, Pasadena, CA 91101 USA. [Strandet, M.; Weiss, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Welikala, N.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France. RP Spilker, JS (reprint author), Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. EM jspilker@as.arizona.edu RI Aravena, Manuel/O-2361-2014; Holzapfel, William/I-4836-2015; OI Bethermin, Matthieu/0000-0002-3915-2015; Stark, Antony/0000-0002-2718-9996; Marrone, Daniel/0000-0002-2367-1080; Reichardt, Christian/0000-0003-2226-9169; De Breuck, Carlos/0000-0002-6637-3315 FU U.S. National Science Foundation [AST-1312950]; National Science Foundation [ANT-0638937]; Kavli Foundation; Gordon and Betty Moore Foundation; Commonwealth of Australia; [PHY-1125897] FX This material is based on work supported by the U.S. National Science Foundation under grant No. AST-1312950. The SPT is supported by the National Science Foundation through grant ANT-0638937, with partial support through PHY-1125897, the Kavli Foundation and the Gordon and Betty Moore Foundation. This paper makes use of the following ALMA data: ADS/JAO.ALMA2011.0.00957.S and 2011.0.00958.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. 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. This research has made use of NASA's Astrophysics Data System. NR 119 TC 18 Z9 18 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2014 VL 785 IS 2 AR 149 DI 10.1088/0004-637X/785/2/149 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800068 ER PT J AU Bulyshev, A Amzajerdian, F Roback, VE Hines, G Pierrottet, D Reisse, R AF Bulyshev, Alexander Amzajerdian, Farzin Roback, Vincent E. Hines, Glenn Pierrottet, Diego Reisse, Robert TI Three-dimensional super-resolution: theory, modeling, and field test results SO APPLIED OPTICS LA English DT Article ID IMAGE-RECONSTRUCTION AB Many flash lidar applications continue to demand higher three-dimensional image resolution beyond the current state-of-the-art technology of the detector arrays and their associated readout circuits. Even with the available number of focal plane pixels, the required number of photons for illuminating all the pixels may impose impractical requirements on the laser pulse energy or the receiver aperture size. Therefore, image resolution enhancement by means of a super-resolution algorithm in near real time presents a very attractive solution for a wide range of flash lidar applications. This paper describes a super-resolution technique and illustrates its performance and merits for generating three-dimensional image frames at a video rate. (C) 2014 Optical Society of America C1 [Bulyshev, Alexander] Analyt Mech Associates, Hampton, VA 23666 USA. [Amzajerdian, Farzin; Roback, Vincent E.; Hines, Glenn; Reisse, Robert] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Pierrottet, Diego] Coherent Applicat Inc, Hampton, VA 23666 USA. RP Bulyshev, A (reprint author), Analyt Mech Associates, Hampton, VA 23666 USA. EM alexander.bulyshev-1@nasa.gov NR 19 TC 6 Z9 6 U1 0 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 APR 20 PY 2014 VL 53 IS 12 BP 2583 EP 2594 DI 10.1364/AO.53.002583 PG 12 WC Optics SC Optics GA AF2ZZ UT WOS:000334582400005 PM 24787583 ER PT J AU Epstein, CR Elsworth, YP Johnson, JA Shetrone, M Mosser, B Hekker, S Tayar, J Harding, P Pinsonneault, M Aguirre, VS Basu, S Beers, TC Bizyaev, D Bedding, TR Chaplin, WJ Frinchaboy, PM Garcia, RA Perez, AEG Hearty, FR Huber, D Ivans, II Majewski, SR Mathur, S Nidever, D Serenelli, A Schiavon, RP Schneider, DP Schonrichi, R Sobeck, JS Stassun, KG Stello, D Zasowski, G AF Epstein, Courtney R. Elsworth, Yvonne P. Johnson, Jennifer A. Shetrone, Matthew Mosser, Benoit Hekker, Saskia Tayar, Jamie Harding, Paul Pinsonneault, Marc Aguirre, Victor Silva Basu, Sarbani Beers, Timothy C. Bizyaev, Dmitry Bedding, Timothy R. Chaplin, William J. Frinchaboy, Peter M. Garcia, Rafael A. Perez, Ana E. Garcia Hearty, Fred R. Huber, Daniel Ivans, Inese I. Majewski, Steven R. Mathur, Savita Nidever, David Serenelli, Aldo Schiavon, Ricardo P. Schneider, Donald P. Schoenrichi, Ralph Sobeck, Jennifer S. Stassun, Keivan G. Stello, Dennis Zasowski, Gail TI TESTING THE ASTEROSEISMIC MASS SCALE USING METAL-POOR STARS CHARACTERIZED WITH APOGEE AND KEPLER SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE asteroseismology; Galaxy: halo; stars: fundamental parameters ID SOLAR-LIKE OSCILLATIONS; DIGITAL SKY SURVEY; MILKY-WAY; NGC 6791; GLOBULAR-CLUSTERS; RED GIANTS; HIPPARCOS PARALLAXES; STELLAR POPULATIONS; BRANCH STARS; AGE AB Fundamental stellar properties, such as mass, radius, and age, can be inferred using asteroseismology. Cool stars with convective envelopes have turbulent motions that can stochastically drive and damp pulsations. The properties of the oscillation frequency power spectrum can be tied to mass and radius through solar-scaled asteroseismic relations. Stellar properties derived using these scaling relations need verification over a range of metallicities. Because the age and mass of halo stars are well-constrained by astrophysical priors, they provide an independent, empirical check on asteroseismic mass estimates in the low-metallicity regime. We identify nine metal-poor red giants (including six stars that are kinematically associated with the halo) from a sample observed by both the Kepler space telescope and the Sloan Digital Sky Survey-III APOGEE spectroscopic survey. We compare masses inferred using asteroseismology to those expected for halo and thick-disk stars. Although our sample is small, standard scaling relations, combined with asteroseismic parameters from the APOKASC Catalog, produce masses that are systematically higher ((Delta M) = 0.17 +/- 0.05 M-circle dot) than astrophysical expectations. The magnitude of the mass discrepancy is reduced by known theoretical corrections to the measured large frequency separation scaling relationship. Using alternative methods for measuring asteroseismic parameters induces systematic shifts at the 0.04 M-circle dot level. We also compare published asteroseismic analyses with scaling relationship masses to examine the impact of using the frequency of maximum power as a constraint. Upcoming APOKASC observations will provide a larger sample of similar to 100 metal-poor stars, important for detailed asteroseismic characterization of Galactic stellar populations. C1 [Epstein, Courtney R.; Johnson, Jennifer A.; Tayar, Jamie; Pinsonneault, Marc; Schoenrichi, Ralph; Zasowski, Gail] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Elsworth, Yvonne P.; Chaplin, William J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Johnson, Jennifer A.; Zasowski, Gail] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Shetrone, Matthew] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Mosser, Benoit] Univ Paris 06, Univ Denis Diderot, Observ Paris, LESIA,CNRS, F-92195 Meudon, France. [Hekker, Saskia] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Harding, Paul] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Aguirre, Victor Silva] Dept Phys & Astron, Stellar Astrophys Ctr, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Beers, Timothy C.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Beers, Timothy C.] JINA, Sunspot, NM 88349 USA. [Bizyaev, Dmitry] Apache Point Observ, Sunspot, NM 88349 USA. [Bedding, Timothy R.; Stello, Dennis] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Frinchaboy, Peter M.] Texas Christian Univ, Dept Phys & Astron, Ft Worth, TX 76129 USA. [Garcia, Rafael A.] Univ Paris 07, CEA DSM CNRS, Ctr Saclay, IRFU SAp,Lab AIM, F-91191 Gif Sur Yvette, France. [Perez, Ana E. Garcia; Hearty, Fred R.; Majewski, Steven R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ivans, Inese I.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Mathur, Savita] Space Sci Inst, Boulder, CO 80301 USA. [Nidever, David] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Serenelli, Aldo] IEEC CSIC, Inst Space Sci, Fac Cincies, Campus UAB, E-08193 Bellaterra, Spain. [Schiavon, Ricardo P.] Liverpool John Moores Univ, IC2, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Schoenrichi, Ralph] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England. [Sobeck, Jennifer S.] Univ Chicago, JINA, Chicago, IL 60637 USA. [Sobeck, Jennifer S.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Zasowski, Gail] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Epstein, CR (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM epstein@astronomy.ohio-state.edu OI Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776; Serenelli, Aldo/0000-0001-6359-2769 FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University; Physics Frontier Center/Joint Institute for Nuclear Astrophysics (JINA) [PHY 08-22648]; NASA [NNX12AE17G]; Netherlands Organization for Scientific Research; ERC [338251]; MICINN [AYA2011-24704]; Danish National Research Foundation [DNRF106]; ASTERISK project (AS-TERoseismic Investigations with SONG and Kepler); European Research Council [267864]; [AST-1211673] FX Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.; We thank Andrea Miglio and the APOKASC team for helpful discussions. C. R. E., J.A.J., and M. P. acknowledge support by AST-1211673, T. C. B. by PHY 08-22648: Physics Frontier Center/Joint Institute for Nuclear Astrophysics (JINA), and S. M. by the NASA grant NNX12AE17G. S. H. acknowledges support from the Netherlands Organization for Scientific Research and ERC Starting Grant #338251 Stellar Ages. A. S. is partially supported by the MICINN grant AYA2011-24704. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant agreement No. DNRF106). V. S. A. is supported by the ASTERISK project (AS-TERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement No. 267864). NR 50 TC 31 Z9 31 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2014 VL 785 IS 2 AR L28 DI 10.1088/2041-8205/785/2/L28 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE9VR UT WOS:000334359800009 ER PT J AU Kipping, DM Bastien, FA Stassun, KG Chaplin, WJ Huber, D Buchhave, LA AF Kipping, D. M. Bastien, F. A. Stassun, K. G. Chaplin, W. J. Huber, D. Buchhave, L. A. TI FLICKER AS A TOOL FOR CHARACTERIZING PLANETS THROUGH ASTERODENSITY PROFILING SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: activity; stars: solar-type; techniques: photometric ID CANDIDATE HOST STARS; FIELD STARS; ASTEROSEISMOLOGY; OSCILLATIONS; ROTATION; AGES; VARIABILITY AB Variability in the time series brightness of a star on a timescale of 8 hr, known as "flicker," has been previously demonstrated to serve as a proxy for the surface gravity of a star by Bastien et al. Although surface gravity is crucial for stellar classification, it is the mean stellar density that is most useful when studying transiting exoplanets, due to its direct impact on the transit light curve shape. Indeed, an accurate and independent measure of the stellar density can be leveraged to infer subtle properties of a transiting system, such as the companion's orbital eccentricity via asterodensity profiling (AP). We here calibrate flicker to the mean stellar density of 439 Kepler targets with asteroseismology, allowing us to derive a new empirical relation given by log(10)(rho star (kg m(- 3))) = 5.413 - 1.850 log(10)(F-8 (ppm)). The calibration is valid for stars with 4500 < T-eff < 6500 K, KP < 14, and flicker estimates corresponding to stars with 3.25 < log g star < 4.43. Our relation has a model error in the stellar density of 31.7% and so has similar to 8 times lower precision than that from asteroseismology but is applicable to a sample similar to 40 times greater. Flicker therefore provides an empirical method to enable AP on hundreds of planetary candidates from present and future missions. C1 [Kipping, D. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bastien, F. A.; Stassun, K. G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Stassun, K. G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Chaplin, W. J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Chaplin, W. J.] Aarhus Univ, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huber, D.] SETI Inst, Mountain View, CA 94043 USA. [Buchhave, L. A.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu OI Buchhave, Lars A./0000-0003-1605-5666; Stassun, Keivan/0000-0002-3481-9052 FU NASA Sagan Fellowship; NASA Harriet Jenkins Fellowship; Vanderbilt Provost Graduate Fellowship; UK Science and Technology Facilities Council; NASA Postdoctoral Program at Ames Research Center; Kepler Participating Scientist Program FX D.M.K. is supported by the NASA Sagan Fellowships. F. A. B. is supported by the NASA Harriet Jenkins Fellowship and a Vanderbilt Provost Graduate Fellowship. W.J.C. acknowledges financial support from the UK Science and Technology Facilities Council. D. H. acknowledges support by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA, and support by the Kepler Participating Scientist Program. We thank the anaon. NR 33 TC 7 Z9 7 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 APR 20 PY 2014 VL 785 IS 2 AR L32 DI 10.1088/2041-8205/785/2/L32 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE9VR UT WOS:000334359800013 ER PT J AU Yamaguchi, H Badenes, C Petre, R Nakano, T Castro, D Enoto, T Hiraga, JS Hughes, JP Maeda, Y Nobukawa, M Safi-Harb, S Slane, PO Smith, RK Uchida, H AF Yamaguchi, Hiroya Badenes, Carles Petre, Robert Nakano, Toshio Castro, Daniel Enoto, Teruaki Hiraga, Junko S. Hughes, John P. Maeda, Yoshitomo Nobukawa, Masayoshi Safi-Harb, Samar Slane, Patrick O. Smith, Randall K. Uchida, Hiroyuki TI DISCRIMINATING THE PROGENITOR TYPE OF SUPERNOVA REMNANTS WITH IRON K-SHELL EMISSION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: abundances; ISM: supernova remnants; X-rays: ISM ID X-RAY-EMISSION; LARGE-MAGELLANIC-CLOUD; XMM-NEWTON OBSERVATIONS; IA SUPERNOVA; SHOCKED EJECTA; RCW 86; CHANDRA; SPECTROSCOPY; EXPLOSION; SUZAKU AB Supernova remnants (SNRs) retain crucial information about both their parent explosion and circumstellar material left behind by their progenitor. However, the complexity of the interaction between supernova ejecta and ambient medium often blurs this information, and it is not uncommon for the basic progenitor type (Ia or core-collapse) of well-studied remnants to remain uncertain. Here we present a powerful new observational diagnostic to discriminate between progenitor types and constrain the ambient medium density of SNRs using solely Fe K-shell X-ray emission. We analyze all extant Suzaku observations of SNRs and detect Fe K alpha emission from 23 young or middle-aged remnants, including five first detections (IC 443, G292.0+ 1.8, G337.2-0.7, N49, and N63A). The Fe Ka centroids clearly separate progenitor types, with the Fe-rich ejecta in Type Ia remnants being significantly less ionized than in core-collapse SNRs. Within each progenitor group, the Fe Ka luminosity and centroid are well correlated, with more luminous objects having more highly ionized Fe. Our results indicate that there is a strong connection between explosion type and ambient medium density, and suggest that Type Ia supernova progenitors do not substantially modify their surroundings at radii of up to several parsecs. We also detect a K-shell radiative recombination continuum of Fe in W49B and IC 443, implying a strong circumstellar interaction in the early evolutionary phases of these core-collapse remnants. C1 [Yamaguchi, Hiroya; Petre, Robert; Enoto, Teruaki] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yamaguchi, Hiroya] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Yamaguchi, Hiroya; Slane, Patrick O.; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Badenes, Carles] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Badenes, Carles] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, Pittsburgh, PA 15260 USA. [Badenes, Carles] Univ Pittsburgh, Pittsburgh, PA 15260 USA. [Nakano, Toshio; Hiraga, Junko S.] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Castro, Daniel] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. [Enoto, Teruaki] RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Maeda, Yoshitomo] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Nobukawa, Masayoshi] Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. [Safi-Harb, Samar] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. RP Yamaguchi, H (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM hiroya.yamaguchi@nasa.gov RI XRAY, SUZAKU/A-1808-2009; OI Enoto, Teruaki/0000-0003-1244-3100 NR 51 TC 27 Z9 27 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 APR 20 PY 2014 VL 785 IS 2 AR L27 DI 10.1088/2041-8205/785/2/L27 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE9VR UT WOS:000334359800008 ER PT J AU Sidery, T Aylott, B Christensen, N Farr, B Farr, W Feroz, F Gair, J Grover, K Graff, P Hanna, C Kalogera, V Mandel, I O'Shaughnessy, R Pitkin, M Price, L Raymond, V Rover, C Singer, L van der Sluys, M Smith, RJE Vecchio, A Veitch, J Vitale, S AF Sidery, T. Aylott, B. Christensen, N. Farr, B. Farr, W. Feroz, F. Gair, J. Grover, K. Graff, P. Hanna, C. Kalogera, V. Mandel, I. O'Shaughnessy, R. Pitkin, M. Price, L. Raymond, V. Roever, C. Singer, L. van der Sluys, M. Smith, R. J. E. Vecchio, A. Veitch, J. Vitale, S. TI Reconstructing the sky location of gravitational-wave detected compact binary systems: Methodology for testing and comparison SO PHYSICAL REVIEW D LA English DT Article ID ELECTROMAGNETIC COUNTERPARTS; INSPIRALS AB The problem of reconstructing the sky position of compact binary coalescences detected via gravitational waves is a central one for future observations with the ground-based network of gravitational-wave laser interferometers, such as Advanced LIGO and Advanced Virgo. Different techniques for sky localization have been independently developed. They can be divided in two broad categories: fully coherent Bayesian techniques, which are high latency and aimed at in-depth studies of all the parameters of a source, including sky position, and "triangulation-based" techniques, which exploit the data products from the search stage of the analysis to provide an almost real-time approximation of the posterior probability density function of the sky location of a detection candidate. These techniques have previously been applied to data collected during the last science runs of gravitational-wave detectors operating in the so-called initial configuration. Here, we develop and analyze methods for assessing the self consistency of parameter estimation methods and carrying out fair comparisons between different algorithms, addressing issues of efficiency and optimality. These methods are general, and can be applied to parameter estimation problems other than sky localization. We apply these methods to two existing sky localization techniques representing the two above-mentioned categories, using a set of simulated inspiral-only signals from compact binary systems with a total mass of <= 20M(circle dot) and nonspinning components. We compare the relative advantages and costs of the two techniques and show that sky location uncertainties are on average a factor approximate to 20 smaller for fully coherent techniques than for the specific variant of the triangulation-based technique used during the last science runs, at the expense of a factor approximate to 1000 longer processing time. C1 [Sidery, T.; Farr, B.; Farr, W.; Grover, K.; Mandel, I.; Smith, R. J. E.; Vecchio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Christensen, N.] Carleton Coll, Northfield, MN 55057 USA. [Farr, B.; Farr, W.; Kalogera, V.] Northwestern Univ, Dept Phys & Astron, CIERA, Evanston, IL 60208 USA. [Feroz, F.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Gair, J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Graff, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hanna, C.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [O'Shaughnessy, R.] Univ Wisconsin, Ctr Gravitat & Cosmol, Milwaukee, WI 53211 USA. [Pitkin, M.] Univ Glasgow, SUPA, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Price, L.; Raymond, V.; Singer, L.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Roever, C.] Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-30167 Hannover, Germany. [Roever, C.] Univ Med Ctr, Dept Med Stat, D-37073 Gottingen, Germany. [van der Sluys, M.] Radboud Univ Nijmegen, NL-6500 GL Nijmegen, Netherlands. [Veitch, J.] Nikhef, NL-1098 XG Amsterdam, Netherlands. [Vitale, S.] MIT, Cambridge, MA 02139 USA. RP Sidery, T (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. EM tsidery@star.sr.bham.ac.uk RI Vecchio, Alberto/F-8310-2015; OI Vecchio, Alberto/0000-0002-6254-1617; Rover, Christian/0000-0002-6911-698X; Farr, Ben/0000-0002-2916-9200; O'Shaughnessy, Richard/0000-0001-5832-8517; Mandel, Ilya/0000-0002-6134-8946; Pitkin, Matthew/0000-0003-4548-526X; Veitch, John/0000-0002-6508-0713 FU Foundation for Fundamental Research on Matter (FOM); Netherlands Organization for Scientific Research (NWO); NSF [PHY-1204371, PHY-1307020, DGE-0824162, PHY-0970074, PHY-0757058]; Oak Ridge Associated Universities; California Institute of Technology division of Physics, Mathematics Astronomy; LIGO Laboratory; UWM Research Growth Initiative FX 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). N.C. was supported by the NSF Grant No. PHY-1204371. P.G. was supported by a NASA postdoctoral fellowship from the Oak Ridge Associated Universities. B.F., W.F. and V.K. were supported by the NSF Grant No. PHY-1307020, and B.F. was also supported by the NSF Grant No. DGE-0824162. V.R. was supported by a prize postdoctoral fellowship from the California Institute of Technology division of Physics, Mathematics & Astronomy and LIGO Laboratory. R.O.S. was supported by the NSF Grant No. PHY-0970074 and the UWM Research Growth Initiative. 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 cooperative agreement no. PHY-0757058. NR 39 TC 25 Z9 25 U1 0 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 APR 18 PY 2014 VL 89 IS 8 AR 084060 DI 10.1103/PhysRevD.89.084060 PG 11 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AG2HH UT WOS:000335236500004 ER PT J AU Schmidt, GA AF Schmidt, Gavin A. TI Behind the Curve Science and the Politics of Global Warming SO SCIENCE LA English DT Book Review C1 [Schmidt, Gavin A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Schmidt, GA (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM gs210@columbia.edu RI Schmidt, Gavin/D-4427-2012 OI Schmidt, Gavin/0000-0002-2258-0486 NR 2 TC 0 Z9 0 U1 1 U2 11 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD APR 18 PY 2014 VL 344 IS 6181 BP 256 EP 256 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AF1LD UT WOS:000334474500019 ER PT J AU Quintana, EV Barclay, T Raymond, SN Rowe, JF Bolmont, E Caldwell, DA Howell, SB Kane, SR Huber, D Crepp, JR Lissauer, JJ Ciardi, DR Coughlin, JL Everett, ME Henze, CE Horch, E Isaacson, H Ford, EB Adams, FC Still, M Hunter, RC Quarles, B Selsis, F AF Quintana, Elisa V. Barclay, Thomas Raymond, Sean N. Rowe, Jason F. Bolmont, Emeline Caldwell, Douglas A. Howell, Steve B. Kane, Stephen R. Huber, Daniel Crepp, Justin R. Lissauer, Jack J. Ciardi, David R. Coughlin, Jeffrey L. Everett, Mark E. Henze, Christopher E. Horch, Elliott Isaacson, Howard Ford, Eric B. Adams, Fred C. Still, Martin Hunter, Roger C. Quarles, Billy Selsis, Franck TI An Earth-Sized Planet in the Habitable Zone of a Cool Star SO SCIENCE LA English DT Article ID LOW-MASS STARS; MAIN-SEQUENCE STARS; M-DWARF STARS; SUN-LIKE STAR; SUPER-EARTHS; ECLIPSING BINARY; GLIESE 581D; SYSTEMS; VALIDATION; RADII AB The quest for Earth-like planets is a major focus of current exoplanet research. Although planets that are Earth-sized and smaller have been detected, these planets reside in orbits that are too close to their host star to allow liquid water on their surfaces. We present the detection of Kepler-186f, a 1.11 +/- 0.14 Earth-radius planet that is the outermost of five planets, all roughly Earth-sized, that transit a 0.47 +/- 0.05 solar-radius star. The intensity and spectrum of the star's radiation place Kepler-186f in the stellar habitable zone, implying that if Kepler-186f has an Earth-like atmosphere and water at its surface, then some of this water is likely to be in liquid form. C1 [Quintana, Elisa V.; Rowe, Jason F.; Caldwell, Douglas A.; Huber, Daniel; Coughlin, Jeffrey L.] SETI Inst, Mountain View, CA 94043 USA. [Quintana, Elisa V.; Barclay, Thomas; Rowe, Jason F.; Caldwell, Douglas A.; Howell, Steve B.; Huber, Daniel; Lissauer, Jack J.; Coughlin, Jeffrey L.; Henze, Christopher E.; Hunter, Roger C.; Quarles, Billy] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barclay, Thomas; Still, Martin] Bay Area Environm Res Inst, West Sonoma, CA 95476 USA. [Raymond, Sean N.; Bolmont, Emeline; Selsis, Franck] Univ Bordeaux, Lab Astrophys Bordeaux, UMR 5804, F-33270 Floirac, France. [Raymond, Sean N.; Bolmont, Emeline; Selsis, Franck] CNRS, Lab Astrophys Bordeaux, UMR 5804, F-33270 Floirac, France. [Kane, Stephen R.] San Francisco State Univ, San Francisco, CA 94132 USA. [Crepp, Justin R.] Univ Notre Dame, Notre Dame, IN 46556 USA. [Lissauer, Jack J.] Stanford Univ, Dept Geol & Environm Sci, Stanford, CA 94305 USA. [Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Horch, Elliott] So Connecticut State Univ, New Haven, CT 06515 USA. [Isaacson, Howard] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Ford, Eric B.] Penn State Univ, Davey Lab 525, Ctr Exoplanets & Habitable, University Pk, PA 16802 USA. [Ford, Eric B.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Adams, Fred C.] Univ Michigan, Dept Phys, Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 USA. [Adams, Fred C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Quintana, EV (reprint author), SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA. EM elisa.quintana@nasa.gov RI Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Ciardi, David/0000-0002-5741-3047 FU Research Opportunities in Space and Earth Sciences Kepler Participating Scientist Program [NNX12AD21G]; NASA [NNA13AA93A, NAS5-26555]; NASA Postdoctoral Program at the Ames Research Center; Kepler Participating Scientist Program; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; European Research Council [209622: E3ARTHs]; NASA Science Mission directorate; NASA Office of Space Science [NNX13AC07G]; National Science Foundation (NSF); National Research Council (Canada); Comision Nacional de Investigacion Cientifica y Tecnologica (Chile); Australian Research Council (Australia); Ministerio da Ciencia, Tecnologia e Inovacao (Brazil); Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina) FX The authors working at NASA Ames thank the SETI Institute for hosting them during the U. S. government shutdown. E. V. Q. and J.F.R. acknowledge support from the Research Opportunities in Space and Earth Sciences Kepler Participating Scientist Program Grant NNX12AD21G. S.N.R.'s contribution was performed as part of the NASA Astrobiology Institute's Virtual Planetary Laboratory Lead Team, supported by NASA under cooperative agreement no. NNA13AA93A. D. H. acknowledges support by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA, and the Kepler Participating Scientist Program. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. F. S. acknowledges support from the European Research Council (Starting Grant 209622: E3ARTHs). This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. This research also made use of NASA's Astrophysics Data System. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). The Space Telescope Science Institute is operated by the Association of Universities for Research in Astronomy, under NASA contract NAS5-26555. Support for MAST for non-Hubble Space Telescope data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This research made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with NASA under the Exoplanet Exploration Program. The Gemini Observatory is operated by the Association of Universities for Research in Astronomy, under a cooperative agreement with the National Science Foundation (NSF) on behalf of the Gemini partnership: NSF (United States), the National Research Council (Canada), the Comision Nacional de Investigacion Cientifica y Tecnologica (Chile), the Australian Research Council (Australia), the Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and the Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). NR 37 TC 88 Z9 89 U1 28 U2 136 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 APR 18 PY 2014 VL 344 IS 6181 BP 277 EP 280 DI 10.1126/science.1249403 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AF1LD UT WOS:000334474500029 PM 24744370 ER PT J AU Barcelo, SJ Kim, A Gibson, GA Norris, KJ Yamakawa, M Li, ZY AF Barcelo, Steven J. Kim, Ansoon Gibson, Gary A. Norris, Kate J. Yamakawa, Mineo Li, Zhiyong TI Deterministic nanoparticle assemblies: from substrate to solution SO NANOTECHNOLOGY LA English DT Article DE nanoparticle; self-assembly; plasmonics; SERS; chemical sensing ID ENHANCED RAMAN-SCATTERING; LIVING MICE; GOLD; SURFACE; SPECTROSCOPY; NANOSTRUCTURES; ARRAYS; SILVER; JUNCTIONS; TRIMERS AB The deterministic assembly of metallic nanoparticles is an exciting field with many potential benefits. Many promising techniques have been developed, but challenges remain, particularly for the assembly of larger nanoparticles which often have more interesting plasmonic properties. Here we present a scalable process combining the strengths of top down and bottom up fabrication to generate deterministic 2D assemblies of metallic nanoparticles and demonstrate their stable transfer to solution. Scanning electron and high-resolution transmission electron microscopy studies of these assemblies suggested the formation of nanobridges between touching nanoparticles that hold them together so as to maintain the integrity of the assembly throughout the transfer process. The application of these nanoparticle assemblies as solution-based surface-enhanced Raman scattering (SERS) materials is demonstrated by trapping analyte molecules in the nanoparticle gaps during assembly, yielding uniformly high enhancement factors at all stages of the fabrication process. C1 [Barcelo, Steven J.; Gibson, Gary A.; Yamakawa, Mineo; Li, Zhiyong] Hewlett Packard Labs, Palo Alto, CA 94043 USA. [Kim, Ansoon] Korea Res Inst Stand & Sci, Taejon, South Korea. [Norris, Kate J.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. [Norris, Kate J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Barcelo, SJ (reprint author), Hewlett Packard Labs, Palo Alto, CA 94043 USA. EM Zhiyong.li@hp.com NR 45 TC 2 Z9 2 U1 6 U2 57 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 APR 18 PY 2014 VL 25 IS 15 AR 155302 DI 10.1088/0957-4484/25/15/155302 PG 6 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA AD6TN UT WOS:000333394100006 PM 24642827 ER PT J AU Franz, HB Kim, ST Farquhar, J Day, JMD Economos, RC McKeegan, KD Schmitt, AK Irving, AJ Hoek, J Dottin, J AF Franz, Heather B. Kim, Sang-Tae Farquhar, James Day, James M. D. Economos, Rita C. McKeegan, Kevin D. Schmitt, Axel K. Irving, Anthony J. Hoek, Joost Dottin, James, III TI Isotopic links between atmospheric chemistry and the deep sulphur cycle on Mars SO NATURE LA English DT Article ID MARTIAN METEORITE; MINERAL ASSEMBLAGES; LOS-ANGELES; PETROGENESIS; NAKHLITES; CHONDRITES; COMPONENTS; REGOLITH; ALH84001; SULFATE AB The geochemistry of Martian meteorites provides a wealth of information about the solid planet and the surface and atmospheric processes that occurred on Mars. The degree to which Martian magmas may have assimilated crustal material, thus altering the geochemical signatures acquired from their mantle sources, is unclear(1). This issue features prominently in efforts to understand whether the source of light rare-earth elements in enriched shergottites lies in crustal material incorporated into melts(1,2) or in mixing between enriched and depleted mantle reservoirs(3). Sulphur isotope systematics offer insight into some aspects of crustal assimilation. The presence of igneous sulphides in Martian meteorites with sulphur isotope signatures indicative of mass-independent fractionation suggests the assimilation of sulphur both during passage of magmas through the crust of Mars and at sites of emplacement. Here we report isotopic analyses of 40 Martian meteorites that represent more than half of the distinct known Martian meteorites, including 30 shergottites (28 plus 2 pairs, where pairs are separate fragments of a single meteorite), 8 nakhlites (5 plus 3 pairs), Allan Hills 84001 and Chassigny. Our data provide strong evidence that assimilation of sulphur into Martian magmas was a common occurrence throughout much of the planet's history. The signature of mass-independent fractionation observed also indicates that the atmospheric imprint of photochemical processing preserved in Martian meteoritic sulphide and sulphate is distinct from that observed in terrestrial analogues, suggesting fundamental differences between the dominant sulphur chemistry in the atmosphere of Mars and that in the atmosphere of Earth(4). C1 [Franz, Heather B.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Franz, Heather B.; Farquhar, James; Hoek, Joost; Dottin, James, III] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Franz, Heather B.; Farquhar, James; Hoek, Joost; Dottin, James, III] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Kim, Sang-Tae] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON L8S 4K1, Canada. [Day, James M. D.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Economos, Rita C.; McKeegan, Kevin D.; Schmitt, Axel K.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Irving, Anthony J.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. RP Franz, HB (reprint author), NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. EM heather.b.franz@nasa.gov RI McKeegan, Kevin/A-4107-2008; Kim, Sang-Tae/C-2768-2013; UCLA, SIMS/A-1459-2011; OI McKeegan, Kevin/0000-0002-1827-729X; Schmitt, Axel/0000-0002-9029-4211 FU US National Science Foundation Instrumentation and Facilities Program; NASA Cosmochemistry grants [NNX09AF72G, NNX13AL13G] FX We acknowledge the Meteorite Working Group, L. Welzenbach, T. McCoy, S. Ralew, M. N. Rao, L. Nyquist, J. Zipfel, C. Smith, H. Kojima, A. Treiman, T. Bunch and B. Zanda for providing meteorite samples analysed in this study. We also thank P. Piccoli for assistance with electron microprobe analyses. The manuscript benefited from independent reviews by M. Thiemens, P. Cartigny, S. Ono, D. Johnston and B. Wing during revision. The UCLA ion microprobe facility is partly supported by a grant from the US National Science Foundation Instrumentation and Facilities Program. This work was supported by NASA Cosmochemistry grants NNX09AF72G and NNX13AL13G to J.F. NR 38 TC 25 Z9 25 U1 5 U2 62 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 APR 17 PY 2014 VL 508 IS 7496 BP 364 EP + DI 10.1038/nature13175 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AF0KP UT WOS:000334403000045 PM 24740066 ER PT J AU Ackermann, M Ajello, M Albert, A Allafort, A Baldini, L Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Blandford, RD Bloom, ED Bonamente, E Bottacini, E Bouvier, A Brandt, TJ Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cecchi, C Charles, E Chaves, RCG Chekhtman, A Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S Dalton, M D'Ammando, F de Angelis, A de Palma, F Dermer, CD Digel, SW Di Venere, L Silva, EDE Drell, PS Drlica-Wagner, A Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Franckowiak, A Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Gomez-Vargas, GA Grenier, IA Grove, JE Guiriec, S Gustafsson, M Hadasch, D Hanabata, Y Harding, AK Hayashida, M Hayashi, K Hewitt, JW Horan, D Hou, X Hughes, RE Inoue, Y Jackson, MS Jogler, T Johannesson, G Johnson, AS Kamae, T Kawano, T Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Longo, F Loparco, F Lovellette, MN Lubrano, P Mayer, M Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nemmen, R Nuss, E Ohsugi, T Okumura, A Orienti, M Orlando, E Ormes, JF Paneque, D Panetta, JH Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Porter, TA Raino, S Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Ritz, S Roth, M Schaal, M Schulz, A Sgro, C Siskind, EJ Spandre, G Spinelli, P Strong, AW Takahashi, H Takeuchi, Y Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Torres, DF Tosti, G Troja, E Tronconi, V Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Werner, M Winer, BL Wood, KS Wood, M Yang, Z AF Ackermann, M. Ajello, M. Albert, A. Allafort, A. Baldini, L. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Blandford, R. D. Bloom, E. D. Bonamente, E. Bottacini, E. Bouvier, A. Brandt, T. J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cecchi, C. Charles, E. Chaves, R. C. G. Chekhtman, A. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. Dalton, M. D'Ammando, F. de Angelis, A. de Palma, F. Dermer, C. D. Digel, S. W. Di Venere, L. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Gomez-Vargas, G. A. Grenier, I. A. Grove, J. E. Guiriec, S. Gustafsson, M. Hadasch, D. Hanabata, Y. Harding, A. K. Hayashida, M. Hayashi, K. Hewitt, J. W. Horan, D. Hou, X. Hughes, R. E. Inoue, Y. Jackson, M. S. Jogler, T. Johannesson, G. Johnson, A. S. Kamae, T. Kawano, T. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Mayer, M. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nemmen, R. Nuss, E. Ohsugi, T. Okumura, A. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Porter, T. A. Raino, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Ritz, S. Roth, M. Schaal, M. Schulz, A. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Strong, A. W. Takahashi, H. Takeuchi, Y. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Tronconi, V. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Werner, M. Winer, B. L. Wood, K. S. Wood, M. Yang, Z. CA LAT Collaboration TI Inferred Cosmic-Ray Spectrum from Fermi Large Area Telescope gamma-Ray Observations of Earth's Limb SO PHYSICAL REVIEW LETTERS LA English DT Article ID ENERGY-SPECTRUM; HELIUM SPECTRA; EMISSION; GALAXY; ATMOSPHERE; PROTON; ALBEDO; MODEL; EGRET AB Recent accurate measurements of cosmic-ray (CR) species by ATIC-2, CREAM, and PAMELA reveal an unexpected hardening in the proton and He spectra above a few hundred GeV, a gradual softening of the spectra just below a few hundred GeV, and a harder spectrum of He compared to that of protons. These newly discovered features may offer a clue to the origin of high-energy CRs. We use the Fermi Large Area Telescope observations of the gamma-ray emission from Earth's limb for an indirect measurement of the local spectrum of CR protons in the energy range similar to 90 GeV-6 TeV (derived from a photon energy range 15 GeV-1 TeV). Our analysis shows that single power law and broken power law spectra fit the data equally well and yield a proton spectrum with index 2.68 +/- 0.04 and 2.61 +/- 0.08 above similar to 200 GeV, respectively. C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Albert, A.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Okumura, A.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, WW Hansen Expt Phys, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Albert, A.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Okumura, A.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.; Bellazzini, R.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.; Tronconi, V.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Bouvier, A.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Ritz, S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Brandt, T. J.; Ferrara, E. C.; Guiriec, S.; Harding, A. K.; Hewitt, J. W.; McEnery, J. E.; Nemmen, R.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brigida, M.; de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.] Consorzio Interuniv Fis Spaziale, I-10133 Turin, Italy. [Caraveo, P. A.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Ist Nazl Astrofis Osservatorio Astron Roma, I-00040 Rome, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univ & Particules Montpellier, CNRS, IN2P3, Montpellier, France. [Conrad, J.; Larsson, S.] Univ Stockholm, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.; Jackson, M. S.; Larsson, S.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden. [Conrad, J.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etudes Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Dalton, M.; Hou, X.; Mehault, J.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [D'Ammando, F.; Giroletti, M.; Orienti, M.] Univ Udine, Dipartmento Fis, I-33100 Udine, Italy. [D'Ammando, F.; Giroletti, M.; Orienti, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [de Angelis, A.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Dermer, C. D.; Drlica-Wagner, A.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Fukazawa, Y.; Kawano, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Gomez-Vargas, G. A.; Morselli, A.; Vitale, V.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. [Gomez-Vargas, G. A.] Univ Autonoma Madrid, Inst Fis Teor, IFT UAM CSIC, E-28049 Madrid, Spain. [Gomez-Vargas, G. A.] Univ Libre Bruxelles, Serv Phys Theor, B-1050 Brussels, Belgium. [Guiriec, S.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Guiriec, S.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Gustafsson, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] JAXA, Inst Space & Aeronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Hanabata, Y.; Hayashida, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA. [Hayashi, K.] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Hughes, R. E.; Winer, B. L.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Jackson, M. S.] CNRS, IRAP, F-31028 Toulouse 4, France. [Johannesson, G.] Univ Toulouse, GAHEC, UPS OMP, IRAP, F-31028 Toulouse, France. [Knoedlseder, J.] Univ Stockholm, Dept Astron, SE-10691 Stockholm, Sweden. [Knoedlseder, J.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Larsson, S.; McEnery, J. E.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Larsson, S.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Latronico, L.] Mahidol Univ, Fac Sci, Dept Phys, Bangkok 10400, Thailand. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Mitthumsiri, W.; Moiseev, A. A.] Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Mitthumsiri, W.; Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA. [Moiseev, A. A.; Nemmen, R.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Moiseev, A. A.; Nemmen, R.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Murgia, S.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Nemmen, R.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Okumura, A.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Ormes, J. F.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa. [Paneque, D.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Razzano, M.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Razzaque, S.] NYCB Real Time Comp Inc, New York, NY 11560 USA. [Roth, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Schaal, M.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Siskind, E. J.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain. [Strong, A. W.] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain. [Takeuchi, Y.] Univ Roma Tor Vergata, Dipartmento Fis, I-00133 Rome, Italy. RP Ackermann, M (reprint author), DESY, D-15738 Zeuthen, Germany. EM funk@slac.stanford.edu; warit.mit@mahidol.ac.th; imos@stanford.edu RI Di Venere, Leonardo/C-7619-2017; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; giglietto, nicola/I-8951-2012; Gomez-Vargas, German/C-7138-2015; Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; Orlando, E/R-5594-2016 OI Di Venere, Leonardo/0000-0003-0703-824X; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Torres, Diego/0000-0002-1522-9065; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; FU NASA [NNX11AQ06 G, NNX13AC47 G]; K.A. Wallenberg Foundation; Italian Ministry of Education, University and Research (MIUR) [FIRB-2012-RBFR12PM1 F] FX The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for both the development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is gratefully acknowledged. I. V. M. acknowledges support from NASA Grants No. NNX11AQ06 G and No. NNX13AC47 G. Royal Swedish Academy of Sciences Research Fellow J. Conrad, funded by a grant from the K.A. Wallenberg Foundation, NASA Postdoctoral Program Fellow S. Guiriec, USA. M. Razzano Funded by Contract No. FIRB-2012-RBFR12PM1 F from the Italian Ministry of Education, University and Research (MIUR). NR 33 TC 14 Z9 14 U1 2 U2 14 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 APR 17 PY 2014 VL 112 IS 15 AR 151103 DI 10.1103/PhysRevLett.112.151103 PG 7 WC Physics, Multidisciplinary SC Physics GA AF3FQ UT WOS:000334597300003 PM 24785023 ER PT J AU Li, Y Thompson, DWJ Stephens, GL Bony, S AF Li, Ying Thompson, David W. J. Stephens, Graeme L. Bony, Sandrine TI A global survey of the instantaneous linkages between cloud vertical structure and large-scale climate SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SEA-SURFACE TEMPERATURE; GENERAL-CIRCULATION MODEL; TROPICAL DEEP CONVECTION; EQUATORIAL PLANETARY-WAVES; BREWER-DOBSON CIRCULATION; 1998 EL-NINO; BOUNDARY-LAYER; ANNUAL CYCLE; A-TRAIN; MARINE STRATOCUMULUS C1 [Li, Ying; Thompson, David W. J.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Bony, Sandrine] Univ Paris 06, CNRS, Meteorol Dynam Lab, IPSL, Paris, France. RP Li, Y (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. EM yingli@atmos.colostate.edu RI Thompson, David/F-9627-2012; OI Bony, Sandrine/0000-0002-4791-4438 FU CloudSAT via NASA JPL; NSF Climate Dynamics program FX We are indebted to Bjorn Stevens, Mark Zelinka, and Robert Wood for providing comments and suggestions. We would also like to thank Hui Su and two anonymous referees for their thorough reviews and insightful comments, which have led to considerable improvement in this work. Y.L. is funded by CloudSAT via NASA JPL and the NSF Climate Dynamics program. DWJT is funded by the NSF Climate Dynamics program. NR 142 TC 16 Z9 16 U1 2 U2 26 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 16 PY 2014 VL 119 IS 7 BP 3770 EP 3792 DI 10.1002/2013JD020669 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF7PZ UT WOS:000334908300009 ER PT J AU Li, JLF Lee, WL Waliser, DE Neelin, JD Stachnik, JP Lee, T AF Li, J. -L. F. Lee, W. -L. Waliser, D. E. Neelin, J. David Stachnik, Justin P. Lee, Tong TI Cloud-precipitation-radiation-dynamics interaction in global climate models: A snow and radiation interaction sensitivity experiment SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID COMMUNITY ATMOSPHERE MODEL; IN-SITU; ECMWF; CIRCULATIONS; FEEDBACKS; SATELLITE; PACIFIC; SYSTEM; RADAR; OCEAN C1 [Li, J. -L. F.; Waliser, D. E.; Stachnik, Justin P.; Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Lee, W. -L.] Acad Sinica, RCEC, Taipei, Taiwan. [Neelin, J. David] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. RP Li, JLF (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Juilin.F.Li@jpl.nasa.gov RI Stachnik, Justin/A-5609-2015 FU NASA Making Earth System Data Records for Use in Research Environments (MEaSUREs); Earth Science Data Records Uncertainty (ESDR-ERR); NOAA [NA11OAR4310099]; National Aeronautics and Space Administration FX We thank Akio Arakawa at UCLA, Sun Won, Qing Yue, Seungwon Lee, Eric Fetzer, and Bin Guan at JPL as well as H.-H. Hsu at Academia Sinica, Taiwan, for useful comments. This work has been supported in part by the NASA Making Earth System Data Records for Use in Research Environments (MEaSUREs) and Earth Science Data Records Uncertainty (ESDR-ERR) programs and in part by the NOAA NA11OAR4310099 (J.D.N.). The contributions by D.E.W. and J.L.L. to this study were carried out on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 44 TC 9 Z9 9 U1 0 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 16 PY 2014 VL 119 IS 7 BP 3809 EP 3824 DI 10.1002/2013JD021038 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF7PZ UT WOS:000334908300011 ER PT J AU Shindell, D Racherla, P Milly, G AF Shindell, Drew Racherla, Pavan Milly, George TI Reply to comment by Laprise on "The added value to global model projections of climate change by dynamical downscaling: A case study over the continental U. S. using the GISS-ModelE2 and WRF models" SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article C1 [Shindell, Drew; Racherla, Pavan; Milly, George] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Shindell, D (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM drew.t.shindell@nasa.gov RI Shindell, Drew/D-4636-2012 NR 6 TC 2 Z9 2 U1 1 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 APR 16 PY 2014 VL 119 IS 7 BP 3882 EP 3885 DI 10.1002/2013JD020732 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF7PZ UT WOS:000334908300015 ER PT J AU Muhlbauer, A Ackerman, TP Comstock, JM Diskin, GS Evans, SM Lawson, RP Marchand, RT AF Muhlbauer, Andreas Ackerman, Thomas P. Comstock, Jennifer M. Diskin, Glenn S. Evans, Stuart M. Lawson, R. Paul Marchand, Roger T. TI Impact of large-scale dynamics on the microphysical properties of midlatitude cirrus SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CLOUD PARTICLE ENSEMBLES; RADAR OBSERVATIONS; ICE SUPERSATURATION; SPARTICUS CAMPAIGN; SIZE SPECTRA; A-TRAIN; AIRCRAFT; PARAMETERIZATIONS; CLIMATOLOGY; TEMPERATURE C1 [Muhlbauer, Andreas; Ackerman, Thomas P.] Univ Washington, Joint Inst Study Atmosphere & Oceans, Seattle, WA 98195 USA. [Ackerman, Thomas P.; Evans, Stuart M.; Marchand, Roger T.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Comstock, Jennifer M.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Diskin, Glenn S.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Lawson, R. Paul] Spec Inc, Boulder, CO USA. RP Muhlbauer, A (reprint author), Univ Washington, Joint Inst Study Atmosphere & Oceans, Seattle, WA 98195 USA. EM andreasm@atmos.washington.edu RI Muhlbauer, Andreas/A-4493-2015; OI Evans, Stuart/0000-0002-1873-0752 FU National Science Foundation (NSF) [1144017]; Joint Institute for the Study of the Atmosphere and Ocean (JISAO) under NOAA [NA10OAR4320148, 2138]; Department of Energy (DOE) Atmospheric Measurement Program FX Andreas Muhlbauer and Thomas P. Ackerman acknowledge funding received by the National Science Foundation (NSF) under grant 1144017. This publication is partially funded by the Joint Institute for the Study of the Atmosphere and Ocean (JISAO) under NOAA Cooperative Agreement NA10OAR4320148, Contribution 2138. Jennifer Comstock was supported by the Department of Energy (DOE) Atmospheric Measurement Program. We thank Ann M. Fridlind (NASA-GISS) for stimulating discussions on an earlier version of the manuscript and highly appreciate comments and suggestions from three anonymous reviewers that helped to improve the clarity and presentation of the manuscript. NR 60 TC 13 Z9 13 U1 0 U2 19 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 16 PY 2014 VL 119 IS 7 BP 3976 EP 3996 DI 10.1002/2013JD020035 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF7PZ UT WOS:000334908300021 ER PT J AU Li, J Carlson, BE Lacis, AA AF Li, Jing Carlson, Barbara E. Lacis, Andrew A. TI Application of spectral analysis techniques in the intercomparison of aerosol data: Part III. Using combined PCA to compare spatiotemporal variability of MODIS, MISR, and OMI aerosol optical depth SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SEA-SURFACE TEMPERATURE; RUSSIAN WILDFIRES; EASTERN FINLAND; AERONET; INSTRUMENT; PRODUCTS; TRENDS; INDIA; LAND; ENSO C1 [Li, Jing; Carlson, Barbara E.; Lacis, Andrew A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Li, Jing] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. RP Li, J (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM jl2862@columbia.edu FU NASA [509496.02.08.04.24] FX The authors would like to thank the MODIS, MISR, and OMI team for providing the AOD data used in this study. We thank the AERONET for providing the reference data. Thanks are also given to the anonymous reviewers for providing helpful comments and suggestions. The study is funded by NASA grant 509496.02.08.04.24. Jing Li is funded by the NASA Postdoctoral Program (NPP). NR 53 TC 10 Z9 10 U1 1 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 16 PY 2014 VL 119 IS 7 BP 4017 EP 4042 DI 10.1002/2013JD020538 PG 26 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF7PZ UT WOS:000334908300023 ER PT J AU Kiemle, C Kawa, SR Quatrevalet, M Browell, EV AF Kiemle, C. Kawa, S. R. Quatrevalet, M. Browell, E. V. TI Performance simulations for a spaceborne methane lidar mission SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ATMOSPHERIC CO2; MU-M; REFLECTANCE; SURFACE; COLUMN; SENSITIVITY; RETRIEVALS; VALIDATION; CH4 C1 [Kiemle, C.; Quatrevalet, M.] 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, Hampton, VA 23665 USA. RP Kiemle, C (reprint author), Deutsch Zentrum Luft & Raumfahrt DLR, Inst Phys Atmosphare, Oberpfaffenhofen, Germany. EM Christoph.Kiemle@dlr.de FU MERLIN scientific advisory group FX Valuable contributions to this work came from Sebastian Bretl (DLR) and from Jim Abshire and Clark Weaver (both NASA). We acknowledge the support of the MERLIN scientific advisory group headed by the principal investigators Gerhard Ehret (DLR) and Pierre Flamant (LMD). NR 28 TC 7 Z9 7 U1 0 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 16 PY 2014 VL 119 IS 7 BP 4365 EP 4379 DI 10.1002/2013JD021253 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF7PZ UT WOS:000334908300041 ER PT J AU Jaross, G Bhartia, PK Chen, G Kowitt, M Haken, M Chen, Z Xu, P Warner, J Kelly, T AF Jaross, Glen Bhartia, Pawan K. Chen, Grace Kowitt, Mark Haken, Michael Chen, Zhong Xu, Philippe Warner, Jeremy Kelly, Thomas TI OMPS Limb Profiler instrument performance assessment SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SCATTER MEASUREMENTS; OSIRIS INSTRUMENT; ODIN SATELLITE; O-3 PROFILES; SUITE OMPS; SCIAMACHY; RETRIEVAL; ALGORITHM; MISSION; SENSOR C1 [Jaross, Glen; Bhartia, Pawan K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chen, Grace; Kowitt, Mark; Haken, Michael; Chen, Zhong; Warner, Jeremy; Kelly, Thomas] Sci Syst & Applicat Inc, Lanham, MD USA. [Xu, Philippe] Sci Applicat Int Corp, Beltsville, MD USA. RP Jaross, G (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM glen.jaross@nasa.gov RI Bhartia, Pawan/A-4209-2016 OI Bhartia, Pawan/0000-0001-8307-9137 NR 26 TC 10 Z9 10 U1 0 U2 4 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 APR 16 PY 2014 VL 119 IS 7 BP 4399 EP 4412 DI 10.1002/2013JD020482 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF7PZ UT WOS:000334908300043 ER PT J AU Seftor, CJ Jaross, G Kowitt, M Haken, M Li, J Flynn, LE AF Seftor, C. J. Jaross, G. Kowitt, M. Haken, M. Li, J. Flynn, L. E. TI Postlaunch performance of the Suomi National Polar-orbiting Partnership Ozone Mapping and Profiler Suite (OMPS) nadir sensors SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID INSTRUMENT C1 [Seftor, C. J.; Kowitt, M.; Haken, M.; Li, J.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Jaross, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Flynn, L. E.] NOAA, College Pk, MD USA. RP Seftor, CJ (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM colin.seftor@ssaihq.com RI Flynn, Lawrence/B-6321-2009 OI Flynn, Lawrence/0000-0001-6856-2614 NR 19 TC 15 Z9 15 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 16 PY 2014 VL 119 IS 7 BP 4413 EP 4428 DI 10.1002/2013JD020472 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF7PZ UT WOS:000334908300044 ER PT J AU Zhao, H Li, X Blake, JB Fennell, JF Claudepierre, SG Baker, DN Jaynes, AN Malaspina, DM Kanekal, SG AF Zhao, H. Li, X. Blake, J. B. Fennell, J. F. Claudepierre, S. G. Baker, D. N. Jaynes, A. N. Malaspina, D. M. Kanekal, S. G. TI Peculiar pitch angle distribution of relativistic electrons in the inner radiation belt and slot region SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE pitch angle distribution; radiation belt electrons; inner radiation belt; slot region; plasmasphere; wave-particle interaction ID VAN-ALLEN BELT; SOLAR-WIND; MAGNETOSONIC WAVES; DIFFUSION; STORM; DST; MAGNETOSPHERE; PREDICTION; INDEXES; MODEL AB The relativistic electrons in the inner radiation belt have received little attention in the past due to sparse measurements and unforgiving contamination from the inner belt protons. The high-quality measurements of the Magnetic Electron Ion Spectrometer instrument onboard Van Allen Probes provide a great opportunity to investigate the dynamics of relativistic electrons in the low L region. In this letter, we report the newly unveiled pitch angle distribution (PAD) of the energetic electrons with minima at 90 degrees near the magnetic equator in the inner belt and slot region. Such a PAD is persistently present throughout the inner belt and appears in the slot region during storms. One hypothesis for 90 degrees minimum PADs is that off 90 degrees electrons are preferentially heated by chorus waves just outside the plasmapause (which can be at very low L during storms) and/or fast magnetosonic waves which exist both inside and outside the plasmasphere. Key Points Peculiar pitch angle distribution in the inner belt and slot region is reported Pitch angle distribution with minimum at 90 degrees persists in inner belt Chorus/fast magnetosonic wave heating is suggested as a possible mechanism C1 [Zhao, H.; Li, X.; Baker, D. N.; Jaynes, A. N.; Malaspina, D. M.] Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Zhao, H.; Li, X.] Univ Colorado Boulder, Dept Aerosp Engn Sci, Boulder, CO USA. [Blake, J. B.; Fennell, J. F.; Claudepierre, S. G.] Aerosp Corp, Los Angeles, CA 90009 USA. [Kanekal, S. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zhao, H (reprint author), Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. EM hong.zhao@colorado.edu FU NSF (CubeSat program) [AGSW 0940277]; NASA [NNX10AQ48G, NAS5-01072] FX We would like to thank Richard Selesnick and Mike Temerin, Lauren Blum, Quintin Schiller, and Sam Califf for helpful discussions. This work is mainly supported by NSF (CubeSat program) grant AGSW 0940277, NASA grant NNX10AQ48G, and NASA contract NAS5-01072 (Van Allen Probes mission). We thank the World Data Center for Geomagnetism, Kyoto, for providing Dst and AE indices. The predicted Dst and AE indices are available at http://lasp.colorado.edu/space_weather/dsttemerin/dsttemerin.html. NR 35 TC 17 Z9 18 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD APR 16 PY 2014 VL 41 IS 7 BP 2250 EP 2257 DI 10.1002/2014GL059725 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AF8RJ UT WOS:000334983000003 ER PT J AU Mazarico, E Barker, MK Neumann, GA Zuber, MT Smith, DE AF Mazarico, Erwan Barker, Michael K. Neumann, Gregory A. Zuber, Maria T. Smith, David E. TI Detection of the lunar body tide by the Lunar Orbiter Laser Altimeter SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Moon; tide; LOLA; crossover ID RECONNAISSANCE ORBITER; MISSION; GRAIL; MOON AB The Lunar Orbiter Laser Altimeter instrument onboard the Lunar Reconnaissance Orbiter spacecraft collected more than 5 billion measurements in the nominal 50km orbit over similar to 10,000 orbits. The data precision, geodetic accuracy, and spatial distribution enable two-dimensional crossovers to be used to infer relative radial position corrections between tracks to better than similar to 1m. We use nearly 500,000 altimetric crossovers to separate remaining high-frequency spacecraft trajectory errors from the periodic radial surface tidal deformation. The unusual sampling of the lunar body tide from polar lunar orbit limits the size of the typical differential signal expected at ground track intersections to similar to 10cm. Nevertheless, we reliably detect the topographic tidal signal and estimate the associated Love number h(2) to be 0.03710.0033, which is consistent with but lower than recent results from lunar laser ranging. C1 [Mazarico, Erwan; Zuber, Maria T.; Smith, David E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Mazarico, Erwan; Barker, Michael K.; Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Barker, Michael K.] Sigma Space, Lanham, MD USA. RP Mazarico, E (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM mazarico@mit.edu RI Mazarico, Erwan/N-6034-2014; Neumann, Gregory/I-5591-2013 OI Mazarico, Erwan/0000-0003-3456-427X; Neumann, Gregory/0000-0003-0644-9944 FU NASA [NNX09AM53G, NNG09HP18C] FX This work was supported by NASA grants NNX09AM53G and NNG09HP18C. We thank the LRO project and the LOLA Engineering and Science teams. We also thank T. Sabaka for his advice and assistance with the least squares inversion. The authors thank C.K. Shum and J.G. Williams for their constructive comments. NR 23 TC 10 Z9 10 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD APR 16 PY 2014 VL 41 IS 7 BP 2282 EP 2288 DI 10.1002/2013GL059085 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AF8RJ UT WOS:000334983000007 ER PT J AU Desai, SD Ray, RD AF Desai, Shailen D. Ray, Richard D. TI Consideration of tidal variations in the geocenter on satellite altimeter observations of ocean tides SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE ocean tides; geocenter; altimetry ID MISSION; EARTH; DEFORMATION; JASON-1 AB Tidal geocenter motion has been previously ignored when developing ocean tide models from satellite altimetry. Accounting for tidal geocenter motion is necessary because the best orbit determinations for altimetric satellites position sea-surface heights relative to the center of mass of the total Earth system, including the ocean tides. But the ocean tides are presumed relative to the Earth's crust and thus are effectively relative to the center of figure. By accounting for this effect, we find improved agreement between an altimeter-based ocean tide model and bottom pressure recorder observations. The variance of differences between these two observations is reduced by 31% and 43% for the two tidal constituents with the largest contributions to geocenter variations, O-1 and K-1, respectively. With this accommodation the predicted contribution from altimeter-based ocean tide models to geocenter variations is amplified by 15-22%, providing improved agreement with observations, especially for the K-1 component. Key Points Tidal geocenter motion impacts ocean tide observations from satellite altimetry Geocenter motion has been previously ignored in altimetric ocean tide solutions Consistency between models and observations markedly improved for K1 and O1 C1 [Desai, Shailen D.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Ray, Richard D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Desai, SD (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM shailen.desai@jpl.nasa.gov RI Ray, Richard/D-1034-2012 FU National Aeronautics and Space Administration; National Aeronautics and Space Administration's Ocean Surface Topography project FX The bottom-pressure-record data used in this study are available as supporting information to Ray [2013] at http://onlinelibrary.wiley.com/doi/10.1002/jgrc.20336/suppinfo. SDD performed the work described in this paper at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. RDR was supported by the National Aeronautics and Space Administration's Ocean Surface Topography project. NR 19 TC 3 Z9 3 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD APR 16 PY 2014 VL 41 IS 7 BP 2454 EP 2459 DI 10.1002/2014GL059614 PG 6 WC Geosciences, Multidisciplinary SC Geology GA AF8RJ UT WOS:000334983000029 ER PT J AU Mlynczak, MG Hunt, LA Mertens, CJ Marshall, BT Russell, JM Woods, T Thompson, RE Gordley, LL AF Mlynczak, Martin G. Hunt, Linda A. Mertens, Christopher J. Marshall, B. Thomas Russell, James M., III Woods, Thomas Thompson, R. Earl Gordley, Larry L. TI Influence of solar variability on the infrared radiative cooling of the thermosphere from 2002 to 2014 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE thermosphere; radiative cooling; solar cycle; carbon dioxide; nitric oxide ID NITRIC-OXIDE; SABER EXPERIMENT; STORMS; MESOSPHERE; EMISSION AB Infrared radiative cooling of the thermosphere by carbon dioxide (CO2, 15 mu m) and by nitric oxide (NO, 5.3 mu m) has been observed for 12years by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument on the Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics satellite. For the first time we present a record of the two most important thermospheric infrared cooling agents over a complete solar cycle. SABER has documented dramatic variability in the radiative cooling on time scales ranging from days to the 11 year solar cycle. Deep minima in global mean vertical profiles of radiative cooling are observed in 2008-2009. Current solar maximum conditions, evidenced in the rates of radiative cooling, are substantially weaker than prior maximum conditions in 2002-2003. The observed changes in thermospheric cooling correlate well with changes in solar ultraviolet irradiance and geomagnetic activity during the prior maximum conditions. NO and CO2 combine to emit 7x10(18) more Joules annually at solar maximum than at solar minimum. Key Points First record of thermospheric IR cooling rates over a complete solar cycle IR cooling in current solar maximum conditions much weaker than prior maximum Variability in thermospheric IR cooling observed on scale of days to 11 years C1 [Mlynczak, Martin G.; Mertens, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Hunt, Linda A.] SSAI, Hampton, VA USA. [Marshall, B. Thomas; Thompson, R. Earl; Gordley, Larry L.] G&A Tech Software, Newport News, VA USA. [Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. [Woods, Thomas] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Mlynczak, MG (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM m.g.mlynczak@nasa.gov FU NASATIMED project; NASA Living with a Star program FX The authors would like to thank the NASATIMED project and the NASA Living with a Star program for support. The data reported in this letter may be obtained directly by sending an email request to m.g.mlynczak@nasa.gov. NR 21 TC 7 Z9 7 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 APR 16 PY 2014 VL 41 IS 7 BP 2508 EP 2513 DI 10.1002/2014GL059556 PG 6 WC Geosciences, Multidisciplinary SC Geology GA AF8RJ UT WOS:000334983000037 ER PT J AU Durand, M Neal, J Rodriguez, E Andreadis, KM Smith, LC Yoon, Y AF Durand, Michael Neal, Jeffrey Rodriguez, Ernesto Andreadis, Konstantinos M. Smith, Laurence C. Yoon, Yeosang TI Estimating reach-averaged discharge for the River Severn from measurements of river water surface elevation and slope SO JOURNAL OF HYDROLOGY LA English DT Article DE River discharge; Remote sensing; Inverse methods; Open channels; Bayesian analysis ID DATA ASSIMILATION; INVERSE PROBLEM; FLOOD WAVE; PARAMETER; UNCERTAINTY; ROUGHNESS; AMAZON; STATE; OPTIMIZATION; INFORMATION AB An algorithm is presented that calculates a best estimate of river bathymetry, roughness coefficient, and discharge based on input measurements of river water surface elevation (h) and slope (S) using the Metropolis algorithm in a Bayesian Markov Chain Monte Carlo scheme, providing an inverse solution to the diffusive approximation to the shallow water equations. This algorithm has potential application to river Is and S measurements from the forthcoming Surface Water and Ocean Topography (SWOT) satellite mission. The algorithm was tested using in situ data as a proxy for satellite measurements along a 22.4 km reach of the River Severn, UK. First, the algorithm was run with gage measurements of h and S during a small, in-bank event in June 2007. Second, the algorithm was run with measurements of Is and S estimated from four remote sensing images during a major out-of-bank flood event in July 2007. River width was assumed to be known for both events. Algorithm-derived estimates of river bathymetry were validated using in situ measurements, and estimates of roughness coefficient were compared to those used in an operational hydraulic model. Algorithm-derived estimates of river discharge were evaluated using gaged discharge. For the in-bank event, when lateral inflows from smaller tributaries were assumed to be known, the method provided an accurate discharge estimate (10% RMSE). When lateral inflows were assumed unknown, discharge RMSE increased to 36%. Finally, if just one of the three river reaches was assumed to be have known bathymetry, solutions for bathymetry, roughness and discharge for all three reaches were accurately retrieved, with a corresponding discharge RMSE of 15.6%. For the out-of-bank flood event, the lateral inflows were unknown, and the final discharge RMSE was 19%. These results suggest that it should be possible to estimate river discharge via SWOT observations of river water surface elevation, slope and width. (c) 2014 Elsevier B.V. All rights reserved. C1 [Durand, Michael] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. [Durand, Michael] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA. [Neal, Jeffrey] Univ Bristol, Sch Geog Sci, Bristol, Avon, England. [Rodriguez, Ernesto; Andreadis, Konstantinos M.] CALTECH, Pasadena, CA 91011 USA. [Rodriguez, Ernesto; Andreadis, Konstantinos M.] NASA, Jet Prop Lab, Pasadena, CA 91011 USA. [Smith, Laurence C.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA. [Durand, Michael; Yoon, Yeosang] Ohio State Univ, Columbus, OH 43210 USA. RP Durand, M (reprint author), Ohio State Univ, 275 Mendenhall Lab,125 South Oval Mall, Columbus, OH 43210 USA. EM durand.8@osu.edu RI Neal, Jeffrey/C-8723-2009; Durand, Michael/D-2885-2013; Smith, Laurence/E-7785-2012 OI Neal, Jeffrey/0000-0001-5793-9594; Smith, Laurence/0000-0001-6866-5904 FU NASA Physical Oceanography Grant [NNX10AE96G] FX We thank the Environment Agency of England and Wales for providing river cross-section and gauging stations data. This work was supported by NASA Physical Oceanography Grant NNX10AE96G. Three anonymous reviewers helped improve the quality of the manuscript. NR 46 TC 27 Z9 28 U1 0 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 EI 1879-2707 J9 J HYDROL JI J. Hydrol. PD APR 16 PY 2014 VL 511 BP 92 EP 104 DI 10.1016/j.jhydrol.2013.12.050 PG 13 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA AG2VJ UT WOS:000335274900010 ER PT J AU Wang, K Day, JMD Korotev, RL Zeigler, RA Moynier, F AF Wang, Kun Day, James M. D. Korotev, Randy L. Zeigler, Ryan A. Moynier, Frederic TI Iron isotope fractionation during sulfide-rich felsic partial melting in early planetesimals SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE iron isotopes; GRA 06128/9; brachinites; brachinite-like achondrites; partial melting; sulfide melts ID EARLY SOLAR-SYSTEM; UNEQUILIBRATED ORDINARY CHONDRITES; PARENT-BODY; MAGMATIC DIFFERENTIATION; CONTINENTAL-CRUST; OSMIUM ISOTOPE; FE ISOTOPES; METEORITES; ORIGIN; ACCRETION AB New Fe isotope data of feldspar-rich meteorites Graves Nunataks 06128 and 06129 (GRA 06128/9) reveal that they are the only known examples of crustal materials with isotopically light Fe isotope compositions (delta Fe-66 = -0.08 +/- 0.06 parts per thousand; delta Fe-66 is defined as the per mule deviation of a sample's Fe-56/Fe-54 ratio from the IRMM-014 standard) in the Solar System. In contrast, associated brachinites, as well as brachinite-like achondrites, have Fe isotope compositions (delta Fe-56 = +0.01 +/- 0.02 parts per thousand) that are isotopically similar to carbonaceous chondrites and the bulk terrestrial mantle. In order to understand the cause of Fe isotope variations in the GRA 06128/9 and brachinite parent body, we also report the Fe isotope compositions of metal, silicate and sulfide fractions from three ordinary chondrites (Semarkona, Kernouve, Saint-Severin). Metals from ordinary chondrites are enriched in the heavier isotopes of Fe (average delta Fe-56 = 0.15 parts per thousand), sulfide fractions are enriched in the lighter isotopes of Fe (average delta Fe-56 = -0.14 parts per thousand), and the delta Fe-56 values of the silicates are coincident with that of the bulk rock (average delta Fe-56 = 0.03 parts per thousand). The enrichment of light isotopes of Fe isotopes in GRA 06128/9 is consistent with preferential melting of sulfides in precursor chondritic source materials leading to the formation of Fe-S-rich felsic melts. Conceptual models show that melt generation to form a GRA 06128/9 parental melt occurred prior to the onset of higher-temperature basaltic melting (<1200 degrees C) in a volatile-rich precursor and led to the generation of buoyant felsic melt with a strong Fe-S signature. These models not only reveal the origin of enrichment in light isotopes of Fe for GRA 06128/9, but are also consistent with petrological and geochemical observations, experimental studies for the origin of Fe-S-rich felsic melts, and for the cessation of early melting on some asteroidal parent bodies because of the effective removal of the major radioactive heat-source, Al-26. The mode of origin for GRA 06128/9 contrasts strongly with crust formation on Earth, the Moon. Mars and other asteroids, where mantle differentiation and/or oxygen activity are the major controls on crustal Fe isotope compositions. (C)2014 Elsevier B.V. All rights reserved. C1 [Wang, Kun; Korotev, Randy L.; Moynier, Frederic] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Wang, Kun; Korotev, Randy L.; Moynier, Frederic] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Day, James M. D.] Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, La Jolla, CA 92093 USA. [Zeigler, Ryan A.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate Acquisit, Houston, TX 77058 USA. [Moynier, Frederic] Univ Paris Diderot, Inst Phys Globe Paris, F-75238 Paris 05, France. RP Wang, K (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. EM kunwang@fas.harvard.edu FU NASA Earth and Space Science Fellowship [NNX12AL84H]; NASA Cosmochemistry program [NNX12AH70G, NNX12AH75G] FX Nicolas Dauphas is thanked for generously providing access to the MC-ICP-MS facility at the University of Chicago and Corliss K. Sio is thanked for assistance with analyses at the facility. This work was supported by the NASA Earth and Space Science Fellowship (NNX12AL84H to K.W.) and by funding from the NASA Cosmochemistry program (NNX12AH70G to F.M. and NNX12AH75G to J.M.D.D.). F.M. thanks a Chaire d'Excellence Sorbonne Paris Cite #IDEX13C445. Helen Williams and Paolo Sossi are thanked for their careful and constructive reviews and Tim Elliott is thanked for his thoughtful editorial handling. NR 65 TC 6 Z9 6 U1 3 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD APR 15 PY 2014 VL 392 BP 124 EP 132 DI 10.1016/j.epsl.2014.02.022 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CA8BI UT WOS:000349141100014 ER PT J AU Woodworth, AA Neudeck, PG Sayir, A Sola, F Dudley, M Raghothamachar, B AF Woodworth, A. A. Neudeck, P. G. Sayir, A. Sola, F. Dudley, M. Raghothamachar, B. TI Investigation of single crystal 4H-SiC growth by the Solvent-Laser Heated Floating Zone technique SO JOURNAL OF CRYSTAL GROWTH LA English DT Article DE X-ray diffraction; X-ray topography; Floating zone technique; Traveling solvent zone growth; Silicon carbide; Wide band gap semiconductor ID SILICON-CARBIDE; DEVICES; SI; TEMPERATURE; MECHANISM; LAYERS AB The Solvent-Laser Heated Floating Zone (solvent-LHFZ) growth technique has been implemented to grow long single crystal silicon carbide (SiC) fibers. This technique combines the long fiber growth ability of laser heated floating zone with crystal growth by traveling solvent method's ability to grow single crystal SiC. This paper presents a complete look at the initial SiC growth study by solvent-LtFZ. This study shows that solvent-LHFZ readily grows single crystal SiC, growth rates are a function of both growth temperature and carbon concentration in the crystal growth source material, solvent incorporation is a function of carbon concentration in the crystal growth source material, and that an ordered growth front must be achieved in order to grow a long single crystal SiC fiber. (C) 2014 Elsevier B.V. All rights reserved C1 [Woodworth, A. A.; Neudeck, P. G.; Sayir, A.; Sola, F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Dudley, M.; Raghothamachar, B.] SUNY Stony Brook, Dept Mat Sci & Engn, Stony Brook, NY 11794 USA. RP Woodworth, AA (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM andrew.a.woodworth@nasa.gov FU NASA Vehicle Systems Safety Technologies Project in the Aviation Safety Program; US Department of Energy Vehicle Technology Program via Space Act Agreement [SAA3-1048, DE-EE0001093/ 001]; Susan Rogers (DOE); U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-ACO298CH10886] FX NASA Postdoctoral Program Fellowship supported by NASA Vehicle Systems Safety Technologies Project in the Aviation Safety Program, US Department of Energy Vehicle Technology Program via Space Act Agreement (SAA3-1048) (DOE IA # DE-EE0001093/ 001) monitored by Susan Rogers (DOE). Use of the National Synchrotron Light Source, Brookhaven National Laboratoiy, was supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract no. DE-ACO298CH10886. Technical help from Fredric Dynys, David Spry and Andrew Trunek (NASA), J. Anthony Powell (Sest Inc.), Thomas Sabo (0AI/Case Western Reserve University), Michelle Mrdenovich-Hill and Beth Osborn (Sierra Lobo) and Charles Blaha (Jacobs Technologies) is gratefully acknowledged. NR 37 TC 2 Z9 2 U1 4 U2 21 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0248 EI 1873-5002 J9 J CRYST GROWTH JI J. Cryst. Growth PD APR 15 PY 2014 VL 392 BP 34 EP 40 DI 10.1016/j.jcrysgro.2013.12.050 PG 7 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA AG9WS UT WOS:000335771300006 ER PT J AU Peng, ZX Mahoney, JJ Vanderkluysen, L Hooper, PR AF Peng, Zhan X. Mahoney, John J. Vanderkluysen, Loyc Hooper, Peter R. TI Sr, Nd and Pb isotopic and chemical compositions of central Deccan Traps lavas and relation to southwestern Deccan stratigraphy SO JOURNAL OF ASIAN EARTH SCIENCES LA English DT Article DE Deccan Traps; Geochemistry; Large igneous provinces; Chemical stratigraphy ID FLOOD-BASALT PROVINCE; GEOCHEMICAL STRATIGRAPHY; INDIA; MAHABALESHWAR; FLOWS; ELEMENT; SECTION; GEOLOGY; ORIGIN; SYSTEM AB Sr, Nd and Pb isotopic compositions, and major and trace element abundances of lavas in five central Deccan Traps sections are generally very similar to those of lavas in the southwestern Deccan (Western Ghats escarpment). The combination of strong isotopic and chemical similarities between lavas of the two regions indicates that they shared a closely similar petrogenesis. Our results indicate that, unlike many lavas in the northeastern Deccan, most of the lavas studied in the central Deccan sections can be grouped into different stratigraphic members and chemical types (CTs) belonging to four formations (Thakurvadi, Bhimashankar, Khandala, and Poladpur) present in the type sections of the Western Ghats. Bhimashankar- and Thakurvadi-type lavas are found in a section near Outram, whereas only Khandala-type lavas make up the Mhaishmal, Ellora and Ajanta sections to the east, and only Poladpur-type lavas are present in the easternmost section at Lonar. This west-east sequence is the same as that seen going upward in the Western Ghats stratigraphy, except that Bushe-type lavas, which are located stratigraphically between the Khandala and Poladpur formations in the Western Ghats, have not been found in this study. Overall, our results indicate that the Khandala and Poladpur formations extend over west-east distances of more than 300 km, and some individual members (e.g., the Dhak Dongar) may extend over as much as 500 km. The regional dip from Igatpuri in the southwest to Lonar in the east-central Deccan is less than 0.5 degrees to the east, which is similar to the southward regional dip in the southwestern Deccan. Near-horizontal flows in the central and southwestern Deccan areas suggest that post-Deccan tectonic activity has had limited effects on the studied area. Large volumes of basaltic lavas derived from eruptive centers in the western Deccan may have covered both the central and southwestern Deccan areas. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Peng, Zhan X.] NASA, Lyndon B Johnson Space Ctr, Engn & Sci Contract Grp, Houston, TX 77058 USA. [Mahoney, John J.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. [Vanderkluysen, Loyc] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Hooper, Peter R.] Washington State Univ, Dept Geol, Pullman, WA 99162 USA. RP Peng, ZX (reprint author), NASA, Lyndon B Johnson Space Ctr, Engn & Sci Contract Grp, Houston, TX 77058 USA. EM zxpeng37@gmail.com; loyc@asu.edu OI Vanderkluysen, Loyc/0000-0001-8263-1604 FU U.S. National Science Foundation [EAR-8816192, EAR-9104897, EAR-9418168] FX We thank N. Chatterjee and M. Bodas for their careful reviews of the manuscript, and handling editor H. Sheth for his many helpful comments. We are grateful to K. Spencer for his help with laboratory work. ZXP and LV are forever grateful to co-authors J. Mahoney and P. Hooper, who were admirable teachers and mentors; we regret that they could not see this work to its completion and hope to honor their memory with the publication of this work. This study was funded by U.S. National Science Foundation grants EAR-8816192, EAR-9104897 and EAR-9418168. NR 47 TC 7 Z9 7 U1 2 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1367-9120 EI 1878-5786 J9 J ASIAN EARTH SCI JI J. Asian Earth Sci. PD APR 15 PY 2014 VL 84 SI SI BP 83 EP 94 DI 10.1016/j.jseaes.2013.10.025 PG 12 WC Geosciences, Multidisciplinary SC Geology GA AF1NW UT WOS:000334481600008 ER PT J AU Aponte, JC Tarozo, R Alexandre, MR Alexander, CMO Charnley, SB Hallmann, C Summons, RE Huang, YS AF Aponte, Jose C. Tarozo, Rafael Alexandre, Marcelo R. Alexander, Conel M. O'D. Charnley, Steven B. Hallmann, Christian Summons, Roger E. Huang, Yongsong TI Chirality of meteoritic free and IOM-derived monocarboxylic acids and implications for prebiotic organic synthesis SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID CIRCULARLY-POLARIZED-LIGHT; STAR-FORMATION REGIONS; AMINO-ACIDS; MURCHISON METEORITE; ASYMMETRIC AUTOCATALYSIS; CARBONACEOUS METEORITES; ENANTIOMERIC EXCESSES; MOLECULAR-WEIGHT; DENSE CLOUDS; HOMOCHIRALITY AB The origin of homochirality and its role in the development of life on Earth are among the most intriguing questions in science. It has been suggested that carbonaceous chondrites seeded primitive Earth with the initial organic compounds necessary for the origin of life. One of the strongest pieces of evidence supporting this theory is that certain amino acids in carbonaceous chondrites display a significant L-enantiomeric excess (ee), similar to those use by terrestrial life. Analyses of ee in meteoritic molecules other than amino acids would shed more light on the origins of homochirality. In this study we investigated the stereochemistry of two groups of compounds: (1) free monocarboxylic acids (MCAs) from CM2 meteorites LON 94101 and Murchison; and (2) the aliphatic side chains present in the insoluble organic matter (IOM) and extracted in the form of monocarboxylic acids (MCAs) from EET 87770 (CR2) and Orgueil (CI1). Contrary to the well-known ee observed for amino acids in meteorites, we found that meteoritic branched free and IOM-derived MCAs with 5-8 carbon atoms are essentially racemic. The racemic nature of these compounds is used to discuss the possible influence of ultraviolet circularly polarized light (UVCPL) and aqueous alterations on the parent body on chirality observed in in carbonaceous chondrites. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Aponte, Jose C.; Tarozo, Rafael; Huang, Yongsong] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Alexandre, Marcelo R.] Univ Fed Sergipe, Dept Quim, BR-49100000 Sao Cristovao, SE, Brazil. [Alexander, Conel M. O'D.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Charnley, Steven B.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Hallmann, Christian; Summons, Roger E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Hallmann, Christian] Max Planck Inst Biogeochem, D-28359 Bremen, Germany. [Hallmann, Christian] Univ Bremen, MARUM, D-28359 Bremen, Germany. RP Aponte, JC (reprint author), NASA, Goddard Space Flight Ctr, NASA Postdoctoral Program, Greenbelt, MD 20771 USA. EM jose.c.aponte@nasa.gov; yongsong_huang@brown.edu RI Alexander, Conel/N-7533-2013 OI Alexander, Conel/0000-0002-8558-1427 FU NSF; NASA; NASA Astrobiology and Exobiology Grant [NNX09AM82G]; Agouron Institute; NASA Astrobiology Institute [NNA08CN84A] FX US Antarctic meteorite samples are recovered by the Antarctic Search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated by the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Curation Office at NASA Johnson Space Center. This research was entirely supported by NASA Astrobiology and Exobiology Grant NNX09AM82G to YH. JCA is grateful to the NASA Postdoctoral Program Administered by Oak Ridge Associated Universities. RES and CH were supported by the Agouron Institute and the NASA Astrobiology Institute (NNA08CN84A). JCA and YH acknowledge Michel Nuevo for helpful discussions during preparation of the manuscript, and associate editor George Cooper and three anonymous reviewers for their valuable criticisms during the review process. NR 65 TC 11 Z9 11 U1 2 U2 33 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 APR 15 PY 2014 VL 131 BP 1 EP 12 DI 10.1016/j.gca.2014.01.035 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AD5YS UT WOS:000333330100001 ER PT J AU Danielski, C Deroo, P Waldmann, IP Hollis, MDJ Tinetti, G Swain, MR AF Danielski, C. Deroo, P. Waldmann, I. P. Hollis, M. D. J. Tinetti, G. Swain, M. R. TI 0.94-2.42 mu m GROUND-BASED TRANSMISSION SPECTRA OF THE HOT JUPITER HD-189733b SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; planets and satellites: atmospheres; planets and satellites: individual (HD-189733b); techniques: spectroscopic ID EXOPLANET HD 189733B; HUBBLE-SPACE-TELESCOPE; INFRARED-EMISSION-SPECTRUM; EXTRASOLAR PLANET; SPITZER OBSERVATIONS; WATER-ABSORPTION; ATMOSPHERIC HAZE; CARBON-MONOXIDE; ORBITAL MOTION; LINE LISTS AB We present here new transmission spectra of the hot Jupiter HD-189733b using the SpeX instrument on the NASA Infrared Telescope Facility. We obtained two nights of observations where we recorded the primary transit of the planet in the J, H, and K bands simultaneously, covering a spectral range from 0.94 to 2.42 mu m. We used Fourier analysis and other detrending techniques validated previously on other data sets to clean the data. We tested the statistical significance of our results by calculating the autocorrelation function, and we found that, after the detrending, autocorrelative noise is diminished at most frequencies. Additionally, we repeated our analysis on the out-of-transit data only, showing that the residual telluric contamination is well within the error bars. While these techniques are very efficient when multiple nights of observations are combined together, our results prove that even one good night of observations is enough to provide statistically meaningful data. Our observed spectra are consistent with space-based data recorded in the same wavelength interval by multiple instruments, indicating that ground-based facilities are becoming a viable and complementary option to spaceborne observatories. The best fit to the features in our data was obtained with water vapor. Our error bars are not small enough to address the presence of additional molecules; however, by combining the information contained in other data sets with our results, it is possible to explain all the available observations with a modeled atmospheric spectrum containing water vapor, methane, carbon monoxide, and hazes/clouds. C1 [Danielski, C.; Waldmann, I. P.; Hollis, M. D. J.; Tinetti, G.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Deroo, P.; Swain, M. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Danielski, C (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM camilla@star.ucl.ac.uk OI Hollis, Morgan/0000-0002-8058-9075 NR 59 TC 12 Z9 12 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 35 DI 10.1088/0004-637X/785/1/35 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300035 ER PT J AU Helgason, K Cappelluti, N Hasinger, G Kashlinsky, A Ricotti, M AF Helgason, K. Cappelluti, N. Hasinger, G. Kashlinsky, A. Ricotti, M. TI THE CONTRIBUTION OF z less than or similar to 6 SOURCES TO THE SPATIAL COHERENCE IN THE UNRESOLVED COSMIC NEAR-INFRARED AND X-RAY BACKGROUNDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; dark ages; reionization; first stars; diffuse radiation; large-scale structure of universe ID ACTIVE GALACTIC NUCLEI; HALO OCCUPATION DISTRIBUTION; QUASAR LUMINOSITY FUNCTION; STAR-FORMATION HISTORY; LARGE-SCALE STRUCTURE; POINT-SOURCE CATALOG; INTERGALACTIC MEDIUM; REDSHIFT SURVEY; THEORETICAL-MODELS; GALAXY POPULATION AB A spatial clustering signal has been established in Spitzer/IRAC measurements of the unresolved cosmic near-infrared background (CIB) out to large angular scales, similar to 1 degrees. This CIB signal, while significantly exceeding the contribution from the remaining known galaxies, was further found to be coherent at a highly statistically significant level with the unresolved soft cosmic X-ray background (CXB). This measurement probes the unresolved CXB to very faint source levels using deep near-IR source subtraction. We study contributions from extragalactic populations at low to intermediate redshifts to the measured positive cross-power signal of the CIB fluctuations with the CXB. We model the X-ray emission from active galactic nuclei (AGNs), normal galaxies, and hot gas residing in virialized structures, calculating their CXB contribution including their spatial coherence with all infrared emitting counterparts. We use a halo model framework to calculate the auto and cross-power spectra of the unresolved fluctuations based on the latest constraints of the halo occupation distribution and the biasing of AGNs, galaxies, and diffuse emission. At small angular scales (less than or similar to 1'), the 4.5 mu m versus 0.5-2 keV coherence can be explained by shot noise from galaxies and AGNs. However, at large angular scales (similar to 10'), we find that the net contribution from the modeled populations is only able to account for similar to 3% of the measured CIBxCXB cross-power. The discrepancy suggests that the CIBxCXB signal originates from the same unknown source population producing the CIB clustering signal out to similar to 1 degrees. C1 [Helgason, K.; Ricotti, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Helgason, K.; Kashlinsky, A.] NASA Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Cappelluti, N.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Cappelluti, N.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Hasinger, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Kashlinsky, A.] SSAI, Lanham, MD 20706 USA. RP Helgason, K (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM kari@astro.umd.edu OI Cappelluti, Nico/0000-0002-1697-186X FU NASA Headquarters under the NASA Earth and Space Sciences Fellowship Program [NNX11AO05H] FX K.H.acknowledges useful discussions with R.Arendt, A.Ferrara, B.Lehmer, and R.Mushotzky.This work was supported by NASA Headquarters under the NASA Earth and Space Sciences Fellowship Program Grant-NNX11AO05H. NR 79 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 38 DI 10.1088/0004-637X/785/1/38 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300038 ER PT J AU Jontof-Hutter, D Lissauer, JJ Rowe, JF Fabrycky, DC AF Jontof-Hutter, Daniel Lissauer, Jack J. Rowe, Jason F. Fabrycky, Daniel C. TI KEPLER-79'S LOW DENSITY PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (KOI-152, Kepler-79); techniques: photometric ID TRANSIT TIMING OBSERVATIONS; SUB-NEPTUNE EXOPLANETS; SUPER-EARTH; LIGHT-CURVE; ASTROPHYSICAL PARAMETERS; EXTRASOLAR PLANETS; HOT NEPTUNE; LOW-MASS; M DWARF; K STAR AB Kepler-79 (KOI-152) has four planetary candidates ranging in size from 3.5 to 7 times the size of the Earth, in a compact configuration with orbital periods near a 1: 2: 4: 6 chain of commensurability, from 13.5 to 81.1 days. All four planets exhibit transit timing variations with periods that are consistent with the distance of each planet to resonance with its neighbors. We perform a dynamical analysis of the system based on transit timing measurements over 1282 days of Kepler photometry. Stellar parameters are obtained using a combination of spectral classification and the stellar density constraints provided by light curve analysis and orbital eccentricity solutions from our dynamical study. Our models provide tight bounds on the masses of all four transiting bodies, demonstrating that they are planets and that they orbit the same star. All four of Kepler-79's transiting planets have low densities given their sizes, which is consistent with other studies of compact multiplanet transiting systems. The largest of the four, Kepler-79 d (KOI-152.01), has the lowest bulk density yet determined among sub-Saturn mass planets. C1 [Jontof-Hutter, Daniel; Lissauer, Jack J.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rowe, Jason F.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Jontof-Hutter, D (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Daniel.S.Jontof-Hutter@nasa.gov OI Fabrycky, Daniel/0000-0003-3750-0183 FU NASA Postdoctoral Program FX D.J. gratefully acknowledges the support of the NASA Postdoctoral Program and thanks Yanqin Wu for a helpful review. We also thank Billy Quarles and Bill Borucki for helpful discussions of this paper. NR 50 TC 35 Z9 35 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 APR 10 PY 2014 VL 785 IS 1 AR 15 DI 10.1088/0004-637X/785/1/15 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300015 ER PT J AU Lansbury, GB Alexander, DM Del Moro, A Gandhi, P Assef, RJ Stern, D Aird, J Ballantyne, DR Balokovic, M Bauer, FE Boggs, SE Brandt, WN Christensen, FE Craig, WW Elvis, M Grefenstette, BW Hailey, CJ Harrison, FA Hickox, RC Koss, M LaMassa, SM Luo, B Mullaney, JR Teng, SH Urry, CM Zhang, WW AF Lansbury, G. B. Alexander, D. M. Del Moro, A. Gandhi, P. Assef, R. J. Stern, D. Aird, J. Ballantyne, D. R. Balokovic, M. Bauer, F. E. Boggs, S. E. Brandt, W. N. Christensen, F. E. Craig, W. W. Elvis, M. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Hickox, R. C. Koss, M. LaMassa, S. M. Luo, B. Mullaney, J. R. Teng, S. H. Urry, C. M. Zhang, W. W. TI NuSTAR OBSERVATIONS OF HEAVILY OBSCURED QUASARS AT z similar to 0.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; HARD X-RAY; SEYFERT 2 GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; RESOLUTION SPECTRAL TEMPLATES; XMM-NEWTON OBSERVATIONS; COMPTON-THICK QUASARS; MU-M; TYPE-2 QUASARS AB We present NuSTAR hard X-ray observations of three Type 2 quasars at z approximate to 0.4-0.5, optically selected from the Sloan Digital Sky Survey. Although the quasars show evidence for being heavily obscured, Compton-thick systems on the basis of the 2-10 keV to [O III] luminosity ratio and multiwavelength diagnostics, their X-ray absorbing column densities (N-H) are poorly known. In this analysis, (1) we study X-ray emission at > 10 keV, where X-rays from the central black hole are relatively unabsorbed, in order to better constrain N-H. (2) We further characterize the physical properties of the sources through broad-band near-UV to mid-IR spectral energy distribution analyses. One of the quasars is detected with NuSTAR at > 8 keV with a no-source probability of < 0.1%, and its X-ray band ratio suggests near Compton-thick absorption with N-H greater than or similar to 5 Chi 10(23) cm(-2). The other two quasars are undetected, and have low X-ray to mid-IR luminosity ratios in both the low-energy (2-10 keV) and high-energy (10-40 keV) X-ray regimes that are consistent with extreme, Compton-thick absorption (N-H greater than or similar to 10(24) cm(-2)). We find that for quasars at z similar to 0.5, NuSTAR provides a significant improvement compared to lower energy (< 10 keV) Chandra and XMM-Newton observations alone, as higher column densities can now be directly constrained. C1 [Lansbury, G. B.; Alexander, D. M.; Del Moro, A.; Gandhi, P.; Aird, J.; Mullaney, J. R.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Assef, R. J.] Univ Diego Port, Nucl Astron Fac Ingn, Santiago, Chile. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ballantyne, D. R.] Georgia Inst Technol, Ctr Relativist Astrophys, Sch Phys, Atlanta, GA 30332 USA. [Balokovic, M.; Grefenstette, B. W.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 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. [Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Koss, M.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [LaMassa, S. M.; Urry, C. M.] Yale Univ, Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA. [Teng, S. H.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lansbury, GB (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. EM g.b.lansbury@durham.ac.uk RI Boggs, Steven/E-4170-2015; Koss, Michael/B-1585-2015; Brandt, William/N-2844-2015; OI Urry, Meg/0000-0002-0745-9792; Boggs, Steven/0000-0001-9567-4224; Koss, Michael/0000-0002-7998-9581; Brandt, William/0000-0002-0167-2453; Alexander, David/0000-0002-5896-6313 FU Science and Technology Facilities Council (STFC) [ST/K501979/1, ST/I001573/1, ST/J003697/1]; Leverhulme Trust; Gemini-CONICYT [32120009]; NSF AST [1008067]; International Fulbright Science and Technology Award; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024, Anillo ACT1101]; Caltech NuSTAR [44A-1092750]; NASA ADP [NNX10AC99G]; NASA ADAP [NNX12AE38G]; National Science Foundation [1211096]; Swiss National Science Foundation [PP00P2_ 138979/1]; NASA [NNG08FD60C]; National Aeronautics and Space Administration; ASI Science Data Center (ASDC, Italy); California Institute of Technology (USA) FX We acknowledge financial support from the Science and Technology Facilities Council (STFC) grants ST/K501979/1 (G.B.L.), ST/I001573/1 (D.M.A. and A.D.M.) and ST/J003697/1 (P.G.), the Leverhulme Trust (D.M.A. and J.R.M.), Gemini-CONICYT grant 32120009 (R.J.A.), NSF AST award 1008067 (D.R.B.), the International Fulbright Science and Technology Award (M.B.), Basal-CATA PFB-06/2007 (F.E.B.), CONICYT-Chile grant FONDECYT 1101024 (F.E.B.), CONICYT-Chile grant Anillo ACT1101 (F.E.B.), Caltech NuSTAR subcontract 44A-1092750 (W.N.B. and B.L.), NASA ADP grant NNX10AC99G (W.N.B.and B.L.), NASA ADAP award NNX12AE38G (R.C.H.), National Science Foundation grant 1211096 (R.C.H.), and Swiss National Science Foundation grant PP00P2_ 138979/1 (M.K.). We thank the referee for the constructive comments, which helped improve our study. This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). NR 88 TC 28 Z9 28 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 17 DI 10.1088/0004-637X/785/1/17 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300017 ER PT J AU Liu, Y Hoeksema, JT Bobra, M Hayashi, K Schuck, PW Sun, X AF Liu, Y. Hoeksema, J. T. Bobra, M. Hayashi, K. Schuck, P. W. Sun, X. TI MAGNETIC HELICITY IN EMERGING SOLAR ACTIVE REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: interior; Sun: magnetic fields; Sun: photosphere; sunspots ID ELECTRIC-CURRENT HELICITY; FORCE-FREE FIELDS; VECTOR MAGNETOGRAMS; FLUX TUBES; ENERGY; TWIST; SUN; INJECTION; CORONA; EVOLUTION AB Using vector magnetic field data from the Helioseismic and Magnetic Imager instrument aboard the Solar Dynamics Observatory, we study magnetic helicity injection into the corona in emerging active regions (ARs) and examine the hemispheric helicity rule. In every region studied, photospheric shearing motion contributes most of the helicity accumulated in the corona. In a sample of 28 emerging ARs, 17 follow the hemisphere rule (61% +/- 18% at a 95% confidence interval). Magnetic helicity and twist in 25 ARs (89% +/- 11%) have the same sign. The maximum magnetic twist, which depends on the size of an AR, is inferred in a sample of 23 emerging ARs with a bipolar magnetic field configuration. C1 [Liu, Y.; Hoeksema, J. T.; Bobra, M.; Hayashi, K.; Sun, X.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Schuck, P. W.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Liu, Y (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. RI Sun, Xudong/M-3245-2013 OI Sun, Xudong/0000-0003-4043-616X FU NASA to Stanford University [NAS5-02139]; Heliophysics Guest Investigators grant FX The authors thank the team members who have made great contributions to the Solar Dynamics Observatory mission and for their hard work. The authors thank the anonymous referee for comments and suggestions that improved this paper. This investigation was supported by NASA Contract NAS5-02139 (HMI) to Stanford University. This study was also supported by NASA's Living with a Star program grant and Heliophysics Guest Investigators grant. NR 51 TC 12 Z9 12 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 APR 10 PY 2014 VL 785 IS 1 AR 13 DI 10.1088/0004-637X/785/1/13 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300013 ER PT J AU Luna, M Knizhnik, K Muglach, K Karpen, J Gilbert, H Kucera, TA Uritsky, V AF Luna, M. Knizhnik, K. Muglach, K. Karpen, J. Gilbert, H. Kucera, T. A. Uritsky, V. TI OBSERVATIONS AND IMPLICATIONS OF LARGE-AMPLITUDE LONGITUDINAL OSCILLATIONS IN A SOLAR FILAMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : filaments, prominences; Sun : flares; Sun : oscillations ID MAGNETIC-STRUCTURE; PERIODIC MOTION; ACTIVE-REGION; POLAR CROWN; PROMINENCES; SDO/AIA; EVOLUTION; DYNAMICS; THREADS; CHANNEL AB On 2010 August 20, an energetic disturbance triggered large-amplitude longitudinal oscillations in a nearby filament. The triggering mechanism appears to be episodic jets connecting the energetic event with the filament threads. In the present work, we analyze this periodic motion in a large fraction of the filament to characterize the underlying physics of the oscillation as well as the filament properties. The results support our previous theoretical conclusions that the restoring force of large-amplitude longitudinal oscillations is solar gravity, and the damping mechanism is the ongoing accumulation of mass onto the oscillating threads. Based on our previous work, we used the fitted parameters to determine the magnitude and radius of curvature of the dipped magnetic field along the filament, as well as the mass accretion rate onto the filament threads. These derived properties are nearly uniform along the filament, indicating a remarkable degree of cohesiveness throughout the filament channel. Moreover, the estimated mass accretion rate implies that the footpoint heating responsible for the thread formation, according to the thermal nonequilibrium model, agrees with previous coronal heating estimates. We estimate the magnitude of the energy released in the nearby event by studying the dynamic response of the filament threads, and discuss the implications of our study for filament structure and heating. C1 [Luna, M.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Luna, M.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Knizhnik, K.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Knizhnik, K.; Muglach, K.; Karpen, J.; Gilbert, H.; Kucera, T. A.; Uritsky, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Muglach, K.] ARTEP Inc, Ellicott City, MD 21042 USA. [Uritsky, V.] Catholic Univ Amer, NASA GSFC, Greenbelt, MD 20771 USA. RP Luna, M (reprint author), Inst Astrofis Canarias, E-38200 Tenerife, Spain. OI Kucera, Therese/0000-0001-9632-447X FU Spanish Ministry of Economy [AYA2011-24808, CSD2007-00050]; NASA's Heliophysics LWS and SR programs; National Science Foundation [0962619]; LWS TRT Program; European Research Council [277829]; Catholic University of America FX M.L. gratefully acknowledges partial financial support by the Spanish Ministry of Economy through projects AYA2011-24808 and CSD2007-00050. This work contributes to the deliverables identified in FP7 European Research Council grant agreement 277829, "Magnetic Connectivity through the Solar Partially Ionized Atmosphere" (PI: E. Khomenko). K.K. acknowledges support for this work by a coop agreement between the Catholic University of America and NASA Goddard Space Flight Center, sponsored by NASA's Heliophysics LWS and SR programs. K.M. gratefully acknowledges funding from the National Science Foundation via grant # 0962619. SDO is a mission for NASA's Living With a Star program. H.G., J.K., and T.K. also thank the LWS TR&T Program for support. We also thank S. Antiochos, I. Arregui, A. Asensio-Ramos, J. L. Ballester, C. R. DeVore, A. D iaz, A. Lopez-Ariste, F. Moreno-Insertis, R. Oliver, D. Orozco-Suarez, and J. Terradas for helpful discussions and suggestions. NR 42 TC 17 Z9 17 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 79 DI 10.1088/0004-637X/785/1/79 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300079 ER PT J AU Nelson, T Chomiuk, L Roy, N Sokoloski, JL Mukai, K Krauss, MI Mioduszewski, AJ Rupen, MP Weston, J AF Nelson, Thomas Chomiuk, Laura Roy, Nirupam Sokoloski, J. L. Mukai, Koji Krauss, Miriam I. Mioduszewski, Amy J. Rupen, Michael P. Weston, Jennifer TI THE 2011 OUTBURST OF RECURRENT NOVA T PYX: RADIO OBSERVATIONS REVEAL THE EJECTA MASS AND HINT AT COMPLEX MASS LOSS SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; radio continuum : stars; stars : individual (T Pyxidis); white dwarfs ID CLASSICAL NOVAE; SPECTROSCOPIC EVOLUTION; CATACLYSMIC VARIABLES; MERLIN OBSERVATIONS; ORBITAL PERIOD; RS-OPHIUCHI; PYXIDIS; EMISSION; PHASE; SHELL AB Despite being the prototype of its class, T Pyx is arguably the most unusual and poorly understood recurrent nova. Here, we use radio observations from the Karl G. Jansky Very Large Array to trace the evolution of the ejecta over the course of the 2011 outburst of T Pyx. The radio emission is broadly consistent with thermal emission from the nova ejecta. However, the radio flux began rising surprisingly late in the outburst, indicating that the bulk of the radio- emitting material was either very cold, or expanding very slowly, for the first similar to 50 days of the outburst. Considering a plausible range of volume filling factors and geometries for the ejecta, we find that the high peak flux densities of the radio emission require a massive ejection of (1-30) Chi 10(-5) M-circle dot. This ejecta mass is much higher than the values normally associated with recurrent novae, and is more consistent with a nova on a white dwarf well below the Chandrasekhar limit. C1 [Nelson, Thomas] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Chomiuk, Laura] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Chomiuk, Laura; Roy, Nirupam; Krauss, Miriam I.; Mioduszewski, Amy J.; Rupen, Michael P.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Sokoloski, J. L.; Weston, Jennifer] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Mukai, Koji] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Mukai, Koji] CRESST, Greenbelt, MD 20771 USA. [Mukai, Koji] NASA GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA. RP Nelson, T (reprint author), Univ Minnesota, Sch Phys & Astron, 116 Church St SE, Minneapolis, MN 55455 USA. EM tnelson@physics.umn.edu FU National Science Foundation [AST-1217778] FX We are grateful to H. Uthas, R. Williams, M. Shara, J. Patterson, S. Starrfield, M. Kato and D. Prialnik for illuminating discussions, and to the anonymous referee for their feedback on this work. We thank NRAO for the generous allocation of director's discretionary time that made this work possible. We are also grateful to the VLA commissioning team, including J. McMullin, J. Wrobel, E. Momjian, L. Sjouwerman, and G. van Moorsel, for their assistance in the acquisition of this data set. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work was carried out while L. Chomiuk and N. Roy were Jansky Fellows of the National Radio Astronomy Observatory. J.L.S. and J.W. acknowledge support from the National Science Foundation through award AST-1217778. Finally, we acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. NR 64 TC 19 Z9 19 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 APR 10 PY 2014 VL 785 IS 1 AR 78 DI 10.1088/0004-637X/785/1/78 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300078 ER PT J AU Obenberger, KS Hartman, JM Taylor, GB Craig, J Dowell, J Helmboldt, JF Henning, PA Schinzel, FK Wilson, TL AF Obenberger, K. S. Hartman, J. M. Taylor, G. B. Craig, J. Dowell, J. Helmboldt, J. F. Henning, P. A. Schinzel, F. K. Wilson, T. L. TI LIMITS ON GAMMA-RAY BURST PROMPT RADIO EMISSION USING THE LWA1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst COLFAML; general ID BLACK-HOLE; SEARCH; PULSES; SKY; AFTERGLOWS; TELESCOPE; SPECTRUM; DENSITY; MISSION; SCALE AB As a backend to the first station of the Long Wavelength Array (LWA1), the Prototype All Sky Imager has been imaging the sky >-26 degrees declination during 34 gamma-ray bursts (GRBs) between 2012 January and 2013 May. Using this data, we were able to put the most stringent limits to date on prompt low-frequency emission from GRBs. While our limits depend on the zenith angle of the observed GRB, we estimate a 1 sigma rms sensitivity of 68, 65, and 70 Jy for 5 s integrations at 37.9, 52.0, and 74.0 MHz at zenith. These limits are relevant for pulses >= 5 s and are limited by dispersion smearing. For 5 s pulses, we are limited to dispersion measures (DMs) <= 220, 570, and 1600 pc cm(-3) for the frequencies above. For pulses lasting longer than 5 s, the DM limits increase linearly with the duration of the pulse. We also report two interesting transients, which are, as of yet, of unknown origin and are not coincident with any known GRBs. For general transients, we give rate density limits of <= 7.5 Chi 10(-3), 2.9 Chi 10(-2), and 1.4 Chi 10(-2) yr(-1) deg(-2) with pulse energy densities > 1.3 Chi 10(-22), 1.1 Chi 10(-22), and 1.4 Chi 10(-22) J m(-2) Hz(-1) and pulse widths of 5 s at the frequencies given above. C1 [Obenberger, K. S.; Taylor, G. B.; Craig, J.; Dowell, J.; Henning, P. A.; Schinzel, F. K.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Hartman, J. M.] NASA Jet Prop Lab, Pasadena, CA 91109 USA. [Helmboldt, J. F.; Wilson, T. L.] US Naval Res Lab, Washington, DC 20375 USA. RP Obenberger, KS (reprint author), Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. RI Helmboldt, Joseph/C-8105-2012 FU Office of Naval Research [N00014-07-C-0147]; National Science Foundation [AST-1139963, AST-1139974] FX Construction of the LWA1 has been supported by the Office of Naval Research under Contract N00014-07-C-0147. Support for operations and continuing development of the LWA1 is provided by the National Science Foundation under grants AST-1139963 and AST-1139974 of the University Radio Observatory program. NR 38 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 27 DI 10.1088/0004-637X/785/1/27 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300027 ER PT J AU Parchevsky, KV Zhao, J Hartlep, T Kosovichev, AG AF Parchevsky, K. V. Zhao, J. Hartlep, T. Kosovichev, A. G. TI VERIFICATION OF THE HELIOSEISMOLOGY TRAVEL-TIME MEASUREMENT TECHNIQUE AND THE INVERSION PROCEDURE FOR SOUND SPEED USING ARTIFICIAL DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun COLFAML; helioseismology; Sun COLFAML; oscillations; sunspots; waves ID ACOUSTIC-WAVE-FIELD; DISTANCE HELIOSEISMOLOGY; NUMERICAL SIMULATIONS; 3-DIMENSIONAL INVERSION; HOLOGRAPHY; SUNSPOTS; SUN; PERTURBATIONS; SENSITIVITY; FLOWS AB We performed three-dimensional numerical simulations of the solar surface acoustic wave field for the quiet Sun and for three models with different localized sound-speed perturbations in the interior with deep, shallow, and two-layer structures. We used the simulated data generated by two solar acoustics codes that employ the same standard solar model as a background model, but utilize different integration techniques and different models of stochastic wave excitation. Acoustic travel times were measured using a time-distance helioseismology technique, and compared with predictions from ray theory frequently used for helioseismic travel-time inversions. It is found that the measured travel-time shifts agree well with the helioseismic theory for sound-speed perturbations, and for the measurement procedure with and without phase-speed filtering of the oscillation signals. This testing verifies the whole measuring-filtering-inversion procedure for static sound-speed anomalies with small amplitude inside the Sun outside regions of strong magnetic field. It is shown that the phase-speed filtering, frequently used to extract specific wave packets and improve the signal-to-noise ratio, does not introduce significant systematic errors. Results of the sound-speed inversion procedure show good agreement with the perturbation models in all cases. Due to its smoothing nature, the inversion procedure may overestimate sound-speed variations in regions with sharp gradients of the sound-speed profile. C1 [Parchevsky, K. V.; Zhao, J.; Hartlep, T.; Kosovichev, A. G.] Stanford Univ, HEPL, Stanford, CA 94305 USA. [Hartlep, T.] NASA, Ames Res Ctr, BAER Inst, Mountain View, CA 94043 USA. [Kosovichev, A. G.] Big Bear Solar Observ, Big Bear City, CA 92314 USA. [Kosovichev, A. G.] New Jersey Inst Technol, Dept Phys, Newark, NJ 07102 USA. [Kosovichev, A. G.] Crimean Astrophys Observ, UA-98409 Nauchnyi, Crimea, Ukraine. RP Parchevsky, KV (reprint author), Stanford Univ, HEPL, Stanford, CA 94305 USA. EM akosovichev@solar.stanford.edu RI Zhao, Junwei/A-1177-2007; OI Hartlep, Thomas/0000-0002-5062-9507 FU NASA Living With a Star TR T program FX This work was partially supported by the NASA Living With a Star TR& T program. The numerical simulations were carried out using the NASA Ames Research Center and XSEDE computational resources. NR 32 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 APR 10 PY 2014 VL 785 IS 1 AR 40 DI 10.1088/0004-637X/785/1/40 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300040 ER PT J AU Pesnell, WD Bryans, P AF Pesnell, W. D. Bryans, P. TI THE TIME-DEPENDENT CHEMISTRY OF COMETARY DEBRIS IN THE SOLAR CORONA SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: general; comets: individual (C/2011 W3); Sun: corona; Sun: general ID EXTREME-ULTRAVIOLET EMISSION; SUN-GRAZING COMET; X-RAY; SUNGRAZING COMETS; ATOMIC DATABASE; MISSION; SOHO; SPECTRA; CHIANTI; LINES AB Recent improvements in solar observations have greatly progressed the study of sungrazing comets. They can now be imaged along the entirety of their perihelion passage through the solar atmosphere, revealing details of their composition and structure not measurable through previous observations in the less volatile region of the orbit further from the solar surface. Such comets are also unique probes of the solar atmosphere. The debris deposited by sungrazers is rapidly ionized and subsequently influenced by the ambient magnetic field. Measuring the spectral signature of the deposited material highlights the topology of the magnetic field and can reveal plasma parameters such as the electron temperature and density. Recovering these variables from the observable data requires a model of the interaction of the cometary species with the atmosphere through which they pass. The present paper offers such a model by considering the time-dependent chemistry of sublimated cometary species as they interact with the solar radiation field and coronal plasma. We expand on a previous simplified model by considering the fully time-dependent solutions of the emitting species' densities. To compare with observations, we consider a spherically symmetric expansion of the sublimated material into the corona and convert the time-dependent ion densities to radial profiles. Using emissivities from the CHIANTI database and plasma parameters derived from a magnetohydrodynamic simulation leads to a spatially dependent emission spectrum that can be directly compared with observations. We find our simulated spectra to be consistent with observation. C1 [Pesnell, W. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bryans, P.] NASA, ADNET Syst Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Pesnell, WD (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA. RI Pesnell, William/D-1062-2012 OI Pesnell, William/0000-0002-8306-2500 NR 32 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 APR 10 PY 2014 VL 785 IS 1 AR 50 DI 10.1088/0004-637X/785/1/50 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300050 ER PT J AU Revalski, M Nowak, D Wiita, PJ Wehrle, AE Unwin, SC AF Revalski, Mitchell Nowak, Dawid Wiita, Paul J. Wehrle, Ann E. Unwin, Stephen C. TI INVESTIGATING THE VARIABILITY OF ACTIVE GALACTIC NUCLEI USING COMBINED MULTI-QUARTER KEPLER DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: jets; galaxies: photometry; galaxies: Seyfert; quasars: general ID RAPID OPTICAL VARIABILITY; DAMPED RANDOM-WALK; MODELS; QUASARS AB We used photometry from the Kepler satellite to characterize the variability of four radio-loud active galactic nuclei (AGNs) on timescales from years to minutes. The Kepler satellite produced nearly continuous high precision data sets which provided better temporal coverage than possible with ground based observations. We have now accumulated 11 quarters of data, eight of which were reported in our previous paper. In addition to constructing power spectral densities (PSDs) and characterizing the variability of the last three quarters, we have linked together the individual quarters using a multiplicative scaling process, providing data sets spanning similar to 2.8 yr with >98% coverage at a 30 minute sampling rate. We compute PSDs on these connected data sets that yield power law slopes at low frequencies in the approximate range of -1.5 to -2.0, with white noise seen at higher frequencies. These PSDs are similar to those of both the individual quarters and to those of ground-based optical observations of other AGNs. We also have explored a PSD binning method intended to reduce a bias toward shallow slope fits by evenly distributing the points within the PSDs. This tends to steepen the computed PSD slopes, especially when the low frequencies are relatively poorly fit. We detected flares lasting several days in which the brightness increased by similar to 15%-20% in one object, as well a smaller flare in another. Two AGNs showed only small, similar to 1%-2%, fluctuations in brightness. C1 [Revalski, Mitchell; Nowak, Dawid; Wiita, Paul J.] Coll New Jersey, Dept Phys, Ewing, NJ 08628 USA. [Wehrle, Ann E.] Space Sci Inst, Boulder, CO 80301 USA. [Unwin, Stephen C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Revalski, M (reprint author), Coll New Jersey, Dept Phys, POB 7718, Ewing, NJ 08628 USA. EM revalsm1@tcnj.edu OI Wiita, Paul/0000-0002-1029-3746 FU NASA Kepler Guest Observer Program [NNX11B90G, NNX12AC83G]; Mentored Undergraduate Summer Experience (MUSE) Program at TCNJ; National Aeronautics and Space Administration FX We thank Victoria Calafut for assistance in developing original PSD codes and scripts. We are grateful to Paolo Di Lorenzo, Daniel Silano, and Daniel Sprague for developing codes and techniques used in Paper I that were also employed here. We thank Brandon Kelly for providing his DRW code and the anonymous referee for comments which improved the scope of this manuscript. We acknowledge support from the NASA Kepler Guest Observer Program through grants NNX11B90G and NNX12AC83G (PI: A.E.W.) and from the 2013 Mentored Undergraduate Summer Experience (MUSE) Program at TCNJ (PI: P.J.W.) during which most of this work was carried out. 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 24 TC 11 Z9 11 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 60 DI 10.1088/0004-637X/785/1/60 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300060 ER PT J AU Stacy, A Bromm, V AF Stacy, Athena Bromm, Volker TI THE FIRST STARS: A LOW-MASS FORMATION MODE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; dark ages, reionization, first stars; stars: formation; stars: Population III ID POPULATION-III STARS; EXTREMELY METAL-POOR; PRIMORDIAL STELLAR EVOLUTION; SUPERMASSIVE BLACK-HOLES; ASYMPTOTIC GIANT BRANCH; LAMBDA-CDM UNIVERSE; DARK-MATTER HALOES; SMALL-SCALE DYNAMO; HIGH-REDSHIFT; GALAXY FORMATION AB We perform numerical simulations of the growth of a Population III stellar system under photodissociating feedback. We start from cosmological initial conditions at z = 100, self-consistently following the formation of a minihalo at z = 15 and the subsequent collapse of its central gas to high densities. The simulations resolve scales as small as similar to 1 AU, corresponding to gas densities of 1016 cm(-3). Using sink particles to represent the growing protostars, we evolve the stellar system for the next 5000 yr. We find that this emerging stellar group accretes at an unusually low rate compared with minihalos which form at earlier times (z = 20-30), or with lower baryonic angular momentum. The stars in this unusual system will likely reach masses ranging from <1 M-circle dot to similar to 5 M-circle dot by the end of their main-sequence lifetimes, placing them in the mass range for which stars will undergo an asymptotic giant branch (AGB) phase. Based upon the simulation, we predict the rare existence of Population III stars that have survived to the present day and have been enriched by mass overflow from a previous AGB companion. C1 [Stacy, Athena] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stacy, Athena] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Bromm, Volker] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Bromm, Volker] Univ Texas Austin, Texas Cosmol Ctr, Austin, TX 78712 USA. RP Stacy, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM athena.stacy@berkeley.edu FU JWST Postdoctoral Fellowship through the NASA Postdoctoral Program (NPP); NASA through Astrophysics Theory and Fundamental Physics Program [NNX09AJ33G]; NSF [AST-1009928] FX The authors thank the anonymous referee who helped them improve this manuscript. A.S. is grateful for support from the JWST Postdoctoral Fellowship through the NASA Postdoctoral Program (NPP). V.B. acknowledges support from NASA through Astrophysics Theory and Fundamental Physics Program grant NNX09AJ33G and from NSF through grant AST-1009928. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 126 TC 30 Z9 30 U1 0 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 APR 10 PY 2014 VL 785 IS 1 AR 73 DI 10.1088/0004-637X/785/1/73 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300073 ER PT J AU Teng, SH Brandt, WN Harrison, FA Luo, B Alexander, DM Bauer, FE Boggs, SE Christensen, FE Comastri, A Craig, WW Fabian, AC Farrah, D Fiore, F Gandhi, P Grefenstette, BW Hailey, CJ Hickox, RC Madsen, KK Ptak, AF Rigby, JR Risaliti, G Saez, C Stern, D Veilleux, S Walton, DJ Wik, DR Zhang, WW AF Teng, Stacy H. Brandt, W. N. Harrison, F. A. Luo, B. Alexander, D. M. Bauer, F. E. Boggs, S. E. Christensen, F. E. Comastri, A. Craig, W. W. Fabian, A. C. Farrah, D. Fiore, F. Gandhi, P. Grefenstette, B. W. Hailey, C. J. Hickox, R. C. Madsen, K. K. Ptak, A. F. Rigby, J. R. Risaliti, G. Saez, C. Stern, D. Veilleux, S. Walton, D. J. Wik, D. R. Zhang, W. W. TI NuSTAR REVEALS AN INTRINSICALLY X-RAY WEAK BROAD ABSORPTION LINE QUASAR IN THE ULTRALUMINOUS INFRARED GALAXY MARKARIAN 231 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; quasars: individual (Mrk 231); X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; ADVECTION-DOMINATED ACCRETION; DIGITAL SKY SURVEY; XMM-NEWTON; SEYFERT-GALAXIES; CHANDRA SURVEY; EMISSION-LINE; LOCAL ULIRGS; ENERGY-DISTRIBUTIONS AB We present high-energy (3-30 keV) NuSTAR observations of the nearest quasar, the ultraluminous infrared galaxy (ULIRG) Markarian 231 (Mrk 231), supplemented with new and simultaneous low-energy (0.5-8 keV) data from Chandra. The source was detected, though at much fainter levels than previously reported, likely due to contamination in the large apertures of previous non-focusing hard X-ray telescopes. The full band (0.5-30 keV) X-ray spectrum suggests the active galactic nucleus (AGN) in Mrk 231 is absorbed by a patchy and Compton-thin (N-H similar to 1.2(-0.3)(+0.3) Chi 10(23) cm(-2)) column. The intrinsic X-ray luminosity (L0.5-30 keV similar to 1.0 Chi 10(43) erg s(-1)) is extremely weak relative to the bolometric luminosity where the 2-10 keV to bolometric luminosity ratio is similar to 0.03% compared to the typical values of 2%-15%. Additionally, Mrk 231 has a low X-ray-to-optical power law slope (alpha(OX) similar to -1.7). It is a local example of a low-ionization broad absorption line quasar that is intrinsically X-ray weak. The weak ionizing continuum may explain the lack of mid-infrared [O Iv], [Ne v], and [Ne vI] fine-structure emission lines which are present in sources with otherwise similar AGN properties. We argue that the intrinsic X-ray weakness may be a result of the super-Eddington accretion occurring in the nucleus of this ULIRG, and may also be naturally related to the powerful wind event seen in Mrk 231, a merger remnant escaping from its dusty cocoon. C1 [Teng, Stacy H.; Rigby, J. R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Harrison, F. A.; Grefenstette, B. W.; Madsen, K. K.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Alexander, D. M.; Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Comastri, A.] INAF Osserv Astron Bologna, I-40127 Bologna, Italy. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Fabian, A. C.] Inst Astron, Cambridge CB3 0HA, England. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Fiore, F.] Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Ptak, A. F.; Wik, D. R.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Risaliti, G.] INAF Osserv Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Veilleux, S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. RP Teng, SH (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. EM stacy.h.teng@nasa.gov RI Rigby, Jane/D-4588-2012; Boggs, Steven/E-4170-2015; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; OI Rigby, Jane/0000-0002-7627-6551; Boggs, Steven/0000-0001-9567-4224; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Risaliti, Guido/0000-0002-3556-977X; Alexander, David/0000-0002-5896-6313; Fiore, Fabrizio/0000-0002-4031-4157 FU NASA [NNG08FD60C]; California Institute of Technology; National Aeronautics and Space Administration; NuSTAR Data Analysis Software (NuSTARDAS); ASI Science Data Center (ASDC, Italy); California Institute of Technology (USA); ESA Member States; USA (NASA); Jet Propulsion Laboratory, Caltech; Jet Propulsion Laboratory, Caltech, under contract with NASA; NASA Postdoctoral Program (NPP) Fellowship; California Institute of Technology (Caltech) NuSTAR [44A-1092750]; NASA ADP [NNX10AC99G]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024, Anillo ACT1101]; ASI/INAF [I/037/12/0011/13]; STFC [ST/J003697/1] FX We are grateful to the anonymous referee for providing useful comments which improved our manuscript. We thank Wayne Baumgartner, Bret Lehmer, Richard Mushotzky, Jeremy Schnittman, Tahir Yaqoob, and Andreas Zezas for useful discussions. We would also like to thank Lee Armus who provided useful comments in the early planning phase of the NuSTAR ULIRG program. We also thank Roberto Maiolino, David Rupke, and Eckhard Sturm who are co-investigators of the Chandra program. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The scientific results reported in this article are based in part on observations made by the Chandra X-Ray Observatory and data obtained from the Chandra Data Archive published previously in cited articles. This work, in part, made use of observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). We made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, Caltech, under contract with NASA. S.H.T. is supported by a NASA Postdoctoral Program (NPP) Fellowship. W.N.B. and B.L. acknowledge support by California Institute of Technology (Caltech) NuSTAR subcontract 44A-1092750 and NASA ADP grant NNX10AC99G. F.E.B. acknowledges support from Basal-CATA (PFB-06/2007) and CONICYT-Chile (under grants FONDECYT 1101024 and Anillo ACT1101). A.C. acknowledges support from ASI/INAF grant I/037/12/0011/13. P.G. acknowledges support from STFC grant reference ST/J003697/1. NR 97 TC 34 Z9 34 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 19 DI 10.1088/0004-637X/785/1/19 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300019 ER PT J AU Tomsick, JA Gotthelf, EV Rahoui, F Assef, RJ Bauer, FE Bodaghee, A Boggs, SE Christensen, FE Craig, WW Fornasini, FM Grindlay, J Hailey, CJ Harrison, FA Krivonos, R Natalucci, L Stern, D Zhang, WW AF Tomsick, John A. Gotthelf, Eric V. Rahoui, Farid Assef, Roberto J. Bauer, Franz E. Bodaghee, Arash Boggs, Steven E. Christensen, Finn E. Craig, William W. Fornasini, Francesca M. Grindlay, Jonathan Hailey, Charles J. Harrison, Fiona A. Krivonos, Roman Natalucci, Lorenzo Stern, Daniel Zhang, William W. TI NuSTAR J163433-4738.7: A FAST X-RAY TRANSIENT IN THE GALACTIC PLANE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: stellar content; stars: variables: general; surveys; X-rays: individual NuSTAR J1634334738.7); X-rays: stars ID MILKY-WAY; BINARIES; SUPERFLARE; EVOLUTION; CATALOG; MISSION; GALAXY; SWIFT; FLARE; WIND AB During hard X-ray observations of the Norma spiral arm region by the Nuclear Spectroscopic Telescope Array (NuSTAR) in 2013 February, a new transient source, NuSTAR J163433-4738.7, was detected at a significance level of 8s in the 3-10 keV bandpass. The source is consistent with having a constant NuSTAR count rate over a period of 40 ks and is also detected simultaneously by Swift at lower significance. The source is not significantly detected by NuSTAR, Swift, or Chandra in the days before or weeks after the discovery of the transient, indicating that the strong X-ray activity lasted between similar to 0.5 and 1.5 days. Near-infrared imaging observations were carried out before and after the X-ray activity, but we are not able to identify the counterpart. The combined NuSTAR and Swift energy spectrum is consistent with a power law with a photon index of Gamma = 4.1(-1.0)(+1.5) (90% confidence errors), a blackbody with kT = 1.2 +/- 0.3 keV, or a Bremsstrahlung model with kT = 3.0(-1.2)(+2.1) keV. The reduced-chi(2) values for the three models are not significantly different, ranging from 1.23 to 1.44 for 8 degrees of freedom. The spectrum is strongly absorbed with N-Pi = (2.8(-1.4)(+2.3)) x 10(23) cm(-2), (9(-7)(+15)) x 10(22) cm(-2), and (1.7(-0.9)(+1.7)) x 10(23) cm(-2), for the power-law, blackbody, and Bremsstrahlung models, respectively. Although the high column density could be due to material local to the source, it is consistent with absorption from interstellar material along the line of sight at a distance of 11 kpc, which would indicate an X-ray luminosity >10(34) erg s(-1). Although we do not reach a definitive determination of the nature of NuSTAR J163433-4738.7, we suggest that it may be an unusually bright active binary or a magnetar. C1 [Tomsick, John A.; Bodaghee, Arash; Boggs, Steven E.; Craig, William W.; Fornasini, Francesca M.; Krivonos, Roman] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Gotthelf, Eric V.; Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Rahoui, Farid] European So Observ, D-85748 Garching, Germany. [Rahoui, Farid] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Assef, Roberto J.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. [Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 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. [Fornasini, Francesca M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Grindlay, Jonathan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Natalucci, Lorenzo] INAF IAPS, Ist Nazl Astrofis, I-00133 Rome, Italy. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tomsick, JA (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM jtomsick@ssl.berkeley.edu RI Boggs, Steven/E-4170-2015 OI Boggs, Steven/0000-0001-9567-4224 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; Gemini-CONICYT [32120009]; Basal-CATA [PFB-06/2007]; CONICYT-Chile through FONDECYT [1101024]; CONICYT-Chile through Gemini-CONICYT [32120003]; CONICYT-Chile through Anillo [ACT1101]; Italian Space Agency (ASI) by ASI/INAF grant [I/037/12/0-011/13] 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. The authors 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 (Italy) and the California Institute of Technology (USA). R.J.A. was supported by Gemini-CONICYT grant 32120009. F.E.B. was supported by Basal-CATA PFB-06/2007 and CONICYT-Chile (through FONDECYT 1101024, Gemini-CONICYT 32120003, and Anillo ACT1101). L.N. wishes to acknowledge the Italian Space Agency (ASI) for financial support by ASI/INAF grant I/037/12/0-011/13. The authors thank Harvey Tananbaum for providing Chandra Director's Discretionary Time for this project. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 36 TC 2 Z9 2 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 4 DI 10.1088/0004-637X/785/1/4 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300004 ER PT J AU Younes, G Kouveliotou, C van der Horst, AJ Baring, MG Granot, J Watts, AL Bhat, PN Collazzi, A Gehrels, N Gorgone, N Gogus, E Gruber, D Grunblatt, S Huppenkothen, D Kaneko, Y von Kienlin, A van der Klis, M Lin, L Mcenery, J van Putten, T Wijers, RAMJ AF Younes, G. Kouveliotou, C. van der Horst, A. J. Baring, M. G. Granot, J. Watts, A. L. Bhat, P. N. Collazzi, A. Gehrels, N. Gorgone, N. Gogus, E. Gruber, D. Grunblatt, S. Huppenkothen, D. Kaneko, Y. von Kienlin, A. van der Klis, M. Lin, L. Mcenery, J. van Putten, T. Wijers, R. A. M. J. TI TIME RESOLVED SPECTROSCOPY OF SGR J1550-5418 BURSTS DETECTED WITH FERMI/GAMMA-RAY BURST MONITOR SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : individual (SGR J1550-5418); stars : magnetars; X-rays : bursts ID SOFT GAMMA-REPEATERS; MAGNETIZED NEUTRON-STARS; PULSAR 1E 1547.0-5408; X-RAY; STATISTICAL PROPERTIES; 2009 OUTBURST; GIANT FLARES; SGR-1900+14; MAGNETARS; EMISSION AB We report on a time-resolved spectroscopy of the 63 brightest bursts of SGR J1550-5418, detected with the Fermi/Gamma-ray Burst Monitor during its 2008-2009 intense bursting episode. We performed spectral analysis down to 4 ms timescales to characterize the spectral evolution of the bursts. Using a Comptonized model, we find that the peak energy, E-peak, anti-correlates with flux, while the low-energy photon index remains constant at similar to-0.8 up to a flux limit F approximate to 10(-5) erg s(-1) cm(-2). Above this flux value, the E-peak-flux correlation changes sign, and the index positively correlates with the flux reaching similar to 1 at the highest fluxes. Using a two blackbody model, we find that the areas and fluxes of the two emitting regions correlate positively. Further, we study here for the first time the evolution of the temperatures and areas as a function of flux. We find that the area-kT relation follows the lines of constant luminosity at the lowest fluxes, R-2 proportional to kT(-4), with a break at the higher fluxes (F > 10(-5.5) erg s(-1) cm(-2)). The area of the high-kT component increases with the flux while its temperature decreases, which we interpret as being due to an adiabatic cooling process. The area of the low-kT component, on the other hand, appears to saturate at the highest fluxes, toward R-max approximate to 30 km. Assuming that crust quakes are responsible for soft gamma repeater (SGR) bursts and considering Rmax as the maximum radius of the emitting photon-pair plasma fireball, we relate this saturation radius to a minimum excitation radius of the magnetosphere, and we put a lower limit on the internal magnetic field of SGR J1550-5418, B-int greater than or similar to 4.5 Chi 10(15) G. C1 [Younes, G.] Univ Space Res Assoc, Huntsville, AL 35806 USA. [Younes, G.; Kouveliotou, C.] NSSTC, Huntsville, AL 35805 USA. [Kouveliotou, C.; Collazzi, A.] NASA, George C Marshall Space Flight Ctr, Astrophys Off, Huntsville, AL 35812 USA. [van der Horst, A. J.; Watts, A. L.; Huppenkothen, D.; van der Klis, M.; van Putten, T.; Wijers, R. A. M. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel. [Bhat, P. N.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA. [Gehrels, N.; Mcenery, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gogus, E.; Kaneko, Y.; Lin, L.] Sabanci Univ, TR-34956 Istanbul, Turkey. [Gruber, D.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Grunblatt, S.] Univ Hawaii Manoa, Honolulu, HI 96822 USA. RP Younes, G (reprint author), Univ Space Res Assoc, 6767 Old Madison Pike,Suite 450, Huntsville, AL 35806 USA. OI Wijers, Ralph/0000-0002-3101-1808 FU GBM/Magnetar Key Project (NASA) [NNH07ZDA001-GLAST]; NWO Vidi grant; European Research Council [247295] FX This publication is part of the GBM/Magnetar Key Project (NASA grant NNH07ZDA001-GLAST; PI: C. Kouveliotou). A.L.W. acknowledges support from an NWO Vidi grant. A.J.v.d.H. and R.A.M.J.W. acknowledge support from the European Research Council via Advanced Grant No. 247295. NR 67 TC 9 Z9 9 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 APR 10 PY 2014 VL 785 IS 1 AR 52 DI 10.1088/0004-637X/785/1/52 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300052 ER PT J AU Archambault, S Aune, T Behera, B Beilicke, M Benbow, W Berger, K Bird, R Biteau, J Bugaev, V Byrum, K Cardenzana, JV Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fleischhack, H Fortson, L Furniss, A Galante, N Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Johnson, CA Kaaret, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Kumar, S Lang, MJ Madhavan, AS Maier, G McCann, A Meagher, K Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Park, N Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Rajotte, J Reyes, LC Reynolds, PT Richards, GT Roache, E Sembroski, GH Shahinyan, K Staszak, D Telezhinsky, I Tucci, JV Tyler, J Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Weinstein, A Welsing, R Wilhelm, A Williams, DA Ackermann, M Ajello, M Albert, A Baldini, L Bastieri, D Bellazzini, R Bissaldi, E Bregeon, J Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cavazzuti, E Charles, E Chiang, J Ciprini, S Claus, R Cutini, S D'Ammando, F de Angelis, A de Palma, F Dermer, CD Digel, SW Di Venere, L Drell, PS Favuzzi, C Franckowiak, A Fusco, P Gargano, F Gasparrini, D Giglietto, N Giordano, F Giroletti, M Grenier, IA Guiriec, S Jogler, T Kuss, M Larsson, S Latronico, L Longo, F Loparco, F Lubrano, P Madejski, GM Mayer, M Mazziotta, MN Michelson, PF Mizuno, T Monzani, ME Morselli, A Murgia, S Nuss, E Ohsugi, T Ormes, JF Paneque, D Perkins, JS Piron, F Pivato, G Raino, S Razzano, M Reimer, A Reimer, O Ritz, S Schaal, M Sgro, C Siskind, EJ Spinelli, P Takahashi, H Tibaldo, L Tinivella, M Troja, E Vianello, G Werner, M Wood, M AF Archambault, S. Aune, T. Behera, B. Beilicke, M. Benbow, W. Berger, K. Bird, R. Biteau, J. Bugaev, V. Byrum, K. Cardenzana, J. V. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fleischhack, H. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Johnson, C. A. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Kumar, S. Lang, M. J. Madhavan, A. S. Maier, G. McCann, A. Meagher, K. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Rajotte, J. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Sembroski, G. H. Shahinyan, K. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Weinstein, A. Welsing, R. Wilhelm, A. Williams, D. A. Ackermann, M. Ajello, M. Albert, A. Baldini, L. Bastieri, D. Bellazzini, R. Bissaldi, E. Bregeon, J. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cavazzuti, E. Charles, E. Chiang, J. Ciprini, S. Claus, R. Cutini, S. D'Ammando, F. de Angelis, A. de Palma, F. Dermer, C. D. Digel, S. W. Di Venere, L. Drell, P. S. Favuzzi, C. Franckowiak, A. Fusco, P. Gargano, F. Gasparrini, D. Giglietto, N. Giordano, F. Giroletti, M. Grenier, I. A. Guiriec, S. Jogler, T. Kuss, M. Larsson, S. Latronico, L. Longo, F. Loparco, F. Lubrano, P. Madejski, G. M. Mayer, M. Mazziotta, M. N. Michelson, P. F. Mizuno, T. Monzani, M. E. Morselli, A. Murgia, S. Nuss, E. Ohsugi, T. Ormes, J. F. Paneque, D. Perkins, J. S. Piron, F. Pivato, G. Raino, S. Razzano, M. Reimer, A. Reimer, O. Ritz, S. Schaal, M. Sgro, C. Siskind, E. J. Spinelli, P. Takahashi, H. Tibaldo, L. Tinivella, M. Troja, E. Vianello, G. Werner, M. Wood, M. CA VERITAS Collaboration Fermi LAT Collaboration TI DEEP BROADBAND OBSERVATIONS OF THE DISTANT GAMMA-RAY BLAZAR PKS 1424+240 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE BL Lacertae objects: individual (PKS 1424+240)-cosmic background radiation; gamma rays: galaxies ID EXTRAGALACTIC BACKGROUND LIGHT; SPACE-TELESCOPE MISSION; LARGE-AREA TELESCOPE; ENERGY COSMIC-RAY; TEV BLAZARS; SPECTRA; REDSHIFT; ABSORPTION; RADIATION; UNIVERSE AB We present deep VERITAS observations of the blazar PKS 1424+240, along with contemporaneous Fermi Large Area Telescope, Swift X-ray Telescope, and Swift UV Optical Telescope data between 2009 February 19 and 2013 June 8. This blazar resides at a redshift of z >= 0.6035, displaying a significantly attenuated gamma-ray flux above 100 GeV due to photon absorption via pair-production with the extragalactic background light. We present more than 100 hr of VERITAS observations over three years, a multiwavelength light curve, and the contemporaneous spectral energy distributions. The source shows a higher flux of (2.1 +/- 0.3) x 10(-7) photons m(-2) s(-1) above 120 GeV in 2009 and 2011 as compared to the flux measured in 2013, corresponding to (1.02 +/- 0.08) x 10-7 photons m(-2) s(-1) above 120 GeV. The measured differential very high energy (VHE; E >= 100 GeV) spectral indices are Gamma = 3.8 +/- 0.3, 4.3 +/- 0.6 and 4.5 +/- 0.2 in 2009, 2011, and 2013, respectively. No significant spectral change across the observation epochs is detected. We find no evidence for variability at gamma-ray opacities of greater than tau = 2, where it is postulated that any variability would be small and occur on timescales longer than a year if hadronic cosmic-ray interactions with extragalactic photon fields provide a secondary VHE photon flux. The data cannot rule out such variability due to low statistics. C1 [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Aune, T.; Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Behera, B.; Chen, X.; Federici, S.; Fleischhack, H.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.; Wilhelm, A.] DESY, D-15738 Zeuthen, Germany. [Beilicke, M.; Bugaev, V.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Galante, N.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Biteau, J.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Biteau, J.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Byrum, K.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cardenzana, J. V.; Krennrich, F.; Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Federici, S.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Griffiths, S. T.; Kaaret, P.] Stanford Univ, SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Humensky, T. B.; Nieto, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kieda, D.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [McCann, A.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Moriarty, P.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Moriarty, P.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Park, N.; Wakely, S. P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Reyes, L. C.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Reynolds, P. T.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Furniss, A.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Ackermann, M.; Buehler, R.; Mayer, M.] DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Albert, A.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Franckowiak, A.; Jogler, T.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Reimer, A.; Reimer, O.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Albert, A.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Franckowiak, A.; Jogler, T.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Reimer, A.; Reimer, O.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.; Bellazzini, R.; Kuss, M.; Razzano, M.; Sgro, C.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bastieri, D.; Buson, S.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Pivato, G.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bissaldi, E.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Bissaldi, E.] Univ Trieste, I-34127 Trieste, Italy. [Bregeon, J.; Nuss, E.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France. [Caliandro, G. A.] CIFS, I-10133 Turin, Italy. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Rome, Italy. [D'Ammando, F.; Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Dermer, C. D.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Grenier, I. A.] Univ Paris Diderot, CNRS, CEA IRFU, CEA Saclay,Lab AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Guiriec, S.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Guiriec, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Larsson, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Larsson, S.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Latronico, L.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Longo, F.; Lubrano, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Lubrano, P.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Morselli, A.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA. [Murgia, S.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Ormes, J. F.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Razzano, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Razzano, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.; Werner, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Reimer, A.; Reimer, O.; Werner, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ritz, S.] Natl Acad Sci, Natl Res Council, Res Associate, Washington, DC 20001 USA. [Schaal, M.; Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. Univ Maryland, Dept Phys, College Pk, MD 20742 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Archambault, S (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM amy.furniss@gmail.com RI Reimer, Olaf/A-3117-2013; Bissaldi, Elisabetta/K-7911-2016; Di Venere, Leonardo/C-7619-2017; Morselli, Aldo/G-6769-2011; Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Sgro, Carmelo/K-3395-2016; OI Reimer, Olaf/0000-0001-6953-1385; Bissaldi, Elisabetta/0000-0001-9935-8106; Di Venere, Leonardo/0000-0003-0703-824X; Cui, Wei/0000-0002-6324-5772; Morselli, Aldo/0000-0002-7704-9553; Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Bastieri, Denis/0000-0002-6954-8862; Giroletti, Marcello/0000-0002-8657-8852; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the UK; NASA through the Space Telescope Science Institute [HST-GO-12863]; NASA [NAS 5-26555]; INAF in Italy; CNES in France FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution; by NSERC in Canada; by Science Foundation Ireland (SFI 10/RFP/AST2748); and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument.; Support for program HST-GO-12863 was provided by NASA, awarded through the Space Telescope Science Institute, operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555.; The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States; CEA/Irfu and IN2P3/CNRS in France; ASI and INFN in Italy; MEXT, KEK, and JAXA in Japan; and the K. A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. NR 50 TC 19 Z9 19 U1 1 U2 11 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 APR 10 PY 2014 VL 785 IS 1 AR L16 DI 10.1088/2041-8205/785/1/L16 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE9RA UT WOS:000334345000016 ER PT J AU Shields, AL Bitz, CM Meadows, VS Joshi, MM Robinson, TD AF Shields, Aomawa L. Bitz, Cecilia M. Meadows, Victoria S. Joshi, Manoj M. Robinson, Tyler D. TI SPECTRUM-DRIVEN PLANETARY DEGLACIATION DUE TO INCREASES IN STELLAR LUMINOSITY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrobiology; planetary systems; radiative transfer; stars: low-mass ID MAIN-SEQUENCE STARS; M-DWARF STARS; SNOWBALL EARTH; HABITABLE ZONE; ALBEDO FEEDBACK; EVOLUTION; SURFACE; CLIMATE; EXOPLANETS; MODEL AB Distant planets in globally ice-covered, "nowball," states may depend on increases in their host stars' luminosity to become hospitable for surface life. Using a general circulation model, we simulated the equilibrium climate response of a planet to a range of instellations from an F-, G-, or M-dwarf star. The range of instellation that permits both complete ice cover and at least partially ice-free climate states is a measure of the climate hysteresis that a planet can exhibit. An ice-covered planet with high climate hysteresis would show a higher resistance to the initial loss of surface ice coverage with increases in instellation, and abrupt, extreme ice loss once deglaciation begins. Our simulations indicate that the climate hysteresis depends sensitively on the host star spectral energy distribution. Under fixed CO2 conditions, a planet orbiting an M-dwarf star exhibits a smaller climate hysteresis, requiring smaller instellation to initiate deglaciation than planets orbiting hotter, brighter stars. This is due to the higher absorption of near-infrared radiation by ice on the surfaces and greenhouse gases and clouds in the atmosphere of an M-dwarf planet. Increases in atmospheric CO2 further lower the climate hysteresis, as M-dwarf snowball planets exhibit a larger radiative response than G-dwarf snowball planets for the same increase in CO2. For a smaller hysteresis, planets near the outer edge of the habitable zone will thaw earlier in their evolutionary history, and will experience a less abrupt transition out of global ice cover. C1 [Shields, Aomawa L.; Meadows, Victoria S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Shields, Aomawa L.; Meadows, Victoria S.] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA. [Bitz, Cecilia M.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Joshi, Manoj M.] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England. [Robinson, Tyler D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Shields, AL (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA. EM aomawa@astro.washington.edu RI Joshi, Manoj/C-1795-2008; Bitz, Cecilia/S-8423-2016; OI Joshi, Manoj/0000-0002-2948-2811; Bitz, Cecilia/0000-0002-9477-7499; Robinson, Tyler/0000-0002-3196-414X FU National Science Foundation [DGE-0718124, DGE-1256082]; National Aeronautics and Space Administration through the NASA Astrobiology Institute [NNH05ZDA001C] FX This material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under Grant Nos. DGE-0718124 and DGE-1256082. This work was performed as part of the NASA Astrobiology Institute's Virtual Planetary Laboratory Lead Team, supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement solicitation NNH05ZDA001C. We thank Dorian Abbot and Raymond Pierrehumbert for helpful insight on this work, and an anonymous reviewer for extremely helpful comments that greatly improved the Letter. NR 41 TC 11 Z9 11 U1 1 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 APR 10 PY 2014 VL 785 IS 1 AR L9 DI 10.1088/2041-8205/785/1/L9 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE9RA UT WOS:000334345000009 ER PT J AU Su, Y Gomory, P Veronig, A Temmer, M Wang, TJ Vanninathan, K Gan, WQ Li, YP AF Su, Yang Goemoery, Peter Veronig, Astrid Temmer, Manuela Wang, Tongjiang Vanninathan, Kamalam Gan, Weiqun Li, YouPing TI SOLAR MAGNETIZED TORNADOES: ROTATIONAL MOTION IN A TORNADO-LIKE PROMINENCE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: corona; Sun: filaments, prominences; Sun: UV radiation ID NEUTRAL HYDROGEN; VORTEX FLOWS; FILAMENTS; SPECTROMETER; ABSORPTION; HELICITY; FEATURES; THREADS; HINODE; FIELDS AB Su et al. proposed a new explanation for filament formation and eruption, where filament barbs are rotating magnetic structures driven by underlying vortices on the surface. Such structures have been noticed as tornado-like prominences when they appear above the limb. They may play a key role as the source of plasma and twist in filaments. However, no observations have successfully distinguished rotational motion of the magnetic structures in tornado-like prominences from other motions such as oscillation and counter-streaming plasma flows. Here we report evidence of rotational motions in a tornado-like prominence. The spectroscopic observations in two coronal lines were obtained from a specifically designed Hinode/EIS observing program. The data revealed the existence of both cold and million-degree-hot plasma in the prominence leg, supporting the so-called prominence-corona transition region. The opposite velocities at the two sides of the prominence and their persistent time evolution, together with the periodic motions evident in SDO/AIA dark structures, indicate a rotational motion of both cold and hot plasma with a speed of similar to 5 km s(-1). C1 [Su, Yang; Veronig, Astrid; Temmer, Manuela; Vanninathan, Kamalam] Graz Univ, Inst Phys, IGAM Kanzelhohe Observ, A-8010 Graz, Austria. [Goemoery, Peter] Slovak Acad Sci, Astron Inst, SK-05960 Tatranska Lomnica, Slovakia. [Wang, Tongjiang] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Wang, Tongjiang] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Solar Phys Lab, Greenbelt, MD 20771 USA. [Gan, Weiqun; Li, YouPing] Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Astron, Nanjing 210008, Jiangsu, Peoples R China. RP Su, Y (reprint author), Graz Univ, Inst Phys, IGAM Kanzelhohe Observ, Univ Pl 5, A-8010 Graz, Austria. EM yang.su@uni-graz.at RI Su, Yang/J-5381-2014; Veronig, Astrid/B-8422-2009; OI Temmer, Manuela/0000-0003-4867-7558 FU Osterreichischer Austauschdienst (OeAD); Slovak Research and Development Agency (SRDA) [SK 16/2013, SK-AT-0003-12]; Austrian Science Fund (FWF) [P24092-N16, V195-N16]; European Community [263086]; Science Grant Agency [VEGA 2/0108/12]; Slovak Research and Development Agency [APVV-0816-11]; NASA [NNX12AB34G, NNG11PL10A] FX The H alpha data was taken by the Solar Magnetic Activity Research Telescope (SMART) at Hida Observatory, Kyoto University. We downloaded the data from the SMART T1 Data Archive (http://www.hida.kyoto-u.ac.jp/SMART/T1.html). SDO is a mission for NASA's Living With a Star (LWS) Program. This work was supported by the project of the Osterreichischer Austauschdienst (OeAD) and the Slovak Research and Development Agency (SRDA) under grant Nos. SK 16/2013 and SK-AT-0003-12. Y.S., A. V., M. T., and K. V. acknowledge the Austrian Science Fund (FWF): P24092-N16 and V195-N16. Y.S. and A. V. also acknowledge the European Community Framework Programme 7, High Energy Solar Physics Data in Europe (HESPE), grant agreement No.: 263086. P. G. acknowledges the support from grant VEGA 2/0108/12 of the Science Grant Agency and from the project of the Slovak Research and Development Agency under the Contract No. APVV-0816-11. The work of T. W. was supported by NASA grant NNX12AB34G and the NASA cooperative agreement NNG11PL10A to CUA. Y.L. and W. G. acknowledge 11233008 from NNSFC and 2011CB811402 from MSTC. NR 30 TC 14 Z9 14 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 10 PY 2014 VL 785 IS 1 AR L2 DI 10.1088/2041-8205/785/1/L2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE9RA UT WOS:000334345000002 ER PT J AU Bauschlicher, CW Ricca, A AF Bauschlicher, Charles W., Jr. Ricca, Alessandra TI Loss of a C2H (n) fragment from pyrene and circumcoronene SO THEORETICAL CHEMISTRY ACCOUNTS LA English DT Article DE DFT; Polycyclic aromatic hydrocarbon; Loss of C2Hn ID POLYCYCLIC AROMATIC-HYDROCARBONS; REAXFF; DFTB AB Reactions at the edge of pyrene and circumcoronene are studied using the B3LYP approach in conjunction with the 4-31G and 6-31G** basis sets. The loss of a C2H (n) fragment from the edge of either molecule requires more than 7 eV, which is much larger than for the loss of an H atom. Some paths can be broken down into a series of less energetic steps, but this does not change the overall endothermicity of the process. The exception is a path where a hydrogen atom adds to pyrene or circumcoronene. The resulting molecule rearranges to have a side group, which is subsequently lost. This process has an overall endothermicity of only about 2.5 eV. This path is actually less endothermic than the loss of an H atom from the same species. C1 [Bauschlicher, Charles W., Jr.] NASA, Entry Syst & Technol Div, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ricca, Alessandra] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. RP Bauschlicher, CW (reprint author), NASA, Entry Syst & Technol Div, Ames Res Ctr, Mail Stop 230-3, Moffett Field, CA 94035 USA. EM Charles.W.Bauschlicher@nasa.gov FU NASA's Astrophysics Theory and Fundamental Physics (ATFP) program [NNX09AD18G] FX AR thanks NASA's Astrophysics Theory and Fundamental Physics (ATFP) (NNX09AD18G) program for its generous support of this work. NR 15 TC 1 Z9 1 U1 0 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1432-881X EI 1432-2234 J9 THEOR CHEM ACC JI Theor. Chem. Acc. PD APR 8 PY 2014 VL 133 IS 5 AR 1479 DI 10.1007/s00214-014-1479-4 PG 5 WC Chemistry, Physical SC Chemistry GA AF1BO UT WOS:000334449600001 ER PT J AU Guanter, L Zhang, YG Jung, M Joiner, J Voigt, M Berry, JA Frankenberg, C Huete, AR Zarco-Tejada, P Lee, JE Moran, MS Ponce-Campos, G Beer, C Camps-Valls, G Buchmann, N Gianelle, D Klumpp, K Cescatti, A Baker, JM Griffis, TJ AF Guanter, Luis Zhang, Yongguang Jung, Martin Joiner, Joanna Voigt, Maximilian Berry, Joseph A. Frankenberg, Christian Huete, Alfredo R. Zarco-Tejada, Pablo Lee, Jung-Eun Moran, M. Susan Ponce-Campos, Guillermo Beer, Christian Camps-Valls, Gustavo Buchmann, Nina Gianelle, Damiano Klumpp, Katja Cescatti, Alessandro Baker, John M. Griffis, Timothy J. TI Global and time-resolved monitoring of crop photosynthesis with chlorophyll fluorescence SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE crop productivity; carbon fluxes; Earth observation; carbon modeling; spaceborne spectroscopy ID SUN-INDUCED FLUORESCENCE; GROSS PRIMARY PRODUCTION; CARBON-DIOXIDE; CLIMATE; PRODUCTIVITY; SPACE; GOSAT; HEAT; AGRICULTURE; VARIABILITY AB Photosynthesis is the process by which plants harvest sunlight to produce sugars from carbon dioxide and water. It is the primary source of energy for all life on Earth; hence it is important to understand how this process responds to climate change and human impact. However, model-based estimates of gross primary production (GPP, output from photosynthesis) are highly uncertain, in particular over heavily managed agricultural areas. Recent advances in spectroscopy enable the space-based monitoring of sun-induced chlorophyll fluorescence (SIF) from terrestrial plants. Here we demonstrate that spaceborne SIF retrievals provide a direct measure of the GPP of cropland and grassland ecosystems. Such a strong link with crop photosynthesis is not evident for traditional remotely sensed vegetation indices, nor for more complex carbon cycle models. We use SIF observations to provide a global perspective on agricultural productivity. Our SIF-based crop GPP estimates are 50-75% higher than results from state-of-the-art carbon cycle models over, for example, the US Corn Belt and the Indo-Gangetic Plain, implying that current models severely underestimate the role of management. Our results indicate that SIF data can help us improve our global models for more accurate projections of agricultural productivity and climate impact on crop yields. Extension of our approach to other ecosystems, along with increased observational capabilities for SIF in the near future, holds the prospect of reducing uncertainties in the modeling of the current and future carbon cycle. C1 [Guanter, Luis; Zhang, Yongguang; Voigt, Maximilian] Free Univ Berlin, Inst Space Sci, D-12165 Berlin, Germany. [Jung, Martin] Max Planck Inst Biogeochem, Dept Biogeochem Syst, D-07745 Jena, Germany. [Joiner, Joanna] NASA, Lab Atmospher Chem & Dynam Code 614, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Berry, Joseph A.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Huete, Alfredo R.] Univ Technol Sydney, Plant Funct Biol & Climate Change Cluster, Sydney, NSW 2007, Australia. [Zarco-Tejada, Pablo] CSIC, Inst Agr Sostenible, Cordoba 14004, Spain. [Lee, Jung-Eun] Brown Univ, Providence, RI 02912 USA. [Moran, M. Susan; Ponce-Campos, Guillermo] ARS, USDA, Tucson, AZ 85719 USA. [Beer, Christian] Stockholm Univ, Dept Appl Environm Sci, S-10691 Stockholm, Sweden. [Beer, Christian] Stockholm Univ, Bolin Ctr Climate Res, S-10691 Stockholm, Sweden. [Camps-Valls, Gustavo] Univ Valencia, Image Proc Lab, Valencia 46980, Spain. [Buchmann, Nina] Eidgenossiche Tech Hsch Zurich, CH-8092 Zurich, Switzerland. [Gianelle, Damiano] Fdn Edmund Mach, Res & Innovat Ctr, Sustainable Agroecosyst & Bioresources Dept, I-38010 San Michele All Adige, Italy. [Klumpp, Katja] INRA, Grassland Ecosyst Res Unit, F-63122 Clermont Ferrand, France. [Cescatti, Alessandro] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-20127 Ispra, Italy. [Baker, John M.] ARS, USDA, St Paul, MN 55108 USA. [Griffis, Timothy J.] Univ Minnesota, Dept Soil Water & Climate, St Paul, MN 55108 USA. RP Guanter, L (reprint author), Free Univ Berlin, Inst Space Sci, D-12165 Berlin, Germany. EM luis.guanter@wew.fu-berlin.de RI Griffis, Timothy/A-5707-2011; Joiner, Joanna/D-6264-2012; Beer, Christian/D-2296-2013; Zarco-Tejada, Pablo J./A-6874-2012; Guanter, Luis/I-1588-2015; Buchmann, Nina/E-6095-2011; Gianelle, Damiano/G-9437-2011; Huete, Alfredo/C-1294-2008; Frankenberg, Christian/A-2944-2013 OI Zhang, Yongguang/0000-0001-8286-300X; Zarco-Tejada, Pablo J./0000-0003-1433-6165; Guanter, Luis/0000-0002-8389-5764; Gianelle, Damiano/0000-0001-7697-5793; Huete, Alfredo/0000-0003-2809-2376; Frankenberg, Christian/0000-0002-0546-5857 FU German Research Foundation; National Aeronautics and Space Administration (NASA) [NNH10DA001N]; NASA Soil Moisture Active Passive Science Definition Team [08-SMAPSDT08-0042]; W. M. Keck Foundation FX We thank T. Meyers (National Oceanic and Atmospheric Administration Air Resources Laboratory), D. Cook and R. Matamala (Argonne National Laboratory), A. Suyker ( University of Nebraska), C. Bernhofer (Technische Universitat Dresden), Z. Nagy (Szent Istvan University), M. Aubinet (Universite de Liege), W. Kutsch (Johann Heinrich von Thuenen Institut), and K. Schneider (University of Cologne) for kindly providing eddy covariance data. We acknowledge C. Monfreda (Arizona State University), P. H. Verburg (Vrije Universiteit University Amsterdam), and N. Ramankutty (McGill University) for the crop fraction and NPP data sets and/or advice on their use, Eumetsat for the GOME-2 data, the Trendy project for the process-based model runs, and the USDA NASS for their agricultural inventory data. We also thank the two anonymous reviewers and Dr. Asner for their valuable suggestions and comments. MODIS MOD17 GPP data were downloaded from the server of the Numerical Terradynamic Simulation Group at the University of Montana, MODIS MOD13 data were obtained from the MODIS Land Processes Distributed Active Archive Center archive, and MERIS-MTCI from the Infoterra Ltd server. This work used eddy covariance data acquired by AmeriFlux and GHG-Europe. The work by L. G., Y.Z., and M. V. has been funded by the Emmy Noether Programme (GlobFluo project) of the German Research Foundation. J.J. is supported by the National Aeronautics and Space Administration (NASA) Carbon Cycle Science program (NNH10DA001N) and G.P.-C. is supported by NASA Soil Moisture Active Passive Science Definition Team (08-SMAPSDT08-0042). We also thank the W. M. Keck Foundation for funding the New Methods to Measure Photosynthesis from Space workshop held at the Caltech Keck Institute for Space Studies. NR 43 TC 108 Z9 110 U1 19 U2 158 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 APR 8 PY 2014 VL 111 IS 14 BP E1327 EP E1333 DI 10.1073/pnas.1320008111 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AE4VU UT WOS:000333985200005 PM 24706867 ER PT J AU Ruffatto, D Parness, A Spenko, M AF Ruffatto, Donald, III Parness, Aaron Spenko, Matthew TI Improving controllable adhesion on both rough and smooth surfaces with a hybrid electrostatic/gecko-like adhesive SO JOURNAL OF THE ROYAL SOCIETY INTERFACE LA English DT Article DE adhesion; electrostatic; gecko; manipulation ID DIRECTIONAL ADHESION; DRY ADHESIVES; GECKO; ATTACHMENT; ROBOT AB This paper describes a novel, controllable adhesive that combines the benefits of electrostatic adhesives with gecko-like directional dry adhesives. When working in combination, the two technologies create a positive feedback cycle whose adhesion, depending on the surface type, is often greater than the sum of its parts. The directional dry adhesive brings the electrostatic adhesive closer to the surface, increasing its effect. Similarly, the electrostatic adhesion helps engage more of the directional dry adhesive fibrillar structures, particularly on rough surfaces. This paper presents the new hybrid adhesive's manufacturing process and compares its performance to three other adhesive technologies manufactured using a similar process: reinforced PDMS, electrostatic and directional dry adhesion. Tests were performed on a set of ceramic tiles with varying roughness to quantify its effect on shear adhesive force. The relative effectiveness of the hybrid adhesive increases as the surface roughness is increased. Experimental data are also presented for different substrate materials to demonstrate the enhanced performance achieved with the hybrid adhesive. Results show that the hybrid adhesive provides up to 5.1 x greater adhesion than the electrostatic adhesive or directional dry adhesive technologies alone. C1 [Ruffatto, Donald, III; Spenko, Matthew] IIT, Dept Mech Engn, Chicago, IL 60616 USA. [Parness, Aaron] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. RP Ruffatto, D (reprint author), IIT, Dept Mech Engn, Chicago, IL 60616 USA. EM druffatt@hawk.iit.edu FU ONR [N00014-10-1-0769]; NASA Office of the Chief Technologist's Space Technology Research Fellowship FX This work was supported by ONR grant no. N00014-10-1-0769 and a NASA Office of the Chief Technologist's Space Technology Research Fellowship. NR 49 TC 19 Z9 19 U1 5 U2 41 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1742-5689 EI 1742-5662 J9 J R SOC INTERFACE JI J. R. Soc. Interface PD APR 6 PY 2014 VL 11 IS 93 AR 20131089 DI 10.1098/rsif.2013.1089 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC2ZO UT WOS:000332385000013 PM 24451392 ER PT J AU Ma, WP Jacobs, G Gao, P Jermwongratanachai, T Shafer, WD Pendyala, VRR Yen, CH Klettlinger, JLS Davis, BH AF Ma, Wenping Jacobs, Gary Gao, Pei Jermwongratanachai, Thani Shafer, Wilson D. Pendyala, Venkat Ramana Rao Yen, Chia H. Klettlinger, Jennifer L. S. Davis, Burtron H. TI Fischer-Tropsch synthesis: Pore size and Zr promotional effects on the activity and selectivity of 25%Co/Al2O3 catalysts SO APPLIED CATALYSIS A-GENERAL LA English DT Article DE Fischer-Tropsch synthesis; Co/Al2O3; Cobalt; Zr; Hydrocarbon selectivity; XANES; EXAFS ID IN-SITU EXAFS; CARBON-MONOXIDE HYDROGENATION; ZIRCONIA-MODIFIED ALUMINA; SUPPORTED COBALT; CO/AL2O3 CATALYSTS; CO HYDROGENATION; REDUCTION; RHENIUM; REDUCIBILITY; OXIDATION AB The effects of pore size (10.8 and 25 nm) and zirconium loading (0-5%) on Fischer-Tropsch synthesis (FTS) performance of 25%Co/Al2O3 catalysts were systematically studied at a CO conversion level of similar to 50% under industrially relevant conditions. The catalysts were characterized by adsorption and X-ray spectroscopic techniques in order to understand the relationships between the catalyst physicochemical properties and the FTS performance parameters. Unpromoted wide pore 25%Co/Al2O3 displayed greater stability (CO% rate loss over 150 h of testing: 5.2 versus 27.6%) and 40% higher activity than the narrow pore catalyst. Addition of 1-5% Zr improved the initial activity of the 25%Co/Al2O3 catalysts by 25-71% regardless of support pore size, but the catalyst deactivation rates increased. The activity improvements by Zr for the wide pore and narrow pore catalysts are due to different reasons. XRD, hydrogen-chemisorption, and XANES results suggested that Zr primarily increased Co dispersion for the wide pore catalyst whereas it mainly increased Co reduction for the narrow pore catalysts. The smaller mean Co cluster size observed with the wide pore Co catalyst resulted from a relatively higher fraction of Co residing inside the pores as compared to the narrow pore catalyst. The unpromoted wide pore catalyst exhibited lower CH4 selectivity (5.9-6.3 versus 8.3-8.9%) and higher C5+ selectivity (88-89.2 versus 80-82%) compared with the narrow pore one. Zr addition decreased CH4 selectivity and increased C5+, selectivity for the narrow pore 25%Co/Al2O3 catalyst, but the opposite trend was observed with the wide pore Co catalyst. Explanations for the selectivity trends (including olefins and CO2) are provided based on the effects of Co size and location, and the resulting changes in H-2/CO mass transport within pores of the Co/Al2O3 catalysts with and without Zr promoter. (C) 2014 Elsevier B.V. All rights reserved. C1 [Ma, Wenping; Jacobs, Gary; Gao, Pei; Jermwongratanachai, Thani; Shafer, Wilson D.; Pendyala, Venkat Ramana Rao; Davis, Burtron H.] Univ Kentucky, Ctr Appl Energy Res, Lexington, KY 40511 USA. [Yen, Chia H.; Klettlinger, Jennifer L. S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Davis, BH (reprint author), Univ Kentucky, Ctr Appl Energy Res, 2540 Res Pk Dr, Lexington, KY 40511 USA. EM burtron.davis@uky.edu RI Jacobs, Gary/M-5349-2015 OI Jacobs, Gary/0000-0003-0691-6717 FU NASA [NNX11AI75A]; Commonwealth of Kentucky FX The authors thank NASA (Grant No. NNX11AI75A) and the Commonwealth of Kentucky for financial support for this research project. NR 43 TC 5 Z9 5 U1 4 U2 58 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0926-860X EI 1873-3875 J9 APPL CATAL A-GEN JI Appl. Catal. A-Gen. PD APR 5 PY 2014 VL 475 BP 314 EP 324 DI 10.1016/j.apcata.2014.01.016 PG 11 WC Chemistry, Physical; Environmental Sciences SC Chemistry; Environmental Sciences & Ecology GA AG7PP UT WOS:000335610400039 ER PT J AU Brekke, C Holt, B Jones, C Skrunes, S AF Brekke, Camilla Holt, Benjamin Jones, Cathleen Skrunes, Stine TI Discrimination of oil spills from newly formed sea ice by synthetic aperture radar SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Arctic oil spills; Sea ice; Emulsions; SAR; Polarimetry; Mixture modeling ID OF-THE-ART; SAR; SCATTERING; PARAMETERS; SATELLITE AB In this paper we examine the potential of multi-polarization SAR systems to detect and discriminate oil pollution from uncontaminated recently formed thin sea ice in the Arctic Ocean, where both oil and thin sea ice have similar low backscatter returns on SAR imagery. In this study, we present a theoretical model of the relative permittivity of oil-in-sea-ice mixtures and apply it to determine the effect of dielectric properties on the co-polarized backscatter ratio for sea ice, ocean, and oil. To support the theoretical discussion, we invstigate available multi-polarization and multi-frequency SAR measurements. We compare SAR data collected over oil spills in sea-water in the Gulf of Mexico and the North Sea with available similar data covering sea ice in the Arctic region. The results suggest that multi-polarization SAR systems will be useful to detect Arctic oil spills should a spill occur in new and young sea ice conditions, particularly in the marginal ice zones adjacent to the main polar ice pack. (c) 2014 Elsevier Inc. All rights reserved. C1 [Brekke, Camilla; Skrunes, Stine] UiT Arctic Univ Norway, Dept Phys & Technol, Tromso, Norway. [Holt, Benjamin; Jones, Cathleen] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Brekke, C (reprint author), UiT Arctic Univ Norway, Dept Phys & Technol, Tromso, Norway. EM camilla.brekke@uit.no FU NSC/KSAT; AIRSAR and UAVSAR data are courtesy of NASA/JPL-Caltech; Jet Propulsion Laboratory, California Institute of Technology FX The Radarsat-2 data is provided by NSC/KSAT under the NorwegianCanadian Radarsat agreement 2011. The AIRSAR and UAVSAR data are courtesy of NASA/JPL-Caltech. This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 64 TC 10 Z9 10 U1 2 U2 27 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 APR 5 PY 2014 VL 145 BP 1 EP 14 DI 10.1016/j.rse.2014.01.015 PG 14 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AG0NW UT WOS:000335113200001 ER PT J AU Kuusinen, N Tomppo, E Shuai, Y Berninger, F AF Kuusinen, Nea Tomppo, Erkki Shuai, Yanmin Berninger, Frank TI Effects of forest age on albedo in boreal forests estimated from MODIS and Landsat albedo retrievals SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Albedo; Boreal forest; Forest age; Linear unmixing; MODIS; Landsat ID BROAD-BAND CONVERSIONS; CONIFEROUS FOREST; SURFACE ALBEDO; BIDIRECTIONAL REFLECTANCE; THEMATIC MAPPER; BRDF MODELS; NARROW-BAND; IN-SITU; SNOW; BALANCE AB The relationship between boreal forest age and albedo in the visible, near-infrared and shortwave broadband was studied using MODIS and Landsat albedo retrievals and forest resource maps. The dependency of forest albedo on stand age was estimated from MODIS albedo retrievals using a linear unmixing approach combined with nonlinear regression. Exponential function was appropriate to describe the decline of coniferous forest albedo with stand age in all seasons and the decline of deciduous broadleaved albedo in winter. The effect of stand age on albedo was stronger for spruce than for pine, and the variation in albedo as a function of stand age was larger in winter than in summer for all species and wavelength regions. When applied to the test data, the albedo values predicted using the estimated age dependent albedo functions produced somewhat better results than when using only the species specific mean albedos as predictors. The tendency of the albedo values predicted using the age dependent functions towards the mean of the observed values suggested that the models did not cover all variation in the species specific forest albedos. A larger variation in the predicted albedos was obtained when age dependent albedo functions were estimated using Landsat albedo estimates. (c) 2014 Elsevier Inc All rights reserved. C1 [Kuusinen, Nea; Berninger, Frank] Univ Helsinki, Dept Forest Sci, FIN-00014 Helsinki, Finland. [Tomppo, Erkki] Finnish Forest Res Inst, Vantaa 01301, Finland. [Shuai, Yanmin] NASA, Goddard Space Flight Ctr, ERT Inc, Greenbelt, MD 20771 USA. RP Kuusinen, N (reprint author), Univ Helsinki, Dept Forest Sci, POB 27, FIN-00014 Helsinki, Finland. EM nea.j.kuusinen@helsinki.fi OI Berninger, Frank/0000-0001-7718-1661 FU Helsinki University Centre for Environment (HENVI); Center of Excellence in Physics, Chemistry, Biology and Meteorology of Atmospheric Composition and Climate Change of the Academy of Finland; Nordic Centre of Excellence: Cryosphere-Atmosphere Interactions in a Changing Arctic Climate (CRAICC) FX The study was funded by the Helsinki University Centre for Environment (HENVI), the Center of Excellence in Physics, Chemistry, Biology and Meteorology of Atmospheric Composition and Climate Change of the Academy of Finland and the Nordic Centre of Excellence: Cryosphere-Atmosphere Interactions in a Changing Arctic Climate (CRAICC). We also thank an anonymous reviewer for useful suggestions for the manuscript NR 48 TC 13 Z9 13 U1 2 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 APR 5 PY 2014 VL 145 BP 145 EP 153 DI 10.1016/jsse.2014.02.005 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AG0NW UT WOS:000335113200013 ER PT J AU Roy, DP Wulder, MA Loveland, TR Woodcock, CE Allen, RG Anderson, MC Helder, D Irons, JR Johnson, DM Kennedy, R Scambos, T Schaaf, CB Schott, JR Sheng, Y Vermote, EF Belward, AS Bindschadler, R Cohen, WB Gao, F Hipple, JD Hostert, P Huntington, J Justice, CO Kilic, A Kovalskyy, V Lee, ZP Lymbumer, L Masek, JG McCorkel, J Shuai, Y Trezza, R Vogelmann, J Wynne, RH Zhu, Z AF Roy, D. P. Wulder, M. A. Loveland, T. R. Woodcock, C. E. Allen, R. G. Anderson, M. C. Helder, D. Irons, J. R. Johnson, D. M. Kennedy, R. Scambos, Ta. Schaaf, C. B. Schott, J. R. Sheng, Y. Vermote, E. F. Belward, A. S. Bindschadler, R. Cohen, W. B. Gao, F. Hipple, J. D. Hostert, P. Huntington, J. Justice, C. O. Kilic, A. Kovalskyy, V. Lee, Z. P. Lymbumer, L. Masek, J. G. McCorkel, J. Shuai, Y. Trezza, R. Vogelmann, J. Wynne, R. H. Zhu, Z. TI Landsat-8: Science and product vision for terrestrial global change research SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Landsat 8; OLI; TIRS; Landsat Science Team ID CONTERMINOUS UNITED-STATES; DATA CONTINUITY MISSION; TERM ACQUISITION PLAN; ABSOLUTE RADIOMETRIC CALIBRATION; PLUS ATMOSPHERIC CORRECTION; GREENLAND ICE-SHEET; FOREST COVER CHANGE; LEAF-AREA INDEX; TIME-SERIES; LAND-COVER AB Landsat 8, a NASA and USGS collaboration, acquires global moderate-resolution measurements of the Earth's terrestrial and polar regions in the visible, near-infrared, short wave, and thermal infrared. Landsat 8 extends the remarkable 40 year Landsat record and has enhanced capabilities including new spectral bands in the blue and cirrus cloud-detection portion of the spectrum, two thermal bands, improved sensor signal-to-noise performance and associated improvements in radiometric resolution, and an improved duty cycle that allows collection of a significantly greater number of images per day. This paper introduces the current (2012-2017) Landsat Science Team's efforts to establish an initial understanding of Landsat 8 capabilities and the steps ahead in support of priorities identified by the team. Preliminary evaluation of Landsat 8 capabilities and identification of new science and applications opportunities are described with respect to calibration and radiometric characterization; surface reflectance; surface albedo; surface temperature, evapotranspiration and drought; agriculture; land cover, condition, disturbance and change; fresh and coastal water; and snow and ice. Insights into the development of derived 'higher-lever Landsat products are provided in recognition of the growing need for consistently processed, moderate spatial resolution, large area, long-term terrestrial data records for resource management and for climate and global change studies. The paper concludes with future prospects, emphasizing the opportunities for land imaging constellations by combining Landsat data with data collected from other international sensing systems, and consideration of successor Landsat mission requirements. (c) 2014 The Authors. Published by Elsevier Inc. C1 [Roy, D. P.; Kovalskyy, V.] S Dakota State Univ, Geog Informat Sci Ctr Excellence, Brookings, SD 57007 USA. [Wulder, M. A.] Nat Resources Canada, Pacific Forestry Ctr, Canadian Forest Serv, Victoria, BC V8Z 1M5, Canada. [Loveland, T. R.; Vogelmann, J.] US Geol Survey, EROS, Sioux Falls, SD 57198 USA. [Woodcock, C. E.; Kennedy, R.; Zhu, Z.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. [Allen, R. G.; Trezza, R.] Univ Idaho, Res & Extens Ctr, Kimberly, ID 83341 USA. [Anderson, M. C.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [Helder, D.] S Dakota State Univ, Coll Engn, Brookings, SD 57007 USA. [Irons, J. R.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Johnson, D. M.] USDA, Natl Agr Stat Serv, Fairfax, VA 22030 USA. [Scambos, Ta.] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80303 USA. [Schaaf, C. B.; Lee, Z. P.] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA. [Schott, J. R.] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Sheng, Y.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA. [Vermote, E. F.] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA. [Belward, A. S.] European Commiss, Joint Res Ctr, Inst Environm & Sustainabil, I-20133 Milan, Italy. [Bindschadler, R.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. [Cohen, W. B.] USDA Forest Serv, Corvallis, OR 97331 USA. [Gao, F.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [Hipple, J. D.] USDA, Risk Management Agcy, Washington, DC 20250 USA. [Hostert, P.] Humboldt Univ, Dept Geog, D-10099 Berlin, Germany. [Huntington, J.] Desert Res Inst, Reno, NV 89501 USA. [Justice, C. O.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Kilic, A.] Univ Nebraska, Sch Nat Resources, Dept Civil Engn, Lincoln, NE 68516 USA. [Lymbumer, L.] Geosci Australia, Canberra, ACT 2601, Australia. [Masek, J. G.; McCorkel, J.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Shuai, Y.] NASAs, Goddard Space Flight Ctr, ERT Inc, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Wynne, R. H.] Virginia Tech, Forest Resources & Environm Conservat, Blacksburg, VA 24061 USA. RP Roy, DP (reprint author), S Dakota State Univ, Geog Informat Sci Ctr Excellence, Brookings, SD 57007 USA. RI Masek, Jeffrey/D-7673-2012; Anderson, Martha/C-1720-2015; McCorkel, Joel/D-4454-2012; Zhu, Zhe/K-3518-2015; Wulder, Michael/J-5597-2016; OI Anderson, Martha/0000-0003-0748-5525; McCorkel, Joel/0000-0003-2853-2036; Zhu, Zhe/0000-0001-8283-6407; Wulder, Michael/0000-0002-6942-1896; Vogelmann, James/0000-0002-0804-5823 FU USGS-NASA Landsat Science Team FX We are grateful to the NASA-USGS-industry Landsat Data Continuity Mission (LDCM) development team for their efforts to meet an aggressive launch schedule, and we thank the USGS Climate and Land Use Change Mission's Land Remote Sensing Program and the Earth Resources Observation and Science (EROS) Center for co-sponsoring and funding the USGS-NASA Landsat Science Team. NR 194 TC 249 Z9 259 U1 37 U2 225 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 APR 5 PY 2014 VL 145 BP 154 EP 172 DI 10.1016/j.rse.2014.02.001 PG 19 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AG0NW UT WOS:000335113200014 ER PT J AU Aasi, J Abadie, J Abbott, BP Abbott, R Abbott, T Abernathy, MR Accadia, T Acernese, F Adams, C Adams, T Adhikari, RX Affeldt, C Agathos, M Aggarwal, N Aguiar, OD Ajith, P Allen, B Allocca, A Ceron, EA Amariutei, D Anderson, RA Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, C Areeda, J Ast, S Aston, SM Astone, P Aufmuth, P Aulbert, C Austin, L Aylott, BE Babak, S Baker, PT Ballardin, G Ballmer, SW Barayoga, JC Barker, D Barnum, SH Barone, F Barr, B Barsotti, L Barsuglia, M Barton, MA Bartos, I Bassiri, R Basti, A Batch, J Bauchrowitz, J Bauer, TS Bebronne, M Behnke, B Bejger, M Beker, MG Bell, AS Bell, C Belopolski, I Bergmann, G Berliner, JM Bersanetti, D Bertolini, A Bessis, D Betzwieser, J Beyersdorf, PT Bhadbhade, T Bilenko, IA Billingsley, G Birch, J Bitossi, M Bizouard, MA Black, E Blackburn, JK Blackburn, L Blair, D Blom, M Bock, O Bodiya, TP Boer, M Bogan, C Bond, C Bondu, F Bonelli, L Bonnand, R Bork, R Born, M Boschi, V Bose, S Bosi, L Bowers, J Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brannen, CA Brau, JE Breyer, J Briant, T Bridges, DO Brillet, A Brinkmann, M Brisson, V Britzger, M Brooks, AF Brown, DA Brown, DD Bruckner, F Bulik, T Bulten, HJ Buonanno, A Buskulic, D Buy, C Byer, RL Cadonati, L Cagnoli, G Bustillo, JC Calloni, E Camp, JB Campsie, P Cannon, KC Canuel, B Cao, J Capano, CD Carbognani, F Carbone, L Caride, S Castiglia, A Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Cella, G Cepeda, C Cesarini, E Chakraborty, R Chalermsongsak, T Chao, S Charlton, P Chassande-Mottin, E Chen, X Chen, Y Chincarini, A Chiummo, A Cho, HS Chow, J Christensen, N Chu, Q Chua, SSY Chung, S Ciani, G Clara, F Clark, DE Clark, JA Cleva, F Coccia, E 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Feldbaum, D Ferrante, I Ferrini, F Fidecaro, F Finn, LS Fiori, I Fisher, R Flaminio, R Foley, E Foley, S Forsi, E Fotopoulos, N Fournier, JD Franco, S Frasca, S Frasconi, F Frede, M Frei, M Frei, Z Freise, A Frey, R Fricke, TT Fritschel, P Frolov, VV Fujimoto, MK Fulda, P Fyffe, M Gair, J Gammaitoni, L Garcia, J Garufi, F Gehrels, N Gemme, G Genin, E Gennai, A Gergely, L Ghosh, S Giaime, JA Giampanis, S Giardina, KD Giazotto, A Gil-Casanova, S Gill, C Gleason, J Goetz, E Goetz, R Gondan, L Gonzalez, G Gordon, N Gorodetsky, ML Gossan, S Gossler, S Gouaty, R Graef, C Graff, PB Granata, M Grant, A Gras, S Gray, C Greenhalgh, RJS Gretarsson, AM Griffo, C Groot, P Grote, H Grover, K Grunewald, S Guidi, GM Guido, C Gushwa, KE Gustafson, EK Gustafson, R Hall, B Hall, E Hammer, D Hammond, G Hanke, M Hanks, J Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Hartman, MT Haughian, K Hayama, K Heefner, J Heidmann, A Heintze, M Heitmann, H Hello, P Hemming, G Hendry, M Heng, IS 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CA LIGO Sci Collaboration Virgo Collaboration TI Constraints on Cosmic Strings from the LIGO-Virgo Gravitational-Wave Detectors SO PHYSICAL REVIEW LETTERS LA English DT Article ID INFLATION; LIMITS AB Cosmic strings can give rise to a large variety of interesting astrophysical phenomena. Among them, powerful bursts of gravitational waves (GWs) produced by cusps are a promising observational signature. In this Letter we present a search for GWs from cosmic string cusps in data collected by the LIGO and Virgo gravitational wave detectors between 2005 and 2010, with over 625 days of live time. We find no evidence of GW signals from cosmic strings. From this result, we derive new constraints on cosmic string parameters, which complement and improve existing limits from previous searches for a stochastic background of GWs from cosmic microwave background measurements and pulsar timing data. 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RI Losurdo, Giovanni/K-1241-2014; Steinlechner, Sebastian/D-5781-2013; Kumar, Prem/B-6691-2009; Hild, Stefan/A-3864-2010; Danilishin, Stefan/K-7262-2012; Gammaitoni, Luca/B-5375-2009; Iyer, Bala R./E-2894-2012; Canuel, Benjamin/C-7459-2014; Lee, Chang-Hwan/B-3096-2015; Khalili, Farit/D-8113-2012; McClelland, David/E-6765-2010; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Ward, Robert/I-8032-2014; Bilenko, Igor/D-5172-2012; Costa, Cesar/G-7588-2012; Huerta, Eliu/J-5426-2014; CONTE, ANDREA/J-6667-2012; Salemi, Francesco/F-6988-2014; prodi, giovanni/B-4398-2010; Prokhorov, Leonid/I-2953-2012; Gorodetsky, Michael/C-5938-2008; Strigin, Sergey/I-8337-2012; Mitrofanov, Valery/D-8501-2012; Gemme, Gianluca/C-7233-2008; Bell, Angus/E-7312-2011; Nelemans, Gijs/D-3177-2012; Leonardi, Matteo/G-9694-2015; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Ottaway, David/J-5908-2015; Garufi, Fabio/K-3263-2015; Deleglise, Samuel/B-1599-2015; Neri, Igor/F-1482-2010; Aggarwal, Nancy/M-7203-2015; Shaddock, Daniel/A-7534-2011; Vicere, Andrea/J-1742-2012; Rocchi, Alessio/O-9499-2015; Pinto, Innocenzo/L-3520-2016; Ferrante, Isidoro/F-1017-2012; Bondu, Francois/A-2071-2012; Travasso, Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Cesarini, Elisabetta/C-4507-2017; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Martelli, Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Strain, Kenneth/D-5236-2011; Miao, Haixing/O-1300-2013; Howell, Eric/H-5072-2014; Gehring, Tobias/A-8596-2016; Heidmann, Antoine/G-4295-2016; Ott, Christian/G-2651-2011; Marchesoni, Fabio/A-1920-2008; Zhu, Xingjiang/E-1501-2016; Frasconi, Franco/K-1068-2016; Groot, Paul/K-4391-2016 OI Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Murphy, David/0000-0002-8538-815X; Pitkin, Matthew/0000-0003-4548-526X; Veitch, John/0000-0002-6508-0713; Davies, Gareth/0000-0002-4289-3439; Principe, Maria/0000-0002-6327-0628; Allen, Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Vitale, Salvatore/0000-0003-2700-0767; Kanner, Jonah/0000-0001-8115-0577; Freise, Andreas/0000-0001-6586-9901; Nitz, Alexander/0000-0002-1850-4587; Sorazu, Borja/0000-0002-6178-3198; Zweizig, John/0000-0002-1521-3397; Del Pozzo, Walter/0000-0003-3978-2030; O'Shaughnessy, Richard/0000-0001-5832-8517; Pierro, Vincenzo/0000-0002-6020-5521; Coccia, Eugenio/0000-0002-6669-5787; Vetrano, Flavio/0000-0002-7523-4296; Denker, Timo/0000-0003-1259-5315; Naticchioni, Luca/0000-0003-2918-0730; calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Boschi, Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418; Husa, Sascha/0000-0002-0445-1971; Papa, M.Alessandra/0000-0002-1007-5298; Vocca, Helios/0000-0002-1200-3917; Aulbert, Carsten/0000-0002-1481-8319; Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Guidi, Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431; Losurdo, Giovanni/0000-0003-0452-746X; Steinlechner, Sebastian/0000-0003-4710-8548; Danilishin, Stefan/0000-0001-7758-7493; Gammaitoni, Luca/0000-0002-4972-7062; Iyer, Bala R./0000-0002-4141-5179; Lee, Chang-Hwan/0000-0003-3221-1171; McClelland, David/0000-0001-6210-5842; Vecchio, Alberto/0000-0002-6254-1617; Vedovato, Gabriele/0000-0001-7226-1320; Swinkels, Bas/0000-0002-3066-3601; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Whelan, John/0000-0001-5710-6576; Fairhurst, Stephen/0000-0001-8480-1961; prodi, giovanni/0000-0001-5256-915X; Gorodetsky, Michael/0000-0002-5159-2742; Gemme, Gianluca/0000-0002-1127-7406; Bell, Angus/0000-0003-1523-0821; Nelemans, Gijs/0000-0002-0752-2974; Sigg, Daniel/0000-0003-4606-6526; Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168; Deleglise, Samuel/0000-0002-8680-5170; Neri, Igor/0000-0002-9047-9822; Shaddock, Daniel/0000-0002-6885-3494; Vicere, Andrea/0000-0003-0624-6231; Rocchi, Alessio/0000-0002-1382-9016; Ferrante, Isidoro/0000-0002-0083-7228; Bondu, Francois/0000-0001-6487-5197; Travasso, Flavio/0000-0002-4653-6156; Punturo, Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Martelli, Filippo/0000-0003-3761-8616; Strain, Kenneth/0000-0002-2066-5355; Miao, Haixing/0000-0003-4101-9958; Howell, Eric/0000-0001-7891-2817; Gehring, Tobias/0000-0002-4311-2593; Heidmann, Antoine/0000-0002-0784-5175; Ott, Christian/0000-0003-4993-2055; Marchesoni, Fabio/0000-0001-9240-6793; Zhu, Xingjiang/0000-0001-7049-6468; Frasconi, Franco/0000-0003-4204-6587; Groot, Paul/0000-0002-4488-726X FU United States National Science Foundation; Science and Technology Facilities Council of the United Kingdom; Max-Planck-Society; State of Niedersachsen/Germany; Italian Istituto Nazionale di Fisica Nucleare; French Centre National de la Recherche Scientifique; Australian Research Council; International Science Linkages program of the Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Foundation for Fundamental Research; the Netherlands Organisation for Scientific Research; Polish Ministry of Science and Higher Education; FOCUS Programme of Foundation for Polish Science; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; OTKA of Hungary; Lyon Institute of Origins (LIO); National Research Foundation of Korea, Industry Canada; Province of Ontario through the Ministry of Economic Development and Innovation; National Science and Engineering Research Council Canada; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P. Sloan Foundation FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, OTKA of Hungary, the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the National Science and Engineering Research Council Canada, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. NR 43 TC 25 Z9 25 U1 6 U2 64 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 APR 4 PY 2014 VL 112 IS 13 AR 131101 DI 10.1103/PhysRevLett.112.131101 PG 10 WC Physics, Multidisciplinary SC Physics GA AE9PJ UT WOS:000334339800002 PM 24745400 ER PT J AU Iess, L Stevenson, DJ Parisi, M Hemingway, D Jacobson, RA Lunine, JI Nimmo, F Armstrong, JW Asmar, SW Ducci, M Tortora, P AF Iess, L. Stevenson, D. J. Parisi, M. Hemingway, D. Jacobson, R. A. Lunine, J. I. Nimmo, F. Armstrong, J. W. Asmar, S. W. Ducci, M. Tortora, P. TI The Gravity Field and Interior Structure of Enceladus SO SCIENCE LA English DT Article ID WATER RESERVOIR; SOUTH-POLE; TITAN; PLUME AB The small and active Saturnian moon Enceladus is one of the primary targets of the Cassini mission. We determined the quadrupole gravity field of Enceladus and its hemispherical asymmetry using Doppler data from three spacecraft flybys. Our results indicate the presence of a negative mass anomaly in the south-polar region, largely compensated by a positive subsurface anomaly compatible with the presence of a regional subsurface sea at depths of 30 to 40 kilometers and extending up to south latitudes of about 50 degrees. The estimated values for the largest quadrupole harmonic coefficients (10(6)J(2) = 5435.2 +/- 34.9, 10(6)C(22) = 1549.8 +/- 15.6, 1 sigma) and their ratio (J(2)/C-22 = 3.51 +/- 0.05) indicate that the body deviates mildly from hydrostatic equilibrium. The moment of inertia is around 0.335MR(2), where M is the mass and R is the radius, suggesting a differentiated body with a low-density core. C1 [Iess, L.; Parisi, M.; Ducci, M.] Univ Roma La Sapienza, Dipartimento Ingn Meccan & Aerospaziale, I-00184 Rome, Italy. [Stevenson, D. J.] CALTECH, Pasadena, CA 91125 USA. [Hemingway, D.; Nimmo, F.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Jacobson, R. A.; Armstrong, J. W.; Asmar, S. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lunine, J. I.] Cornell Univ, Dept Astron, Ithaca, NY 14850 USA. [Tortora, P.] Univ Bologna, Dipartimento Ingn Ind, I-47121 Forli, Italy. RP Iess, L (reprint author), Univ Roma La Sapienza, Dipartimento Ingn Meccan & Aerospaziale, Via Eudossiana 18, I-00184 Rome, Italy. EM luciano.iess@uniroma1.it RI Hemingway, Douglas/F-6332-2014; IESS, Luciano/F-4902-2011 OI Hemingway, Douglas/0000-0001-5617-207X; IESS, Luciano/0000-0002-6230-5825 FU Italian Space Agency; NASA FX L.I., M.P., M.D., and P.T. acknowledge support from the Italian Space Agency. D.H., F.N., and J.I.L. are grateful to NASA for support through the Cassini Project. The work of R.A.J., J.W.A., and S.W.A. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The Doppler data and ancillary information used in this analysis are archived in NASA's Planetary Data System. NR 21 TC 48 Z9 49 U1 10 U2 67 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 APR 4 PY 2014 VL 344 IS 6179 BP 78 EP 80 DI 10.1126/science.1250551 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AE1RD UT WOS:000333746100055 PM 24700854 ER PT J AU Muller, CL Kidd, C AF Muller, Catherine L. Kidd, Chris TI Debugging geographers: teaching programming to non-computer scientists SO JOURNAL OF GEOGRAPHY IN HIGHER EDUCATION LA English DT Article DE FORTRAN programming; R; Linux; module design; meteorology; postgraduate teaching in geography ID STUDENTS AB The steep learning curve associated with computer programming can be a daunting prospect, particularly for those not well aligned with this way of logical thinking. However, programming is a skill that is becoming increasingly important. Geography graduates entering careers in atmospheric science are one example of a particularly diverse group who often require a better knowledge and understanding of computing. Critically, there is a necessity in the field for people with a diverse range of data analysis and modelling abilities. This article outlines the module design and evaluation of an introductory programming course for non-computer scientists within a UK geography department. C1 [Muller, Catherine L.] Univ Birmingham Edgbaston, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England. [Kidd, Chris] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Kidd, Chris] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Muller, CL (reprint author), Univ Birmingham Edgbaston, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England. EM c.l.muller@bham.ac.uk RI Muller, Catherine L./E-9744-2011 OI Muller, Catherine L./0000-0002-5176-5949 NR 44 TC 5 Z9 5 U1 0 U2 7 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0309-8265 EI 1466-1845 J9 J GEOGR HIGHER EDUC JI J. Geogr. High. Educ. PD APR 3 PY 2014 VL 38 IS 2 BP 175 EP 192 DI 10.1080/03098265.2014.908275 PG 18 WC Education & Educational Research; Geography SC Education & Educational Research; Geography GA AG1TH UT WOS:000335198500002 ER PT J AU Potter, C AF Potter, Christopher TI Global assessment of damage to coastal ecosystem vegetation from tropical storms SO REMOTE SENSING LETTERS LA English DT Article ID HURRICANE-FIRE INTERACTIONS; RECENT HISTORY; FOREST; DISTURBANCES; HYPOTHESIS; YUCATAN; MEXICO; IMPACT; RECORD AB This study reports on the first comprehensive global assessment of tropical storm (TS) impacts on coastal ecosystem vegetation along the landfall pathways of major hurricanes, cyclones and typhoons using satellite data of land cover vegetation for the years 2006 to 2012. Wind damage has been shown to reduce live vegetation pools of carbon, accelerate ecosystem respiration fluxes of carbon dioxide and thereby represent a potentially significant positive feedback to terrestrial greenhouse gas emissions. Based on quarterly detection of changes in Moderate Resolution Imaging Spectroradiometer (MODIS) satellite vegetation greenness, all major TS pathways during the time period were ranked in terms of area of vegetation damage observed. Comparison of vegetation disturbance area along major TS pathways to average rates of disturbance within the same coastal zones (for years during which no TS activity was observed) verified the satellite capability to detect TS ecosystem impacts. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Potter, C (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM chris.potter@nasa.gov NR 25 TC 0 Z9 0 U1 2 U2 11 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 2150-704X EI 2150-7058 J9 REMOTE SENS LETT JI Remote Sens. Lett. PD APR 3 PY 2014 VL 5 IS 4 BP 315 EP 322 DI 10.1080/2150704X.2014.902546 PG 8 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA AG0EL UT WOS:000335088000002 ER PT J AU Frost, DA McAuley, WC Kluver, B Wastel, M Maynard, D Flagg, TA AF Frost, Deborah A. McAuley, W. Carlin Kluver, Bryon Wastel, Mike Maynard, Desmond Flagg, Thomas A. TI Methods and Accuracy of Sexing Sockeye Salmon Using Ultrasound for Captive Broodstock Management SO NORTH AMERICAN JOURNAL OF AQUACULTURE LA English DT Article ID MATURATIONAL STATUS; PACIFIC SALMON; ULTRASONOGRAPHY; STOCKS AB Ultrasound has been widely used to noninvasively examine the internal anatomy and reproductive status of many fish species. Since 2003, ultrasonography has been an integral part of broodstock management for Endangered Species Act-listed endangered Redfish Lake Sockeye Salmon Oncorhynchus nerka. Initial ultrasound screenings for each year's broodstock were conducted 3 to 4 months prior to anticipated maturation, before external signs of maturation developed. In keeping with the natural life history of these fish, this permitted the separation of nonmaturing fish from maturing fish so the immature fish could maintain feeding and growth. It also permitted maturing seawater-reared fish to be transferred to freshwater for final maturation. Designing a spawning matrix to maintain genetic diversity requires knowledge of the sex of each fish before spawning. Approximately 1 month prior to spawning, a second ultrasound was performed to verify sex identification and thus ensure the accuracy of the spawning matrix. Over a 9-year period, 2,662 fish were examined. The accuracy of sexing age-3 adult Sockeye Salmon ranged from 94.0% to 100%, with an average of 97.7%, while the accuracy of sexing age-4 adult fish ranged from 92.0% to 100%, with an average of 94.4%. The average accuracy was similar for fish examined in seawater or freshwater (98.1% versus 97.3%, respectively). Ultrasound was shown to be an accurate and effective tool for managing the husbandry of our captive broodstock life history. Received September 13, 2013; accepted January 2, 2014 C1 [Frost, Deborah A.; McAuley, W. Carlin; Kluver, Bryon; Wastel, Mike; Maynard, Desmond; Flagg, Thomas A.] Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Environm & Fisheries Sci Div, Manchester Res Stn, Manchester, WA 98353 USA. RP Frost, DA (reprint author), Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Environm & Fisheries Sci Div, Manchester Res Stn, POB 130, Manchester, WA 98353 USA. EM debbie.frost@noaa.gov FU BPA FX This Redfish Lake Sockeye Salmon gene rescue program is a cooperative between NMFS, the Idaho Department of Fish and Game, the Bonneville Power Administration (BPA), the Shoshone Bannock Tribes, and others involved with salmon conservation in the Columbia River Basin. The program is funded by the BPA and coordinated through the Northwest Power and Conservation Council's Fish and Wildlife Program. Mention of specific products does not constitute endorsement by NOAA. NR 14 TC 1 Z9 2 U1 2 U2 16 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 1522-2055 EI 1548-8454 J9 N AM J AQUACULT JI N. Am. J. Aqualcult. PD APR 3 PY 2014 VL 76 IS 2 BP 153 EP 158 DI 10.1080/15222055.2014.886647 PG 6 WC Fisheries SC Fisheries GA AE9NE UT WOS:000334333700009 ER PT J AU Ade, PAR Akiba, Y Anthony, AE Arnold, K Atlas, M Barron, D Boettger, D Borrill, J Borys, C Chapman, S Chinone, Y Dobbs, M Elleflot, T Errard, J Fabbian, G Feng, C Flanigan, D Gilbert, A Grainger, W Halverson, NW Hasegawa, M Hattori, K Hazumi, M Holzapfel, WL Hori, Y Howard, J Hyland, P Inoue, Y Jaehnig, GC Jaffe, A Keating, B Kermish, Z Keskitalo, R Kisner, T Le Jeune, M Lee, AT Leitch, EM Linder, E Lungu, M Matsuda, F Matsumura, T Meng, X Miller, NJ Morii, H Moyerman, S Myers, MJ Navaroli, M Nishino, H Paar, H Peloton, J Poletti, D Quealy, E Rebeiz, G Reichardt, CL Richards, PL Ross, C Rotermund, K Schanning, I Schenck, DE Sherwin, BD Shimizu, A Shimmin, C Shimon, M Siritanasak, P Smecher, G Spieler, H Stebor, N Steinbach, B Stompor, R Suzuki, A Takakura, S Tikhomirov, A Tomaru, T Wilson, B Yadav, A Zahn, O AF Ade, P. A. R. Akiba, Y. Anthony, A. E. Arnold, K. Atlas, M. Barron, D. Boettger, D. Borrill, J. Borys, C. Chapman, S. Chinone, Y. Dobbs, M. Elleflot, T. Errard, J. Fabbian, G. Feng, C. Flanigan, D. Gilbert, A. Grainger, W. Halverson, N. W. Hasegawa, M. Hattori, K. Hazumi, M. Holzapfel, W. L. Hori, Y. Howard, J. Hyland, P. Inoue, Y. Jaehnig, G. C. Jaffe, A. Keating, B. Kermish, Z. Keskitalo, R. Kisner, T. Le Jeune, M. Lee, A. T. Leitch, E. M. Linder, E. Lungu, M. Matsuda, F. Matsumura, T. Meng, X. Miller, N. J. Morii, H. Moyerman, S. Myers, M. J. Navaroli, M. Nishino, H. Paar, H. Peloton, J. Poletti, D. Quealy, E. Rebeiz, G. Reichardt, C. L. Richards, P. L. Ross, C. Rotermund, K. Schanning, I. Schenck, D. E. Sherwin, B. D. Shimizu, A. Shimmin, C. Shimon, M. Siritanasak, P. Smecher, G. Spieler, H. Stebor, N. Steinbach, B. Stompor, R. Suzuki, A. Takakura, S. Tikhomirov, A. Tomaru, T. Wilson, B. Yadav, A. Zahn, O. CA POLARBEAR Collaboration TI Evidence for Gravitational Lensing of the Cosmic Microwave Background Polarization from Cross-Correlation with the Cosmic Infrared Background SO PHYSICAL REVIEW LETTERS LA English DT Article ID SOUTH-POLE TELESCOPE; POWER SPECTRUM; HERSCHEL ATLAS; DAMPING TAIL; PROBE; MAPS; SKY; GHZ AB We reconstruct the gravitational lensing convergence signal from cosmic microwave background (CMB) polarization data taken by the POLARBEAR experiment and cross-correlate it with cosmic infrared background maps from the Herschel satellite. From the cross spectra, we obtain evidence for gravitational lensing of the CMB polarization at a statistical significance of 4.0 sigma and indication of the presence of a lensing B-mode signal at a significance of 2.3 sigma. We demonstrate that our results are not biased by instrumental and astrophysical systematic errors by performing null tests, checks with simulated and real data, and analytical calculations. This measurement of polarization lensing, made via the robust cross-correlation channel, not only reinforces POLARBEAR auto-correlation measurements, but also represents one of the early steps towards establishing CMB polarization lensing as a powerful new probe of cosmology and astrophysics. C1 [Ade, P. A. R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3XQ, S Glam, Wales. [Akiba, Y.; Hasegawa, M.; Hazumi, M.; Inoue, Y.; Shimizu, A.] Grad Univ Adv Studies, Kanagawa 2400115, Japan. [Anthony, A. E.; Halverson, N. W.; Jaehnig, G. C.; Schenck, D. E.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Arnold, K.; Atlas, M.; Barron, D.; Boettger, D.; Elleflot, T.; Feng, C.; Keating, B.; Matsuda, F.; Moyerman, S.; Navaroli, M.; Paar, H.; Schanning, I.; Shimon, M.; Siritanasak, P.; Stebor, N.; Wilson, B.; Yadav, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Borrill, J.; Errard, J.; Keskitalo, R.; Kisner, T.] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, La Jolla, CA 92093 USA. [Borrill, J.; Errard, J.; Kisner, T.; Linder, E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Borys, C.] CALTECH, Pasadena, CA 91125 USA. [Chapman, S.; Ross, C.; Rotermund, K.; Tikhomirov, A.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Chinone, Y.; Hasegawa, M.; Hattori, K.; Hazumi, M.; Hori, Y.; Matsumura, T.; Morii, H.; Takakura, S.; Tomaru, T.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan. [Chinone, Y.; Flanigan, D.; Holzapfel, W. L.; Howard, J.; Lee, A. T.; Lungu, M.; Meng, X.; Myers, M. J.; Quealy, E.; Reichardt, C. L.; Richards, P. L.; Sherwin, B. D.; Shimmin, C.; Steinbach, B.; Suzuki, A.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Dobbs, M.; Gilbert, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 0G4, Canada. [Fabbian, G.; Le Jeune, M.; Peloton, J.; Poletti, D.; Stompor, R.] Univ Paris Diderot, AstroParticule & Cosmol, CNRS IN2P3, CEA Irfu,Obs Paris,Sorbonne Paris Cite, Paris, France. [Fabbian, G.] Int Sch Adv Studies SISSA, I-34014 Trieste, Italy. [Flanigan, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Grainger, W.] STFC, Rutherford Appleton Lab, Swindon SN2 1SZ, Wilts, England. [Anthony, A. E.; Halverson, N. W.; Schenck, D. E.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.; Jaehnig, G. C.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Hazumi, M.; Nishino, H.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Univ WPI, Kashiwa, Chiba 2778583, Japan. [Howard, J.] Univ Oxford, Dept Phys, Oxford OX1 2JD, England. [Hyland, P.] Austin Coll, Dept Phys, Sherman, TX 75090 USA. [Jaffe, A.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. [Leitch, E. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Leitch, E. M.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Kermish, Z.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Lee, A. T.; Linder, E.; Spieler, H.; Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Miller, N. J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Quealy, E.] Napa Valley Coll, Dept Phys, Napa, CA 94558 USA. [Rebeiz, G.] Univ Calif San Diego, Dept Elect & Comp Engn, La Jolla, CA 92093 USA. [Sherwin, B. D.] Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA. [Shimon, M.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Smecher, G.] Three Speed Log Inc, Vancouver, BC V6A 2J8, Canada. [Takakura, S.] Osaka Univ, Toyonaka, Osaka 5600043, Japan. RP Sherwin, BD (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. EM sherwin@berkeley.edu RI Holzapfel, William/I-4836-2015; OI Fabbian, Giulio/0000-0002-3255-4695; Reichardt, Christian/0000-0003-2226-9169 FU DOE [DE-AC02-05CH11231]; NSF [AST-0618398, AST-1212230]; MEXT KAKENHI [21111002]; KEK Cryogenics Science Center; Natural Sciences and Engineering Research Council and Canadian Institute for Advanced Research; NASA Postdoctoral Program; Miller Fellowship; Simons Foundation; Joan and Irwin Jacobs; Comision Nacional de Investigacicn Cientfica y Tecnologica de Chile (CONICYT) FX We thank Frank Wuerthwein, Igor Sfiligoi, Terrence Martin, and Robert Konecny for their insight and support, and thank Nolberto Oyarce and Jos, Cortes for their invaluable contributions. Calculations were performed at the Department of Energy Open Science Grid [39] at the University of California, San Diego, accessed via the GlideinWMS [40], at Central Computing System, owned and operated by the Computing Research Center at KEK, and at NERSC which is supported by the DOE under Contract No. DE-AC02-05CH11231. The POLARBEAR project is funded by the NSF under Grants No. AST0618398 and No. AST-1212230. The KEK authors were supported by MEXT KAKENHI Grant No. 21111002, and acknowledge support from KEK Cryogenics Science Center. The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council and Canadian Institute for Advanced Research. N. M., B. D. S., and K. A. acknowledge support from the NASA Postdoctoral Program, a Miller Fellowship, and the Simons Foundation, respectively. M. S. gratefully acknowledges support from Joan and Irwin Jacobs. The James Ax Observatory operates in the Parque Astroncmico Atacama in Northern Chile under the auspices of the Comisicn Nacional de Investigacicn Cient fica y Tecnolcgica de Chile (CONICYT). Finally, we acknowledge the tremendous contributions by Huan Tran to the POLARBEAR project. NR 39 TC 34 Z9 34 U1 2 U2 9 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD APR 2 PY 2014 VL 112 IS 13 AR 131302 DI 10.1103/PhysRevLett.112.131302 PG 6 WC Physics, Multidisciplinary SC Physics GA AE9OP UT WOS:000334337500006 PM 24745402 ER PT J AU Kostas, VI Stenger, MB Knapp, CF Shapiro, R Wang, SQ Diedrich, A Evans, JM AF Kostas, Vladimir I. Stenger, Michael B. Knapp, Charles F. Shapiro, Robert Wang, Siqi Diedrich, Andre Evans, Joyce M. TI Cardiovascular Models of Simulated Moon and Mars Gravities: Head-Up Tilt vs. Lower Body Unweighting SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE alter-G; LBPP; orthostatic intolerance ID POSITIVE-PRESSURE; ORTHOSTATIC INTOLERANCE; RESPONSES; SPACEFLIGHT; POSTURE; COUNTERMEASURE; WOMEN; REST AB Introduction: In this study we compare two models [head-up tilt (HUT) vs. body unweighting using lower body positive pressure (LBPP)] to simulate Moon, Mars, and Earth gravities. A literature search did not reveal any comparisons of this type performed previously. We hypothesized that segmental fluid volume shifts (thorax, abdomen, upper and lower leg), cardiac output, and blood pressure (BP), heart rate (HR), and total peripheral resistance to standing would be similar in the LBPP and HUT models. Methods: There were 21 subjects who were studied while supine (simulation of spaceflight) and standing at 100% (Earth), 40% (Mars), and 20% (Moon) bodyweight produced by LBPP in Alter-G and while supine and tilted at 80, 20, and 100 HUT (analogues of Earth, Mars, and Moon gravities, respectively). Results: Compared to supine, fluid shifts from the chest to the abdomen, increases in HR, and decreases in stroke volume were greater at 100% bodyweight than at reduced weights in response to both LBPP and HUT. Differences between the two models were found for systolic BP, diastolic BP, mean arterial BP, stroke volume, total peripheral resistance, and thorax and abdomen impedances, while HR, cardiac output, and upper and lower leg impedances were similar. Conclusions: Bodyweight unloading via both LBPP and HUT resulted in cardiovascular changes similar to those anticipated in actual reduced gravity environments. The LBPP model/Alter-G has the advantage of providing an environment that allows dynamic activity at reduced body-weight; however, the significant increase in blood pressures in the Alter-G may favor the HUT model. C1 [Kostas, Vladimir I.; Knapp, Charles F.; Shapiro, Robert; Wang, Siqi; Evans, Joyce M.] Univ Kentucky, Lexington, KY 40506 USA. [Stenger, Michael B.] NASA, Lyndon B Johnson Space Ctr, Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. [Diedrich, Andre] Vanderbilt Univ, Nashville, TN 37235 USA. RP Evans, JM (reprint author), Univ Kentucky, Ctr Biomed Engn, Rm 1,600 Rose St, Lexington, KY 40506 USA. EM jevans1@uky.edu FU KY NASA EPSCoR Research Area [NNX07AT58A, NNX07AL55A] FX We would like to thank L. Christine Ribeiro (NASA JSC), Elizabeth Salmon (UK), Dan Irwin (UK), and Matt Haaga (UK) for data analysis and Tim Matz (NASA JSC) for ultrasound data. This study was supported by KY NASA EPSCoR Research Area I Grant # NNX07AT58A and Grant # NNX07AL55A. NR 21 TC 3 Z9 3 U1 1 U2 3 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD APR PY 2014 VL 85 IS 4 BP 414 EP 419 DI 10.3357/ASEM.3687.2014 PG 6 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA CB6FF UT WOS:000349721600003 PM 24754202 ER PT J AU De Witt, JK Schaffner, G Ploutz-Snyder, LL AF De Witt, John K. Schaffner, Grant Ploutz-Snyder, Lori L. TI Bungee Force Level, Stiffness, and Variation During Treadmill Locomotion in Simulated Microgravity SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE exercise; treadmill; bungee force; countermeasures ID INTERNATIONAL-SPACE-STATION; FOOT FORCES; EXERCISE; BONE AB Introduction: Crewmembers performing treadmill exercise on the International Space Station must wear a harness with an external gravity replacement force that is created by elastomer bungees. The quantification of the total external force, displacement, stiffness, and force variation is important for understanding the forces applied to the crewmember during typical exercise. Methods: Data were collected during static trials in the laboratory from a single subject and four subjects were tested while walking at 1.34 m.s(-1) and running at 2.24 m.s(-1) and 3.13 m.s(-1) on a treadmill during simulated microgravity in parabolic flight. The external force was provided by bungees and carabiner clips in configurations commonly used by crewmembers. Total external force, displacement, and force variation in the bungee system were measured, from which stiffness was computed. Results: Mean external force ranged from 431 to 804 N (54-131% bodyweight) across subjects and conditions. Mean displacement was 4 to 8 cm depending upon gait speed. Mean stiffness was affected by bungee configuration and ranged from 1.73 to 29.20 N.cm(-1). Force variation for single bungee configurations was 2.61-4.48% of total external force and between 4.30-57.5% total external force for two-bungee configurations. Conclusions: The external force supplied to crewmembers by elastomer bungees provided a range of loading levels with variations that occur throughout the gait cycle. The quantification of bungee-loading characteristics is important to better define the system currently used by crewmembers during exercise. C1 [De Witt, John K.] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. Univ Space Res Assoc, Houston, TX USA. Univ Cincinnati, Cincinnati, OH USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP De Witt, JK (reprint author), Wyle Sci Technol & Engn Grp, 1290 Hercules,Ste 120, Houston, TX 77058 USA. EM jolm.k.dewitt@nasa.gov NR 10 TC 3 Z9 3 U1 0 U2 8 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD APR PY 2014 VL 85 IS 4 BP 449 EP 455 DI 10.3357/ASEM.3217.2014 PG 7 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA CB6FF UT WOS:000349721600009 PM 24754208 ER PT J AU Morgan, J Heer, M Hargens, A Macias, B Hudson, E Shackelford, L Zwart, S Smith, S AF Morgan, Jennifer Heer, Martina Hargens, Allen Macias, Brandon Hudson, Edgar Shackelford, Linda Zwart, Sara Smith, Scott TI Bone metabolism and renal stone risk during bed rest for men and women SO FASEB JOURNAL LA English DT Meeting Abstract CT Experimental Biology Meeting CY APR 26-30, 2014 CL San Diego, CA SP Cenveo, LI COR, Wiley, Mead Johnson Pediat Nutr Inst, IPRECIO, F1000 Res, Amer Assoc Anatomists, Amer Physiol Soc, Amer Soc Biochem & Mol Biol, Amer Soc Investigat Pathol, Amer Soc Nutr, Amer Soc Pharmacol & Expt Therapeut C1 [Hudson, Edgar] JES Tech, Houston, TX USA. [Shackelford, Linda; Smith, Scott] NASA, Houston, TX USA. [Morgan, Jennifer] NASA, ORAU, Houston, TX USA. [Hargens, Allen; Macias, Brandon] Univ Calif San Diego, San Diego, CA USA. [Heer, Martina] Univ Bonn, Bonn, Germany. [Zwart, Sara] NASA, USRA, Houston, TX USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 EI 1530-6860 J9 FASEB J JI Faseb J. PD APR PY 2014 VL 28 IS 1 SU S MA 257.8 PG 2 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA AX0MP UT WOS:000346646700331 ER PT J AU Philip, S Martin, RV Pierce, JR Jimenez, JL Zhang, Q Canagaratna, MR Spracklen, DV Nowlan, CR Lamsal, LN Cooper, MJ Krotkov, NA AF Philip, S. Martin, R. V. Pierce, J. R. Jimenez, J. L. Zhang, Q. Canagaratna, M. R. Spracklen, D. V. Nowlan, C. R. Lamsal, L. N. Cooper, M. J. Krotkov, N. A. TI Spatially and seasonally resolved estimate of the ratio of organic mass to organic carbon SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Organic aerosol; Organic carbon; NO2; AMS; OMI; GEOS-Chem ID UNITED-STATES; HYDROCARBON-LIKE; INTEX-B; AEROSOL; SPECTROMETER; PARTICLES; EMISSIONS; VISIBILITY; CHEMISTRY; PITTSBURGH AB Particulate organic matter is of interest for air quality and climate research, but the relationship between ambient organic mass (OM) and organic carbon (CC) remains ambiguous both in measurements and in modeling. We present a simple method to derive an estimate of the spatially and seasonally resolved global, lower tropospheric, ratio between OM and CC. We assume ambient NO2 concentrations as a surrogate for fresh emission which mostly determines the continental scale OM/OC ratio. For this, we first develop a parameterization for the OM/OC ratio using the primary organic aerosol (POA) fraction of total OM estimated globally from Aerosol Mass Spectrometer (AMS) measurements, and evaluate it with high mass resolution AMS data. Second, we explore the ability of ground-level NO2 concentrations derived from the OMI satellite sensor to serve as a proxy for fresh emissions that have a high POA fraction, and apply NO2 data to derive ambient POA fraction. The combination of these two methods yields an estimate of OM/OC from NO2 measurements. Although this method has inherent deficiencies over biomass burning, free-tropospheric, and marine environments, elsewhere it offers more information than the currently used global-mean OM/OC ratios. The OMI-derived global OM/OC ratio ranges from 1.3 to 2.1 (mu g/mu gC), with distinct spatial variation between urban and rural regions. The seasonal OM/OC ratio has a summer maximum and a winter minimum over regions dominated by combustion emissions. This dataset serves as a tool for interpreting organic carbon measurements, and for evaluating modeling of atmospheric organics. We also develop an additional parameterization for models to estimate the ratio of primary OM to OC from simulated NOx concentrations. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Philip, S.; Martin, R. V.; Pierce, J. R.; Nowlan, C. R.; Cooper, M. J.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pierce, J. R.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Jimenez, J. L.] Univ Colorado, Dept Chem & Biochem, CIRES, Boulder, CO 80309 USA. [Zhang, Q.] Univ Calif Davis, Dept Environm Toxicol, Davis, CA 95616 USA. [Canagaratna, M. R.] Aerodyne Res Inc, Billerica, MA USA. [Spracklen, D. V.] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England. [Lamsal, L. N.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA. [Lamsal, L. N.; Krotkov, N. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Philip, S (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. EM philip.sajeev@dal.ca RI Pierce, Jeffrey/E-4681-2013; Jimenez, Jose/A-5294-2008; Zhang, Qi/F-9653-2010; Martin, Randall/C-1205-2014; Krotkov, Nickolay/E-1541-2012; Spracklen, Dominick/B-4890-2014; OI Pierce, Jeffrey/0000-0002-4241-838X; Jimenez, Jose/0000-0001-6203-1847; Martin, Randall/0000-0003-2632-8402; Krotkov, Nickolay/0000-0001-6170-6750; Nowlan, Caroline/0000-0002-8718-9752 FU NSERC; DOE (BER/ASR) [DE SC0006035/DE-SC0006711/DE-FG02-11ER65293]; [DE-FG02-11ER65293] FX This work was supported by NSERC. JLJ was supported by DOE (BER/ASR) DE SC0006035/DE-SC0006711/DE-FG02-11ER65293. QZ was supported by DE-FG02-11ER65293. We thank Aaron van Donkelaar and Ian Folkins for useful comments. NR 61 TC 11 Z9 12 U1 5 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD APR PY 2014 VL 87 BP 34 EP 40 DI 10.1016/j.atmosenv.2013.11.065 PG 7 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AY2QR UT WOS:000347434900005 ER PT J AU Zhang, QG Knapp, C Smith, J Evans, J AF Zhang, Qingguang Knapp, Charles Smith, Jeffrey Evans, Joyce TI Cardiovascular responses to orthostatic stress after 90 minutes head-down bed rest and artificial gravity exposure in hypovolemic men and women SO FASEB JOURNAL LA English DT Meeting Abstract C1 [Smith, Jeffrey] NASA, Ames Res Ctr, Mountain View, CA USA. [Zhang, Qingguang; Knapp, Charles; Evans, Joyce] Univ Kentucky, Dept Biomed Engn, Lexington, KY USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 EI 1530-6860 J9 FASEB J JI Faseb J. PD APR PY 2014 VL 28 IS 1 SU S MA 1169.18 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA AX0OG UT WOS:000346651002256 ER PT J AU Sim, BW JanakiRam, RD Lau, BH AF Sim, Ben W. JanakiRam, Ram D. Lau, Benton H. TI Reduced In-Plane, Low-Frequency Noise of an Active Flap Rotor SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article AB Results from a joint DARPA/Boeing/NASA/Army wind tunnel test demonstrated the ability to reduce in-plane, low-frequency noise of the full-scale Boeing-SMART(Smart Material Actuated Rotor Technology) rotor with active flaps. Test data reported in this paper illustrated that near-field acoustic energy in the first six blade-passing harmonics could be reduced by up to 6 dB at a moderate-airspeed, level flight condition at an advance ratio of 0.30. Reduced noise levels were attributed to selective active flap schedules that modified in-plane blade airloads on the advancing side of the rotor, generating counteracting acoustic pulses that partially offset the negative pressure peaks associated with in-plane, steady thickness noise. These favorable reduced-noise operating states are a strong function of the active flap actuation amplitude, frequency, and phase. The reduced noise levels resulted in reduction of predicted aural detection distance, but incurred vibratory load penalties due to increased hub shear forces. C1 [Sim, Ben W.] US Army Res Dev & Engn Command, AeroflightDynam Directorate, Moffett Field, CA 94035 USA. [JanakiRam, Ram D.] Boeing Co, Flight Technol, Mesa, AZ USA. [Lau, Benton H.] NASA, Aeromech Branch, Ames Res Ctr, Moffett Field, CA USA. RP Sim, BW (reprint author), US Army Res Dev & Engn Command, AeroflightDynam Directorate, Moffett Field, CA 94035 USA. EM ben.w.sim@us.army.mil NR 20 TC 2 Z9 2 U1 0 U2 1 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 EI 2161-6027 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD APR PY 2014 VL 59 IS 2 AR 022002 DI 10.4050/JAHS.59.022002 PG 17 WC Engineering, Aerospace SC Engineering GA AS6HW UT WOS:000344365800002 ER PT J AU Isaacson, DR Sadovsky, AV Davis, D AF Isaacson, D. R. Sadovsky, A. V. Davis, D. TI Tactical Scheduling for Precision Air Traffic Operations: Past Research and Current Problems SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS LA English DT Article ID LANDINGS C1 [Isaacson, D. R.; Sadovsky, A. V.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Davis, D.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. RP Isaacson, DR (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM douglas.r.isaacson@nasa.gov NR 57 TC 4 Z9 4 U1 0 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 1940-3151 EI 2327-3097 J9 J AEROSP INFORM SYST JI J. Aerosp. Inf. Syst. PD APR PY 2014 VL 11 IS 4 BP 234 EP 256 DI 10.2514/1.I010119 PG 23 WC Engineering, Aerospace SC Engineering GA AP4RO UT WOS:000342066200006 ER PT J AU Carney, LT Reinsch, SS Lane, PD Solberg, OD Jansen, LS Williams, KP Trent, JD Lane, TW AF Carney, Laura T. Reinsch, Sigrid S. Lane, Pamela D. Solberg, Owen D. Jansen, Lara S. Williams, Kelly P. Trent, Jonathan D. Lane, Todd W. TI Microbiome analysis of a microalgal mass culture growing in municipal wastewater in a prototype OMEGA photobioreactor SO ALGAL RESEARCH-BIOMASS BIOFUELS AND BIOPRODUCTS LA English DT Article DE Photobioreactor; Microbiome; Second generation sequencing; Algal pathogens; Biocontaminant ID DIVERSITY; ALGAE; BACTERIA; GROWTH; RDNA; QUANTIFICATION; IDENTIFICATION; ENVIRONMENT; ASSOCIATION; COMMUNITIES AB Large-scale cultivation of microalgae for biofuels may avoid competing for agriculture, water, and fertilizer by using wastewater and avoid competing for land by using the Offshore Membrane Enclosures for Growing Algae (OMEGA) system. Some microalgae thrive in wastewater; however, wastewater also contains a complex mixture of organisms. An algae culture in wastewater from a San Francisco Treatment Facility in a 1600-L OMEGA culture system was monitored by standard methods. Prima facie evidence of a chytrid infection prompted a detailed investigation of the microbiome over a 13-day period using second generation sequencing of hypervariable regions of the small subunit rRNA genes. The observed bacteria, initially dominated by.-proteobacteria, shifted to Cytophagia, Flavobacteriia, and Sphingobacteriia after addition of exogenous nutrients. The dominant algae genera introduced with the inoculum, Desmodesmus and Scenedesmus, remained over 70% of the sequence reads on day 13, although the optical density and fluorescence of the culture declined. Nonalgal eukarya, initially dominated by unclassified alveolates, chrysophytes, and heliozoan grazers, shifted to chytrid fungi on day 5 and continued to day 13. The results of this microbiome analysis can facilitate the development of probe or primer based surveillance systems for routine monitoring of large-scale microalgae cultures. Published by Elsevier B.V. C1 [Carney, Laura T.; Lane, Pamela D.; Solberg, Owen D.; Jansen, Lara S.; Williams, Kelly P.; Lane, Todd W.] Sandia Natl Labs, Livermore, CA 94551 USA. [Reinsch, Sigrid S.; Trent, Jonathan D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lane, TW (reprint author), Sandia Natl Labs, POB 969,MS 9292, Livermore, CA 94551 USA. EM twlane@sandia.gov OI Lane, Todd/0000-0002-5816-2649 FU U.S. Department of Energy's National Nuclear Security Administration [DE-AC04-94AL85000]; Biomass Program of the Office of Energy Efficiency and Renewable Energy U.S. Department of Energy [NL0022897]; NASA; California Energy Commission FX Sandia National Laboratories is a multi-program laboratory managed and operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Corporation, for the U.S. Department of Energy's National Nuclear Security Administration under contract DE-AC04-94AL85000. Microbiome analysis carried out at Sandia National Laboratories was supported by the Biomass Program of the Office of Energy Efficiency and Renewable Energy U.S. Department of Energy under Award #NL0022897. We thank the OMEGA team for technical support, especially Sasha Tozzi, John Malinowski, Hiromi Kagawa, Tsegereda Embaye, Kit Clark, Linden Harris, Patrick Wiley, John Rask, Rus Adams, Zach Hall and the staff at the San Francisco Southeast Wastewater Treatment Plant. We acknowledge Heather McDonald for editorial assistance. The OMEGA project was funded by NASA and the California Energy Commission. NR 64 TC 15 Z9 15 U1 4 U2 65 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2211-9264 J9 ALGAL RES JI Algal Res. PD APR PY 2014 VL 4 BP 52 EP 61 DI 10.1016/j.algal.2013.11.006 PG 10 WC Biotechnology & Applied Microbiology SC Biotechnology & Applied Microbiology GA AM6MP UT WOS:000339979600008 ER PT J AU Stehlik, LL Pessutti, J Rosendale, J Phelan, B AF Stehlik, Linda L. Pessutti, Jeff Rosendale, John Phelan, Beth TI Residence time and habitat duration for predators in a small mid-Atlantic estuary SO FISHERY BULLETIN LA English DT Article ID FLOUNDER PSEUDOPLEURONECTES-AMERICANUS; BLUEFISH POMATOMUS-SALTATRIX; JUVENILE WINTER FLOUNDER; MIGRATORY STRIPED BASS; SOUTHERN NEW-JERSEY; ACOUSTIC TELEMETRY; FISH RECRUITMENT; MORONE-SAXATILIS; EAST-COAST; DYNAMICS AB Residence times of individual fishes should reflect the durations over which habitat resources support survival, metabolic maintenance, and adequate growth. From May to October in 2006 and 2007, we measured residencies of ultrasonically tagged age-1+ Striped Bass (Morone saxatilis; n=46), age-0 and age-1+ Bluefish (Pomatomus saltatrix; n=45 and 35) and age-1+ Weakfish (Cynoscion regalis; n=41) in a small estuarine tributary in New Jersey with 32 ultrasonic receivers to monitor movements and sensors to measure habitat resources. Striped Bass and age-1+ Bluefish used the estuary for medians of 9.5 days (d) (max=58 d) and 22 d (max=88 d), and age-0 Bluefish and Weakfish were resident for medians of 30 d (max=52 d) and 41 d (max=88 d), respectively. Small individuals <500 mm TL were likely to remain in the estuary longer at warmer temperatures than were large individuals. Size-dependent temperature responses were similar to optimal temperatures for growth reported in previous studies. Freshwater discharge also influenced residence time. All species were likely to remain in the estuary until freshwater discharge rates fell to a value associated with the transition of the estuarine state from a partially to fully mixed state. This transition weakens flows into the upstream salt front where prey concentrations usually are high. Time of estuarine residence appeared to be regulated by temperatures that controlled scopes for growth and the indirect effects of freshwater discharge on prey productivity and concentration. Changes in the seasonal phenology of temperature, precipitation, and human water use could alter the durations over which small estuarine tributaries serve as suitable habitats. C1 [Stehlik, Linda L.; Pessutti, Jeff; Rosendale, John; Phelan, Beth] NOAA, Behav Ecol Branch, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv,James J Howard Marine, Highlands, NJ 07732 USA. RP Stehlik, LL (reprint author), NOAA, Behav Ecol Branch, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv,James J Howard Marine, 74 Magruder Rd, Highlands, NJ 07732 USA. NR 57 TC 0 Z9 0 U1 3 U2 16 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 EI 1937-4518 J9 FISH B-NOAA JI Fish. Bull. PD APR-JUL PY 2014 VL 112 IS 2-3 BP 144 EP 158 DI 10.7755/FB.112.2-3.4 PG 15 WC Fisheries SC Fisheries GA AM7XE UT WOS:000340081200004 ER PT J AU Asami, F Enoto, T Iwakiri, W Yamada, S Tamagawa, T Mihara, T Nagase, F AF Asami, Fumi Enoto, Teruaki Iwakiri, Wataru Yamada, Shin'ya Tamagawa, Toru Mihara, Tatehiro Nagase, Fumiaki TI Broad-band spectroscopy of Hercules X-1 with Suzaku SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE binaries: spectroscopic; pulsars: individual (Hercules X-1); X-rays: stars ID X-RAY BINARIES; PULSE-PHASE; COMPTON REFLECTION; CYCLOTRON LINE; 35-DAY CYCLE; X-1; SPECTRUM; BEPPOSAX; STATE; ABSORPTION AB Hercules X-1 was observed with Suzaku in the main-on state from 2005 to 2010. The 0.4-100 keV wide-band spectra obtained in four observations showed a broad hump around 4-9 keV in addition to narrow Fe lines at 6.4 and 6.7 keV. The hump was seen in all the four observations regardless of the selection of the continuum models. Thus it is considered a stable and intrinsic spectral feature in Her X-1. The broad hump lacked a sharp structure like an absorption edge. Thus it was represented by two different spectral models: an ionized partial covering or an additional broad line at 6.5 keV. The former required a persistently existing ionized absorber, whose origin was unclear. In the latter case, the Gaussian fitting of the 6.5-keV line needs a large width of sigma = 1.0-1.5 keV and a large equivalent width of 400-900 eV. If the broad line originates from Fe fluorescence of accreting matter, its large width may be explained by the Doppler broadening in the accretion flow. However, the large equivalent width may be inconsistent with a simple accretion geometry. C1 [Asami, Fumi; Enoto, Teruaki; Iwakiri, Wataru; Yamada, Shin'ya; Tamagawa, Toru] RIKEN, Nishina Ctr, Wako, Saitama 3510198, Japan. [Asami, Fumi; Tamagawa, Toru] Tokyo Univ Sci, Dept Phys, Shinjuku Ku, Tokyo 1628601, Japan. [Enoto, Teruaki] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mihara, Tatehiro] RIKEN, MAXI Team, Wako, Saitama 3510198, Japan. [Nagase, Fumiaki] Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2298510, Japan. RP Asami, F (reprint author), RIKEN, Nishina Ctr, 2-1 Hirosawa, Wako, Saitama 3510198, Japan. EM asami@crab.riken.jp RI XRAY, SUZAKU/A-1808-2009; Mihara, Tatehiro/C-5536-2017 OI Mihara, Tatehiro/0000-0002-6337-7943 FU JSPS Fellows FX This work was supported by a Grant-in-Aid for JSPS Fellows. NR 32 TC 1 Z9 1 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD APR PY 2014 VL 66 IS 2 AR 44 DI 10.1093/pasj/psu005 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL8YZ UT WOS:000339427200006 ER PT J AU Sasano, M Makishima, K Sakurai, S Zhang, Z Enoto, T AF Sasano, Makoto Makishima, Kazuo Sakurai, Soki Zhang, Zhongli Enoto, Teruaki TI Suzaku view of the neutron star in the dipping source 4U 1822-37 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE accretion, accretion disks; stars: magnetic fields; X-rays: binaries ID X-RAY BINARIES; ACCRETION DISK; BOARD SUZAKU; SOURCE X1822-371; MAGNETIC-FIELDS; ORBITAL-PERIOD; EMISSION-LINES; SPIN PERIOD; SPECTROSCOPY; PULSARS AB The dipping X-ray source 4U 1822-37 was observed by Suzaku on 2006 October 20 for a net exposure of 37 ks. The source was detected with the XIS at a 1-10 keV flux of 5.5 x 10(-10) erg cm(-2) s(-1), and with the HXD (HXD-PIN) at a 10-50 keV flux of 8.9 x 10(-10) erg cm(-2) s(-1). With HXD-PIN, the pulsation was detected at a barycentric period of 0.592437 s, and its change rate was reconfirmed as -2.43 x 10(-12) s s(-1). The 1-50 keV spectra of 4U 1822-37 were found to be very similar to those of Her X-1 in the slopes, cutoff, and iron lines. Three iron lines (Fe K alpha, Fe XXV, and Fe XXVI) were detected, on top of a 1-50 keV continuum that is described by an NPEX model plus a soft blackbody. In addition, a cyclotron resonance scattering feature was detected significantly (> 99% confidence), at an energy of 33 +/- 2 keV with a depth of 0.4(-0.3)(+0.6). Therefore, the neutron star in this source is concluded to have a strong magnetic field of 2.8 x 10(12) G. Further assuming that the source has a relatively high intrinsic luminosity of several times 10(37) erg s(-1), its spectral and timing properties are consistently explained. C1 [Sasano, Makoto; Makishima, Kazuo; Sakurai, Soki; Zhang, Zhongli] Univ Tokyo, Sch Sci, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Makishima, Kazuo; Enoto, Teruaki] RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. [Makishima, Kazuo] Univ Tokyo, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. [Enoto, Teruaki] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Sasano, M (reprint author), Univ Tokyo, Sch Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. EM sasano@juno.phys.s.u-tokyo.ac.jp RI XRAY, SUZAKU/A-1808-2009 FU JSPS [23244024, 24-3320] FX We thank all members of the Suzaku hardware and software teams and the Science Working Group. M. S., K. M., and T. E. are supported by the Japan Society for the Promotion of Science (JSPS) Research Fellowship for Young Scientists, Grant-in-Aid for Scientific Research (A) (23244024) from JSPS, and Grant-in-Aid for JSPS Fellows, 24-3320, respectively. NR 40 TC 7 Z9 7 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD APR PY 2014 VL 66 IS 2 AR 35 DI 10.1093/pasj/psu002 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL8YZ UT WOS:000339427200003 ER PT J AU Frazer, RE Coleman, DS Mills, RD AF Frazer, Ryan E. Coleman, Drew S. Mills, Ryan D. TI Zircon U-Pb geochronology of the Mount Givens Granodiorite: Implications for the genesis of large volumes of eruptible magma SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID CENTRAL SIERRA-NEVADA; FISH CANYON MAGMA; JUAN VOLCANIC FIELD; TUFF AEGEAN ARC; NEW-ZEALAND; AR-40/AR-39 CHRONOLOGY; PLUTON EMPLACEMENT; ADAMELLO BATHOLITH; CALDERA COMPLEX; INTRUSIVE SUITE AB The Mount Givens Granodiorite, a large pluton in the central Sierra Nevada batholith, California, is similar in area to zoned intrusive suites yet is comparatively chemically and texturally homogenous. New zircon U-Pb geochronology indicates that the pluton was constructed over at least 7 Ma from 97.92 +/- 0.06 Ma to 90.87 +/- 0.05 Ma. Combining the new geochronology with the exposed volume of the pluton yields an estimated magma flux of <0.001 km(3)/a. The geochronologic data are at odds with the previously speculated links between plutons such as the Mount Givens Granodiorite and large-volume homogeneous ignimbrites (often termed monotonous intermediates). Existing data indicate that large plutons accumulate at rates of <= 0.001 km(3)/a, 1-2 orders of magnitude less than fluxes calculated for dated monotonous intermediates. If monotonous intermediates are remobilized, erupted plutons accumulated at rates comparable to dated examples, they should preserve a record of zircon growth of up to 10 Ma. Alternatively, the long history of zircon growth recorded in plutons may be erased during the processes of reheating and remobilization that precede supervolcano eruption. However, zircon dissolution modeling, based on hypothetical temperature-time histories for preeruptive monotonous intermediates, indicates that rejuvenation events would not sufficiently dissolve zircon. We suggest that eruptions of monotonous intermediates occur during high magmatic flux events, leaving little behind in the intrusive rock record, whereas low fluxes favor pluton accumulation. C1 [Frazer, Ryan E.; Coleman, Drew S.] Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27514 USA. [Mills, Ryan D.] NASA JSC, Astromat Res & Explorat Sci Directorate, Houston, TX USA. RP Frazer, RE (reprint author), Univ N Carolina, Dept Geol Sci, Mitchell Hall, Chapel Hill, NC 27514 USA. EM ryan.frazer@unc.edu FU UNC Department of Geological Sciences Martin Fund; Sigma Xi; Geological Society of America FX Frazer was supported by grants from the UNC Department of Geological Sciences Martin Fund, Sigma Xi, and the Geological Society of America. Courtney Beck and Daniel Gurganus provided field assistance, and Jeremy Inglis and Miquela Ingalls gave useful laboratory aid. Informal reviews by Allen Glazner and Kevin Stewart on an earlier version of the manuscript helped refine the ideas presented here. We thank Bruce Watson for discussions about zircon dissolution. Editor Michael Walter, Catherine Annen, and an anonymous reviewer provided comments that led to a much stronger presentation. NR 108 TC 12 Z9 12 U1 1 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD APR PY 2014 VL 119 IS 4 BP 2907 EP 2924 DI 10.1002/2013JB010716 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AJ4ZG UT WOS:000337688600018 ER PT J AU Chambon, P Zhang, SQ Hou, AY Zupanski, M Cheung, S AF Chambon, Philippe Zhang, Sara Q. Hou, Arthur Y. Zupanski, Milija Cheung, Samson TI Assessing the impact of pre-GPM microwave precipitation observations in the Goddard WRF ensemble data assimilation system SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE precipitation; ensemble data assimilation; microwave observations; forecasts verification; Global Precipitation Measurement Mission ID RADAR RAINFALL PRODUCT; CLOUD-RESOLVING MODEL; VARIATIONAL ASSIMILATION; KALMAN FILTER; PART I; RADIANCES; FORECASTS; SCHEME; IMAGER; RATES AB The forthcoming Global Precipitation Measurement (GPM) Mission will provide next-generation precipitation observations from a constellation of satellites. Since precipitation by nature has large variability and low predictability at cloud-resolving scales, the impact of precipitation data on the skills of mesoscale numerical weather prediction (NWP) is largely affected by the characterization of background and observation errors and the representation of nonlinear cloud/precipitation physics in an NWP data assimilation system. We present a data impact study on the assimilation of precipitation-affected microwave (MW) radiances from a pre-GPM satellite constellation using the Goddard WRF Ensemble Data Assimilation System (Goddard WRF-EDAS). A series of assimilation experiments are carried out in a Weather Research Forecast (WRF) model domain of 9 km resolution in western Europe. Sensitivities to observation error specifications, background error covariance estimated from ensemble forecasts with different ensemble sizes, and MW channel selections are examined through single-observation assimilation experiments. An empirical bias correction for precipitation-affected MW radiances is developed based on the statistics of radiance innovations in rainy areas. The data impact is assessed by full data assimilation cycling experiments for a storm event that occurred in France in September 2010. Results show that the assimilation of MW precipitation observations from a satellite constellation mimicking GPM has a positive impact on the accumulated rain forecasts verified with surface radar rain estimates. The case-study on a convective storm also reveals that the accuracy of ensemble-based background error covariance is limited by sampling errors and model errors such as precipitation displacement and unresolved convective scale instability. C1 [Chambon, Philippe] Univ Space Res Assoc, Columbia, MD USA. [Chambon, Philippe; Zhang, Sara Q.; Hou, Arthur Y.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Zupanski, Milija] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. [Cheung, Samson] Univ Calif Davis, Dept Math, Davis, CA 95616 USA. RP Zhang, SQ (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA. EM sara.q.zhang@nasa.gov RI Measurement, Global/C-4698-2015 FU Global precipitation Measurement (GPM) Flight Project at NASA Goddard Space Flight Center; French Ministry of the environment FX The authors thank Wesley Berg at Colorado State University for providing the SSMIS FCDR inter-calibrated brightness temperature dataset, and Meteo-France and HyMex database teams (ESPRI/IPSL, SEDOO/OMP) for providing the surface rainfall product from the ARAMIS radar network. Jean-Francois Mahfouf and Chris Kidd are acknowledged for their helpful remarks. Jan Angevine is recognized for editing the manuscript. The authors are grateful to two anonymous reviewers for their insightful and constructive comments that improved the article. This research is supported by the Global precipitation Measurement (GPM) Flight Project at NASA Goddard Space Flight Center and the French Ministry of the environment. Computations were performed at NASA Advanced Supercomputing (NAS). NR 50 TC 3 Z9 3 U1 4 U2 12 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD APR PY 2014 VL 140 IS 681 BP 1219 EP 1235 DI 10.1002/qj.2215 PN B PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ4ED UT WOS:000337623500008 ER PT J AU Holdaway, D Errico, R AF Holdaway, D. Errico, R. TI Using Jacobian sensitivities to assess a linearization of the relaxed Arakawa-Schubert convection scheme SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE adjoint; tangent linear; convection; 4D-Var; sensitivity; principle components; parametrization ID 4-DIMENSIONAL VARIATIONAL ASSIMILATION; MOIST PHYSICS SCHEMES; OPERATIONAL IMPLEMENTATION; ADJOINT SENSITIVITY; INITIAL CONDITIONS; OBSERVATION IMPACT; PROGNOSTIC CLOUD; MESOSCALE MODEL; ECMWF MODEL; PRECIPITATION AB The inclusion of linearized moist physics can increase the accuracy of 4D-Var data assimilation and adjoint-based sensitivity analysis. Moist processes such as convection can exhibit nonlinear behaviour. As a result, representation of these processes in a linear way requires much care; a straightforward linearization may yield a poor approximation to the behaviour of perturbations of interest and could contain numerical instability. Here, an extensive numerical study of the Jacobian of the relaxed Arakawa-Schubert (RAS) convection scheme is shown. A Jacobian based on perturbations at individual model levels can be used to understand the physical behaviour of the RAS scheme, predict how sensitive that behaviour is to the prognostic variables and determine the stability of a linearization of the scheme. The linearity of the scheme is also considered by making structured perturbations, constructed from the principle components of the model variables. Based on the behaviour of the Jacobian operator and the results when using structured perturbations, a suitable method for linearizing the RAS scheme is determined. For deep, strong convection, the structures of the RAS Jacobian are reasonably simple, the rate at which finite-amplitude estimates of the structures change with respect to input perturbations is small and the eigenmodes of the Jacobian are not prohibitively unstable. For deep convection, an exact linearization is therefore suitable. For shallow convection, the RAS scheme can be more sensitive to the input prognostic variables due to the faster time-scales and proximity to switches. Linearization of the RAS therefore requires some simplifications to smooth the behaviour for shallow convection. It is noted that the physical understanding of the scheme gained from examining the Jacobian provides a useful tool to the developers of nonlinear physical parametrizations. C1 [Holdaway, D.; Errico, R.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Holdaway, D.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Greenbelt, MD USA. [Errico, R.] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD USA. RP Holdaway, D (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA. EM dan.holdaway@nasa.gov RI Holdaway, Daniel/Q-5198-2016 OI Holdaway, Daniel/0000-0002-3672-2588 NR 38 TC 2 Z9 2 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD APR PY 2014 VL 140 IS 681 BP 1319 EP 1332 DI 10.1002/qj.2210 PN B PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ4ED UT WOS:000337623500017 ER PT J AU Igel, MR van den Heever, SC Stephens, GL Posselt, DJ AF Igel, Matthew R. van den Heever, Susan C. Stephens, Graeme L. Posselt, Derek J. TI Convective-scale responses of a large-domain, modelled tropical environment to surface warming SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE convection; climate; cloud-resolving models ID CLOUD-RESOLVING MODEL; WATER-VAPOR; TROPOSPHERIC HUMIDITY; EXTREME PRECIPITATION; HYDROLOGICAL CYCLE; MOISTURE-CONTENT; DEEP CONVECTION; SIMULATIONS; CLIMATE; TRENDS AB This article explores the response of convective-scale atmospheric characteristics to surface temperature through the lens of large-domain, cloud-system-resolving model experiments run at radiative convective equilibrium. We note several features reminiscent of the response to surface warming in atmospheric general circulation models. These include an increase in the rain rate that is smaller than the modelled increase in precipitable water, a systematic decrease in sensible heating and an increase in clear-sky cooling. However, in contrast to climate models, we note that tropospheric relative humidity increases and column-integrated water vapour increases at the rate anticipated from the Clausius-Clapeyron relationship, but only when compared with the troposphere mean temperature rather than surface temperature. Also shown are results elucidating the changes in the vertically integrated water budget and the distribution of high precipitation rates shifting toward higher rates. Moist static energy distributions are analyzed and, from these, clouds are implicated in effecting the final equilibrium state of the atmosphere. The results indicate that, while there are aspects of the tropical equilibrium that are represented realistically in current general circulation model climate-change experiments, there are potentially influential local interactions that are sufficiently important as to alter the mean response of the tropical water and energy balance to changes in sea-surface temperature. Convection is shown to dictate the equilibrium state across all scales, including those unresolved in climate models, rather than only responding to surface-induced changes. C1 [Igel, Matthew R.; van den Heever, Susan C.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Posselt, Derek J.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Igel, MR (reprint author), Colorado State Univ, Dept Atmospher Sci, 1371 Campus Delivery, Ft Collins, CO 80523 USA. EM MattIgel@atmos.colostate.edu RI Igel, Matthew/A-5727-2013; van den Heever, Susan/E-8728-2011; Posselt, Derek/I-4912-2012 OI Igel, Matthew/0000-0001-8916-544X; van den Heever, Susan/0000-0001-9843-3864; Posselt, Derek/0000-0002-5670-5822 FU NASA CloudSat grant [5-319160]; NASA [49683]; NASA Modelling, Analysis, and Prediction grant [NNX09AJ43G] FX This work was supported by NASA CloudSat grant 5-319160. S. van den Heever was supported by NASA grant 49683. A. D. Posselt was supported by NASA Modelling, Analysis, and Prediction grant NNX09AJ43G. The authors thank two anonymous reviewers who helped to make this document more precise. NR 60 TC 1 Z9 1 U1 0 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD APR PY 2014 VL 140 IS 681 BP 1333 EP 1343 DI 10.1002/qj.2230 PN B PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ4ED UT WOS:000337623500018 ER PT J AU Baker, WE Atlas, R Cardinali, C Clement, A Emmitt, GD Gentry, BM Hardesty, RM Kallen, E Kavaya, MJ Langland, R Ma, ZZ Masutani, M McCarty, W Pierce, RB Pu, ZX Riishojgaard, LP Ryan, J Tucker, S Weissmann, M Yoe, JG AF Baker, Wayman E. Atlas, Robert Cardinali, Carla Clement, Amy Emmitt, George D. Gentry, Bruce M. Hardesty, R. Michael Kaellen, Erland Kavaya, Michael J. Langland, Rolf Ma, Zaizhong Masutani, Michiko McCarty, Will Pierce, R. Bradley Pu, Zhaoxia Riishojgaard, Lars Peter Ryan, James Tucker, Sara Weissmann, Martin Yoe, James G. TI LIDAR-MEASURED WIND PROFILES The Missing Link in the Global Observing System SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID DATA ASSIMILATION SYSTEM; VARIATIONAL DATA ASSIMILATION; INCOHERENT DOPPLER LIDAR; OBSERVATION IMPACT; AIRBORNE DEMONSTRATOR; SPECTRAL ANALYZER; ERA-40 REANALYSIS; MIDDLE ATMOSPHERE; EDGE TECHNIQUE; SOLID-STATE C1 [Baker, Wayman E.] NOAA, Mchenry, MD USA. [Atlas, Robert] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA. [Cardinali, Carla; Kaellen, Erland] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. [Clement, Amy] Univ Miami, Miami, FL USA. [Emmitt, George D.] Simpson Weather Associates, Charlottesville, VA USA. [Gentry, Bruce M.; McCarty, Will] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Hardesty, R. Michael] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Kavaya, Michael J.] NASA Langley Res Ctr, Hampton, VA USA. [Langland, Rolf] Naval Res Lab, Monterey, CA USA. [Riishojgaard, Lars Peter] World Meteorol Org, Geneva, Switzerland. [Ma, Zaizhong; Yoe, James G.] Joint Ctr Satellite Data Assimilat, College Pk, MD USA. [Masutani, Michiko] NOAA, Environm Modeling Ctr, College Pk, MD USA. [Pierce, R. Bradley] NOAA, Natl Environm Satellite Data & Informat Serv, Madison, WI USA. [Pu, Zhaoxia] Univ Utah, Salt Lake City, UT USA. [Ryan, James] Univ New Hampshire, Durham, NH 03824 USA. [Tucker, Sara] Ball Aerosp & Technol Corp, Boulder, CO USA. [Weissmann, Martin] Univ Munich, Hans Ertel Ctr Weather Res, Munich, Germany. RP Baker, WE (reprint author), 253 Gleanings Dr, Mchenry, MD 21541 USA. EM wayman.baker@gmail.com RI Weissmann, Martin/C-9084-2013; Pierce, Robert Bradley/F-5609-2010; Atlas, Robert/A-5963-2011; Manager, CSD Publications/B-2789-2015 OI Pierce, Robert Bradley/0000-0002-2767-1643; Atlas, Robert/0000-0002-0706-3560; FU Earth Science Division at NASA headquarters; NASA Earth Science Technology Office at the Goddard Space Flight Center; SWA; German Federal Ministry of Transport, Building and Urban Development FX The authors thank Dr. Ramesh Kakar of the Earth Science Division at NASA headquarters and Dr. George Komar of the NASA Earth Science Technology Office at the Goddard Space Flight Center for supporting research with DWL data, including airborne campaigns, and funding hardware risk reduction studies to advance the readiness of the DWL technology for space. The authors thank Dr. John Cortinas and NOAA's Office of Weather and Air Quality for contributing to the support for DWL OSSEs through NOAA's OSSE Testbed. The expert assistance of Paul Berrisford of ECMWF is sincerely acknowledged. Sidney Wood and Steven Greco of Simpson Weather Associates (SWA) are acknowledged for their dedication to producing simulated space-based DWL observations used in the OSSEs and processing and analyzing data from the U.S. Navy's airborne DWL. Funding for manuscript preparation and submission was provided by SWA. M. Weissmann is part of the Hans-Ertel Centre for Weather Research, a network of universities, research institutes, and Deutscher Wetterdienst funded by the German Federal Ministry of Transport, Building and Urban Development. NR 131 TC 24 Z9 25 U1 3 U2 24 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 APR PY 2014 VL 95 IS 4 BP 543 EP 564 DI 10.1175/BAMS-D-12-00164.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AI8MK UT WOS:000337170300006 ER PT J AU Kirtman, BP Min, D Infanti, JM Kinter, JL Paolino, DA Zhang, Q van den Dool, H Saha, S Mendez, MP Becker, E Peng, PT Tripp, P Huang, J DeWitt, DG Tippett, MK Barnston, AG Li, SH Rosati, A Schubert, SD Rienecker, M Suarez, M Li, ZE Marshak, J Lim, YK Tribbia, J Pegion, K Merryfield, WJ Denis, B Wood, EF AF Kirtman, Ben P. Min, Dughong Infanti, Johnna M. Kinter, James L., III Paolino, Daniel A. Zhang, Qin van den Dool, Huug Saha, Suranjana Mendez, Malaquias Pena Becker, Emily Peng, Peitao Tripp, Patrick Huang, Jin DeWitt, David G. Tippett, Michael K. Barnston, Anthony G. Li, Shuhua Rosati, Anthony Schubert, Siegfried D. Rienecker, Michele Suarez, Max Li, Zhao E. Marshak, Jelena Lim, Young-Kwon Tribbia, Joseph Pegion, Kathleen Merryfield, William J. Denis, Bertrand Wood, Eric F. TI THE NORTH AMERICAN MULTIMODEL ENSEMBLE Phase-1 Seasonal-to-Interannual Prediction; Phase-2 toward Developing Intraseasonal Prediction SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID DATA ASSIMILATION SYSTEM; UNITED-STATES; FORECAST SYSTEM; ENSO PREDICTION; CLIMATE; MODEL; IMPACT; SKILL; PROBABILITY; CALIBRATION C1 [Kirtman, Ben P.; Min, Dughong; Infanti, Johnna M.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Kinter, James L., III; Paolino, Daniel A.] Ctr Ocean Land Atmosphere Studies, Calverton, MD USA. [Zhang, Qin; van den Dool, Huug; Saha, Suranjana; Mendez, Malaquias Pena; Becker, Emily; Peng, Peitao; Tripp, Patrick; Huang, Jin] NOAA, Natl Ctr Environm Predict, Camp Springs, MD USA. [DeWitt, David G.; Tippett, Michael K.; Barnston, Anthony G.; Li, Shuhua] Int Res Inst Climate & Soc, Palisades, NY USA. [Tippett, Michael K.] King Abdulaziz Univ, Dept Meteorol, Ctr Excellence Climate Change Res, Jeddah 21413, Saudi Arabia. [Rosati, Anthony] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Schubert, Siegfried D.; Rienecker, Michele; Suarez, Max; Li, Zhao E.; Marshak, Jelena; Lim, Young-Kwon] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Tribbia, Joseph] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Pegion, Kathleen] Univ Colorado, CIRES, Boulder, CO 80309 USA. [Merryfield, William J.; Denis, Bertrand] Environm Canada, Fredericton, NB, Canada. [Wood, Eric F.] Princeton Univ, Princeton, NJ 08544 USA. RP Kirtman, BP (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. EM bkirtman@rsmas.miami.edu RI Tippett, Michael/C-6286-2011 OI Tippett, Michael/0000-0002-7790-5364 FU NOAA MAPP program; NOAA MAPP; NSF; NASA; DOE FX The phase-1 NMME project was supported by the NOAA MAPP program, and the phase-2 NMME project is support by NOAA MAPP, NSF, NASA, and the DOE. NR 34 TC 98 Z9 98 U1 3 U2 34 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 APR PY 2014 VL 95 IS 4 BP 585 EP 601 DI 10.1175/BAMS-D-12-00050.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AI8MK UT WOS:000337170300009 ER PT J AU Lin, HW McCarty, JL Wang, DD Rogers, BM Morton, DC Collatz, GJ Jin, YF Randerson, JT AF Lin, Hsiao-Wen McCarty, Jessica L. Wang, Dongdong Rogers, Brendan M. Morton, Douglas C. Collatz, G. James Jin, Yufang Randerson, James T. TI Management and climate contributions to satellite-derived active fire trends in the contiguous United States SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article DE agriculture; air quality; carbon cycle; wildfire; aerosols ID IMAGING SPECTRORADIOMETER MODIS; BURNED AREA; FOREST-FIRES; WILDFIRE; NORTH; VALIDATION; ALGORITHMS; WEATHER; EMISSIONS; INCREASE AB Fires in croplands, plantations, and rangelands contribute significantly to fire emissions in the United States, yet are often overshadowed by wildland fires in efforts to develop inventories or estimate responses to climate change. Here we quantified decadal trends, interannual variability, and seasonality of Terra Moderate Resolution Imaging Spectroradiometer (MODIS) observations of active fires (thermal anomalies) as a function of management type in the contiguous U.S. during 2001-2010. We used the Monitoring Trends in Burn Severity database to identify active fires within the perimeter of large wildland fires and land cover maps to identify active fires in croplands. A third class of fires defined as prescribed/other included all residual satellite active fire detections. Large wildland fires were the most variable of all three fire types and had no significant annual trend in the contiguous U.S. during 2001-2010. Active fires in croplands, in contrast, increased at a rate of 3.4% per year. Cropland and prescribed/other fire types combined were responsible for 77% of the total active fire detections within the U.S and were most abundant in the south and southeast. In the west, cropland active fires decreased at a rate of 5.9% per year, likely in response to intensive air quality policies. Potential evaporation was a dominant regulator of the interannual variability of large wildland fires, but had a weaker influence on the other two fire types. Our analysis suggests it may be possible to modify landscape fire emissions within the U.S. by influencing the way fires are used in managed ecosystems. C1 [Lin, Hsiao-Wen; Rogers, Brendan M.; Jin, Yufang; Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [McCarty, Jessica L.] Michigan Tech Res Inst, Ann Arbor, MI USA. [Wang, Dongdong] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Morton, Douglas C.; Collatz, G. James] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. RP Lin, HW (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. EM hwlin@uci.edu RI Wang, Dongdong/M-1969-2014; collatz, george/D-5381-2012; Morton, Douglas/D-5044-2012 OI Wang, Dongdong/0000-0002-2076-576X; FU NASA [NNX08AR69G, NNX10AL14G, NNX11AF96G]; Taiwan Merit Fellowship [TMF-94-1A-016] FX This research was funded by NASA grants NNX08AR69G and NNX10AL14G to Jin and NNX11AF96G to Randerson. Lin received support from Taiwan Merit Fellowship (TMF-94-1A-016). The audience may access the data in this paper via contacting the authors. NR 72 TC 5 Z9 5 U1 3 U2 25 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 APR PY 2014 VL 119 IS 4 BP 645 EP 660 DI 10.1002/2013JG002382 PG 16 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA AI9UN UT WOS:000337285500011 ER PT J AU Komendera, E Reishus, D Dorsey, JT Doggett, WR Correll, N AF Komendera, Erik Reishus, Dustin Dorsey, John T. Doggett, William R. Correll, Nikolaus TI Precise truss assembly using commodity parts and low precision welding SO INTELLIGENT SERVICE ROBOTICS LA English DT Article DE Robotic assembly; Autonomous robots; Precision manipulation; Space robotics; Distributed robots AB Hardware and software design and system integration for an intelligent precision jigging robot (IPJR), which allows high precision assembly using commodity parts and low-precision bonding, is described. Preliminary 2D experiments that aremotivated by the problem of assembling space telescope optical benches and very large manipulators on orbit using inexpensive, stock hardware and low-precision welding are also described. An IPJR is a robot that acts as the precise "jigging", holding parts of a local structure assembly site in place, while an external low precision assembly agent cuts and welds members. The prototype presented in this paper allows an assembly agent (for this prototype, a human using only low precision tools), to assemble a 2D truss made of wooden dowels to a precision on the order of millimeters over a span on the order of meters. The analysis of the assembly error and the results of building a square structure and a ring structure are discussed. Options for future work, to extend the IPJR paradigm to building in 3D structures at micron precision are also summarized. C1 [Komendera, Erik; Reishus, Dustin; Correll, Nikolaus] Univ Colorado, Dept Comp Sci, Boulder, CO 80309 USA. [Dorsey, John T.; Doggett, William R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Komendera, E (reprint author), Univ Colorado, Dept Comp Sci, Boulder, CO 80309 USA. EM erik.komendera@colorado.edu; dustin.reishus@colorado.edu; john.t.dorsey@nasa.gov; bill.doggett@nasa.gov; nikolaus.correll@colorado.edu FU NASA Office of the Chief Technologist's Space Technology Research Fellowship FX This work was supported by a NASA Office of the Chief Technologist's Space Technology Research Fellowship. NR 17 TC 2 Z9 2 U1 1 U2 9 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1861-2776 EI 1861-2784 J9 INTEL SERV ROBOT JI Intell. Serv. Robot. PD APR PY 2014 VL 7 IS 2 SI SI BP 93 EP 102 DI 10.1007/s11370-013-0144-4 PG 10 WC Robotics SC Robotics GA AI4QN UT WOS:000336850000005 ER PT J AU Sun-Mack, S Minnis, P Chen, Y Kato, S Yi, YH Gibson, SC Heck, PW Winker, DM AF Sun-Mack, Sunny Minnis, Patrick Chen, Yan Kato, Seiji Yi, Yuhong Gibson, Sharon C. Heck, Patrick W. Winker, David M. TI Regional Apparent Boundary Layer Lapse Rates Determined from CALIPSO and MODIS Data for Cloud-Height Determination SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID A-TRAIN; SATELLITE AB Reliably determining low-cloud heights using a cloud-top temperature from satellite infrared imagery is often challenging because of difficulties in characterizing the local thermal structure of the lower troposphere with the necessary precision and accuracy. To improve low-cloud-top height estimates over water surfaces, various methods have employed lapse rates anchored to the sea surface temperature to replace the boundary layer temperature profiles that relate temperature to altitude. To further improve low-cloud-top height retrievals, collocated Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) and Aqua Moderate Resolution Imaging Spectroradiometer (MODIS) data taken from July 2006 to June 2007 and from June 2009 to May 2010 (2 yr) for single-layer low clouds are used here with numerical weather model analyses to develop regional mean boundary apparent lapse rates. These parameters are designated as apparent lapse rates because they are defined using the cloud-top temperatures from satellite retrievals and surface skin temperatures; they do not represent true lapse rates. Separate day and night, seasonal mean lapse rates are determined for 100-resolution snow-free land, water, and coastal regions, while zonally dependent lapse rates are developed for snow/ice-covered areas for use in the Clouds and the Earth's Radiant Energy System (CERES) Edition 4 cloud property retrieval system (CCPRS-4). The derived apparent lapse rates over ice-free water range from 5 to 9K km(-1) with mean values of about 6.9 and 7.2K km(-1) during the day and night, respectively. Over land, the regional values vary from 3 to 8K km(-1), with day and night means of 5.5 and 6.2K km(-1), respectively. The zonal-mean apparent lapse rates over snow and ice surfaces generally decrease with increasing latitude, ranging from 4 to 8K km(-1). All of the CCPRS-4 lapse rates were used along with five other lapse rate techniques to retrieve cloud-top heights for 2 months of independent Aqua MODIS data. When compared with coincident CALIPSO data for October 2007, the mean cloud-top height differences between CCPRS-4 and CALIPSO during the daytime (nighttime) are 0.04 +/- 0.61 km(0.10 +/- 0.62 km) over ice-free water, 20.06 +/- 0.85 km(-0.01 +/- 0.83 km) over snow-free land, and 0.38 +/- 0.95km (0.03 +/- 0.92 km) over snow-covered areas. The CCPRS-4 regional monthly means are generally unbiased and lack spatial error gradients seen in the comparisons for most of the other techniques. Over snow-free land, the regional monthly-mean errors range from -0.28 +/- 0.74 km during daytime to 0.04 +/- 0.78 km at night. The water regional monthly means are, on average, 0.04 +/- 0.44 km less than the CALIPSO values during day and night. Greater errors are realized for snow-covered regions. Overall, the CCPRS-4 lapse rates yield the smallest RMS differences for all times of day over all areas both for individual retrievals and monthly means. These new regional apparent lapse rates, used in processing CERES Edition 4 data, should provide more accurate low-cloud-type heights than previously possible using satellite imager data. C1 [Sun-Mack, Sunny; Chen, Yan; Yi, Yuhong; Gibson, Sharon C.] SSAI, Hampton, VA 23666 USA. [Minnis, Patrick; Kato, Seiji; Winker, David M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Heck, Patrick W.] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI USA. RP Sun-Mack, S (reprint author), SSAI, 1 Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA. EM szedung.sun-mack-1@nasa.gov RI Minnis, Patrick/G-1902-2010 OI Minnis, Patrick/0000-0002-4733-6148 FU NASA CERES Project FX Thanks are given to the three anonymous reviewers for their helpful comments. This research was supported by the NASA CERES Project. The CCCM data were obtained at http://ceres.larc.nasa.gov/compare_products-ed2.php. The GOES and Rapid Refresh analyses were acquired at the NASA Langley Satellite Imagery and Cloud Products Page: http://cloudsgate2.larc.nasa.gov/index.html. NR 33 TC 10 Z9 10 U1 2 U2 7 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 APR PY 2014 VL 53 IS 4 BP 990 EP 1011 DI 10.1175/JAMC-D-13-081.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH9GG UT WOS:000336449300013 ER PT J AU Kratz, DP Stackhouse, PW Gupta, SK Wilber, AC Sawaengphokhai, P McGarragh, GR AF Kratz, David P. Stackhouse, Paul W., Jr. Gupta, Shashi K. Wilber, Anne C. Sawaengphokhai, Parnchai McGarragh, Greg R. TI The Fast Longwave and Shortwave Flux (FLASHFlux) Data Product: Single-Scanner Footprint Fluxes SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID ANGULAR-DISTRIBUTION MODELS; SYNCHRONOUS SATELLITE DATA; ENERGY SYSTEM INSTRUMENT; SURFACE RADIATION; SOLAR-RADIATION; TERRA SATELLITE; ANNUAL CYCLE; PART II; CERES; BUDGET AB The Clouds and the Earth's Radiant Energy Systems (CERES) project utilizes radiometric measurements taken aboard the Terra and Aqua spacecrafts to derive the world-class data products needed for climate research. Achieving the exceptional fidelity of the CERES data products, however, requires a considerable amount of processing to assure quality and to verify accuracy and precision, which results in the CERES data being released more than 6 months after the satellite observations. For most climate studies such delays are of little consequence; however, there are a significant number of near-real time uses for CERES data products. The Fast Longwave and Shortwave Radiative Flux (FLASHFlux) data product was therefore developed to provide a rapid release version of the CERES results, which could be made available to the research and applications communities within 1 week of the satellite observations by exchanging some accuracy for speed. FLASHFlux has both achieved this 1-week processing objective and demonstrated the ability to provide remarkably good agreement when compared with the CERES data products for both the instantaneous single-scanner footprint (SSF) fluxes and the time-and space-averaged (TISA) fluxes. This paper describes the methods used to expedite the production of the FLASHFlux SSF fluxes by utilizing data from the CERES and Moderate Resolution Imaging Spectroradiometer instruments, as well as other meteorological sources. This paper also reports on the validation of the FLASHFlux SSF results against ground-truth measurements and the intercomparison of FLASHFlux and CERES SSF results. A complementary paper will discuss the production and validation of the FLASHFlux TISA fluxes. C1 [Kratz, David P.; Stackhouse, Paul W., Jr.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Gupta, Shashi K.; Wilber, Anne C.; Sawaengphokhai, Parnchai] Sci Syst & Applicat Inc, Hampton, VA USA. [McGarragh, Greg R.] Colorado State Univ, Ft Collins, CO 80523 USA. RP Kratz, DP (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM david.p.kratz@nasa.gov FU NASA Science Mission Directorate as part of the CERES project FX ARM data have been made available through the U.S. Department of Energy as part of the Atmospheric Radiation Measurement Program. GMD data have been made available through NOAA's Earth System Research Laboratory/Global Monitoring Division-Radiation (G-RAD). SURFRAD data have been made available through NOAA's Air Resources Laboratory/Surface Radiation Research Branch. Snow and ice data were provided through the National Snow and Ice Data Center. The authors thank D. A. Rutan for providing access to the CERES/ARM Validation Experiment (CAVE) database, and A. C. Edwards and J. C. Mikovitz for providing programming assistance. The authors would also like to thank G. G. Gibson and N. G. Loeb for providing valuable advice and suggestions regarding the manuscript. This research was supported through the NASA Science Mission Directorate as part of the CERES project. NR 59 TC 4 Z9 4 U1 0 U2 8 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 APR PY 2014 VL 53 IS 4 BP 1059 EP 1079 DI 10.1175/JAMC-D-13-061.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH9GG UT WOS:000336449300017 ER PT J AU Kulie, MS Hiley, MJ Bennartz, R Kneifel, S Tanelli, S AF Kulie, Mark S. Hiley, Michael J. Bennartz, Ralf Kneifel, Stefan Tanelli, Simone TI Triple-Frequency Radar Reflectivity Signatures of Snow: Observations and Comparisons with Theoretical Ice Particle Scattering Models SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID SIZE SPECTRA; CLOUD ICE; MICROWAVE-FREQUENCIES; PRECIPITATION RADAR; WAKASA BAY; DISTRIBUTIONS; PARAMETERIZATION; APPROXIMATION; MIDLATITUDE; SNOWFLAKES AB An observation-based study is presented that utilizes aircraft data from the 2003 Wakasa Bay Advanced Microwave Scanning Radiometer Precipitation Validation Campaign to assess recent advances in the modeling of microwave scattering properties of nonspherical ice particles in the atmosphere. Previous work has suggested that a triple-frequency (Ku-Ka-W band) reflectivity framework appears capable of identifying key microphysical properties of snow, potentially providing much-needed constraints on significant sources of uncertainty in current snowfall retrieval algorithms used for microwave remote sensing instruments. However, these results were based solely on a modeling framework. In contrast, this study considers the triple-frequency approach from an observational perspective using airborne radar observations from the Wakasa Bay field campaign. After accounting for several challenges with the observational dataset, such as beam mismatching and attenuation, observed dual-wavelength ratio results are presented that confirm both the utility of a multifrequency approach to snowfall retrieval and the validity of the unique signatures predicted by complex aggregate ice particle scattering models. This analysis provides valuable insight into the microphysics of frozen precipitation that can in turn be applied to more readily available single-and dual-frequency systems, providing guidance for future precipitation retrieval algorithms. C1 [Kulie, Mark S.; Hiley, Michael J.; Bennartz, Ralf] Univ Madison, Space Sci & Engn Ctr, Dept Atmospher & Ocean Sci, Madison, WI 53706 USA. [Kneifel, Stefan] Univ Cologne, Inst Geophys & Meteorol, Cologne, Germany. [Tanelli, Simone] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Kulie, MS (reprint author), Univ Madison, Space Sci & Engn Ctr, 1225 W Dayton St, Madison, WI 53706 USA. EM mskulie@wisc.edu RI Kneifel, Stefan/A-2044-2015; Kulie, Mark/C-3289-2011 OI Kneifel, Stefan/0000-0003-2220-2968; Kulie, Mark/0000-0003-1400-1007 FU NASA [NNX10AG83G, NNX12AQ76G, NNX13AG47G]; Precipitation Measurement Mission Program; Aerosol Clouds and Ecosystems Science Working Group FX This work was partially supported by NASA Grants NNX10AG83G, NNX12AQ76G, and NNX13AG47G. A portion of this research (Tanelli) was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Support by the Precipitation Measurement Mission Program and the Aerosol Clouds and Ecosystems Science Working Group are acknowledged. Data for the ACR during the Wakasa Bay Experiment were acquired and processed by Dr. Richard Austin. The APR-2 deployment was made possible by Dr. Eastwood Im and Dr. Stephen L. Durden. Constructive comments by three anonymous reviewers are also gratefully recognized. NR 55 TC 10 Z9 10 U1 1 U2 17 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 APR PY 2014 VL 53 IS 4 BP 1080 EP 1098 DI 10.1175/JAMC-D-13-066.1 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH9GG UT WOS:000336449300018 ER PT J AU Neigh, CSR Bolton, DK Diabate, M Williams, JJ Carvalhais, N AF Neigh, Christopher S. R. Bolton, Douglas K. Diabate, Mouhamad Williams, Jennifer J. Carvalhais, Nuno TI An Automated Approach to Map the History of Forest Disturbance from Insect Mortality and Harvest with Landsat Time-Series Data SO REMOTE SENSING LA English DT Article DE Landsat; AVHRR; forest; disturbance; mortality; insect; harvest; US; classification; decision tree ID MOUNTAIN PINE-BEETLE; REMOTELY SENSED DATA; ACCURACY ASSESSMENT; UNITED-STATES; BURN SEVERITY; PHOTOSYNTHETIC TRENDS; BUDWORM DEFOLIATION; LANDSCAPE PATTERNS; SAMPLING DESIGNS; FIRE DISTURBANCE AB Forests contain a majority of the aboveground carbon (C) found in ecosystems, and understanding biomass lost from disturbance is essential to improve our C-cycle knowledge. Our study region in the Wisconsin and Minnesota Laurentian Forest had a strong decline in Normalized Difference Vegetation Index (NDVI) from 1982 to 2007, observed with the National Ocean and Atmospheric Administration's (NOAA) series of Advanced Very High Resolution Radiometer (AVHRR). To understand the potential role of disturbances in the terrestrial C-cycle, we developed an algorithm to map forest disturbances from either harvest or insect outbreak for Landsat time-series stacks. We merged two image analysis approaches into one algorithm to monitor forest change that included: (1) multiple disturbance index thresholds to capture clear-cut harvest; and (2) a spectral trajectory-based image analysis with multiple confidence interval thresholds to map insect outbreak. We produced 20 maps and evaluated classification accuracy with air-photos and insect air-survey data to understand the performance of our algorithm. We achieved overall accuracies ranging from 65% to 75%, with an average accuracy of 72%. The producer's and user's accuracy ranged from a maximum of 32% to 70% for insect disturbance, 60% to 76% for insect mortality and 82% to 88% for harvested forest, which was the dominant disturbance agent. Forest disturbances accounted for 22% of total forested area (7349 km(2)). Our algorithm provides a basic approach to map disturbance history where large impacts to forest stands have occurred and highlights the limited spectral sensitivity of Landsat time-series to outbreaks of defoliating insects. We found that only harvest and insect mortality events can be mapped with adequate accuracy with a non-annual Landsat time-series. This limited our land cover understanding of NDVI decline drivers. We demonstrate that to capture more subtle disturbances with spectral trajectories, future observations must be temporally dense to distinguish between type and frequency in heterogeneous landscapes. C1 [Neigh, Christopher S. R.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Bolton, Douglas K.] Univ British Columbia, Dept Forest Resources Management, Vancouver, BC V6T 1Z4, Canada. [Diabate, Mouhamad] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Williams, Jennifer J.] Royal Bot Gardens, Herbarium, Richmond TW9 3AE, Surrey, England. [Carvalhais, Nuno] Max Planck Inst Biogeochem, D-07701 Jena, Germany. [Carvalhais, Nuno] Univ Nova Lisboa, FCT, DCEA, P-2829516 Caparica, Portugal. RP Bolton, DK (reprint author), Univ British Columbia, Dept Forest Resources Management, Vancouver, BC V6T 1Z4, Canada. EM christopher.s.neigh@nasa.gov; doug.k.bolton@alumni.ubc.ca; mdiabate@gmail.com; jenjwilliams@gmail.com; ncarval@bgc-jena.mpg.de RI Neigh, Christopher/D-4700-2012; OI Neigh, Christopher/0000-0002-5322-6340; Carvalhais, Nuno/0000-0003-0465-1436 FU NASA's Terrestrial Ecology program [NNH08ZDA001N-TE, NNH10ZDA001N-CARBON] FX This study was made possible by NASA's Terrestrial Ecology program under grants NNH08ZDA001N-TE and NNH10ZDA001N-CARBON. NR 91 TC 8 Z9 8 U1 1 U2 26 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD APR PY 2014 VL 6 IS 4 BP 2782 EP 2808 DI 10.3390/rs6042782 PG 27 WC Remote Sensing SC Remote Sensing GA AI3FT UT WOS:000336746900010 ER PT J AU Bhatt, R Doelling, DR Wu, AS Xiong, XX Scarino, BR Haney, CO Gopalan, A AF Bhatt, Rajendra Doelling, David R. Wu, Aisheng Xiong, Xiaoxiong (Jack) Scarino, Benjamin R. Haney, Conor O. Gopalan, Arun TI Initial Stability Assessment of S-NPP VIIRS Reflective Solar Band Calibration Using Invariant Desert and Deep Convective Cloud Targets SO REMOTE SENSING LA English DT Article DE satellite calibration; S-NPP VIIRS; radiometric stability; MODIS; CERES; invariant calibration targets ID ANGULAR-DISTRIBUTION MODELS; RADIATIVE FLUX ESTIMATION; ENERGY SYSTEM INSTRUMENT; NEAR-INFRARED CHANNELS; TERRA SATELLITE; ATMOSPHERE; SITES; VALIDATION; SENSORS; AVHRR AB The latest CERES FM-5 instrument launched onboard the S-NPP spacecraft will use the VIIRS visible radiances from the NASA Land Product Evaluation and Analysis Tool Elements (PEATE) product for retrieving the cloud properties associated with its TOA flux measurement. In order for CERES to provide climate quality TOA flux datasets, the retrieved cloud properties must be consistent throughout the record, which is dependent on the calibration stability of the VIIRS imager. This paper assesses the NASA calibration stability of the VIIRS reflective solar bands using the Libya-4 desert and deep convective clouds (DCC). The invariant targets are first evaluated for temporal natural variability. It is found for visible (VIS) bands that DCC targets have half of the variability of Libya-4. For the shortwave infrared (SWIR) bands, the desert has less variability. The brief VIIRS record and target variability inhibits high confidence in identifying any trends that are less than +/- 0.6%/yr for most VIS bands, and +/- 2.5%/yr for SWIR bands. None of the observed invariant target reflective solar band trends exceeded these trend thresholds. Initial assessment results show that the VIIRS data have been consistently calibrated and that the VIIRS instrument stability is similar to or better than the MODIS instrument. C1 [Bhatt, Rajendra; Scarino, Benjamin R.; Haney, Conor O.; Gopalan, Arun] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Doelling, David R.] NASA, Langley Res Ctr, Hampton, VA 23666 USA. [Wu, Aisheng] Sigma Space Corp, Lanham, MD 20706 USA. [Xiong, Xiaoxiong (Jack)] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bhatt, R (reprint author), Sci Syst & Applicat Inc, 1 Enterprise Pkwy, Hampton, VA 23666 USA. EM rajendra.bhatt@nasa.gov; david.r.doelling@nasa.gov; Aisheng.Wu@sigmaspace.com; Xiaoxiong.Xiong.1@gsfc.nasa.gov; benjamin.r.scarino@nasa.gov; conor.o.haney@nasa.gov; arun.gopalan-1@nasa.gov RI Richards, Amber/K-8203-2015 FU National Aeronautics and Space Administration Earth Science Enterprise Office through the CERES Program; National Aeronautics and Space Administration Earth Science Enterprise Office through CLARREO Program; National Aeronautics and Space Administration Earth Science Enterprise Office through Satellite Calibration Interconsistency Program; National Atmospheric and Oceanic Administration Climate Data Records Program [MOA IA1-1016] FX This work was supported by the National Aeronautics and Space Administration Earth Science Enterprise Office through the CERES, CLARREO and the Satellite Calibration Interconsistency Programs and by the National Atmospheric and Oceanic Administration Climate Data Records Program through Grant MOA IA1-1016. NR 32 TC 21 Z9 21 U1 0 U2 5 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD APR PY 2014 VL 6 IS 4 BP 2809 EP 2826 DI 10.3390/rs6042809 PG 18 WC Remote Sensing SC Remote Sensing GA AI3FT UT WOS:000336746900011 ER PT J AU Anyamba, A Small, JL Tucker, CJ Pak, EW AF Anyamba, Assaf Small, Jennifer L. Tucker, Compton J. Pak, Edwin W. TI Thirty-two Years of Sahelian Zone Growing Season Non-Stationary NDVI3g Patterns and Trends SO REMOTE SENSING LA English DT Article DE Sahel; NDVI; rainfall; climate record; growing season; standardized anomalies; extremes; trend patterns ID DIFFERENCE VEGETATION INDEX; AFRICAN SAHEL; SPECTRAL REFLECTANCE; SAHARA DESERT; SOIL-EROSION; WEST-AFRICA; NOAA-AVHRR; EL-NINO; RAINFALL; CLIMATE AB We update the Global Inventory Modeling and Mapping Studies (GIMMS) analysis of Sahelian vegetation dynamics and trends using the normalized difference vegetation index (NDVI; version 3g) 1981 to 2012 data set. We compare the annual NDIV3g and July to October growing season averages with the three rainfall data sets: the Africa Rainfall Climatology from 1983 to 2012, the Variability Analyses of Surface Climate Observations Version-1.1 from 1951 to 2000, and the Nicholson ground-station precipitation rainfall data from 1981 to 1994. We use the Nicholson ground-station annual precipitation data to determine the reliability of the two continental precipitation data sets for specific locations and specific times, extrapolate these confirmed relationships over the Sahelian Zone from 1983 to 2012 with the Africa Rainfall Climatology, and then place these zonal findings within the 1951 to 2000 record of the Variability Analyses of Surface Climate Observations Version-1.1 precipitation data set. We confirm the extreme nature of the 1984-1985 Sahelian drought, a signature event that marked the minima during the 1980s desiccation period followed within ten years by near-maxima rainfall event in 1994 and positive departures is NDVI, marking beginning of predominantly wetter conditions that have persisted to 2012. We also show the NDVI3g data capture effective rainfall, the rainfall that is utilized by plants to grow, as compared to rainfall that evaporates or is runoff. Using our effective rainfall concept, we estimate average effective rainfall for the entire Sahelian Zone for the 1984 extreme drought was 223 mm/yr as compared to 406 mm/yr in during the 1994 wet period. We conclude that NDVI3g data can used as a proxy for analyzing and interpreting decadal-scale land surface variability and trends over semi arid-lands. C1 [Anyamba, Assaf; Small, Jennifer L.; Tucker, Compton J.; Pak, Edwin W.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, GIMMS Grp, Greenbelt, MD 20771 USA. RP Anyamba, A (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, GIMMS Grp, Code 618-0, Greenbelt, MD 20771 USA. EM assaf.anyamba@nasa.gov; Jennifer.l.small@nasa.gov; Compton.j.tucker@nasa.gov; edwin.w.pak@nasa.gov FU USDA Foreign Agricultural Service Global Agricultural Monitoring project FX This work was made possible by funding from USDA Foreign Agricultural Service Global Agricultural Monitoring project through its support of our operational GIMMS NOAA AVHRR NDVI production that is critical input into the NDVI3g long term series data set. We want to extend thanks to three anonymous reviewers whose comments and critical reviews served to improve this manuscript. NR 64 TC 18 Z9 21 U1 1 U2 28 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD APR PY 2014 VL 6 IS 4 BP 3101 EP 3122 DI 10.3390/rs6043101 PG 22 WC Remote Sensing SC Remote Sensing GA AI3FT UT WOS:000336746900025 ER PT J AU Groce, A Havelund, K Holzmann, G Joshi, R Xu, RG AF Groce, Alex Havelund, Klaus Holzmann, Gerard Joshi, Rajeev Xu, Ru-Gang TI Establishing flight software reliability: testing, model checking, constraint-solving, monitoring and learning SO ANNALS OF MATHEMATICS AND ARTIFICIAL INTELLIGENCE LA English DT Article DE File systems; Testing; Model checking; Verification; Flight software; Formal proof ID RULE SYSTEMS; FORMAL VERIFICATION; SYMBOLIC EXECUTION; TEST-GENERATION; COMPILER; PROGRAMS; SOLVER; EAGLE; TOOL AB In this paper we discuss the application of a range of techniques to the verification of mission-critical flight software at NASA's Jet Propulsion Laboratory. For this type of application we want to achieve a higher level of confidence than can be achieved through standard software testing. Unfortunately, given the current state of the art, especially when efforts are constrained by the tight deadlines and resource limitations of a flight project, it is not feasible to produce a rigorous formal proof of correctness of even a well-specified stand-alone module such as a file system (much less more tightly coupled or difficult-to-specify modules). This means that we must look for a practical alternative in the area between traditional testing and proof, as we attempt to optimize rigor and coverage. The approaches we describe here are based on testing, model checking, constraint-solving, monitoring, and finite-state machine learning, in addition to static code analysis. The results we have obtained in the domain of file systems are encouraging, and suggest that for more complex properties of programs with complex data structures, it is possibly more beneficial to use constraint solvers to guide and analyze execution (i.e., as in testing, even if performed by a model checking tool) than to translate the program and property into a set of constraints, as in abstraction-based and bounded model checkers. Our experience with non-file-system flight software modules shows that methods even further removed from traditional static formal methods can be assisted by formal approaches, yet readily adopted by test engineers and software developers, even as the key problem shifts from test generation and selection to test evaluation. C1 [Groce, Alex] Oregon State Univ, Sch Elect Engn & Comp Sci, Corvallis, OR 97331 USA. [Havelund, Klaus; Holzmann, Gerard; Joshi, Rajeev] CALTECH, Jet Prop Lab, Lab Reliable Software, Pasadena, CA 91109 USA. [Xu, Ru-Gang] Univ Calif Los Angeles, Dept Comp Sci, Los Angeles, CA 90095 USA. RP Groce, A (reprint author), Oregon State Univ, Sch Elect Engn & Comp Sci, Corvallis, OR 97331 USA. EM agroce@gmail.com FU National Aeronautics and Space Administration; NASA ESAS 6G FX The research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Funding was also provided by NASA ESAS 6G. (C) 2008. All Rights Reserved NR 102 TC 3 Z9 3 U1 2 U2 13 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1012-2443 EI 1573-7470 J9 ANN MATH ARTIF INTEL JI Ann. Math. Artif. Intell. PD APR PY 2014 VL 70 IS 4 SI SI BP 315 EP 349 DI 10.1007/s10472-014-9408-8 PG 35 WC Computer Science, Artificial Intelligence; Mathematics, Applied SC Computer Science; Mathematics GA AH8DZ UT WOS:000336365800002 ER PT J AU Stecker, FW AF Stecker, Floyd W. TI Limiting superluminal electron and neutrino velocities using the 2010 Crab Nebula flare and the IceCube PeV neutrino events SO ASTROPARTICLE PHYSICS LA English DT Article DE Lorentz invariance; Neutrino; Electron ID HIGH-ENERGY NEUTRINOS; SN1987A; TESTS; BURST AB The observation of two PeV-scale neutrino events reported by Ice Cube allows one to place constraints on Lorentz invariance violation (LIV) in the neutrino sector. After first arguing that at least one of the PeV IceCube events was of extragalactic origin, I derive an upper limit for the difference between putative superluminal neutrino and electron velocities of <=similar to 5.6 x 10(-19) in units where c = 1, confirming that the observed PeV neutrinos could have reached Earth from extragalactic sources. I further derive a new constraint on the superluminal electron velocity, obtained from the observation of synchrotron radiation from the Crab Nebula flare of September, 2010. The inference that the >1 GeV gamma-rays from synchrotron emission in the flare were produced by electrons of energy up to similar to 5.1 PeV indicates the non-occurrence of vacuum Cerenkov radiation by these electrons. This implies a new, strong constraint on superluminal electron velocities delta(e) <=similar to 5 x 10(-21). It immediately follows that one then obtains an upper limit on the superluminal neutrino velocity alone of delta(v) <= similar to 5.6 x 10(-19), many orders of magnitude better than the time-of-flight constraint from the SN1987A neutrino burst. However, if the electrons are sublurninal the constraint on |delta(e)| <=similar to 8 x 10(-17), obtained from the Crab Nebula gamma-ray spectrum, places a weaker constraint on superluminal neutrino velocity of delta(v) <=similar to 8 x 10(-17). Published by Elsevier B.V. C1 NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Stecker, FW (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. EM floyd.w.stecker@nasa.gov NR 41 TC 10 Z9 10 U1 0 U2 0 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 APR PY 2014 VL 56 BP 16 EP 18 DI 10.1016/j.astropartphys.2014.02.007 PG 3 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AH7UO UT WOS:000336341000003 ER PT J AU Palucis, MC Dietrich, WE Hayes, AG Williams, RME Gupta, S Mangold, N Newsom, H Hardgrove, C Calef, F Sumner, DY AF Palucis, Marisa C. Dietrich, William E. Hayes, Alexander G. Williams, Rebecca M. E. Gupta, Sanjeev Mangold, Nicholas Newsom, Horton Hardgrove, Craig Calef, Fred, III Sumner, Dawn Y. TI The origin and evolution of the Peace Vallis fan system that drains to the Curiosity landing area, Gale Crater, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Peace Vallis Fan; MSL; Gale Crater; Mars ID LARGE ALLUVIAL FANS; SEDIMENTARY-ROCKS; CLIMATE; CONSTRAINTS; ANTARCTICA; DEPOSITS; RIVERS; MOUND; WATER AB The landing site for the Curiosity rover is located at the distal end of the Peace Vallis fan in Gale Crater. Peace Vallis fan covers 80km(2) and is fed by a 730km(2) catchment, which drains an upland plains area through a 15km wide gap in the crater rim. Valley incision into accumulated debris delivered sediment through a relatively low density valley network to a main stem channel to the fan. An estimated total fan volume of 0.9km(3) matches the calculated volume of removal due to valley incision (0.8km(3)) and indicates a mean thickness of 9m. The fan profile is weakly concave up with a mean slope of 1.5% for the lower portion. Numerous inverted channels outcrop on the western surface of the fan, but on the eastern portion such channels are rare suggesting a change in process from distributary channel domination on the west to sheet flow on the eastern portion of the fan. Runoff (discharge/watershed area) to produce the fan is estimated to be more than 600m, perhaps as much as 6000m, indicating a hydrologic cycle that likely lasted at least thousands of years. Atmospheric precipitation (possibly snow) not seepage produced the runoff. Based on topographic data, Peace Vallis fan likely onlapped Bradbury Rise and spilled into a topographic low to the east of the rise. This argues that the light-toned fractured terrain within this topographic low corresponds to the distal deposits of Peace Vallis fan, and in such a setting, lacustrine deposits are expected. C1 [Palucis, Marisa C.; Dietrich, William E.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Hayes, Alexander G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Williams, Rebecca M. E.] Planetary Sci Inst, Tucson, AZ USA. [Gupta, Sanjeev] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London, England. [Mangold, Nicholas] Univ Nantes, Lab Planetol & Geodynam Nantes, CNRS UMR 6112, Nantes, France. [Newsom, Horton] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Hardgrove, Craig] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Calef, Fred, III] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA. [Sumner, Dawn Y.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. RP Palucis, MC (reprint author), Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. EM mpalucis@berkeley.edu RI Hayes, Alexander/P-2024-2014 OI Hayes, Alexander/0000-0001-6397-2630 FU NASA under the Mars Program Office FX This research was conducted for the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA under the Mars Program Office. We would like to thank Alan Howard, the entire MSL team, but especially John Grotzinger, Bernard Hallet, Ron Sletten, and Mike Malin for insightful discussions along the way. We greatly appreciate the comments and suggestions provided by our reviewers, especially those from Bob Craddock. We also thank the teams responsible for the orbital data, namely, the HiRISE, CTX, and HRSC teams. We give special thanks to Malin Space Science Systems, the USGS at Flagstaff, and Scott Mansfield, Jonathan Joseph, and Thomas Gautier from Cornell for image and data processing. NR 58 TC 28 Z9 28 U1 3 U2 27 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 APR PY 2014 VL 119 IS 4 BP 705 EP 728 DI 10.1002/2013JE004583 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AH6BF UT WOS:000336215000001 ER PT J AU Hamilton, VE Vasavada, AR Sebastian, E Juarez, MD Ramos, M Armiens, C Arvidson, RE Carrasco, I Christensen, PR De Pablo, MA Goetz, W Gomez-Elvira, J Lemmon, MT Madsen, MB Martin-Torres, FJ Martinez-Frias, J Molina, A Palucis, MC Rafkin, SCR Richardson, MI Yingst, RA Zorzano, MP AF Hamilton, Victoria E. Vasavada, Ashwin R. Sebastian, Eduardo Juarez, Manuel de la Torre Ramos, Miguel Armiens, Carlos Arvidson, Raymond E. Carrasco, Isaias Christensen, Philip R. De Pablo, Miguel A. Goetz, Walter Gomez-Elvira, Javier Lemmon, Mark T. Madsen, Morten B. Javier Martin-Torres, F. Martinez-Frias, Jesus Molina, Antonio Palucis, Marisa C. Rafkin, Scot C. R. Richardson, Mark I. Yingst, R. Aileen Zorzano, Maria-Paz TI Observations and preliminary science results from the first 100 sols of MSL Rover Environmental Monitoring Station ground temperature sensor measurements at Gale Crater SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; ground temperature; thermal inertia; thermophysics ID THERMAL EMISSION SPECTROMETER; CANDIDATE LANDING SITES; IMAGING-SYSTEM THEMIS; SURFACE-PROPERTIES; OPTICAL DEPTH; MARS; INERTIA; WATER; MISSION; ICE AB We describe preliminary results from the first 100 sols of ground temperature measurements along the Mars Science Laboratory's traverse from Bradbury Landing to Rocknest in Gale. The ground temperature data show long-term increases in mean temperature that are consistent with seasonal evolution. Deviations from expected temperature trends within the diurnal cycle are observed and may be attributed to rover and environmental effects. Fits to measured diurnal temperature amplitudes using a thermal model suggest that the observed surfaces have thermal inertias in the range of 265-375J m(-2) K-1 s(-1/2), which are within the range of values determined from orbital measurements and are consistent with the inertias predicted from the observed particle sizes on the uppermost surface near the rover. Ground temperatures at Gale Crater appear to warm earlier and cool later than predicted by the model, suggesting that there are multiple unaccounted for physical conditions or processes in our models. Where the Mars Science Laboratory (MSL) descent engines removed a mobile layer of dust and fine sediments from over rockier material, the diurnal temperature profile is closer to that expected for a homogeneous surface, suggesting that the mobile materials on the uppermost surface may be partially responsible for the mismatch between observed temperatures and those predicted for materials having a single thermal inertia. Models of local stratigraphy also implicate thermophysical heterogeneity at the uppermost surface as a potential contributor to the observed diurnal temperature cycle. Key Points Diurnal ground temperatures vary with location Diurnal temperature curves are not well matched by a homogeneous thermal model GTS data are consistent with a varied stratigraphy and thermophysical properties C1 [Hamilton, Victoria E.; Rafkin, Scot C. R.] Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Vasavada, Ashwin R.; Juarez, Manuel de la Torre] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Sebastian, Eduardo; Armiens, Carlos; Carrasco, Isaias; Gomez-Elvira, Javier; Javier Martin-Torres, F.; Martinez-Frias, Jesus; Molina, Antonio; Zorzano, Maria-Paz] Ctr Astrobiol CSIC INTA, Madrid, Spain. [Ramos, Miguel; Molina, Antonio] Univ Alcala De Henares, Dept Fis & Matemat, Alcala De Henares, Spain. [Arvidson, Raymond E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Christensen, Philip R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [De Pablo, Miguel A.] Univ Alcala De Henares, Dept Geol Geog & Medio Ambiente, Alcala De Henares, Spain. [Goetz, Walter] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Lemmon, Mark T.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA. [Madsen, Morten B.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Javier Martin-Torres, F.] Inst Andaluz Ciencias Tierra CSIC UGR, Granada, Spain. [Martinez-Frias, Jesus] Inst Geociencias CSIC UCM, Madrid, Spain. [Palucis, Marisa C.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Richardson, Mark I.] Ashima Res, Pasadena, CA USA. [Yingst, R. Aileen] Planetary Sci Inst, Tucson, AZ USA. RP Hamilton, VE (reprint author), Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA. EM hamilton@boulder.swri.edu RI de Pablo, Miguel Angel/J-6442-2014; Gomez-Elvira, Javier/K-5829-2014; Ramos, Miguel/K-2230-2014; Lemmon, Mark/E-9983-2010; Zorzano, Maria-Paz/C-5784-2015; Martin-Torres, Francisco Javier/G-6329-2015; Zorzano, Maria-Paz/F-2184-2015 OI Molina, Antonio/0000-0002-5038-2022; de Pablo, Miguel Angel/0000-0002-4496-2741; Gomez-Elvira, Javier/0000-0002-9068-9846; Ramos, Miguel/0000-0003-3648-6818; Lemmon, Mark/0000-0002-4504-5136; Zorzano, Maria-Paz/0000-0002-4492-9650; Martin-Torres, Francisco Javier/0000-0001-6479-2236; Zorzano, Maria-Paz/0000-0002-4492-9650 FU Mars Science Laboratory; Mars Odyssey Participating Scientist Programs; Economy and Competitivity Ministry [AYA2011-25720, AYA2012-38707]; Mars Science Laboratory project; Deutsche Forschungsgemeinschaft (DFG) [GO 2288/1-1]; Danish Council for Independent Research/Natural Sciences (FNU) [0602-02713B] FX V.E.H. is supported by the Mars Science Laboratory and 2001 Mars Odyssey Participating Scientist Programs. E. S., C. A., M. R., I. C., J.G.-E., M. A. D. P., J.M.-T., and M.-P.Z. are supported by the Economy and Competitivity Ministry (projects AYA2011-25720 and AYA2012-38707). A. V., M. T. L., and M.T.J. are supported by the Mars Science Laboratory project. W. G. acknowledges partial funding by the Deutsche Forschungsgemeinschaft (DFG grant GO 2288/1-1). M. B. M. is supported by the Danish Council for Independent Research/Natural Sciences (FNU grant 0602-02713B). We greatly appreciate all of the scientists and engineers who spent many years working to make the MSL mission such a success. We also thank the MSL Science Team for their support of the REMS investigation, and we deeply appreciate the REMS PULs and PDLs (who do the daily hard work of planning and validating REMS data, usually in the middle of the Spanish night). We are grateful to Tim Parker and Fred Calef at JPL for rapid updates to and information about the rover localization data. Others who have contributed their time and/or advice include Elena McCartney (MSSS), Larry Edwards (NASA Ames), the MSLICE team at JPL, Josh Bandfield (SSI), Hugh Kieffer (Celestial Reasonings), Than Putzig (SwRI), Bob Haberle (NASA Ames), F. Scott Anderson (SwRI), Chris Edwards (Caltech), Mike Smith (GSFC), Mike Wolff (SSI), Jonathan Hill (ASU), Kelly Bender (ASU), Dale Noss (ASU), and Kimm Murray (ASU). Last, but definitely not the least, we thank Josh Bandfield and an anonymous reviewer for thorough, constructive critiques that helped improve the manuscript. NR 81 TC 17 Z9 17 U1 0 U2 15 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 APR PY 2014 VL 119 IS 4 BP 745 EP 770 DI 10.1002/2013JE004520 PG 26 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AH6BF UT WOS:000336215000003 ER PT J AU Stephan, K Jaumann, R De Sanctis, MC Tosi, F Ammannito, E Krohn, K Zambon, F Marchi, S Ruesch, O Matz, KD Preusker, F Roatsch, T Raymond, CA Russell, CT AF Stephan, K. Jaumann, R. De Sanctis, M. C. Tosi, F. Ammannito, E. Krohn, K. Zambon, F. Marchi, S. Ruesch, O. Matz, K. -D. Preusker, F. Roatsch, T. Raymond, C. A. Russell, C. T. TI Small fresh impact craters on asteroid 4 Vesta: A compositional and geological fingerprint SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Vesta; asteroid; surface; composition ID DIFFUSE-REFLECTANCE SPECTRA; DAWN MISSION; HED METEORITES; DARK MATERIAL; SOLAR-SYSTEM; PARENT BODY; SURFACE; DIOGENITES; MINERALS; HETEROGENEITY AB Small morphologically fresh impact craters (<10km in diameter) on Vesta's surface with a photometrically distinct ejecta blanket are expected to represent fresh surface material and thus provide the opportunity to study the composition of the unweathered surface. Dawn-Framing Camera and Visual and Infrared Spectrometer (VIR) data reveal impact craters with bright, dark, and mixed, i.e., partly bright and dark, ejecta existing on Vesta's surface, which not only differ in the visible albedo from their surroundings but also in their composition. Differences in the composition are related to the visible albedo and/or the geographic location of the impact craters. Bright ejecta, only seen in the southern Vestan hemisphere, are dominated by howardite/eucrite-like material as expected for Vesta's upper crust. Dark ejecta associated with dark impact craters are dominated by a strongly absorbing, spectrally neutral compound, supporting an origin from carbon-rich impactors. Few impact craters of intermediate albedo in Vesta's southern hemisphere contain material resembling diogenites, which are expected to exist in the deeper parts of Vesta's interior. The geological settings suggest that the diogenite-like material represents a part of a layer of diogenitic material surrounding the Rheasilvia basin or local concentrations of diogenitic material as part of the ejecta excavated during the latter stage of the Rheasilvia impact event. The spectral differences between eucrite- and diogenite-dominated materials also could be verified due to spin-forbidden absorptions in the visible spectral range, which are known from laboratory spectra of pyroxenes, but, which have been identified in the VIR spectra of Vesta for the first time. Key Points Fresh impact craters reflect Vesta's unweathered surface composition Vesta's surface varies significantly on a local scale Distribution of materials is related to the formation of Rheasilvia basin C1 [Stephan, K.; Jaumann, R.; Krohn, K.; Matz, K. -D.; Preusker, F.; Roatsch, T.] DLR, Inst Planetary Res, Berlin, Germany. [Jaumann, R.] Free Univ Berlin, Inst Geosci, Berlin, Germany. [De Sanctis, M. C.; Tosi, F.; Ammannito, E.; Zambon, F.] INAF IAPS, Ist Astrofis & Planetol Spaziali, Rome, Italy. [Marchi, S.] NASA, Lunar Sci Inst, Boulder, CO USA. [Ruesch, O.] Univ Munster, Inst Planetol, D-48149 Munster, Germany. [Raymond, C. A.] CALTECH, JPL, Pasadena, CA 91125 USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys, Los Angeles, CA USA. RP Stephan, K (reprint author), DLR, Inst Planetary Res, Berlin, Germany. EM Katrin.Stephan@dlr.de OI De Sanctis, Maria Cristina/0000-0002-3463-4437; Tosi, Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592 FU ASI-INAF [I/004/12/0] FX We thank the Dawn engineering and science team for the development, cruise, orbital insertion, and operations of the Dawn spacecraft at Vesta. This work was performed at the DLR Institute of Planetary Research with support from the VIR visible and infrared mapping spectrometer team at the INAF Institute for Space Astrophysics and Planetology (IAPS) in Rome, Italy, JPL in Pasadena, and UCLA in Los Angeles. The VIR team is founded by ASI-INAF grant I/004/12/0. NR 92 TC 10 Z9 10 U1 0 U2 3 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 APR PY 2014 VL 119 IS 4 BP 771 EP 797 DI 10.1002/2013JE004388 PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AH6BF UT WOS:000336215000004 ER PT J AU Hwang, KJ Goldstein, ML Vinas, AF Schriver, D Ashour-Abdalla, M AF Hwang, K. -J. Goldstein, M. L. Vinas, A. F. Schriver, D. Ashour-Abdalla, M. TI Wave-particle interactions during a dipolarization front event SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Dipolarization front; wave particle interaction; Electron beams; Whistler waves; plasma heating ID AURORAL ELECTRON-BEAM; MAGNETIC RECONNECTION; ACCELERATION; CLUSTER; PLASMA; MAGNETOSPHERE; PROPAGATION; EVOLUTION; NOISE; SHEET AB We present Cluster observations of wave-particle interactions during an earthward propagating dipolarization front (DF) and associated fast plasma bulk flows detected at the central current sheet in Earth's magnetotail. During this period, flux tubes behind the DF frequently contain more energetic or hotter ions than did the preexisting flux tubes ahead of the DF. On the other hand, electrons within the DF flux tubes heat less, or are even colder, than were the preexisting populations and are often accompanied by superposed isolated beams. At the same time, electrostatic emissions are strongly enhanced over a wide range of frequencies (up to several times the electron cyclotron frequency) behind the DFs. This low-frequency electrostatic wave power is well correlated with ion energization. From linear theory, we find two wave modes: a high-frequency beam mode and a low-frequency whistler mode that are associated with the electron beam component. We attribute the generation of whistlers to electron beams that persist for a while before undergoing rapid thermalization. The existence of isolated beam components behind DFs detected during the 4 s Cluster spin period indicates that DFs either provide a continuous source of electron beams or facilitate a physical process that maintains the beams against rapid thermalization. Our analysis suggests that the earthward motion of the DF flux tube, via Fermi acceleration as the magnetic field lines behind the DF shorten, can lead to the persistent electron beams that generate whistler mode waves, which in turn can heat ions. This scenario, by which free energy in electron beams generates waves that then heat ions, accounts for the Cluster observations of different energization behaviors between electrons and ions behind DFs. C1 [Hwang, K. -J.; Goldstein, M. L.; Vinas, A. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hwang, K. -J.] Univ Maryland Baltimore Cty, Goddard Planetary & Heliophys Inst, Baltimore, MD 21228 USA. [Schriver, D.; Ashour-Abdalla, M.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. RP Hwang, KJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Kyoung-Joo.Hwang@nasa.gov FU NASA's Magnetospheric Multiscale Mission Interdisciplinary Science (MMS/IDS) grant; Cluster mission; NASA MMS/IDS grant [NNX08A048G]; NASA [NNX12AD13G] FX K.J.H., M. L. G., and A. V. were supported, in part, by NASA's Magnetospheric Multiscale Mission Interdisciplinary Science (MMS/IDS) grant to the Goddard Space Flight Center and by the Cluster mission. Maha Ashour-Abdalla and David Schriver were supported by NASA MMS/IDS grant NNX08A048G and NASA grant NNX12AD13G. NR 48 TC 10 Z9 10 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD APR PY 2014 VL 119 IS 4 BP 2484 EP 2493 DI 10.1002/2013JA019259 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6CP UT WOS:000336218600010 ER PT J AU Omidi, N Sibeck, D Gutynska, O Trattner, KJ AF Omidi, N. Sibeck, D. Gutynska, O. Trattner, K. J. TI Magnetosheath filamentary structures formed by ion acceleration at the quasi-parallel bow shock SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE magnetosheath; ion acceleration; density structures; temperature structures; Temperature Structures ID HOT FLOW ANOMALIES; CYCLOTRON ANISOTROPY INSTABILITIES; MAGNETIC-FIELD VARIATIONS; GLOBAL HYBRID SIMULATION; UPSTREAM SOLAR-WIND; LOW-FREQUENCY WAVES; EARTHS MAGNETOSHEATH; ULF WAVES; DENSITY-FLUCTUATIONS; DIAMAGNETIC CAVITIES AB Results from 2.5-D electromagnetic hybrid simulations show the formation of field-aligned, filamentary plasma structures in the magnetosheath. They begin at the quasi-parallel bow shock and extend far into the magnetosheath. These structures exhibit anticorrelated, spatial oscillations in plasma density and ion temperature. Closer to the bow shock, magnetic field variations associated with density and temperature oscillations may also be present. Magnetosheath filamentary structures (MFS) form primarily in the quasi-parallel sheath; however, they may extend to the quasi-perpendicular magnetosheath. They occur over a wide range of solar wind Alfvenic Mach numbers and interplanetary magnetic field directions. At lower Mach numbers with lower levels of magnetosheath turbulence, MFS remain highly coherent over large distances. At higher Mach numbers, magnetosheath turbulence decreases the level of coherence. Magnetosheath filamentary structures result from localized ion acceleration at the quasi-parallel bow shock and the injection of energetic ions into the magnetosheath. The localized nature of ion acceleration is tied to the generation of fast magnetosonic waves at and upstream of the quasi-parallel shock. The increased pressure in flux tubes containing the shock accelerated ions results in the depletion of the thermal plasma in these flux tubes and the enhancement of density in flux tubes void of energetic ions. This results in the observed anticorrelation between ion temperature and plasma density. C1 [Omidi, N.] Solana Sci Inc, Solana Beach, CA 92075 USA. [Sibeck, D.; Gutynska, O.] NASA GSFC, Greenbelt, MD USA. [Trattner, K. J.] Univ Colorado, LASP, Boulder, CO 80309 USA. RP Omidi, N (reprint author), Solana Sci Inc, Solana Beach, CA 92075 USA. EM omidi@solanasci.com FU NSF [AGS-1007449, AGS-1103227, 1102572] FX Work for this project was supported by NSF grants AGS-1007449, AGS-1103227, and 1102572. NR 76 TC 7 Z9 7 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD APR PY 2014 VL 119 IS 4 BP 2593 EP 2604 DI 10.1002/2013JA019587 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6CP UT WOS:000336218600017 ER PT J AU Hajra, R Echer, E Tsurutani, BT Gonzalez, WD AF Hajra, Rajkumar Echer, Ezequiel Tsurutani, Bruce T. Gonzalez, Walter D. TI Solar wind-magnetosphere energy coupling efficiency and partitioning: HILDCAAs and preceding CIR storms during solar cycle 23 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Solar wind-magnetosphere energy coupling efficiency; Magnetospheric energy partitioning; HILDCAAs; CIR storms; Joule heating; Ring current injection ID COROTATING INTERACTION REGIONS; INTERPLANETARY MAGNETIC-FIELD; MAGNETOPAUSE BOUNDARY-LAYER; GEOMAGNETIC-ACTIVITY; CORONAL HOLES; ALFVEN WAVES; DIFFUSION-PROCESSES; EPSILON-PARAMETER; EVENTS; AE AB A quantitative study on the energetics of the solar wind-magnetosphere-ionosphere system during High-Intensity, Long-Duration, Continuous AE Activity (HILDCAA) events for solar cycle 23 (from 1995 through 2008) is presented. For all HILDCAAs, the average energy transferred to the magnetospheric/ionospheric system was similar to 6.3x1016 J, and the ram kinetic energy of the incident solar wind was similar to 7.1x1018 J. For individual HILDCAA events the coupling efficiency, defined as the ratio of the solar wind energy input to the solar wind kinetic energy, varied between 0.3% and 2.8%, with an average value of similar to 0.9%. The solar wind coupling efficiency for corotating interaction region (CIR)-driven storms prior to the HILDCAA events was found to vary from similar to 1% to 5%, with an average value of similar to 2%. Both of these values are lower than the> 5% coupling efficiency noted for interplanetary coronal mass ejection (and sheath)-driven magnetic storms. During HILDCAAs, similar to 67% of the solar wind energy input went into Joule heating, similar to 22% into auroral precipitation, and similar to 11% into the ring current energy. The CIR-storm Joule heating (similar to 49%) was noticeably less than that during HILDCAAs, while the ring current energies were comparable for the two. Joule dissipation was higher for HILDCAAs that followed CIR-storms (88%) than for isolated HILDCAAs (similar to 60%). Possible physical interpretations for the statistical results obtained in this paper are discussed. C1 [Hajra, Rajkumar; Echer, Ezequiel; Gonzalez, Walter D.] Inst Nacl Pesquisas Espaciais, Sao Paulo, Brazil. [Tsurutani, Bruce T.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Hajra, R (reprint author), Inst Nacl Pesquisas Espaciais, Sao Paulo, Brazil. EM rajkumarhajra@yahoo.co.in RI Hajra, Rajkumar/C-1246-2011; OI Hajra, Rajkumar/0000-0003-1583-182X; Hajra, Rajkumar/0000-0003-0447-1531 FU Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP); Brazilian CNPq agency [301233/2011-0]; NASA FX The work of RH is financially supported by Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) through post-doctoral research fellowship at INPE. One of the authors (EE) would like to thank to the Brazilian CNPq (301233/2011-0) agency for financial support. Portions of this research were performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. NR 91 TC 10 Z9 10 U1 1 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD APR PY 2014 VL 119 IS 4 BP 2675 EP 2690 DI 10.1002/2013JA019646 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6CP UT WOS:000336218600023 ER PT J AU Valek, PW Goldstein, J McComas, DJ Fok, MC Mitchell, DG AF Valek, P. W. Goldstein, J. McComas, D. J. Fok, M-C. Mitchell, D. G. TI Large magnetic storms as viewed by TWINS: A study of the differences in the medium energy ENA composition SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE magnetic storms; ENA; oxygen; TWINS; medium energy; composition ID RING CURRENT; INNER MAGNETOSPHERE; GEOMAGNETIC STORM; HYDROGEN; TIME; SPECTRA; IMAGES; IONS; CIR; O+ AB During large geomagnetic storms (Dst-100 nT), oxygen can become a significant component of the energetic particles of the inner magnetosphere. Until recently, there were no available global observations of the medium energy (<50keV) oxygen populations. Using observations from the Two Wide-angle Imaging Neutral-atom Spectrometers (TWINS) Energetic Neutral Atom (ENA) imagers we present a study of nine large storms of solar cycle 24 as a function of storm phase. For these storms we observe that the H and O ENA fluxes and their temperatures increase in tandem during the storm's initial phase. However, there is no increase in the O+/H+ ratio in the inner magnetosphere until the storm main phase. Also seen during the main phase is an energy dispersion with higher-energy (32keV) H ENAs seen before the arrival of O ENAs of the same energy. The O ENAs take longer to return to prestorm levels during the recovery phases. This longer recovery time is likely because of the large difference between the storm time and prestorm O populations compared to H (i.e., there is always some prestorm H in the inner magnetosphere, but effectively no O prestorm). These results imply that medium-energy O ENAs evolve over long time scales (hours to days) as opposed to the shorter substorm time scales of the higher-energy (>52keV) O ENAs. C1 [Valek, P. W.; Goldstein, J.; McComas, D. J.] SwRI, San Antonio, TX 78238 USA. [Valek, P. W.; Goldstein, J.; McComas, D. J.] UTSA, Dept Phys, San Antonio, TX USA. [Fok, M-C.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Mitchell, D. G.] JHU, Appl Phys Lab, Laurel, MD USA. RP Valek, PW (reprint author), SwRI, San Antonio, TX 78238 USA. EM PValek@swri.edu OI Valek, Philip/0000-0002-2318-8750 FU NASA TWINS mission in NASA's explorer program FX This work was funded as part of the NASA TWINS mission in NASA's explorer program. Real-time Dst and SYM-H data were kindly provided by the World Data Center for Geomagnetism, Kyoto University, Japan. Solar wind data are from the ACE spacecraft and shifted in time by OMNI. NR 41 TC 4 Z9 4 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD APR PY 2014 VL 119 IS 4 BP 2819 EP 2835 DI 10.1002/2014JA019782 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6CP UT WOS:000336218600030 ER PT J AU Korth, H Anderson, BJ Gershman, DJ Raines, JM Slavin, JA Zurbuchen, TH Solomon, SC McNutt, RL AF Korth, Haje Anderson, Brian J. Gershman, Daniel J. Raines, Jim M. Slavin, James A. Zurbuchen, Thomas H. Solomon, Sean C. McNutt, Ralph L., Jr. TI Plasma distribution in Mercury's magnetosphere derived from MESSENGER Magnetometer and Fast Imaging Plasma Spectrometer observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Mercury; MESSENGER; magnetosphere; plasma pressure; plasma distribution; plasma entry ID KELVIN-HELMHOLTZ INSTABILITY; SOLAR-WIND; MAGNETOTAIL BOUNDARY; GEOTAIL OBSERVATIONS; ION COMPOSITION; MAGNETIC-FIELD; MAGNETOPAUSE; SHEET; MAGNETOSHEATH; INSTRUMENT AB We assess the statistical spatial distribution of plasma in Mercury's magnetosphere from observations of magnetic pressure deficits and plasma characteristics by the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft. The statistical distributions of proton flux and pressure were derived from 10months of Fast Imaging Plasma Spectrometer (FIPS) observations obtained during the orbital phase of the MESSENGER mission. The Magnetometer-derived pressure distributions compare favorably with those deduced from the FIPS observations at locations where depressions in the magnetic field associated with the presence of enhanced plasma pressures are discernible in the Magnetometer data. The magnitudes of the magnetic pressure deficit and the plasma pressure agree on average, although the two measures of plasma pressure may deviate for individual events by as much as a factor of similar to 3. The FIPS distributions provide better statistics in regions where the plasma is more tenuous and reveal an enhanced plasma population near the magnetopause flanks resulting from direct entry of magnetosheath plasma into the low-latitude boundary layer of the magnetosphere. The plasma observations also exhibit a pronounced north-south asymmetry on the nightside, with markedly lower fluxes at low altitudes in the northern hemisphere than at higher altitudes in the south on the same field line. This asymmetry is consistent with particle loss to the southern hemisphere surface during bounce motion in Mercury's offset dipole magnetic field. C1 [Korth, Haje; Anderson, Brian J.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Gershman, Daniel J.; Raines, Jim M.; Slavin, James A.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Gershman, Daniel J.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. RP Korth, H (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. EM haje.korth@jhuapl.edu RI Slavin, James/H-3170-2012; McNutt, Ralph/E-8006-2010 OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166 FU NASA [NAS5-97271, NASW-00002] FX 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. NR 57 TC 12 Z9 12 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD APR PY 2014 VL 119 IS 4 BP 2917 EP 2932 DI 10.1002/2013JA019567 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6CP UT WOS:000336218600035 ER PT J AU Dong, JR Ek, M Hall, D Peters-Lidard, C Cosgrove, B Miller, J Riggs, G Xia, YL AF Dong, Jiarui Ek, Mike Hall, Dorothy Peters-Lidard, Christa Cosgrove, Brian Miller, Jeff Riggs, George Xia, Youlong TI Using Air Temperature to Quantitatively Predict the MODIS Fractional Snow Cover Retrieval Errors over the Continental United States SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Drought; Snowpack; Snow cover; Surface temperature; Seasonal variability ID DATA ASSIMILATION SYSTEM; WATER EQUIVALENT; ACCURACY ASSESSMENT; MAPPING ACCURACY; VALIDATION; PRODUCTS; AREA; SNOTEL; DEPTH; NLDAS AB Understanding and quantifying satellite-based, remotely sensed snow cover uncertainty are critical for its successful utilization. The Moderate Resolution Imaging Spectroradiometer (MODIS) snow cover errors have been previously recognized to be associated with factors such as cloud contamination, snowpack grain sizes, vegetation cover, and topography; however, the quantitative relationship between the retrieval errors and these factors remains elusive. Joint analysis of the MODIS fractional snow cover (FSC) from Collection 6 (C6) and in situ air temperature and snow water equivalent measurements provides a unique look at the error structure of the MODIS C6 FSC products. Analysis of the MODIS FSC dataset over the period from 2000 to 2005 was undertaken over the continental United States (CONUS) with an extensive observational network. When compared to MODIS Collection 5 (C5) snow cover area, the MODIS C6 FSC product demonstrates a substantial improvement in detecting the presence of snow cover in Nevada [30% increase in probability of detection (POD)], especially in the early and late snow seasons; some improvement over California (10% POD increase); and a relatively small improvement over Colorado (2% POD increase). However, significant spatial and temporal variations in accuracy still exist, and a proxy is required to adequately predict the expected errors in MODIS C6 FSC retrievals. A relationship is demonstrated between the MODIS FSC retrieval errors and temperature over the CONUS domain, captured by a cumulative double exponential distribution function. This relationship is shown to hold for both in situ and modeled daily mean air temperature. Both of them are useful indices in filtering out the misclassification of MODIS snow cover pixels and in quantifying the errors in the MODIS C6 product for various hydrological applications. C1 [Dong, Jiarui; Ek, Mike; Xia, Youlong] NOAA, NCEP, EMC, College Pk, MD 20740 USA. [Dong, Jiarui; Xia, Youlong] IM Syst Grp, Rockville, MD USA. [Hall, Dorothy; Miller, Jeff; Riggs, George] NASA, Cryospher Sci Lab, GSFC, Greenbelt, MD USA. [Peters-Lidard, Christa] NASA, Hydrol Sci Lab, GSFC, Greenbelt, MD USA. [Cosgrove, Brian] NOAA, NWS, OHD, Silver Spring, MD USA. [Miller, Jeff] Wyle Inc, Houston, TX USA. [Riggs, George] SSAI Inc, Lanham, MD USA. RP Dong, JR (reprint author), NOAA, NCEP, EMC, 5830 Univ Res Ct, College Pk, MD 20740 USA. EM jiarui.dong@noaa.gov RI Peters-Lidard, Christa/E-1429-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876 FU NOAA Climate Program Office (CPO) Modeling, Analysis, Predictions, and Projections (MAPP) program FX We thank Kingtse Mo from NOAA/NCEP/CPC for her contributions. This work was directly funded by the NOAA Climate Program Office (CPO) Modeling, Analysis, Predictions, and Projections (MAPP) program. The NASA EOS Project supported the participation of D. Hall, J. Miller, and G. Riggs. NR 55 TC 2 Z9 2 U1 0 U2 7 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD APR PY 2014 VL 15 IS 2 BP 551 EP 562 DI 10.1175/JHM-D-13-060.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AE7LN UT WOS:000334179500002 ER PT J AU Tokay, A Roche, RJ Bashor, PG AF Tokay, Ali Roche, Rigoberto J. Bashor, Paul G. TI An Experimental Study of Spatial Variability of Rainfall SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Hydrometeorology; In situ atmospheric observations ID SMALL-SCALE RAINFALL; VALIDATION; RADAR; PRODUCTS; TMPA; QPE AB Spatial variability of rainfall was studied through a gauge network on the Delmarva Peninsula. The gauge network consists of 11 dual- or triple-tipping-bucket sites ranging from 1- to 150-km separation distances. The time of the tip (0.254 mm) was recorded to a datalogger, and a continuous dataset was available from all sites for over 5 yr (May 2005-July 2010). A three-parameter exponential function was fitted to the paired correlations and the resultant correlation distance was 8-13 km during summer and 51-85 km during winter. The correlation distances showed pronounced year-to-year variability as being 8-43 km and 13-67 km during spring and autumn, respectively. The airmass convection was the main weather system during summer while nor'easters played an important role during winter. The 30-min integration and two-tip rain/no-rain threshold was selected for the base of this study. The correlation distance increased with longer integration periods and was 17 and 32 km for 30 min and 1 h, respectively. C1 [Tokay, Ali] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Greenbelt, MD USA. [Tokay, Ali] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Roche, Rigoberto J.] Florida Int Univ, Miami, FL 33199 USA. [Bashor, Paul G.] Comp Sci Corp, Wallops Isl, VA USA. [Bashor, Paul G.] NASA, Wallops Flight Facil, Wallops Isl, VA USA. RP Tokay, A (reprint author), NASA, Goddard Space Flight Ctr, Code 612-0, Greenbelt, MD 20771 USA. EM ali.tokay-1@nasa.gov FU NASA's Global Precipitation Measurement Mission; NASA Goddard Space Flight Center; Precipitation Measurement Mission (PMM) [NNX07AF45G, NNX10AJ12G] FX The second author was a summer intern under NASA's Water Escapes program; Fernando Miralles of Florida International University is the principal investigator. Acknowledgements extend to Robert Meneghini of the NASA Goddard Space Flight Center and S. Joseph Munchak of the University of Maryland for their valuable comments. Special thanks to Joseph Turk, Editor of the Journal of Hydrometeorology, for his guidance throughout the review process. We are also thankful for the constructive comments from the anonymous reviewers. This study was funded under NASA's Global Precipitation Measurement Mission under Arthur Hou, project scientist, NASA Goddard Space Flight Center, and the Precipitation Measurement Mission (PMM) NNX07AF45G and NNX10AJ12G under Ramesh Kakar, program scientist, NASA Headquarters. Acknowledgments extend to Mathew Schwaller, GPM ground validation manager, NASA Goddard Space Flight Center, for his continuous support. NR 17 TC 8 Z9 8 U1 1 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD APR PY 2014 VL 15 IS 2 BP 801 EP 812 DI 10.1175/JHM-D-13-031.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AE7LN UT WOS:000334179500017 ER PT J AU Panerai, F Martin, A Mansour, NN Sepka, SA Lachaud, J AF Panerai, Francesco Martin, Alexandre Mansour, Nagi N. Sepka, Steven A. Lachaud, Jean TI Flow-Tube Oxidation Experiments on the Carbon Preform of a Phenolic-Impregnated Carbon Ablator SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER LA English DT Article ID THERMAL RESPONSE; HIGH-TEMPERATURE; PYROLYSIS-GAS; GRAPHITE; PROGRAM; IMAGE AB Oxidation experiments on the carbon preform of a phenolic-impregnated carbon ablator were performed in a flow-tube reactor facility, at temperatures between 700 and 1300K, under dry air gas at pressures between 1.6x103 and 6.0x104Pa. Mass loss, volumetric recession and density changes were measured at different test conditions. An analysis of the diffusion/reaction competition within the porous material, based on the Thiele number, allows identification of low temperature and low-pressure conditions to be dominated by in-depth volume oxidation. Experiments above 1000K were found at transition conditions, where diffusion and reaction occur at similar scales. The microscopic oxidation behavior of the fibers was characterized by scanning electron microscopy and energy dispersive x-ray analysis. The material was found to oxidize at specific sites, forming a pitting pattern distributed over the surface of the fibers. Calcium- and oxygen-rich residues from the oxidation reactions were observed at several locations. C1 [Panerai, Francesco; Martin, Alexandre] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA. [Panerai, Francesco; Martin, Alexandre] Univ Kentucky, Ctr Computat Sci, Lexington, KY 40506 USA. [Mansour, Nagi N.] NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA. [Sepka, Steven A.] ERC Inc, Moffett Field, CA 94035 USA. [Lachaud, Jean] Univ Calif Santa Cruz, Moffett Field, CA 94035 USA. RP Panerai, F (reprint author), Univ Kentucky, Dept Mech Engn, 261 Ralph G Anderson Building, Lexington, KY 40506 USA. RI Martin, Alexandre/L-9520-2014; OI Martin, Alexandre/0000-0003-2216-2468; Lachaud, Jean/0000-0001-7397-1025 FU NASA [NNX10CC53P, NNX10AV39A]; Hypersonic Entry, Descent, and Landing (EDL) Program FX Financial support to the first author of this work was provided by the NASA Small Business Innovation Research Phase-2 Award NNX10CC53P and the NASA Kentucky Experimental Program to Stimulate Competitive Research Award NNX10AV39A. Support by the Hypersonic Entry, Descent, and Landing (EDL) Program for the effort is gratefully acknowledged. We thank the unwavering encouragements by M. J. Wright from the NASA Ames Research Center and A. M. Calomino from the NASA Langley Research Center. We are also thankful to J. Chavez Garcia, J. W. Ridge, and M. Gusman from ERC, Inc. for support on scanning electron microscopy, assistance at the flow-tube laboratory, and for the training on samples' encapsulation, respectively. The comments of F. S. Milos and Y. K. Chen from the NASA Ames Research Center are greatly appreciated. NR 38 TC 6 Z9 6 U1 0 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0887-8722 EI 1533-6808 J9 J THERMOPHYS HEAT TR JI J. Thermophys. Heat Transf. PD APR PY 2014 VL 28 IS 2 BP 181 EP 190 DI 10.2514/1.T4265 PG 10 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA AH6GX UT WOS:000336229800002 ER PT J AU Lachaud, J Mansour, NN AF Lachaud, Jean Mansour, Nagi N. TI Porous-Material Analysis Toolbox Based on OpenFOAM and Applications SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER LA English DT Article ID PHENOLIC RESIN; CARBON/PHENOLIC COMPOSITE; PYROLYSIS; ABLATION; HEAT AB The Porous-material Analysis Toolbox based on OpenFOAM is a fully portable OpenFOAM library. It is implemented to test innovative multiscale physics-based models for reacting porous materials that undergo recession. Current developments are focused on ablative materials. The ablative material response module implemented in the Porous-material Analysis Toolbox relies on an original high-fidelity ablation model. The governing equations are volume-averaged forms of the conservation equations for gas mass, gas species, solid mass, gas momentum, and total energy. It may also simply be used as a state-of-the-art ablation model when the right model options are chosen. As applications, three physical analyses are presented: 1)volume-averaged study of the oxidation of a carbon-fiber preform under dry air, 2)three-dimensional analysis of the pyrolysis gas flow in a porous ablative material sample facing an arcjet, and 3)comparison of a state-of-the-art and a high-fidelity model for the thermal and chemical response of a carbon/phenolic ablative material. C1 [Lachaud, Jean] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Mansour, Nagi N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lachaud, J (reprint author), Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. EM jlachaud@ucsc.edu; nagi.n.mansour@nasa.gov OI Lachaud, Jean/0000-0001-7397-1025 FU NASA's Fundamental Aeronautic Program Hypersonics Nasa Research Announcement (NRA) [NNX12AG47A]; Space Technology Research Grants Program FX This research was originally funded by NASA's Fundamental Aeronautic Program Hypersonics Nasa Research Announcement (NRA) grant NNX12AG47A. It is currently supported by the Space Technology Research Grants Program. The authors would like to thank G. Blanquart (Caltech) for providing a preliminary reduced mechanism of his combustion database. NR 21 TC 6 Z9 6 U1 1 U2 5 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0887-8722 EI 1533-6808 J9 J THERMOPHYS HEAT TR JI J. Thermophys. Heat Transf. PD APR PY 2014 VL 28 IS 2 BP 191 EP 202 DI 10.2514/1.T4262 PG 12 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA AH6GX UT WOS:000336229800003 ER PT J AU Welsh, T Burek-Huntington, K Savage, K Rosenthal, B Dubey, JP AF Welsh, Trista Burek-Huntington, Kathy Savage, Kate Rosenthal, Benjamin Dubey, J. P. TI Sarcocystis canis Associated Hepatitis in a Steller Sea Lion (Eumetopias jubatus) from Alaska SO JOURNAL OF WILDLIFE DISEASES LA English DT Article ID TOXOPLASMA-GONDII; NEOSPORA-CANINUM; INFECTIONS; PARASITES; NEURONA AB Sarcocystis canis infection was associated with hepatitis in a Steller sea lion (Eumetopias jubatus). Intrahepatocellular protozoal schizonts were among areas of necrosis and inflammation. The parasite was genetically identical to S. canis and is the first report in a Steller sea lion, indicating another intermediate host species for S. canis. C1 [Welsh, Trista] Univ Georgia, Coll Vet Med, Athens, GA 30605 USA. [Burek-Huntington, Kathy] Alaska Vet Pathol Serv, Eagle River, AK 99577 USA. [Savage, Kate] Natl Marine Fisheries Serv, Protected Resources Div, Juneau, AK 99802 USA. [Rosenthal, Benjamin; Dubey, J. P.] ARS, USDA, Beltsville Agr Res Ctr, Anim Parasit Dis Lab,BARC East, Beltsville, MD 20705 USA. RP Welsh, T (reprint author), Flyinvet, 10174 Airpark Loop, Givens Hotsprings, ID 83641 USA. EM trista.welsh@gmail.com OI Rosenthal, Benjamin/0000-0002-0224-3773 NR 10 TC 0 Z9 0 U1 2 U2 12 PU WILDLIFE DISEASE ASSOC, INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 0090-3558 EI 1943-3700 J9 J WILDLIFE DIS JI J. Wildl. Dis. PD APR PY 2014 VL 50 IS 2 BP 405 EP 408 DI 10.7589/2013-03-079 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA AH6JT UT WOS:000336237900036 PM 24484486 ER PT J AU Carrier, MJ Ngodock, H Smith, S Jacobs, G Muscarella, P Ozgokmen, T Haus, B Lipphardt, B AF Carrier, Matthew J. Ngodock, Hans Smith, Scott Jacobs, Gregg Muscarella, Philip Ozgokmen, Tamay Haus, Brian Lipphardt, Bruce TI Impact of Assimilating Ocean Velocity Observations Inferred from Lagrangian Drifter Data Using the NCOM-4DVAR SO MONTHLY WEATHER REVIEW LA English DT Article DE Inverse methods; Variational analysis; Model initialization; Numerical analysis; modeling; Ocean models ID VARIATIONAL ASSIMILATION; MODELING SYSTEM; EQUATION; SURFACE; IMPLEMENTATION; CIRCULATION; FORMULATION AB Eulerian velocity fields are derived from 300 drifters released in the Gulf of Mexico by The Consortium for Advanced Research on Transport of Hydrocarbon in the Environment (CARTHE) during the summer 2012 Grand Lagrangian Deployment (GLAD) experiment. These data are directly assimilated into the Navy Coastal Ocean Model (NCOM) four-dimensional variational data assimilation (4DVAR) analysis system in a series of experiments to investigate their impact on the model circulation. The NCOM-4DVAR is a newly developed tool for data analysis, formulated for weak-constraint data assimilation based on the indirect representer method. The assimilation experiments take advantage of this velocity data along with other available data sources from in situ and satellite measurements of surface and subsurface temperature and salinity. Three different experiments are done: (i) A nonassimilative NCOM free run, (ii) an assimilative NCOM run that utilizes temperature and salinity observations, and (iii) an assimilative NCOM run that uses temperature and salinity observations as well as the GLAD velocity observations. The resulting analyses and subsequent forecasts are compared to assimilated and future GLAD velocity and temperature/salinity observations to determine the performance of each experiment and the impact of the GLAD data on the analysis and the forecast. It is shown that the NCOM-4DVAR is able to fit the observations not only in the analysis step, but also in the subsequent forecast. It is also found that the GLAD velocity data greatly improves the characterization of the circulation, with the forecast showing a better fit to future GLAD observations than those experiments without the velocity data included. C1 [Carrier, Matthew J.; Ngodock, Hans; Smith, Scott; Jacobs, Gregg] Naval Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. [Muscarella, Philip] Amer Soc Engn Educ, Washington, DC USA. [Ozgokmen, Tamay; Haus, Brian] Univ Miami, Miami, FL USA. [Lipphardt, Bruce] Univ Delaware, Newark, DE USA. RP Carrier, MJ (reprint author), Naval Res Lab, Stennis Space Ctr, Bldg 1009,Balch Blvd, Stennis Space Ctr, MS 39529 USA. EM matthew.carrier@nrlssc.navy.mil FU BP/The Gulf of Mexico Research Initiative (GoMRI) through the Consortium for Advanced Research on Transport of Hydrocarbon in the Environment (CARTHE); Office of Naval Research Program Element [0601153N] FX The authors would like to acknowledge Emanuel Coelho for his work in processing the GLAD drifter observations into Eulerian velocity measurements used in this assimilation study. The authors would like to thank the anonymous reviewers for their helpful comments during the revision process. The authors would also like to state that this research was made possible in part by a grant from BP/The Gulf of Mexico Research Initiative (GoMRI) through the Consortium for Advanced Research on Transport of Hydrocarbon in the Environment (CARTHE). This work was also sponsored by the Office of Naval Research Program Element 0601153N as part of the projects "A Multiscale Approach to Assessing Predictability of ASW Environment" and "The Rapid Transition Project (RTP) for 4Dvar NCOM in RELO and COAMPS5 with merged NCODA/NAVDAS-AR." NR 35 TC 10 Z9 10 U1 0 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 EI 1520-0493 J9 MON WEATHER REV JI Mon. Weather Rev. PD APR PY 2014 VL 142 IS 4 BP 1509 EP 1524 DI 10.1175/MWR-D-13-00236.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AD7IC UT WOS:000333436300008 ER PT J AU Noble, E Druyan, LM Fulakeza, M AF Noble, Erik Druyan, Leonard M. Fulakeza, Matthew TI The Sensitivity of WRF Daily Summertime Simulations over West Africa to Alternative Parameterizations. Part I: African Wave Circulation SO MONTHLY WEATHER REVIEW LA English DT Article DE Africa; Waves; atmospheric; Vorticity; Model evaluation; performance; Parameterization; Regional models ID EASTERLY WAVE; WEATHER RESEARCH; MODEL PERFORMANCE; FORECASTING-MODEL; DATA ASSIMILATION; REGIONAL MODEL; CLIMATE-CHANGE; CONVECTION; ATLANTIC; MONSOON AB The performance of the NCAR Weather Research and Forecasting Model (WRF) as a West African regional-atmospheric model is evaluated. The study tests the sensitivity of WRF-simulated vorticity maxima associated with African easterly waves to 64 combinations of alternative parameterizations in a series of simulations in September. In all, 104 simulations of 12-day duration during 11 consecutive years are examined. The 64 combinations combine WRF parameterizations of cumulus convection, radiation transfer, surface hydrology, and PBL physics. Simulated daily and mean circulation results are validated against NASA's Modern-Era Retrospective Analysis for Research and Applications (MERRA) and NCEP/Department of Energy Global Reanalysis 2. Precipitation is considered in a second part of this two-part paper. A wide range of 700-hPa vorticity validation scores demonstrates the influence of alternative parameterizations. The best WRF performers achieve correlations against reanalysis of 0.40-0.60 and realistic amplitudes of spatiotemporal variability for the 2006 focus year while a parallel-benchmark simulation by the NASA Regional Model-3 (RM3) achieves higher correlations, but less realistic spatiotemporal variability. The largest favorable impact on WRF-vorticity validation is achieved by selecting the Grell-Devenyi cumulus convection scheme, resulting in higher correlations against reanalysis than simulations using the Kain-Fritch convection. Other parameterizations have less-obvious impact, although WRF configurations incorporating one surface model and PBL scheme consistently performed poorly. A comparison of reanalysis circulation against two NASA radiosonde stations confirms that both reanalyses represent observations well enough to validate the WRF results. Validation statistics for optimized WRF configurations simulating the parallel period during 10 additional years are less favorable than for 2006. C1 [Noble, Erik] Univ Colorado, Environm Studies Program, Boulder, CO 80309 USA. [Noble, Erik] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Druyan, Leonard M.; Fulakeza, Matthew] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. RP Noble, E (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM erik.noble@nasa.gov FU NASA Cooperative Agreement [NNX11AR61G, NNX11AR63A]; National Science Foundation [AGS-1000874] FX The authors gratefully acknowledge the inspiration and encouragement for this project of the late Professor Thomas T. Warner. We also gratefully acknowledge many very constructive suggestions of two anonymous reviewers. EUN was supported by NASA Cooperative Agreement NNX11AR61G. LMD and MF were supported by National Science Foundation Grant AGS-1000874 and NASA Cooperative Agreement NNX11AR63A. MERRA data were obtained from NASA's GMAO website (http://gmao.gsfc.nasa.gov/merra), NAMMA radiosonde data were obtained from NASA's Global Hydrology Center website (http://airbornescience.nsstc.nasa.gov/namma), and NCEP Reanalysis-2 data were provided by the NOAA/ESRL/Physical Sciences Division, Boulder, Colorado, from their website (http://www.esrl.noaa.gov/psd). NR 58 TC 4 Z9 4 U1 0 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 EI 1520-0493 J9 MON WEATHER REV JI Mon. Weather Rev. PD APR PY 2014 VL 142 IS 4 BP 1588 EP 1608 DI 10.1175/MWR-D-13-00194.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AD7IC UT WOS:000333436300013 ER PT J AU Balakrishnan, K AF Balakrishnan, Kaushik TI Explosion-driven Rayleigh-Taylor instability in gas-particle mixtures SO PHYSICS OF FLUIDS LA English DT Article ID RICHTMYER-MESHKOV INSTABILITIES; BUOYANCY-DRAG MODEL; BLAST-WAVE; NUMERICAL-SIMULATION; HEAT-TRANSFER; SHOCK-TUBE; DISPERSION; BUBBLE; CLOUDS; SPHERE AB The structure and growth of an explosion-driven Rayleigh-Taylor instability in gas-particle mixtures is investigated using two-dimensional numerical simulations. Particle concentration and diameter are varied and the growth of the ensuing mixing layer and its dependence on these parameters is investigated. The hydrodynamic structures are subdued and lose their coherence with increase in solid particle concentrations. When the solid particle concentration is fixed but particle diameter varied, a non-monotic behavior is observed. It is found that an intermediate particle size results in the widest mixing zone and degree of mixing. This is due to the differences in the spatial accumulation of the particles as they disperse. Small particles accumulate in the bubbles and around the spikes of the Rayleigh-Taylor structures; intermediate-sized particles in the tips of the spikes and as roots into the driver fluid; large particles accumulate primarily in the spikes and as thin, elongated roots into the driver fluid. Such differences are attributed to the response time or Stokes number of the particles. Finally, future directions for extending the current research are summarized. (C) 2014 AIP Publishing LLC. C1 [Balakrishnan, Kaushik] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Res Div, Berkeley, CA 94720 USA. RP Balakrishnan, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM kaushikb258@gmail.com NR 33 TC 3 Z9 3 U1 2 U2 14 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-6631 EI 1089-7666 J9 PHYS FLUIDS JI Phys. Fluids PD APR PY 2014 VL 26 IS 4 AR 043303 DI 10.1063/1.4873175 PG 15 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA AH5FA UT WOS:000336152700026 ER PT J AU Vogt, SS Radovan, M Kibrick, R Butler, RP Alcott, B Allen, S Arriagada, P Bolte, M Burt, J Cabak, J Chloros, K Cowley, D Deich, W Dupraw, B Earthman, W Epps, H Faber, S Fischer, D Gates, E Hilyard, D Holden, B Johnston, K Keiser, S Kanto, D Katsuki, M Laiterman, L Lanclos, K Laughlin, G Lewis, J Lockwood, C Lynam, P Marcy, G McLean, M Miller, J Misch, T Peck, M Pfister, T Phillips, A Rivera, E Sandford, D Saylor, M Stover, R Thompson, M Walp, B Ward, J Wareham, J Wei, MZ Wright, C AF Vogt, Steven S. Radovan, Matthew Kibrick, Robert Butler, R. Paul Alcott, Barry Allen, Steve Arriagada, Pamela Bolte, Mike Burt, Jennifer Cabak, Jerry Chloros, Kostas Cowley, David Deich, William Dupraw, Brian Earthman, Wayne Epps, Harland Faber, Sandra Fischer, Debra Gates, Elinor Hilyard, David Holden, Brad Johnston, Ken Keiser, Sandy Kanto, Dick Katsuki, Myra Laiterman, Lee Lanclos, Kyle Laughlin, Greg Lewis, Jeff Lockwood, Chris Lynam, Paul Marcy, Geoffrey McLean, Maureen Miller, Joe Misch, Tony Peck, Michael Pfister, Terry Phillips, Andrew Rivera, Eugenio Sandford, Dale Saylor, Mike Stover, Richard Thompson, Matthew Walp, Bernie Ward, James Wareham, John Wei, Mingzhi Wright, Chris TI APF-The Lick Observatory Automated Planet Finder SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID ECHELLE-SPECTROMETER; SPECTROGRAPH; TELESCOPE; FITS; REPRESENTATIONS; SYSTEM; I. AB The Automated Planet Finder (APF) is a facility purpose-built for the discovery and characterization of extrasolar planets through high-cadence Doppler velocimetry of the reflex barycentric accelerations of their host stars. Located atop Mount Hamilton, the APF facility consists of a 2.4 m telescope and its Levy spectrometer, an optical echelle spectrometer optimized for precision Doppler velocimetry. APP features a fixed-forivat spectral range from 374-970 nm, and delivers a "throughput" (resolution x slit width product) of 114,000", with spectral resolutions up to 150,000. Overall system efficiency (fraction of photons incident on the primary mirror that are detected by the science CCD) on blaze at 560 nm in planet-hunting mode is 15%. First-light tests on the radial-velocity (RV) standard stars HD 185144 and HD 9407 demonstrate sub-meter-per-second precision (rms per observation) held over a 3 month period. This paper reviews the basic features of the telescope, dome, and spectrometer, and gives a brief summary of first-light performance. C1 [Vogt, Steven S.; Radovan, Matthew; Kibrick, Robert; Alcott, Barry; Allen, Steve; Bolte, Mike; Burt, Jennifer; Cabak, Jerry; Chloros, Kostas; Cowley, David; Deich, William; Dupraw, Brian; Earthman, Wayne; Epps, Harland; Faber, Sandra; Gates, Elinor; Hilyard, David; Holden, Brad; Kanto, Dick; Katsuki, Myra; Laiterman, Lee; Lanclos, Kyle; Laughlin, Greg; Lewis, Jeff; Lockwood, Chris; Lynam, Paul; McLean, Maureen; Miller, Joe; Misch, Tony; Peck, Michael; Pfister, Terry; Phillips, Andrew; Rivera, Eugenio; Sandford, Dale; Saylor, Mike; Stover, Richard; Thompson, Matthew; Ward, James; Wareham, John; Wei, Mingzhi; Wright, Chris] Univ Calif Santa Cruz, Univ Calif Observ, Santa Cruz, CA 95064 USA. [Butler, R. Paul; Arriagada, Pamela; Keiser, Sandy] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Fischer, Debra] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Johnston, Ken] US Naval Observ, Washington, DC 20392 USA. [Marcy, Geoffrey] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Walp, Bernie] NASA, Stratospher Observ Infrared Astron, Dryden Flight Res Ctr, Edwards AFB, CA 93523 USA. RP Vogt, SS (reprint author), Univ Calif Santa Cruz, Univ Calif Observ, Santa Cruz, CA 95064 USA. RI Butler, Robert/B-1125-2009 FU R-California; NASA [NAG5-13448]; NSF [AST-0307493] FX We are deeply indebted to Congressman Jerry Lewis (R-California, retired) for securing the Congressional earmark funding that formed the cornerstone of this project Thanks to Andrew Gray and Ian Ritchie of EOS, for their advice and assistance regarding APF telescope balance, encoder alignment, and various other telescope and dome operational procedures; to former EOST staff members Kevin Harris and Elwood Downey, for their suggestions regarding APF servo tuning, and to Andrew Lowman, for his advice regarding thermal compensation of M2 focus. We thank Vilma and Dave Anderson of Rayleigh Optical for the superb job they did on polishing and figuring the 2.4 m primary mirror. We are grateful to Gillian Knave and Craig Sonsetti of NIST for providing the critical high-resolution FT'S scans of the iodine cell. We would also like to acknowledge the excellent coating work done for us by Ric Shimshock and the folks at MLD Technologies LLC. We are especially grateful to Joe Wampler, Phil Crane, and Anne Kinney of NASA for their critical infusion of funds through NASA grant NAG5-13448 that funded the spectrometer and allowed us to super-size APF from a 1.8 m to a 2.4 m. We are grateful to Wayne Rosing of Las Cumbres Observatory for his donation of the 5-axis mill which was used to fabricate the determinate structure nodes. We especially would like to thank Ken and Gloria Levy for their generous contribution that helped fund completion of the spectrometer, Geoff Marcy and Susan Kegley for their personal contribution, and the Nick Konidaris family for their generous contribution. Finally, we are most grateful to the NSF for grant AST-0307493 that funded much of the observing software and commissioning activities. NR 28 TC 20 Z9 20 U1 0 U2 1 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 APR PY 2014 VL 126 IS 938 BP 359 EP 379 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH5TK UT WOS:000336193800005 ER PT J AU Howell, SB Sobeck, C Haas, M Still, M Barclay, T Mullally, F Troeltzsch, J Aigrain, S Bryson, ST Caldwell, D Chaplin, WJ Cochran, WD Huber, D Marcy, GW Miglio, A Najita, JR Smith, M Twicken, JD Fortney, JJ AF Howell, Steve B. Sobeck, Charlie Haas, Michael Still, Martin Barclay, Thomas Mullally, Fergal Troeltzsch, John Aigrain, Suzanne Bryson, Stephen T. Caldwell, Doug Chaplin, William J. Cochran, William D. Huber, Daniel Marcy, Geoffrey W. Miglio, Andrea Najita, Joan R. Smith, Marcie Twicken, J. D. Fortney, Jonathan J. TI The K2 Mission: Characterization and Early Results SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID RAPID OPTICAL VARIABILITY; ACTIVE GALACTIC NUCLEI; RED-GIANT STARS; MICROLENS PARALLAXES; STELLAR POPULATIONS; KEPLER OBSERVATIONS; PLANETARY SYSTEMS; LIGHT CURVES; SOLAR-TYPE; X-RAY AB The K2 mission will make use of the Kepler spacecraft and its assets to expand upon Kepler's groundbreaking discoveries in the fields of exoplanets and astrophysics through new and exciting observations. K2 will use an innovative way of operating the spacecraft to observe target fields along the ecliptic for the next 2-3 years. Early science commissioning observations have shown an estimated photometric precision near 400 ppm in a single 30 minute observation, and a 6-hr photometric precision of 80 ppm (both at V = 12). The K2 mission offers long-term, simultaneous optical observation of thousands of objects at a precision far better than is achievable from ground-based telescopes. Ecliptic fields will be observed for approximately 75 days enabling a unique exoplanet survey which fills the gaps in duration and sensitivity between the Kepler and TESS missions, and offers prelaunch exoplanet target identification for JWST transit spectroscopy. Astrophysics observations with K2 will include studies of young open clusters, bright stars, galaxies, supernovae, and asteroseismology. C1 [Howell, Steve B.; Sobeck, Charlie; Haas, Michael; Still, Martin; Barclay, Thomas; Mullally, Fergal; Bryson, Stephen T.; Caldwell, Doug; Huber, Daniel; Smith, Marcie; Twicken, J. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Still, Martin; Barclay, Thomas] Bay Area Environm Res Inst, West Sonoma, CA 95476 USA. [Mullally, Fergal; Caldwell, Doug; Huber, Daniel; Smith, Marcie; Twicken, J. D.] SETI Inst, Mountain View, CA 94043 USA. [Troeltzsch, John] Ball Aerosp & Technol Corp, Boulder, CO 80306 USA. [Aigrain, Suzanne] Univ Oxford, Dept Phys, Subdept Astrophys, Oxford OX1 3RH, England. [Chaplin, William J.; Miglio, Andrea] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Chaplin, William J.; Miglio, Andrea] Aarhus Univ, SAC, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Cochran, William D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Marcy, Geoffrey W.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Najita, Joan R.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Howell, SB (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RI Caldwell, Douglas/L-7911-2014 OI Caldwell, Douglas/0000-0003-1963-9616 NR 64 TC 272 Z9 272 U1 2 U2 10 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 APR PY 2014 VL 126 IS 938 BP 398 EP 408 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH5TK UT WOS:000336193800008 ER PT J AU Slaba, TC Blattnig, SR AF Slaba, Tony C. Blattnig, Steve R. TI GCR environmental models I: Sensitivity analysis for GCR environments SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE galactic cosmic rays; space radiation; uncertainty quantification ID ADVANCED COMPOSITION EXPLORER; COSMIC-RAY MODEL; RADIATION PROTECTION; SPACE RADIATION; EXPOSURE; HZETRN AB Accurate galactic cosmic ray (GCR) models are required to assess crew exposure during long-duration missions to the Moon or Mars. Many of these models have been developed and compared to available measurements, with uncertainty estimates usually stated to be less than 15%. However, when the models are evaluated over a common epoch and propagated through to effective dose, relative differences exceeding 50% are observed. This indicates that the metrics used to communicate GCR model uncertainty can be better tied to exposure quantities of interest for shielding applications. This is the first of three papers focused on addressing this need. In this work, the focus is on quantifying the extent to which each GCR ion and energy group, prior to entering any shielding material or body tissue, contributes to effective dose behind shielding. Results can be used to more accurately calibrate model-free parameters and provide a mechanism for refocusing validation efforts on measurements taken over important energy regions. Results can also be used as references to guide future nuclear cross-section measurements and radiobiology experiments. It is found that GCR with Z>2 and boundary energies below 500MeV/n induce less than 5% of the total effective dose behind shielding. This finding is important given that most of the GCR models are developed and validated against Advanced Composition Explorer/Cosmic Ray Isotope Spectrometer (ACE/CRIS) measurements taken below 500MeV/n. It is therefore possible for two models to very accurately reproduce the ACE/CRIS data while inducing very different effective dose values behind shielding. Key Points GCR model uncertainty may be higher than 15% GCR ions below 500 MeV/n contribute less than 5% to effective dose ACE/CRIS measurements induce less than 5% of effective dose C1 [Slaba, Tony C.; Blattnig, Steve R.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Slaba, TC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM tony.c.slaba@nasa.gov FU Human Research Program under the Human Exploration and Operations Mission Directorate of NASA FX This work was supported by the Human Research Program under the Human Exploration and Operations Mission Directorate of NASA. The authors would like to thank Pat O'Neill for providing the BON2011 source code. The data presented in this paper may be obtained by contacting the authors. NR 26 TC 7 Z9 7 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD APR PY 2014 VL 12 IS 4 BP 217 EP 224 DI 10.1002/2013SW001025 PG 8 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AG9IE UT WOS:000335731800004 ER PT J AU Slaba, TC Blattnig, SR AF Slaba, Tony C. Blattnig, Steve R. TI GCR environmental models II: Uncertainty propagation methods for GCR environments SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE space radiation; galactic cosmic rays; uncertainty quantification ID ADVANCED COMPOSITION EXPLORER; RADIATION; HZETRN AB In order to assess the astronaut exposure received within vehicles or habitats, accurate models of the ambient galactic cosmic ray (GCR) environment are required. Many models have been developed and compared to measurements, with uncertainty estimates often stated to be within 15%. However, intercode comparisons can lead to differences in effective dose exceeding 50%. This is the second of three papers focused on resolving this discrepancy. The first paper showed that GCR heavy ions with boundary energies below 500 MeV/n induce less than 5% of the total effective dose behind shielding. Yet, due to limitations on available data, model development and validation are heavily influenced by comparisons to measurements taken below 500 MeV/n. In the current work, the focus is on developing an efficient method for propagating uncertainties in the ambient GCR environment to effective dose values behind shielding. A simple approach utilizing sensitivity results from the first paper is described and shown to be equivalent to a computationally expensive Monte Carlo uncertainty propagation. The simple approach allows a full uncertainty propagation to be performed once GCR uncertainty distributions are established. This rapid analysis capability may be integrated into broader probabilistic radiation shielding analysis and also allows error bars (representing boundary condition uncertainty) to be placed around point estimates of effective dose. Key Points Sensitivity results can be used to propagate uncertainties Fast method developed for propagating boundary condition uncertainties GCR ions with E<500 MeV/n have small impact on effective dose C1 [Slaba, Tony C.; Blattnig, Steve R.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Slaba, TC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM tony.c.slaba@nasa.gov FU Human Research Program under the Human Exploration and Operations Mission Directorate of NASA FX This work was supported by the Human Research Program under the Human Exploration and Operations Mission Directorate of NASA. The data presented in this paper may be obtained by contacting the authors. NR 20 TC 4 Z9 4 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD APR PY 2014 VL 12 IS 4 BP 225 EP 232 DI 10.1002/2013SW001026 PG 8 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AG9IE UT WOS:000335731800005 ER PT J AU Slaba, TC Xu, XJ Blattnig, SR Norman, RB AF Slaba, Tony C. Xu, Xiaojing Blattnig, Steve R. Norman, Ryan B. TI GCR environmental models III: GCR model validation and propagated uncertainties in effective dose SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE Space Radiation; Galactic Cosmic Rays; Uncertainty Quantification ID COSMIC-RAY PROTON; ADVANCED COMPOSITION EXPLORER; ENERGY-SPECTRA; HELIUM SPECTRA; CHARGE COMPOSITION; NUCLEI; RADIATION; SPACE AB This is the last of three papers focused on quantifying the uncertainty associated with galactic cosmic rays (GCR) models used for space radiation shielding applications. In the first paper, it was found that GCR ions with Z>2 and boundary energy below 500MeV/nucleon induce less than 5% of the total effective dose behind shielding. This is an important finding since GCR model development and validation have been heavily biased toward Advanced Composition Explorer/Cosmic Ray Isotope Spectrometer measurements below 500MeV/nucleon. Weights were also developed that quantify the relative contribution of defined GCR energy and charge groups to effective dose behind shielding. In the second paper, it was shown that these weights could be used to efficiently propagate GCR model uncertainties into effective dose behind shielding. In this work, uncertainties are quantified for a few commonly used GCR models. A validation metric is developed that accounts for measurements uncertainty, and the metric is coupled to the fast uncertainty propagation method. For this work, the Badhwar-O'Neill (BON) 2010 and 2011 and the Matthia GCR models are compared to an extensive measurement database. It is shown that BON2011 systematically overestimates heavy ion fluxes in the range 0.5-4GeV/nucleon. The BON2010 and BON2011 also show moderate and large errors in reproducing past solar activity near the 2000 solar maximum and 2010 solar minimum. It is found that all three models induce relative errors in effective dose in the interval [-20%, 20%] at a 68% confidence level. The BON2010 and Matthia models are found to have similar overall uncertainty estimates and are preferred for space radiation shielding applications. Key Points BON2011 over estimates heavy ion flux at relevant energies BON2010 and Matthia models have similar overall uncertainty statements GCR model uncertainty may be reduced by calibrating to high energy data C1 [Slaba, Tony C.; Blattnig, Steve R.; Norman, Ryan B.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Xu, Xiaojing] Sci Syst & Applicat Inc, Hampton, VA USA. RP Slaba, TC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM tony.c.slaba@nasa.gov RI Norman, Ryan/D-5095-2017 OI Norman, Ryan/0000-0002-9103-7225 FU Human Research Program under the Human Exploration and Operations Mission Directorate of NASA; NASA [NNL11AA00B] FX This work was supported by the Human Research Program under the Human Exploration and Operations Mission Directorate of NASA and by NASA grant NNL11AA00B. The authors would like to thank Pat O'Neill for providing the BON2011 source code and Daniel Matthia for providing the Matthia source code. The data presented in this paper may be obtained by contacting the authors. NR 41 TC 4 Z9 4 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD APR PY 2014 VL 12 IS 4 BP 233 EP 245 DI 10.1002/2013SW001027 PG 13 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AG9IE UT WOS:000335731800006 ER PT J AU Kim, RS Moon, YJ Gopalswamy, N Park, YD Kim, YH AF Kim, R. -S. Moon, Y. -J. Gopalswamy, N. Park, Y. -D. Kim, Y. -H. TI Two-step forecast of geomagnetic storm using coronal mass ejection and solar wind condition SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE geomagnetic storm forecast; coronal mass ejection; solar wind ID CME EARTHWARD DIRECTION; INTERPLANETARY SHOCK; HALO CMES; MAGNETIC STORMS; RING CURRENT; ART.; GEOEFFECTIVENESS; PARAMETERS; MODEL; DST AB To forecast geomagnetic storms, we had examined initially observed parameters of coronal mass ejections (CMEs) and introduced an empirical storm forecast model in a previous study. Now we suggest a two-step forecast considering not only CME parameters observed in the solar vicinity but also solar wind conditions near Earth to improve the forecast capability. We consider the empirical solar wind criteria derived in this study (B-z-5 nT or E-y 3 mV/m for t 2 h for moderate storms with minimum Dst less than -50 nT) and a Dst model developed by Temerin and Li (2002, 2006) (TL model). Using 55 CME-Dst pairs during 1997 to 2003, our solar wind criteria produce slightly better forecasts for 31 storm events (90%) than the forecasts based on the TL model (87%). However, the latter produces better forecasts for 24 nonstorm events (88%), while the former correctly forecasts only 71% of them. We then performed the two-step forecast. The results are as follows: (i) for 15 events that are incorrectly forecasted using CME parameters, 12 cases (80%) can be properly predicted based on solar wind conditions; (ii) if we forecast a storm when both CME and solar wind conditions are satisfied (), the critical success index becomes higher than that from the forecast using CME parameters alone, however, only 25 storm events (81%) are correctly forecasted; and (iii) if we forecast a storm when either set of these conditions is satisfied (), all geomagnetic storms are correctly forecasted. Key Points This study is for the improvement of empirical geomagnetic storm forecast We use the initially observed CME parameters as the first-step of the forecast We also use the solar wind parameters for near-real forecast C1 [Kim, R. -S.; Park, Y. -D.; Kim, Y. -H.] Korea Astron & Space Sci Inst, Astron & Space Program Div, Taejon, South Korea. [Moon, Y. -J.] Kyung Hee Univ, Sch Space Res, Yongin, South Korea. [Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD 20771 USA. RP Kim, RS (reprint author), Korea Astron & Space Sci Inst, Astron & Space Program Div, Taejon, South Korea. EM rskim@kasi.re.kr RI Moon, Yong-Jae/E-1711-2013; OI Gopalswamy, Nat/0000-0001-5894-9954 FU Construction of Korean Space Weather Center as the project of KASI; KASI Basic Research Fund; Research Fellowship for Young Scientists of KRCF; WCU program [R31-10016]; Basic Research Promotion Fund through the National Research Foundation of Korea - Ministry of Education, Science, and Technology [20090071744, 20100014501] FX We thank the referees for careful reading of the manuscript and valuable suggestions and criticism that led to significant improvement of the paper. This work was supported by the Construction of Korean Space Weather Center as the project of KASI, the KASI Basic Research Fund, and Research Fellowship for Young Scientists of KRCF. Y.-J.M. has been supported by the WCU program (R31-10016) and Basic Research Promotion Fund (20090071744 and 20100014501) through the National Research Foundation of Korea funded by the Ministry of Education, Science, and Technology. NR 39 TC 2 Z9 2 U1 0 U2 5 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 APR PY 2014 VL 12 IS 4 BP 246 EP 256 DI 10.1002/2014SW001033 PG 11 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AG9IE UT WOS:000335731800007 ER PT J AU Posner, A Hesse, M St Cyr, OC AF Posner, A. Hesse, M. St Cyr, O. C. TI The main pillar: Assessment of space weather observational asset performance supporting nowcasting, forecasting, and research to operations SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE SWx Forecasting; Space Hardware; Assessment ID INTERPLANETARY MAGNETIC-FIELD; CORONAL MASS EJECTIONS; ADVANCED COMPOSITION EXPLORER; EARTH CONNECTION EVENTS; 29-31 OCTOBER 2003; SOLAR-WIND; GEOMAGNETIC STORMS; ENERGETIC PARTICLES; ARRIVAL TIMES; PROPAGATION AB Space weather forecasting critically depends upon availability of timely and reliable observational data. It is therefore particularly important to understand how existing and newly planned observational assets perform during periods of severe space weather. Extreme space weather creates challenging conditions under which instrumentation and spacecraft may be impeded or in which parameters reach values that are outside the nominal observational range. This paper analyzes existing and upcoming observational capabilities for forecasting, and discusses how the findings may impact space weather research and its transition to operations. A single limitation to the assessment is lack of information provided to us on radiation monitor performance, which caused us not to fully assess (i.e., not assess short term) radiation storm forecasting. The assessment finds that at least two widely spaced coronagraphs including L4 would provide reliability for Earth-bound CMEs. Furthermore, all magnetic field measurements assessed fully meet requirements. However, with current or even with near term new assets in place, in the worst-case scenario there could be a near-complete lack of key near-real-time solar wind plasma data of severe disturbances heading toward and impacting Earth's magnetosphere. Models that attempt to simulate the effects of these disturbances in near real time or with archival data require solar wind plasma observations as input. Moreover, the study finds that near-future observational assets will be less capable of advancing the understanding of extreme geomagnetic disturbances at Earth, which might make the resulting space weather models unsuitable for transition to operations. Key Points Manuscript assesses current and near-future space weather assets Current assets unreliable for forecasting of severe geomagnetic storms Near-future assets will not improve the situation C1 [Posner, A.; Hesse, M.; St Cyr, O. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Posner, A.] NASA Headquarters, Washington, DC USA. RP Posner, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM arik.posner@nasa.gov OI Posner, Arik/0000-0003-1572-8734 FU NASA FX The authors gratefully acknowledge the support provided by the NASA mission and instrument teams in 2011 and helpful suggestions provided by the reviewers of the manuscript in 2012 and 2013. We also acknowledge the anonymous NOAA review provided to us in early 2013. NR 92 TC 3 Z9 3 U1 0 U2 5 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 APR PY 2014 VL 12 IS 4 BP 257 EP 276 DI 10.1002/2013SW001007 PG 20 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AG9IE UT WOS:000335731800008 ER PT J AU Cotton, MM Bruhn, RL Sauber, J Burgess, E Forster, RR AF Cotton, Michelle M. Bruhn, Ronald L. Sauber, Jeanne Burgess, Evan Forster, Richard R. TI Ice surface morphology and flow on Malaspina Glacier, Alaska: Implications for regional tectonics in the Saint Elias orogen SO TECTONICS LA English DT Article DE tectonics; glaciers; remote sensing; Saint Elias; Alaska; Yakutat ID GROUND DEFORMATION MEASUREMENTS; 1979 ST-ELIAS; ELEVATION CHANGES; SOUTHERN ALASKA; CANADA; USA; TERRANE; THRUST; SYSTEM; IMAGES AB The Saint Elias Mountains in southern Alaska are located at a structural syntaxis where the coastal thrust and fold belt of the Fairweather plate boundary intersects thrust faults and folds generated by collision of the Yakutat Terrane. The axial trace of this syntaxis extends southeastward out of the Saint Elias Mountains and beneath Malaspina Glacier where it is hidden from view and cannot be mapped using conventional methods. Here we examine the surface morphology and flow patterns of Malaspina Glacier to infer characteristics of the bedrock topography and organization of the syntaxis. Faults and folds beneath the eastern part of the glacier trend northwest and reflect dextral transpression near the terminus of the Fairweather fault system. Those beneath the western part of the glacier trend northeast and accommodate folding and thrust faulting during collision and accretion of the Yakutat Terrane. Mapping the location and geometry of the structural syntaxis provides important constraints on spatial variations in seismicity, fault kinematics, and crustal shortening beneath Malaspina Glacier, as well as the position of the collisional deformation front within the Yakutat Terrane. We also speculate that the geometrical complexity of intersecting faults within the syntaxis formed a barrier to rupture propagation during two regional Mw 8.1 earthquakes in September 1899. Key Points Structural domains of Malaspina Glacier Glacial morphology and flow reflect basal topography and structural geology Feature tracking of ice velocities on Malaspina Glacier C1 [Cotton, Michelle M.; Bruhn, Ronald L.] Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA. [Sauber, Jeanne] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Burgess, Evan; Forster, Richard R.] Univ Utah, Dept Geog, Salt Lake City, UT USA. RP Cotton, MM (reprint author), Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA. EM michellemariecotton@gmail.com FU National Aeronautics and Space Administration (NASA) [NNX08AX88G]; NASA Science Innovation Fund at Goddard Space Flight Center; NASA Earth Science Space Fellowship; NASA [NNX08AP27G] FX National Aeronautics and Space Administration (NASA) grant entitled "Geodetic Imaging of Glacioseismotectonic Processes in Southern Alaska" (NNX08AX88G) awarded to J. Sauber, R. R. Forster, and R. L. Bruhn supported this research. J. Sauber was also supported by funding from the NASA 2012 Science Innovation Fund at Goddard Space Flight Center. E. Burgess was funded under the NASA Earth Science Space Fellowship. E. Burgess and R. R. Forster were also partially supported by NASA grant NNX08AP27G. We thank the editors at Tectonics and those who reviewed the manuscript, J. B. Chapman and L. Stearns, for their input and help. NR 45 TC 2 Z9 2 U1 3 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0278-7407 EI 1944-9194 J9 TECTONICS JI Tectonics PD APR PY 2014 VL 33 IS 4 BP 581 EP 595 DI 10.1002/2013TC003381 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AH6PT UT WOS:000336253800011 ER PT J AU Thurlow, ME Co, DT O'Brien, AS Hannun, RA Lapson, LB Hanisco, TF Anderson, JG AF Thurlow, M. E. Co, D. T. O'Brien, A. S. Hannun, R. A. Lapson, L. B. Hanisco, T. F. Anderson, J. G. TI The development and deployment of a ground-based, laser-induced fluorescence instrument for the in situ detection of iodine monoxide radicals SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID MARINE BOUNDARY-LAYER; LOWER STRATOSPHERE; POTENTIAL INFLUENCE; RATE COEFFICIENTS; MOLECULAR-IODINE; FREE TROPOSPHERE; REACTIVE IODINE; EASTERN PACIFIC; OZONE DEPLETION; GASEOUS IODINE AB High abundances of iodine monoxide (IO) are known to exist and to participate in local photochemistry of the marine boundary layer. Of particular interest are the roles IO plays in the formation of new particles in coastal marine environments and in depletion episodes of ozone and mercury in the Arctic polar spring. This paper describes a ground-based instrument that measures IO at mixing ratios less than one part in 10(12). The IO radical is measured by detecting laser-induced fluorescence at wavelengths longer that 500 nm. Tunable visible light is used to pump the A(2)Pi(3/2) (v' = 2) <- X-2 Pi(3/2) (v '' = 0) transition of IO near 445 nm. The laser light is produced by a solid-state, Nd: YAG-pumped Ti:Sapphire laser at 5 kHz repetition rate. The laser-induced fluorescence instrument performs reliably with very high signal-to-noise ratios (> 10) achieved in short integration times (< 1 min). The observations from a validation deployment to the Shoals Marine Lab on Appledore Island, ME are presented and are broadly consistent with in situ observations from European Coastal Sites. Mixing ratios ranged from the instrumental detection limit (< 1 pptv) to 10 pptv. These data represent the first in situ point measurements of IO in North America. (C) 2014 AIP Publishing LLC. C1 [Thurlow, M. E.; Co, D. T.; O'Brien, A. S.; Hannun, R. A.; Lapson, L. B.; Hanisco, T. F.; Anderson, J. G.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [Co, D. T.] Northwestern Univ, Argonne Northwestern Solar Energy Res Ctr, Evanston, IL 60208 USA. [Co, D. T.] Northwestern Univ, Dept Chem, Evanston, IL 60208 USA. [O'Brien, A. S.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. [Hanisco, T. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Thurlow, ME (reprint author), Harvard Univ, Dept Chem & Chem Biol, 12 Oxford St, Cambridge, MA 02138 USA. EM thurlow@huarp.harvard.edu FU National Science Foundation [0733875] FX The authors wish to thank Norton Allen, Joe Demusz, Mike Greenberg, Matt Knight, Terry Martin, Danny Spillane, Ed Thomspon, and Chris Tuozzolo for engineering support. M. T. wishes to thank the staff of the Shoals Marine Laboratory and Charles Praska for logistical assistance and Steven Wofsy and Roisin Commane for technical advice. This work was supported by the National Science Foundation (Award No.: 0733875). NR 83 TC 0 Z9 0 U1 1 U2 17 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 APR PY 2014 VL 85 IS 4 AR 044101 DI 10.1063/1.4869857 PG 14 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA AH1ZN UT WOS:000335920600043 PM 24784629 ER PT J AU Wollack, EJ Kinzer, RE Rinehart, SA AF Wollack, E. J. Kinzer, R. E., Jr. Rinehart, S. A. TI A cryogenic infrared calibration target SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID LIGHT TRAP; DESIGN; SUBMILLIMETER; REFLECTANCE; ABSORBER; REGION AB A compact cryogenic calibration target is presented that has a peak diffuse reflectance, R <= 0.003, from 800 to 4800 cm(-1) (12 - 2 mu m). Upon expanding the spectral range under consideration to 400-10 000 cm(-1) (25 - 1 mu m) the observed performance gracefully degrades to R <= 0.02 at the band edges. In the implementation described, a high-thermal-conductivity metallic substrate is textured with a pyramidal tiling and subsequently coated with a thin lossy dielectric coating that enables high absorption and thermal uniformity across the target. The resulting target assembly is lightweight, has a low-geometric profile, and has survived repeated thermal cycling from room temperature to similar to 4 K. Basic design considerations, governing equations, and test data for realizing the structure described are provided. The optical properties of selected absorptive materials-Acktar Fractal Black, Aeroglaze Z306, and Stycast 2850 FT epoxy loaded with stainless steel powder-are characterized and presented. C1 [Wollack, E. J.; Kinzer, R. E., Jr.; Rinehart, S. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wollack, EJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM edward.j.wollack@nasa.gov RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU NASA ROSES/APRA program FX The authors gratefully acknowledge financial support from the NASA ROSES/APRA program and thank E. Sharp and C. Wheeler for their contributions to preparation and fabrication of the structures presented here. R. Kinzer was supported by an appointment to the NASA Postdoctoral Program at GSFC, administered by the Oak Ridge Associated Universities. NR 33 TC 4 Z9 4 U1 1 U2 7 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 APR PY 2014 VL 85 IS 4 AR 044707 DI 10.1063/1.4871108 PG 5 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA AH1ZN UT WOS:000335920600052 PM 24784638 ER PT J AU Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Blandford, RD Borgland, AW Bregeon, J Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cavazzuti, E Cecchi, C Chaves, RCG Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J D'Ammando, F de Angelis, A Dermer, CD Digel, SW Silva, EDE Drell, PS Drlica-Wagner, A Favuzzi, C Focke, WB Franckowiak, A Fukazawa, Y Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Hadasch, D Hayashida, M Hays, E Hughes, RE Jackson, MS Jogler, T Knodlseder, J Kuss, M Lande, J Larsson, S Longo, F Loparco, F Lovellette, MN Lubrano, P Mazziotta, MN Mehault, J Michelson, PF Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nemmen, R Nuss, E Ohsugi, T Omodei, N Orienti, M Orlando, E Paneque, D Perkins, JS Piron, F Pivato, G Prokhorov, D Raino, S Razzano, M Razzaque, S Reimer, A Reimer, O Ritz, S Romoli, C Sanchez-Conde, M Sanchez, DA Sgro, C Siskind, EJ Spandre, G Spinelli, P Takahashi, H Tanaka, T Tibaldo, L Tinivella, M Tosti, G Troja, E Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Winer, BL Wood, KS Yang, Z AF Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Blandford, R. D. Borgland, A. W. Bregeon, J. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cavazzuti, E. Cecchi, C. Chaves, R. C. G. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. D'Ammando, F. de Angelis, A. Dermer, C. D. Digel, S. W. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Focke, W. B. Franckowiak, A. Fukazawa, Y. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Hadasch, D. Hayashida, M. Hays, E. Hughes, R. E. Jackson, M. S. Jogler, T. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Mazziotta, M. N. Mehault, J. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nemmen, R. Nuss, E. Ohsugi, T. Omodei, N. Orienti, M. Orlando, E. Paneque, D. Perkins, J. S. Piron, F. Pivato, G. Prokhorov, D. Raino, S. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Ritz, S. Romoli, C. Sanchez-Conde, M. Sanchez, D. A. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Takahashi, H. Tanaka, T. Tibaldo, L. Tinivella, M. Tosti, G. Troja, E. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Winer, B. L. Wood, K. S. Yang, Z. TI Fermi LARGE AREA TELESCOPE OBSERVATIONS OF BLAZAR 3C 279 OCCULTATIONS BY THE SUN SO ASTROPHYSICAL JOURNAL LA English DT Article DE astroparticle physics; gamma rays: general; occultations; quasars: individual (3C 279); Sun: X-rays, gamma rays ID ACTIVE GALACTIC NUCLEI; GAMMA-RAY EMISSION; MAGNETIC-FIELDS; PAIR HALOS; EGRET DATA; CONSEQUENCES; PHOTON; AXION AB Observations of occultations of bright. gamma-ray sources by the Sun may reveal predicted pair halos around blazars and/or new physics, such as, e.g., hypothetical light dark matter particles-axions. We use Fermi Gamma-Ray Space Telescope (Fermi) data to analyze four occultations of blazar 3C 279 by the Sun on October 8 each year from 2008 to 2011. A combined analysis of the observations of these occultations allows a point-like source at the position of 3C 279 to be detected with significance of approximate to 3 sigma, but does not reveal any significant excess over the flux expected from the quiescent Sun. The likelihood ratio test rules out complete transparency of the Sun to the blazar. gamma-ray emission at a 3s confidence level. C1 [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Pivato, G.; Romoli, C.; Tibaldo, L.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bechtol, K.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Prokhorov, D.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Tanaka, T.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Bechtol, K.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Prokhorov, D.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Tanaka, T.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Bellazzini, R.; Bregeon, J.; Kuss, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bruel, P.] Ecole Polytech, CNRS IN2P3, Lab Leprince Ringuet, Palaiseau, France. [Caliandro, G. A.; Hadasch, D.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cavazzuti, E.; Ciprini, S.; Gasparrini, D.; Giommi, P.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Cecchi, C.; D'Ammando, F.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA IRFU CNRS, F-91191 Gif Sur Yvette, France. [Cheung, C. C.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS IN2P3, Lab Univers & Particules Montpellier, Montpellier, France. [D'Ammando, F.; Mehault, J.] IASF Palermo, I-90146 Palermo, Italy. [Chekhtman, A.; D'Ammando, F.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Grp Coll Udine, Ist Nazl Fis Nucl, Sez Trieste, I-33100 Udine, Italy. [Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.; Hays, E.; Nemmen, R.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Jackson, M. S.] Royal Inst Technol KTH, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden. [Jackson, M. S.; Larsson, S.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Knoedlseder, J.; Yang, Z.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France. [Larsson, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Moiseev, A. A.; Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA. [Moiseev, A. A.; Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. RP Barbiellini, G (reprint author), Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. EM imos@stanford.edu; phdmitry@stanford.edu RI Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Orlando, E/R-5594-2016; OI Reimer, Olaf/0000-0001-6953-1385; Caraveo, Patrizia/0000-0003-2478-8018; Morselli, Aldo/0000-0002-7704-9553; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Giordano, Francesco/0000-0002-8651-2394; giommi, paolo/0000-0002-2265-5003; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Bastieri, Denis/0000-0002-6954-8862; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Gasparrini, Dario/0000-0002-5064-9495 NR 24 TC 4 Z9 4 U1 1 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 118 DI 10.1088/0004-637X/784/2/118 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400033 ER PT J AU Burlaga, LF Ness, NF AF Burlaga, L. F. Ness, N. F. TI VOYAGER 1 OBSERVATIONS OF THE INTERSTELLAR MAGNETIC FIELD AND THE TRANSITION FROM THE HELIOSHEATH SO ASTROPHYSICAL JOURNAL LA English DT Article DE Cosmic rays; ISM: magnetic fields; solar wind; Sun: heliosphere ID GALACTIC COSMIC-RAYS; OUTER HELIOSPHERE; TERMINATION SHOCK; STRENGTH FLUCTUATIONS; RADIO-EMISSION; SOLAR ROTATION; HELIOPAUSE; INTERPLANETARY; REGION; PLASMA AB Voyager 1 (V1) has been observing interstellar magnetic fields for more than one year beginning approximate to 2012/209, when V1 crossed a current sheet, a "CS0" having the structure of a tangential discontinuity. The inclination of this current sheet is consistent with an interstellar magnetic field B draped on a blunt heliopause. Two other current sheets (sector boundaries) were observed at approximate to 2012/167 and approximate to 2011/276 with high inclinations (99 degrees +/- 10 degrees. and 89 degrees +/- 10 degrees, respectively). From 2013.0 to approximate to 2013.6, the difference between the azimuthal angle lambda of B from the Parker spiral angle at the latitude 34 degrees.6 of V1 was lambda - lambda(P) = 22 degrees +/- 3 degrees and the corresponding difference of the elevation angle delta was delta - delta(P) = 23 degrees +/- 8 degrees. During 2012, the deviation from the Parker spiral angle was somewhat smaller. The interstellar magnetic field has a "west to east polarity," opposite to the direction of planetary motions. The magnitude of B varied smoothly in the range 0.38-0.59 nT with an average B = 0.486 +/- 0.045 after 2012/237.7. The transition from heliosheath to interstellar magnetic fields is related to a "two-step" increase in the cosmic ray intensity observed by V1 from approximate to 2012.30 to approximate to 2012.65. The first step increase began near the end of an unusual "away-polarity" sector, and it reached a plateau when V1 moved into a "toward-polarity" sector that ended at CS0. The second step increase began slowly after V1 crossed CS0, and it ended abruptly at 2012/237.728. C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA. EM lburlagahsp@verizon.net; nfnudel@yahoo.com NR 45 TC 38 Z9 39 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 146 DI 10.1088/0004-637X/784/2/146 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400061 ER PT J AU Cannon, BE Smith, CW Isenberg, PA Vasquez, BJ Murphy, N Nuno, RG AF Cannon, Bradford E. Smith, Charles W. Isenberg, Philip A. Vasquez, Bernard J. Murphy, Neil Nuno, Raquel G. TI ULYSSES OBSERVATIONS OF MAGNETIC WAVES DUE TO NEWBORN INTERSTELLAR PICKUP IONS. I. NEW OBSERVATIONS AND LINEAR ANALYSIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE instabilities; magnetic fields; solar wind; Sun: heliosphere; waves ID DISTANT SOLAR-WIND; OUTER HELIOSPHERE; TERMINATION SHOCK; PROTONS; TURBULENCE; HYDROGEN; EVOLUTION; ENERGY; SYSTEM; FIELD AB We have examined Ulysses magnetic field data using dynamic spectrogram techniques that compute wave amplitude, polarization, and direction of propagation over a broad range of frequencies and time. Events were identified that showed a strong polarization signature and an enhancement of power above the local proton gyrofrequency. We perform a statistical study of 502 wave events in an effort to determine when, where, and why they are observed. Most notably, we find that waves arising from newborn interstellar pickup ions are relatively rare and difficult to find. The quantities normally employed in theories of wave growth are neutral atom density and quantities related to their ionization and the subsequent dynamics such as wind speed, solar wind flux, and magnetic field orientation. We find the observations of waves to be largely uncorrelated to these quantities except for mean field direction where quasi-radial magnetic fields are favored and solar wind proton flux where wave observations appear to be favored by low flux conditions which runs contrary to theoretical expectations of wave generation. It would appear that an explanation based on source physics and instability growth rates alone is not adequate to account for the times when these waves are seen. C1 [Cannon, Bradford E.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Smith, Charles W.; Isenberg, Philip A.; Vasquez, Bernard J.] Univ New Hampshire, Inst Study Earth Oceans & Space, Dept Phys, Durham, NH 03824 USA. [Smith, Charles W.; Isenberg, Philip A.; Vasquez, Bernard J.] Univ New Hampshire, Inst Study Earth Oceans & Space, Ctr Space Sci, Durham, NH 03824 USA. [Murphy, Neil] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Nuno, Raquel G.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. RP Cannon, BE (reprint author), Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. EM bc13h@my.fsu.edu; Charles.Smith@unh.edu; Phil.Isenberg@unh.edu; Bernie.Vasquez@unh.edu; Neil.Murphy@jpl.nasa.gov; raquel.nuno@asu.edu FU NASA Guest Investigator [NNX07AH75G]; NSF [ATM0635863, AGS0962506]; Caltech [44A1085631]; NASA [NNX13AF97G, NNX11AJ37G]; NASA Space Grant program FX This work was supported in part by NASA Guest Investigator grant NNX07AH75G and NSF grant ATM0635863. C.W.S. is supported by Caltech subcontract 44A1085631 to the University of New Hampshire in support of the ACE/MAG instrument. Part of the ACE mandate is to better understand the role of pickup ions in the heliosphere. P.A.I. and B.J.V. are supported by NASA grants NNX13AF97G and NNX11AJ37G as well as NSF grant AGS0962506. B.E.C. was an undergraduate physics major working within the Space Science Center at the time this work was performed and worked as an undergraduate intern at JPL during the summer of 2012, supported by the NASA Space Grant program. Portions of this research were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 40 TC 9 Z9 9 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 150 DI 10.1088/0004-637X/784/2/150 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400065 ER PT J AU Duchene, G Arriaga, P Wyatt, M Kennedy, G Sibthorpe, B Lisse, C Holland, W Wisniewski, J Clampin, M Kalas, P Pinte, C Wilner, D Booth, M Horner, J Matthews, B Greaves, J AF Duchene, G. Arriaga, P. Wyatt, M. Kennedy, G. Sibthorpe, B. Lisse, C. Holland, W. Wisniewski, J. Clampin, M. Kalas, P. Pinte, C. Wilner, D. Booth, M. Horner, J. Matthews, B. Greaves, J. TI SPATIALLY RESOLVED IMAGING OF THE TWO-COMPONENT eta Crv DEBRIS DISK WITH HERSCHEL SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; stars: individual (eta Crv) ID SUN-LIKE STARS; TERRESTRIAL PLANET FORMATION; MAIN-SEQUENCE STARS; CIRCUMSTELLAR DISK; KUIPER-BELT; SPACE-TELESCOPE; HD 207129; HOT DUST; COLLISIONAL EVOLUTION; SOLAR NEIGHBORHOOD AB We present far-infrared and submillimeter images of the eta Crv debris disk system obtained with Herschel and SCUBA-2, as well as Hubble Space Telescope visible and near-infrared coronagraphic images. In the 70 mu m Herschel image, we clearly separate the thermal emission from the warm and cold belts in the system, find no evidence for a putative dust population located between them, and precisely determine the geometry of the outer belt. We also find marginal evidence for azimuthal asymmetries and a global offset of the outer debris ring relative to the central star. Finally, we place stringent upper limits on the scattered light surface brightness of the outer ring. Using radiative transfer modeling, we find that it is impossible to account for all observed properties of the system under the assumption that both rings contain dust populations with the same properties. While the outer belt is in reasonable agreement with the expectations of steady-state collisional cascade models, albeit with a minimum grain size that is four times larger than the blow-out size, the inner belt appears to contain copious amounts of small dust grains, possibly below the blow-out size. This suggests that the inner belt cannot result from a simple transport of grains from the outer belt and rather supports a more violent phenomenon as its origin. We also find that the emission from the inner belt has not declined over three decades, a much longer timescale than its dynamical timescale, which indicates that the belt is efficiently replenished. C1 [Duchene, G.; Arriaga, P.; Kalas, P.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Wyatt, M.; Kennedy, G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sibthorpe, B.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Lisse, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Holland, W.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Wisniewski, J.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Clampin, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pinte, C.] France UMI 3386, CNRS INSU, UMI FCA, Paris, France. [Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Booth, M.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile. [Horner, J.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Horner, J.] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. [Matthews, B.] Natl Res Council Canada Herzberg Astron & Astroph, Victoria, BC V9E 2E7, Canada. [Greaves, J.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. RP Duchene, G (reprint author), UJF Grenoble 1, CNRS, INSU, Inst Planetol & Astrophys IPAG,UMR 5274, F-38041 Grenoble, France. RI Lisse, Carey/B-7772-2016 OI Lisse, Carey/0000-0002-9548-1526 FU NASA [1353184, NNX11AD21G]; ANR [ANR-07-BLAN-0221, ANR-2010-JCJC-0504-01, ANR-2010-JCJC-0501-01]; European Commission's 7th Framework Program [PERG06-GA-2009-256513]; European Union through ERC [279973]; NSF [AST-0909188]; JPL/NASA [NMO711043]; NSERC Discovery Accelerator Supplement FX We are grateful to Tushar Mittal, Christine Chen, and Karl Stapelfeldt for discussions regarding various aspects of the data analyzed here, and to Angelo Ricarte and Noel Moldvai for their contribution to the modified blackbody model used in this work. We thank the DEBRIS team for many and varied fruitful discussions throughout the duration of this project. In particular, we are grateful to Paul Harvey for his review of a draft of this manuscript. Comments from an anonymous referee also helped improved this manuscript. This work was supported in part by NASA through a contract (No. 1353184, PI: H. M. Butner) issued by the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. We acknowledge the Service Commun de Calcul Intensif de l'Observatoire de Grenoble (SCCI) for computations on the super-computer funded by ANR (contracts ANR-07-BLAN-0221, ANR-2010-JCJC-0504-01 and ANR-2010-JCJC-0501-01) and the European Commission's 7th Framework Program (contract PERG06-GA-2009-256513). M.W. and G.K. are grateful for support from the European Union through ERC grant number 279973. C.L. acknowledges support from grants NASA NNX11AB21G and NSF AAG-NNX09AU31G in working on this project. P.K. acknowledges support from NASA NNX11AD21G, NSF AST-0909188, and JPL/NASA award NMO711043. M.B. acknowledges support from an NSERC Discovery Accelerator Supplement. Data presented in this paper were obtained with Herschel, an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. Additional data presented in this work were obtained at the JCMT, which is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK, the Netherlands Organisation for Scientific Research and the National Research Council of Canada. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 95 TC 18 Z9 18 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 148 DI 10.1088/0004-637X/784/2/148 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400063 ER PT J AU Hamaguchi, K Corcoran, MF Russell, CMP Pollock, AMT Gull, TR Teodoro, M Madura, TI Damineli, A Pittard, JM AF Hamaguchi, Kenji Corcoran, Michael F. Russell, Christopher M. P. Pollock, A. M. T. Gull, Theodore R. Teodoro, Mairan Madura, Thomas I. Damineli, Augusto Pittard, Julian M. TI X-RAY EMISSION FROM ETA CARINAE NEAR PERIASTRON IN 2009. I. A TWO-STATE SOLUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; stars: early-type; stars: individual (Eta Carinae); stars: winds; outflows X-rays: stars ID BINARY WR 140; COLLIDING WINDS; EVENT; COMPANION; VARIABILITY; LAMBDA-4686; COLLISION; MINIMUM; STARS AB X-ray emission from the supermassive binary system. Car declines sharply around periastron. This X-ray minimum has two distinct phases-the lowest flux phase in the first similar to 3 weeks and a brighter phase thereafter. In 2009, the Chandra X-ray Observatory monitored the first phase five times and found the lowest observed flux at similar to 1.9 x 10(-12) erg cm(-2) s(-1) (3-8 keV). The spectral shape changed such that the hard band above similar to 4 keV dropped quickly at the beginning and the soft band flux gradually decreased to its lowest observed value in similar to 2 weeks. The hard band spectrum had begun to recover by that time. This spectral variation suggests that the shocked gas producing the hottest X-ray gas near the apex of the wind-wind collision (WWC) is blocked behind the dense inner wind of the primary star, which later occults slightly cooler gas downstream. Shocked gas previously produced by the system at earlier orbital phases is suggested to produce the faint residual X-ray emission seen when the emission near the apex is completely blocked by the primary wind. The brighter phase is probably caused by the re-appearance of the WWC plasma, whose emissivity significantly declined during the occultation. We interpret this to mean that the X-ray minimum is produced by a hybrid mechanism of an occultation and a decline in the emissivity of the WWC shock. We constrain timings of superior conjunction and periastron based on these results. C1 [Hamaguchi, Kenji; Corcoran, Michael F.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA. [Hamaguchi, Kenji; Corcoran, Michael F.] NASA, Xray Astrophys Lab, GSFC, Greenbelt, MD 20771 USA. [Hamaguchi, Kenji] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Corcoran, Michael F.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Russell, Christopher M. P.] Hokkai Gakuen Univ, Fac Engn, Toyohira Ku, Sapporo, Hokkaido 0628605, Japan. [Pollock, A. M. T.] European Space Agcy, E-28691 Madrid, Spain. [Gull, Theodore R.; Teodoro, Mairan; Madura, Thomas I.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Damineli, Augusto] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508900 Sao Paulo, Brazil. [Pittard, Julian M.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. RP Hamaguchi, K (reprint author), NASA, CRESST, GSFC, Greenbelt, MD 20771 USA. EM Kenji.Hamaguchi@nasa.gov RI Damineli, Augusto/P-8829-2016; OI Damineli, Augusto/0000-0002-7978-2994; Pittard, Julian/0000-0003-2244-5070 FU NASA's Astrobiology Institute [RTOP 344-53-51] FX This work was performed while K. H. was supported by the NASA's Astrobiology Institute (RTOP 344-53-51) to the Goddard Center for Astrobiology (PI: Michael J. Mumma). This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. We appreciate the Chandra operation scientist Scott J. Wolk for important advice on enhancing efficiency of the Chandra observations and useful comments on the paper draft by David B. Henley and Kris Davidson. NR 41 TC 11 Z9 11 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 125 DI 10.1088/0004-637X/784/2/125 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400040 ER PT J AU Hardegree-Ullman, EE Gudipati, MS Boogert, ACA Lignell, H Allamandola, LJ Stapelfeldt, KR Werner, M AF Hardegree-Ullman, E. E. Gudipati, M. S. Boogert, A. C. A. Lignell, H. Allamandola, L. J. Stapelfeldt, K. R. Werner, M. TI LABORATORY DETERMINATION OF THE INFRARED BAND STRENGTHS OF PYRENE FROZEN IN WATER ICE: IMPLICATIONS FOR THE COMPOSITION OF INTERSTELLAR ICES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: ISM; ISM: abundances; methods: laboratory: molecular; stars: protostars ID POLYCYCLIC AROMATIC-HYDROCARBONS; YOUNG STELLAR OBJECTS; 3 MICRON SPECTRA; SPECTROSCOPIC DATABASE; ABSORPTION FEATURES; MONOCEROS R2/IRS-3; FACILE GENERATION; RADICAL CATIONS; AMINO-ACIDS; SOLID H2O AB Broad infrared emission features (e.g., at 3.3, 6.2, 7.7, 8.6, and 11.3 mu m) from the gas phase interstellar medium have long been attributed to polycyclic aromatic hydrocarbons (PAHs). A significant portion (10%-20%) of the Milky Way's carbon reservoir is locked in PAH molecules, which makes their characterization integral to our understanding of astrochemistry. In molecular clouds and the dense envelopes and disks of young stellar objects (YSOs), PAHs are expected to be frozen in the icy mantles of dust grains where they should reveal themselves through infrared absorption. To facilitate the search for frozen interstellar PAHs, laboratory experiments were conducted to determine the positions and strengths of the bands of pyrene mixed with H2O and D2O ices. The D2O mixtures are used tomeasure pyrene bands that aremasked by the strong bands of H2O, leading to the first laboratory determination of the band strength for the CH stretching mode of pyrene in water ice near 3.25 mu m. Our infrared band strengths were normalized to experimentally determined ultraviolet band strengths, and we find that they are generally similar to 50% larger than those reported by Bouwman et al. based on theoretical strengths. These improved band strengths were used to reexamine YSO spectra published by Boogert et al. to estimate the contribution of frozen PAHs to absorption in the 5-8 mu m spectral region, taking into account the strength of the 3.25 mu m CH stretching mode. It is found that frozen neutral PAHs contain 5%-9% of the cosmic carbon budget and account for 2%-9% of the unidentified absorption in the 5-8 mu m region. C1 [Hardegree-Ullman, E. E.] Rensselaer Polytech Inst, New York Ctr Astrobiol, Troy, NY 12180 USA. [Hardegree-Ullman, E. E.] Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA. [Hardegree-Ullman, E. E.; Boogert, A. C. A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Gudipati, M. S.; Werner, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gudipati, M. S.] Univ Maryland, IPST, College Pk, MD 20742 USA. [Boogert, A. C. A.] NASA Ames Res Ctr, SOFIA Sci Ctr, USRA, Moffett Field, CA 94035 USA. [Lignell, H.] Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. [Lignell, H.] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. [Allamandola, L. J.] NASA Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Stapelfeldt, K. R.] NASA Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. RP Hardegree-Ullman, EE (reprint author), Rensselaer Polytech Inst, New York Ctr Astrobiol, 110 8th St, Troy, NY 12180 USA. EM hardee@rpi.edu; gudipati@jpl.nasa.gov RI Gudipati, Murthy/F-7575-2011 FU NASA Astrobiology Institute to Rensselaer Polytechnic Institute [NNA09DA80A]; Jet Propulsion Laboratory's DRDF and R&TD funding for infrastructure of the "Ice Spectroscopy Laboratory"; Spitzer Space Telescope; Finnish Cultural Foundation; IPAC Visiting Graduate Student Fellowship FX This research was carried out at the Jet Propulsion Laboratory and IPAC, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Support for this research was provided in part by funding from the NASA Astrobiology Institute to Rensselaer Polytechnic Institute (award NNA09DA80A). The experimental part of this work was enabled through partial funding from the Jet Propulsion Laboratory's DRDF and R&TD funding for infrastructure of the "Ice Spectroscopy Laboratory" and was carried out by H.L. and M. S. G., supported by an astrophysics laboratory research award funded by the Spitzer Space Telescope. H.L. also acknowledges the Finnish Cultural Foundation for financial support. We thank Dr. Irene Li Barnett and Dr. Antti Lignell, who were involved in building the experimental setup used and initial training of H.L. Data analysis was carried out by E.H-U. at the California Institute of Technology (supervised by A.B. and M.S.G.), funded by an IPAC Visiting Graduate Student Fellowship. NR 42 TC 5 Z9 5 U1 2 U2 19 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 APR 1 PY 2014 VL 784 IS 2 AR 172 DI 10.1088/0004-637X/784/2/172 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400087 ER PT J AU Lionello, R Velli, M Downs, C Linker, JA Mikic, Z Verdini, A AF Lionello, Roberto Velli, Marco Downs, Cooper Linker, Jon A. Mikic, Zoran Verdini, Andrea TI VALIDATING A TIME-DEPENDENT TURBULENCE-DRIVEN MODEL OF THE SOLAR WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); solar wind; turbulence; waves ID ALFVEN WAVES; MHD TURBULENCE; CORONAL HOLES; MAGNETOHYDRODYNAMIC TURBULENCE; TRANSITION REGION; STELLAR CORONAE; ENERGY-BALANCE; ACCELERATION; TRANSPORT; FLOW AB Although the mechanisms responsible for heating the Sun's corona and accelerating the solar wind are still being actively investigated, it is largely accepted that photospheric motions provide the energy source and that the magnetic field must play a key role in the process. Verdini et al. presented a model for heating and accelerating the solar wind based on the turbulent dissipation of Alfven waves. We first use a time-dependent model of the solar wind to reproduce one of Verdini et al.'s solutions; then, we extend its application to the case where the energy equation includes thermal conduction and radiation losses, and the upper chromosphere is part of the computational domain. Using this model, we explore the parameter space and describe the characteristics of a fast solar wind solution. We discuss how this formulation may be applied to a three-dimensional MHD model of the corona and solar wind. C1 [Lionello, Roberto; Downs, Cooper; Linker, Jon A.; Mikic, Zoran] Predict Sci Inc, San Diego, CA 92121 USA. [Velli, Marco] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Verdini, Andrea] Observ Royal Belgique, B-1180 Brussels, Belgium. RP Lionello, R (reprint author), Predict Sci Inc, 9990 Mesa Rim Rd,Suite 170, San Diego, CA 92121 USA. EM lionel@predsci.com; mvelli@mail.jpl.nasa.gov; cdowns@predsci.com; linker@predsci.com; mikic@predsci.com; verdini@oma.be FU NASA's LWS TR&T and HTP programs; Center for Integrated Space Weather Modeling; NASA Solar Probe Plus Observatory Scientist contract; Texas Advanced Computing Center (TACC) in Austin; NASA Advanced Supercomputing Division (NAS) at Ames Research Center FX Work carried out at PSI was supported by NASA's LWS TR&T and HTP programs, and the Center for Integrated Space Weather Modeling (an NSF Science and Technology Center). This work was carried out in part by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. M. V. was supported by the NASA Solar Probe Plus Observatory Scientist contract. Computational resources were provided by the NSF supported Texas Advanced Computing Center (TACC) in Austin and the NASA Advanced Supercomputing Division (NAS) at Ames Research Center. NR 55 TC 16 Z9 16 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 DI 10.1088/0004-637X/784/2/120 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400035 ER PT J AU Mackay, DH DeVore, CR Antiochos, SK AF Mackay, Duncan H. DeVore, C. Richard Antiochos, Spiro K. TI GLOBAL-SCALE CONSEQUENCES OF MAGNETIC-HELICITY INJECTION AND CONDENSATION ON THE SUN SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; Sun: activity; Sun: corona ID DRIVEN VORTEX FLOWS; SOLAR CORONA; HEMISPHERIC PATTERN; FILAMENT CHANNELS; FLUX TRANSPORT; FINE-STRUCTURE; FIELDS; PROMINENCES; CHIRALITY; EVOLUTION AB In the recent paper of Antiochos, a new concept for the injection of magnetic helicity into the solar corona by small-scale convective motions and its condensation onto polarity inversion lines (PILs) was developed. We investigate this concept through global simulations of the Sun's photospheric and coronal magnetic fields, and compare the results with the hemispheric pattern of solar filaments. Assuming that the vorticity of the cells is predominantly counterclockwise/clockwise in the northern/southern hemisphere, the convective motions inject negative/positive helicity into each hemisphere. The simulations show that: (1) on a north-south oriented PIL, both differential rotation and convective motions inject the same sign of helicity, which matches that required to reproduce the hemispheric pattern of filaments. (2) On a high-latitude east-west oriented polar crown or subpolar crown PIL, the vorticity of the cells has to be approximately 2-3 times greater than the local differential-rotation gradient in order to overcome the incorrect sign of helicity injection from differential rotation. (3) In the declining phase of the cycle, as a bipole interacts with the polar field, in some cases, helicity condensation can reverse the effect of differential rotation along the east-west lead arm but not in all cases. The results show that this newly developed concept of magnetic helicity injection and condensation, in conjunction with the mechanisms used in Yeates et al., is a viable explanation for the hemispheric pattern of filaments. Future observational studies should focus on examining the vorticity component within convective motions to determine both its magnitude and latitudinal variation relative to the differential-rotation gradient on the Sun. C1 [Mackay, Duncan H.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. [DeVore, C. Richard] Naval Res Lab, Washington, DC 20375 USA. [DeVore, C. Richard; Antiochos, Spiro K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mackay, DH (reprint author), Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. EM dhm@st-and.ac.uk RI DeVore, C/A-6067-2015; Antiochos, Spiro/D-4668-2012 OI DeVore, C/0000-0002-4668-591X; Antiochos, Spiro/0000-0003-0176-4312 FU STFC; Leverhulme Trust; European Commission [263340]; NASA TR&T and SRT programs FX D.H.M. would like to thank STFC, the Leverhulme Trust, and the European Commission's Seventh Framework Programme (FP7/2007-2013) under grant agreement SWIFF (project 263340, http://www.swiff.eu) for their financial support. C.R.D. and S.K.A. wish to acknowledge the NASA TR&T and SR&T programs for supporting their contributions to the work. All of us thank Judy Karpen for lending her artistic expertise in creating the figures used in the Appendix and for helpful comments on the manuscript. We also appreciate Anthony Yeates' alerting us to the observations of J.A. Bonet and collaborators. D.H.M. and C.R.D. participated in a team investigation of solar prominences at the International Space Science Institute, where this collaboration was conceived and initiated. We are grateful to ISSI for hosting us, to Nicolas Labrosse for leading the team, and to Zoran Mikic and the rest of the group for stimulating discussions. NR 50 TC 10 Z9 10 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 164 DI 10.1088/0004-637X/784/2/164 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400079 ER PT J AU Mainzer, A Bauer, J Grav, T Masiero, J Cutri, RM Wright, E Nugent, CR Stevenson, R Clyne, E Cukrov, G Masci, F AF Mainzer, A. Bauer, J. Grav, T. Masiero, J. Cutri, R. M. Wright, E. Nugent, C. R. Stevenson, R. Clyne, E. Cukrov, G. Masci, F. TI THE POPULATION OF TINY NEAR-EARTH OBJECTS OBSERVED BY NEOWISE SO ASTROPHYSICAL JOURNAL LA English DT Article DE atlases; catalogs; infrared: general; minor planets; asteroids: general; surveys ID THERMAL-MODEL CALIBRATION; INFRARED-SURVEY-EXPLORER; WISE/NEOWISE OBSERVATIONS; PHASE CURVES; ASTEROIDS; PHOTOMETRY; SYSTEM AB Only a very small fraction of the asteroid population at size scales comparable to the object that exploded over Chelyabinsk, Russia has been discovered to date, and physical properties are poorly characterized. We present previously unreported detections of 105 close approaching near-Earth objects (NEOs) by the Wide-field Infrared Survey Explorer (WISE) mission's NEOWISE project. These infrared observations constrain physical properties such as diameter and albedo for these objects, many of which are found to be smaller than 100 m. Because these objects are intrinsically faint, they were detected by WISE during very close approaches to the Earth, often at large apparent on-sky velocities. We observe a trend of increasing albedo with decreasing size, but as this sample of NEOs was discovered by visible light surveys, it is likely that selection biases against finding small, dark NEOs influence this finding. C1 [Mainzer, A.; Bauer, J.; Masiero, J.; Nugent, C. R.; Stevenson, R.; Clyne, E.; Cukrov, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bauer, J.; Cutri, R. M.; Masci, F.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Grav, T.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Wright, E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM amainzer@jpl.nasa.gov OI Masiero, Joseph/0000-0003-2638-720X FU National Aeronautics and Space Administration; Planetary Science Division of the National Aeronautics and Space Administration FX This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. We thank our referee, Dr. Alan Harris of Pasadena, for his helpful comments that materially improved this manuscript. We gratefully acknowledge the extraordinary services specific to NEOWISE contributed by the International Astronomical Union's Minor Planet Center, operated by the Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for Astronomical Telegrams, operated by Harvard University. We also thank the worldwide community of dedicated amateur and professional astronomers devoted to minor planet follow-up observations. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 41 TC 13 Z9 13 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 APR 1 PY 2014 VL 784 IS 2 AR 110 DI 10.1088/0004-637X/784/2/110 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400025 ER PT J AU Nguyen, AN Messenger, S AF Nguyen, Ann N. Messenger, Scott TI RESOLVING THE STELLAR SOURCES OF ISOTOPICALLY RARE PRESOLAR SILICATE GRAINS THROUGH Mg AND Fe ISOTOPIC ANALYSES SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; novae, cataclysmic variables; nuclear reactions, nucleosynthesis, abundances; stars: winds, outflows; supernovae: general ID ASYMPTOTIC GIANT BRANCH; LARGE-MAGELLANIC-CLOUD; AGB STARS; MASSIVE STARS; SOLAR-SYSTEM; SIC GRAINS; CARBONACEOUS CHONDRITE; INTERSTELLAR GRAINS; CHEMICAL EVOLUTION; GALACTIC EVOLUTION AB We conducted multi-element isotopic analyses of 11 presolar silicate grains from the Acfer 094 meteorite having unusual O isotopic compositions. Eight grains are O-18-rich, one is O-16-rich, and two are extremely O-17-rich. We constrained the grains' stellar sources by measuring their Si and Mg isotopic ratios, and also the Fe-54/Fe-56 and Fe-57/Fe-56 ratios for five grains. The Mg and Fe isotopic measurements were conducted after surrounding matrix grains were removed for more accurate ratios. Most of the O-18-rich silicates had anomalous Mg isotopic ratios, and their combined isotopic constraints are consistent with origins in low-mass Type II supernovae (SNe II) rather than high-metallicity stars. The isotopic ratios of the O-16-rich silicate are also consistent with an SN origin. Mixing small amounts of interior stellar material with the stellar envelope replicated all measured isotopic ratios except for Si-29/ Si-28 and Fe-54/Fe-56 in some grains. The Si-29/Si-28 ratios of all SN-derived grains are matched by doubling the Si-29 yield in the Ne- and Si-burning zones. The Fe-54/Fe-56 ratios of the grains imply elemental fractionation in the Si/S zone, or introduction of isotopically solar Fe by secondary processing. The two highly 17O-rich silicates exhibited significant Mg-25 and/or Mg-26 enrichments and their isotopic ratios are best explained by strong dilution of 1.15M(circle dot) CO nova matter. We estimate that similar to 12% and 1% of presolar silicates have SN and nova origins, respectively, similar to presolar SiC and oxides. This implies that asymptotic giant branch stars are the dominant dust producers in the galaxy. C1 [Nguyen, Ann N.; Messenger, Scott] NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. [Nguyen, Ann N.] NASA, Lyndon B Johnson Space Ctr, Jacobs, Houston, TX 77058 USA. RP Nguyen, AN (reprint author), NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. EM lan-anh.n.nguyen@nasa.gov FU NASA Cosmochemistry [12-COS12-0058] FX We thank M. Ito for assistance with Mg isotopic measurements and Z. Rahman for FIB preparation of the samples. We are grateful to F. Gyngard, S. Woosley, and A. Heger for providing stellar model results. This manuscript was improved by comments from an anonymous reviewer. This work was supported by NASA Cosmochemistry grant 12-COS12-0058. NR 84 TC 5 Z9 5 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 149 DI 10.1088/0004-637X/784/2/149 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400064 ER PT J AU Peacock, MB Zepf, SE Maccarone, TJ Kundu, A Gonzalez, AH Lehmer, BD Maraston, C AF Peacock, Mark B. Zepf, Stephen E. Maccarone, Thomas J. Kundu, Arunav Gonzalez, Anthony H. Lehmer, Bret D. Maraston, Claudia TI EVIDENCE FOR A CONSTANT INITIAL MASS FUNCTION IN EARLY-TYPE GALAXIES BASED ON THEIR X-RAY BINARY POPULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: stellar content; stars: luminosity function; mass function; X-rays: binaries ID CHANDRA MONITORING OBSERVATIONS; GLOBULAR-CLUSTER CONNECTION; HUBBLE-SPACE-TELESCOPE; SURFACE BRIGHTNESS FLUCTUATIONS; INFRARED FUNDAMENTAL PLANE; ELLIPTIC GALAXIES; STELLAR POPULATIONS; DEEP CHANDRA; SYSTEMATIC VARIATION; LUMINOSITY FUNCTIONS AB A number of recent studies have proposed that the stellar initial mass function (IMF) of early type galaxies varies systematically as a function of galaxy mass, with higher mass galaxies having bottom-heavy IMFs. These bottom-heavy IMFs have more low-mass stars relative to the number of high mass stars, and therefore naturally result in proportionally fewer neutron stars (NSs) and black holes (BHs). In this paper, we specifically predict the variation in the number of BHs and NSs based on the power-law IMF variation required to reproduce the observed mass-to-light ratio trends with galaxy mass. We then test whether such variations are observed by studying the field low-mass X-ray binary (LMXB) populations of nearby early-type galaxies. In these binaries, an NS or BH accretes matter from a low-mass donor star. Their number is therefore expected to scale with the number of BHs and NSs present in a galaxy. We find that the number of LMXBs per K-band light is similar among the galaxies in our sample. These data therefore demonstrate the uniformity of the slope of the IMF from massive stars down to those now dominating the K-band light and are consistent with an invariant IMF. Our results are inconsistent with an IMF which varies from a Kroupa/Chabrier like IMF for low-mass galaxies to a steep power-law IMF (with slope x = 2.8) for high mass galaxies. We discuss how these observations constrain the possible forms of the IMF variations and how future Chandra observations can enable sharper tests of the IMF. C1 [Peacock, Mark B.; Zepf, Stephen E.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Maccarone, Thomas J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Kundu, Arunav] Eureka Sci Inc, Oakland, CA 100 USA. [Kundu, Arunav] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Lehmer, Bret D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Lehmer, Bret D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Maraston, Claudia] Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. RP Peacock, MB (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM mpeacock@msu.edu FU NASA through ADAP [NNX11AG12G]; Chandra [AR4-15007X]; NASA through Chandra [GO0-11111A, AR1-12009X] FX M.B.P. and S.E.Z. acknowledge support from NASA through the ADAP grant NNX11AG12G and through the Chandra award AR4-15007X. A.K. acknowledges support for this work provided by NASA through Chandra awards GO0-11111A and AR1-12009X. NR 88 TC 16 Z9 16 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 APR 1 PY 2014 VL 784 IS 2 AR 162 DI 10.1088/0004-637X/784/2/162 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400077 ER PT J AU Regnier, S Alexander, CE Walsh, RW Winebarger, AR Cirtain, J Golub, L Korreck, KE Mitchell, N Platt, S Weber, M De Pontieu, B Title, A Kobayashi, K Kuzin, S DeForest, CE AF Regnier, S. Alexander, C. E. Walsh, R. W. Winebarger, A. R. Cirtain, J. Golub, L. Korreck, K. E. Mitchell, N. Platt, S. Weber, M. De Pontieu, B. Title, A. Kobayashi, K. Kuzin, S. DeForest, C. E. TI SPARKLING EXTREME-ULTRAVIOLET BRIGHT DOTS OBSERVED WITH Hi-C SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: magnetic fields; Sun: UV radiation ID DYNAMICS-OBSERVATORY SDO; SOLAR MAGNETIC ELEMENTS; CORONA; REGIONS; DIAGNOSTICS; NANOFLARES; RESOLUTION; TELESCOPE; EVENTS; PLASMA AB Observing the Sun at high time and spatial scales is a step toward understanding the finest and fundamental scales of heating events in the solar corona. The high-resolution coronal (Hi-C) instrument has provided the highest spatial and temporal resolution images of the solar corona in the EUV wavelength range to date. Hi-C observed an active region on 2012 July 11 that exhibits several interesting features in the EUV line at 193 angstrom. One of them is the existence of short, small brightenings "sparkling" at the edge of the active region; we call these EUV bright dots (EBDs). Individual EBDs have a characteristic duration of 25 s with a characteristic length of 680 km. These brightenings are not fully resolved by the SDO/AIA instrument at the same wavelength; however, they can be identified with respect to the Hi-C location of the EBDs. In addition, EBDs are seen in other chromospheric/coronal channels of SDO/AIA, which suggests a temperature between 0.5 and 1.5 MK. Based on their frequency in the Hi-C time series, we define four different categories of EBDs: single peak, double peak, long duration, and bursty. Based on a potential field extrapolation from an SDO/HMI magnetogram, the EBDs appear at the footpoints of large-scale, trans-equatorial coronal loops. The Hi-C observations provide the first evidence of small-scale EUV heating events at the base of these coronal loops, which have a free magnetic energy of the order of 10(26) erg. C1 [Regnier, S.; Alexander, C. E.; Walsh, R. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Winebarger, A. R.; Cirtain, J.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Golub, L.; Korreck, K. E.; Weber, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mitchell, N.; Platt, S.] Univ Cent Lancashire, Sch Comp Engn & Phys Sci, Preston PR1 2HE, Lancs, England. [De Pontieu, B.; Title, A.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Kobayashi, K.] Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA. [Kuzin, S.] Russian Acad Sci, PN Lebedev Phys Inst, Moscow 119991, Russia. [DeForest, C. E.] Southwest Res Inst, Boulder, CO 80302 USA. RP Regnier, S (reprint author), Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. RI Regnier, Stephane/H-9107-2012; Kuzin, Sergey/M-3435-2015; Regnier, Stephane/K-2423-2015; Platt, Simon/C-6048-2008 OI Regnier, Stephane/0000-0001-8954-4183; Regnier, Stephane/0000-0001-8954-4183; Platt, Simon/0000-0003-4431-8814 NR 32 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 134 DI 10.1088/0004-637X/784/2/134 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400049 ER PT J AU Scully, ST Malkan, MA Stecker, FW AF Scully, Sean T. Malkan, Matthew A. Stecker, Floyd W. TI AN EMPIRICAL DETERMINATION OF THE INTERGALACTIC BACKGROUND LIGHT USING NEAR-INFRARED DEEP GALAXY SURVEY DATA OUT TO 5 mu m AND THE GAMMA-RAY OPACITY OF THE UNIVERSE SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (PKS 1424+240); diffuse radiation; gamma rays: general ID LUMINOSITY FUNCTION; OPTICAL DEPTH; PKS 1424+240; LOWER-LIMIT; K-BAND; TO 4; EVOLUTION; REDSHIFT; SPECTRA; BLAZARS AB We extend our previous model-independent determination of the intergalactic background light, based purely on galaxy survey data, out to a wavelength of 5 mu m. Our approach enables us to constrain the range of photon densities, based on the uncertainties from observationally determined luminosity densities and colors. We further determine a 68% confidence upper and lower limit on the opacity of the universe to gamma-rays up to energies of 1.6/(1 + z) TeV. A comparison of our lower limit redshift-dependent opacity curves to the opacity limits derived from the results of both ground-based air Cerenkov telescope and Fermi-LAT observations of PKS 1424+240 allows us to place a new upper limit on the redshift of this source, independent of IBL modeling. C1 [Scully, Sean T.] James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA. [Malkan, Matthew A.; Stecker, Floyd W.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Stecker, Floyd W.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Scully, ST (reprint author), James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA. EM Floyd.W.Stecker@nasa.gov NR 43 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 APR 1 PY 2014 VL 784 IS 2 AR 138 DI 10.1088/0004-637X/784/2/138 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400053 ER PT J AU Swain, MR Line, MR Deroo, P AF Swain, Mark R. Line, Michael R. Deroo, Pieter TI ON THE DETECTION OF MOLECULES IN THE ATMOSPHERE OF HD 189733b USING HST NICMOS TRANSMISSION SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; planetary systems; planets and satellites: atmospheres; planets and satellites: individual (HD 189733b); radiative transfer ID HUBBLE-SPACE-TELESCOPE; KECK INTERFEROMETER; EXTRASOLAR PLANET; SUPER-EARTHS; SPECTRUM; WATER; RETRIEVAL; HD189733B; WASP-12B; 209458B AB The Hubble Space Telescope/NICMOS transmission spectrum measurements of HD 189733b that suggest the detection of methane (CH4) in an exoplanet atmosphere have been a source of significant controversy. With what is probably the best analyzed exoplanet spectroscopy data set to date, different teams, using different methods, have claimed evidence both contradicting and supporting the original findings. Here, we report results from a uniform spectral retrieval analysis of the three independent published spectra together with null hypothesis testing. Based on Bayesian model comparison, we find that two of the three spectra show strong evidence (>= 3.6 sigma) for the detection of molecular features mainly due to water and methane while the third is consistent with a weak molecular detection at the 2.2 sigma level. We interpret the agreement in the spectral modulation established by previous authors and the atmospheric retrieval results presented here, as a confirmation of the original detection of molecular absorbers in the atmosphere of HD 189733b. C1 [Swain, Mark R.; Deroo, Pieter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Line, Michael R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Swain, MR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Mark.R.Swain@jpl.nasa.gov NR 44 TC 21 Z9 21 U1 0 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 APR 1 PY 2014 VL 784 IS 2 AR 133 DI 10.1088/0004-637X/784/2/133 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400048 ER PT J AU Acikmese, B Mandic, M Speyer, JL AF Acikmese, Behcet Mandic, Milan Speyer, Jason L. TI Decentralized observers with consensus filters for distributed discrete-time linear systems SO AUTOMATICA LA English DT Article DE Observers; Distributed systems; Graph theory; Linear matrix inequalities ID MULTIAGENT SYSTEMS; COMMUNICATION; ESTIMATORS; TOPOLOGIES; NETWORKS; GRAPHS; AGENTS AB This paper presents a decentralized observer with a consensus filter for the state observation of discrete-time linear distributed systems. Each agent in the distributed system has an observer with a model of the plant that utilizes the set of locally available measurements, which may not make the full plant state detectable. This lack of detectability is overcome by utilizing a consensus filter that blends the state estimate of each agent with its neighbors' estimates. It is proven that the state estimates of the proposed observer exponentially converge to the actual plant states under arbitrarily changing, but connected, communication and pseudo-connected sensing graph topologies. Except these connectivity properties, full knowledge of the sensing and communication graphs is not needed at the design time. As a byproduct, we obtained a result on the location of eigenvalues, i.e., the spectrum, of the Laplacian for a family of graphs with self-loops. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Acikmese, Behcet] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA. [Mandic, Milan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Speyer, Jason L.] Univ Calif Los Angeles, Mech & Aerosp Engn Dept, Los Angeles, CA 90095 USA. [Speyer, Jason L.] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA. RP Acikmese, B (reprint author), Univ Texas Austin, Dept Aerosp Engn & Engn Mech, 210 E 24th St, Austin, TX 78712 USA. EM behcet@austin.utexas.edu; Milan.Mandic@jpl.nasa.gov; speyer@seas.ucla.edu NR 34 TC 8 Z9 8 U1 2 U2 20 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0005-1098 EI 1873-2836 J9 AUTOMATICA JI Automatica PD APR PY 2014 VL 50 IS 4 BP 1037 EP 1052 DI 10.1016/j.automatica.2014.02.008 PG 16 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA AG7WA UT WOS:000335628300004 ER PT J AU Friedman, BH Stephens, CL Thayer, JF AF Friedman, Bruce H. Stephens, Chad L. Thayer, Julian F. TI Redundancy analysis of autonomic and self-reported, responses to induced emotions SO BIOLOGICAL PSYCHOLOGY LA English DT Article DE Emotion concordance; Emotion synchrony; Autonomic nervous system; Multivariate analysis; Redundancy analysis ID TORONTO-ALEXITHYMIA-SCALE; CANONICAL CORRELATION; BASIC EMOTIONS; NATURAL KINDS; VAGAL TONE; MULTIVARIATE; SPECIFICITY; IMAGERY; DISCRIMINANT; PERSPECTIVE AB The issue of concordance among the elements of emotional states has been prominent in the literature since Lang (1968) explored the topic in relation to therapy for anxiety. Since that time, a consensus has emerged that concordance among these components is relatively low. To address this issue, redundancy analysis, a technique for examining directional relationships between two sets of multivariate data, was applied to data from a previously published study (Stephens, Christie,& Friedman, 2010). Subjects in this study listened to emotion-inducing music and viewed affective films while a montage of autonomic variables, as well as self-reported affective responses, were recorded. Results indicated that approximately 27-28% of the variance in self-reported affect could be explained by autonomic variables, and vice-versa. When all of the constraints of this emotion research paradigm are considered, these levels of explained variance indicate substantial coherence between feelings and physiology during the emotion inductions. These results are considered vis-a-vis the low levels of coherence that have often been reported in the literature. (C) 2013 Elsevier B.V. All rights reserved. C1 [Friedman, Bruce H.] Virginia Polytech Inst & State Univ, Dept Psychol 0436, Blacksburg, VA 24061 USA. [Stephens, Chad L.] Virginia Polytech Inst & State Univ, Blacksburg, VA 24061 USA. [Stephens, Chad L.] NASA, Langley Res Ctr, Hampton, VA USA. [Thayer, Julian F.] Ohio State Univ, Dept Psychol, Columbus, OH 43210 USA. RP Friedman, BH (reprint author), Virginia Polytech Inst & State Univ, Dept Psychol 0436, Blacksburg, VA 24061 USA. EM bhfriedm@vt.edu NR 86 TC 8 Z9 8 U1 19 U2 37 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0301-0511 EI 1873-6246 J9 BIOL PSYCHOL JI Biol. Psychol. PD APR PY 2014 VL 98 BP 19 EP 28 DI 10.1016/j.biopsycho.2013.12.006 PG 10 WC Psychology, Biological; Behavioral Sciences; Psychology; Psychology, Experimental SC Psychology; Behavioral Sciences GA AG6AE UT WOS:000335499900003 PM 24380823 ER PT J AU Czabaj, MW Ratcliffe, JG Davidson, BD AF Czabaj, M. W. Ratcliffe, J. G. Davidson, B. D. TI Observation of intralaminar cracking in the edge crack torsion specimen SO ENGINEERING FRACTURE MECHANICS LA English DT Article DE Polymer matrix composites; Toughness testing; Delamination; Mode III; Damage tolerance; Fracture mechanics ID III INTERLAMINAR FRACTURE; I PLUS III; COMPOSITE-MATERIALS; ECT TEST; MODE; TOUGHNESS; SHEAR AB The edge crack torsion (ECT) test is evaluated to determine its suitability for measuring fracture toughness associated with the onset of mode III delamination in laminated composites. ECT specimens with preimplanted midplane inserts of different lengths are tested and examined using nondestructive and destructive techniques. Ultrasonic inspections of all tested specimens reveal that delamination growth occurs one ply interface beneath the midplane. This is confirmed by sectioning and optical microscopy, which also show that macroscopic delamination advance results from a coalescence of angled intralaminar matrix cracks that form in-between and then extend through the midplane plies. The relative orientation of these intralaminar cracks is approximately 45 with respect to the midplane, suggesting that their formation is caused by resolved principal tensile stresses arising due to the global mode III shear loading. Examination of ECT specimens tested to loads below the level corresponding to the onset of delamination growth reveals that initiation of intralaminar cracking occurs prior to or concurrently with the onset of nonlinearity in the specimen's force-displacement response. The existence of intralaminar cracking prior to delamination growth and the resulting delamination extension at an unintended interface render the ECT test, in its current form, unsuitable for characterizing the onset of mode III delamination growth. The broader implications of the mechanisms observed in this study are also discussed with respect to the current understanding of shear-driven delamination in tape-laminate composites. Published by Elsevier Ltd. C1 [Czabaj, M. W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Ratcliffe, J. G.] Natl Inst Aerosp, Hampton, VA 23666 USA. [Davidson, B. D.] Syracuse Univ, Syracuse, NY 13244 USA. RP Czabaj, MW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM michael.w.czabaj@nasa.gov NR 32 TC 5 Z9 5 U1 1 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0013-7944 EI 1873-7315 J9 ENG FRACT MECH JI Eng. Fract. Mech. PD APR PY 2014 VL 120 BP 1 EP 14 DI 10.1016/j.engfracmech.2014.03.002 PG 14 WC Mechanics SC Mechanics GA AG7PV UT WOS:000335611200001 ER PT J AU Bue, BD AF Bue, Brian D. TI An Evaluation of Low-Rank Mahalanobis Metric Learning Techniques for Hyperspectral Image Classification SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Classification; Compact Reconnaissance Imaging Spectrometer for Mars (CRISM); dimensionality reduction; hyperspectral; low rank; Mahalanobis; metric learning ID ALGORITHM AB We provide a comparative study of several state-of-the-art Mahalanobis metric learning algorithms evaluated on three well-studied, high-dimensional hyperspectral images captured by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instrument. We focus on the problem of low-rank Mahalanobis metric learning, where our objective is to learn an n x m projection matrix, where m << n. Low-rank metrics offer a "plug-in" enhancement to similarity-based classifiers that can reduce computation time and improve classification accuracy with fewer training samples, enabling operations in resource-constrained environments such as onboard spacecraft. Our results indicate that applying a simple shrinkage-based regularization procedure to multi-class Linear Discriminant Analysis (LDA) produces comparable or better classification accuracies than the low-rank extensions of several widely used Mahalanobismetric learning algorithms, at considerably lower computational cost. C1 CALTECH, Jet Prop Lab, NASA, Machine Learning & Instrument Auton Grp, Pasadena, CA 91101 USA. RP Bue, BD (reprint author), CALTECH, Jet Prop Lab, NASA, Machine Learning & Instrument Auton Grp, Pasadena, CA 91101 USA. EM bbue@jpl.nasa.gov NR 32 TC 5 Z9 5 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD APR PY 2014 VL 7 IS 4 BP 1079 EP 1088 DI 10.1109/JSTARS.2014.2302002 PG 10 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA AG4LB UT WOS:000335390000008 ER PT J AU Cardoso, AS Chakraborty, PS Lourenco, NE England, TD Saha, P Howard, DC Fleischhauer, DM Warner, JH McMorrow, D Buchner, SP Paki-Amouzou, P Thrivikraman, TK Cressler, JD AF Cardoso, Adilson S. Chakraborty, Partha S. Lourenco, Nelson E. England, Troy D. Saha, Prabir Howard, Duane C. Fleischhauer, David M. Warner, Jeffrey H. McMorrow, Dale Buchner, Stephen P. Paki-Amouzou, Pauline Thrivikraman, Tushar K. Cressler, John D. TI Evaluating the Effects of Single Event Transients in FET-Based Single-Pole Double-Throw RF Switches SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE Bulk FET; low insertion loss switch; radiation; RF switch; SiGe Bi CMOS; single event transient (SET); single-pole double-throw (SPDT); SOI ID LOW-NOISE AMPLIFIER; 130 NM CMOS; TECHNOLOGY; MITIGATION; DEVICES AB The impact of single event transients (SETs) on single-pole double-throw (SPDT) RF switch circuits designed in a commercially-available, 180 nm second-generation SiGe BiCMOS (IBM 7HP) technology is investigated. The intended application for these SPDT RF switches requires a 1 GHz to 20 GHz band of operation, relatively low insertion loss (< 3.0 dB at 20 GHz), and moderate isolation (> 15 dB at 20 GHz). Two-photon absorption experiment results reveal that the SPDT switches are vulnerable to SETs due to biasing effects as well as the triple-well (TW) nFETs, which are found to be more sensitive to SETs than bulk nFETs. From these results, potential implications are discussed and mitigation strategies are proposed. To verify one of the proposed mitigation techniques, SPDT switches were also designed in a 180 nm twin-well SOI CMOS (IBM 7RF-SOI) technology. A different biasing technique is implemented to help improve the SET response. The fabricated SOI SPDT switches achieve an insertion loss of < 1.04 dB at 20 GHz and > 21 dB isolation at 20 GHz. For this circuit, no transients were observed even at very high laser energies (approximate to 5 nJ). C1 [Cardoso, Adilson S.; Chakraborty, Partha S.; Lourenco, Nelson E.; England, Troy D.; Saha, Prabir; Howard, Duane C.; Fleischhauer, David M.; Cressler, John D.] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. [Warner, Jeffrey H.; McMorrow, Dale; Buchner, Stephen P.] Naval Res Lab, Washington, DC 20375 USA. [Paki-Amouzou, Pauline] Def Threat Reduct Agcy, Ft Belvoir, VA 22060 USA. [Thrivikraman, Tushar K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cardoso, AS (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. EM cardosoa@gatech.edu RI Chakraborty, Partha/K-6963-2014 FU Defense Threat Reduction Agency [HDTRA1-09-C-0031]; SPAWAR; NASA-NEPP FX This work was supported in part by the Defense Threat Reduction Agency under HDTRA1-09-C-0031, in part by SPAWAR, and in part by NASA-NEPP. NR 23 TC 4 Z9 4 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD APR PY 2014 VL 61 IS 2 BP 756 EP 765 DI 10.1109/TNS.2014.2301448 PG 10 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA AF7YI UT WOS:000334931100008 ER PT J AU Prieskorn, ZR Hill, JE Kaaret, PE Black, JK AF Prieskorn, Z. R. Hill, J. E. Kaaret, P. E. Black, J. K. TI Photoelectron Track Length Distributions Measured in a Negative Ion Time Projection Chamber SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE Negative ion time projection chamber; nitromethane; photoelectron track length; X-ray detectors; CH3NO2 ID GAS PROPORTIONAL COUNTER; RESOLUTION; RANGE AB We report photoelectron track length distributions between 3 and 8 keV in gas mixtures of Ne + CO2 + CH3NO2 (260: 80: 10 Torr) and CO2 + CH3NO2 (197.5: 15 Torr). The measurements were made using a negative ion time projection chamber (NITPC) at the National Synchrotron Light Source (NSLS) at the Brookhaven National Laboratory (BNL). We report the first quantitative analysis of photoelectron track length distributions in a gas. The distribution of track lengths at a given energy is best fit by a lognormal distribution. A powerlaw distribution of the form, f(E) = a(E/E-o)(n) is found to fit the relationship between mean track length and energy. We find n = 1.20 +/- 0.07 for Ne + CO2 + CH3NO2 and n = 1.20 +/-0.09 for CO2 + CH3NO2. Understanding the distribution of photoelectron track lengths in proportional counter gases is important for optimizing the pixel size and the dimensions of the active region in electron-drift time projection chambers (TPCs) and NITPC X-ray polarimeters. C1 [Prieskorn, Z. R.] Penn State Univ, University Pk, PA 16802 USA. [Hill, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kaaret, P. E.] Univ Iowa, Iowa City, IA 52240 USA. [Black, J. K.] Rock Creek Sci, Silver Spring, MD 20910 USA. RP Prieskorn, ZR (reprint author), Penn State Univ, University Pk, PA 16802 USA. EM prieskorn@psu.edu; joanne.e.hill@nasa.gov; Philip-kaaret@uiowa.edu; kevin.black@nasa.gov FU NASA Goddard Space Flight Center [NNX08AF46G] FX This work was funded under NASA grant NNX08AF46G at the NASA Goddard Space Flight Center. Beamline X19 A at the Brookhaven National Laboratory National Synchrotron Light Source was utilized to make the measurements presented in this experiment. The authors would like to thank Syed Khalid for his help at BNL. We would also like to thank Israel Moya, Christian Urba, Richard Koenecke and Tracy L Pluchak-Rosnak for their expert technical contributions to the project. NR 24 TC 0 Z9 0 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD APR PY 2014 VL 61 IS 2 BP 894 EP 900 DI 10.1109/TNS.2014.2312107 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA AF7YI UT WOS:000334931100024 ER PT J AU Clements, DL Braglia, FG Hyde, AK Perez-Fournon, I Bock, J Cava, A Chapman, S Conley, A Cooray, A Farrah, D Solares, EAG Marchetti, L Marsden, G Oliver, SJ Roseboom, IG Schulz, B Smith, AJ Vaccari, M Vieira, J Viero, M Wang, L Wardlow, J Zemcov, M de Zotti, G AF Clements, D. L. Braglia, F. G. Hyde, A. K. Perez-Fournon, I. Bock, J. Cava, A. Chapman, S. Conley, A. Cooray, A. Farrah, D. Solares, E. A. Gonzalez Marchetti, L. Marsden, G. Oliver, S. J. Roseboom, I. G. Schulz, B. Smith, A. J. Vaccari, M. Vieira, J. Viero, M. Wang, L. Wardlow, J. Zemcov, M. de Zotti, G. TI Herschel Multitiered Extragalactic Survey: clusters of dusty galaxies uncovered by Herschel and Planck SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: high redshift; galaxies: starburst; submillimetre: galaxies ID WIDE-FIELD SURVEY; DEEP SUBMILLIMETER SURVEY; IN-FLIGHT PERFORMANCE; IRAC SHALLOW SURVEY; SIMILAR-TO 1; STAR-FORMATION; PHOTOMETRIC REDSHIFTS; INFRARED GALAXIES; SPIRE INSTRUMENT; SPACE-TELESCOPE AB The potential for Planck to detect clusters of dusty, star-forming galaxies at z > 1 is tested by examining the Herschel-SPIRE images of Planck Early Release Compact Source Catalog sources lying in fields observed by the Herschel Multitiered Extragalactic Survey. Of the 16 Planck sources that lie in the similar to 90 sq. deg. examined, we find that 12 are associated with single bright Herschel sources. The remaining four are associated with overdensities of Herschel sources, making them candidate clusters of dusty, star-forming galaxies. We use complementary optical/near-IR data for these 'clumps' to test this idea, and find evidence for the presence of galaxy clusters in all four cases. We use photometric redshifts and red sequence galaxies to estimate the redshifts of these clusters, finding that they range from 0.8 to 2.3. These redshifts imply that the Herschel sources in these clusters, which contribute to the detected Planck flux, are forming stars very rapidly, with typical total cluster star formation rates > 1000 M-circle dot yr(-1). The high-redshift clusters discovered in these observations are used to constrain the epoch of cluster galaxy formation, finding that the galaxies in our clusters are 1-1.5 Gyr old at z similar to 1-2. Prospects for the discovery of further clusters of dusty galaxies are discussed, using not only all sky Planck surveys, but also deeper, smaller area, Herschel surveys. C1 [Clements, D. L.; Braglia, F. G.; Hyde, A. K.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Perez-Fournon, I.] IAC, E-38200 Tenerife, Spain. [Perez-Fournon, I.] ULL, Dept Astrofis, E-38205 Tenerife, Spain. [Bock, J.; Cooray, A.; Schulz, B.; Vieira, J.; Viero, M.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cava, A.] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain. [Cava, A.] Univ Geneva, Observ Geneve, CH-1290 Versoix, Switzerland. [Chapman, S.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA. [Cooray, A.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Solares, E. A. Gonzalez] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Marchetti, L.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Marchetti, L.] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy. [Marsden, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Oliver, S. J.; Roseboom, I. G.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Astron Ctr, Brighton BN1 9QH, E Sussex, England. [Roseboom, I. G.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Schulz, B.] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa. [de Zotti, G.] INAF OAPd, I-35122 Padua, Italy. [de Zotti, G.] SISSA, I-34136 Trieste, Italy. RP Clements, DL (reprint author), Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England. EM d.clements@imperial.ac.uk RI Wardlow, Julie/C-9903-2015; Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017; OI Wardlow, Julie/0000-0003-2376-8971; Vaccari, Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275; De Zotti, Gianfranco/0000-0003-2868-2595; Marchetti, Lucia/0000-0003-3948-7621 FU CSA (Canada); NAOC (China); CEA, (France); CNES, (France); CNRS, (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, (UK); UKSA (UK); NASA (USA); ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI, (Italy); CNR, (Italy); INAF (Italy); DoE (USA); STFC (UK); CSIC (Spain); MICINN (Spain); JA (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ESA (France); CNR (Italy); PRACE (EU); UK STFC; UKSA; Science and Technology Facilities Council [ST/I000976/1]; ASI/INAF [I/072/09/0]; Italian Space Agency (ASI Herschel Science Contract) [I/005/07/0] FX SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). The development of Planck has been supported by ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal). The development of Planck has been supported by ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). The data presented in this paper will be released through the Herschel Database in Marseille HeDaM (hedam.oamp.fr/HerMES). The authors would like to thank Mattia Negrello for the provision of Fig. 14. This work is funded in part by the UK STFC and UKSA. SJO, LW and AS acknowledge support from the Science and Technology Facilities Council [grant number ST/I000976/1], GdZ acknowledges financial support by ASI/INAF agreement I/072/09/0. Lucia Marchetti, and Mattia Vaccari were supported by the Italian Space Agency (ASI Herschel Science Contract I/005/07/0). NR 75 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 APR PY 2014 VL 439 IS 2 BP 1193 EP 1211 DI 10.1093/mnras/stt2253 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6OS UT WOS:000334114000001 ER PT J AU Matsuura, M Bernard-Salas, J Evans, TL Volk, KM Hrivnak, BJ Sloan, GC Chu, YH Gruendl, R Kraemer, KE Peeters, E Szczerba, R Wood, PR Zijlstra, AA Hony, S Ita, Y Kamath, D Lagadec, E Parker, QA Reid, WA Shimonishi, T Van Winckel, H Woods, PM Kemper, F Meixner, M Otsuka, M Sahai, R Sargent, BA Hora, JL McDonald, I AF Matsuura, Mikako Bernard-Salas, Jeronimo Evans, T. Lloyd Volk, Kevin M. Hrivnak, Bruce J. Sloan, G. C. Chu, You-Hua Gruendl, Robert Kraemer, Kathleen E. Peeters, Els Szczerba, R. Wood, P. R. Zijlstra, Albert A. Hony, S. Ita, Yoshifusa Kamath, Devika Lagadec, Eric Parker, Quentin A. Reid, Warren A. Shimonishi, Takashi Van Winckel, H. Woods, Paul M. Kemper, F. Meixner, Margaret Otsuka, M. Sahai, R. Sargent, B. A. Hora, J. L. McDonald, Iain TI Spitzer Space Telescope spectra of post-AGB stars in the Large Magellanic Cloud - polycyclic aromatic hydrocarbons at low metallicities SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: AGB and post-AGB; circumstellar matter; galaxies: individual: Large Magellanic Cloud; infrared: stars ID R-CORONAE-BOREALIS; YOUNG STELLAR OBJECTS; 21 MU-M; RICH PROTOPLANETARY NEBULAE; ASYMPTOTIC GIANT BRANCH; LONG-PERIOD VARIABLES; EXTREME CARBON STARS; WOLF-RAYET STARS; INFRARED-EMISSION BANDS; LUMINOUS BLUE VARIABLES AB This paper reports variations of polycyclic aromatic hydrocarbons (PAHs) features that were found in Spitzer Space Telescope spectra of carbon-rich post-asymptotic giant branch (post-AGB) stars in the Large Magellanic Cloud (LMC). The paper consists of two parts. The first part describes our Spitzer spectral observing programme of 24 stars including post-AGB candidates. The latter half of this paper presents the analysis of PAH features in 20 carbon-rich post-AGB stars in the LMC, assembled from the Spitzer archive as well as from our own programme. We found that five post-AGB stars showed a broad feature with a peak at 7.7 mu m, that had not been classified before. Further, the 10-13 mu m PAH spectra were classified into four classes, one of which has three broad peaks at 11.3, 12.3 and 13.3 mu m rather than two distinct sharp peaks at 11.3 and 12.7 mu m, as commonly found in H ii regions. Our studies suggest that PAHs are gradually processed while the central stars evolve from post-AGB phase to planetary nebulae, changing their composition before PAHs are incorporated into the interstellar medium. Although some metallicity dependence of PAH spectra exists, the evolutionary state of an object is more significant than its metallicity in determining the spectral characteristics of PAHs for LMC and Galactic post-AGB stars. C1 [Matsuura, Mikako; Woods, Paul M.] Univ London Univ Coll, Dept Phys & Astron, London WC1E 6BT, England. [Bernard-Salas, Jeronimo] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Bernard-Salas, Jeronimo] Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France. [Evans, T. Lloyd] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Volk, Kevin M.; Meixner, Margaret] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Hrivnak, Bruce J.] Valparaiso Univ, Dept Phys & Astron, Valparaiso, IN 46383 USA. [Sloan, G. C.; Lagadec, Eric] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Chu, You-Hua; Gruendl, Robert] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Kraemer, Kathleen E.] Boston Coll, Inst Sci Res, Newton, MA 02459 USA. [Peeters, Els] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Peeters, Els] SETI Inst, Mountain View, CA 94043 USA. [Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Wood, P. R.; Kamath, Devika] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Zijlstra, Albert A.; McDonald, Iain] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Hony, S.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Ita, Yoshifusa] Tohoku Univ, Grad Sch Sci, Astron Inst, Sendai, Miyagi 9808578, Japan. [Parker, Quentin A.; Reid, Warren A.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia. [Parker, Quentin A.] Macquarie Univ, Res Ctr Astron Astrophys & Astrophoton MQAAAstro, N Ryde, NSW 2109, Australia. [Parker, Quentin A.] Australian Astron Observ, Epping, NSW 2121, Australia. [Shimonishi, Takashi] Kobe Univ, Grad Sch Sci, Dept Earth & Planetary Sci, Nada Kobe 6578501, Japan. [Van Winckel, H.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Woods, Paul M.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Kemper, F.; Otsuka, M.] AS NTU, Acad Sin, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sargent, B. A.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. [Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Matsuura, M (reprint author), Univ London Univ Coll, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM mikako@star.ucl.ac.uk RI Kemper, Francisca/D-8688-2011; Woods, Paul/E-6926-2011; OI Kemper, Francisca/0000-0003-2743-8240; Woods, Paul/0000-0003-4340-3590; Hora, Joseph/0000-0002-5599-4650; Kraemer, Kathleen/0000-0002-2626-7155; Van Winckel, Hans/0000-0001-5158-9327 FU NASA [1378453]; National Aeronautics and Space Administration; National Science Foundation; Marie Curie Actions IRSES of EU [269193]; Polish NCN [2011/01/B/ST9/02031]; National Science Council [NSC100-2112-M-001-023-MY3]; NASA; Spitzer Guest Observer programme FX MM thanks Professor I. D. Howarth for his inputs about the classifications of high-mass stars. We thank Dr J. P. Searle for providing the Herschel measurements of IRAS 05189-7008 fluxes. Support for this research was provided by NASA through contract 1378453 issued by JPL/Caltech. 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 research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France. RSz acknowledges support from Marie Curie Actions IRSES (project No. 269193) of EU and from Polish NCN grant 2011/01/B/ST9/02031. FK acknowledges financial support from the National Science Council under grant number NSC100-2112-M-001-023-MY3. RS'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 JPL/Caltech in support of his Spitzer Guest Observer programme. NR 135 TC 13 Z9 13 U1 2 U2 9 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 APR PY 2014 VL 439 IS 2 BP 1472 EP 1493 DI 10.1093/mnras/stt2495 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6OS UT WOS:000334114000016 ER PT J AU Marsden, D Gralla, M Marriage, TA Switzer, ER Partridge, B Massardi, M Morales, G Addison, G Bond, JR Crichton, D Das, S Devlin, M Dunner, R Hajian, A Hilton, M Hincks, A Hughes, JP Irwin, K Kosowsky, A Menanteau, F Moodley, K Niemack, M Page, L Reese, ED Schmitt, B Sehgal, N Sievers, J Staggs, S Swetz, D Thornton, R Wollack, E AF Marsden, Danica Gralla, Megan Marriage, Tobias A. Switzer, Eric R. Partridge, Bruce Massardi, Marcella Morales, Gustavo Addison, Graeme Bond, J. Richard Crichton, Devin Das, Sudeep Devlin, Mark Duenner, Rolando Hajian, Amir Hilton, Matt Hincks, Adam Hughes, John P. Irwin, Kent Kosowsky, Arthur Menanteau, Felipe Moodley, Kavilan Niemack, Michael Page, Lyman Reese, Erik D. Schmitt, Benjamin Sehgal, Neelima Sievers, Jonathan Staggs, Suzanne Swetz, Daniel Thornton, Robert Wollack, Edward TI The Atacama Cosmology Telescope: dusty star-forming galaxies and active galactic nuclei in the Southern survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; surveys; galaxies: active; galaxies: high-redshift ID COEVAL OBSERVATIONS PROJECT; CLERK MAXWELL TELESCOPE; SOURCE CATALOG; EXTRAGALACTIC SOURCES; POLE TELESCOPE; BOLOMETER CAMERA; BLAZAR SEQUENCE; NUMBER COUNTS; BRIGHTNESS TEMPERATURES; REDSHIFT DISTRIBUTION AB We present a catalogue of 191 extragalactic sources detected by the Atacama Cosmology Telescope (ACT) at 148 and/or 218 GHz in the 2008 Southern survey. Flux densities span 14 -1700 mJy, and we use source spectral indices derived using ACT-only data to divide our sources into two subpopulations: 167 radio galaxies powered by central active galactic nuclei (AGN) and 24 dusty star-forming galaxies (DSFGs). We cross-identify 97 per cent of our sources (166 of the AGN and 19 of the DSFGs) with those in currently available catalogues. When combined with flux densities from the Australia Telescope 20 GHz survey and follow-up observations with the Australia Telescope Compact Array, the synchrotron-dominated population is seen to exhibit a steepening of the slope of the spectral energy distribution from 20 to 148 GHz, with the trend continuing to 218 GHz. The ACT dust-dominated source population has a median spectral index, alpha(148-218), of 3.7(-0.86)(+0.62), and includes both local galaxies and sources with redshift around 6. Dusty sources with no counterpart in existing catalogues likely belong to a recently discovered subpopulation of DSFGs lensed by foreground galaxies or galaxy groups. C1 [Marsden, Danica] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Marsden, Danica; Devlin, Mark; Reese, Erik D.; Schmitt, Benjamin] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Gralla, Megan; Marriage, Tobias A.; Crichton, Devin] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Switzer, Eric R.; Wollack, Edward] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Massardi, Marcella] Astron Observ Padova, INAF, I-35122 Padua, Italy. [Morales, Gustavo; Duenner, Rolando] Pontificia Univ Catolica Chile, Fac Fis, Dept Astronomia & Astrofis, Santiago 22, Chile. [Addison, Graeme] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T IZ4, Canada. [Bond, J. Richard; Hajian, Amir; Hincks, Adam; Sievers, Jonathan] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA. [Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA. [Hilton, Matt; Moodley, Kavilan; Sievers, Jonathan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Hughes, John P.; Menanteau, Felipe] State Univ New Jersey, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Irwin, Kent; Swetz, Daniel] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Niemack, Michael] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Page, Lyman; Sievers, Jonathan; Staggs, Suzanne] Princeton Univ, Jadwin Hall, Princeton, NJ 08544 USA. [Sehgal, Neelima] SUNY Stony Brook, Phys & Astron Dept, Stony Brook, NY 11794 USA. [Thornton, Robert] West Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA. RP Marsden, D (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM danica@physics.ucsb.edu RI Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Menanteau, Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074 FU US National Science Foundation [AST-0408698, AST-0965625]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation (CFI); NSF Physics Frontier Center [PHY-0114422]; SciNet; Canada Foundation for Innovation (CFI) under the Compute Canada; Government of Ontario; Ontario Research Fund Research Excellence; University of Toronto; Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT); Commonwealth of Australia; National Aeronautics and Space Administration; [PHY-0355328]; [PHY-0855887]; [PHY-1214379]; [AST-0707731]; [PIRE-0507768]; [OISE-0530095] FX This work was supported by the US National Science Foundation through awards AST-0408698 and AST-0965625 for the ACT project, and PHY-0355328, PHY-0855887, PHY-1214379, AST-0707731 and PIRE-0507768 (award number OISE-0530095). Funding was also provided by Princeton University, the University of Pennsylvania and a Canada Foundation for Innovation (CFI) award to UBC. ES acknowledges support by NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics. The PIRE programme enabled this research through exchanges between Chile, South Africa, Spain and the US. Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by SciNet is funded by the Canada Foundation for Innovation (CFI) under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund Research Excellence and the University of Toronto. Data acquisition electronics were developed with assistance from the CFI. ACT operates in the Parque Astronmico Atacama in northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT).; We thank the staff at the Australia Telescope Compact Array site, Narrabri (NSW), for the valuable support they provide in running the telescope. ATCA is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO.; This research made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 80 TC 11 Z9 11 U1 0 U2 8 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 APR PY 2014 VL 439 IS 2 BP 1556 EP 1574 DI 10.1093/mnras/stu001 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6OS UT WOS:000334114000021 ER PT J AU Ng, C Bailes, M Bates, SD Bhat, NDR Burgay, M Burke-Spolaor, S Champion, DJ Coster, P Johnston, S Keith, MJ Kramer, M Levin, L Petroff, E Possenti, A Stappers, BW van Straten, W Thornton, D Tiburzi, C Bassa, CG Freire, PCC Guillemot, L Lyne, AG Tauris, TM Shannon, RM Wex, N AF Ng, C. Bailes, M. Bates, S. D. Bhat, N. D. R. Burgay, M. Burke-Spolaor, S. Champion, D. J. Coster, P. Johnston, S. Keith, M. J. Kramer, M. Levin, L. Petroff, E. Possenti, A. Stappers, B. W. van Straten, W. Thornton, D. Tiburzi, C. Bassa, C. G. Freire, P. C. C. Guillemot, L. Lyne, A. G. Tauris, T. M. Shannon, R. M. Wex, N. TI The High Time Resolution Universe pulsar survey - X. Discovery of four millisecond pulsars and updated timing solutions of a further 12 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: neutron; pulsars: general; pulsars: individual: PSR J1017-7156; pulsars: individual: PSR J1543-5149; pulsars: individual: PSR J1801-3210; pulsars: individual: PSR J1811-2405 ID LARGE-AREA TELESCOPE; GAMMA-RAY PULSARS; BINARY PULSARS; NEUTRON-STAR; GRAVITATIONAL-RADIATION; EQUIVALENCE PRINCIPLES; GALACTIC DISTRIBUTION; INITIAL DISCOVERIES; RADIO-EMISSION; FREE-ELECTRONS AB We report on the discovery of four millisecond pulsars (MSPs) in the High Time Resolution Universe (HTRU) pulsar survey being conducted at the Parkes 64 m radio telescope. All four MSPs are in binary systems and are likely to have white dwarf companions. In addition, we present updated timing solutions for 12 previously published HTRU MSPs, revealing new observational parameters such as five proper motion measurements and significant temporal dispersion measure variations in PSR J1017-7156. We discuss the case of PSR J1801-3210, which shows no significant period derivative P after four years of timing data. Our best-fitting solution shows a P of the order of 10(-23), an extremely small number compared to that of a typical MSP. However, it is likely that the pulsar lies beyond the Galactic Centre, and an unremarkable intrinsic P is reduced to close to zero by the Galactic potential acceleration. Furthermore, we highlight the potential to employ PSR J1801-3210 in the strong equivalence principle test due to its wide and circular orbit. In a broader comparison with the known MSP population, we suggest a correlation between higher mass functions and the presence of eclipses in 'very low mass binary pulsars', implying that eclipses are observed in systems with high orbital inclinations. We also suggest that the distribution of the total mass of binary systems is inversely related to the Galactic height distribution. Finally, we report on the first detection of PSRs J1543-5149 and J1811-2404 as gamma-ray pulsars. C1 [Ng, C.; Champion, D. J.; Kramer, M.; Freire, P. C. C.; Guillemot, L.; Tauris, T. M.; Wex, N.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Bailes, M.; Bhat, N. D. R.; Coster, P.; Petroff, E.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Bailes, M.; Bhat, N. D. R.; Petroff, E.; van Straten, W.] Swinburne Univ Technol, ARC Ctr Excellence All Sky Astrophys CAASTRO, Hawthorn, Vic 3122, Australia. [Bates, S. D.; Levin, L.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Bhat, N. D. R.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Burgay, M.; Possenti, A.; Tiburzi, C.] Osservatorio Astron Cagliari, I-09012 Capoterra, CA, Italy. [Burke-Spolaor, S.] NASA Jet Prop Lab, Pasadena, CA 91106 USA. [Coster, P.; Johnston, S.; Keith, M. J.; Petroff, E.; Thornton, D.; Shannon, R. M.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Kramer, M.; Stappers, B. W.; Thornton, D.; Bassa, C. G.; Lyne, A. G.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Tiburzi, C.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, CA, Italy. [Guillemot, L.] Univ Orleans, CNRS, Lab Phys & Chim Environm & Espace, F-45071 Orleans 02, France. [Tauris, T. M.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. RP Ng, C (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM cherryng@mpifr-bonn.mpg.de OI Champion, David/0000-0003-1361-7723; Shannon, Ryan/0000-0002-7285-6348; Burgay, Marta/0000-0002-8265-4344; van Straten, Willem/0000-0003-2519-7375 FU Commonwealth of Australia; Parkes Pulsar Timing Array Project [P456]; International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne 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. A large amount of the timing data for PSR J1017-7156 has been taken as part of the Parkes Pulsar Timing Array Project P456.; The authors would like to thank Patrick Lazarus for providing an automated RFI cleaning routine, Dominic Schnitzeler for useful discussions on pulsar distances, Joris Verbiest for his expertise on the use of TEMPO2, Charlotte Sobey and Gregory Desvignes for advices on data calibration, Kejia Lee for his help in plotting Fig. 7, Chris Flynn for sharing his knowledge on Galactic stellar density, Megan DeCesar from the Fermi collaboration for reviewing the paper and providing many constructive suggestions, and Lijing Shao for carefully reading the manuscripts. CN was supported for this research through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. NR 86 TC 18 Z9 19 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 APR PY 2014 VL 439 IS 2 BP 1865 EP 1883 DI 10.1093/mnras/stu067 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6OS UT WOS:000334114000038 ER PT J AU Delvecchio, I Gruppioni, C Pozzi, F Berta, S Zamorani, G Cimatti, A Lutz, D Scott, D Vignali, C Cresci, G Feltre, A Cooray, A Vaccari, M Fritz, J Le Floc'h, E Magnelli, B Popesso, P Oliver, S Bock, J Carollo, M Contini, T Le Fevre, O Lilly, S Mainieri, V Renzini, A Scodeggio, M AF Delvecchio, I. Gruppioni, C. Pozzi, F. Berta, S. Zamorani, G. Cimatti, A. Lutz, D. Scott, D. Vignali, C. Cresci, G. Feltre, A. Cooray, A. Vaccari, M. Fritz, J. Le Floc'h, E. Magnelli, B. Popesso, P. Oliver, S. Bock, J. Carollo, M. Contini, T. Le Fevre, O. Lilly, S. Mainieri, V. Renzini, A. Scodeggio, M. TI Tracing the cosmic growth of supermassive black holes to z similar to 3 with Herschel(star) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: nuclei; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; DEEP-FIELD-SOUTH; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMATION HISTORY; ULTRALUMINOUS INFRARED GALAXIES; RAY LUMINOSITY FUNCTION; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; X-RAY; XMM-NEWTON AB We study a sample of Herschel selected galaxies within the Great Observatories Origins Deep Survey-South and the Cosmic Evolution Survey fields in the framework of the Photodetector Array Camera and Spectrometer (PACS) Evolutionary Probe project. Starting from the rich multiwavelength photometric data sets available in both fields, we perform a broad-band spectral energy distribution decomposition to disentangle the possible active galactic nucleus (AGN) contribution from that related to the host galaxy. We find that 37 per cent of the Herschel-selected sample shows signatures of nuclear activity at the 99 per cent confidence level. The probability of revealing AGN activity increases for bright (L1-1000 > 10(11) L-circle dot) star-forming galaxies at z > 0.3, becoming about 80 per cent for the brightest (L1-1000 > 10(12) L-circle dot) infrared (IR) galaxies at z >= 1. Finally, we reconstruct the AGN bolometric luminosity function and the supermassive black hole growth rate across cosmic time up to z similar to 3 from a far-IR perspective. This work shows general agreement with most of the panchromatic estimates from the literature, with the global black hole growth peaking at z similar to 2 and reproducing the observed local black hole mass density with consistent values of the radiative efficiency epsilon(rad) (similar to 0.07). C1 [Delvecchio, I.; Pozzi, F.; Cimatti, A.; Vignali, C.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Gruppioni, C.; Zamorani, G.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Berta, S.; Lutz, D.; Popesso, P.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Cresci, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Feltre, A.] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy. [Feltre, A.; Mainieri, V.] ESO, D-85748 Garching, Germany. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Cooray, A.; Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa. [Fritz, J.] Vakgrp Fys Sterrenkunde Univ, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Le Floc'h, E.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Magnelli, B.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Oliver, S.] Univ Sussex, Dept Phys & Astron, Astron Ctr, Brighton BN1 9QH, E Sussex, England. [Bock, J.] CALTECH, Pasadena, CA 91125 USA. [Carollo, M.; Lilly, S.] ETH Honggerberg, Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Contini, T.] Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France. [Le Fevre, O.] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Renzini, A.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Scodeggio, M.] INAF IASF Milano, I-20133 Milan, Italy. RP Delvecchio, I (reprint author), Univ Bologna, Dipartimento Fis & Astron, Via Ranzani 1, I-40127 Bologna, Italy. EM ivan.delvecchio@unibo.it RI Vignali, Cristian/J-4974-2012; Vaccari, Mattia/R-3431-2016; OI Cresci, Giovanni/0000-0002-5281-1417; Vignali, Cristian/0000-0002-8853-9611; Vaccari, Mattia/0000-0002-6748-0577; Scodeggio, Marco/0000-0002-2282-5850; Gruppioni, Carlotta/0000-0002-5836-4056; Scott, Douglas/0000-0002-6878-9840; Zamorani, Giovanni/0000-0002-2318-301X; Delvecchio, Ivan/0000-0001-8706-2252 FU 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) FX This paper uses data from Herschel's photometers PACS and SPIRE. 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) and 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 Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM(France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). NR 193 TC 34 Z9 33 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2014 VL 439 IS 3 BP 2736 EP 2754 DI 10.1093/mnras/stu130 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PB UT WOS:000334114900038 ER PT J AU Szypryt, P Duggan, GE Mazin, BA Meeker, SR Strader, MJ van Eyken, JC Marsden, D O'Brien, K Walter, AB Ulbricht, G Prince, TA Stoughton, C Bumble, B AF Szypryt, P. Duggan, G. E. Mazin, B. A. Meeker, S. R. Strader, M. J. van Eyken, J. C. Marsden, D. O'Brien, K. Walter, A. B. Ulbricht, G. Prince, T. A. Stoughton, C. Bumble, B. TI Direct detection of SDSS J0926+3624 orbital expansion with ARCONS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: close; binaries: eclipsing; stars: individual: SDSS J0926+3624; cataclysmic variables; white dwarfs ID AM CVN STARS; CATACLYSMIC VARIABLES; BINARIES AB AM Canum Venaticorum (AM CVn) stars belong to a class of ultracompact, short-period binaries with spectra dominated largely by helium. SDSS J0926+3624 is of particular interest as it is the first observed eclipsing AM CVn system. We observed SDSS J0926+3624 with the Array Camera for Optical to Near-IR Spectrophotometry (ARCONS) at the Palomar 200 ' telescope. ARCONS uses a relatively new type of energy-resolved photon counters called Microwave Kinetic Inductance Detectors. ARCONS, sensitive to radiation from 350 to 1100 nm, has a time resolution of several microseconds and can measure the energy of a photon to similar to 10 per cent. We present the light curves for these observations and examine changes in orbital period from prior observations. Using a quadratic ephemeris model, we measure a period rate of change P = (3.07 +/- 0.56) x 10(-13). In addition, we use the high timing resolution of ARCONS to examine the system's high-frequency variations and search for possible quasi-periodic oscillations (QPOs). Finally, we use the instrument's spectral resolution to examine the light curves in various wavelength bands. We do not find any high-frequency QPOs or significant spectral variability throughout an eclipse. C1 [Szypryt, P.; Duggan, G. E.; Mazin, B. A.; Meeker, S. R.; Strader, M. J.; van Eyken, J. C.; Marsden, D.; Walter, A. B.; Ulbricht, G.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Duggan, G. E.; Prince, T. A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [O'Brien, K.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Stoughton, C.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Bumble, B.] NASA, Jet Prop Lab, Pasadena, CA 91125 USA. RP Szypryt, P (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM pszypryt@physics.ucsb.edu RI Mazin, Ben/B-8704-2011; Ulbricht, Gerhard/P-7487-2016 OI Mazin, Ben/0000-0003-0526-1114; Ulbricht, Gerhard/0000-0002-6497-3763 FU NASA [NNX11AD55G, NNX10AF58G]; NASA Office of the Chief Technologist's Space Technology Research Fellowship, NASA [NNX11AN29H]; Keck Institute for Space Studies; Fermi Research Alliance, LLC [De-AC02-07CH11359] FX The MKID detectors used in this work were developed under NASA grant NNX11AD55G, and the readout was partially developed under NASA grant NNX10AF58G. SRM was supported by a NASA Office of the Chief Technologist's Space Technology Research Fellowship, NASA grant NNX11AN29H. This work was partially supported by the Keck Institute for Space Studies. Fermilab is operated by Fermi Research Alliance, LLC under Contract no. De-AC02-07CH11359 with the United States Department of Energy. The authors would like to thank Shri Kulkarni, Director of the Caltech Optical Observatories for facilitating this project, as well as the excellent staff of the Palomar Observatory. This project also greatly benefitted from the support of Mike Werner, Paul Goldsmith, and Jonas Zmuidzinas at JPL. NR 23 TC 6 Z9 6 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2014 VL 439 IS 3 BP 2765 EP 2770 DI 10.1093/mnras/stu137 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PB UT WOS:000334114900040 ER PT J AU Matt, G Marinucci, A Guainazzi, M Brenneman, LW Elvis, M Lohfink, A Arevalo, P Boggs, SE Cappi, M Christensen, FE Craig, WW Fabian, AC Fuerst, F Hailey, CJ Harrison, FA Parker, M Reynolds, CS Stern, D Walton, DJ Zhang, WW AF Matt, G. Marinucci, A. Guainazzi, M. Brenneman, L. W. Elvis, M. Lohfink, A. Arevalo, P. Boggs, S. E. Cappi, M. Christensen, F. E. Craig, W. W. Fabian, A. C. Fuerst, F. Hailey, C. J. Harrison, F. A. Parker, M. Reynolds, C. S. Stern, D. Walton, D. J. Zhang, W. W. TI The soft-X-ray emission of Ark 120. XMM-Newton, NuSTAR, and the importance of taking the broad view SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; galaxies: active; galaxies: individual: Ark 120 ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; LINE REGION SIZES; SUZAKU OBSERVATIONS; CENTRAL MASSES; SKY SURVEY; SPECTRA; EXCESS; PHOTOIONIZATION; SEYFERT-1 AB We present simultaneous XMM-Newton and NuSTAR observations of the 'bare' Seyfert 1 galaxy, Ark 120, a system in which ionized absorption is absent. The NuSTAR hard-X-ray spectral coverage allows us to constrain different models for the excess soft-X-ray emission. Among phenomenological models, a cutoff power law best explains the soft-X-ray emission. This model likely corresponds to Comptonization of the accretion disc seed UV photons by a population of warm electrons: using Comptonization models, a temperature of similar to 0.3 keV and an optical depth of similar to 13 are found. If the UV-to-X-ray optxagnf model is applied, the UV fluxes from the XMM-Newton Optical Monitor suggest an intermediate black hole spin. Contrary to several other sources observed by NuSTAR, no high-energy cutoff is detected with a lower limit of 190 keV. C1 [Matt, G.; Marinucci, A.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Guainazzi, M.] European Space Astron Ctr ESA, E-28080 Madrid, Spain. [Brenneman, L. W.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lohfink, A.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Arevalo, P.] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Santiago 22, Chile. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Cappi, M.] IASF Bologna, INAF, I-40129 Bologna, Italy. [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. [Fabian, A. C.; Parker, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Fuerst, F.; Harrison, F. A.; Walton, D. J.] 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. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Matt, G (reprint author), Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy. EM matt@fis.uniroma3.it RI Boggs, Steven/E-4170-2015; Cappi, Massimo/F-4813-2015; OI Boggs, Steven/0000-0001-9567-4224; Cappi, Massimo/0000-0001-6966-8920 FU National Aeronautics and Space Administration; ESA Member States; USA (NASA); Italian Space Agency under grant ASI/INAF [I/037/12/0-011/13]; European Union [312789] FX We thank the anonymous referee for useful comments which helped us to improve the clarity of the paper, and Chris Done for comments and advices on the OPTXAGNF model. This work has 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 NUSTARDAS jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The work is also 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). GM and AM 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. NR 32 TC 26 Z9 26 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2014 VL 439 IS 3 BP 3016 EP 3021 DI 10.1093/mnras/stu159 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PB UT WOS:000334114900063 ER PT J AU Maccarone, TJ Lehmer, BD Leyder, JC Antoniou, V Hornschemeier, A Ptak, A Wik, D Zezas, A AF Maccarone, Thomas J. Lehmer, Bret D. Leyder, J. C. Antoniou, Vallia Hornschemeier, Ann Ptak, Andrew Wik, Daniel Zezas, Andreas TI A new candidate Wolf-Rayet X-ray binary in NGC 253 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: Wolf-Rayet; galaxies: individual: NGC 253; galaxies: starburst; X-rays: binaries ID STAR-FORMATION HISTORY; DOUBLE BLACK-HOLE; GRAVITATIONAL-RADIATION; GLOBULAR-CLUSTER; IC-10 X-1; MASS; ACCRETION; EVOLUTION; GALAXIES; VARIABILITY AB We have discovered a persistent, but highly variable X-ray source in the nearby starburst galaxy NGC 253. The source varies at the level of a factor of about 5 in count rate on time-scales of a few hours. Two long observations of the source with Chandra and XMM-Newton show suggestive evidence for the source having a period of about 14-15 hours, but the time sampling in existing data is insufficient to allow a firm determination that the source is periodic. Given the amplitude of variation and the location in a nuclear starburst, the source is likely to be a Wolf-Rayet X-ray binary, with the tentative period being the orbital period of the system. In light of the fact that we have demonstrated that careful examination of the variability of moderately bright X-ray sources in nearby galaxies can turn up candidate Wolf-Rayet X-ray binaries, we discuss the implications of Wolf-Rayet X-ray binaries for predictions of the gravitational wave source event rate, and, potentially, interpretations of the events. C1 [Maccarone, Thomas J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Lehmer, Bret D.; Ptak, Andrew] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Lehmer, Bret D.; Leyder, J. C.; Hornschemeier, Ann; Ptak, Andrew; Wik, Daniel] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Leyder, J. C.] European Space Agcy, European Space Astron Ctr, E-28691 Madrid, Spain. [Antoniou, Vallia] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Antoniou, Vallia] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zezas, Andreas] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. RP Maccarone, TJ (reprint author), Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. EM thomas.maccarone@ttu.edu RI Zezas, Andreas/C-7543-2011; Antoniou, Vallia/E-3837-2013 OI Zezas, Andreas/0000-0001-8952-676X; Antoniou, Vallia/0000-0001-7539-1593 NR 60 TC 6 Z9 6 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 APR PY 2014 VL 439 IS 3 BP 3064 EP 3072 DI 10.1093/mnras/stu167 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PB UT WOS:000334114900068 ER PT J AU Wolters, SD Weissman, PR Christou, A Duddy, SR Lowry, SC AF Wolters, Stephen D. Weissman, Paul R. Christou, Apostolis Duddy, Samuel R. Lowry, Stephen C. TI Spectral similarity of unbound asteroid pairs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; minor planets, asteroids: general ID SPECTROSCOPIC SURVEY; PHASE-II; ORIGIN AB Infrared (IR) spectroscopy between 0.8 and 2.5 mu has been obtained for both components of three unbound asteroid pairs, using the NASA Infrared Telescope Facility with the SpeX instrument. Pair primary (2110) Moore-Sitterly is classified as an S-type following the Bus-DeMeo taxonomy; the classification for secondary (44612) 1999 RP27 is ambiguous: S/Sq/Q/K/L-type. Primary (10484) Hecht and secondary (44645) 1999 RC118 are classified as V-types. IR spectra for Moore-Sitterly and Hecht are each linked with available visual photometry. The classifications for primary (88604) 2001 QH293 and (60546) 2000 EE85 are ambiguous: S/Sq/Q/K/L-type. Subtle spectral differences between them suggest that the primary may have more weathered material on its surface. Dynamical integrations have constrained the ages of formation: 2110-44612 > 782 kyr; 10484-44645 = 348 (+823,-225) kyr; 88604-60546 = 925 (+842,-754) kyr. The spectral similarity of seven complete pairs is ranked in comparison with nearby background asteroids. Two pairs, 17198-229056 and 19289-278067, have significantly different spectra between the components, compared to the similarity of spectra in the background population. The other pairs are closer than typical, supporting an interpretation of each pair's formation from a common parent body. C1 [Wolters, Stephen D.; Weissman, Paul R.] CALTECH, Planetary Sci Sect, Jet Prop Lab, Pasadena, CA 91109 USA. [Christou, Apostolis] Armagh Observ, Armagh BT61 9DG, North Ireland. [Duddy, Samuel R.; Lowry, Stephen C.] Univ Kent, Sch Phys Sci, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NH, Kent, England. RP Wolters, SD (reprint author), Open Univ, Walton Hall, Milton Keynes MK7 6AA, Bucks, England. EM s.d.wolters@open.ac.uk FU University of Hawaii [NNX-08AE38A]; National Aeronautics and Space Administration; Science Mission Directorate; NASA; National Science Foundation [0506716, 0907766]; NASA [NAG5-12355, 09-NEOO009-0001]; Northern Ireland Department of Culture, Arts and Leisure (DCAL); SFI/HEA Irish Centre for High-End Computing (ICHEC) FX Visiting Astronomer at the IRTF, which is operated by the University of Hawaii under Cooperative Agreement no. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. A part of this work was performed at the Jet Propulsion Laboratory under a contract with NASA. Taxonomic-type results presented in this work were determined, in part, using a Bus-DeMeo Taxonomy Classification Web tool by Stephen M. Slivan, developed at MIT with the support of National Science Foundation Grant 0506716 and NASA Grant NAG5-12355. Part of the data utilized in this publication were obtained and made available by the MIT-UH-IRTF Joint Campaign for NEO Reconnaissance. The MIT component of this work is supported by NASA grant 09-NEOO009-0001, and by the National Science Foundation under grants nos 0506716 and 0907766. Astronomical research at the Armagh Observatory is funded by the Northern Ireland Department of Culture, Arts and Leisure (DCAL). We thank an anonymous referee for many helpful comments that improved this manuscript. AC acknowledges the SFI/HEA Irish Centre for High-End Computing (ICHEC) for the provision of computational facilities and support. NR 26 TC 6 Z9 6 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 APR PY 2014 VL 439 IS 3 BP 3085 EP 3093 DI 10.1093/mnras/stu171 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PB UT WOS:000334114900070 ER PT J AU Fairen, AG Stokes, CR Davies, NS Schulze-Makuch, D Rodriguez, JAP Davila, AF Uceda, ER Dohm, JM Baker, VR Clifford, SM McKay, CP Squyres, SW AF Fairen, Alberto G. Stokes, Chris R. Davies, Neil S. Schulze-Makuch, Dirk Rodriguez, J. Alexis P. Davila, Alfonso F. Uceda, Esther R. Dohm, James M. Baker, Victor R. Clifford, Stephen M. Mckay, Christopher P. Squyres, Steven W. TI A cold hydrological system in Gale crater, Mars SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Mars; Gale crater; Glacial/periglacial modification; Glacio-fluvial activity; Fluvial erosion; Ground ice ID ART. NO. 5111; DICHOTOMY BOUNDARY; ROCK GLACIERS; VALLES MARINERIS; MELAS-CHASMA; EVOLUTION; ICE; ANTARCTICA; GLACIATION; DRUMLINS AB Gale crater is a similar to 154-km-diameter impact crater formed during the Late Noachian/Early Hesperian at the dichotomy boundary on Mars. Here we describe potential evidence for ancient glacial, periglacial and fluvial (including glacio-fluvial) activity within Gale crater, and the former presence of ground ice and lakes. Our interpretations are derived from morphological observations using high-resolution datasets, particularly HiRISE and HRSC. We highlight a potential ancient lobate rock-glacier complex in parts of the northern central mound, with further suggestions of glacial activity in the large valley systems towards the southeast central mound. Wide expanses of ancient ground ice may be indicated by evidence for very cohesive ancient river banks and for the polygonal patterned ground common on the crater floor west of the central mound. We extend the interpretation to fluvial and lacustrine activity to the west of the central mound, as recorded by a series of interconnected canyons, channels and a possible lake basin. The emerging picture from our regional landscape analyses is the hypothesis that rock glaciers may have formerly occupied the central mound. The glaciers would have provided the liquid water required for carving the canyons and channels. Associated glaciofluvial activity could have led to liquid water running over ground ice-rich areas on the basin floor, with resultant formation of partially and/or totally ice-covered lakes in parts of the western crater floor. All this hydrologic activity is Hesperian or younger. Following this, we envisage a time of drying, with the generation of polygonal patterned ground and dune development subsequent to the disappearance of the surface liquid and frozen water. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Fairen, Alberto G.; Squyres, Steven W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Fairen, Alberto G.] Ctr Astrobiol, Torrejon De Ardoz 28850, Spain. [Stokes, Chris R.] Univ Durham, Dept Geog, Durham DH1 3LE, England. [Davies, Neil S.] Univ Cambridge, Dept Earth Sci, Cambridge CB3 3EQ, England. [Schulze-Makuch, Dirk] Washington State Univ, Sch Environm, Pullman, WA 99164 USA. [Rodriguez, J. Alexis P.; Mckay, Christopher P.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Davila, Alfonso F.] SETI Inst, Mountain View, CA 94043 USA. [Uceda, Esther R.] Univ Autonoma Madrid, Fac Ciencias, E-28049 Madrid, Spain. [Dohm, James M.] Tokyo Inst Technol, Earth Life Sci Inst, Tokyo 1528551, Japan. [Dohm, James M.; Baker, Victor R.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Clifford, Stephen M.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Lunar & Planetary Inst, Houston, TX 77058 USA. RP Fairen, AG (reprint author), Cornell Univ, Dept Astron, 426 Space Sci Bldg, Ithaca, NY 14853 USA. EM agfairen@cornell.edu RI Stokes, Chris/A-1957-2011; Davila, Alfonso/A-2198-2013; OI Stokes, Chris/0000-0003-3355-1573; Davila, Alfonso/0000-0002-0977-9909; Schulze-Makuch, Dirk/0000-0002-1923-9746 FU European Research Council under the European Union's Seventh Framework Programme [307496]; Philip Leverhulme Prize FX The authors would like to thank the MRO HiRISE and CTX Teams, and the MEX HRSC Team, for their efforts in producing the excellent datasets and observations used here. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013), ERC Grant agreement no. 307496. C. R.S. acknowledges financial support provided by a Philip Leverhulme Prize. This is LPI Contribution 1778. NR 84 TC 15 Z9 15 U1 2 U2 19 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 APR PY 2014 VL 93-94 BP 101 EP 118 DI 10.1016/j.pss.2014.03.002 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG2WO UT WOS:000335278000011 ER PT J AU Lipatov, AS Sittler, EC Hartle, RE Cooper, JF Simpson, DG AF Lipatov, A. S. Sittler, E. C., Jr. Hartle, R. E. Cooper, J. F. Simpson, D. G. TI Titan's plasma environment: 3D hybrid kinetic modeling of the TA flyby and comparison with CAPS-ELS and RPWS LP observations SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Ionospheres; Atmospheres; Induced magnetospheres; Magnetic barrier; Alfven wing; Satellites; Pickup ion ID SOLAR-WIND; SATURNS MAGNETOSPHERE; MHD MODEL; IONOSPHERE; SIMULATION; SPECTROMETER; T9; ENCOUNTER; VOYAGER-1; EXOSPHERE AB In this report we discuss the global plasma environment of the TA flyby from the perspective of 3D hybrid modeling. In our model the background, pickup, and ionospheric ions are considered as particles, whereas the electrons are described as a fluid. Inhomogeneous photoionization, electron-impact ionization and charge exchange are included in our model. We also take into account the collisions between the ions and neutrals. Our modeling shows that mass loading of the background plasma (H+, O+) by pickup ions H-2(+), CH4+ and N-2(+) differs from the T9 encounter simulations when O+ ions are not introduced into the background plasma. In our hybrid modeling we use Chamberlain profiles for the atmospheric components. We also include a simple ionosphere model with average mass M=28 amu ions that were generated inside the ionosphere. Titan's interior is considered as a weakly conducting body. Special attention has been paid to comparing the simulated pickup ion density distribution with CAPS-ELS and with RPWS LP observations by the Cassini-Huygens spacecraft along the TA trajectory. Our modeling shows an asymmetry of the ion density distribution and the magnetic field, including the formation of Alfven wing-like structures. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Lipatov, A. S.] NASA, Goddard Space Flight Ctr, GPHI UMBC, Greenbelt, MD 20771 USA. [Lipatov, A. S.] Moscow Inst Phys & Technol, Fac Problems Phys & Power Engn, Moscow, Russia. [Sittler, E. C., Jr.; Hartle, R. E.; Cooper, J. F.; Simpson, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lipatov, AS (reprint author), NASA, Goddard Space Flight Ctr, GPHI UMBC, Greenbelt, MD 20771 USA. EM Alexander.Lipatov-1@nasa.gov; Edward.C.Sittler@nasa.gov; Richard.E.Hartle@nasa.gov; John.F.Cooper@nasa.gov; David.G.Simpson@nasa.gov RI Cooper, John/D-4709-2012 FU NASA Cassini Data Analysis Program [08-CDAP08-0043]; GPHI UMBC [900-37-172, 670-90-315]; NASA GSFC; NASA Ames Advanced Supercomputing (NAS) [SMD-09-1124, SMD-13-1517] FX A.S.L., E.C.S., R.E.H., J.F.C., and D.G.S. were supported by the Grant Analysis of Titan's Interaction with Saturn's Magnetosphere using Cassini Titan Flyby Data and Kinetic-Fluid Model from the NASA Cassini Data Analysis Program (08-CDAP08-0043, PI - E.C. Sittler Jr.). A.S.L. was also supported in part by the grants/tasks 900-37-172 and 670-90-315 between the GPHI UMBC and NASA GSFC. Computational resources (supercomputers Endeavour and Pleiades (Ivy Bridge)) were provided by the NASA Ames Advanced Supercomputing (NAS) Division (Projects SMD-09-1124 and SMD-13-1517). The authors thank the referees for fruitful comments. NR 57 TC 2 Z9 2 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD APR PY 2014 VL 93-94 BP 119 EP 128 DI 10.1016/j.pss.2014.02.012 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG2WO UT WOS:000335278000012 ER PT J AU Petch, J Hill, A Davies, L Fridlind, A Jakob, C Lin, YL Xie, SEC Zhu, P AF Petch, Jon Hill, Adrian Davies, Laura Fridlind, Ann Jakob, Christian Lin, Yanluan Xie, Shaoecheng Zhu, Ping TI Evaluation of intercomparisons of four different types of model simulating TWP-ICE SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE convection; numerical modelling; microphysics ID WEATHER PREDICTION; CLOUD; RAIN AB Four model intercomparisons were run and evaluated using the TWP-ICE field campaign, each involving different types of atmospheric model. Here we highlight what can be learnt from having single-column model (SCM), cloud-resolving model (CRM), global atmosphere model (GAM) and limited-area model (LAM) intercomparisons all based around the same field campaign. We also make recommendations for anyone planning further large multi-model intercomparisons to ensure they are of maximum value to the model development community. CRMs tended to match observations better than other model types, although there were exceptions such as outgoing long-wave radiation. All SCMs grew large temperature and moisture biases and performed worse than other model types for many diagnostics. The GAMs produced a delayed and significantly reduced peak in domain-average rain rate when compared to the observations. While it was shown that this was in part due to the analysis used to drive these models, the LAMs were also driven by this analysis and did not have the problem to the same extent. Based on differences between the models with parametrized convection (SCMs and GAMs) and those without (CRMs and LAMs), we speculate that that having explicit convection helps to constrain liquid water whereas the ice contents are controlled more by the representation of the microphysics. C1 [Petch, Jon; Hill, Adrian] Met Off, Exeter EX1 3PB, Devon, England. [Davies, Laura] Univ Melbourne, Melbourne, Vic 3010, Australia. [Fridlind, Ann] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Jakob, Christian] Monash Univ, Sch Math, Melbourne, Vic 3004, Australia. [Lin, Yanluan] Tsinghua Univ, Ctr Earth Syst Sci, Beijing 100084, Peoples R China. [Xie, Shaoecheng] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Zhu, Ping] Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA. RP Petch, J (reprint author), Met Off, FitzRoy Rd, Exeter EX1 3PB, Devon, England. EM jon.petch@metoffice.gov.uk RI lin, yanluan/A-6333-2015; Xie, Shaocheng/D-2207-2013; Jakob, Christian/A-1082-2010 OI Xie, Shaocheng/0000-0001-8931-5145; Jakob, Christian/0000-0002-5012-3207 FU NASA Radiation Sciences Program; US DOE Office of Science, Office of Biological and Environmental Research [DE-AI02-06ER64173, DE-SC0006712]; US Department of Energy (DOE), Office of Science, Office of Biological and Environmental Research by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; Atmospheric Radiation Measurement Program of the Office of Science at the US Department of Energy; DOE ASR [DE-FG02-09ER64737]; Office of Science (BER), US Department of Energy; US DOE ASR program [DE-FG02-09ER64742] FX A. Fridlind was supported by the NASA Radiation Sciences Program and the US DOE Office of Science, Office of Biological and Environmental Research, through contracts DE-AI02-06ER64173 and DE-SC0006712. The contributions of S. Xie to this work were performed under the auspices of the US Department of Energy (DOE), Office of Science, Office of Biological and Environmental Research by Lawrence Livermore National Laboratory under contract no. DE-AC52-07NA27344 and supported by the Atmospheric Radiation Measurement Program of the Office of Science at the US Department of Energy. Ping Zhu wishes to acknowledge his support by the DOE ASR program under grant DE-FG02-09ER64737. Yanluan Lin was supported by the Office of Science (BER), US Department of Energy. Laura Davies and Christian Jakob were supported by the US DOE ASR program under grant DE-FG02-09ER64742. NR 19 TC 6 Z9 6 U1 0 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD APR PY 2014 VL 140 IS 680 BP 826 EP 837 DI 10.1002/qj.2192 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF7WU UT WOS:000334926800009 ER PT J AU Errico, RM Prive, NC AF Errico, Ronald M. Prive, Nikki C. TI An estimate of some analysis-error statistics using the Global Modeling and Assimilation Office observing-system simulation framework SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE OSSE; atmospheric analysis; data assimilation; analysis error ID VALIDATION AB The observing-system simulation experiment (OSSE) framework developed at the National Aeronautics and Space Administration (NASA), Global Modeling and Assimilation Office (GMAO) is used to estimate some characteristics of analysis error. This is possible because, within the framework, the true state of the simulated atmosphere is known and, after suitable interpolation to a common grid, can be simply differenced with the analysis to compute errors explicitly. The only assumption is that the OSSE is sufficiently realistic so that error statistics derived from it adequately describe those obtained when analyzing observations of the real atmosphere. Attention here is restricted to the troposphere during the months of July and August at 0000 and 1200 UTC using an observation data set from 2011. Analysis-error statistics presented here include geographical distributions of temporal variances, power spectra of spherical harmonics and correlations in meridional, latitudinal and vertical directions. Our most noteworthy results include the revelation through spectral analysis that only synoptic scales are well analyzed and that horizontal correlation lengths in the extratropics are short, with little vertical variation, and the dominance of rotational wind errors in contrast to divergent ones. Also examined are fractional reductions in background-error variances due to analysis of observations. These reveal that in most geographical regions throughout the troposphere, errors are reduced by analyzing observations, as intended. The reductions are typically small, however (-10% in most regions), as should be expected from consideration of the equilibration of errors implied by the Kalman-filter equations. C1 [Errico, Ronald M.; Prive, Nikki C.] Morgan State Univ, Goddard Earth Sci Technol & Res Ctr, Baltimore, MD 21239 USA. [Errico, Ronald M.; Prive, Nikki C.] NASA, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Errico, RM (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA. EM ronald.m.errico@nasa.gov OI Prive, Nikki/0000-0001-8309-8741 FU GMAO FX This OSSE was conducted with the assistance of Ricardo Todling, Meta Sienkiewicz and Joseph Stassi at the GMAO. The ECMWF nature run was provided by Erik Andersson through arrangements made by Michiko Masutani. Support for this project was encouraged by Michele Rienecker and provided by GMAO core funding. NR 11 TC 7 Z9 7 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD APR PY 2014 VL 140 IS 680 BP 1005 EP 1012 DI 10.1002/qj.2180 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF7WU UT WOS:000334926800024 ER PT J AU Coy, L Reynolds, CA AF Coy, Lawrence Reynolds, Carolyn A. TI Singular vectors and their nonlinear evolution during the January 2009 stratospheric sudden warming SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE stratosphere dynamics; sudden warming; singular vectors ID ADAPTIVE OBSERVING GUIDANCE; ATLANTIC TROPICAL CYCLONES; TARGETED OBSERVATIONS; PREDICTION SYSTEM; GROWTH; MODEL; FLOW; PREDICTABILITY; PERTURBATIONS; CIRCULATION AB The evolution and structure of stratospheric singular vectors (SVs) during the major stratospheric sudden warming (SSW) of January 2009 are investigated. SV analyses, optimized for growth at stratospheric levels over 72 h, were examined for selected dates before and during the SSW. It was found that the initial and final SV fields have larger horizontal structures during the SSW event than before the SSW event. A high-altitude forecast model was initialized with perturbations taken from the initial time SV structures and integrated for 144 h to study growth and nonlinear changes in a highly disturbed polar vortex. When large-amplitude initial SV perturbations were forecast during the SSW, large changes occurred in the descent of the SSW event and poleward focusing of the Eliassen-Palm fluxes. Examination of the development of SV analysis suggests that stratospheric SV growth occurs through wave-action conservation as initial SV perturbations propagate into the polar vortex jet. C1 [Coy, Lawrence] Naval Res Lab, Washington, DC USA. [Reynolds, Carolyn A.] Naval Res Lab, Monterey, CA USA. RP Coy, L (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM lawrence.coy@nasa.gov OI Reynolds, Carolyn/0000-0003-4690-4171 FU Office of Naval Research FX This research was funded by the Office of Naval Research and performed at the Naval Research Laboratory. Additional support was received via a grant of computer time from the DOD High Performance Computing Modernization Program. NR 39 TC 0 Z9 0 U1 1 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD APR PY 2014 VL 140 IS 680 BP 1013 EP 1024 DI 10.1002/qj.2181 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF7WU UT WOS:000334926800025 ER PT J AU Rochdane, S Bounoua, L Zhang, P Imhoff, ML Messouli, M Yacoubi-Khebiza, M AF Rochdane, Saloua Bounoua, Lahouari Zhang, Ping Imhoff, Marc L. Messouli, Mohammed Yacoubi-Khebiza, Mohammed TI Combining Satellite Data and Models to Assess Vulnerability to Climate Change and Its Impact on Food Security in Morocco SO SUSTAINABILITY LA English DT Article DE satellite; model; vulnerability index; climate change; food security; Morocco ID NET PRIMARY PRODUCTION; MODIS; ADAPTATION; VEGETATION AB This work analyzes satellite and socioeconomic data to explore the relationship between food and wood demand and supply, expressed in terms of net primary production (NPP), in Morocco. A vulnerability index is defined as the ratio of demand to supply as influenced by population, affluence, technology and climate indicators. The present situation (1995-2007), as well as projections of demand and supply, following the Intergovernmental Panel on Climate Change, Scenarios A2 and B2, are analyzed for a 2025 horizon. We find that the food NPP demand increased by 34.5%, whereas the wood consumption NPP demand decreased by 19.3% between 1995 and 2007. The annual NPP required to support the population's food and wood appropriation was 29.73 million tons of carbon (MTC) in 2007, while the landscape NPP production for the same year was 60.24 MTC; indicating that the population appropriates about 50% of the total NPP resources. Both scenarios show increases in demand and decreases in supply. Under A2, it would take more than 1.25 years for terrestrial ecosystems in Morocco to produce the NPP appropriated by populations in one year. This number is 0.70 years under B2. This already high vulnerability for food and wood products is likely to be exacerbated with climate changes and population increase. C1 [Rochdane, Saloua; Messouli, Mohammed; Yacoubi-Khebiza, Mohammed] Cadi Ayyad Univ, Fac Sci Semlalia, Dept Environm Sci, Marrakech 40000, Morocco. [Bounoua, Lahouari; Zhang, Ping] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zhang, Ping] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Imhoff, Marc L.] Joint Global Change Res Inst 5825 Univ Res Court, College Pk, MD 20742 USA. RP Bounoua, L (reprint author), NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Code 618, Greenbelt, MD 20771 USA. EM rochdane@yahoo.fr; lahouari.bounoua@nasa.gov; ping.zhang@nasa.gov; Marc.Imhoff@pnnl.gov; messouli@ucam.ac.ma; yacoubi@ucam.ac.ma FU African Climate Change Fellowship Program (ACCFP); System for Analysis Research and Training (START) secretariat FX The authors would like to thank the African Climate Change Fellowship Program (ACCFP) and the System for Analysis Research and Training (START) secretariat for their financial support. Thanks are also extended to the staff of the Biospheric Sciences Laboratory of NASA's Goddard Space Flight Center. NR 36 TC 2 Z9 2 U1 3 U2 22 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2071-1050 J9 SUSTAINABILITY-BASEL JI Sustainability PD APR PY 2014 VL 6 IS 4 BP 1729 EP 1746 DI 10.3390/su6041729 PG 18 WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Environmental Sciences; Environmental Studies SC Science & Technology - Other Topics; Environmental Sciences & Ecology GA AF7VA UT WOS:000334921800006 ER PT J AU Ade, PAR Aghanim, N Alves, MIR Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bonaldi, A Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Butler, RC Cardoso, JF Catalano, A Chamballu, A Chiang, HC Chiang, LY Christensen, PR Clements, DL Colombi, S Colombo, LPL Couchot, F Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Dickinson, C Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Dupac, X Ensslin, TA Eriksen, HK Falgarone, E Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Ghosh, T Giard, M Giardino, G Gonzalez-Nuevo, J Gorski, KM Gregorio, A Gruppuso, A Hansen, FK Harrison, D Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Holmes, WA Hornstrup, A Hovest, W Jaffe, AH Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leonardi, R Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S Mazzotta, P Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Oxborrow, CA Pagano, L Pajot, F Paladini, R Paoletti, D Pasian, F Patanchon, G Peel, M Perdereau, O Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Pratt, GW Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rubino-Martin, JA Rusholme, B Sandri, M Savini, G Scott, D Spencer, LD Starck, JL Stolyarov, V Sureau, F Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Valenziano, L Valiviita, J Van Tent, B Verstraete, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Alves, M. I. R. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Catalano, A. Chamballu, A. Chiang, H. C. Chiang, L. -Y. Christensen, P. R. Clements, D. L. Colombi, S. Colombo, L. P. L. Couchot, F. Crill, B. P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Dickinson, C. Diego, J. M. Dole, H. Donzelli, S. Dore, O. Douspis, M. Dupac, X. Ensslin, T. A. Eriksen, H. K. Falgarone, E. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Ghosh, T. Giard, M. Giardino, G. Gonzalez-Nuevo, J. Gorski, K. M. Gregorio, A. Gruppuso, A. Hansen, F. K. Harrison, D. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Holmes, W. A. Hornstrup, A. Hovest, W. Jaffe, A. H. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leonardi, R. Levrier, F. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Mazzotta, P. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Pagano, L. Pajot, F. Paladini, R. Paoletti, D. Pasian, F. Patanchon, G. Peel, M. Perdereau, O. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Pratt, G. W. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Savini, G. Scott, D. Spencer, L. D. Starck, J. -L. Stolyarov, V. Sureau, F. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Tavagnacco, D. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Valenziano, L. Valiviita, J. Van Tent, B. Verstraete, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck intermediate results. XIV. Dust emission at millimetre wavelengths in the Galactic plane SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: general; Galaxy: general; radiation mechanisms: general; radio continuum: ISM; submillimeter: ISM ID PRE-LAUNCH STATUS; SPECTRAL ENERGY-DISTRIBUTIONS; MU-M; MAGNETIC NANOPARTICLES; TEMPERATURE-DEPENDENCE; SUBMILLIMETER EXCESS; MICROWAVE EMISSION; INTERSTELLAR DUST; MAGELLANIC CLOUDS; MOLECULAR CLOUDS AB We use Planck HFI data combined with ancillary radio data to study the emissivity index of the interstellar dust emission in the frequency range 100-353 GHz, or 3-0.8 mm, in the Galactic plane. We analyse the region l = 20 degrees-44 degrees and vertical bar b vertical bar <= 4 degrees where the free-free emission can be estimated from radio recombination line data. We fit the spectra at each sky pixel with a modified blackbody model and two opacity spectral indices, beta(mm) and beta(FIR), below and above 353 GHz, respectively. We find that beta(mm) is smaller than beta(FIR), and we detect a correlation between this low frequency power-law index and the dust optical depth at 353 GHz, tau(353). The opacity spectral index beta(mm) increases from about 1.54 in the more diffuse regions of the Galactic disk, vertical bar b vertical bar = 3 degrees-4 degrees and tau(353) similar to 5 x 10(-5), to about 1.66 in the densest regions with an optical depth of more than one order of magnitude higher. We associate this correlation with an evolution of the dust emissivity related to the fraction of molecular gas along the line of sight. This translates into beta(mm) similar to 1.54 for a medium that is mostly atomic and beta(mm) similar to 1.66 when the medium is dominated by molecular gas. We find that both the two-level system model and magnetic dipole emission by ferromagnetic particles can explain the results. These results improve our understanding of the physics of interstellar dust and lead towards a complete model of the dust spectrum of the Milky Way from far-infrared to millimetre wavelengths. C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, Observ Paris,Sorbonne Paris Cite,APC, F-75205 Paris 13, France. [Lahteenmaki, A.] Aalto Univ, Metsahovi Radio Observ, Aalto 00076, Finland. [Lahteenmaki, A.] Aalto Univ, Dept Radio Sci & Engn, Aalto 00076, Finland. [Kunz, M.] African Inst Math Sci, ZA-7701 Rondebosch, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, I-00198 Rome, Italy. [Ashdown, M.; Curto, A.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa. [Kneissl, R.] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Santiago 0355, Chile. [Bond, J. R.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse 4, France. [Crill, B. P.; Dore, O.; Hildebrandt, S. R.; Rocha, G.; Savini, G.] CALTECH, Pasadena, CA 91125 USA. [Hernandez-Monteagudo, C.] Ctr Estudios Fis Cosmos Aragon, Teruel 44001, Spain. [Borrill, J.; Keskitalo, R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Rebolo, R.] CSIC, Madrid 28037, Spain. [Chamballu, A.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Hornstrup, A.; Linden-Vornle, M.; Norgaard-Nielsen, H. U.; Oxborrow, C. 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A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Zelenchukskiy Region, Karachai Cherke, Russia. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR7095, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Alves, MIR (reprint author), Univ Paris 11, UMR8617, CNRS, Inst Astrophys Spatiale, Batiment 121, F-91405 Orsay, France. EM marta.alves@ias.u-psud.fr RI Butler, Reginald/N-4647-2015; Remazeilles, Mathieu/N-1793-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Ghosh, Tuhin/E-6899-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Lopez-Caniego, Marcos/M-4695-2013; Bobin, Jerome/P-3729-2014; Battaner, Eduardo/P-7019-2014; Vielva, Patricio/F-6745-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015 OI Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Cuttaia, Francesco/0000-0001-6608-5017; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Pierpaoli, Elena/0000-0002-7957-8993; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Peel, Mike/0000-0003-3412-2586; Scott, Douglas/0000-0002-6878-9840; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Finelli, Fabio/0000-0002-6694-3269; De Zotti, Gianfranco/0000-0003-2868-2595; Sandri, Maura/0000-0003-4806-5375; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Morgante, Gianluca/0000-0001-9234-7412; Matarrese, Sabino/0000-0002-2573-1243; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Bobin, Jerome/0000-0003-1457-7890; Vielva, Patricio/0000-0003-0051-272X; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; FU ESA (France); CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MICINN (Spain); JA (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU); European Research Council under the European Union [267934] FX We acknowledge the use of the HEALPix (Gorski et al. 2005) package and IRAS data. The Planck Collaboration acknowledges support from: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). A detailed description of the Planck Collaboration and a list of its members can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page-Planck-Collaborati on. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no 267934. NR 92 TC 17 Z9 17 U1 2 U2 19 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 APR PY 2014 VL 564 AR A45 DI 10.1051/0004-6361/201322367 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000045 ER PT J AU Beck, PG Hambleton, K Vos, J Kallinger, T Bloemen, S Tkachenko, A Garcia, RA Ostensen, RH Aerts, C Kurtz, DW De Ridder, J Hekker, S Pavlovski, K Mathur, S De Smedt, K Derekas, A Corsaro, E Mosser, B Van Winckel, H Huber, D Degroote, P Davies, GR Prsa, A Debosscher, J Elsworth, Y Nemeth, P Siess, L Schmid, VS Papics, PI de Vries, BL van Marle, AJ Marcos-Arenal, P Lobel, A AF Beck, P. G. Hambleton, K. Vos, J. Kallinger, T. Bloemen, S. Tkachenko, A. Garcia, R. A. Ostensen, R. H. Aerts, C. Kurtz, D. W. De Ridder, J. Hekker, S. Pavlovski, K. Mathur, S. De Smedt, K. Derekas, A. Corsaro, E. Mosser, B. Van Winckel, H. Huber, D. Degroote, P. Davies, G. R. Prsa, A. Debosscher, J. Elsworth, Y. Nemeth, P. Siess, L. Schmid, V. S. Papics, P. I. de Vries, B. L. van Marle, A. J. Marcos-Arenal, P. Lobel, A. TI Pulsating red giant stars in eccentric binary systems discovered from Kepler space-based photometry A sample study and the analysis of KIC 5006817 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: solar-type; binaries: general; stars: rotation; Sun: oscillations; stars: individual: KIC5006817; asteroseismology ID SOLAR-LIKE OSCILLATIONS; SUBDWARF-B-STARS; STELLAR ASTROPHYSICS MESA; ECLIPSING BINARY; LIGHT CURVES; FORMATION CHANNELS; SCALING RELATIONS; EQUILIBRIUM TIDE; VELOCITY CURVES; MAIN-SEQUENCE AB Context. The unparalleled photometric data obtained by NASA's Kepler Space Telescope has led to improved understanding of red giant stars and binary stars. Seismology allows us to constrain the properties of red giants. In addition to eclipsing binaries, eccentric non-eclipsing binaries that exhibit ellipsoidal modulations have been detected with Kepler. Aims. We aim to study the properties of eccentric binary systems containing a red giant star and to derive the parameters of the primary giant component. Methods. We applied asteroseismic techniques to determine the masses and radii of the primary component of each system. For a selected target, light and radial velocity curve modelling techniques were applied to extract the parameters of the system and its primary component. Stellar evolution and its effects on the evolution of the binary system were studied from theoretical models. Results. The paper presents the asteroseismic analysis of 18 pulsating red giants in eccentric binary systems, for which masses and radii were constrained. The orbital periods of these systems range from 20 to 440 days. The results of our ongoing radial velocity monitoring progranune with the Hermes spectrograph reveal an eccentricity range of e = 0.2 to 0.76. As a case study we present a detailed analysis of KIC 5006817, whose rich oscillation spectrum allows for detailed seismic analysis. From seismology we constrain the rotational period of the envelope to be at least 165 d, which is roughly twice the orbital period. The stellar core rotates 13 times faster than the surface. From the spectrum and radial velocities we expect that the Doppler beaming signal should have a maximum amplitude of 300 ppm in the light curve. Fixing the mass and radius to the asteroseismically determined values, we find from our binary modelling a value of the gravity darkening exponent that is significantly larger than expected. Through binary modelling, we determine the mass of the secondary component to be 0.29 +/- 0.03 M circle dot. Conclusions. For KIC 5006817 we exclude pseudo-synchronous rotation of the red giant with the orbit. The comparison of the results from seismology and modelling of the light curse shows a possible alignment of the rotational and orbital axis at the 2 sigma level. Red giant eccentric systems could be progenitors of cataclysmic variables and hot subdwarf B stars. C1 [Beck, P. G.; Hambleton, K.; Vos, J.; Bloemen, S.; Tkachenko, A.; Ostensen, R. H.; Aerts, C.; De Ridder, J.; De Smedt, K.; Corsaro, E.; Van Winckel, H.; Degroote, P.; Debosscher, J.; Nemeth, P.; Schmid, V. S.; Papics, P. I.; de Vries, B. L.; van Marle, A. J.; Marcos-Arenal, P.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium. [Hambleton, K.; Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Kallinger, T.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Garcia, R. A.] Univ Paris 07, IRFU SAp, CEA DSM CNRS, Lab AIM, F-91191 Gif Sur Yvette, France. [Aerts, C.] Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Pavlovski, K.] Univ Zagreb, Fac Sci, Dept Phys, Zagreb 10000, Croatia. [Mathur, S.] Space Sci Inst, Boulder, CO 80301 USA. [Derekas, A.] Hungarian Acad Sci, Res Ctr F Astron & Earth Sci, Konkoly Observ, H-1121 Budapest, Hungary. [Mosser, B.] Univ Paris 07, Observ Paris, Univ Paris 06, LESIA,CNRS, F-92195 Meudon, France. [Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Davies, G. R.; Elsworth, Y.] Univ Birmingham, Sch Phys & Astron, Birmingham B13 2TT, W Midlands, England. [Prsa, A.] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Siess, L.] Univ Libre Bruxelles, Inst Astron & Astrophys, B-1050 Brussels, Belgium. [Lobel, A.] Royal Observ Belgium, B-1180 Brussels, Belgium. RP Beck, PG (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium. EM paul.beck@ster.kuleuven.be RI Nemeth, Peter/E-4515-2016; Derekas, Aliz/G-2091-2016; Marcos-Arenal, Pablo/O-4719-2016; OI Davies, Guy/0000-0002-4290-7351; Nemeth, Peter/0000-0003-0963-0239; Derekas, Aliz/0000-0002-6526-9444; Marcos-Arenal, Pablo/0000-0003-1549-9396; Kallinger, Thomas/0000-0003-3627-2561; Garcia, Rafael/0000-0002-8854-3776 FU NASA's Science Mission Directorate; NASA [NNX12AE17G]; Research Council of the KU Leuven [GOA/2013/012]; European Research Council under the European Community [227224]; European Community [312844]; UK STFC PhD grant; EWO-Handers [06260-G.0728.11]; Austrian Science Fund [FWF P23608]; Fund for Scientific Research; Netherlands Organisation for Scientific Research (NWO); Aspirant Ph.D. Fellow of the FWO, Belgium; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences; Hungarian OTKA [K76816, K83790, MBO8C 81013, KTIA URKUT_10 1 2011-0019]; Hungarian Academy of Sciences FX We acknowledge the work of the team behind Kepler. Funding for the Kepler Mission is provided by NASA's Science Mission Directorate. The ground-based follow-up observations are based on spectroscopy made with the Mercator Telescope, operated on the island of La Palma by the Flemish Community, at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This work partially used data analyzed under the NASA grant NNX12AE17G. This research is (partially) funded by the Research Council of the KU Leuven under grant agreement GOA/2013/012. The research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme FP7/2007-2013)/ERC grant agreement no 227224 (PROSPERITY). The research leading to these results has received funding 'from the European Community's Seventh Framework Programme FP7-SPACE-2011-1 , project number 312844 (SPACEINN). K.H. was supported by a UK STFC PhD grant. J.D.R., T.K. and E.C. acknowledge the support of the EWO-Handers wider project 06260- G.0728.11. T.K. also acknowledges financial support from the Austrian Science Fund (FWF P23608). A.T. was supported by the Fund for Scientific Research. S.H. was supported by the Netherlands Organisation for Scientific Research (NWO). V.S.S. is an Aspirant Ph.D. Fellow of the FWO, Belgium. A.D. is supported by a Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. This project has been supported by the Hungarian OTKA Grants K76816, K83790, MBO8C 81013 and KTIA URKUT_10 1 2011-0019 grant and the "Lendulet2009" Young Researchers Programme of the Hungarian Academy of Sciences. P.G.B thanks Nick Cox for observational work. NR 96 TC 30 Z9 30 U1 1 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2014 VL 564 AR A36 DI 10.1051/0004-6361/201322477 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000036 ER PT J AU Deleuil, M Almenara, JM Santerne, A Barros, SCC Havel, M Hebrard, G Bonomo, AS Bouchy, F Bruno, U Damiani, C Diaz, RF Montagnier, U Moutou, C AF Deleuil, M. Almenara, J. -M. Santerne, A. Barros, S. C. C. Havel, M. Hebrard, G. Bonomo, A. S. Bouchy, F. Bruno, U. Damiani, C. Diaz, R. F. Montagnier, U. Moutou, C. TI SOPHIE velocimetry of Kepler transit candidates XI. Kepler-412 system: probing the properties of a new inflated hot Jupiter SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; techniques: photometric; techniques: radial velocities; stars: fundamental parameters ID COROT SPACE MISSION; EXTRASOLAR PLANETS; GIANT PLANET; LIGHT CURVES; ATMOSPHERIC CHARACTERIZATION; SECONDARY ECLIPSE; DWARF COMPANION; HIGH ALBEDO; MASS STARS; EXOPLANETS AB Context. Hot Jupiters are still a fascinating exoplanet population that presents a diversity we are still far from understanding. High-precision photometric observations combined with radial velocity measurements give us a unique opportunity to constrain their properties better, on both their internal structure and their atmospheric bulk properties. Aims. We initiated a follow-up program of Kepler-released planet candidates with the goal of confirming the planetary nature of a number of them through radial velocity measurements. For those that successfully passed the radial velocity screening, we furthermore performed a detailed exploration of their properties to characterize the systems. As a byproduct, these systematic observations allow us to consolidate the exoplanets' occurrence rate. Methods. We performed a complete analysis of the Kepler-412 system, listed as planet candidate KOI-202 in the Kepler catalog, by combining the Kepler observations from Q1 to Q15, to ground-based spectroscopic observations that allowed us to derive radial velocity measurements, together with the host-star parameters and properties. We also analyzed the light curve to derive the star's rotation period and the phase function of the planet, including the secondary eclipse. Results. We secured the planetary nature of Kepler-412b. We found the planet has a mass of 0.939 +/- 0.085 M-Jup and a radius of 1.325 +/- 0.043 R-Jup, which makes it a member of the bloated giant subgroup. It orbits its G3 V host star in 1.72 days. The system has an isochronal age of 5.1 Gyr, consistent with its moderate stellar activity as observed in the Kepler light curve and the rotation of the star of 17.2 +/- 1.6 days. From the detected secondary we derived the day-side temperature as a function of the geometric albedo. We estimated that the geometrical albedo A(g), should be between 0.094 +/- 0.015 and 0.013 (+0.017)(-0.013) and the brightness of the day side 2380 +/- 40 K. The measured night-side flux corresponds to a night-side brightness temperature of 2154 +/- 83 K, much greater than what is expected for a planet with homogeneous heat redistribution. From the comparison to star and planet evolution models, we found that dissipation should operate in the deep interior of the planet. This modeling also shows that despite its inflated radius, the planet presents a noticeable amount of heavy elements, which accounts for a mass fraction of 0.11 +/- 0.04. C1 [Deleuil, M.; Almenara, J. -M.; Santerne, A.; Barros, S. C. C.; Bouchy, F.; Bruno, U.; Damiani, C.; Diaz, R. F.; Moutou, C.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. [Santerne, A.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Havel, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hebrard, G.; Montagnier, U.] Observ Haute Provence, F-04670 St Michel Lobservatoire, France. [Hebrard, G.; Montagnier, U.] Inst Astrophys Paris, F-75014 Paris, France. [Bonomo, A. S.] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, Italy. RP Deleuil, M (reprint author), Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. EM magali.deleuil@lam.fr OI Barros, Susana/0000-0003-2434-3625; Santerne, Alexandre/0000-0002-3586-1316; Diaz, Rodrigo/0000-0001-9289-5160 FU PNP of CNRS/INSU; French ANR; CNES via postdoctoral fellowship program; European Research Council/European Community under the FP7 [239953]; NASA Postdoctoral Program at the Ames Research Center; INAF/HARPS-N fellowship; [98761]; [251091]; [426808] FX This work is based on observations collected with the NASA's satellite Kepler, the SOPHIE spectrograph on the 1.93-m telescope at the Observatoire de Haute-Provence (CNRS), France. The authors thank the staff at the Haute-Provence Observatory. They also acknowledge the PNP of CNRS/INSU and the French ANR for their support. The team at LAM acknowledges support by grants 98761 (SCCB), 251091 (JMA), and 426808 (CD). R.F.D. was supported by the CNES via its postdoctoral fellowship program. A.S. acknowledges support from the European Research Council/European Community under the FP7 through Starting Grant agreement number 239953. M.H. 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. ASB gratefully acknowledges support through INAF/HARPS-N fellowship. NR 67 TC 10 Z9 10 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2014 VL 564 AR A56 DI 10.1051/0004-6361/201323017 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000056 ER PT J AU Guarrasi, M Reale, E Orlando, S Mignone, A Klimchuk, JA AF Guarrasi, M. Reale, E. Orlando, S. Mignone, A. Klimchuk, J. A. TI MHD modeling of coronal loops: the transition region throat SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: corona; Sun: magnetic fields; Sun: transition region; magnetohydrodynamics (MHD) ID SOLAR CORONA; THERMAL CONDUCTION; RADIATIVE LOSSES; ATOMIC DATABASE; MAGNETIC-FIELD; EMISSION-LINES; SIMULATIONS; DYNAMICS; CORE; ABUNDANCES AB Context. The expansion of coronal loops in the transition region may considerably influence the diagnostics of the plasma emission measure. The cross-sectional area of the loops is expected to depend on the temperature and pressure, and might be sensitive to the heating rate. Aims. The approach here is to study the area response to slow changes in the coronal heating rate, and check the current interpretation in terms of steady heating models. Methods. We study the area response with a time-dependent 2D magnetohydrodynamic (MHD) loop model, including the description of the expanding magnetic field, coronal heating and losses by thermal conduction, and radiation from optically thin plasma. We run a simulation for a loop 50 Mm long and quasi-statically heated to about 4 MK. Results. We find that the area can change substantially with the quasi-steady heating rate, e.g., by similar to 40% at 0.5 MK as the loop temperature varies between 1 MK and 4 MK, and, therefore, affects the interpretation of the differential emission measure vs. temperature (DEM(T)) curves. C1 [Guarrasi, M.; Reale, E.] Univ Palermo, Dipartimento Fis & Chim, I-90134 Palermo, Italy. [Reale, E.; Orlando, S.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Mignone, A.] Univ Turin, Dipartimento Fis Gen, I-10125 Turin, Italy. [Klimchuk, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Guarrasi, M (reprint author), Univ Palermo, Dipartimento Fis & Chim, Piazza Parlamento 1, I-90134 Palermo, Italy. EM m.guarrasi@cineca.it RI Klimchuk, James/D-1041-2012; OI Klimchuk, James/0000-0003-2255-0305; Orlando, Salvatore/0000-0003-2836-540X; Reale, Fabio/0000-0002-1820-4824 FU Italian Minister dell'Universita e Ricerca; Agenzia Spaziale Italiana (ASI) [I/023/09/0, I/015/07/0]; CINECA under the ISCRA initiative [HP10CWS0PW, HP10B54VL7]; HPC facility (SCAN) of the INAF - Osservatorio Astronomico di Palermo; NASA FX We thank the anonymous referee for constructive comments and suggestions. We acknowledge support from the Italian Minister dell'Universita e Ricerca and Agenzia Spaziale Italiana (ASI), contract I/023/09/0 and I/015/07/0. PLUTO was developed at the Astronomical Observatory of Turin in collaboration with the Department of Physics at the University of Turin. We acknowledge the CINECA awards no. HP10CWS0PW and no. HP10B54VL7 under the ISCRA initiative, and the HPC facility (SCAN) of the INAF - Osservatorio Astronomico di Palermo, for the availability of high-performance computing resources and support. CHIANTI is a collaborative project involving the NRL (USA), the Universities of Florence (Italy) and Cambridge (UK), and George Mason University (USA). The work of J.A.K. was supported by the NASA Supporting Research and Technology Program. We thank the International Space Science Institute (ISSI) for hosting the International Team of S. Bradshaw and H. Mason: Coronal Heating - Using Observables to Settle the Question of Steady vs. Impulsive Heating. NR 33 TC 5 Z9 5 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2014 VL 564 AR A48 DI 10.1051/0004-6361/201322848 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000048 ER PT J AU Langer, WD Pineda, JL Velusamy, T AF Langer, W. D. Pineda, J. L. Velusamy, T. TI The scale height of gas traced by [C II] in the Galactic plane SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: structure; ISM: clouds; ISM: atoms; infrared: ISM ID MILKY-WAY; MOLECULAR CLOUDS; COLLISIONAL EXCITATION; HI DISTRIBUTION; GALAXY; EMISSION; EQUILIBRIUM; PRESSURE; DISK; COBE AB Context. The distribution of various interstellar gas components and the pressure in the interstellar medium (ISM) is a result of the interplay of different dynamical mechanisms and energy sources on the gas in the Milky Way. The scale heights of the different gas tracers, such as H I and CO, are a measure of these processes. The scale height of [C II] emission in the Galactic plane is important for understanding those ISM components not traced by CO or H I. Aims. We determine the average distribution of [C II] perpendicular to the plane in the inner Galactic disk and compare it to the distributions of other key gas tracers, such as CO and H I. Methods. We calculated the vertical, z, distribution of [C II] in the inner Galactic disk by adopting a model for the emission that combines the latitudinal, b, spectrally unresolved BICE survey, with the spectrally resolved Herschel Galactic plane survey of [C II] at b = 0 degrees. Our model assumed a Gaussian emissivity distribution vertical to the plane, and related the distribution in z to that of the latitude b using the spectrally resolved [C II] Herschel survey as the boundary solution for the emissivity at b = 0 degrees. Results. We find that the distribution of [C II] perpendicular to the plane has a full-width half-maximum of 172 pc, larger than that of CO, which averages similar to 110 pc in the inner Galaxy, but smaller than that of H I, similar to 230 pc, and is offset by -28 pc. Conclusions. We explain the difference in distributions of [C II], CO, and H I as due to [C II] tracing a mix of ISM components. Models of hydrostatic equilibrium of clouds in the disk predict different scale heights, for the same interstellar pressure. The diffuse molecular clouds with [C II] but no CO emission likely have a scale height intermediate between the low density atomic hydrogen H I clouds and the dense CO molecular clouds. C1 [Langer, W. D.; Pineda, J. L.; Velusamy, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Langer, WD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Willlam.Langer@jpl.nasa.gov NR 32 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2014 VL 564 AR A101 DI 10.1051/0004-6361/201323281 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000101 ER PT J AU Menu, J van Boekel, R Henning, T Chandler, CJ Linz, H Benisty, M Lacour, S Min, M Waelkens, C Andrews, SM Calvet, N Carpenter, JM Corder, SA Deller, AT Greaves, JS Harris, RJ Isella, A Kwon, W Lazio, J Le Bouquin, JB Menard, F Mundy, LG Perez, LM Ricci, L Sargent, AI Storm, S Testi, L Wilner, DJ AF Menu, J. van Boekel, R. Henning, Th. Chandler, C. J. Linz, H. Benisty, M. Lacour, S. Min, M. Waelkens, C. Andrews, S. M. Calvet, N. Carpenter, J. M. Corder, S. A. Deller, A. T. Greaves, J. S. Harris, R. J. Isella, A. Kwon, W. Lazio, J. Le Bouquin, J. -B. Menard, F. Mundy, L. G. Perez, L. M. Ricci, L. Sargent, A. I. Storm, S. Testi, L. Wilner, D. J. TI On the structure of the transition disk around TW Hydrae SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE protoplanetary disks; techniques: interferometric; stars: individual: TW Hya ID INTERSTELLAR SILICATE MINERALOGY; HERBIG AE/BE STARS; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; HD 100546; SCATTERED-LIGHT; GRAIN-GROWTH; RADIATIVE-TRANSFER; ACCRETION DISKS; INNER HOLE AB Context. For over a decade, the structure of the inner cavity in the transition disk of TW Hydrae has been a subject of debate. Modeling the disk with data obtained at different wavelengths has led to a variety of proposed disk structures. Rather than being inconsistent, the individual models might point to the different faces of physical processes going on in disks, such as dust growth and planet formation. Aims. Our aim is to investigate the structure of the transition disk again and to find to what extent we can reconcile apparent model differences. Methods. A large set of high-angular-resolution data was collected from near-infrared to centimeter wavelengths. We investigated the existing disk models and established a new self-consistent radiative-transfer model. A genetic fitting algorithm was used to automatize the parameter fitting, and uncertainties were investigated in a Bayesian framework. Results. Simple disk models with a vertical inner rim and a radially homogeneous dust composition from small to large grains cannot reproduce the combined data set. Two modifications are applied to this simple disk model: (1) the inner rim is smoothed by exponentially decreasing the surface density in the inner similar to 3 AU, and (2) the largest grains (>100 mu m) are concentrated towards the inner disk region. Both properties can be linked to fundamental processes that determine the evolution of protoplanetary disks: the shaping by a possible companion and the different regimes of dust-grain growth, respectively. Conclusions. The full interferometric data set from near-infrared to centimeter wavelengths requires a revision of existing models for the TW Hya disk. We present a new model that incorporates the characteristic structures of previous models but deviates in two key aspects: it does not have a sharp edge at 4 AU, and the surface density of large grains differs from that of smaller grains. This is the first successful radiative-transfer-based model for a full set of interferometric data. C1 [Menu, J.; Waelkens, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Menu, J.; van Boekel, R.; Henning, Th.; Linz, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Chandler, C. J.; Perez, L. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Benisty, M.; Le Bouquin, J. -B.; Menard, F.] CNRS UJF Grenoble 1, UMR 5274, Inst Planetol & Astrophys Grenoble, F-38041 Grenoble, France. [Lacour, S.] Univ Paris Diderot, CNRS, UPMC, LESIA,Observ Paris, F-92195 Meudon, France. [Min, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Andrews, S. M.; Harris, R. J.; Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Calvet, N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Carpenter, J. M.; Isella, A.; Ricci, L.; Sargent, A. I.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Corder, S. A.] Joint ALMA Observ, Santiago 7630000, Chile. [Deller, A. T.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Greaves, J. S.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Kwon, W.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Lazio, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA. [Menard, F.] Univ Chile, CNRS INSU France UMI 3386, UMI FCA, Santiago, Chile. [Menard, F.] Univ Chile, Dept Astron, Santiago, Chile. [Mundy, L. G.; Storm, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Testi, L.] European So Observ, D-85748 Garching, Germany. [Testi, L.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Menu, J (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Louvain, Belgium. EM jonathan.menu@ster.kuleuven.be OI Deller, Adam/0000-0001-9434-3837 FU FWO travel grant [V448412N]; Millennium Science Initiative (Chilean Ministry of Economy) [Nucleus P10-022F]; EU FP7 [284405]; Smithsonian Institution; Academia Sinica FX J. Menu wishes to thank B. Acke for useful discussions, K. Johnston for support with the CASA software, and P. Degroote for providing SED analysis/fitting software. We are grateful to I. Pascucci and to the anonymous referee for comments that helped improving the manuscript. J. Menu acknowledges an FWO travel grant for a long research stay abroad (V448412N). F. Menard acknowledges support from the Millennium Science Initiative (Chilean Ministry of Economy), through grant "Nucleus P10-022F". F. Menard also acknowledges funding from the EU FP7-2011 under Grant Agreement No 284405. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The National Radio Astronomy Observatory is a facility of the National Science Foundation NR 126 TC 31 Z9 31 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2014 VL 564 AR A93 DI 10.1051/0004-6361/201322961 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000093 ER PT J AU Rauch, T Werner, K Quinet, P Kruk, JW AF Rauch, T. Werner, K. Quinet, P. Kruk, J. W. TI Stellar laboratories II. New Zn IV and Zn V oscillator strengths and their validation in the hot white dwarfs G191-B2B and RE 0503-289 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE atomic data; line: identification; stars: abundances; stars: individual: G191-B2B; virtual observatory tools; stars: individual: RE 0503-289 ID SPECTRAL-ANALYSIS; PHOTOSPHERES AB Context. For the spectral analysis of high-resolution and high-signal-to-noise (S/N) spectra of hot stars, state-of-the-art non-local thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that is used for their calculation. In a recent analysis of the ultraviolet (UV) spectrum of the DA-type white dwarf G191-B2B, 21 Zn IV lines were newly identified. Because of the lack of Zn IV data, transition probabilities of the isoelectronic Ge VI were adapted for a first, coarse determination of the photospheric Zn abundance. Aims. Reliable Zn IV and Zn V oscillator strengths are used to improve the Zn abundance determination and to identify more Zn lines in the spectra of G191-B2B and the DO-type white dwarf RE 0503-289. Methods. We performed new calculations of Zn IV and Zn V oscillator strengths to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models for the analysis of the in Zn IV - V spectrum exhibited in high-resolution and high-S/N UV observations of G191-B2B and RE 0503-289. Results. In the UV spectrum of G191-B2B, we identify 31 Zn IV and 16 Zn V lines. Most of these are identified for the first time in any star. We can reproduce well almost all of them at log Zn = -5.52 +/- 0.2 (mass fraction, about 1.7 times solar). In particular, the in Zn IV / Zn V ionization equilibrium, which is a very sensitive T-eff indicator, is well reproduced with the previously determined T-eff = 60 000 +/- 2000 K and log g = 7.60 +/- 0.05. In the spectrum of RE 0503-289, we identified 128 Zn V lines for the first time and determined log Zn = -3.57 +/- 0.2 (155 times solar). Conclusions. Reliable measurements and calculations of atomic data are a pre-requisite for stellar-atmosphere modeling. Observed Zn IV and Zn V line profiles in two white dwarf (G191-B2B and RE 0503-289) ultraviolet spectra were well reproduced with our newly calculated oscillator strengths. This allowed us to determine the photospheric Zn abundance of these two stars precisely. C1 [Rauch, T.; Werner, K.] Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany. [Quinet, P.] Univ Mons UMONS, B-7000 Mons, Belgium. [Quinet, P.] Univ Liege, IPNAS, B-4000 Liege, Belgium. [Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rauch, T (reprint author), Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, Sand 1, D-72076 Tubingen, Germany. EM rauch@astro.uni-tuebingen.de FU German Aerospace Center (DLR) [05 OR 0806]; Belgian FRS-FNRS; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX T.R. is supported by the German Aerospace Center (DLR, grant 05 OR 0806). Financial support from the Belgian FRS-FNRS is also acknowledged. PQ is research director of this organization. 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 10 TC 11 Z9 11 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2014 VL 564 AR A41 DI 10.1051/0004-6361/201423491 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000041 ER PT J AU Schonherr, G Schwarm, FW Falkner, S Dauser, T Ferrigno, C Kuhnel, M Klochkov, D Kretschmar, P Becker, PA Wolff, MT Pottschmidt, K Falanga, M Kreykenbohm, I Furst, F Staubert, R Wilms, J AF Schoenherr, G. Schwarm, F. -W. Falkner, S. Dauser, T. Ferrigno, C. Kuehnel, M. Klochkov, D. Kretschmar, P. Becker, P. A. Wolff, M. T. Pottschmidt, K. Falanga, M. Kreykenbohm, I. Fuerst, F. Staubert, R. Wilms, J. TI Formation of phase lags at the cyclotron energies in the pulse profiles of magnetized, accreting neutron stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: binaries; stars: neutron; methods: numerical ID X-RAY PULSARS; BEAM PATTERN; CENTAURUS X-3; 4U 0115+63; GEOMETRY; SCATTERING; LINE; RADIATION; FEATURES; SPECTRA AB Context. Accretion-powered X-ray pulsars show highly energy-dependent and complex pulse-profile morphologies. Significant deviations from the average pulse profile can appear, in particular close to the cyclotron line energies. These deviations can be described as energy-dependent phase lags, that is, as energy-dependent shifts of main features in the pulse profile. Aims. Using a numerical study we explore the effect of cyclotron resonant scattering on observable, energy-resolved pulse profiles. Methods. We generated the observable emission as a function of spin phase, using Monte Carlo simulations for cyclotron resonant scattering and a numerical ray-tracing routine accounting for general relativistic light-bending effects on the intrinsic emission from the accretion columns. Results. We find strong changes in the pulse profile coincident with the cyclotron line energies. Features in the pulse profile vary strongly with respect to the average pulse profile with the observing geometry and shift and smear out in energy additionally when assuming a non-static plasma. Conclusions. We demonstrate how phase lags at the cyclotron energies arise as a consequence of the effects of angular redistribution of X-rays by cyclotron resonance scattering in a strong magnetic field combined with relativistic effects. We also show that phase lags are strongly dependent on the accretion geometry. These intrinsic effects will in principle allow us to constrain a system's accretion geometry. C1 [Schoenherr, G.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Schoenherr, G.; Schwarm, F. -W.; Falkner, S.; Dauser, T.; Kuehnel, M.; Kreykenbohm, I.; Wilms, J.] Dr Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany. [Ferrigno, C.] Univ Geneva, INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. [Klochkov, D.; Staubert, R.] Univ Tubingen, Abt Astron, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Kretschmar, P.] European Space Astron Ctr ESA ESAC, Sci Operat Dept, Madrid 28691, Spain. [Becker, P. A.] George Mason Univ, Fairfax, VA 22030 USA. [Wolff, M. T.] Naval Res Lab, Div Space Sci, High Energy Space Environm Branch, Washington, DC 20375 USA. [Pottschmidt, K.] Univ Maryland Baltimore Cty, CRESST, Greenbelt, MD 20771 USA. [Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Falanga, M.] Int Space Sci Inst, CH-3012 Bern, Switzerland. [Fuerst, F.] CALTECH, Pasadena, CA 91125 USA. RP Schonherr, G (reprint author), Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany. EM g.schoenherr@aip.de RI Wilms, Joern/C-8116-2013; OI Wilms, Joern/0000-0003-2065-5410; Falkner, Sebastian/0000-0001-5209-991X; Kretschmar, Peter/0000-0001-9840-2048 FU Bundesministerium fur Wirtschaft und Technologie through Deutsches Zentrum fur Luft- und Raumfahrt [50 OR 1113]; US Office of Naval Research; NASA ADAP Program [NNH13AV18I] FX We thank the International Space Science Institute ISSI in Bern (CH) for granting two International Team meetings on "The physics of the accretion column of X-ray pulsars", which have much inspired this collaborative work. We also thank the Bundesministerium fur Wirtschaft und Technologie for funding through Deutsches Zentrum fur Luft- und Raumfahrt grant 50 OR 1113. M.T.W. is supported by the US Office of Naval Research and the NASA ADAP Program under grant NNH13AV18I. We thank the anonymous referee for very useful comments. NR 27 TC 5 Z9 5 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 APR PY 2014 VL 564 AR L8 DI 10.1051/0004-6361/201322448 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000147 ER PT J AU Wu, SC Remington, RW Folk, CL AF Wu, Shu-Chieh Remington, Roger W. Folk, Charles L. TI Onsets do not override top-down goals, but they are responded to more quickly SO ATTENTION PERCEPTION & PSYCHOPHYSICS LA English DT Article DE Attentional capture; Visual search; Selective attention ID ABRUPT ONSETS; PRIORITIZING SELECTION; CONTROL SETTINGS; STIMULUS-DRIVEN; VISUAL MARKING; CAPTURE; ATTENTION; ADDITIVITY; SEARCH; COVERT AB Do onsets automatically capture attention? Spatial-cuing experiments often reveal no capture by onset cues in searches for color targets. However, recent experiments have shown faster responses to an uncued color target presented as an abrupt onset than as a change to an existing item, which has been argued to reflect capture by the onset. In the present experiment, we tested whether this onset advantage reflects the capture of attention or processing independent of shifts of attention. In a modified spatial-cuing paradigm, noninformative color precues were paired with color targets presented as abrupt onsets or as no-onset characters. Critically, the number of other onset items in the target display was manipulated, which has previously been shown to disrupt attention allocation to any particular item. It was reasoned that if the onset advantage for uncued color targets reflects attentional capture, then the appearance of additional onsets should eliminate this advantage. The results showed that even with multiple onsets on the target display, the onset advantage remained additive with cue validity. The additive effects are inconsistent with automatic capture by onsets, suggesting instead that the onset advantage arises from an independent source. C1 [Wu, Shu-Chieh] San Jose State Univ, Moffett Field, CA 94035 USA. [Wu, Shu-Chieh] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Remington, Roger W.] Univ Queensland, St Lucia, Qld, Australia. [Folk, Charles L.] Villanova Univ, Villanova, PA 19085 USA. RP Wu, SC (reprint author), San Jose State Univ, Mail Stop 262-4, Moffett Field, CA 94035 USA. EM shu-chieh.wu@nasa.gov FU Australian Research Council Discovery Grant [DP120103721] FX R.W.R. and C.L.F. were supported by Australian Research Council Discovery Grant No. DP120103721. Portions of this article were presented at the 52nd Annual Meeting of the Psychonomic Society, Seattle, Washington, November 2011. We thank Alexandra Shelley for her assistance in recruiting and testing participants, and two anonymous reviewers for comments on the manuscript. NR 17 TC 5 Z9 6 U1 0 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1943-3921 EI 1943-393X J9 ATTEN PERCEPT PSYCHO JI Atten. Percept. Psychophys. PD APR PY 2014 VL 76 IS 3 BP 649 EP 654 DI 10.3758/s13414-014-0637-z PG 6 WC Psychology; Psychology, Experimental SC Psychology GA AF2CX UT WOS:000334521300001 PM 24596080 ER PT J AU Perrot, D Molotch, NP Musselman, KN Pugh, ET AF Perrot, Danielle Molotch, Noah P. Musselman, Keith N. Pugh, Evan T. TI Modelling the effects of the mountain pine beetle on snowmelt in a subalpine forest SO ECOHYDROLOGY LA English DT Article DE snow-vegetation interactions; mountain pine beetle; snowmelt modeling; tree death ID BOREAL FOREST; ENERGY-BALANCE; NIWOT RIDGE; ACCUMULATION; RADIATION; ABLATION; CANOPY; SOIL; STREAMFLOW; EPIDEMIC AB The recent mountain pine beetle epidemic in the Colorado River Basin has resulted in widespread tree mortality in pine stands across the Colorado Plateau. Because of complex micro-scale (i.e. tree well scale) interactions between vegetation and snow processes, one of the most significant issues resulting from this epidemic is the potential hydrologic impacts of the effects of changing forest structure. Using SNTHERM, we conducted a comparative modelling scenario analysis of the snowpack along a transect between two trees over the course of the snow ablation season (28 February-30 June) under four forest stand conditions to assess changes in snowpack characteristics because of loss of canopy biomass. We found that the red phase scenario (intermediate phase of tree death) exhibited a 4-day earlier snow disappearance date than the living stand scenario and grey phase scenario (advanced phase of tree death), although the timing of isothermal conditions at 0 degrees C was identical. The modelled clearcut scenario snowpack became isothermal at 0 degrees C 10days earlier than the living, red phase, or grey phase scenarios. The clearcut modelling scenario also exhibited the greatest homogenization of snow properties, and the spatio-temporal distribution of snow disappearance at the tree well scale was 70% as variable as the living, red phase and grey phase modelling scenarios. These results provide insight to the processes responsible for changing hydrologic dynamics in snow-dominated forest ecosystems with the onset of vegetation stress and death and may help inform future forest management strategies. Copyright (c) 2012 John Wiley & Sons, Ltd. C1 [Perrot, Danielle; Molotch, Noah P.] Univ Colorado, Inst Arctic & Alpine Res, Dept Geog, Boulder, CO 80309 USA. [Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Musselman, Keith N.] Univ Calif Los Angeles, Dept Civil & Environm Engn, Los Angeles, CA USA. [Pugh, Evan T.] Univ Colorado, Dept Geol, Boulder, CO 80309 USA. RP Perrot, D (reprint author), Univ Colorado, Dept Geog, Inst Arctic & Alpine Res Campus,Box 450, Boulder, CO 80309 USA. EM danielle.perrot@colorado.edu RI Molotch, Noah/C-8576-2009 FU National Science Foundation Hydrological Sciences grants [EAR1032295, EAR1032308, EAR 1141764] FX This project was funded by the National Science Foundation Hydrological Sciences grants EAR1032295, EAR1032308, and EAR 1141764. Many thanks to Sean Burns, Mark Williams and Christopher Knight. NR 61 TC 6 Z9 6 U1 1 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1936-0584 EI 1936-0592 J9 ECOHYDROLOGY JI Ecohydrology PD APR PY 2014 VL 7 IS 2 BP 226 EP 241 DI 10.1002/eco.1329 PG 16 WC Ecology; Environmental Sciences; Water Resources SC Environmental Sciences & Ecology; Water Resources GA AF4HC UT WOS:000334671600005 ER PT J AU Jee, S Shariff, K AF Jee, SolKeun Shariff, Karim TI Detached-eddy simulation based on the v(2) - f model SO INTERNATIONAL JOURNAL OF HEAT AND FLUID FLOW LA English DT Article DE Detached-eddy simulation; v(2) - f model; Hybrid RANS/LES ID CIRCULAR-CYLINDER; TURBULENCE MODEL; ISOTROPIC TURBULENCE; FLOW; CHANNELS; CLOSURE; WAKE AB Detached-eddy simulation (DES) based on the v(2) - f Reynolds-averaged Navier-Stokes (RANS) model is developed and tested. The v(2) - f model incorporates anisotropy of near-wall turbulence, which is absent in other RANS models commonly used for DES. The v(2) - f RANS model is modified in order that in the DES formulation it reduces to a transport equation for the subgrid-scale kinetic energy in isotropic turbulence. First, three coefficients in the elliptic relaxation equation are modified and the modification is tested for RANS of channel flow. Next, the proposed v(2) - f DES model is formulated. The constant, Cam, required in the DES formulation is calibrated by simulating both decaying and statistically-steady isotropic turbulence. The formulation is tested for flow around a circular cylinder at a Reynolds number of 3900, in which case turbulence develops after separation. Simulations indicate that this model represents the turbulent wake nearly as accurately as the dynamic Smagorinsky model. For comparison, Spalart-Allmaras (SA) based DES is also included in the cylinder flow simulations. Finally, the proposed model is tested for a separated turbulent boundary layer on an airfoil. The delayed-DES (DDES) approach is found to be necessary. The v(2) - f DDES calculation gives good predictions for the aerodynamic forces and the pressure distribution measured in experiments. The proposed model is also compared with SA-DDES for the airfoil. (C) 2013 Elsevier Inc. All rights reserved. C1 [Jee, SolKeun; Shariff, Karim] NASA, Ames Res Ctr, Moffett Field, CA 94043 USA. RP Jee, S (reprint author), United Technol Res Ctr, 411 Silver Lane,MS 129-89, E Hartford, CT 06108 USA. EM jees@utrc.utc.com; karim.shariff@nasa.gov OI Shariff, Karim/0000-0002-7256-2497 FU SolKeun Jee to the NASA Postdoctoral Program at the Ames Research Center FX The authors thank Dr. Michael Rogers and Dr. Scott Murman of NASA Ames Research Center for helpful discussions and their suggestions on a draft version of the manuscript. This research was supported by appointment of SolKeun Jee to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 48 TC 2 Z9 2 U1 0 U2 18 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0142-727X EI 1879-2278 J9 INT J HEAT FLUID FL JI Int. J. Heat Fluid Flow PD APR PY 2014 VL 46 BP 84 EP 101 DI 10.1016/j.ijheatfluidflow.2013.12.006 PG 18 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA AG0KA UT WOS:000335103200007 ER PT J AU Das, S Louis, T Nolta, MR Addison, GE Battistelli, ES Bond, JR Calabrese, E Crichton, D Devlin, MJ Dicker, S Dunkley, J Dunner, R Fowler, JW Gralla, M Hajian, A Halpern, M Hasselfield, M Hilton, M Hincks, AD Hlozek, R Huffenberger, KM Hughes, JP Irwin, KD Kosowsky, A Lupton, RH Marriage, TA Marsden, D Menanteau, F Moodley, K Niemack, MD Page, LA Partridge, B Reese, ED Schmitt, BL Sehgal, N Sherwin, BD Sievers, JL Spergel, DN Staggs, ST Swetz, DS Switzer, ER Thornton, R Trac, H Wollack, E AF Das, Sudeep Louis, Thibaut Nolta, Michael R. Addison, Graeme E. Battistelli, Elia S. Bond, J. Richard Calabrese, Erminia Crichton, Devin Devlin, Mark J. Dicker, Simon Dunkley, Joanna Duenner, Rolando Fowler, Joseph W. Gralla, Megan Hajian, Amir Halpern, Mark Hasselfield, Matthew Hilton, Matt Hincks, Adam D. Hlozek, Renee Huffenberger, Kevin M. Hughes, John P. Irwin, Kent D. Kosowsky, Arthur Lupton, Robert H. Marriage, Tobias A. Marsden, Danica Menanteau, Felipe Moodley, Kavilan Niemack, Michael D. Page, Lyman A. Partridge, Bruce Reese, Erik D. Schmitt, Benjamin L. Sehgal, Neelima Sherwin, Blake D. Sievers, Jonathan L. Spergel, David N. Staggs, Suzanne T. Swetz, Daniel S. Switzer, Eric R. Thornton, Robert Trac, Hy Wollack, Ed TI The Atacama Cosmology Telescope: temperature and gravitational lensing power spectrum measurements from three seasons of data SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE CMBR experiments; gravitational lensing; Sunyaev-Zeldovich effect; CMBR theory ID SOUTH-POLE TELESCOPE; MICROWAVE BACKGROUND ANISOTROPIES; DAMPING TAIL; 148 GHZ; MAPS; CONSTRAINTS; PARAMETERS; SCALE; FIELD; QUAD AB We present the temperature power spectra. of the cosmic microwave background (CMD) derived from the three seasons of data from the Atacama Cosmology Telescope (ACT) at 148 Ealiz and 218 GHz as well as the (Toss-frequency spectrum between the two channels. We detect and correct. for contamination due to the Galactic cirrus in our equatorial maps. We present the results of a number of tests for possible systematic error and conclude that any effects are not significant compared to the statistical errors we quote. Where they overlap we cross-correlate the ACT and the South Pole Telescope (APT) maps and show they are consistent. The measurements of higher-order peaks in the CMB power spectrum provide an additional test of the ACDM cosmological model, and help constrain extensions beyond the standard model. The small angular scale power sped rum also provides constraining power on the Sunyaev-Zel'clovich effects and extragalactic foregrounds. We also present a measurement of the CMB gravitational lensing convergence power spectrum at 4.6 sigma detection significance. C1 [Das, Sudeep] Argonne Natl Lab, Lemont, IL 60439 USA. [Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA. [Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Louis, Thibaut; Addison, Graeme E.; Calabrese, Erminia; Dunkley, Joanna] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Nolta, Michael R.; Bond, J. Richard; Hajian, Amir; Hincks, Adam D.; Sievers, Jonathan L.; Switzer, Eric R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Addison, Graeme E.; Battistelli, Elia S.; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Crichton, Devin; Gralla, Megan; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Devlin, Mark J.; Dicker, Simon; Marsden, Danica; Reese, Erik D.; Schmitt, Benjamin L.; Thornton, Robert] Univ Penn, Dept Astron & Astrophys, Philadelphia, PA 19104 USA. [Duenner, Rolando] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Fowler, Joseph W.; Niemack, Michael D.; Swetz, Daniel S.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Fowler, Joseph W.; Niemack, Michael D.; Page, Lyman A.; Sherwin, Blake D.; Sievers, Jonathan L.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Hasselfield, Matthew; Hlozek, Renee; Marriage, Tobias A.; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Hilton, Matt] Univ Nottingham, Sch Phys & Astron, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England. [Hilton, Matt; Moodley, Kavilan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Huffenberger, Kevin M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. [Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Marsden, Danica] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. [Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Sehgal, Neelima] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Thornton, Robert] West Chester Univ Pennsylvania, Dept Phys, W Chester, PA 19383 USA. [Trac, Hy] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Das, S (reprint author), Argonne Natl Lab, 9700 S Cass Ave, Lemont, IL 60439 USA. EM sudeepphys@gmail.com RI Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012; OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451; Huffenberger, Kevin/0000-0001-7109-0099; Menanteau, Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074 FU U.S. National Science Foundation [AST-0408698, AST-0965625]; ACT project [PHY-0855887, PHY-1214379]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation (CFI) award; Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT); CFI; Compute Canada; Government of Ontario; Ontario Research Fund - Research Excellence; University of Toronto; David Schramm Fellowship at Argonne National Laboratory; Berkeley Center for Cosmological Physics fellowship; FONDECYT grant; BASAL grant FX This work was supported by the U.S. National Science Foundation through awards AST-0408698 and AST-0965625 for the ACT project, as well as awards PHY-0855887 and PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to ITBC. ACT operates in the Parque Astronomico Atacama in northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT). Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund - Research Excellence; and the University of Toronto. SD acknowledges support from the David Schramm Fellowship at Argonne National Laboratory and the Berkeley Center for Cosmological Physics fellowship. RD acknowledges support from FONDECYT and BASAL grants. NR 47 TC 111 Z9 111 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD APR PY 2014 IS 4 AR 014 DI 10.1088/1475-7516/2014/04/014 PG 36 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AF1TK UT WOS:000334496500014 ER PT J AU Sears, DWG AF Sears, Derek W. G. TI Oral histories in meteoritics and planetary science - XXII: John T. Wasson SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID IRON METEORITES; CHONDRITES; ORIGIN; CHONDRULES; GERMANIUM; GALLIUM; MAGMA; MELT AB Abstract In this interview, John Wasson (Fig. ) describes his childhood and undergraduate years in Arkansas and his desire to pursue nuclear chemistry as a graduate student at MIT. Upon graduation, John spent time in Munich (Technische Hochschule), the Air Force Labs in Cambridge, MA, and a sabbatical at the University of Bern where he developed his interests in meteorites. Upon obtaining his faculty position at UCLA, John established a neutron activation laboratory and began a long series of projects on the bulk compositions of iron meteorites and chondrites. He developed the chemical classification scheme for iron meteorites, gathered a huge set of iron meteorite compositional data with resultant insights into their formation, and documented the refractory and moderately volatile element trends that characterize the chondrites and chondrules. He also spent several years studying field relations and compositions of layered tektites from Southeast Asia, proposing an origin by radiant heating from a mega-Tunguska explosion. Recently, John has explored oxygen isotope patterns in meteorites and their constituents believing the oxygen isotope results to be some of the most important discoveries in cosmochemistry. John also describes the role of postdoctoral colleagues and their important work, his efforts in the reorganization and modernization of the Meteoritical Society, his contributions in reshaping the journal Meteoritics, and how, with UCLA colleagues, he organized two meetings of the society. John Wasson earned the Leonard Medal of the Meteoritical Society in 1992 and the J. Lawrence Smith Medal of the National Academy in 2003. C1 NASA, Space Sci & Astrobiol Div, Bay Area Environm Res Inst, Ames Res Ctr, Mountain View, CA 94035 USA. RP Sears, DWG (reprint author), NASA, Space Sci & Astrobiol Div, Bay Area Environm Res Inst, Ames Res Ctr, MS245-3, Mountain View, CA 94035 USA. EM derek.sears@nasa.gov FU NASA FX This interview was recorded on February 6th, 2013, and edited by the author and JW. I am grateful to NASA for financial support and to John Friedrich and Hazel Sears for reviews, and Hazel also for proofing. NR 21 TC 0 Z9 0 U1 1 U2 9 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 APR PY 2014 VL 49 IS 4 BP 706 EP 721 DI 10.1111/maps.12266 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AF4KG UT WOS:000334680200013 ER PT J AU Nicolau, E Fonseca, JJ Rodriguez-Martinez, JA Richardson, TMJ Flynn, M Griebenow, K Cabrera, CR AF Nicolau, Eduardo Fonseca, Jose J. Rodriguez-Martinez, Jose A. Richardson, Tra-My Justine Flynn, Michael Griebenow, Kai Cabrera, Carlos R. TI Evaluation of a Urea Bioelectrochemical System for Wastewater Treatment Processes SO ACS SUSTAINABLE CHEMISTRY & ENGINEERING LA English DT Article DE Resource recovery; Water reclamation; Urea degradation; Electrochemical cell; Bioreactor ID AMMONIA ELECTROLYSIS; HYDROGEN-PRODUCTION; RECLAMATION; DEGRADATION; CREATININE; OXIDATION; PLATINUM; OSMOSIS; PHENOL AB Due to the high cost of delivering supplies to space, the recovery of potable water from spacecraft wastewater is critical for life support of crewmembers in short- and long-term missions. It is estimated that in future long-term space missions, human wastes such as urine will contribute more than 50% of the total waste. Thus, we will demonstrate how unused components, such as urea, can be recovered and reused in wastewater recycling processes. In this system, a urea bioreactor (GAC-urease) converts urea to ammonia. Then, an electrochemical cell converts the ammonia to power. The combined system is referred to as the Urea Bioreactor Electrochemical (UBE) unit. The results of this research showed the feasibility of interfacing wastewater-recycling processes with bioelectrochemical systems to achieve water recycling while reusing useful resources. The UBE systems removed > 80% of organic carbons and converted approximately 86% of the urea to ammonia. Therefore, the concept herein proposed has the potential to be used in water recycling applications with emphasis in contaminant recovery from wastewater for useful resources and energy. C1 [Nicolau, Eduardo; Fonseca, Jose J.; Rodriguez-Martinez, Jose A.; Griebenow, Kai; Cabrera, Carlos R.] Univ Puerto Rico, Dept Chem, San Juan, PR 00931 USA. [Nicolau, Eduardo; Fonseca, Jose J.; Rodriguez-Martinez, Jose A.; Griebenow, Kai; Cabrera, Carlos R.] Univ Puerto Rico, NASA Ctr Adv Nanoscale Mat, San Juan, PR 00931 USA. [Nicolau, Eduardo; Cabrera, Carlos R.] Univ Puerto Rico, Sect El Cinco, San Juan, PR 00926 USA. [Richardson, Tra-My Justine; Flynn, Michael] NASA, Bioengn Branch, Ames Res Ctr, Mountain View, CA 94036 USA. RP Nicolau, E (reprint author), Univ Puerto Rico, Dept Chem, Rio Piedras Campus,POB 23346, San Juan, PR 00931 USA. EM eduardo.nicolau@upr.edu; carlos.cabrera2@upr.edu RI Rodriguez-Martinez, Jose/F-3554-2010; OI Rodriguez-Martinez, Jose/0000-0002-1191-2887; Cabrera, Carlos/0000-0002-3342-8666 FU NASA Center for Advanced Nanoscale Materials [NNX08BA48A, NNX13AD20A]; NASA Graduate Student Researchers Program [NNX08AV42H] FX This work was financially supported in part by the NASA Center for Advanced Nanoscale Materials under Grant NNX08BA48A, NNX13AD20A, and the NASA Graduate Student Researchers Program under Grant NNX08AV42H. The authors are also grateful to David Beeler for comments and editing and Kevin Howard. NR 26 TC 3 Z9 3 U1 4 U2 51 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 2168-0485 J9 ACS SUSTAIN CHEM ENG JI ACS Sustain. Chem. Eng. PD APR PY 2014 VL 2 IS 4 BP 749 EP 754 DI 10.1021/sc400342x PG 6 WC Chemistry, Multidisciplinary; GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Engineering, Chemical SC Chemistry; Science & Technology - Other Topics; Engineering GA AE6IA UT WOS:000334092600026 ER PT J AU Armstrong, JC Barnes, R Domagal-Goldman, S Breiner, J Quinn, TR Meadows, VS AF Armstrong, J. C. Barnes, R. Domagal-Goldman, S. Breiner, J. Quinn, T. R. Meadows, V. S. TI Effects of Extreme Obliquity Variations on the Habitability of Exoplanets SO ASTROBIOLOGY LA English DT Article ID PLANET-PLANET SCATTERING; MAIN-SEQUENCE STARS; CLIMATE MODEL; ECCENTRICITY; ZONE; STABILIZATION; CATALOG; SYSTEMS; EARTH AB We explore the impact of obliquity variations on planetary habitability in hypothetical systems with high mutual inclination. We show that large-amplitude, high-frequency obliquity oscillations on Earth-like exoplanets can suppress the ice-albedo feedback, increasing the outer edge of the habitable zone. We restricted our exploration to hypothetical systems consisting of a solar-mass star, an Earth-mass planet at 1 AU, and 1 or 2 larger planets. We verified that these systems are stable for 10(8) years with N-body simulations and calculated the obliquity variations induced by the orbital evolution of the Earth-mass planet and a torque from the host star. We ran a simplified energy balance model on the terrestrial planet to assess surface temperature and ice coverage on the planet's surface, and we calculated differences in the outer edge of the habitable zone for planets with rapid obliquity variations. For each hypothetical system, we calculated the outer edge of habitability for two conditions: (1) the full evolution of the planetary spin and orbit and (2) the eccentricity and obliquity fixed at their average values. We recovered previous results that higher values of fixed obliquity and eccentricity expand the habitable zone, but we also found that obliquity oscillations further expand habitable orbits in all cases. Terrestrial planets near the outer edge of the habitable zone may be more likely to support life in systems that induce rapid obliquity oscillations as opposed to fixed-spin planets. Such planets may be the easiest to directly characterize with space-borne telescopes. Key Words: Exoplanets-Habitable zone-Energy balance models. Astrobiology 14, 277-291. C1 [Armstrong, J. C.] Weber State Univ, Dept Phys, Ogden, UT 84408 USA. [Barnes, R.; Breiner, J.; Quinn, T. R.; Meadows, V. S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Domagal-Goldman, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Armstrong, JC (reprint author), Weber State Univ, Dept Phys, Ogden, UT 84408 USA. EM jcarmstrong@weber.edu FU NASA Astrobiology Institute's Virtual Planetary Lab lead team; NAI Director's Discretionary Fund FX This work was supported by the NASA Astrobiology Institute's Virtual Planetary Lab lead team and an award from the NAI Director's Discretionary Fund. NR 44 TC 16 Z9 16 U1 2 U2 12 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD APR 1 PY 2014 VL 14 IS 4 BP 277 EP 291 DI 10.1089/ast.2013.1129 PG 15 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AF0UX UT WOS:000334430700002 PM 24611714 ER PT J AU Marlow, JJ LaRowe, DE Ehlmann, BL Amend, JP Orphan, VJ AF Marlow, Jeffrey J. LaRowe, Douglas E. Ehlmann, Bethany L. Amend, Jan P. Orphan, Victoria J. TI The Potential for Biologically Catalyzed Anaerobic Methane Oxidation on Ancient Mars SO ASTROBIOLOGY LA English DT Article ID PARTIAL MOLAL PROPERTIES; YELLOWSTONE-NATIONAL-PARK; SEA HYDROTHERMAL SYSTEMS; MEXICO COLD SEEPS; HIGH-PRESSURES; SULFATE REDUCTION; THERMODYNAMIC PROPERTIES; GEOCHEMICAL CONSTRAINTS; TRANSPORT-PROPERTIES; MERIDIANI-PLANUM AB This study examines the potential for the biologically mediated anaerobic oxidation of methane (AOM) coupled to sulfate reduction on ancient Mars. Seven distinct fluids representative of putative martian groundwater were used to calculate Gibbs energy values in the presence of dissolved methane under a range of atmospheric CO2 partial pressures. In all scenarios, AOM is exergonic, ranging from -31 to -135 kJ/mol CH4. A reaction transport model was constructed to examine how environmentally relevant parameters such as advection velocity, reactant concentrations, and biomass production rate affect the spatial and temporal dependences of AOM reaction rates. Two geologically supported models for ancient martian AOM are presented: a sulfate-rich groundwater with methane produced from serpentinization by-products, and acid-sulfate fluids with methane from basalt alteration. The simulations presented in this study indicate that AOM could have been a feasible metabolism on ancient Mars, and fossil or isotopic evidence of this metabolic pathway may persist beneath the surface and in surface exposures of eroded ancient terrains. Key Words: Mars-Methanotrophy-Methane. Astrobiology 14, 292-307. C1 [Marlow, Jeffrey J.; Ehlmann, Bethany L.; Orphan, Victoria J.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [LaRowe, Douglas E.; Amend, Jan P.] Univ So Calif, Dept Earth Sci, Los Angeles, CA USA. [Ehlmann, Bethany L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Amend, Jan P.] Univ So Calif, Dept Biol Sci, Los Angeles, CA 90089 USA. RP Marlow, JJ (reprint author), CALTECH, Div Geol & Planetary Sci, 1200 E Calif Ave,MC 100-23, Pasadena, CA 91125 USA. EM jjmarlow@caltech.edu RI Orphan, Victoria/K-1002-2014 OI Orphan, Victoria/0000-0002-5374-6178 FU NETL-National Academy of Sciences Methane Hydrate Research Fellowship; Life Underground NASA Astrobiology Institute (NAI) based at USC FX J.J.M. would like to thank Dawn Cardace, Andrew Dale, and Megan Newcombe for helpful discussion and consultation and the NETL-National Academy of Sciences Methane Hydrate Research Fellowship for financial support. D.E.L. and J.P.A. would like to acknowledge financial support from the Life Underground NASA Astrobiology Institute (NAI) based at USC. V.J.O. acknowledges the Penn State Astrobiology Research Center NAI. NR 149 TC 2 Z9 2 U1 1 U2 31 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD APR 1 PY 2014 VL 14 IS 4 BP 292 EP 307 DI 10.1089/ast.2013.1078 PG 16 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AF0UX UT WOS:000334430700003 PM 24684241 ER PT J AU Russell, MJ Barge, LM Bhartia, R Bocanegra, D Bracher, PJ Branscomb, E Kidd, R McGlynn, S Meier, DH Nitschke, W Shibuya, T Vance, S White, L Kanik, I AF Russell, Michael J. Barge, Laura M. Bhartia, Rohit Bocanegra, Dylan Bracher, Paul J. Branscomb, Elbert Kidd, Richard McGlynn, Shawn Meier, David H. Nitschke, Wolfgang Shibuya, Takazo Vance, Steve White, Lauren Kanik, Isik TI The Drive to Life on Wet and Icy Worlds SO ASTROBIOLOGY LA English DT Article ID CITY HYDROTHERMAL FIELD; RESPIRATORY COMPLEX I; INSOLUBLE ORGANIC-MATTER; EARTHS EARLY ATMOSPHERE; MID-ATLANTIC RIDGE; NUVVUAGITTUQ SUPRACRUSTAL BELT; MINERAL INDUCED FORMATION; IRON-SULFUR CLUSTERS; SULFATE GREEN RUST; PREBIOTIC SYNTHESIS AB This paper presents a reformulation of the submarine alkaline hydrothermal theory for the emergence of life in response to recent experimental findings. The theory views life, like other self-organizing systems in the Universe, as an inevitable outcome of particular disequilibria. In this case, the disequilibria were two: (1) in redox potential, between hydrogen plus methane with the circuit-completing electron acceptors such as nitrite, nitrate, ferric iron, and carbon dioxide, and (2) in pH gradient between an acidulous external ocean and an alkaline hydrothermal fluid. Both CO2 and CH4 were equally the ultimate sources of organic carbon, and the metal sulfides and oxyhydroxides acted as protoenzymatic catalysts. The realization, now 50 years old, that membrane-spanning gradients, rather than organic intermediates, play a vital role in life's operations calls into question the idea of "prebiotic chemistry." It informs our own suggestion that experimentation should look to the kind of nanoengines that must have been the precursors to molecular motors-such as pyrophosphate synthetase and the like driven by these gradients-that make life work. It is these putative free energy or disequilibria converters, presumably constructed from minerals comprising the earliest inorganic membranes, that, as obstacles to vectorial ionic flows, present themselves as the candidates for future experiments. Key Words: Methanotrophy-Origin of life. Astrobiology 14, 308-343. C1 [Russell, Michael J.; Barge, Laura M.; Bhartia, Rohit; Kidd, Richard; Meier, David H.; Vance, Steve; White, Lauren; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bocanegra, Dylan] Art Ctr Bridge, Pasadena, CA USA. [Bracher, Paul J.] CALTECH, Beckman Inst, Pasadena, CA 91109 USA. [Bracher, Paul J.] St Louis Univ, Dept Chem, St Louis, MO 63103 USA. [Branscomb, Elbert] UIUC, Inst Genom Biol, Champaign, IL USA. [McGlynn, Shawn] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91109 USA. [Nitschke, Wolfgang] CNRS, Bioenerget & Ingn Prot UPR9036, IFR88, Marseille, France. [Shibuya, Takazo] Japan Agcy Marine Earth Sci & Technol JAMSTEC, Precambrian Ecosyst Lab PEL, Yokosuka, Kanagawa, Japan. [White, Lauren] Univ Calif Santa Barbara, Dept Chem & Biochem, Santa Barbara, CA 93106 USA. RP Russell, MJ (reprint author), CALTECH, Jet Prop Lab, Chem & Astrobiol Sect 3225, MS 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mrussell@jpl.nasa.gov OI Nitschke, Wolfgang/0000-0003-2084-3032; Bracher, Paul/0000-0001-5769-8364 FU National Aeronautics and Space Administration; NASA Exobiology and Evolutionary Biology award [NNH06ZDA001N]; NASA Astrobiology Institute (Icy Worlds); NASA Astrobiology Institute (Universal Biology) FX We thank John Allen, Ariel Anbar, Jean Bedard, Billy Brazelton, John Callas, Ivria Doloboff, Kevin Hand, Mickey Honchell, Michael Malaska, Randall Mielke, Ken Nealson, Yuk Yung, and the Thermodynamics, Disequilibrium and Evolution (TDE) NAI Focus Group for discussions, and two anonymous reviewers for their suggestions. The research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration, with support by a NASA Exobiology and Evolutionary Biology award (NNH06ZDA001N) and supported by the NASA Astrobiology Institute (Icy Worlds). E.B. is supported by the NASA Astrobiology Institute (Universal Biology). NR 476 TC 43 Z9 44 U1 22 U2 156 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD APR 1 PY 2014 VL 14 IS 4 BP 308 EP 343 DI 10.1089/ast.2013.1110 PG 36 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AF0UX UT WOS:000334430700004 PM 24697642 ER PT J AU McKay, CP Anbar, AD Porco, C Tsou, P AF McKay, Christopher P. Anbar, Ariel D. Porco, Carolyn Tsou, Peter TI Follow the Plume: The Habitability of Enceladus SO ASTROBIOLOGY LA English DT Article ID SOUTH-POLE; LIFE; ORIGIN; SEARCH; MARS; METHANE; WATER AB The astrobiological exploration of other worlds in our Solar System is moving from initial exploration to more focused astrobiology missions. In this context, we present the case that the plume of Enceladus currently represents the best astrobiology target in the Solar System. Analysis of the plume by the Cassini mission indicates that the steady plume derives from a subsurface liquid water reservoir that contains organic carbon, biologically available nitrogen, redox energy sources, and inorganic salts. Furthermore, samples from the plume jetting out into space are accessible to a low-cost flyby mission. No other world has such well-studied indications of habitable conditions. Thus, the science goals that would motivate an Enceladus mission are more advanced than for any other Solar System body. The goals of such a mission must go beyond further geophysical characterization, extending to the search for biomolecular evidence of life in the organic-rich plume. This will require improved in situ investigations and a sample return. Key Words: Ice-Life detection-Icy moon. Astrobiology 14, 352-355. C1 [McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Anbar, Ariel D.] Arizona State Univ, Tempe, AZ USA. [Porco, Carolyn] Space Sci Inst, CICLOPS, Boulder, CO USA. [Tsou, Peter] Sample Explorat Syst, La Canada Flintridge, CA USA. RP McKay, CP (reprint author), NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA. EM chris.mckay@nasa.gov NR 27 TC 12 Z9 12 U1 7 U2 66 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD APR 1 PY 2014 VL 14 IS 4 BP 352 EP 355 DI 10.1089/ast.2014.1158 PG 4 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AF0UX UT WOS:000334430700006 PM 24684187 ER PT J AU Akrami, Y Fantaye, Y Shafieloo, A Eriksen, HK Hansen, FK Banday, AJ Gorski, KM AF Akrami, Y. Fantaye, Y. Shafieloo, A. Eriksen, H. K. Hansen, F. K. Banday, A. J. Gorski, K. M. TI POWER ASYMMETRY IN WMAP AND PLANCK TEMPERATURE SKY MAPS AS MEASURED BY A LOCAL VARIANCE ESTIMATOR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmic background radiation; cosmology: observations; methods: statistical ID MICROWAVE-ANISOTROPY-PROBE; DIRECTIONAL SPHERICAL WAVELETS; BACKGROUND ANISOTROPY; NON-GAUSSIANITY; VIIH MODELS; ANOMALIES; ISOTROPY; UNIVERSE; FIELD AB We revisit the question of hemispherical power asymmetry in the WMAP and Planck temperature sky maps by measuring the local variance over the sky and on disks of various sizes. For the 2013 Planck sky map we find that none of the 1000 available isotropic Planck "Full Focal Plane" simulations have a larger variance asymmetry than that estimated from the data, suggesting the presence of an anisotropic signature formally significant at least at the 3.3 sigma level. For the WMAP 9 year data we find that 5 out of 1000 simulations have a larger asymmetry. The preferred direction for the asymmetry from the Planck data is (l, b) = (212 degrees, -13 degrees), in good agreement with previous reports of the same hemispherical power asymmetry. C1 [Akrami, Y.; Fantaye, Y.; Eriksen, H. K.; Hansen, F. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Fantaye, Y.] Univ Roma Tor Vergata, Dept Math, Rome, Italy. [Shafieloo, A.] Asia Pacific Ctr Theoret Phys, Pohang 790784, Gyeongbuk, South Korea. [Shafieloo, A.] POSTECH, Dept Phys, Pohang 790784, Gyeongbuk, South Korea. [Banday, A. J.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Banday, A. J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Gorski, K. M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Akrami, Y (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, N-0315 Oslo, Norway. EM yashar.akrami@astro.uio.no; y.t.fantaye@astro.uio.no; arman@apctp.org OI Akrami, Yashar/0000-0002-2407-7956 FU ERC Starting Grant [StG2010-257080]; ERC [277742 Pascal]; Korean Ministry of Education, Science and Technology (MEST); Gyeongsangbuk-Do; Pohang City; National Research Foundation of Korea [NRF-2013R1A1A2013795]; OYI grant from the Norwegian research council FX We thank Claudio Llinares, Eamon M. Scullion, and Amir Hajian for helpful discussions. Y.A. and H.K.E. acknowledge support through the ERC Starting Grant StG2010-257080. Y.F. is supported by ERC Grant 277742 Pascal. A.S. thanks the Korean Ministry of Education, Science and Technology (MEST), Gyeongsangbuk-Do, and Pohang City for the support of the Independent Junior Research Groups at the Asia Pacific Center for Theoretical Physics (APCTP). A.S. would like to acknowledge the support of the National Research Foundation of Korea (NRF-2013R1A1A2013795). F.K.H. acknowledges OYI grant from the Norwegian research council. We acknowledge the use of resources from the Norwegian national super-computing facilities, NOTUR. Maps and results have been derived using the HEALPix (http://healpix.jpl.nasa.gov) software package developed by Gorski et al. (2005). NR 51 TC 69 Z9 69 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 1 PY 2014 VL 784 IS 2 AR L42 DI 10.1088/2041-8205/784/2/L42 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD5ZX UT WOS:000333333400025 ER PT J AU Bellm, EC Barriere, NM Bhalerao, V Boggs, SE Cenko, SB Christensen, FE Craig, WW Forster, K Fryer, CL Hailey, CJ Harrison, FA Horesh, A Kouveliotou, C Madsen, KK Miller, JM Ofek, EO Perley, DA Rana, VR Reynolds, SP Stern, D Tomsick, JA Zhang, WW AF Bellm, Eric C. Barriere, Nicolas M. Bhalerao, Varun Boggs, Steven E. Cenko, S. Bradley Christensen, Finn E. Craig, William W. Forster, Karl Fryer, Chris L. Hailey, Charles J. Harrison, Fiona A. Horesh, Assaf Kouveliotou, Chryssa Madsen, Kristin K. Miller, Jon M. Ofek, Eran O. Perley, Daniel A. Rana, Vikram R. Reynolds, Stephen P. Stern, Daniel Tomsick, John A. Zhang, William W. TI X-RAY SPECTRAL COMPONENTS OBSERVED IN THE AFTERGLOW OF GRB 130925A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma-ray burst: individual (GRB 130925A) ID MASSIVE BLACK-HOLE; SUPERNOVA; BURSTS; STAR; EMISSION; SEARCH; SIGNATURES; COLLAPSARS; ACCRETION; OUTBURST AB We have identified spectral features in the late-time X-ray afterglow of the unusually long, slow-decaying GRB 130925A using NuSTAR, Swift/X-Ray Telescope, and Chandra. A spectral component in addition to an absorbed power law is required at >4 sigma significance, and its spectral shape varies between two observation epochs at 2 x 10(5) and 10(6) s after the burst. Several models can fit this additional component, each with very different physical implications. A broad, resolved Gaussian absorption feature of several keV width improves the fit, but it is poorly constrained in the second epoch. An additive blackbody or second power-law component provide better fits. Both are challenging to interpret: the blackbody radius is near the scale of a compact remnant (10(8) cm), while the second power-law component requires an unobserved high-energy cutoff in order to be consistent with the non-detection by Fermi/Large Area Telescope. C1 [Bellm, Eric C.; Forster, Karl; Harrison, Fiona A.; Madsen, Kristin K.; Perley, Daniel A.; Rana, Vikram R.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Barriere, Nicolas M.; Boggs, Steven E.; Craig, William W.; Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bhalerao, Varun] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Cenko, S. Bradley; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Fryer, Chris L.] Los Alamos Natl Lab, CCS 2, Los Alamos, NM 87545 USA. [Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Horesh, Assaf; Ofek, Eran O.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Astrophys Off ZP12, Huntsville, AL 35812 USA. [Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Reynolds, Stephen P.] NC State Univ, Dept Phys, Raleigh, NC 27695 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bellm, EC (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. EM ebellm@caltech.edu RI Boggs, Steven/E-4170-2015; Horesh, Assaf/O-9873-2016; OI Boggs, Steven/0000-0001-9567-4224; Horesh, Assaf/0000-0002-5936-1156; Bhalerao, Varun/0000-0002-6112-7609; Madsen, Kristin/0000-0003-1252-4891; Rana, Vikram/0000-0003-1703-8796 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration FX This work was supported under NASA contract No. NNG08FD60C and uses data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations team for executing the target of opportunity observations. This research has used the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). These results are based in part on observations made by the Chandra X-ray Observatory. We thank the Chandra director for granting discretionary time and the Chandra team for prompt execution of the observations. NR 47 TC 10 Z9 10 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 1 PY 2014 VL 784 IS 2 AR L19 DI 10.1088/2041-8205/784/2/L19 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD5ZX UT WOS:000333333400002 ER PT J AU Burgess, JM Preece, RD Ryde, F Veres, P Meszaros, P Connaughton, V Briggs, M Pe'er, A Iyyani, S Goldstein, A Axelsson, M Baring, MG Bhat, PN Byrne, D Fitzpatrick, G Foley, S Kocevski, D Omodei, N Paciesas, WS Pelassa, V Kouveliotou, C Xiong, SL Yu, HF Zhang, BB Zhu, S AF Burgess, J. Michael Preece, Robert D. Ryde, Felix Veres, Peter Meszaros, Peter Connaughton, Valerie Briggs, Michael Pe'er, Asaf Iyyani, Shabnam Goldstein, Adam Axelsson, Magnus Baring, Matthew G. Bhat, P. N. Byrne, David Fitzpatrick, Gerard Foley, Suzanne Kocevski, Daniel Omodei, Nicola Paciesas, William S. Pelassa, Veronique Kouveliotou, Chryssa Xiong, Shaolin Yu, Hoi-Fung Zhang, Binbin Zhu, Sylvia TI AN OBSERVED CORRELATION BETWEEN THERMAL AND NON-THERMAL EMISSION IN GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma-ray burst: general; radiation mechanisms: non-thermal; radiation mechanisms: thermal ID FERMI-LAT OBSERVATIONS; PHOTOSPHERIC EMISSION; SPECTRAL CATALOG; PROMPT EMISSION; GRB OUTFLOWS; MODEL; DISSIPATION; EFFICIENCY; ACCELERATION; RECONNECTION AB Recent observations by the Fermi Gamma-ray Space Telescope have confirmed the existence of thermal and non-thermal components in the prompt photon spectra of some gamma-ray bursts (GRBs). Through an analysis of six bright Fermi GRBs, we have discovered a correlation between the observed photospheric and non-thermal gamma-ray emission components of several GRBs using a physical model that has previously been shown to be a good fit to the Fermi data. From the spectral parameters of these fits we find that the characteristic energies, E-p and kT, of these two components are correlated via the relation E-p proportional to T-alpha which varies from GRB to GRB. We present an interpretation in which the value of the index alpha indicates whether the jet is dominated by kinetic or magnetic energy. To date, this jet composition parameter has been assumed in the modeling of GRB outflows rather than derived from the data. C1 [Burgess, J. Michael; Preece, Robert D.] Univ Alabama, Dept Space Sci, Huntsville, AL 35899 USA. [Burgess, J. Michael; Preece, Robert D.; Connaughton, Valerie; Briggs, Michael; Bhat, P. N.; Pelassa, Veronique; Xiong, Shaolin; Zhang, Binbin] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Burgess, J. Michael; Ryde, Felix; Iyyani, Shabnam; Axelsson, Magnus] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Ryde, Felix; Iyyani, Shabnam; Axelsson, Magnus] AlbaNova, Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Veres, Peter; Meszaros, Peter] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Pe'er, Asaf] Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland. [Iyyani, Shabnam; Kouveliotou, Chryssa] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden. [Goldstein, Adam] NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Axelsson, Magnus] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Baring, Matthew G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Byrne, David; Fitzpatrick, Gerard; Foley, Suzanne] Univ Coll Dublin, Dublin 4, Ireland. [Foley, Suzanne; Yu, Hoi-Fung] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kocevski, Daniel; Omodei, Nicola] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Kocevski, Daniel; Omodei, Nicola] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Paciesas, William S.] Univ Space Res Assoc, Huntsville, AL 35805 USA. [Zhu, Sylvia] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Zhu, Sylvia] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Burgess, JM (reprint author), Univ Alabama, Dept Space Sci, Huntsville, AL 35899 USA. EM jmichaelburgess@gmail.com; rob.preece@nasa.gov; felix@particle.kth.se; veres@gwu.edu; npp@astro.psu.edu RI Zhang, Binbin/C-9035-2013; Iyyani, Shabnam/D-8736-2017; OI Zhang, Binbin/0000-0003-2002-116X; Iyyani, Shabnam/0000-0002-2525-3464; Preece, Robert/0000-0003-1626-7335; Burgess, James/0000-0003-3345-9515; Veres, Peter/0000-0002-2149-9846; Axelsson, Magnus/0000-0003-4378-8785 NR 47 TC 14 Z9 14 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 1 PY 2014 VL 784 IS 2 AR L43 DI 10.1088/2041-8205/784/2/L43 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD5ZX UT WOS:000333333400026 ER PT J AU Furst, F Pottschmidt, K Wilms, J Kennea, J Bachetti, M Bellm, E Boggs, SE Chakrabarty, D Christensen, FE Craig, WW Hailey, CJ Harrison, F Stern, D Tomsick, JA Walton, DJ Zhang, W AF Fuerst, Felix Pottschmidt, Katja Wilms, Joern Kennea, Jamie Bachetti, Matteo Bellm, Eric Boggs, Steven E. Chakrabarty, Deepto Christensen, Finn E. Craig, William W. Hailey, Charles J. Harrison, Fiona Stern, Daniel Tomsick, John A. Walton, Dominic J. Zhang, William TI NuSTAR DISCOVERY OF A CYCLOTRON LINE IN KS 1947+300 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; radiation: dynamics; stars: neutron; X-rays: binaries; X-rays: individual (KS 1947+300) ID X-RAY; COMPTONIZATION MODELS; INTERSTELLAR-MEDIUM; SPECTROSCOPY; KS-1947+300; ENERGY; TELESCOPE; PULSARS; MISSION; RXTE AB We present a spectral analysis of three simultaneous Nuclear Spectroscopy Telescope Array and Swift/XRT observations of the transient Be-neutron star binary KS 1947+300 taken during its outburst in 2013/2014. These broadband observations were supported by Swift/XRT monitoring snapshots every three days, which we use to study the evolution of the spectrum over the outburst. We find strong changes of the power-law photon index, which shows a weak trend of softening with increasing X-ray flux. The neutron star shows very strong pulsations with a period of P approximate to 18.8 s. The 0.8-79 keV broadband spectrum can be described by a power law with an exponential cutoff and a blackbody component at low energies. During the second observation we detect a cyclotron resonant scattering feature at 12.5 keV, which is absent in the phase-averaged spectra of observations 1 and 3. Pulse phase-resolved spectroscopy reveals that the strength of the feature changes strongly with pulse phase and is most prominent during the broad minimum of the pulse profile. At the same phases the line also becomes visible in the first and third observation at the same energy. This discovery implies that KS 1947+300 has a magnetic field strength of B approximate to 1.1 x 10(12)(1 + z) G, which is at the lower end of known cyclotron line sources. C1 [Fuerst, Felix; Bellm, Eric; Harrison, Fiona; Walton, Dominic J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Pottschmidt, Katja] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Pottschmidt, Katja] CRESST, Greenbelt, MD 20771 USA. [Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Wilms, Joern] Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany. [Wilms, Joern] ECAP, D-96049 Bamberg, Germany. [Kennea, Jamie] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Bachetti, Matteo] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France. [Bachetti, Matteo] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Boggs, Steven E.; Craig, William W.; Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Furst, F (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RI Wilms, Joern/C-8116-2013; Boggs, Steven/E-4170-2015; OI Wilms, Joern/0000-0003-2065-5410; Boggs, Steven/0000-0001-9567-4224; Bellm, Eric/0000-0001-8018-5348; Bachetti, Matteo/0000-0002-4576-9337 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; Deutsches Zentrum fur Luft-und Raumfahrt under DLR grant [50 OR 1113] FX We would like to thank Matthias Kuhnel, Ralf Ballhausen, Fritz Schwarm, and Peter Kretschmar for useful discussions. This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of ISIS functions provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/). We thank the Deutsches Zentrum fur Luft-und Raumfahrt for partial support under DLR grant 50 OR 1113. We thank the anonymous referee for useful comments. NR 32 TC 10 Z9 10 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 1 PY 2014 VL 784 IS 2 AR L40 DI 10.1088/2041-8205/784/2/L40 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD5ZX UT WOS:000333333400023 ER PT J AU Yang, B Keane, J Meech, K Owen, T Wainscoat, R AF Yang, Bin Keane, Jacqueline Meech, Karen Owen, Tobias Wainscoat, Richard TI MULTI-WAVELENGTH OBSERVATIONS OF COMET C/2011 L4 (PAN-STARRS) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE comets: individual (C/2011 L4); infrared: planetary systems; Oort Cloud ID DUST RELEASE RATES; HALE-BOPP; WATER ICE; MU-M; GAS; GRAINS; SPECTROGRAPH; OUTBURSTS; DISTANCE; NUCLEI AB The dynamically new comet C/2011 L4 (Pan-STARRS) is one of the brightest comets observed since the great comet C/1995 O1 (Hale-Bopp). Here, we present our multi-wavelength observations of C/2011 L4 during its in-bound passage to the inner solar system. A strong absorption band of water ice at 2.0 mu m was detected in the near-infrared spectra, obtained with the 8 m Gemini-North and 3 m Infrared Telescope Facility Telescopes. The companion 1.5 mu m band of water ice, however, was not observed. Spectral modeling shows that the absence of the 1.5 mu m feature can be explained by the presence of sub-micron-sized fine ice grains. No gas lines (i.e., CN, HCN, or CO) were observed pre-perihelion in either the optical or the submillimeter. We derived 3 sigma upper limits for the CN and CO production rates. The comet exhibited a very strong continuum in the optical and its slope seemed to become redder as the comet approached the Sun. Our observations suggest that C/2011 L4 is an unusually dust-rich comet with a dust-to-gas mass ratio >4. C1 [Yang, Bin; Keane, Jacqueline; Meech, Karen] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA. [Yang, Bin] European So Observ, Santiago 19, Chile. [Meech, Karen; Owen, Tobias; Wainscoat, Richard] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Yang, B (reprint author), Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA. EM yangbin@ifa.hawaii.edu FU NASA Astrobiology Institute through the Office of Space Science [NNA08DA77A]; NSF [AST-1010059] FX We thank Jason X. Prochaska and Kate Rubin for helping us with the GMOS data reduction and Zahed Wahhaj and David Jewitt for valuable discussions and constructive suggestions. We thank the JCMT staff for their assistance. B.Y. was supported by the NASA Astrobiology Institute under Cooperative Agreement No. NNA08DA77A issued through the Office of Space Science. Work was supported in part by NSF grant AST-1010059. NR 49 TC 8 Z9 8 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 APR 1 PY 2014 VL 784 IS 2 AR L23 DI 10.1088/2041-8205/784/2/L23 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD5ZX UT WOS:000333333400006 ER PT J AU Chen, CH Mittal, T Kuchner, M Forrest, WJ Lisse, CM Manoj, P Sargent, BA Watson, DM AF Chen, Christine H. Mittal, Tushar Kuchner, Marc Forrest, William J. Lisse, Carey M. Manoj, P. Sargent, Benjamin A. Watson, Dan M. TI THE SPITZER INFRARED SPECTROGRAPH DEBRIS DISK CATALOG. I. CONTINUUM ANALYSIS OF UNRESOLVED TARGETS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; circumstellar matter; infrared: stars; zodiacal dust ID MAIN-SEQUENCE STARS; M-CIRCLE-DOT; SOLAR-TYPE STARS; LOW-MASS STARS; T-TAURI STARS; A-TYPE STARS; STELLAR KINEMATIC GROUPS; PICTORIS MOVING GROUP; SUN-LIKE STARS; MULTIBAND IMAGING PHOTOMETER AB During the Spitzer Space Telescope cryogenic mission, Guaranteed Time Observers, Legacy Teams, and General Observers obtained Infrared Spectrograph (IRS) observations of hundreds of debris disk candidates. We calibrated the spectra of 571 candidates, including 64 new IRAS and Multiband Imaging Photometer for Spitzer (MIPS) debris disks candidates, modeled their stellar photospheres, and produced a catalog of excess spectra for unresolved debris disks. For 499 targets with IRS excess but without strong spectral features (and a subset of 420 targets with additional MIPS 70 mu m observations), we modeled the IRS (and MIPS data) assuming that the dust thermal emission was well-described using either a one- or two-temperature blackbody model. We calculated the probability for each model and computed the average probability to select among models. We found that the spectral energy distributions for the majority of objects (similar to 66%) were better described using a two-temperature model with warm (T-gr similar to 100-500 K) and cold (T-gr similar to 50-150 K) dust populations analogous to zodiacal and Kuiper Belt dust, suggesting that planetary systems are common in debris disks and zodiacal dust is common around host stars with ages up to similar to 1 Gyr. We found that younger stars generally have disks with larger fractional infrared luminosities and higher grain temperatures and that higher-mass stars have disks with higher grain temperatures. We show that the increasing distance of dust around debris disks is inconsistent with self-stirred disk models, expected if these systems possess planets at 30-150 AU. Finally, we illustrate how observations of debris disks may be used to constrain the radial dependence of material in the minimum mass solar nebula. C1 [Chen, Christine H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Mittal, Tushar] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Kuchner, Marc] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Forrest, William J.; Watson, Dan M.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Manoj, P.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Sargent, Benjamin A.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. [Sargent, Benjamin A.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA. RP Chen, CH (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM cchen@stsci.edu RI Lisse, Carey/B-7772-2016 OI Lisse, Carey/0000-0002-9548-1526 FU STScI Director's Discretionary Fund; NASA; NSF; JPL/Caltech FX We would like to thank Chas Beichman, Mike Fitzgerald, Laura Hanley, Hannah Jang-Condell, Margaret Moerchen, our referee (Farisa Morales), and our editor (Eric Feigelson) for their helpful comments and suggestions. This work is based on observations made with the Spitzer Space Telescope, which is operated by JPL/Caltech under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech and by the STScI Director's Discretionary Fund. This research made use of the SIMBAD database, operated at CDS, Strasbourg, France, and data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/Caltech, funded by NASA and the NSF. NR 192 TC 61 Z9 61 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2014 VL 211 IS 2 AR 25 DI 10.1088/0067-0049/211/2/25 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE5KT UT WOS:000334028600009 ER PT J AU Heays, AN Ajello, JM Aguilar, A Lewis, BR Gibson, ST AF Heays, A. N. Ajello, J. M. Aguilar, A. Lewis, B. R. Gibson, S. T. TI THE HIGH-RESOLUTION EXTREME-ULTRAVIOLET SPECTRUM OF N-2 BY ELECTRON IMPACT SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE line: identification; minor planets, asteroids: individual (Titan); molecular data; planets and satellites: atmospheres; radiation mechanisms: non-thermal; ultraviolet: general ID VUV ABSORPTION-SPECTRUM; EMISSION CROSS-SECTION; MOLECULAR NITROGEN; DIATOMIC-MOLECULES; RYDBERG STATES; DISSOCIATIVE EXCITATION; SCATTERING-THEORY; EXCITED-STATES; PREDISSOCIATION; SPECTROSCOPY AB We have analyzed high-resolution (FWHM = 0.2 angstrom) extreme-ultraviolet (EUV, 800-1350 angstrom) laboratory emission spectra of molecular nitrogen excited by an electron impact at 20 and 100 eV under (mostly) optically thin, single-scattering experimental conditions. A total of 491 emission features were observed from N-2 electronic-vibrational transitions and atomic Ni and NII multiplets and their emission cross sections were measured. Molecular emission was observed at vibrationally excited ground-state levels as high as v '' = 17, from the a(1)Pi(g), b(1)Pi(u), and b '(1)Sigma(+)(u) excited valence states and the Rydberg series c '(n+1) (1)Sigma u(+), c(n) (1)Pi(u), and O-n (1)Pi(u) for n between 3 and 9. The frequently blended molecular emission bands were disentangled with the aid of a sophisticated and predictive quantum-mechanical model of excited states that includes the strong coupling between valence and Rydberg electronic states and the effects of predissociation. Improved model parameters describing electronic transition moments were obtained from the experiment and allowed for a reliable prediction of the vibrationally summed electronic emission cross section, including an extrapolation to unobserved emission bands and those that are optically thick in the experimental spectra. Vibrationally dependent electronic excitation functions were inferred from a comparison of emission features following 20 and 100 eV electron-impact collisional excitation. The electron-impact-induced fluorescence measurements are compared with Cassini Ultraviolet Imaging Spectrograph observations of emissions from Titan's upper atmosphere. C1 [Heays, A. N.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Heays, A. N.; Lewis, B. R.; Gibson, S. T.] Australian Natl Univ, Res Sch Phys & Engn, Canberra, ACT 0200, Australia. [Ajello, J. M.; Aguilar, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Heays, AN (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM heays@strw.leidenuniv.nl OI Heays, Alan/0000-0002-7716-9192 FU National Aeronautics and Space Administration (NASA); NASA's Cassini Data Analysis Program; Geospace program; National Science Foundation; Astronomy and Physics Research and Analysis Program; Space Physics Program Offices; Australian Research Council Discovery Program [DP0558962, DP0773050]; Netherlands Organisation for Scientific Research (NWO) [648.000.002]; Planetary Atmospheres program FX This work was performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech), under a contract with the National Aeronautics and Space Administration (NASA). We gratefully acknowledge financial support through NASA's Cassini Data Analysis Program, Geospace and Planetary Atmospheres programs, the National Science Foundation, the Astronomy and Physics Research and Analysis Program, and Space Physics Program Offices. Calculations of the N2 photodissociation cross sections were supported by the Australian Research Council Discovery Program, through grant Nos. DP0558962 and DP0773050. A. H. was supported by grant number 648.000.002 from the Netherlands Organisation for Scientific Research (NWO) via the Dutch Astrochemistry Network. NR 101 TC 8 Z9 8 U1 1 U2 25 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 APR PY 2014 VL 211 IS 2 DI 10.1088/0067-0049/211/2/28 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE5KT UT WOS:000334028600012 ER PT J AU Subramanian, A Jochum, M Miller, AJ Neale, R Seo, H Waliser, D Murtugudde, R AF Subramanian, Aneesh Jochum, Markus Miller, Arthur J. Neale, Richard Seo, Hyodae Waliser, Duane Murtugudde, Raghu TI The MJO and global warming: a study in CCSM4 SO CLIMATE DYNAMICS LA English DT Article DE MJO; Climate change; CCSM4 ID MADDEN-JULIAN OSCILLATION; PRECIPITATION EXTREMES; ATMOSPHERIC CIRCULATION; EQUATORIAL PACIFIC; HYDROLOGICAL CYCLE; CLIMATE-CHANGE; IDEALIZED GCM; WIDE-RANGE; EL-NINO; ENSO AB The change in Madden-Julian oscillation (MJO) amplitude and variance in response to anthropogenic climate change is assessed in the 1A degrees nominal resolution community climate system model, version 4 (CCSM4), which has a reasonable representation of the MJO characteristics both dynamically and statistically. The twentieth century CCSM4 run is compared with the warmest twenty-first century projection (representative concentration pathway 8.5, or RCP8.5). The last 20 years of each simulation are compared in their MJO characteristics, including spatial variance distributions of winds, precipitation and outgoing longwave radiation, histograms of event amplitude, phase and duration, and composite maps of phases. The RCP8.5 run exhibits increased variance in intraseasonal precipitation, larger-amplitude MJO events, stronger MJO rainfall in the central and eastern tropical Pacific, and a greater frequency of MJO occurrence for phases corresponding to enhanced rainfall in the Indian Ocean sector. These features are consistent with the concept of an increased magnitude for the hydrological cycle under greenhouse warming conditions. Conversely, the number of active MJO days decreases and fewer weak MJO events occur in the future climate state. These results motivate further study of these changes since tropical rainfall variability plays such an important role in the region's socio-economic well being. C1 [Subramanian, Aneesh; Miller, Arthur J.] UCSD, SIO, La Jolla, CA 92037 USA. [Jochum, Markus] Niels Bohr Inst, Climate & Geophys Div, DK-2100 Copenhagen, Denmark. [Neale, Richard] Natl Ctr Atmospher Res, Climate & Global Dynam Div, Boulder, CO 80307 USA. [Seo, Hyodae] Woods Hole Oceanog Inst, Dept Phys Oceanog, Woods Hole, MA 02543 USA. [Waliser, Duane] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Murtugudde, Raghu] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Subramanian, A (reprint author), UCSD, SIO, La Jolla, CA 92037 USA. EM acsubram@ucsd.edu RI jochum, markus/C-2960-2015; Subramanian, Aneesh/D-9484-2017 OI jochum, markus/0000-0003-2690-3139; Subramanian, Aneesh/0000-0001-7805-0102 FU ONR [N00014-13-1-0139]; NSF [OCE-0960770]; SUNNY (Scripps/UCSD/NCAR New and Young) Program FX This research forms a part of the Ph.D. dissertation of A.S. We gratefully acknowledge funding from ONR (N00014-13-1-0139) and NSF (OCE-0960770). This research was initiated during a visit by A.S. to NCAR funded by the SUNNY (Scripps/UCSD/NCAR New and Young) Program. A.S. acknowledges NCARs computational support for simulations conducted for this study. We thank Mitch Moncrieff and Brian Mapes for erudite comments, and criticism of this work. A.S. extends heartfelt thanks to Bruce Cornuelle and Ian Eisenman for many invaluable gems of wisdom on science and data analysis. 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 48 TC 7 Z9 7 U1 2 U2 32 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 APR PY 2014 VL 42 IS 7-8 BP 2019 EP 2031 DI 10.1007/s00382-013-1846-1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AE5ZP UT WOS:000334068100019 ER PT J AU Dushaw, BD Menemenlis, D AF Dushaw, Brian D. Menemenlis, Dimitris TI Antipodal acoustic thermometry: 1960, 2004 SO DEEP-SEA RESEARCH PART I-OCEANOGRAPHIC RESEARCH PAPERS LA English DT Article DE Antipodal acoustics; Ocean modeling; Acoustic tomography; Climate change ID NORTH PACIFIC-OCEAN; HEARD ISLAND; HYDROACOUSTIC SIGNALS; UNDERWATER EXPLOSIONS; GENERAL-CIRCULATION; SOUND-TRANSMISSION; RANGE; BERMUDA; SPEED; AUSTRALIA AB On 21 March 1960, sounds from three 300-lb depth charges deployed at 5.5-min intervals off Perth, Australia were recorded by the SOFAR station at Bermuda. The recorded travel time of these signals, about 13,375 s, is a historical measure of the ocean temperature averaged across several ocean basins. The 1960 travel time measurement has about 3-s precision. High-resolution global ocean state estimates for 2004 from the "Estimating the Circulation and Climate of the Ocean, Phase II" (ECCO2) project were combined with ray tracing to determine the paths followed by the acoustic signals. The acoustic paths are refracted geodesics that are slightly deflected by either small-scale topographic features in the Southern Ocean or the coast of Brazil. The refractive influences of intense, small-scale oceanographic features, such as Agulhas Rings or eddies in the Antarctic Circumpolar Current, greatly reduce the necessary topographic deflection and cause the acoustic paths to meander in time. The ECCO2 ocean state estimates, which are constrained by model dynamics and available data, were used to compute present-day travel times. Measured and computed arrival coda were in good agreement. Based on recent estimates of warming of the upper ocean, the travel-time change over the past half-century was nominally expected to be about -9 s, but little difference between measured (1960) and computed (2004) travel times was found. Taking into account uncertainties in the 1960 measurements, the 2004 ocean state estimates, and other approximations, the ocean temperature averaged along the sound channel axis over the antipodal paths has warmed at a rate less than about 4.6 m degrees C yr(-1) (95% confidence). At this time, the estimated uncertainties are comparable in size to the expected warming signal, however. (C) 2014 The Authors. Published by Elsevier Ltd. All rights reserved. C1 [Dushaw, Brian D.] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA. [Menemenlis, Dimitris] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dushaw, BD (reprint author), Univ Washington, Appl Phys Lab, 1013 NE 40th St, Seattle, WA 98105 USA. EM dushaw@apl.washington.edu OI Menemenlis, Dimitris/0000-0001-9940-8409 FU National Science Foundation [OCE-0850357]; Office of Naval Research [N00014-09-1-0446, N00014-12-1-0183] FX This project was supported by National Science Foundation Grant OCE-0850357 and Office of Naval Research Grants N00014-09-1-0446, N00014-12-1-0183. D.M. performed this work at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA) Modeling Analysis and Prediction (MAP) Program. Thanks are due to Lieutenant Commander Ian Jempson RAN (Navigating Officer, ret.) of the Queensland Maritime Museum for providing essential assistance in the interpretation of the HMAS Diamantina Ship's Log and other information. We would like to thank the staffs of the National Archives of Australia and the Australian War Memorial for their helpful efficiency in locating and making available material related to HMAS Diamantina and the 1960 experiment. NR 64 TC 4 Z9 4 U1 0 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0637 EI 1879-0119 J9 DEEP-SEA RES PT I JI Deep-Sea Res. Part I-Oceanogr. Res. Pap. PD APR PY 2014 VL 86 BP 1 EP 20 DI 10.1016/j.dsr.2013.12.008 PG 20 WC Oceanography SC Oceanography GA AE8MR UT WOS:000334256500001 ER PT J AU Kavaya, MJ Beyon, JY Koch, GJ Petros, M Petzar, PJ Singh, UN Trieu, BC Yu, JR AF Kavaya, Michael J. Beyon, Jeffrey Y. Koch, Grady J. Petros, Mulugeta Petzar, Paul J. Singh, Upendra N. Trieu, Bo C. Yu, Jirong TI The Doppler Aerosol Wind (DAWN) Airborne, Wind-Profiling Coherent-Detection Lidar System: Overview and Preliminary Flight Results SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Lidars/Lidar observations; Aircraft observations; Remote sensing; Wind profilers; Profilers, atmospheric ID LASER-RADAR; PERFORMANCE; EFFICIENCY; ERROR; SPACE AB The first airborne wind measurements of a pulsed, 2-mu m solid-state, high-energy, wind-profiling lidar system for airborne measurements are presented. The laser pulse energy is the highest to date in an eye-safe airborne wind lidar system. This energy, the 10-Hz laser pulse rate, the 15-cm receiver diameter, and dual-balanced coherent detection together have the potential to provide much-improved lidar sensitivity to low aerosol backscatter levels compared to earlier airborne-pulsed coherent lidar wind systems. Problems with a laser-burned telescope secondary mirror prevented a full demonstration of the lidar's capability, but the hardware, algorithms, and software were nevertheless all validated. A lidar description, relevant theory, and preliminary results of flight measurements are presented. C1 [Kavaya, Michael J.; Beyon, Jeffrey Y.; Koch, Grady J.; Petros, Mulugeta; Petzar, Paul J.; Singh, Upendra N.; Trieu, Bo C.; Yu, Jirong] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Kavaya, MJ (reprint author), NASA, Langley Res Ctr, 5 N Dryden St,Mail Code 468, Hampton, VA 23681 USA. EM michael.j.kavaya@nasa.gov FU NASA Science Mission Directorate, Earth Science Division, Earth Science Technology Office; NASA Science Mission Directorate, Earth Science Division; NASA Langley Research Center; NASA Langley Research Center, Engineering Directorate; NASA Langley Research Center, Chief Engineer's office FX The authors acknowledge support from NASA Science Mission Directorate, Earth Science Division, Earth Science Technology Office; NASA Science Mission Directorate, Earth Science Division; NASA Langley Research Center; NASA Langley Research Center, Engineering Directorate; and NASA Langley Research Center, Chief Engineer's office. NR 35 TC 7 Z9 10 U1 2 U2 23 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 APR PY 2014 VL 31 IS 4 BP 826 EP 842 DI 10.1175/JTECH-D-12-00274.1 PG 17 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AE6XX UT WOS:000334142400005 ER EF