FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Edwards, JR Boles, JA Baurle, RA AF Edwards, Jack R. Boles, John A. Baurle, Robert A. TI Large-eddy/Reynolds-averaged Navier-Stokes simulation of a supersonic reacting wall jet SO COMBUSTION AND FLAME LA English DT Article DE Supersonic combustion; Large-eddy simulation ID LARGE-EDDY SIMULATION; COMBUSTION; MODELS; FLOWS; FORMULATION AB This work presents results from large-eddy/Reynolds-averaged Navier-Stokes (LES/RANS) simulations of the well-known Burrows-Kurkov supersonic reacting wall-jet experiment. Generally good agreement with experimental mole fraction, stagnation temperature, and Pitot pressure profiles is obtained for non-reactive mixing of the hydrogen jet with a non-vitiated air stream. A lifted flame, stabilized between 15 and 20 cm downstream of the hydrogen jet, is formed for hydrogen injected into a vitiated air stream. Flame stabilization occurs closer to the hydrogen injection location when a three-dimensional combustor geometry (with boundary layer development resolved on all walls) is considered. Volumetric expansion of the reactive shear layer is accompanied by the formation of large eddies which interact strongly with the reaction zone. Time averaged predictions of the reaction zone structure show an under-prediction of the peak water concentration and stagnation temperature, relative to experimental data, but display generally good agreement with the extent of the reaction zone. Reactive scalar scatter plots indicate that the flame exhibits a transition from a partially-premixed flame structure, characterized by intermittent heat release, to a diffusion-flame structure that could probably be described by a strained laminar flamelet model. (C) 2011 Published by Elsevier Inc. on behalf of The Combustion Institute. C1 [Edwards, Jack R.] N Carolina State Univ, Dept Mech & Aerosp Engn, Raleigh, NC 27695 USA. [Boles, John A.] Taitech Inc, Wright Patterson AFB, OH 45433 USA. [Baurle, Robert A.] NASA Langley Res Ctr, Hyperson Air Breathing Prop Branch, Hampton, VA 23681 USA. RP Edwards, JR (reprint author), N Carolina State Univ, Dept Mech & Aerosp Engn, Campus Box 7910, Raleigh, NC 27695 USA. EM jredward@ncsu.edu FU NASA [NNX07AC27A-S01]; National Center for Hypersonic Combined-Cycle Propulsion; AFOSR FX This work is supported by NASA under Cooperative Agreement NNX07AC27A-S01 and by the National Center for Hypersonic Combined-Cycle Propulsion, funded jointly by AFOSR and NASA. Computer resources have been provided by the NASA Advanced Supercomputing (NAS) division. NR 45 TC 6 Z9 8 U1 0 U2 24 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0010-2180 J9 COMBUST FLAME JI Combust. Flame PD MAR PY 2012 VL 159 IS 3 BP 1127 EP 1138 DI 10.1016/j.combustflame.2011.10.009 PG 12 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA 886LH UT WOS:000299855400019 ER PT J AU Keeton, KE Schmidt, LL Slack, KJ Malka, AA AF Keeton, Kathryn E. Schmidt, Lacey L. Slack, Kelley J. Malka, Ari A. TI The Rocket Science of Teams SO INDUSTRIAL AND ORGANIZATIONAL PSYCHOLOGY-PERSPECTIVES ON SCIENCE AND PRACTICE LA English DT Editorial Material C1 [Keeton, Kathryn E.] NASA, Lyndon B Johnson Space Ctr, BHP Program Element, EASI, Houston, TX 77058 USA. [Slack, Kelley J.] NASA, Lyndon B Johnson Space Ctr, LZ Technol, Houston, TX 77058 USA. [Malka, Ari A.] Univ Houston, Houston, TX 77004 USA. RP Keeton, KE (reprint author), NASA, Lyndon B Johnson Space Ctr, BHP Program Element, EASI, 1290 Hercules, Houston, TX 77058 USA. EM kathryn.keeton@nasa.gov NR 1 TC 1 Z9 1 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1754-9426 J9 IND ORGAN PSYCHOL-US JI Ind. Organ. Psychol. PD MAR PY 2012 VL 5 IS 1 BP 32 EP 35 DI 10.1111/j.1754-9434.2011.01399.x PG 4 WC Psychology, Applied SC Psychology GA 886CT UT WOS:000299829700005 ER PT J AU Draper, SL Isheim, D AF Draper, S. L. Isheim, D. TI Environmental embrittlement of a third generation gamma TiAl alloy SO INTERMETALLICS LA English DT Article DE Titanium aluminides; based on TiAl; Environmental embrittlement; Diffusion; Surface properties; Microprobe; Atom probe ID TEMPERATURE EXPOSURE; THERMAL EXPOSURE; MET PX; BEHAVIOR AB Exposure of a Ti-45Al-5Nb alloy to elevated temperatures has been shown to result in a loss of ductility resulting from a near surface effect involving diffusion of oxygen into the alloy. Local electrode atom probe analysis was conducted at 2, 13, and 25 gm distance from the oxide/base-metal interface. Oxygen was preferentially located in the alpha(2) phase with concentrations up to 14.8 at.% and diminishing with increasing distance from the surface. Near surface microstructural changes were only visible up to 10 mu m from the surface but the oxygen diffusion significantly exceeded that distance. The diffusion coefficient of oxygen into the alpha(2) phase was estimated based on the oxygen concentrations obtained from local electrode atom probe analysis. Fluorine ion implantation on the surface was investigated as a possible solution to the embrittlement. Published by Elsevier Ltd. C1 [Draper, S. L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Isheim, D.] Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA. [Isheim, D.] Northwestern Univ, Ctr Atom Probe Tomog NUCAPT, Evanston, IL 60208 USA. RP Draper, SL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 49-1, Cleveland, OH 44135 USA. EM Susan.L.Draper@nasa.gov; isheim@northwestern.edu FU NSF-MRI [DMR-0420532]; ONR-DURIP [N00014-0400798, N00014-0610539, N00014-0910781] FX The authors are grateful to David Hull, NASA Glenn Research Center, for the electron microprobe analysis and A. Donchev, Karl-Winnacker-Institut, of the DECHEMA e.V., for the F ion implantation. The Atom-probe tomographic measurements were performed at the Northwestern University Center for Atom-Probe Tomography (NUCAPT). The LEAP tomograph was purchased and upgraded with funding from NSF-MRI (DMR-0420532) and ONR-DURIP (N00014-0400798, N00014-0610539, N00014-0910781) grants. The authors are thankful to Stephan Gerstl at Imago Scientific Instruments for LEAP analysis of bulk alloy. NR 15 TC 9 Z9 9 U1 0 U2 10 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0966-9795 J9 INTERMETALLICS JI Intermetallics PD MAR PY 2012 VL 22 BP 77 EP 83 DI 10.1016/j.intermet.2011.10.006 PG 7 WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering GA 888DD UT WOS:000299983100012 ER PT J AU Gonzalez, P Tucker, CJ Sy, H AF Gonzalez, P. Tucker, C. J. Sy, H. TI Tree density and species decline in the African Sahel attributable to climate SO JOURNAL OF ARID ENVIRONMENTS LA English DT Article DE Climate change; Climate variability; Desertification; Tree cover; Vegetation shifts ID WEST-AFRICA; WOODY VEGETATION; BURKINA-FASO; NDVI DATA; DROUGHT; DESERTIFICATION; DYNAMICS; MORTALITY; PATTERNS; DATABASE AB Increased aridity and human population have reduced tree cover in parts of the African Sahel and degraded resources for local people. Yet, tree cover trends and the relative importance of climate and population remain unresolved. From field measurements, aerial photos, and Ikonos satellite images, we detected significant 1954-2002 tree density declines in the western Sahel of 18 +/- 14% (P = 0.014, n = 204) and 17 +/- 13% (P = 0.0009, n = 187). From field observations, we detected a significant 1960 2000 species richness decline of 21 +/- 11% (P = 0.0028, n = 14) across the Sahel and a southward shift of the Sahel, Sudan, and Guinea zones. Multivariate analyses of climate, soil, and population showed that temperature most significantly (P < 0.001) explained tree cover changes. Multivariate and bivariate tests and field observations indicated the dominance of temperature and precipitation, supporting attribution of tree cover changes to climate variability. Climate change forcing of Sahel climate variability, particularly the significant (P < 0.05) 1901-2002 temperature increases and precipitation decreases in the research areas, connects Sahel tree cover changes to global climate change. This suggests roles for global action and local adaptation to address ecological change in the Sahel. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Gonzalez, P.] Univ Calif Berkeley, Ctr Forestry, Berkeley, CA 94720 USA. [Tucker, C. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sy, H.] Famine Early Warning Syst Network, Nouakchott, Mauritania. RP Gonzalez, P (reprint author), Univ Calif Berkeley, Ctr Forestry, 163 Mulford, Berkeley, CA 94720 USA. EM pgonzalez@cal.berkeley.edu RI Gonzalez, Patrick/B-9479-2013 OI Gonzalez, Patrick/0000-0002-7105-0561 FU NASA; U.S. Geological Survey FX We gratefully acknowledge field work assistance by Alkhalil Adoum, Elaine Carlson, Issa Khalil, Joseph Sedgo, and Salif Sow, comments from Paul R. Ehrlich, support from Christine A. Rose, allocation of Ikonos images from the NASA Scientific Data Purchase, research funding from NASA and the U.S. Geological Survey, and assistance from the residents of Akar, Aten, Banizumbi, Buurtey Ganuun, Dan Tsuntsu, Fabugu, Fete Ole, Guidimouni, Juude Waalo, Kardofal, Kaylaroom, Marchuut, Nampabuum, Ningelin, Njoobeen Mbataar, Tamaka, and Wolum. NR 50 TC 50 Z9 52 U1 2 U2 42 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0140-1963 EI 1095-922X J9 J ARID ENVIRON JI J. Arid. Environ. PD MAR PY 2012 VL 78 BP 55 EP 64 DI 10.1016/j.jaridenv.2011.11.001 PG 10 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 889LA UT WOS:000300074000007 ER PT J AU Alonso-Perez, S Cuevas, E Querol, X Guerra, JC Perez, C AF Alonso-Perez, S. Cuevas, E. Querol, X. Guerra, J. C. Perez, C. TI African dust source regions for observed dust outbreaks over the Subtropical Eastern North Atlantic region, above 25 degrees N SO JOURNAL OF ARID ENVIRONMENTS LA English DT Article DE Aerosols; African dust; Marine Boundary Layer; Dust sources; Residence time; HYSPLIT ID LONG-RANGE TRANSPORT; SOUTHEASTERN UNITED-STATES; SAHARAN DUST; CANARY-ISLANDS; MINERAL-DUST; AIR-QUALITY; ELEMENTAL COMPOSITION; CHEMICAL-COMPOSITION; SURFACE OBSERVATIONS; SUSPENDED PARTICLES AB High mineral dust-laden air mass potential source regions affecting the Marine Boundary Layer (MBL) of the Subtropical Eastern North Atlantic Region above 25 degrees N (SENAR), directly or by means of gravitational settlement, were objectively identified. We introduced a new hybrid Lagrangian-Eulerian receptor model, in which air mass residence time probability maps in the geographical domain latitude = [5 degrees N, 60 degrees N], longitude = [70 degrees W, 30 degrees E] were combined with TOMS-AI data (TAPI Index), and with simulated Total Suspended Particles (TSP) with the BSC/DREAM model (SDPI Index). Both approaches show a good agreement. For dust gravitational settlement episodes within the MBL, the dust sources are located in southernmost latitudes compared to those associated with lower air mass transport. A seasonal variability in potential dust sources is found with both approaches, TAPI and SDPI. In winter, most dust sources are located within the Sahara in an area bounded by latitude = [18 degrees N, 35 degrees N], longitude = [15 degrees W, 15 degrees E]. In summer, a high dust-laden air mass reservoir above the Atlantic Ocean has been found during episodes for low altitudes, and dust source regions in the Sahara have been identified for middle and upper altitudes. The Bodele depression was found to have a minor impact on dust outbreaks affecting the SENAR. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Alonso-Perez, S.; Cuevas, E.] Izana Atmospher Res Ctr AEMET, Santa Cruz De Tenerife 38071, Spain. [Alonso-Perez, S.; Querol, X.] Inst Environm Assessment & Water Res CSIC, Barcelona 08028, Spain. [Guerra, J. C.] Univ La Laguna, Atmospher Phys Lab, Tenerife 38200, Spain. [Perez, C.] Columbia Univ, Earth Inst, NASA Goddard Inst Space Studies, New York, NY 10025 USA. [Perez, C.] Int Res Inst Climate & Soc, New York, NY 10025 USA. RP Alonso-Perez, S (reprint author), Izana Atmospher Res Ctr AEMET, C La Marina 20,6 Planta, Santa Cruz De Tenerife 38071, Spain. EM salonsop@aemet.es RI Querol, Xavier/E-2800-2014; Alonso Perez, Silvia/M-1035-2014; Cuevas, Emilio/L-2109-2013 OI Querol, Xavier/0000-0002-6549-9899; Alonso Perez, Silvia/0000-0003-0572-6081; Cuevas, Emilio/0000-0003-1843-8302 FU G.D. of Environmental Quality and Assessment from the Spanish Ministry of Environment, Rural and Marine Affairs FX This study was supported by the G.D. of Environmental Quality and Assessment from the Spanish Ministry of Environment, Rural and Marine Affairs. NR 86 TC 13 Z9 13 U1 0 U2 15 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0140-1963 J9 J ARID ENVIRON JI J. Arid. Environ. PD MAR PY 2012 VL 78 BP 100 EP 109 DI 10.1016/j.jaridenv.2011.11.013 PG 10 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 889LA UT WOS:000300074000011 ER PT J AU Jain, A AF Jain, Abhinandan TI Multibody graph transformations and analysis SO NONLINEAR DYNAMICS LA English DT Article DE Multibody systems; Graph theory; Algorithms ID QUASI-VELOCITIES; DYNAMICS; FORMULATION; SYSTEMS; EQUATIONS; DESIGN AB This two-part paper uses graph transformation methods to develop methods for partitioning, aggregating, and constraint embedding for multibody systems. This first part focuses on tree-topology systems and reviews the key notion of spatial kernel operator (SKO) models for such systems. It develops systematic and rigorous techniques for partitioning SKO models in terms of the SKO models of the component subsystems based on the path-induced property of the component subgraphs. It shows that the sparsity structure of key matrix operators and the mass matrix for the multibody system can be described using partitioning transformations. Subsequently, the notions of node contractions and subgraph aggregation and their role in coarsening graphs are discussed. It is shown that the tree property of a graph is preserved after subgraph aggregation if and only if the subgraph satisfies an aggregation condition. These graph theory ideas are used to develop SKO models for the aggregated tree multibody systems. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jain, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Abhi.Jain@jpl.nasa.gov FU National Aeronautics and Space Administration; National Institute of Health [RO1GM082896-01A2] FX The research described in this paper was performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration.7 This project was also supported in part by Grant Number RO1GM082896-01A2 from the National Institute of Health. NR 30 TC 4 Z9 4 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0924-090X J9 NONLINEAR DYNAM JI Nonlinear Dyn. PD MAR PY 2012 VL 67 IS 4 BP 2779 EP 2797 DI 10.1007/s11071-011-0188-y PG 19 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 891AC UT WOS:000300187500037 ER PT J AU Adamovsky, G Lyuksyutov, SF Mackey, JR Floyd, BM Abeywickrema, U Fedin, I Rackaitis, M AF Adamovsky, Grigory Lyuksyutov, Sergei F. Mackey, Jeffrey R. Floyd, Bertram M. Abeywickrema, Ujitha Fedin, Igor Rackaitis, Mindaugas TI Peculiarities of thermo-optic coefficient under different temperature regimes in optical fibers containing fiber Bragg gratings SO OPTICS COMMUNICATIONS LA English DT Article DE Optical materials; Optical fibers; Bragg gratings; Thermodynamic properties; High temperature tests ID THERMAL-STABILITY; SENSOR AB Direct experimental measurements of the thermo-optic for fixed temperature intervals (20-200 degrees C, 200-500 degrees C C, 500-660 degrees C, 660-780 degrees C) in fused silica fiber containing fiber Bragg gratings (FBGs) were conducted. The diffraction efficiency of a FBG fluctuated with temperature between 2.01 x 10(-4) and 0.17 x 10(-4) while the temperature shift of the Bragg's peak was monitored between 1300 and 1311 nm with sub-Angstrom precision. Numerical simulations were focused on FBG's diffraction efficiency calculations accounting for the temperature drift of the gratings, and found to be in excellent agreement with obtained experimental data. It was found that the first-order thermo-optic coefficient changes between 1.29 and 1.85 x 10(-5) K-1 for the linear fit and at T=0 degrees C its value was found to be close to 2.37 x 10(-5) K-1 for the polynomial fit of experimental data. The average thermo-optic coefficient undergoes a minimum in the vicinity of 440 degrees C. Additional observation indicates a negative sign of the second-order thermo-optic coefficient. The value of thermal expansion coefficient was much less (0.5 x 10(-6) K-1) than that for the average thermo-optic coefficient. Based on the energy dispersive spectroscopy it was determined that thermal erasing of the FBGs at a temperature around 780 degrees C corresponds to germanium monoxide diffusion out of core in silica-based fibers. (C) 2011 Elsevier B.V. All rights reserved. C1 [Lyuksyutov, Sergei F.; Abeywickrema, Ujitha; Fedin, Igor] Univ Akron, Dept Phys, Akron, OH 44325 USA. [Rackaitis, Mindaugas] Bridgestone Amer, Ctr Res & Technol, Akron, OH 44317 USA. [Floyd, Bertram M.] Sierra Lobo Inc, Cleveland, OH 44135 USA. [Mackey, Jeffrey R.] ASRC Aerosp Corp, Cleveland, OH 44135 USA. [Adamovsky, Grigory] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA. RP Lyuksyutov, SF (reprint author), Univ Akron, Dept Phys, Akron, OH 44325 USA. EM sfl@uakron.edu FU NASA FX The authors acknowledge support from the Hypersonic Project of the NASA Fundamental Aeronautics Program. One of the co-authors, SFL, a NASA Glenn Research Center 2010 Summer Fellow, also appreciates the support of the NASA Summer Faculty Program. NR 16 TC 11 Z9 12 U1 3 U2 18 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0030-4018 J9 OPT COMMUN JI Opt. Commun. PD MAR 1 PY 2012 VL 285 IS 5 BP 766 EP 773 DI 10.1016/j.optcom.2011.10.084 PG 8 WC Optics SC Optics GA 891EO UT WOS:000300200200048 ER PT J AU Roberts, S Zachrisson, C Kozachkov, H Ullah, A Shapiro, AA Johnson, WL Hofmann, DC AF Roberts, Scott Zachrisson, Carl Kozachkov, Henry Ullah, Adam Shapiro, Andrew A. Johnson, William L. Hofmann, Douglas C. TI Cryogenic Charpy impact testing of metallic glass matrix composites SO SCRIPTA MATERIALIA LA English DT Article DE Bulk metallic glass matrix composites; Charpy; Cryogenic; Toughness ID DUCTILITY; TEMPERATURES; PLASTICITY; TENSILE AB Compact Charpy impact testing was employed to investigate the effect of low temperatures on the impact toughness of bulk metallic glass matrix composites (BMGMCs). Samples were fabricated via suction casting and impacted from room temperature down to liquid nitrogen temperature. Unlike monolithic glasses, BMGMCs do exhibit a steep decrease in toughness as the temperature is reduced from the ambient, caused by embrittlement in the ductile reinforcing phase. However, at cryogenic temperatures, BMGMCs have a toughness equivalent to their glassy matrix. (C) 2011 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Shapiro, Andrew A.; Hofmann, Douglas C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Roberts, Scott; Zachrisson, Carl; Kozachkov, Henry; Ullah, Adam; Shapiro, Andrew A.; Johnson, William L.; Hofmann, Douglas C.] CALTECH, Pasadena, CA 91126 USA. RP Hofmann, DC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM dch@jpl.nasa.gov FU Exploration Systems Mission Directorate (ESMD) Advanced Capabilities Division at the National Aeronautics and Space Administration (NASA) [NNH10ZTT001N]; NASA FX This work was supported by the Exploration Systems Mission Directorate (ESMD) Advanced Capabilities Division at the National Aeronautics and Space Administration (NASA) under contract number NNH10ZTT001N. C.F.Z. acknowledges financial support from AAAS Entry Point's ACCESS, a program sponsored by NASA. 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 18 TC 8 Z9 9 U1 1 U2 44 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6462 J9 SCRIPTA MATER JI Scr. Mater. PD MAR PY 2012 VL 66 IS 5 BP 284 EP 287 DI 10.1016/j.scriptamat.2011.11.011 PG 4 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 890EZ UT WOS:000300129200022 ER PT J AU Durden, SL AF Durden, Stephen L. TI Trends in Intense Typhoon Minimum Sea Level Pressure SO ATMOSPHERE LA English DT Article DE typhoon; tropical cyclone; intensity; climate change ID QUANTILE REGRESSION; TROPICAL CYCLONES; ENSO; PACIFIC AB A number of recent publications have examined trends in the maximum wind speed of tropical cyclones in various basins. In this communication, the author focuses on typhoons in the western North Pacific. Rather than maximum wind speed, the intensity of the storms is measured by their lifetime minimum sea level pressure (MSLP). Quantile regression is used to test for trends in storms of extreme intensity. The results indicate that there is a trend of decreasing intensity in the most intense storms as measured by MSLP over the period 1951-2010. However, when the data are broken into intervals 1951-1987 and 1987-2010, neither interval has a significant trend, but the intensity quantiles for the two periods differ. Reasons for this are discussed, including the cessation of aircraft reconnaissance in 1987. The author also finds that the average typhoon intensity is greater in El Nino years, while the intensity of the strongest typhoons shows no significant relation to El Nino Southern Oscillation. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Durden, SL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sdurden@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 22 TC 1 Z9 1 U1 0 U2 1 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2073-4433 J9 ATMOSPHERE-BASEL JI Atmosphere PD MAR PY 2012 VL 3 IS 1 BP 124 EP 131 DI 10.3390/atmos3010124 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 175QS UT WOS:000321247100006 ER PT J AU Fleischer, I Klingelhofer, G Morris, RV Schroder, C Rodionov, D de Souza, PA AF Fleischer, Iris Klingelhoefer, Goestar Morris, Richard V. Schroeder, Christian Rodionov, Daniel de Souza, Paulo A. CA MIMOS II Team TI In-situ Mossbauer spectroscopy with MIMOS II SO HYPERFINE INTERACTIONS LA English DT Proceedings Paper CT 65th Yamada Conference / 31st International Conference on the Applications of the Mossbauer Effect (ICAME) CY SEP 25-30, 2011 CL Kobe, JAPAN DE Miniaturized Mossbauer spectrometer; MIMOS II; Mars Exploration Rover mission; In-situ Mossbauer spectroscopy; Non-destructive analysis ID GUSEV CRATER; MERIDIANI-PLANUM; SPIRIT ROVER; HEMATITE SPHERULES; BURNS FORMATION; HOME PLATE; MARS; SPECTROMETER; EXPLORATION; DIAGENESIS AB The miniaturized Mossbauer spectrometer MIMOS II was developed for the exploration of planetary surfaces. Two MIMOS II instruments were successfully deployed on the martian surface as payload elements of the NASA Mars Exploration Rover (MER) mission and have returned data since landing in January 2004. Mossbauer spectroscopy has made significant contributions to the success of the MER mission, in particular identification of iron-bearing minerals formed through aqueous weathering processes. As a field-portable instrument and with backscattering geometry, MIMOS II provides an opportunity for non-destructive in-situ investigations for a range of applications. For example, the instrument has been used for analyses of archaeological artifacts, for air pollution studies and for in-field monitoring of green rust formation. AMER-type MIMOS II instrument is part of the payload of the Russian Phobos-Grunt mission, scheduled for launch in November 2011, with the aim of exploring the composition of the martian moon Phobos. An advanced version of the instrument, MIMOS IIA, that incorporates capability for elemental analyses, is currently under development. C1 [Fleischer, Iris; Klingelhoefer, Goestar; Rodionov, Daniel] Johannes Gutenberg Univ Mainz, Inst Inorgan & Analyt Chem, D-55122 Mainz, Germany. [Morris, Richard V.] NASA, Johnson Space Ctr, Houston, TX USA. [Schroeder, Christian] Univ Bayreuth, Tubingen, Germany. [Schroeder, Christian] Univ Tubingen, Tubingen, Germany. [Rodionov, Daniel] Space Res Inst IKI, Moscow, Russia. [de Souza, Paulo A.] Tasmanian ICT Ctr, Hobart, Tas, Australia. RP Fleischer, I (reprint author), Johannes Gutenberg Univ Mainz, Inst Inorgan & Analyt Chem, D-55122 Mainz, Germany. EM fleischi@uni-mainz.de RI de Souza, Paulo/B-8961-2008; Schroder, Christian/B-3870-2009 OI de Souza, Paulo/0000-0002-0091-8925; Schroder, Christian/0000-0002-7935-6039 NR 46 TC 1 Z9 1 U1 2 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0304-3843 J9 HYPERFINE INTERACT JI Hyperfine Interact. PD MAR PY 2012 VL 207 IS 1-3 BP 97 EP 105 DI 10.1007/s10751-011-0437-y PG 9 WC Physics, Atomic, Molecular & Chemical; Physics, Condensed Matter; Physics, Nuclear SC Physics GA 070JM UT WOS:000313502400018 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 MAR PY 2012 VL 2 IS 2 BP 157 EP 160 DI 10.1109/TTHZ.2012.2186714 PG 4 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142AA UT WOS:000318766700001 ER PT J AU Siegel, PH AF Siegel, Peter H. TI Terahertz Pioneers A Series of Interviews With Significant Contributors to Terahertz Science and Technology SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Editorial Material C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91109 USA. [Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91109 USA. [Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91109 USA. NR 0 TC 3 Z9 3 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD MAR PY 2012 VL 2 IS 2 BP 161 EP 161 DI 10.1109/TTHZ.2011.2182389 PG 1 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142AA UT WOS:000318766700002 ER PT J AU Siegel, PH AF Siegel, Peter H. TI Terahertz Pioneer: Robert W. Wilson SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Biographical-Item C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91109 USA. [Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91109 USA. [Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91109 USA. EM phs@caltech.edu NR 1 TC 1 Z9 1 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 MAR PY 2012 VL 2 IS 2 BP 162 EP 166 DI 10.1109/TTHZ.2011.2182390 PG 5 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142AA UT WOS:000318766700003 ER PT J AU Maestrini, A Mehdi, I Siles, JV Ward, JS Lin, R Thomas, B Lee, C Gill, J Chattopadhyay, G Schlecht, E Pearson, J Siegel, P AF Maestrini, Alain Mehdi, Imran Siles, Jose V. Ward, John S. Lin, Robert Thomas, Bertrand Lee, Choonsup Gill, John Chattopadhyay, Goutam Schlecht, Erich Pearson, John Siegel, Peter TI Design and Characterization of a Room Temperature All-Solid-State Electronic Source Tunable From 2.48 to 2.75 THz SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Broadband terahertz (THz) source; frequency multiplier; frequency tripler; local oscillator; planar diode; power-combining; Schottky diode; THz; varactor ID SCHOTTKY DIODES; FREQUENCY; POWER; BAND AB We report on the design, fabrication and test of an all-solid-state, frequency agile source that produces over 1 mu W (-30 dBm) across the 2.48-2.75 THz band at room temperature. This frequency-multiplied source is driven by a W-band synthesizer followed by a power amplifier that delivers 350-450 mW (25.5-26.5 dBm) and a cascade of three balanced frequency triplers. The first stage tripler is based on four power-combined six-anode GaAs Schottky diode devices, and the second stage tripler is based on two four-anode GaAs devices. The output tripler uses a single unbiased device featuring two anodes monolithically integrated onto a thin GaAs membrane. The source delivers a record 18 mu W (-17.5 dBm) at 2.58 THz at room temperature. This frequency multiplied source is analyzed with a Fourier transform spectrometer (FTS) and the unwanted harmonics are found to be at least 29 dB below the desired signal. This source, when used as the local oscillator for a hot-electron bolometer mixer, will enable heterodyne instruments for future space missions to map the cosmologically-important 2.675 THz HD molecular line. C1 [Maestrini, Alain] Univ Paris 06, Paris, France. [Maestrini, Alain] LERMA, Observatoire Paris, Paris, France. [Mehdi, Imran; Siles, Jose V.; Ward, John S.; Lin, Robert; Thomas, Bertrand; Lee, Choonsup; Gill, John; Chattopadhyay, Goutam; Schlecht, Erich; Pearson, John; Siegel, Peter] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Maestrini, A (reprint author), Univ Paris 06, Paris, France. EM alain.maestrini@obspm.fr; Imran.mehdi@jpl.nasa.gov; goutam@jpl.nasa.gov FU National Aeronautics and Space Administration under a contract, at the Universite Pierre et Marie Curie-Paris 6; National Aeronautics and Space Administration at the Observatoire de Paris, France; NASA Astrophysics Research and Analysis Program (APRA), Universite Pierre et Marie Curie; Centre National d'Etudes Spatiales FX This work was supported by National Aeronautics and Space Administration under a contract, at the Universite Pierre et Marie Curie-Paris 6, and at the Observatoire de Paris, France. Funding from NASA Astrophysics Research and Analysis Program (APRA), Universite Pierre et Marie Curie and Centre National d'Etudes Spatiales. NR 33 TC 29 Z9 29 U1 1 U2 11 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD MAR PY 2012 VL 2 IS 2 BP 177 EP 185 DI 10.1109/TTHZ.2012.2183740 PG 9 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142AA UT WOS:000318766700005 ER PT J AU Fung, A Samoska, L Pukala, D Dawson, D Kangaslahti, P Varonen, M Gaier, T Lawrence, C Boll, G Lai, R Mei, XB AF Fung, Andy Samoska, Lorene Pukala, David Dawson, Douglas Kangaslahti, Pekka Varonen, Mikko Gaier, Todd Lawrence, Charles Boll, Greg Lai, Richard Mei, X. B. TI On-Wafer S-Parameter Measurements in the 325-508 GHz Band SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Millimeter wave; monolithic microwave integrated circuits (MMIC); on-wafer; S-parameters; submillimeter wave; terahertz (THz) ID NETWORK ANALYZER MEASUREMENTS; TECHNOLOGY; CIRCUITS; THZ AB We report on two-port on-wafer vector network analyzer measurements in the 325-508 GHz frequency band. Measurements are made with prototype GGB Industries Inc. WR2.2 (325-500 GHz) coplanar waveguide probes and OML Inc. WR2.2 frequency extenders. New probe performance data and characteristics of probe tip calibration using a Thru-Reflect-Line procedure are discussed. Probe S-parameter measurements indicate insertion loss per probe of 5.0 to 9.1 dB in the WR2.2 band. Calibrated dynamic range of about 30 dB or better for insertion and return loss measurement across the band is achieved. These new results for the prototype WR2.2 probes, the calibration procedure, observed errors, and results of on-wafer amplifier measurements are presented. C1 [Fung, Andy; Samoska, Lorene; Pukala, David; Dawson, Douglas; Kangaslahti, Pekka; Varonen, Mikko; Gaier, Todd; Lawrence, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Boll, Greg] GGB Ind Inc, Naples, FL 34101 USA. [Lai, Richard; Mei, X. B.] Northrop Grumman Corp, Redondo Beach, CA 90278 USA. RP Fung, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM andy.fung@jpl.nasa.gov FU NASA ESTO Advanced Component Technologies program [ACT-05]; NASA Innovative Partners Program [IPP-06]; National Aeronautics and Space Administration FX This work was supported in part by the NASA ESTO Advanced Component Technologies ACT-05 program and by the NASA Innovative Partners Program IPP-06. This work was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 26 TC 9 Z9 9 U1 2 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD MAR PY 2012 VL 2 IS 2 BP 186 EP 192 DI 10.1109/TTHZ.2011.2182369 PG 7 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142AA UT WOS:000318766700006 ER PT J AU Bar-Cohen, Y AF Bar-Cohen, Yoseph TI 5 Nature as a Model for Mimicking and Inspiration of New Technologies SO INTERNATIONAL JOURNAL OF AERONAUTICAL AND SPACE SCIENCES LA English DT Review DE Biologically inspired technologies; biomimetics; robotics; actuators; sensors; humanlike robots AB Over 3.8 billion years, through evolution nature came up with many effective continually improving solutions to its challenges. Humans have always been inspired by nature capabilities in problems solving and innovation. These efforts have been intensified in recent years where systematic studies are being made towards better understanding and applying more sophisticated capabilities in this field that is increasingly being titled biomimetics. The ultimate challenge to this field is the development of humanlike robots that talk, interpret speech, walk, as well as make eye-contact and facial expressions with some capabilities that are exceeding the original model from nature. This includes flight where there is no creature that is as large, can fly as high, carry so heavy weight, fly so fast, and able to operate in extreme conditions as the aircraft and other aerospace systems. However, there are many capabilities of biological systems that are not feasible to mimic using the available technology. In this paper, the state-of-the-art of some of the developed biomimetic capabilities, potentials and challenges will be reviewed. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bar-Cohen, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM yosi@jpl.nasa.gov FU National Aeronautics and Space Administration (NASA) FX Some of the research reported in this paper was conducted at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with National Aeronautics and Space Administration (NASA). NR 53 TC 9 Z9 9 U1 3 U2 10 PU KOREAN SOC AERONAUTICAL & SPACE SCIENCES PI SEOULD PA 635-4, YEOGSAM-DONG, KANGNAM-KU, SEOULD, 135-703, SOUTH KOREA SN 2093-274X EI 2093-2480 J9 INT J AERONAUT SPACE JI Int. J. Aeronaut. Space Sci. PD MAR PY 2012 VL 13 IS 1 BP 1 EP 13 DI 10.5139/IJASS.2012.13.1.1 PG 13 WC Engineering, Aerospace SC Engineering GA V35WU UT WOS:000209176800001 ER PT J AU Wu, MLC Reale, O Schubert, SD Suarez, MJ Thorncroft, CD AF Wu, Man-Li C. Reale, Oreste Schubert, Siegfried D. Suarez, Max J. Thorncroft, Chris D. TI African Easterly Jet: Barotropic Instability, Waves, and Cyclogenesis SO JOURNAL OF CLIMATE LA English DT Article ID 3-DIMENSIONAL STRUCTURE; TROPICAL ATLANTIC; HILBERT SPECTRUM; WEST-AFRICA; SUMMER 1981; PART III; DYNAMICS; REANALYSIS; VIEW; OSCILLATION AB This study investigates the structure of the African easterly jet, focusing on instability processes on a seasonal and subseasonal scale, with the goal of identifying features that could provide increased predictability of Atlantic tropical cyclogenesis. The Modern-Era Retrospective Analysis for Research and Applications (MERRA) is used as the main investigating tool. MERRA is compared with other reanalyses datasets from major operational centers around the world and was found to describe very effectively the circulation over the African monsoon region. In particular, a comparison with precipitation datasets from the Global Precipitation Climatology Project shows that MERRA realistically reproduces seasonal precipitation over that region. The verification of the generalized Kuo barotropic instability condition computed from seasonal means is found to have the interesting property of defining well the location where observed tropical storms are detected. This property does not appear to be an artifact of MERRA and is present also in the other adopted reanalysis datasets. Therefore, the fact that the areas where the mean flow is unstable seems to provide a more favorable environment for wave intensification, could be another factor to include in addition to sea surface temperature, vertical shear, precipitation, the role of Saharan air, and others among large-scale forcings affecting development and tropical cyclone frequency. In addition, two prominent modes of variability are found based on a spectral analysis that uses the Hilbert-Huang transform: a 2.5-6-day mode that corresponds well to the African easterly waves and also a 6-9-day mode that seems to be associated with tropicalextratropical interaction. C1 [Wu, Man-Li C.; Schubert, Siegfried D.; Suarez, Max J.] NASA, GMAO, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reale, Oreste] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Thorncroft, Chris D.] SUNY Albany, Dept Earth & Atmospher Sci, Albany, NY 12222 USA. [Reale, Oreste] Univ Space Res Assoc, Columbia, MD USA. RP Wu, MLC (reprint author), NASA, GMAO, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM man-li.c.wu@nasa.gov FU NASA Earth Science Enterprise FX This work was supported by the NASA Earth Science Enterprise's Global Modeling and Analysis Program. We thank the two anonymous reviewers for their helpful comments. NR 56 TC 8 Z9 8 U1 1 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD MAR 1 PY 2012 VL 25 IS 5 BP 1489 EP 1510 DI 10.1175/2011JCLI4241.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 905ZR UT WOS:000301315200007 ER PT J AU Morik, K Bhaduri, K Kargupta, H AF Morik, Katharina Bhaduri, Kanishka Kargupta, Hillol TI Introduction to data mining for sustainability SO DATA MINING AND KNOWLEDGE DISCOVERY LA English DT Editorial Material ID GRASSLAND C1 [Morik, Katharina] TU Dortmund Univ, Fac Comp Sci, Artificial Intelligence Grp, Dortmund, Germany. [Bhaduri, Kanishka] NASA, Ames Res Ctr, Mission Crit Technol Inc, Moffett Field, CA 94035 USA. [Kargupta, Hillol] Univ Maryland Baltimore Cty, Dept Comp Sci & Elect Engn, Baltimore, MD 21228 USA. RP Morik, K (reprint author), TU Dortmund Univ, Fac Comp Sci, Artificial Intelligence Grp, Dortmund, Germany. EM katharina.morik@tu-dortmund.de; Kanishka.Bhaduri-1@nasa.gov; hillol@cs.umbc.edu NR 35 TC 4 Z9 4 U1 7 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1384-5810 J9 DATA MIN KNOWL DISC JI Data Min. Knowl. Discov. PD MAR PY 2012 VL 24 IS 2 SI SI BP 311 EP 324 DI 10.1007/s10618-011-0239-5 PG 14 WC Computer Science, Artificial Intelligence; Computer Science, Information Systems SC Computer Science GA 875TD UT WOS:000299057000001 ER PT J AU Srivastava, AN AF Srivastava, Ashok N. TI Greener aviation with virtual sensors: a case study SO DATA MINING AND KNOWLEDGE DISCOVERY LA English DT Article DE Ensemble learning; Gaussian process; Aviation; Environmental systems; Anomaly detection AB The environmental impact of aviation is enormous given the fact that in the US alone there are nearly 6 million flights per year of commercial aircraft. This situation has driven numerous policy and procedural measures to help develop environmentally friendly technologies which are safe and affordable and reduce the environmental impact of aviation. However, many of these technologies require significant initial investment in newer aircraft fleets and modifications to existing regulations which are both long and costly enterprises. We propose to use an anomaly detection method based on Virtual Sensors to help detect overconsumption of fuel in aircraft which relies only on the data recorded during flight of most existing commercial aircraft, thus significantly reducing the cost and complexity of implementing this method. The Virtual Sensors developed here are ensemble-learning regression models for detecting the overconsumption of fuel based on instantaneous measurements of the aircraft state. This approach requires no additional information about standard operating procedures or other encoded domain knowledge. We present experimental results on three data sets and compare five different Virtual Sensors algorithms. The first two data sets are publicly available and consist of a simulated data set from a flight simulator and a real-world turbine disk. We show the ability to detect anomalies with high accuracy on these data sets. These sets contain seeded faults, meaning that they have been deliberately injected into the system. The second data set is from real-world fleet of 84 jet aircraft where we show the ability to detect fuel overconsumption which can have a significant environmental and economic impact. To the best of our knowledge, this is the first study of its kind in the aviation domain. C1 NASA, Ames Res Ctr, Intelligent Data Understanding Grp, Intelligent Syst Div, Moffett Field, CA 94035 USA. RP Srivastava, AN (reprint author), NASA, Ames Res Ctr, Intelligent Data Understanding Grp, Intelligent Syst Div, Moffett Field, CA 94035 USA. EM ashok.n.srivastava@nasa.gov FU NASA FX The author would like to thank Irving Statler for extremely thoughtful and useful discussions throughout this project. The author also thanks Timothy Woodbury for valuable discussions and Don Simon of NASA Glenn Research Center for providing key references and analytical advice. He would also like to acknowledge Nikunj Oza for valuable discussions and the reviewers for their constructive feedback. The author also thanks our airline partner in providing access to their flight operational data to enable this study. This research was conducted with the support of the NASA Aviation Safety Program's System-Wide Safety and Assurance project. The code used for many of the algorithms in this paper is available as opensource and can be found on DASHlink at https://c3.nasa.gov/dashlink/projects/7/. NR 29 TC 2 Z9 2 U1 1 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1384-5810 J9 DATA MIN KNOWL DISC JI Data Min. Knowl. Discov. PD MAR PY 2012 VL 24 IS 2 SI SI BP 443 EP 471 DI 10.1007/s10618-011-0240-z PG 29 WC Computer Science, Artificial Intelligence; Computer Science, Information Systems SC Computer Science GA 875TD UT WOS:000299057000006 ER PT J AU Yeom, K Park, JH AF Yeom, Kiwon Park, Ji-Hyung TI Morphological approach for autonomous and adaptive systems based on self-reconfigurable modular agents SO FUTURE GENERATION COMPUTER SYSTEMS-THE INTERNATIONAL JOURNAL OF ESCIENCE LA English DT Article DE Morphogenesis; Self-organization; Modular agents; Federation of agents ID ENVIRONMENTS AB This paper describes a novel approach for managing self-organizing, distributed modular components in dynamically changing environments. The main concept is to fabricate a system which is composed of dynamically associated modular agents, that can migrate and reorganize by itself while the system is being executed. Association between modular agents can be varied and transmuted according to components' own migration schemes including deployment based on biological processes. This paper presents a self-organizable architecture, which can reorganize and reconfigure a system based on modular agents. It is contrived through observation of biological phenomena, and implements a platform to host the architecture in dynamically changing environments. We draw several key features of the modular agents, describe the principles of the modular agent based self-organizable framework, and depict how the proposed framework satisfies the functional requirements of network applications, which are made of several agents. We also demonstrate the efficiency and scalability of the framework through examining some simulation results. (C) 2011 Elsevier B.V. All rights reserved. C1 [Yeom, Kiwon] NASA, Human Syst Integrat Div, Ames Res Ctr, Moffett Field, CA 94035 USA. [Yeom, Kiwon; Park, Ji-Hyung] Korea Inst Sci & Technol, Ctr Intelligence & Interact, Seoul, South Korea. RP Yeom, K (reprint author), NASA, Human Syst Integrat Div, Ames Res Ctr, Mail Stop 262-4,Bldg 262,Rm 155,POB 1, Moffett Field, CA 94035 USA. EM kiwon.yeom@nasa.gov FU University of Science and Technology FX This work was supported by University of Science and Technology through UST Post-Doc Research Program. NR 48 TC 3 Z9 4 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-739X EI 1872-7115 J9 FUTURE GENER COMP SY JI Futur. Gener. Comp. Syst. PD MAR PY 2012 VL 28 IS 3 BP 533 EP 543 DI 10.1016/j.future.2011.03.002 PG 11 WC Computer Science, Theory & Methods SC Computer Science GA 871YS UT WOS:000298774200006 ER PT J AU Slegers, NJ Kadish, RT Payton, GE Thomas, J Griffin, MD Dumbacher, D AF Slegers, Nathan J. Kadish, Ronald T. Payton, Gary E. Thomas, John Griffin, Michael D. Dumbacher, Dan TI Learning from failure in systems engineering: A panel discussion SO SYSTEMS ENGINEERING LA English DT Article DE failure; product success; risk; lessons from failure; process AB This paper summarizes the discussion of the Learning from Failure in Systems Engineering panel that was held in Huntsville, AL on November 8, 2010. The panel objective was to discuss how systems engineers respond to and learn from failure and identify future directions important to the community. The panel consisted of four representatives with experience in government, industry, and academia: (1) Ronald Kadish from Booz Allen Hamilton and former director of the Missile Defense Agency, (2) Gary Payton, retired Deputy Under Secretary of the Air Force for Space Programs, (3) John Thomas from Booz Allen Hamilton and President-elect of INCOSE, and (4) Michael Griffin from the University of Alabama, Huntsville and former NASA Administrator. Each panelist was asked to (i) provide an opening statement and elaborate on their experience with failure, (ii) describe when failure is appropriate, (iii) describe how we learn and react to failure, and (iv) identify and discuss techniques to improve how systems engineers react to failure. Several common themes arose from the discussion including: failure is an option, the importance of failure to allow reassessment, and more process is not the solution. Each of these is discussed in turn along with future directions identified for reacting to and learning from failure. (C) 2011 Wiley Periodicals, Inc. Syst Eng C1 [Slegers, Nathan J.] Univ Alabama, Dept Mech & Aerosp Engn, Huntsville, AL 35899 USA. [Kadish, Ronald T.] Booz Allen Hamilton, Ctr Excellence Acquisit & Program Management, Mclean, VA 22102 USA. [Payton, Gary E.] SCI Aerosp Inc, Fairfax Stn, VA 22039 USA. [Thomas, John] Booz Allen Hamilton, Herndon, VA 20171 USA. [Griffin, Michael D.] Univ Alabama, Ctr Syst Studies, Huntsville, AL 35899 USA. [Dumbacher, Dan] NASA, MSFC, Huntsville, AL 35812 USA. RP Slegers, NJ (reprint author), Univ Alabama, Dept Mech & Aerosp Engn, N274 Technol Hall, Huntsville, AL 35899 USA. EM slegers@mae.uah.edu; kadish_ronald@bah.com; gary.payton@sci-aero.com; thomas_john@bah.com; mdg0007@uah.edu; daniel.l.dumbacher@nasa.gov RI 李, 涵/B-4995-2012 NR 20 TC 5 Z9 5 U1 2 U2 8 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1098-1241 J9 SYSTEMS ENG JI Syst. Eng. PD SPR PY 2012 VL 15 IS 1 BP 74 EP 82 DI 10.1002/sys.20195 PG 9 WC Engineering, Industrial; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA 873JB UT WOS:000298877400006 ER PT J AU Bonamente, M Hasler, N Bulbul, E Carlstrom, JE Culverhouse, TL Gralla, M Greer, C Hawkins, D Hennessy, R Joy, M Kolodziejczak, J Lamb, JW Landry, D Leitch, EM Marrone, DP Miller, A Mroczkowski, T Muchovej, S Plagge, T Pryke, C Sharp, M Woody, D AF Bonamente, Massimiliano Hasler, Nicole Bulbul, Esra Carlstrom, John E. Culverhouse, Thomas L. Gralla, Megan Greer, Christopher Hawkins, David Hennessy, Ryan Joy, Marshall Kolodziejczak, Jeffery Lamb, James W. Landry, David Leitch, Erik M. Marrone, Daniel P. Miller, Amber Mroczkowski, Tony Muchovej, Stephen Plagge, Thomas Pryke, Clem Sharp, Matthew Woody, David TI Comparison of pressure profiles of massive relaxed galaxy clusters using the Sunyaev-Zel'dovich and x-ray data SO NEW JOURNAL OF PHYSICS LA English DT Article ID COSMIC DISTANCE SCALE; HUBBLE CONSTANT; WMAP DATA; SAMPLE; CHANDRA; GHZ; SIMULATIONS; COSMOLOGY; FRACTION AB We present the Sunyaev-Zel'dovich (SZ) effect observations of a sample of 25 massive relaxed galaxy clusters observed with the Sunyaev-Zel'dovich array (SZA), an eight-element interferometer that is part of the Combined Array for Research in Millimeter-wave Astronomy (CARMA). We performed an analysis of new SZA data and archival Chandra observations of this sample to investigate the integrated pressure-a proxy for cluster mass-determined from x-ray and SZ observations, two independent probes of the intra-cluster medium (ICM). This analysis makes use of a model for the ICM introduced by Bulbul (2010 Astrophys. J. 720 1038) which can be applied simultaneously to the SZ and x-ray data. With this model, we estimated the pressure profile for each cluster using a joint analysis of the SZ and x-ray data, and using the SZ data alone. We found that the integrated pressures measured from the x-ray and SZ data are consistent. This conclusion is in agreement with recent results obtained using WMAP and Planck data, confirming that SZ and x-ray observations of massive clusters detect the same amount of thermal pressure from the ICM. To test for possible biases introduced by our choice of model, we also fitted the SZ data using the universal pressure profile proposed by Arnaud (2010 Astron. Astrophys. 517 A92) and found consistency between the two models out to r(500) in the pressure profiles and integrated pressures. C1 [Bonamente, Massimiliano; Hasler, Nicole; Bulbul, Esra; Landry, David] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Bonamente, Massimiliano; Joy, Marshall; Kolodziejczak, Jeffery] NASA, George C Marshall Space Flight Ctr, Space Sci VP62, Huntsville, AL 35812 USA. [Carlstrom, John E.; Culverhouse, Thomas L.; Gralla, Megan; Greer, Christopher; Hennessy, Ryan; Leitch, Erik M.; Plagge, Thomas; Pryke, Clem; Sharp, Matthew] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, John E.; Culverhouse, Thomas L.; Gralla, Megan; Greer, Christopher; Hennessy, Ryan; Leitch, Erik M.; Plagge, Thomas; Pryke, Clem; Sharp, Matthew] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Carlstrom, John E.; Pryke, Clem] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Carlstrom, John E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Hawkins, David; Lamb, James W.; Muchovej, Stephen; Woody, David] CALTECH, Owens Valley Radio Observ, Big Pine, CA 93513 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Marrone, Daniel P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Miller, Amber] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Miller, Amber] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Mroczkowski, Tony] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. RP Bonamente, M (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. EM bonamem@uah.edu OI Marrone, Daniel/0000-0002-2367-1080; Mroczkowski, Tony/0000-0003-3816-5372 FU NSF [AST-0604982, AST-0838187, AST-0507545, AST-05-07161]; University of Chicago [PHY-0114422]; NASA [PF0-110077]; Chandra X-ray Center; Smithsonian Astrophysical Observatory for NASA [NAS8-03060] FX The operation of the SZA is supported by the NSF through grants AST-0604982 and AST-0838187. Partial support was also provided by grant PHY-0114422 of the University of Chicago and by NSF grants AST-0507545 and AST-05-07161 to Columbia University. The CARMA operations are supported by the NSF under a cooperative agreement and by the CARMA partner universities. Support for TM was provided by the NASA through Einstein Postdoctoral Fellowship grant number PF0-110077 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. NR 38 TC 28 Z9 28 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD FEB 29 PY 2012 VL 14 AR 025010 DI 10.1088/1367-2630/14/2/025010 PG 18 WC Physics, Multidisciplinary SC Physics GA 919GO UT WOS:000302310900001 ER PT J AU Choukroun, M Sotin, C AF Choukroun, M. Sotin, C. TI Is Titan's shape caused by its meteorology and carbon cycle? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ETHANE; ATMOSPHERE; METHANE; GAS; PHOTOCHEMISTRY; DIFFUSION; MODEL AB Titan's shape is characterized by a difference between the long equatorial radius and the polar radius that is several hundred meters larger than that predicted by the flattening due to its spin rate. The North polar region is covered by large mare filled with hydrocarbons, including ethane. Moreover global circulation models predict ethane precipitation on the polar areas. This study shows that the shape of Titan can be explained by the subsidence associated with the substitution of methane with ethane-rich liquids percolating into the crust which, as suggested by evolution models, may be composed of methane clathrate hydrates. Such substitutions have been observed in laboratory experiments. This process would provide an additional methane source as required for sustaining the presence of this constituent in Titan's atmosphere through its history. A 270 m subsidence of the polar caps is explained by the circulation of 1.5 to 6 x 10(18) kg of ethane in the top three kilometers of an initially methane-clathrate crust. This process would have operated during the last 300-1200 Myr at the present ethane production rate. Citation: Choukroun, M., and C. Sotin (2012), Is Titan's shape caused by its meteorology and carbon cycle?, Geophys. Res. Lett., 39, L04201, doi:10.1029/2011GL050747. C1 [Choukroun, M.; Sotin, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Choukroun, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 79-24, Pasadena, CA 91109 USA. EM mathieu.choukroun@jpl.nasa.gov RI Choukroun, Mathieu/F-3146-2017 OI Choukroun, Mathieu/0000-0001-7447-9139 FU NASA Astrobiology Institute; California Institute of Technology FX The authors thank M. Janssen and A. Le Gall for useful discussions, and K. Lawrence for comments that helped improve the English writing. The authors are grateful to Oded Aharonson and Francis Nimmo for constructive reviews, which helped improve on this article. This work has been conducted at the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. Support by the NASA Astrobiology Institute is acknowledged. Government sponsorship acknowledged. NR 35 TC 30 Z9 30 U1 1 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 29 PY 2012 VL 39 AR L04201 DI 10.1029/2011GL050747,2012 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 903OS UT WOS:000301128200003 ER PT J AU Nichols, JE Huang, YS AF Nichols, Jonathan E. Huang, Yongsong TI Hydroclimate of the northeastern United States is highly sensitive to solar forcing SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID HOLOCENE CLIMATE; RECORD; VARIABILITY; BOGS; PEAT; RECONSTRUCTION; NETHERLANDS; POND; SUN AB Dramatic hydrological fluctuations strongly impact human society, but the driving mechanisms for these changes are unclear. One suggested driver is solar variability, but supporting paleoclimate evidence is lacking. Therefore, long, continuous, high-resolution records from strategic locations are crucial for resolving the scientific debate regarding sensitivity of climate to solar forcing. We present a 6800-year, decadally-resolved biomarker and multidecadally-resolved hydrogen isotope record of hydroclimate from a coastal Maine peatland, The Great Heath (TGH). Regional moisture balance responds strongly and consistently to solar forcing at centennial to millennial timescales, with solar minima concurrent with wet conditions. We propose that the Arctic/North Atlantic Oscillation (AO/NAO) can amplify small solar fluctuations, producing the reconstructed hydrological variations. The Sun may be entering a weak phase, analogous to the Maunder minimum, which could lead to more frequent flooding in the northeastern US at this multidecadal timescale. Citation: Nichols, J. E., and Y. Huang (2012), Hydroclimate of the northeastern United States is highly sensitive to solar forcing, Geophys. Res. Lett., 39, L04707, doi:10.1029/2011GL050720. C1 [Nichols, Jonathan E.] Columbia Univ, Earth Inst, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Nichols, Jonathan E.; Huang, Yongsong] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Nichols, Jonathan E.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Nichols, JE (reprint author), Columbia Univ, Earth Inst, Lamont Doherty Earth Observ, 61 Rte 9W, Palisades, NY 10964 USA. EM jnichols@ldeo.columbia.edu FU National Science Foundation [0402383, 0816739, 1024144]; NASA FX We thank J.M. Russell and M.J. Previdi for critical discussion and reading of the manuscript. The research is supported by grants from National Science Foundation (0402383, 0816739, 1024144) to YH. JEN is currently supported by the NASA Postdoctoral Program. NR 29 TC 11 Z9 11 U1 2 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 29 PY 2012 VL 39 AR L04707 DI 10.1029/2011GL050720 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 903OS UT WOS:000301128200002 ER PT J AU Lu, GP Cummer, SA Blakeslee, RJ Weiss, S Beasley, WH AF Lu, Gaopeng Cummer, Steven A. Blakeslee, Richard J. Weiss, Stephanie Beasley, William H. TI Lightning morphology and impulse charge moment change of high peak current negative strokes SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TIBETAN PLATEAU; MAPPING ARRAY; HIGH-PLAINS; DISCHARGES; FLASHES; THUNDERSTORMS; FIELDS; SPRITES; PROPAGATION; INITIATION AB We have analyzed very high frequency lightning mapping observations and remote magnetic field measurements to investigate connections between lightning morphology and impulse charge moment change (iCMC) of negative cloud-to-ground (CG) strokes with high estimated peak currents. Four lightning morphologies are identified for a total of 2126 strokes within optimum detection range of the North Alabama Lightning Mapping Array, and statistical iCMC distributions are given for each of these types. Almost all (>90%) of the largest impulse charge moments (greater than -200 C km in this data set) are not produced by strokes in ordinary negative CG flashes. Instead, negative strokes with the largest iCMCs are almost exclusively associated with two unusual flash types that both initially develop as positive (normal) intracloud lightning. In the first type the negative stroke with high iCMCs results from a negative leader that descends from the midlevel negative charge region after the upper level negative leader ceases propagating. In the second type, the upper level negative leader of the intracloud lightning progresses toward ground as a so-called bolt from the blue to generate the negative stroke. Measurements of strokes associated with four negative polarity sprites suggest that all four were most likely produced in the first unusual lightning type. Our results highlight that estimated peak current and impulse charge transfer are not always well correlated and that the in-cloud lightning structure strongly influences charge transfer on short time scales in negative CG strokes. C1 [Lu, Gaopeng; Cummer, Steven A.] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA. [Blakeslee, Richard J.] NASA, Earth Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Weiss, Stephanie; Beasley, William H.] Univ Oklahoma, Sch Meteorol, Norman, OK 73019 USA. RP Lu, GP (reprint author), Duke Univ, Dept Elect & Comp Engn, Box 90291,Hudson Hall 05C, Durham, NC 27708 USA. EM gaopeng.lu@duke.edu; cummer@ee.duke.edu; rich.blakeslee@nasa.gov; stepha.weiss@gmail.com; whb@ou.edu RI Lu, Gaopeng/D-9011-2012; Cummer, Steven/A-6118-2008 OI Cummer, Steven/0000-0002-0002-0613 FU National Science Foundation; Defense Advanced Research Projects Agency FX This work was supported by the Physical and Dynamic Meteorology Program of the National Science Foundation and the NIMBUS Program of the Defense Advanced Research Projects Agency. Lucian Zigoneanu is acknowledged for routinely operating the low light level video camera in Duke Forest. NR 60 TC 27 Z9 29 U1 2 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 28 PY 2012 VL 117 AR D04212 DI 10.1029/2011JD016890 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 903PG UT WOS:000301129700002 ER PT J AU Holmes, TRH Jackson, TJ Reichle, RH Basara, JB AF Holmes, Thomas R. H. Jackson, Thomas J. Reichle, Rolf H. Basara, Jeffrey B. TI An assessment of surface soil temperature products from numerical weather prediction models using ground-based measurements SO WATER RESOURCES RESEARCH LA English DT Article ID MICROWAVE EMISSION; MOISTURE RETRIEVAL; PARAMETERIZATION; SALINITY; NETWORK; MISSION; SPACE AB Surface soil temperature estimates at approximately 0.05 m depth are needed to retrieve soil moisture from the planned Soil Moisture Active Passive (SMAP) L-band (1.4 GHz) satellite. Numerical weather prediction (NWP) systems as operated by various weather centers produce global estimates of soil temperature. In this study in situ data collected over the state of Oklahoma are used to assess surface (soil) temperature from three NWP systems: (1) the integrated forecast system from the European Center for Medium range Weather Forecasts (ECMWF), (2) the modern-era retrospective analysis for research and applications (MERRA) from the NASA Global Modeling and Assimilation Office, and (3) the global data assimilation system used by the National Center for Environmental Prediction (NCEP). The results are presented by hour of day with specific attention directed to the SMAP early morning overpass time at around 6 A. M. local time, and the period of 1 April to 1 October 2009. It was found that the NWP systems estimate the 0.05 m soil temperature at this time of day with an overall root mean square error of 1.9 to 2.0 K. It is shown that this error can be reduced to 1.6 to 1.8 K when differences between the modeling and measurement depth are accounted for by synchronizing each NWP set to match the mean phase of the in situ data and adjusting the amplitude in accordance with heat flow principles. These results indicate that with little calibration all products meet the SMAP error budget criteria over Oklahoma. C1 [Holmes, Thomas R. H.; Jackson, Thomas J.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [Basara, Jeffrey B.] Univ Oklahoma, Oklahoma Climatol Survey, Norman, OK 73072 USA. [Reichle, Rolf H.] NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Holmes, TRH (reprint author), USDA ARS, Hydrol & Remote Sensing Lab, 10300 Baltimore Ave,Rm 104,Bldg 007,BARC W, Beltsville, MD 20705 USA. EM thomas.holmes@ars.usda.gov RI Reichle, Rolf/E-1419-2012; Basara, Jeffrey/A-4907-2008; Holmes, Thomas/F-4512-2010 OI Basara, Jeffrey/0000-0002-2096-6844; Holmes, Thomas/0000-0002-4651-0079 FU State of OK through the OK State Regents for Higher Education; State of OK through the OK Department of Public Safety; NASA SMAP Science Definition Team FX The authors would like to thank the Global Modeling and Assimilation Office (GMAO) and the GES DISC (both at NASA Goddard Space Flight Center) for the dissemination of MERRA; the taxpayers of the State of OK for funding the OK mesonet through the OK State Regents for Higher Education and the OK Department of Public Safety; the European Centre for Medium range Weather Forecasting (ECMWF) for the dissemination of their data (by way of the SMAP Test bed), and the National Centers for Environmental Prediction for dissemination of GDAS data (by way of Hiroko Beaudoing of NASA's Hydrological Science Branch). Rolf Reichle was funded by the NASA SMAP Science Definition Team. The USDA is an equal opportunity provider and employer. NR 35 TC 18 Z9 19 U1 0 U2 19 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD FEB 28 PY 2012 VL 48 AR W02531 DI 10.1029/2011WR010538 PG 14 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 903QJ UT WOS:000301133200001 ER PT J AU Barge, LM Doloboff, IJ White, LM Stucky, GD Russell, MJ Kanik, I AF Barge, Laura M. Doloboff, Ivria J. White, Lauren M. Stucky, Galen D. Russell, Michael J. Kanik, Isik TI Characterization of Iron-Phosphate-Silicate Chemical Garden Structures SO LANGMUIR LA English DT Article ID CITY HYDROTHERMAL FIELD; PRECIPITATION TUBES; LIFE; ORIGIN; GROWTH AB Chemical gardens form when ferrous chloride hydrate seed crystals are added or concentrated solutions are injected into solutions of sodium silicate and potassium phosphate. Various precipitation morphologies are observed depending on silicate and phosphate concentrations, including hollow plumes, bulbs, and tubes. The growth of precipitates is controlled by the internal osmotic pressure, fluid buoyancy, and membrane strength. Additionally, rapid bubble-led growth is observed when silicate concentrations are high. ESEM/EDX analysis confirms compositional gradients within the membranes, and voltage measurements across the membranes during growth show a final potential of around 150-200 mV, indicating that electrochemical gradients are maintained across the membranes as growth proceeds. The characterization of chemical gardens formed with iron, silicate, and phosphate, three important components of an early earth prebiotic hydrothermal system, can help us understand the properties of analogous structures that likely formed at submarine alkaline hydrothermal vents in the Hadean-structures offering themselves as the hatchery of life. C1 [Barge, Laura M.; Doloboff, Ivria J.; White, Lauren M.; Russell, Michael J.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [White, Lauren M.; Stucky, Galen D.] Univ Calif Santa Barbara, Dept Chem & Biochem, Santa Barbara, CA 93106 USA. [Stucky, Galen D.] Univ Calif Santa Barbara, Dept Mat, Santa Barbara, CA 93106 USA. RP Barge, LM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM laura.m.barge@jpl.nasa.gov FU ConvEne IGERT Program [NSF-DGE 0801627]; JPL; National Aeronautics and Space Administration with support by the NASA Astrobiology Institute (Icy Worlds); NAI FX L.M.W. was supported by the ConvEne IGERT Program (NSF-DGE 0801627). M.J.R. was supported by the Research and Technology Development Program of the JPL. 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 the NASA Astrobiology Institute (Icy Worlds). We acknowledge useful discussions with members attending the first and second meetings of the NAI-sponsored Thermodynamics Disequilibrium and Evolution Focus Group. NR 34 TC 28 Z9 29 U1 3 U2 30 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0743-7463 J9 LANGMUIR JI Langmuir PD FEB 28 PY 2012 VL 28 IS 8 BP 3714 EP 3721 DI 10.1021/la203727g PG 8 WC Chemistry, Multidisciplinary; Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA 898QU UT WOS:000300757700007 PM 22035594 ER PT J AU Marcus, SL Dickey, JO Fukumori, I de Viron, O AF Marcus, S. L. Dickey, J. O. Fukumori, I. de Viron, O. TI Detection of the Earth rotation response to a rapid fluctuation of Southern Ocean circulation in November 2009 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID OF-DAY VARIATIONS; LENGTH; VARIABILITY; SIGNALS AB At seasonal and shorter periods the solid Earth and its overlying geophysical fluids form a closed dynamical system, which (except for tidal forcing) conserves its total angular momentum. While atmospheric effects dominate changes in the Earth's rate of rotation and hence length-of-day (LOD) on these time scales, the addition of oceanic angular momentum (OAM) estimates has been shown to improve closure of the LOD budget in a statistical sense. Here we demonstrate, for the first time, the signature of a specific, sub-monthly ocean current fluctuation on the Earth's rotation rate, coinciding with recently-reported anomalies which developed in southeast Pacific surface temperature and bottom pressure fields during late 2009. Our results show that concurrent variations in the Antarctic Circumpolar Current (ACC), which saw a sharp drop and recovery in zonal transport during a two-week period in November, were strong enough to cause a detectable change in LOD following the removal of atmospheric angular momentum (AAM) computed from the Modern Era Retrospective Analysis for Research and Applications (MERRA) database. The strong OAM variations driving the LOD-AAM changes were diagnosed from ocean state estimates of the Consortium for Estimating the Circulation and Climate of the Ocean (ECCO) and involved roughly equal contributions from the current and pressure terms, with in situ confirmation for the latter provided by tide-corrected bottom pressure recorder data from the South Drake Passage site of the Antarctic Circumpolar Current Levels by Altimetry and Island Measurements (ACCLAIM) network. Citation: Marcus, S. L., J. O. Dickey, I. Fukumori, and O. de Viron (2012), Detection of the Earth rotation response to a rapid fluctuation of Southern Ocean circulation in November 2009, Geophys. Res. Lett., 39, L04605, doi:10.1029/2011GL050671. C1 [Marcus, S. L.; Dickey, J. O.; Fukumori, I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [de Viron, O.] Univ Paris Diderot, IPGP, PRES Sorbonne Paris Cite, F-75005 Paris, France. RP Marcus, SL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM steven.marcus@jpl.nasa.gov RI de Viron, Olivier/N-6647-2014 OI de Viron, Olivier/0000-0003-3112-9686 FU NASA FX MERRA data used in this study have been provided by the Global Modeling and Assimilation Office (GMAO) at NASA Goddard Space Flight Center through the NASA GES DISC online archive. We thank Chris Hughes of the U.K. National Oceanography Centre and University of Liverpool for assistance in acquiring and processing the ACCLAIM bottom pressure recorder data, and three anonymous reviewers whose comments helped to improve the manuscript. The contribution of OdV to this study is IPGP contribution 3269. The work of S. L. M., J.O.D. and I. F. described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. J.O.D. would like to thank Universite Paris Diderot and Institut de Physique du Globe de Paris for their gracious hospitality during her May and June 2011 visit. NR 23 TC 1 Z9 1 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 28 PY 2012 VL 39 AR L04605 DI 10.1029/2011GL050671 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 903OQ UT WOS:000301127800003 ER PT J AU Knudsen, DJ Kabirzadeh, R Burchill, JK Pfaff, RF Wallis, DD Bounds, SR Clemmons, JH Pincon, JL AF Knudsen, D. J. Kabirzadeh, R. Burchill, J. K. Pfaff, R. F. Wallis, D. D. Bounds, S. R. Clemmons, J. H. Pincon, J. -L. TI Strong magnetic field fluctuations within filamentary auroral density cavities interpreted as VLF saucer sources SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID TRANSVERSE ION-ACCELERATION; HYBRID SOLITARY STRUCTURES; IONOSPHERE; WAVES; PLASMA; DEPLETIONS; MAGNETOSPHERE; EIGENMODES; FREJA; GRADIENTS AB The Geoelectrodynamics and Electro-Optical Detection of Electron and Suprathermal Ion Currents (GEODESIC) sounding rocket encountered more than 100 filamentary density cavities associated with enhanced plasma waves at ELF (< 3 kHz) and VLF (3-10 kHz) frequencies and at altitudes of 800-990 km during an auroral substorm. These cavities were similar in size (similar to 20 m diameter in most cases) to so-called lower-hybrid cavities (LHCs) observed by previous sounding rockets and satellites; however, in contrast, many of the GEODESIC cavities exhibited up to tenfold enhancements in magnetic wave power throughout the VLF band. GEODESIC also observed enhancements of ELF and VLF electric fields both parallel and perpendicular to the geomagnetic field B-0 within cavities, though the VLF E field increases were often not as large proportionally as seen in the magnetic fields. This behavior is opposite to that predicted by previously published theories of LHCs based on passive scattering of externally incident auroral hiss. We argue that the GEODESIC cavities are active wave generation sites capable of radiating VLF waves into the surrounding plasma and producing VLF saucers, with energy supplied by cold, upward flowing electron beams composing the auroral return current. This interpretation is supported by the observation that the most intense waves, both inside and outside cavities, occurred in regions where energetic electron precipitation was largely inhibited or absent altogether. We suggest that the wave-enhanced cavities encountered by GEODESIC were qualitatively different from those observed by earlier spacecraft because of the fortuitous timing of the GEODESIC launch, which placed the payload at apogee within a substorm-related return current during its most intense phase, lasting only a few minutes. C1 [Knudsen, D. J.; Kabirzadeh, R.; Burchill, J. K.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Knudsen, D. J.; Pfaff, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kabirzadeh, R.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. [Wallis, D. D.] Nat Resources Canada, Ottawa, ON K1A 0Y3, Canada. [Bounds, S. R.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Clemmons, J. H.] Aerosp Corp, Los Angeles, CA 90009 USA. [Pincon, J. -L.] CNRS, LPCE, F-45071 Orleans, France. RP Knudsen, DJ (reprint author), Univ Calgary, Dept Phys & Astron, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada. EM knudsen@ucalgary.ca; burchill@phys.ucalgary.ca RI Pfaff, Robert/F-5703-2012; OI Pfaff, Robert/0000-0002-4881-9715; Clemmons, James/0000-0002-5298-5222 FU Canadian Space Agency; NASA [NAG5-5201]; Natural Sciences and Engineering Research Council of Canada FX Funding for the GEODESIC project was provided by the Canadian Space Agency and NASA. The GEODESIC payload was built by Bristol Aerospace, Ltd. Magnetometer data in Figure 3 were provided by the Geophysical Institute at the University of Alaska, Fairbanks. This study was supported by the Natural Sciences and Engineering Research Council of Canada, and by NASA grant NAG5-5201. Thanks to Richard Denton and Susan Swartz of Dartmouth College for providing a Java-based user interface for WHAMP, and to John Bonnell, Anders Eriksson and Mats Andre for helpful discussions. D.J.K. wishes to thank H. deFeraudy for hosting his visit to CETP-IPSL/CNRS, Velizy, France, during which part of this work was carried out. NR 37 TC 1 Z9 2 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD FEB 25 PY 2012 VL 117 AR A02217 DI 10.1029/2011JA017316 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 899NT UT WOS:000300823500003 ER PT J AU Mitsuishi, I Gupta, A Yamasaki, NY Takei, Y Ohashi, T Sato, K Galeazzi, M Henry, JP Kelley, RL AF Mitsuishi, Ikuyuki Gupta, Anjali Yamasaki, Noriko Y. Takei, Yoh Ohashi, Takaya Sato, Kosuke Galeazzi, Massimiliano Henry, J. Patrick Kelley, Richard L. TI Search for X-Ray Emission Associated with the Shapley Supercluster with Suzaku SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE intergalactic medium; supercluster; X-rays: galaxies: clusters ID HOT INTERGALACTIC MEDIUM; WIND CHARGE-EXCHANGE; VIRIAL RADIUS; DIFFUSE EMISSION; GALAXY CLUSTERS; MISSING BARYONS; SCULPTOR WALL; COMA CLUSTER; H I; CORE AB Suzaku performed observations of 3 regions in and around the Shapley supercluster, a region located between A 3558 and A 3556, at similar to 0.9 times the virial radii of both clusters, and two other regions at 1 degrees and 4 degrees away from the first pointing. The 4 degrees-offset observation was used to evaluate the Galactic foreground emission. We did not detect significant redshifted Oxygen emission lines (O VII and O VIII) in the spectra of all three pointings, after subtracting the contribution of foreground and background emission. The upper limit for the redshifted O VIII K alpha line intensity of the warm-hot intergalactic medium (WHIM) is 1.5 x 10(-7) photons s(-1) cm(-2) arcmin-2, which corresponds to an overdensity of similar to 380 (Z/0.1 Z(circle dot))(-1/2) (L/3 Mpc)(-1/2), assuming T = 3 x 10(6) K. We found excess continuum emission in the 1 degrees-offset and on-filament regions, represented by thermal models with k T similar to 1 keV and similar to 2 keV, respectively. The redshifts of both 0 and that of the supercluster (0.048) are consistent with the observed spectra. The similar to 1 keV emission can also be fitted with Ne-rich Galactic (zero redshift) thin thermal emission. The radial intensity profile of the 2 keV component suggests contributions from A 3558 and A 3556, but with significant steepening of the intensity slope in the outer region of A 3558. Finally, we summarized the previous Suzaku search for the WHIM, and discussed the feasibility of constraining the WHIM. An overdensity of <400 could be detectable using O VII and 0 VIII emission lines in a range of 1.4 x 10(6) K < T < 5 x 10(6) K or a continuum emission in a relatively high-temperature range of T > 5 x 10(6) K with the Suzaku XIS. The non-detection with Suzaku suggests that a typical line-of-sight average overdensity is <400. C1 [Mitsuishi, Ikuyuki; Yamasaki, Noriko Y.; Takei, Yoh] Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Gupta, Anjali; Galeazzi, Massimiliano] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [Ohashi, Takaya] Tokyo Metropolitan Univ, Dept Phys, Hachioji, Tokyo 1920397, Japan. [Sato, Kosuke] Tokyo Univ Sci, Dept Phys, Shinjyuku Ku, Tokyo 1628601, Japan. [Henry, J. Patrick] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Kelley, Richard L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mitsuishi, I (reprint author), Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. EM mitsuisi@astro.isas.jaxa.jp RI Yamasaki, Noriko/C-2252-2008; Kelley, Richard/K-4474-2012; XRAY, SUZAKU/A-1808-2009 FU Ministry of Education, Culture, Sports, Science and Technology [10J07487, 15340088, 20340041, 21224003, 22111513] FX I. M. is grateful to Kentaro Someya, Hiroshi Yoshitake, Kazuhiro Sakai and Prof. Kazuhisa Mitsuda for useful advice and discussion. Part of this work was financially supported by the Ministry of Education, Culture, Sports, Science and Technology, Grant-in Aid for Scientific Research 10J07487, 15340088, 20340041, 21224003, and 22111513. NR 67 TC 6 Z9 6 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD FEB 25 PY 2012 VL 64 IS 1 AR 18 DI 10.1093/pasj/64.1.18 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905WS UT WOS:000301307500018 ER PT J AU Sun, AY Green, R Swenson, S Rodell, M AF Sun, Alexander Y. Green, Ronald Swenson, Sean Rodell, Matthew TI Toward calibration of regional groundwater models using GRACE data SO JOURNAL OF HYDROLOGY LA English DT Article DE Groundwater modeling; GRACE; Multiobjective optimization; Water budget analysis ID GENETIC ALGORITHM; FLOW; METHODOLOGY; RECHARGE; SYSTEM AB Regional groundwater models are increasingly used for short- and long-term water resources planning, in anticipation of greater climate variability and population growth. However, many of these models are subject to structural and parametric uncertainties because of the lack of field measurements. In recent years, the Gravity Recovery and Climate Experiment (GRACE) satellite mission has shown great potential for tracking total water storage changes over large regions. The pattern of groundwater storage changes inferred from GRACE may be incorporated as an additional regularization mechanism for calibrating regional groundwater models. Motivated by the demonstrated success of GRACE for monitoring groundwater storage changes, this study explores the combined use of in situ water level measurements and GRACE-derived groundwater storage changes for calibrating regional groundwater models. The resulting optimization problem is solved using an evolutionary optimization algorithm. We demonstrate the proposed calibration strategy for the hydraulically connected Edwards-Trinity Plateau and Pecos Valley aquifers (total area 115,000 km(2)) in west Texas. Monthly GRACE data from 2002 to 2007 were used to recalibrate a regional groundwater model developed for the area. Our results indicate that (i) calibration using in situ data alone may yield multiple plausible solutions, a phenomenon well known to hydrologists; and (ii) GRACE data helped further constrain model parameters over the study period and, thus, may be continuously assimilated, among other sources of data, for enhancing existing regional groundwater models. (C) 2011 Published by Elsevier B.V. C1 [Sun, Alexander Y.; Green, Ronald] SW Res Inst, Geosci & Engn Div, San Antonio, TX USA. [Swenson, Sean] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RP Sun, AY (reprint author), Univ Texas Austin, Bur Econ Geol, Jackson Sch Geosci, Austin, TX 78712 USA. EM asun@swri.org RI Rodell, Matthew/E-4946-2012; Sun, Alexander/A-9959-2011 OI Rodell, Matthew/0000-0003-0106-7437; FU Southwest Research Institute [R8501]; NASA [NNX09AR63G] FX The authors are grateful to J.L. Awange and two other anonymous reviewers for their constructive comments. A. Sun is in debt to Dr. Ian Jones for providing the original ETPV GAM model and for engaging in numerous discussions. A. Sun and R. Green were partly supported by Southwest Research Institute R&D Project R8501 and NASA Grant NNX09AR63G. NR 42 TC 22 Z9 23 U1 1 U2 26 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 J9 J HYDROL JI J. Hydrol. PD FEB 23 PY 2012 VL 422 BP 1 EP 9 DI 10.1016/j.jhydrol.2011.10.025 PG 9 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA 904OP UT WOS:000301208100001 ER PT J AU Huang, CS Retterer, JM de La Beaujardiere, O Roddy, PA Hunton, DE Ballenthin, JO Pfaff, RF AF Huang, Chao-Song Retterer, J. M. de La Beaujardiere, O. Roddy, P. A. Hunton, D. E. Ballenthin, J. O. Pfaff, R. F. TI Observations and simulations of formation of broad plasma depletions through merging process SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EQUATORIAL SPREAD-F; NONLINEAR EVOLUTION; BACKSCATTER PLUMES; DRIFTS; CLIMATOLOGY; GENERATION; JICAMARCA; BUBBLES; GROWTH AB Broad plasma depletions in the equatorial ionosphere near dawn are region in which the plasma density is reduced by 1-3 orders of magnitude over thousands of kilometers in longitude. This phenomenon is observed repeatedly by the Communication/Navigation Outage Forecasting System (C/NOFS) satellite during deep solar minimum. The plasma flow inside the depletion region can be strongly upward. The possible causal mechanism for the formation of broad plasma depletions is that the broad depletions result from merging of multiple equatorial plasma bubbles. The purpose of this study is to demonstrate the feasibility of the merging mechanism with new observations and simulations. We present C/NOFS observations for two cases. A series of plasma bubbles is first detected by C/NOFS over a longitudinal range of 3300-3800 km around midnight. Each of the individual bubbles has a typical width of similar to 100 km in longitude, and the upward ion drift velocity inside the bubbles is 200-400 m s(-1). The plasma bubbles rotate with the Earth to the dawn sector and become broad plasma depletions. The observations clearly show the evolution from multiple plasma bubbles to broad depletions. Large upward plasma flow occurs inside the depletion region over 3800 km in longitude and exists for similar to 5 h. We also present the numerical simulations of bubble merging with the physics-based low-latitude ionospheric model. It is found that two separate plasma bubbles join together and form a single, wider bubble. The simulations show that the merging process of plasma bubbles can indeed occur in incompressible ionospheric plasma. The simulation results support the merging mechanism for the formation of broad plasma depletions. C1 [Huang, Chao-Song; de La Beaujardiere, O.; Roddy, P. A.; Hunton, D. E.; Ballenthin, J. O.] USAF, Space Vehicles Directorate, Res Lab, Kirtland AFB, NM 87117 USA. [Retterer, J. M.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA. [Pfaff, R. F.] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Huang, CS (reprint author), USAF, Space Vehicles Directorate, Res Lab, 3550 Aberdeen Ave SE, Kirtland AFB, NM 87117 USA. EM chaosong.huang@kirtland.af.mil RI Pfaff, Robert/F-5703-2012 OI Pfaff, Robert/0000-0002-4881-9715 FU Air Force Office of Scientific Research (AFOSR) [FA9550-09-1-0321]; Air Force Research Laboratory; Department of Defense; National Aeronautics and Space Administration (NASA); Naval Research Laboratory; Aerospace Corporation FX Work by C.S.H. was supported by the Air Force Office of Scientific Research (AFOSR) award FA9550-09-1-0321. The C/NOFS mission is supported by the Air Force Research Laboratory, the Department of Defense Space Test Program, the National Aeronautics and Space Administration (NASA), the Naval Research Laboratory, and the Aerospace Corporation. NR 39 TC 13 Z9 13 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD FEB 23 PY 2012 VL 117 AR A02314 DI 10.1029/2011JA017084 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 899NR UT WOS:000300823200001 ER PT J AU Jepsen, SM Molotch, NP Williams, MW Rittger, KE Sickman, JO AF Jepsen, Steven M. Molotch, Noah P. Williams, Mark W. Rittger, Karl E. Sickman, James O. TI Interannual variability of snowmelt in the Sierra Nevada and Rocky Mountains, United States: Examples from two alpine watersheds SO WATER RESOURCES RESEARCH LA English DT Article ID COLORADO FRONT RANGE; HIGH-ELEVATION CATCHMENTS; LANDSAT THEMATIC MAPPER; SPATIAL-DISTRIBUTION; ENERGY EXCHANGE; COVER DATA; CLIMATE; MODEL; EQUIVALENT; SURFACE AB The distribution of snow and the energy flux components of snowmelt are intrinsic characteristics of the alpine water cycle controlling the location of source waters and the effect of climate on streamflow. Interannual variability of these characteristics is relevant to the effect of climate change on alpine hydrology. Our objective is to characterize the interannual variability in the spatial distribution of snow and energy fluxes of snowmelt in watersheds of a maritime setting, Tokopah Basin (TOK) in California's southern Sierra Nevada, and a continental setting, Green Lake 4 Valley (GLV4) in Colorado's Front Range, using a 12 year database (1996-2007) of hydrometeorological observations and satellite-derived snow cover. Snowpacks observed in GLV4 exhibit substantially greater spatial variability than in TOK (0.75 versus 0.28 spatial coefficient of variation). In addition, modeling results indicate that the net turbulent energy flux contribution to snowmelt in GLV4 is, on average, 3 times greater in magnitude (mean 29% versus 10%) and interannual variability (standard deviation 17% versus 6%) than in TOK. These energy flux values exhibit strong seasonality, increasing as the melt season progresses to times later in the year (R-2 = 0.54-0.77). This seasonality of energy flux appears to be associated with snowmelt rates that generally increase with onset date of melt (0.02 cm d(-2)). This seasonality in snowmelt rate, coupled to differences in hydrogeology, may account for the observed differences in correspondence between the timing of snowmelt and timing of streamflow in these watersheds. C1 [Jepsen, Steven M.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA. [Molotch, Noah P.; Williams, Mark W.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80303 USA. [Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Rittger, Karl E.] Univ Calif Santa Barbara, Donald Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA. [Sickman, James O.] Univ Calif Riverside, Dept Environm Sci, Riverside, CA 92521 USA. [Molotch, Noah P.; Williams, Mark W.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA. RP Jepsen, SM (reprint author), US Geol Survey, Denver Fed Ctr, Box 25046, Denver, CO 80225 USA. EM noah.molotch@colorado.edu RI Molotch, Noah/C-8576-2009 FU NSF [EAR 1032308, 1032295, 0614207, 0724960, 0738780, 0738930]; NASA [NNX08AH18G]; USGS; Niwot Ridge LTER program; NSF's Boulder Creek Critical Zone Observatory FX Technical support was provided by the following individuals : S. Burns, N. Caine, T. Erickson, M. Colee, J. M. Melack, K. Musselman, T. H. Painter, and K. Skeen. Helpful commentary on the manuscript was provided by D. W. Clow, D. I. Stannard, and 3 anonymous reviewers. Financial support was provided by NSF grants EAR 1032308, 1032295, 0614207, 0724960, 0738780, 0738930, NASA Grant NNX08AH18G, The NASA Postdoctoral Program, The USGS Mendenhall Research Fellowship Program, the Niwot Ridge LTER program, and NSF's Boulder Creek Critical Zone Observatory. Any use of trade, firm, or product names is for descriptive purposes only and does not imply endorsement by the U. S. Government. NR 71 TC 30 Z9 30 U1 2 U2 42 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 J9 WATER RESOUR RES JI Water Resour. Res. PD FEB 23 PY 2012 VL 48 AR W02529 DI 10.1029/2011WR011006 PG 15 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 899NZ UT WOS:000300824300002 ER PT J AU Archidiacono, M De Bernardis, F Cooray, A Melchiorri, A Amblard, A Pagano, L Serra, P AF Archidiacono, Maria De Bernardis, Francesco Cooray, Asantha Melchiorri, Alessandro Amblard, Alexandre Pagano, Luca Serra, Paolo TI Amplitudes of thermal and kinetic Sunyaev-Zel'dovich signals from small-scale CMB anisotropies SO PHYSICAL REVIEW D LA English DT Article ID ATACAMA COSMOLOGY TELESCOPE; SOUTH-POLE TELESCOPE; POWER SPECTRUM; BACKGROUND ANISOTROPIES; GALAXIES; FLUCTUATIONS; SIMULATIONS; PREDICTIONS; SKY AB While the arcminute-scale cosmic microwave background (CMB) anisotropies are due to secondary effects, point sources dominate the total anisotropy power spectrum. At high frequencies the point sources are primarily in the form of dusty, star-forming galaxies. Both Herschel and Planck have recently measured the anisotropy power spectrum of cosmic infrared background (CIB) generated by dusty, star-forming galaxies from degree to subarcminute angular scales, including the nonlinear clustering of these galaxies at multipoles of 3000 to 6000 relevant to CMB secondary anisotropy studies. We scale the CIB angular power spectra to CMB frequencies and interpret the combined WMAP-7 year and arcminute-scale Atacama Cosmology Telescope and South Pole Telescope CMB power spectra measurements to constrain the Sunyaev-Zel'dovich (SZ) effects. Allowing the CIB clustering amplitude to vary, we constrain the amplitudes of thermal and kinetic SZ power spectra at 150 GHz. C1 [Archidiacono, Maria; Melchiorri, Alessandro; Pagano, Luca] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Archidiacono, Maria; Melchiorri, Alessandro; Pagano, Luca] Univ Roma La Sapienza, INFN, I-00185 Rome, Italy. [De Bernardis, Francesco; Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Amblard, Alexandre; Serra, Paolo] NASA Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. RP Archidiacono, M (reprint author), Univ Roma La Sapienza, Dept Phys, Piazzale Aldo Moro 2, I-00185 Rome, Italy. RI Serra, Paolo/G-9678-2014; amblard, alexandre/L-7694-2014; OI Serra, Paolo/0000-0002-7609-3931; amblard, alexandre/0000-0002-2212-5395; Melchiorri, Alessandro/0000-0001-5326-6003 FU NSF [AST-0645427]; NASA [NNX10AD42G] FX It is a pleasure to thank Erminia Calabrese for useful suggestions and comments. M. A. thanks the group at UCI for hospitality while this research was conducted. We thank NSF AST-0645427 and NASA NNX10AD42G for support. NR 30 TC 1 Z9 1 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD FEB 22 PY 2012 VL 85 IS 4 AR 043015 DI 10.1103/PhysRevD.85.043015 PG 7 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 896MQ UT WOS:000300571500003 ER PT J AU McLinden, CA Fioletov, V Boersma, KF Krotkov, N Sioris, CE Veefkind, JP Yang, K AF McLinden, C. A. Fioletov, V. Boersma, K. F. Krotkov, N. Sioris, C. E. Veefkind, J. P. Yang, K. TI Air quality over the Canadian oil sands: A first assessment using satellite observations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID OZONE MONITORING INSTRUMENT; TROPOSPHERIC NO2; RETRIEVAL; SPACE; EMISSIONS; ALGORITHM; SO2; OMI AB Results from the first assessment of air quality over the Canadian oil sands-one of the largest industrial undertakings in human history-using satellite remote sensing observations of two pollutants, nitrogen dioxide (NO2) and sulfur dioxide (SO2), are presented. High-resolution maps were created that revealed distinct enhancements in both species over an area (roughly 30 km x 50 km) of intensive surface mining at scales of a few kilometers. The magnitude of these enhancements, quantified in terms of total mass, are comparable to the largest seen in Canada from individual sources. The rate of increase in NO2 between 2005 and 2010 was assessed at 10.4 +/- 3.5%/year and resulted from increases both in local values as well as the spatial extent of the enhancement. This is broadly consistent with both surface-measurement trends and increases in annual bitumen production. An increase in SO2 was also found, but given larger uncertainties, it is not statistically significant. Citation: McLinden, C. A., V. Fioletov, K. F. Boersma, N. Krotkov, C. E. Sioris, J. P. Veefkind, and K. Yang (2012), Air quality over the Canadian oil sands: A first assessment using satellite observations, Geophys. Res. Lett., 39, L04804, doi: 10.1029/2011GL050273. C1 [McLinden, C. A.; Fioletov, V.; Sioris, C. E.] Environm Canada, Toronto, ON M3H 5T4, Canada. [Boersma, K. F.; Veefkind, J. P.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. [Krotkov, N.; Yang, K.] NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA. [Boersma, K. F.] Eindhoven Univ Technol, Fluid Dynam Lab, NL-5600 MB Eindhoven, Netherlands. [Veefkind, J. P.] Delft Univ Technol, Delft, Netherlands. [Yang, K.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. RP McLinden, CA (reprint author), Environm Canada, 4905 Dufferin St, Toronto, ON M3H 5T4, Canada. EM chris.mclinden@ec.gc.ca RI Krotkov, Nickolay/E-1541-2012; Boersma, Klaas/H-4559-2012; OI Krotkov, Nickolay/0000-0001-6170-6750; Boersma, Klaas/0000-0002-4591-7635; Fioletov, Vitali/0000-0002-2731-5956; Sioris, Christopher/0000-0003-1168-8755 FU NASA Earth Science Division FX The authors thank the Wood Buffalo Environmental Association (WBEA) for the provision of their in-situ data. In particular, CM thanks Kevin Percy of WBEA for helpful discussions. We acknowledge the free use of tropospheric NO2 column data from the GOME, SCIAMACHY, OMI, and GOME-2 sensors from www.temis.nl. We also acknowledge the NASA Earth Science Division for funding of OMI NO2 and SO2 products development and analysis. NR 14 TC 48 Z9 49 U1 1 U2 48 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 22 PY 2012 VL 39 AR L04804 DI 10.1029/2011GL050273 PG 8 WC Geosciences, Multidisciplinary SC Geology GA 899DJ UT WOS:000300794800001 ER PT J AU Renault, L Dewitte, B Marchesiello, P Illig, S Echevin, V Cambon, G Ramos, M Astudillo, O Minnis, P Ayers, JK AF Renault, Lionel Dewitte, Boris Marchesiello, Patrick Illig, Serena Echevin, Vincent Cambon, Gildas Ramos, Marcel Astudillo, Orlando Minnis, Patrick Ayers, J. Kirk TI Upwelling response to atmospheric coastal jets off central Chile: A modeling study of the October 2000 event SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID SEA-SURFACE TEMPERATURE; SUBTROPICAL SOUTH-AMERICA; CALIFORNIA CURRENT SYSTEM; LOW-LEVEL JET; WIND STRESS; WEST-COAST; EL-NINO; EKMAN TRANSPORT; BOUNDARY-LAYER; VARIABILITY AB The spatial and temporal variability of nearshore winds in eastern boundary current systems affect the oceanic heat balance that drives sea surface temperature changes. In this study, regional atmospheric and oceanic simulations are used to document such processes during an atmospheric coastal jet event off central Chile. The event is well reproduced by the atmospheric model and is associated with the migration of an anomalous anticyclone in the southeastern Pacific region during October 2000. A robust feature of the simulation is a sharp coastal wind dropoff, which is insensitive to model resolution. As expected, the simulated oceanic response is a significant sea surface cooling. A surface heat budget analysis shows that vertical mixing is a major contributor to the cooling tendency both in the jet core area and in the nearshore zone where the magnitude of this term is comparable to the magnitude of vertical advection. Sensitivity experiments show that the oceanic response in the coastal area is sensitive to wind dropoff representation. This is because total upwelling, i.e., the sum of coastal upwelling and Ekman pumping, depends on the scale of wind dropoff. Because the latter is much larger than the upwelling scale, coastal wind dropoff has only a weak positive effect on vertical velocities driven by Ekman pumping but has a strong negative effect on coastal upwelling. Interestingly though, the weakening of coastal winds in the dropoff zone has a larger effect on vertical mixing than on vertical advection, with both effects contributing to a reduction of cooling. C1 [Renault, Lionel] Sistema Observ & Prediccio Costaner Illes Balears, Palma De Mallorca, Spain. [Ramos, Marcel; Astudillo, Orlando] Univ Catolica Norte, Fac Ciencias Mar, CEAZA, Coquimbo, Chile. [Ayers, J. Kirk] SSAI, Hampton, VA 23681 USA. [Dewitte, Boris; Marchesiello, Patrick; Illig, Serena; Cambon, Gildas] IRD, Lab Etud Geophys & Oceanog Spatiale, F-31400 Toulouse 9, France. [Echevin, Vincent] IRD, Lab Oceanog & Climat Expt & Approches Numer, F-31400 Toulouse 9, France. [Minnis, Patrick] NASA, Climate Sci Branch, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA. RP Renault, L (reprint author), SOCIB, Parc Bit,Bloc A 2p Pta 3, E-07121 Palma De Mallorca, Spain. EM lrenault@imedea.uib-csic.es RI Cambon, Gildas/A-1882-2016; Minnis, Patrick/G-1902-2010; OI Cambon, Gildas/0000-0002-3899-1204; Minnis, Patrick/0000-0002-4733-6148; Renault, Lionel/0000-0002-3001-2091; ECHEVIN, Vincent/0000-0003-3859-840X FU CNES; NASA; NOAA PACS [NA00AANRG0330]; FONDECYT [1080606]; INNOVA-CHILE [07CN13 IXM-150] FX The altimeter products were produced by SSALTO-DUACS and distributed by AVISO with support from CNES. TMI data are produced by Remote Sensing Systems and sponsored by the NASA Earth Science REASoN DISCOVER Project. The QuikSCAT winds were obtained from CERSAT at IFREMER (Plouzane, France) and Distributed Active Archive Center (PO. DAAC) at the NASA Jet Propulsion Laboratory. We wish to thank Rene Garreaud and Mark Falvey for their support in the early stages of this study, Xavier Capet for helpful discussions, and three anonymous reviewers for their constructive comments that helped to improve the manuscript. Patrick Minnis and Kirk Ayers were supported by the NOAA PACS Program under NOAA agreement NA00AANRG0330 and the NASA Modeling and Analysis Program. Lionel Renault would like to extend his thanks to Joaquin Tintore and Guillermo Vizoso as well as the "Sistema d'observacio i predicciocostaner de les Illes Balears" (SOCIB) for their support during this study. M. Ramos is grateful for support from FONDECYT grant 1080606 and INNOVA-CHILE (project 07CN13 IXM-150). NR 76 TC 16 Z9 16 U1 0 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD FEB 21 PY 2012 VL 117 AR C02030 DI 10.1029/2011JC007446 PG 21 WC Oceanography SC Oceanography GA 899NA UT WOS:000300821500002 ER PT J AU Carter, LM Neish, CD Bussey, DBJ Spudis, PD Patterson, GW Cahill, JT Raney, RK AF Carter, Lynn M. Neish, Catherine D. Bussey, D. B. J. Spudis, Paul D. Patterson, G. Wesley Cahill, Joshua T. Raney, R. Keith TI Initial observations of lunar impact melts and ejecta flows with the Mini-RF radar SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID VENUS; MAGELLAN; CRATERS; STRATIGRAPHY; EMPLACEMENT; MORPHOLOGY; OUTFLOWS; FLUID AB The Mini-RF radar on the Lunar Reconnaissance Orbiter spacecraft has revealed a great variety of crater ejecta flow and impact melt deposits, some of which were not observed in prior radar imaging. The craters Tycho and Glushko have long melt flows that exhibit variations in radar backscatter and circular polarization ratio along the flow. Comparison with optical imaging reveals that these changes are caused by features commonly seen in terrestrial lava flows, such as rafted plates, pressure ridges, and ponding. Small (<20 km) sized craters also show a large variety of deposits, including melt flows and ponds. Two craters have flow features that may be ejecta flows caused by entrained debris flowing across the surface rather than by melted rock. The circular polarization ratios (CPRs) of the impact melt flows are typically very high; even ponded areas have CPR values between 0.7 and 1.0. This high CPR suggests that deposits that appear smooth in optical imagery may be rough at centimeter- and decimeter-scales. In some places, ponds and flows are visible with no easily discernable source crater. These melt deposits may have come from oblique impacts that are capable of ejecting melted material farther downrange. They may also be associated with older, nearby craters that no longer have a radar-bright proximal ejecta blanket. The observed morphology of the lunar crater flows has implications for similar features observed on Venus. In particular, changes in backscatter along many of the ejecta flows are probably caused by features typical of lava flows. C1 [Carter, Lynn M.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Neish, Catherine D.; Bussey, D. B. J.; Patterson, G. Wesley; Cahill, Joshua T.; Raney, R. Keith] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Spudis, Paul D.] Lunar & Planetary Inst, Houston, TX 77058 USA. RP Carter, LM (reprint author), NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA. EM lynn.m.carter@nasa.gov RI Carter, Lynn/D-2937-2012; Neish, Catherine/G-6321-2012; Cahill, Joshua/I-3656-2012 OI Cahill, Joshua/0000-0001-6874-5533 FU NASA LRO [NNX08AM80G] FX We thank the Mini-RF engineering and operations teams for their work in building the instrument and acquiring the data. We also thank the LRO LROC and Kaguya (SELENE) Terrain Camera teams for their efforts to provide the publicly available data sets used in this work. Thanks to Veronica Bray and Wenzhe Fa who provided detailed and helpful reviews. This project was supported through a NASA LRO Participating Scientist grant (NNX08AM80G) to L. Carter. NR 30 TC 22 Z9 23 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB 21 PY 2012 VL 117 AR E00H09 DI 10.1029/2011JE003911 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 899NP UT WOS:000300823000001 ER PT J AU Bahadori, AA Van Baalen, M Shavers, MR Semones, EJ Bolch, WE AF Bahadori, Amir A. Van Baalen, Mary Shavers, Mark R. Semones, Edward J. Bolch, Wesley E. TI Dosimetric impacts of microgravity: an analysis of 5th, 50th and 95th percentile male and female astronauts SO PHYSICS IN MEDICINE AND BIOLOGY LA English DT Article ID RADIATION PROTECTION DOSIMETRY; ADULT VOXEL PHANTOM; BODY-MASS CHANGES; HUMAN PHYSIOLOGY; SPACE-FLIGHT; BONE; SPACEFLIGHT AB Computational phantoms serve an important role in organ dosimetry and risk assessment performed at the National Aeronautics and Space Administration (NASA). A previous study investigated the impact on organ dose equivalents and effective doses from the use of the University of Florida hybrid adult male (UFHADM) and adult female (UFHADF) phantoms at differing height and weight percentiles versus those given by the two existing NASA phantoms, the computerized anatomical man (CAM) and female (CAF) (Bahadori et al 2011 Phys. Med. Biol. 56 1671-94). In the present study, the UFHADM and UFHADF phantoms of different body sizes were further altered to incorporate the effects of microgravity. Body self-shielding distributions are generated using the voxel-based ray tracer (VoBRaT), and the results are combined with depth dose data from the NASA codes BRYNTRN and HZETRN to yield organ dose equivalents and their rates for a variety of space radiation environments. It is found that while organ dose equivalents are indeed altered by the physiological effects of microgravity, the magnitude of the change in overall risk (indicated by the effective dose) is minimal for the spectra and simplified shielding configurations considered. The results also indicate, however, that UFHADMand UFHADF could be useful in designing dose reduction strategies through optimized positioning of an astronaut during encounters with solar particle events. C1 [Bahadori, Amir A.; Bolch, Wesley E.] Univ Florida, Gainesville, FL 32611 USA. [Bahadori, Amir A.] Univ Houston Downtown, Houston, TX 77002 USA. [Van Baalen, Mary; Semones, Edward J.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Shavers, Mark R.] Wyle Integrated Sci & Engn, Houston, TX 77058 USA. RP Bolch, WE (reprint author), Univ Florida, Gainesville, FL 32611 USA. EM wbolch@ufl.edu FU NASA GSRP [NNX09AK14H]; NASA Bioastronautics [NAS9-02078] FX This work was supported by NASA GSRP grant NNX09AK14H and NASA Bioastronautics Contract NAS9-02078. NR 32 TC 1 Z9 2 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0031-9155 J9 PHYS MED BIOL JI Phys. Med. Biol. PD FEB 21 PY 2012 VL 57 IS 4 BP 1047 EP 1070 DI 10.1088/0031-9155/57/4/1047 PG 24 WC Engineering, Biomedical; Radiology, Nuclear Medicine & Medical Imaging SC Engineering; Radiology, Nuclear Medicine & Medical Imaging GA 895IV UT WOS:000300490700013 PM 22298248 ER PT J AU Abramowski, A Acero, F Aharonian, F Akhperjanian, AG Anton, G Balzer, A Barnacka, A de Almeida, UB Becherini, Y Becker, J Behera, B Bernlohr, K Birsin, E Biteau, J Bochow, A Boisson, C Bolmont, J Bordas, P Brucker, J Brun, F Brun, P Bulik, T Busching, I Carrigan, S Casanova, S Cerruti, M Chadwick, PM Charbonnier, A Chaves, RCG Cheesebrough, A Clapson, AC Coignet, G Cologna, G Conrad, J Dalton, M Daniel, MK Davids, ID Degrange, B Deil, C Dickinson, HJ Djannati-Atai, A Domainko, W Drury, LO Dubus, G Dutson, K Dyks, J Dyrda, M Egberts, K Eger, P Espigat, P Fallon, L Farnier, C Fegan, S Feinstein, F Fernandes, MV Fiasson, A Fontaine, G Forster, A Fussling, M Gallant, YA Gast, H Gerard, L Gerbig, D Giebels, B Glicenstein, 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CA HESS Collaboration MAGIC Collaboration VERITAS Collaboration TI THE 2010 VERY HIGH ENERGY gamma-RAY FLARE AND 10 YEARS OF MULTI-WAVELENGTH OBSERVATIONS OF M 87 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (M 87); galaxies: jets; galaxies: nuclei; gamma rays: galaxies; radiation mechanisms: non-thermal ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; SUPERMASSIVE BLACK-HOLE; RADIO GALAXY M87; BASE-LINE ARRAY; TEV EMISSION; CRAB-NEBULA; UNIFIED SCHEMES; SCALE JETS; INNER JET AB The giant radio galaxy M 87 with its proximity (16 Mpc), famous jet, and very massive black hole ((3-6) x 10(9) M-circle dot) provides a unique opportunity to investigate the origin of very high energy (VHE; E > 100 GeV) gamma-ray emission generated in relativistic outflows and the surroundings of supermassive black holes. M 87 has been established as a VHE gamma-ray emitter since 2006. The VHE gamma-ray emission displays strong variability on timescales as short as a day. In this paper, results from a joint VHE monitoring campaign on M 87 by the MAGIC and VERITAS instruments in 2010 are reported. During the campaign, a flare at VHE was detected triggering further observations at VHE (H.E.S.S.), X-rays (Chandra), and radio (43 GHz Very Long Baseline Array, VLBA). The excellent sampling of the VHE gamma-ray light curve enables one to derive a precise temporal characterization of the flare: the single, isolated flare is well described by a two-sided exponential function with significantly different flux rise and decay times of tau(rise)(d) = (1.69 +/- 0.30) days and tau(decay)(d) = (0.611 +/- 0.080) days, respectively. While the overall variability pattern of the 2010 flare appears somewhat different from that of previous VHE flares in 2005 and 2008, they share very similar timescales (similar to day), peak fluxes (Phi(>0.35 TeV) similar or equal to (1-3) x 10(-11) photons cm(-2) s(-1)), and VHE spectra. VLBA radio observations of 43 GHz of the inner jet regions indicate no enhanced flux in 2010 in contrast to observations in 2008, where an increase of the radio flux of the innermost core regions coincided with a VHE flare. On the other hand, Chandra X-ray observations taken similar to 3 days after the peak of the VHE gamma-ray emission reveal an enhanced flux from the core (flux increased by factor similar to 2; variability timescale <2 days). The long-term (2001-2010) multi-wavelength (MWL) light curve of M 87, spanning from radio to VHE and including data from Hubble Space Telescope, Liverpool Telescope, Very Large Array, and European VLBI Network, is used to further investigate the origin of the VHE gamma-ray emission. No unique, common MWL signature of the three VHE flares has been identified. In the outer kiloparsec jet region, in particular in HST-1, no enhanced MWL activity was detected in 2008 and 2010, disfavoring it as the origin of the VHE flares during these years. Shortly after two of the three flares (2008 and 2010), the X-ray core was observed to be at a higher flux level than its characteristic range (determined from more than 60 monitoring observations: 2002-2009). In 2005, the strong flux dominance of HST-1 could have suppressed the detection of such a feature. Published models for VHE gamma-ray emission from M 87 are reviewed in the light of the new data. C1 [Abramowski, A.; Fernandes, M. 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RP Abramowski, A (reprint author), Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany. EM martin.raue@desy.de; stawarz@astro.isas.jaxa.jp; colin@mppmu.mpg.de; mazin@ifae.es; beilicke@physics.wustl.edu; cmhui@physics.utah.edu RI Font, Lluis/L-4197-2014; Contreras Gonzalez, Jose Luis/K-7255-2014; Maneva, Galina/L-7120-2016; Temnikov, Petar/L-6999-2016; Massaro, Francesco/L-9102-2016; Makariev, Martin/M-2122-2016; Torres, Diego/O-9422-2016; Drury, Luke/B-1916-2017; Barrio, Juan/L-3227-2014; Moulin, Emmanuel/B-5959-2017; Martinez Rodriguez, Manel/C-2539-2017; Cortina, Juan/C-2783-2017; Lopez Moya, Marcos/L-2304-2014; Moralejo Olaizola, Abelardo/M-2916-2014; Ribo, Marc/B-3579-2015; Katarzynski, Krzysztof/G-4528-2014; Jamrozy, Marek/F-4507-2015; Casanova, Sabrina/J-8935-2013; Antoranz, Pedro/H-5095-2015; Anton, Gisela/C-4840-2013; Khassen, Yerbol/I-3806-2015; Delgado, Carlos/K-7587-2014; Nieto, Daniel/J-7250-2015; Miranda, Jose Miguel/F-2913-2013; Daniel, Michael/A-2903-2010; Braun, Isabel/C-9373-2012; Prada Moroni, Pier Giorgio/G-5565-2011; Mannheim, Karl/F-6705-2012; Reimer, Olaf/A-3117-2013; van Eldik, Christopher/C-3901-2013; Katz, Uli/E-1925-2013; Cara, Mihai/G-1023-2013; Tjus, Julia/G-8145-2012; Fontaine, Gerard/D-6420-2014; Venter, Christo/E-6884-2011; Rico, Javier/K-8004-2014; Fernandez, Ester/K-9734-2014; Komin, Nukri/J-6781-2015; Fonseca Gonzalez, Maria Victoria/I-2004-2015; Backes, Michael/N-5126-2016; Reichardt, Ignasi/P-7478-2016 OI Giovannini, Gabriele/0000-0003-4916-6362; Prada Moroni, Pier Giorgio/0000-0001-9712-9916; Chadwick, Paula/0000-0002-1468-2685; Kneiske, Tanja M./0000-0002-3210-6200; LA BARBERA, ANTONINO/0000-0002-5880-8913; Font, Lluis/0000-0003-2109-5961; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Temnikov, Petar/0000-0002-9559-3384; Massaro, Francesco/0000-0002-1704-9850; Torres, Diego/0000-0002-1522-9065; Drury, Luke/0000-0002-9257-2270; Barrio, Juan/0000-0002-0965-0259; Moulin, Emmanuel/0000-0003-4007-0145; Cortina, Juan/0000-0003-4576-0452; Cui, Wei/0000-0002-6324-5772; Lopez Moya, Marcos/0000-0002-8791-7908; Moralejo Olaizola, Abelardo/0000-0002-1344-9080; Casanova, Sabrina/0000-0002-6144-9122; Antoranz, Pedro/0000-0002-3015-3601; Anton, Gisela/0000-0003-2039-4724; Khassen, Yerbol/0000-0002-7296-3100; Delgado, Carlos/0000-0002-7014-4101; Nieto, Daniel/0000-0003-3343-0755; Miranda, Jose Miguel/0000-0002-1472-9690; Daniel, Michael/0000-0002-8053-7910; Braun, Isabel/0000-0002-9389-0502; Reimer, Olaf/0000-0001-6953-1385; van Eldik, Christopher/0000-0001-9669-645X; Katz, Uli/0000-0002-7063-4418; Venter, Christo/0000-0002-2666-4812; Rico, Javier/0000-0003-4137-1134; Cesarini, Andrea/0000-0002-8611-8610; leonardo, elvira/0000-0003-0271-7673; de los Reyes Lopez, Raquel/0000-0003-0485-9552; Komin, Nukri/0000-0003-3280-0582; De Lotto, Barbara/0000-0003-3624-4480; Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; Backes, Michael/0000-0002-9326-6400; Reichardt, Ignasi/0000-0003-3694-3820 FU Namibian authorities; German Ministry for Education and Research (BMBF); Max Planck Society; French Ministry for Research; CNRS-IN2P3; CNRS; U.K. Science and Technology Facilities Council (STFC); IPNP of the Charles University; Polish Ministry of Science and Higher Education; South African Department of Science and Technology; National Research Foundation; University of Namibia; German BMBF; German MPG; Italian INFN; Swiss National Fund SNF; Spanish MICINN; Bulgarian NSF [CSD2007-00042, CSD2009-00064, DO02-353]; Academy of Finland [127740]; YIP of the Helmholtz Gemeinschaft; DFG Cluster of Excellence "Origin and Structure of the Universe,"; DFG Collaborative Research Centers [SFB823/C4, SFB876/C3]; Polish MNiSzW [745/N-HESS-MAGIC/2010/0]; US Department of Energy Office of Science; US National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland (SFI) [10/RFP/AST2748]; STFC in the UK; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; NASA [GO0-11120X]; Associated Universities, Inc.; European Community [227290] FX The H.E.S.S. Collaboration acknowledges support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S., as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the U.K. Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Polish Ministry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation, and by the University of Namibia. We appreciate the excellent work of the technical support staff in Berlin, Durham, Hamburg, Heidelberg, Palaiseau, Paris, Saclay, and in Namibia in the construction and operation of the equipment.; The MAGIC Collaboration thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos 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. This work was also supported by the Marie Curie program, by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant DO02-353 of the Bulgarian NSF, by grant 127740 of the Academy of Finland, by the YIP of the Helmholtz Gemeinschaft, 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.; The VERITAS Collaboration acknowledges support from the US Department of Energy Office of Science, the US National Science Foundation, and the Smithsonian Institution, from NSERC in Canada, from Science Foundation Ireland (SFI 10/RFP/AST2748), and from STFC in the UK. We acknowledge the excellent work of the technical support staff at the FLWO and at the collaborating institutions in the construction and operation of the instrument.; The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France.; Analysis of the Chandra data was supported by NASA grant GO0-11120X.; The Very Long Baseline Array is operated by the National Radio Astronomy Observatory, a facility of the NSF, operated under cooperative agreement by Associated Universities, Inc.; The European VLBI Network is a joint facility of European, Chinese, South African, and other radio astronomy institutes funded by their national research councils. This effort is supported by the European Community Framework Programme 7, Advanced Radio Astronomy in Europe, grant agreement no. 227290. NR 107 TC 59 Z9 61 U1 3 U2 42 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 151 DI 10.1088/0004-637X/746/2/151 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300037 ER PT J AU Howell, SB Rowe, JF Bryson, ST Quinn, SN Marcy, GW Isaacson, H Ciardi, DR Chaplin, WJ Metcalfe, TS Monteiro, MJPFG Appourchaux, T Basu, S Creevey, OL Gilliland, RL Quirion, PO Stello, D Kjeldsen, H Christensen-Dalsgaard, J Elsworth, Y Garcia, RA Houdek, G Karoff, C Molenda-Zakowicz, J Thompson, MJ Verner, GA Torres, G Fressin, F Crepp, JR Adams, E Dupree, A Sasselov, DD Dressing, CD Borucki, WJ Koch, DG Lissauer, JJ Latham, DW Buchhave, LA Gautier, TN Everett, M Horch, E Batalha, NM Dunham, EW Szkody, P Silva, DR Mighell, K Holberg, J Ballot, J Bedding, TR Bruntt, H Campante, TL Handberg, R Hekker, S Huber, D Mathur, S Mosser, B Regulo, C White, TR Christiansen, JL Middour, CK Haas, MR Hall, JR Jenkins, JM McCaulif, S Fanelli, MN Kulesa, C McCarthy, D Henze, CE AF Howell, Steve B. Rowe, Jason F. Bryson, Stephen T. Quinn, Samuel N. Marcy, Geoffrey W. Isaacson, Howard Ciardi, David R. Chaplin, William J. Metcalfe, Travis S. Monteiro, Mario J. P. F. G. Appourchaux, Thierry Basu, Sarbani Creevey, Orlagh L. Gilliland, Ronald L. Quirion, Pierre-Olivier Stello, Denis Kjeldsen, Hans Christensen-Dalsgaard, Jorgen Elsworth, Yvonne Garcia, Rafael A. Houdek, Guenter Karoff, Christoffer Molenda-Zakowicz, Joanna Thompson, Michael J. Verner, Graham A. Torres, Guillermo Fressin, Francois Crepp, Justin R. Adams, Elisabeth Dupree, Andrea Sasselov, Dimitar D. Dressing, Courtney D. Borucki, William J. Koch, David G. Lissauer, Jack J. Latham, David W. Buchhave, Lars A. Gautier, Thomas N., III Everett, Mark Horch, Elliott Batalha, Natalie M. Dunham, Edward W. Szkody, Paula Silva, David R. Mighell, Ken Holberg, Jay Ballot, Jerome Bedding, Timothy R. Bruntt, Hans Campante, Tiago L. Handberg, Rasmus Hekker, Saskia Huber, Daniel Mathur, Savita Mosser, Benoit Regulo, Clara White, Timothy R. Christiansen, Jessie L. Middour, Christopher K. Haas, Michael R. Hall, Jennifer R. Jenkins, Jon M. McCaulif, Sean Fanelli, Michael N. Kulesa, Craig McCarthy, Don Henze, Christopher E. TI KEPLER-21b: A 1.6 R-Earth PLANET TRANSITING THE BRIGHT OSCILLATING F SUBGIANT STAR HD 179070 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: activity; stars: individual (HD 179070: KIC 3632418); stars: interiors; stars: late-type; stars: magnetic field; stars: oscillations (including pulsations); techniques: photometric ID SOLAR-TYPE STARS; SUN-LIKE STAR; TIMING VARIATIONS; INITIAL CHARACTERISTICS; ASTEROSEISMIC DATA; BLEND SCENARIOS; MULTIPLE SYSTEM; LIGHT CURVES; SUPER-EARTHS; CADENCE DATA AB We present Kepler observations of the bright (V = 8.3), oscillating star HD 179070. The observations show transit-like events which reveal that the star is orbited every 2.8 days by a small, 1.6 R-Earth object. Seismic studies of HD 179070 using short cadence Kepler observations show that HD 179070 has a frequency-power spectrum consistent with solar-like oscillations that are acoustic p-modes. Asteroseismic analysis provides robust values for the mass and radius of HD 179070, 1.34 +/- 0.06 M-circle dot and 1.86 +/- 0.04 R-circle dot, respectively, as well as yielding an age of 2.84 +/- 0.34 Gyr for this F5 subgiant. Together with ground-based follow-up observations, analysis of the Kepler light curves and image data, and blend scenario models, we conservatively show at the >99.7% confidence level (3 sigma) that the transit event is caused by a 1.64 +/- 0.04 R-Earth exoplanet in a 2.785755 +/- 0.000032 day orbit. The exoplanet is only 0.04 AU away from the star and our spectroscopic observations provide an upper limit to its mass of similar to 10 M-Earth (2 sigma). HD 179070 is the brightest exoplanet host star yet discovered by Kepler. C1 [Howell, Steve B.; Everett, Mark; Silva, David R.; Mighell, Ken] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Middour, Christopher K.; Hall, Jennifer R.; McCaulif, Sean] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. [Fanelli, Michael N.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Rowe, Jason F.; Christiansen, Jessie L.; Jenkins, Jon M.] SETI Inst, Mountain View, CA 94043 USA. [Quinn, Samuel N.; Torres, Guillermo; Fressin, Francois; Adams, Elisabeth; Dupree, Andrea; Sasselov, Dimitar D.; Dressing, Courtney D.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Chaplin, William J.; Elsworth, Yvonne; Karoff, Christoffer; Verner, Graham A.; Hekker, Saskia] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Metcalfe, Travis S.; Thompson, Michael J.; Mathur, Savita] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Metcalfe, Travis S.; Thompson, Michael J.; Mathur, Savita] Natl Ctr Atmospher Res, Div Comp Sci, Boulder, CO 80307 USA. [Monteiro, Mario J. P. F. G.; Campante, Tiago L.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Appourchaux, Thierry] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France. [Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Creevey, Orlagh L.; Bruntt, Hans; Regulo, Clara] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Creevey, Orlagh L.; Regulo, Clara] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Quirion, Pierre-Olivier] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. [Stello, Denis; Bedding, Timothy R.; Huber, Daniel; White, Timothy R.] Univ Sydney, Sydney Inst Astron SIfA, Sch Phys, Sydney, NSW 2006, Australia. [Kjeldsen, Hans; Christensen-Dalsgaard, Jorgen; Campante, Tiago L.; Handberg, Rasmus] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Garcia, Rafael A.] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS,IRFU,SAp, F-91191 Gif Sur Yvette, France. [Houdek, Guenter] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Molenda-Zakowicz, Joanna] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Verner, Graham A.] Univ London, Astron Unit, London E1 4NS, England. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crepp, Justin R.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Szkody, Paula] Univ Washington, Dept Astron, Seattle, WA USA. [Holberg, Jay] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85726 USA. [Ballot, Jerome] Univ Toulouse, Lab Astrophys Toulouse Tarbes, CNRS, F-31400 Toulouse, France. [Mosser, Benoit] Univ Paris 07, Univ Paris 06, LESIA, CNRS,Observ Paris, F-92195 Meudon, France. [Kulesa, Craig; McCarthy, Don] Univ Arizona, Steward Observ, Tucson, AZ 85726 USA. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. RP Howell, SB (reprint author), Natl Opt Astron Observ, Tucson, AZ 85719 USA. RI Ballot, Jerome/G-1019-2010; Monteiro, Mario J.P.F.G./B-4715-2008; Karoff, Christoffer/L-1007-2013; OI Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Karoff, Christoffer/0000-0003-2009-7965; Buchhave, Lars A./0000-0003-1605-5666; Bedding, Timothy/0000-0001-5943-1460; Basu, Sarbani/0000-0002-6163-3472 FU National Aeronautics and Space Administration FX We thank John Johnson for use of some of his Keck Time. This research has made use of the NASA/IPAC/NExScI Star and Exoplanet Database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The authors thank the Kepler Science Office and the Science Operations Center personal for their dedicated effort to the mission and for providing us access to the science office data products. The ground-based observations reported on herein were obtained at Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA. NR 90 TC 73 Z9 73 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 123 DI 10.1088/0004-637X/746/2/123 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300009 ER PT J AU Hwang, U Laming, JM AF Hwang, Una Laming, J. Martin TI A CHANDRA X-RAY SURVEY OF EJECTA IN THE CASSIOPEIA A SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; ISM: individual objects (Cassiopeia A); ISM: supernova remnants; X-rays: ISM ID CORE-COLLAPSE SUPERNOVAE; ISOLATED RADIO PULSARS; A SUPERNOVA; NEUTRON-STAR; 3-DIMENSIONAL STRUCTURE; ACCELERATED ELECTRONS; GAMMA-RAY; CAS-A; INTERSTELLAR-MEDIUM; DRIVEN SUPERNOVA AB We present a survey of the X-ray-emitting ejecta in the Cassiopeia A supernova remnant (SNR) based on an extensive analysis of over 6000 spectral regions extracted on 2.'' 5-10 '' angular scales using the Chandra 1 Ms observation. We interpret these results in the context of hydrodynamical models for the evolution of the remnant. The distributions of fitted temperature and ionization age, and the implied mass coordinates, are highly peaked and suggest that the ejecta were subjected to multiple secondary shocks following reverse shock interaction with ejecta inhomogeneities. Based on the fitted emission measure and element abundances, and an estimate of the emitting volume, we derive masses for the X-ray-emitting ejecta and also show the distribution of the mass of various elements over the remnant. An upper limit to the total shocked Fe mass visible in X-rays appears to be roughly 0.13 M-circle dot, which accounts for nearly all of the mass expected in Fe ejecta. We find two populations of Fe ejecta, that associated with normal Si burning and that possibly associated with alpha-rich freezeout, with a mass ratio of approximately 2:1. Essentially all of the observed Fe (both components) lies well outside the central regions of the SNR, possibly having been ejected by hydrodynamic instabilities during the explosion. We discuss this and its implications for the neutron star kick. C1 [Hwang, Una] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hwang, Una] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21210 USA. [Laming, J. Martin] USN, Res Lab, Washington, DC 20375 USA. RP Hwang, U (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Una.Hwang-1@gsfc.nasa.gov; laming@nrl.navy.mil FU NASA [NNH04ZSS001N]; Office of Naval Research FX We thank Roger Chevalier, Elisabetta Micelotta, Rob Petre, and the referee for helpful comments on the paper. We gratefully acknowledge support through NASA grants to the Chandra Guest Observer Program and NNH04ZSS001N to the Long Term Space Astrophysics Program. J.M.L. was also supported by basic research funds of the Office of Naval Research. NR 109 TC 68 Z9 68 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 130 DI 10.1088/0004-637X/746/2/130 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300016 ER PT J AU Kim, RS Gopalswamy, N Moon, YJ Cho, KS Yashiro, S AF Kim, R. -S. Gopalswamy, N. Moon, Y. -J. Cho, K. -S. Yashiro, S. TI MAGNETIC FIELD STRENGTH IN THE UPPER SOLAR CORONA USING WHITE-LIGHT SHOCK STRUCTURES SURROUNDING CORONAL MASS EJECTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; methods: statistical; shock waves; Sun: corona; Sun: coronal mass ejections ID FARADAY-ROTATION MEASUREMENTS; STANDOFF DISTANCE; ELECTRON-DENSITY; DRIVEN SHOCK; RADIO-BURSTS; LARGE-ANGLE; II BURSTS; WAVES; SDO/AIA; ORIGIN AB To measure the magnetic field strength in the solar corona, we examined 10 fast (>= 1000 km s(-1)) limb coronal mass ejections(CMEs) that show clear shock structures in Solar and Heliospheric Observatory/Large Angle and Spectrometric Coronagraph images. By applying the piston-shock relationship to the observed CME's standoff distance and electron density compression ratio, we estimated the Mach number, Alfven speed, and magnetic field strength in the height range 3-15 solar radii (R-s). The main results from this study are as follows: (1) the standoff distance observed in the solar corona is consistent with those from a magnetohydrodynamic model and near-Earth observations; (2) the Mach number as a shock strength is in the range 1.49-3.43 from the standoff distance ratio, but when we use the density compression ratio, the Mach number is in the range 1.47-1.90, implying that the measured density compression ratio is likely to be underestimated owing to observational limits; (3) the Alfven speed ranges from 259 to 982 km s(-1) and the magnetic field strength is in the range 6-105 mG when the standoff distance is used; (4) if we multiply the density compression ratio by a factor of two, the Alfven speeds and the magnetic field strengths are consistent in both methods; and (5) the magnetic field strengths derived from the shock parameters are similar to those of empirical models and previous estimates. C1 [Kim, R. -S.; Gopalswamy, N.; Cho, K. -S.; Yashiro, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Moon, Y. -J.] Kyung Hee Univ, Sch Space Res, Yongin 446701, South Korea. RP Kim, RS (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. EM rok-soon.kim@nasa.gov RI Gopalswamy, Nat/D-3659-2012; Moon, Yong-Jae/E-1711-2013; OI Gopalswamy, Nat/0000-0001-5894-9954 FU WCU [R31-10016]; National Research Foundation of Korea [20090071744, 20100014501]; Ministry of Education, Science and Technology; Development of Korean Space Weather Center; KASI FX Y.-J.M. has been supported by the WCU program (No. 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. K.-S.C. is supported by the Development of Korean Space Weather Center, a project of KASI, and the KASI basic research fund. NR 53 TC 24 Z9 24 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 118 DI 10.1088/0004-637X/746/2/118 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300004 ER PT J AU Ragland, S Ohnaka, K Hillenbrand, L Ridgway, ST Colavita, MM Akeson, RL Cotton, W Danchi, WC Hrynevich, M Millan-Gabet, R Traub, WA AF Ragland, S. Ohnaka, K. Hillenbrand, L. Ridgway, S. T. Colavita, M. M. Akeson, R. L. Cotton, W. Danchi, W. C. Hrynevich, M. Millan-Gabet, R. Traub, W. A. TI FIRST KECK NULLING OBSERVATIONS OF A YOUNG STELLAR OBJECT: PROBING THE CIRCUMSTELLAR ENVIRONMENT OF THE HERBIG Ae STAR MWC325 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; radiative transfer; stars: individual (MWC325); stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be; techniques: interferometric ID BAND INTERFEROMETRIC OBSERVATIONS; NEAR-INFRARED EMISSION; AE/BE STARS; AB-AURIGAE; INNER DISK; PROTOPLANETARY DISKS; VEGA-TYPE; T TAURI; HR 5999; N-BAND AB We present the first N-band nulling plus K-and L-band V-2 observations of a young stellar object, MWC325, taken with the 85 m baseline Keck Interferometer. The Keck nuller was designed for the study of faint dust signatures associated with debris disks, but it also has a unique capability for studying the temperature and density distribution of denser disks found around young stellar objects. Interferometric observations of MWC325 at K, L, and N encompass a factor of five in spectral range and thus, especially when spectrally dispersed within each band, enable characterization of the structure of the inner disk regions where planets form. Fitting our observations with geometric models such as a uniform disk or a Gaussian disk show that the apparent size increases monotonically with wavelength in the 2-12 mu m wavelength region, confirming the widely held assumption based on radiative transfer models, now with spatially resolved measurements over a broad wavelength range, that disks are extended with a temperature gradient. The effective size is a factor of about 1.4 and 2.2 larger in the L band and N band, respectively, compared to that in the K band. The existing interferometric measurements and the spectral energy distribution can be reproduced by a flat disk or a weakly shadowed nearly flat disk model, with only slight flaring in the outer regions of the disk, consisting of representative "sub-micron" (0.1 mu m) and "micron" (2 mu m) grains of a 50: 50 ratio of silicate and graphite. This is in marked contrast to the disks previously found in other Herbig Ae/Be stars, suggesting a wide variety in the disk properties among Herbig Ae/Be stars. C1 [Ragland, S.; Hrynevich, M.] WM Keck Observ, Kamuela, HI 96743 USA. [Ohnaka, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Hillenbrand, L.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Ridgway, S. T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Colavita, M. M.; Traub, W. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Akeson, R. L.; Millan-Gabet, R.] CALTECH, NExScI, Pasadena, CA 91125 USA. [Cotton, W.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Danchi, W. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ragland, S (reprint author), WM Keck Observ, Kamuela, HI 96743 USA. EM sragland@keck.hawaii.edu FU National Aeronautics and Space Administration (NASA) [NNH09AK731]; W. M. Keck Foundation FX The Keck Interferometer is funded by the National Aeronautics and Space Administration (NASA). Observations presented 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. KI observations were taken through Keck Director's time. We thank E. Appleby, A. Cooper, C. Felizardo, J. Herstein, D. Medeiros, D. Morrison, T. Panteleeva, B. Parvin, B. Smith, K. Summers, K. Tsubota, C. Tyau, E. Wetherell, P. Wizinowich, and J. Woillez for their contributions to KI operations. CHARA observations were taken through NOAO TAC time. We thank Gail Schaefer, P. J. Goldfinger, Chris Farrington, and Theo ten Brummelaar for support of the CHARA observing program and Tabetha Boyajian for advice on data reductions. S. T. R. acknowledges partial support from NASA grant NNH09AK731. NR 65 TC 12 Z9 12 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 126 DI 10.1088/0004-637X/746/2/126 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300012 ER PT J AU Reeves, KK Gibson, SE Kucera, TA Hudson, HS Kano, R AF Reeves, Katharine K. Gibson, Sarah E. Kucera, Therese A. Hudson, Hugh S. Kano, Ryouhei TI THERMAL PROPERTIES OF A SOLAR CORONAL CAVITY OBSERVED WITH THE X-RAY TELESCOPE ON HINODE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: filaments, prominences ID WHOLE SUN MONTH; PROMINENCES; DENSITIES; XRT; SPECTROMETER; TEMPERATURES; TOMOGRAPHY; MISSION; CORE AB Coronal cavities are voids in coronal emission often observed above high latitude filament channels. Sometimes, these cavities have areas of bright X-ray emission in their centers. In this study, we use data from the X-ray Telescope (XRT) on the Hinode satellite to examine the thermal emission properties of a cavity observed during 2008 July that contains bright X-ray emission in its center. Using ratios of XRT filters, we find evidence for elevated temperatures in the cavity center. The area of elevated temperature evolves from a ring-shaped structure at the beginning of the observation, to an elongated structure two days later, finally appearing as a compact round source four days after the initial observation. We use a morphological model to fit the cavity emission, and find that a uniform structure running through the cavity does not fit the observations well. Instead, the observations are reproduced by modeling several short cylindrical cavity "cores" with different parameters on different days. These changing core parameters may be due to some observed activity heating different parts of the cavity core at different times. We find that core temperatures of 1.75 MK, 1.7 MK, and 2.0 MK (for July 19, July 21, and July 23, respectively) in the model lead to structures that are consistent with the data, and that line-of-sight effects serve to lower the effective temperature derived from the filter ratio. C1 [Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gibson, Sarah E.] HAO NCAR, Boulder, CO 80307 USA. [Kucera, Therese A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hudson, Hugh S.] Univ Calif Berkeley, Space Sci Labs, Berkeley, CA 94720 USA. [Hudson, Hugh S.] Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Kano, Ryouhei] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Reeves, KK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 58, Cambridge, MA 02138 USA. EM kreeves@cfa.harvard.edu RI Kucera, Therese/C-9558-2012; Reeves, Katharine/P-9163-2014; OI Kucera, Therese/0000-0001-9632-447X FU International Space Science Institute (ISSI); NASA [NNM07AB07C]; National Science Foundation FX The authors thank the anonymous referee, whose insightful comments helped improve the paper, and Yuhong Fan for useful discussions. The authors also thank the International Space Science Institute (ISSI) for funding a Working Group on Coronal Cavities, where this work began. K. K. Reeves is supported under contract NNM07AB07C from NASA to SAO. T. Kucera is supported by an award from the NASA SHP Program. The National Center for Atmospheric Research is sponsored by the National Science Foundation. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). SoHO is a project of international collaboration between ESA and NASA. The STEREO/SECCHI data used here are produced by an international consortium of the Naval Research Laboratory (USA), Lockheed Martin Solar and Astrophysics Lab (USA), NASA Goddard Space Flight Center (USA) Rutherford Appleton Laboratory (UK), University of Birmingham (UK), Max-Planck-Institut fur Sonnensystemforschung (Germany), Centre Spatiale de Liege (Belgium), Institut d'Optique Theorique et Appliquee (France), and Institut d'Astrophysique Spatiale (France). NR 31 TC 19 Z9 19 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 146 DI 10.1088/0004-637X/746/2/146 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300032 ER PT J AU Sharon, K Gladders, MD Rigby, JR Wuyts, E Koester, BP Bayliss, MB Barrientos, LF AF Sharon, Keren Gladders, Michael D. Rigby, Jane R. Wuyts, Eva Koester, Benjamin P. Bayliss, Matthew B. Barrientos, L. Felipe TI SOURCE-PLANE RECONSTRUCTION OF THE BRIGHT LENSED GALAXY RCSGA 032727-132609 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual: RCS2 032727-13262; gravitational lensing: strong ID HIGH-REDSHIFT; CLUSTER; Z=1.7 AB We present new Hubble Space Telescope/Wide Field Camera 3 imaging data of RCSGA 032727-132609, a bright lensed galaxy at z = 1.7 that is magnified and stretched by the lensing cluster RCS2 032727-132623. Using this new high-resolution imaging, we modify our previous lens model (which was based on ground-based data) to fully understand the lensing geometry, and use it to reconstruct the lensed galaxy in the source plane. This giant arc represents a unique opportunity to peer into 100 pc scale structures in a high-redshift galaxy. This new source reconstruction will be crucial for a future analysis of the spatially resolved rest-UV and rest-optical spectra of the brightest parts of the arc. C1 [Sharon, Keren; Gladders, Michael D.; Wuyts, Eva; Bayliss, Matthew B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Gladders, Michael D.; Wuyts, Eva; Koester, Benjamin P.; Bayliss, Matthew B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Wuyts, Eva] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Barrientos, L. Felipe] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. RP Sharon, K (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM kerens@kicp.uchicago.edu RI Rigby, Jane/D-4588-2012 OI Rigby, Jane/0000-0002-7627-6551 FU NASA through Space Telescope Science Institute [12267]; NASA [NAS 5-26555]; Research Corporation; Carnegie Institute for Science; FONDECYT [1085286] FX Support for program 12267 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. M.D.G. thanks the Research Corporation for support of this work through a Cottrell Scholars award. J.R.R. was supported in part by a Carnegie Fellowship from the Carnegie Institute for Science. L.F.B. is supported by FONDECYT under project 1085286. We thank the referee, M. Limousin, for useful comments. NR 15 TC 23 Z9 23 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 161 DI 10.1088/0004-637X/746/2/161 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300047 ER PT J AU Shin, IG Choi, JY Park, SY Han, C Gould, A Sumi, T Udalski, A Beaulieu, JP Dominik, M Allen, W Bos, M Christie, GW Depoy, DL Dong, S Drummond, J Gal-Yam, A Gaudi, BS Hung, LW Janczak, J Kaspi, S Lee, CU Mallia, F Maoz, D Maury, A McCormick, J Monard, LAG Moorhouse, D Munoz, JA Natusch, T Nelson, C Park, BG Pogge, RW Polishook, D Shvartzvald, Y Shporer, A Thornley, G Yee, JC Abe, F Bennett, DP Bond, IA Botzler, CS Fukui, A Furusawa, K Hayashi, F Hearnshaw, JB Hosaka, S Itow, Y Kamiya, K Kilmartin, PM Kobara, S Korpela, A Lin, W Ling, CH Makita, S Masuda, K Matsubara, Y Miyake, N Muraki, Y Nagaya, M Nishimoto, K Ohnishi, K Okumura, T Omori, K Perrott, YC Rattenbury, N Saito, T Skuljan, L Sullivan, DJ Suzuki, D Sweatman, WL Tristram, PJ Wada, K Yock, PCM Szymanski, MK Kubiak, M Pietrzynski, G Soszynski, I Poleski, R Ulaczyk, K Wyrzykowski, L Kozlowski, S Pietrukowicz, P Albrow, MD Batista, V Bramich, DM Brillant, S Caldwell, JAR Calitz, JJ Cassan, A Cole, A Cook, KH Corrales, E Coutures, C Dieters, S Prester, DD Donatowicz, J Fouque, P Greenhill, J Hoffman, M Jorgensen, UG Kane, SR Kubas, D Marquette, JB Martin, R Meintjes, P Menzies, J Pollard, KR Sahu, KC Wambsganss, J Williams, A Vinter, C Zub, M Allan, A Browne, P Horne, K Snodgrass, C Steele, I Street, R Tsapras, Y Alsubai, KA Bozza, V Browne, P Burgdorf, MJ Novati, SC Dodds, P Dreizler, S Finet, F Gerner, T Glitrup, M Grundahl, F Hardis, S Harpsoe, K Hessman, FV Hinse, TC Hundertmark, M Kains, N Kerins, E Liebig, C Maier, G Mancini, L Mathiasen, M Penny, MT Proft, S Rahvar, S Ricci, D Scarpetta, G Schafer, S Schonebeck, F Skottfelt, J Surdej, J Southworth, J Zimmer, F AF Shin, I. -G. Choi, J. -Y. Park, S. -Y. Han, C. Gould, A. Sumi, T. Udalski, A. Beaulieu, J. -P. Dominik, M. Allen, W. Bos, M. Christie, G. W. Depoy, D. L. Dong, S. Drummond, J. Gal-Yam, A. Gaudi, B. S. Hung, L. -W. Janczak, J. Kaspi, S. Lee, C. -U. Mallia, F. Maoz, D. Maury, A. McCormick, J. Monard, L. A. G. Moorhouse, D. Munoz, J. A. Natusch, T. Nelson, C. Park, B. -G. Pogge, R. W. Polishook, D. Shvartzvald, Y. Shporer, A. Thornley, G. Yee, J. C. Abe, F. Bennett, D. P. Bond, I. A. Botzler, C. S. Fukui, A. Furusawa, K. Hayashi, F. Hearnshaw, J. B. Hosaka, S. Itow, Y. Kamiya, K. Kilmartin, P. M. Kobara, S. Korpela, A. Lin, W. Ling, C. H. Makita, S. Masuda, K. Matsubara, Y. Miyake, N. Muraki, Y. Nagaya, M. Nishimoto, K. Ohnishi, K. Okumura, T. Omori, K. Perrott, Y. C. Rattenbury, N. Saito, To. Skuljan, L. Sullivan, D. J. Suzuki, D. Sweatman, W. L. Tristram, P. J. Wada, K. Yock, P. C. M. Szymanski, M. K. Kubiak, M. Pietrzynski, G. Soszynski, I. Poleski, R. Ulaczyk, K. Wyrzykowski, L. Kozlowski, S. Pietrukowicz, P. Albrow, M. D. Batista, V. Bramich, D. M. Brillant, S. Caldwell, J. A. R. Calitz, J. J. Cassan, A. Cole, A. Cook, K. H. Corrales, E. Coutures, Ch. Dieters, S. Prester, D. Dominis Donatowicz, J. Fouque, P. Greenhill, J. Hoffman, M. Jorgensen, U. G. Kane, S. R. Kubas, D. Marquette, J. -B. Martin, R. Meintjes, P. Menzies, J. Pollard, K. R. Sahu, K. C. Wambsganss, J. Williams, A. Vinter, C. Zub, M. Allan, A. Browne, P. Horne, K. Snodgrass, C. Steele, I. Street, R. Tsapras, Y. Alsubai, K. A. Bozza, V. Browne, P. Burgdorf, M. J. Novati, S. Calchi Dodds, P. Dreizler, S. Finet, F. Gerner, T. Glitrup, M. Grundahl, F. Hardis, S. Harpsoe, K. Hessman, F. V. Hinse, T. C. Hundertmark, M. Kains, N. Kerins, E. Liebig, C. Maier, G. Mancini, L. Mathiasen, M. Penny, M. T. Proft, S. Rahvar, S. Ricci, D. Scarpetta, G. Schaefer, S. Schoenebeck, F. Skottfelt, J. Surdej, J. Southworth, J. Zimmer, F. CA FUN Collaboration MOA Collaboration OGLE Collaboration PLANET Collaboration RoboNet Collaboration MiNDSTEp Consortium TI MICROLENSING BINARIES DISCOVERED THROUGH HIGH-MAGNIFICATION CHANNEL SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; gravitational lensing: micro ID III EWS DATABASE; GRAVITATIONAL LENSING EXPERIMENT; GALACTIC BULGE; EVENTS; PLANETARY; LENSES; MASS; ASTROPHYSICS AB Microlensing can provide a useful tool to probe binary distributions down to low-mass limits of binary companions. In this paper, we analyze the light curves of eight binary-lensing events detected through the channel of high-magnification events during the seasons from 2007 to 2010. The perturbations, which are confined near the peak of the light curves, can be easily distinguished from the central perturbations caused by planets. However, the degeneracy between close and wide binary solutions cannot be resolved with a 3 sigma confidence level for three events, implying that the degeneracy would be an important obstacle in studying binary distributions. The dependence of the degeneracy on the lensing parameters is consistent with a theoretical prediction that the degeneracy becomes severe as the binary separation and the mass ratio deviate from the values of resonant caustics. The measured mass ratio of the event OGLE-2008-BLG-510/MOA-2008-BLG-369 is q similar to 0.1, making the companion of the lens a strong brown dwarf candidate. C1 [Shin, I. -G.; Choi, J. -Y.; Park, S. -Y.; Han, C.] Chungbuk Natl Univ, Dept Phys, Inst Astrophys, Cheongju 371763, South Korea. [Gould, A.; Gaudi, B. S.; Pogge, R. W.; Yee, J. C.; Batista, V.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Sumi, T.; Suzuki, D.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Udalski, A.; Szymanski, M. K.; Kubiak, M.; Pietrzynski, G.; Soszynski, I.; Poleski, R.; Ulaczyk, K.; Wyrzykowski, L.; Kozlowski, S.; Pietrukowicz, P.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Beaulieu, J. -P.; Cassan, A.; Corrales, E.; Coutures, Ch.; Dieters, S.; Kubas, D.; Marquette, J. -B.] Univ Paris 06, Inst Astrophys Paris, UMR7095, CNRS, F-75014 Paris, France. [Dominik, M.; Browne, P.; Horne, K.; Browne, P.; Dodds, P.; Hundertmark, M.; Kains, N.; Liebig, C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Allen, W.] Vintage Lane Observ, Blenheim, New Zealand. [Bos, M.] Molehill Astron Observ, N Shore, New Zealand. [Christie, G. W.; Natusch, T.] Auckland Observ, Auckland, New Zealand. [Depoy, D. L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Dong, S.] Inst Adv Study, Princeton, NJ 08540 USA. [Drummond, J.] Possum Observ, Patutahi, New Zealand. [Gal-Yam, A.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, Weizmann, Israel. [Hung, L. -W.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Janczak, J.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Kaspi, S.; Maoz, D.; Polishook, D.; Shvartzvald, Y.; Shporer, A.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Lee, C. -U.; Park, B. -G.; Hinse, T. C.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Mallia, F.; Maury, A.] Campo Catino Austral Observ, San Pedro De Atacama, Chile. [McCormick, J.] Farm Cove Observ, Auckland, New Zealand. [Monard, L. A. G.] Bronberg Observ, Pretoria, South Africa. [Moorhouse, D.; Thornley, G.] Kumeu Observ, Kumeu, New Zealand. [Munoz, J. A.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. [Nelson, C.] Univ Arizona, Coll Opt Sci, Tucson, AZ 85721 USA. [Abe, F.; Fukui, A.; Furusawa, K.; Hayashi, F.; Hosaka, S.; Itow, Y.; Kamiya, K.; Kobara, S.; Makita, S.; Masuda, K.; Matsubara, Y.; Miyake, N.; Nagaya, M.; Nishimoto, K.; Okumura, T.; Omori, K.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Bond, I. A.; Lin, W.; Ling, C. H.; Skuljan, L.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, N Shore Mail Ctr, Auckland, New Zealand. [Botzler, C. S.; Perrott, Y. C.; Rattenbury, N.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland, New Zealand. [Hearnshaw, J. B.; Albrow, M. D.; Pollard, K. R.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand. [Kilmartin, P. M.; Tristram, P. J.] Mt John Observ, Lake Tekapo 8770, New Zealand. [Korpela, A.; Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand. [Muraki, Y.] Konan Univ, Dept Phys, Kobe, Hyogo 6588501, Japan. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Saito, To.] Tokyo Metropolitan Coll Ind Technol, Tokyo 1168523, Japan. [Pietrzynski, G.] Univ Concepcion, Dept Fis, Concepcion, Chile. [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Bramich, D. M.] European So Observ, D-85748 Garching, Germany. [Brillant, S.; Kubas, D.; Snodgrass, C.] European So Observ, Santiago 19, Chile. [Caldwell, J. A. R.] McDonald Observ, Ft Davis, TX 79734 USA. [Calitz, J. J.; Hoffman, M.; Meintjes, P.] Univ Free State, Fac Nat & Agr Sci, Dept Phys, ZA-9300 Bloemfontein, South Africa. [Cole, A.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, Gpo Hobart, Tas 7001, Australia. [Cook, K. H.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys IGPP, Livermore, CA 94551 USA. [Dieters, S.; Fouque, P.] Univ Toulouse, LATT, CNRS, F-31400 Toulouse, France. [Prester, D. Dominis] Univ Rijeka, Dept Phys, Fac Arts & Sci, Rijeka 51000, Croatia. [Donatowicz, J.] Vienna Univ Technol, Dept Comp, A-1060 Vienna, Austria. [Jorgensen, U. G.; Vinter, C.; Hardis, S.; Harpsoe, K.; Hinse, T. C.; Mathiasen, M.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Jorgensen, U. G.; Harpsoe, K.] Geol Museum, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Kane, S. R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Martin, R.; Williams, A.] Perth Observ, Perth, WA 6076, Australia. [Menzies, J.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Wambsganss, J.; Zub, M.] Heidelberg Univ, Astron Rechen Inst ARI, Zentrum Astron, D-69120 Heidelberg, Germany. [Allan, A.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Snodgrass, C.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Steele, I.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Street, R.; Tsapras, Y.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Alsubai, K. A.] Qatar Fdn, Doha, Qatar. [Bozza, V.; Novati, S. Calchi; Mancini, L.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84081 Baronissi, SA, Italy. [Burgdorf, M. J.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany. [Burgdorf, M. J.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Novati, S. Calchi] Ist Int Alti Studi Sci IIASS, Vietri Sul Mare, SA, Italy. [Dreizler, S.; Hessman, F. V.; Hundertmark, M.; Schaefer, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Finet, F.; Ricci, D.; Surdej, J.] Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Gerner, T.; Liebig, C.; Maier, G.; Proft, S.; Schoenebeck, F.; Zimmer, F.] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, D-69120 Heidelberg, Germany. [Glitrup, M.; Grundahl, F.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Kains, N.] ESO Headquarters, D-85748 Garching, Germany. [Kerins, E.; Penny, M. T.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Mancini, L.] Max Planck Inst Astron, D-619117 Heidelberg, Germany. [Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran. [Scarpetta, G.] Ist Nazl Fis Nucl, Grp Collegato Salerno, Sez Napoli, Milan, Italy. [Southworth, J.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England. RP Shin, IG (reprint author), Chungbuk Natl Univ, Dept Phys, Inst Astrophys, Cheongju 371763, South Korea. RI Gaudi, Bernard/I-7732-2012; Kozlowski, Szymon/G-4799-2013; Williams, Andrew/K-2931-2013; Zimmer, Fabian/M-4765-2014; Hundertmark, Markus/C-6190-2015; Rahvar, Sohrab/A-9350-2008; Dong, Subo/J-7319-2012; Kane, Stephen/B-4798-2013; Greenhill, John/C-8367-2013 OI Ricci, Davide/0000-0002-9790-0552; Penny, Matthew/0000-0001-7506-5640; Snodgrass, Colin/0000-0001-9328-2905; Kozlowski, Szymon/0000-0003-4084-880X; Williams, Andrew/0000-0001-9080-0105; Hundertmark, Markus/0000-0003-0961-5231; Rahvar, Sohrab/0000-0002-7084-5725; Dominik, Martin/0000-0002-3202-0343; Cole, Andrew/0000-0003-0303-3855; FU Creative Research Initiative of National Research Foundation of Korea [2009-0081561]; European Research Council under the European Community [246678]; NSF [AST-1103471, 2009068160]; NASA [NNX08AF40G]; Qatar National Research Fund; Deutsche Forschungsgemeinschaft; Communaute francaise de Belgique-Actions de recherche concertees-Academie universitaire Wallonie-Europe; [JSPS22403003]; [JSPS20340052]; [JSPS18253002]; [JSPS17340074]; [JSPS18749004]; [MEXT19015005]; [JSPS20740104] FX Work by C. H. was supported by Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea. 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. Work by B. S. G. and A. G. was supported in part by NSF grant AST-1103471. Work by B. S. G., A. G., R. W. P., and J.C.Y. was supported in part by NASA grant NNX08AF40G. Work by J.C.Y. was supported by a National Science Foundation Graduate Research Fellowship under grant No. 2009068160. Work by M. H. was supported by Qatar National Research Fund and Deutsche Forschungsgemeinschaft. The MOA experiment was supported by JSPS22403003, JSPS20340052, JSPS18253002, and JSPS17340074. T. S. was supported by the grants JSPS18749004, MEXT19015005, and JSPS20740104. F. F., D. R., and J.S. were supported by the Communaute francaise de Belgique-Actions de recherche concertees-Academie universitaire Wallonie-Europe. NR 39 TC 12 Z9 12 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 127 DI 10.1088/0004-637X/746/2/127 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300013 ER PT J AU Wright, M Zhao, JH Sandell, G Corder, S Goss, WM Zhu, L AF Wright, Melvyn Zhao, Jun-Hui Sandell, Goeran Corder, Stuartt Goss, W. M. Zhu, Lei TI OBSERVATIONS OF A HIGH-MASS PROTOSTAR IN NGC 7538 S SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM: clouds; stars: formation; stars: pre-main sequence; submillimeter: ISM ID SUBMILLIMETER CONTINUUM OBSERVATIONS; STAR-FORMATION; CIRCUMSTELLAR DISKS; NGC-7538 REGION; ACCRETION DISK; DUST EMISSION; ORION-KL; CORES; OBJECTS; MASERS AB We present high angular resolution continuum observations of the high-mass protostar NGC 7538 S with BIMA and CARMA at 3 and 1.4 mm, Very Large Array (VLA) observations at 1.3, 2, 3.5, and 6 cm, and archive Infrared Array Camera (IRAC) observations from the Spitzer Space Observatory, which detect the star at 4.5, 5.8, and 8 mu m. The star looks rather unremarkable in the mid-IR. The excellent positional agreement of the IRAC source with the VLA free-free emission, the OH, CH3OH, H2O masers, and the dust continuum confirms that this is the most luminous object in the NGC 7538 S core. The continuum emission at millimeter wavelengths is dominated by dust emission from the dense cold cloud core surrounding the protostar. Including all array configurations, the emission is dominated by an elliptical source with a size of similar to 8 '' x 3 ''. If we filter out the extended emission we find three compact millimeter sources inside the elliptical core. The strongest one, S-A, coincides with the VLA/IRAC source and resolves into a double source at 1.4 mm, where we have subarcsecond resolution. The measured spectral index, a, between 3 and 1.4 mm is similar to 2.3, and steeper at longer wavelengths, suggesting a low dust emissivity or that the dust is optically thick. We argue that the dust in these accretion disks is optically thick and estimate a mass of an accretion disk or infalling envelope surrounding S-A to be similar to 60 M-circle dot. C1 [Wright, Melvyn] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sandell, Goeran] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Corder, Stuartt] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Goss, W. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Zhu, Lei] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. RP Wright, M (reprint author), Univ Calif Berkeley, Radio Astron Lab, 601 Campbell Hall, Berkeley, CA 94720 USA. FU National Science Foundation; state of California; state of Illinois; state of Maryland; Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; California Institute of Technology; CARMA partner universities FX The BIMA array was operated by the Universities of California (Berkeley), Illinois, and Maryland with support from the National Science Foundation. Support for CARMA construction was derived from the states of California, Illinois, and Maryland, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the Associates of the California Institute of Technology, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. NR 35 TC 5 Z9 5 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 187 DI 10.1088/0004-637X/746/2/187 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300073 ER PT J AU Kaur, R Kaper, L Ellerbroek, LE Russell, DM Altamirano, D Wijnands, R Yang, YJ D'Avanzo, P Postigo, AD Flores, H Fynbo, JPU Goldoni, P Thone, CC van der Horst, A van der Klis, M Kouveliotou, C Wiersema, K Kuulkers, E AF Kaur, Ramanpreet Kaper, Lex Ellerbroek, Lucas E. Russell, David M. Altamirano, Diego Wijnands, Rudy Yang, Yi-Jung D'Avanzo, Paolo Postigo, Antonio de Ugarte Flores, Hector Fynbo, Johan P. U. Goldoni, Paolo Thoene, Christina C. van der Horst, Alexander van der Klis, Michiel Kouveliotou, Chryssa Wiersema, Klaas Kuulkers, Erik TI VERY LARGE TELESCOPE/X-SHOOTER SPECTROSCOPY OF THE CANDIDATE BLACK HOLE X-RAY BINARY MAXI J1659-152 IN OUTBURST SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; binaries: close; black hole physics; X-rays: binaries ID DIFFUSE INTERSTELLAR BANDS; LOW-HARD STATES; OPTICAL SPECTROSCOPY; HIGH-SOFT; GX 339-4; ULTRAVIOLET; EMISSION; EXTINCTION; GX-339-4; MISSION AB We present the optical to near-infrared spectrum of MAXI J1659-152 during the onset of its 2010 X-ray outburst. The spectrum was obtained with X-shooter on the ESO Very Large Telescope early in the outburst simultaneous with high-quality observations at both shorter and longer wavelengths. At the time of the observations, the source was in the low-hard state. The X-shooter spectrum includes many broad (similar to 2000 km s(-1)), double-peaked emission profiles of H, He I, and He II, characteristic signatures of a low-mass X-ray binary during outburst. We detect no spectral signatures of the low-mass companion star. The strength of the diffuse interstellar bands results in a lower limit to the total interstellar extinction of A(V) similar or equal to 0.4 mag. Using the neutral hydrogen column density obtained from the X-ray spectrum we estimate A(V) similar or equal to 1 mag. The radial velocity structure of the interstellar Na I D and Ca II H&K lines results in a lower limit to the distance of similar to 4 +/- 1 kpc, consistent with previous estimates. With this distance and A(V), the dereddened spectral energy distribution represents a flat disk spectrum. The two 10 minute X-shooter spectra show significant variability in the red wing of the emission-line profiles, indicating a global change in the density structure of the disk, though on a timescale much shorter than the typical viscous timescale of the disk. C1 [Kaur, Ramanpreet; Kaper, Lex; Ellerbroek, Lucas E.; Russell, David M.; Altamirano, Diego; Wijnands, Rudy; Yang, Yi-Jung; van der Horst, Alexander; van der Klis, Michiel] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Kaur, Ramanpreet] Univ Wisconsin, Dept Phys, Milwaukee, WI 53211 USA. [D'Avanzo, Paolo] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Postigo, Antonio de Ugarte; Fynbo, Johan P. U.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Postigo, Antonio de Ugarte; Thoene, Christina C.] CSIC, IAA, E-18008 Granada, Spain. [Flores, Hector] Univ Paris Diderot, GEPI, Observ Paris, CNRS, F-92195 Meudon, France. [Goldoni, Paolo] Lab Astroparticule & Cosmol, F-75205 Paris 13, France. [Goldoni, Paolo] CEA Saclay, Serv Astrophys, DSM, IRFU,SAp, F-91191 Gif Sur Yvette, France. [Thoene, Christina C.] Niels Bohr Inst, Niels Bohr Int Acad, DK-2100 Copenhagen, Denmark. [van der Horst, Alexander] NSSTC, USRA, Huntsville, AL 35806 USA. [Kouveliotou, Chryssa] NASA, Space Sci Off, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Wiersema, Klaas] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Kuulkers, Erik] European Space Astron Ctr, European Space Agcy, Madrid 28691, Spain. RP Kaur, R (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM r.kaur@uva.nl RI Fynbo, Johan/L-8496-2014; OI Fynbo, Johan/0000-0002-8149-8298; Thone, Christina/0000-0002-7978-7648; de Ugarte Postigo, Antonio/0000-0001-7717-5085 FU European Research Council FX R.K., R.W., and J.P.U.F. acknowledge support from the European Research Council starting grant. NR 50 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 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2012 VL 746 IS 2 AR L23 DI 10.1088/2041-8205/746/2/L23 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 896ZT UT WOS:000300611100010 ER PT J AU King, AL Miller, JM Raymond, J Fabian, AC Reynolds, CS Kallman, TR Maitra, D Cackett, EM Rupen, MP AF King, A. L. Miller, J. M. Raymond, J. Fabian, A. C. Reynolds, C. S. Kallman, T. R. Maitra, D. Cackett, E. M. Rupen, M. P. TI AN EXTREME X-RAY DISK WIND IN THE BLACK HOLE CANDIDATE IGR J17091-3624 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; X-rays: binaries ID GALAXY NGC 4051; ACCRETION DISKS; ABSORPTION-LINES; WARM ABSORBERS; GRO J1655-40; OUTBURST; CHANDRA; RADIO; SPECTROSCOPY; OUTFLOWS AB Chandra spectroscopy of transient stellar-mass black holes in outburst has clearly revealed accretion disk winds in soft, disk-dominated states, in apparent anti-correlation with relativistic jets in low/hard states. These disk winds are observed to be highly ionized, dense, and to have typical velocities of similar to 1000 km s(-1) or less projected along our line of sight. Here, we present an analysis of two Chandra High Energy Transmission Grating spectra of the Galactic black hole candidate IGR J17091-3624 and contemporaneous Expanded Very Large Array (EVLA) radio observations, obtained in 2011. The second Chandra observation reveals an absorption line at 6.91 +/- 0.01 keV; associating this line with He-like Fe XXV requires a blueshift of 9300(-400)(+500) km s(-1) (0.03c, or the escape velocity at 1000 R-Schw). This projected outflow velocity is an order of magnitude higher than has previously been observed in stellar-mass black holes, and is broadly consistent with some of the fastest winds detected in active galactic nuclei. A potential feature at 7.32 keV, if due to Fe XXVI, would imply a velocity of similar to 14,600 km s(-1) (0.05c), but this putative feature is marginal. Photoionization modeling suggests that the accretion disk wind in IGR J17091-3624 may originate within 43,300 Schwarzschild radii of the black hole and may be expelling more gas than it accretes. The contemporaneous EVLA observations strongly indicate that jet activity was indeed quenched at the time of our Chandra observations. We discuss the results in the context of disk winds, jets, and basic accretion disk physics in accreting black hole systems. C1 [King, A. L.; Miller, J. M.; Maitra, D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Raymond, J.] Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabian, A. C.; Cackett, E. M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Kallman, T. R.] NASA, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cackett, E. M.] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48201 USA. [Rupen, M. P.] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP King, AL (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ashking@umich.edu FU NASA; Chandra Guest Observer program FX We thank the anonymous referee. We thank Michael Nowak for his instrumental help as well. A.L.K. gratefully acknowledges support through the NASA Earth and Space Sciences Fellowship. J.M.M. gratefully acknowledges support through the Chandra Guest Observer program. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 38 TC 49 Z9 49 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2012 VL 746 IS 2 AR L20 DI 10.1088/2041-8205/746/2/L20 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 896ZT UT WOS:000300611100007 ER PT J AU Liu, YD Luhmann, JG Mostl, C Martinez-Oliveros, JC Bale, SD Lin, RP Harrison, RA Temmer, M Webb, DF Odstrcil, D AF Liu, Ying D. Luhmann, Janet G. Moestl, Christian Martinez-Oliveros, Juan C. Bale, Stuart D. Lin, Robert P. Harrison, Richard A. Temmer, Manuela Webb, David F. Odstrcil, Dusan TI INTERACTIONS BETWEEN CORONAL MASS EJECTIONS VIEWED IN COORDINATED IMAGING AND IN SITU OBSERVATIONS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE shock waves; solar-terrestrial relations; solar wind; Sun: coronal mass ejections (CMEs) ID COMPLEX EJECTA; STEREO MISSION; MAGNETIC CLOUD; EARTH; SIMULATION; SHOCK; SUN; SIGNATURES AB The successive coronal mass ejections (CMEs) from 2010 July 30 to August 1 present us the first opportunity to study CME-CME interactions with unprecedented heliospheric imaging and in situ observations from multiple vantage points. We describe two cases of CME interactions: merging of two CMEs launched close in time and overtaking of a preceding CME by a shock wave. The first two CMEs on August 1 interact close to the Sun and form a merged front, which then overtakes the July 30 CME near 1 AU, as revealed by wide-angle imaging observations. Connections between imaging observations and in situ signatures at 1 AU suggest that the merged front is a shock wave, followed by two ejecta observed at Wind which seem to have already merged. In situ measurements show that the CME from July 30 is being overtaken by the shock at 1 AU and is significantly compressed, accelerated, and heated. The interaction between the preceding ejecta and shock also results in variations in the shock strength and structure on a global scale, as shown by widely separated in situ measurements from Wind and STEREO B. These results indicate important implications of CME-CME interactions for shock propagation, particle acceleration, and space weather forecasting. C1 [Liu, Ying D.; Luhmann, Janet G.; Moestl, Christian; Martinez-Oliveros, Juan C.; Bale, Stuart D.; Lin, Robert P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Liu, Ying D.] Chinese Acad Sci, Natl Space Sci Ctr, State Key Lab Space Weather, Beijing, Peoples R China. [Moestl, Christian; Temmer, Manuela] Graz Univ, Inst Phys, A-8010 Graz, Austria. [Moestl, Christian] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Lin, Robert P.] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi, South Korea. [Harrison, Richard A.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Webb, David F.] Boston Coll, Inst Sci Res, Newton, MA 02459 USA. [Odstrcil, Dusan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Liu, YD (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM liuxying@ssl.berkeley.edu RI Bale, Stuart/E-7533-2011; OI Bale, Stuart/0000-0002-1989-3596; Martinez Oliveros, Juan Carlos/0000-0002-2587-1342; Liu, Ying/0000-0002-3483-5909; Moestl, Christian/0000-0001-6868-4152; Temmer, Manuela/0000-0003-4867-7558 FU STEREO [NAS5-03131]; Marie Curie International Outgoing Fellowship; Austrian Science Fund FWF [V195-N16] FX The research was supported by the STEREO project under grant NAS5-03131. C.M. is supported by a Marie Curie International Outgoing Fellowship. M.T. acknowledges the Austrian Science Fund FWF V195-N16. NR 28 TC 43 Z9 46 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2012 VL 746 IS 2 AR L15 DI 10.1088/2041-8205/746/2/L15 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 896ZT UT WOS:000300611100002 ER PT J AU Mroczkowski, T AF Mroczkowski, Tony TI A NEW APPROACH TO OBTAINING CLUSTER MASS FROM SUNYAEV-ZEL'DOVICH EFFECT OBSERVATIONS (vol 728, L35, 2011) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Correction ID ATACAMA COSMOLOGY TELESCOPE; RELAXED GALAXY CLUSTERS; SOUTH-POLE TELESCOPE; REPRESENTATIVE SAMPLE; INTRACLUSTER MEDIUM; PRESSURE PROFILE; POWER SPECTRUM; XMM-NEWTON; MATTER; SIMULATIONS C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mroczkowski, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-237, Pasadena, CA 91109 USA. NR 36 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2012 VL 746 IS 2 AR L29 DI 10.1088/2041-8205/746/2/L29 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 896ZT UT WOS:000300611100016 ER PT J AU Patruno, A Bult, P Gopakumar, A Hartman, JM Wijnands, R van der Klis, M Chakrabarty, D AF Patruno, Alessandro Bult, Peter Gopakumar, Achamveedu Hartman, Jacob M. Wijnands, Rudy van der Klis, Michiel Chakrabarty, Deepto TI ACCELERATED ORBITAL EXPANSION AND SECULAR SPIN-DOWN OF THE ACCRETING MILLISECOND PULSAR SAX J1808.4-3658 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: general; stars: individual (SAX J1808.4-3658); stars: neutron; stars: rotation; X-rays: binaries; X-rays: stars ID BINARY PSR B1957+20; X-RAY PULSAR; XMM-NEWTON; PERIOD CHANGES; 2002 OUTBURST; VARIABILITY; EVOLUTION; QUIESCENCE; J2051-0827; COMPANION AB The accreting millisecond pulsar SAX J1808.4-3658 has shown a peculiar orbital evolution in the past with an orbital expansion much faster than expected from standard binary evolutionary scenarios. Previous limits on the pulsar spin frequency derivative during transient accretion outbursts were smaller than predicted by standard magnetic accretion torque theory, while the spin evolution between outbursts was consistent with magnetic dipole spin-down. In this Letter, we present the results of a coherent timing analysis of the 2011 outburst observed by the Rossi X-Ray Timing Explorer and extend our previous long-term measurements of the orbital and spin evolution over a baseline of 13 years. We find that the expansion of the 2 hr orbit is accelerating at a rate of (P) double over dot(b) similar or equal to 1.6 x 10(-20) s s(-2) and we interpret this as the effect of short-term angular momentum exchange between the mass donor and the orbit. The gravitational quadrupole coupling due to variations in the oblateness of the companion can be a viable mechanism for explaining the observations. No significant spin frequency derivatives are detected during the 2011 outburst (vertical bar(nu) over dot vertical bar less than or similar to 4 x 10(-13) Hz s(-1)) and the long-term spin-down remains stable over 13 years with (nu) over dot similar or equal to 10(-15) Hz s(-1). C1 [Patruno, Alessandro; Bult, Peter; Wijnands, Rudy; van der Klis, Michiel] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Gopakumar, Achamveedu] Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India. [Hartman, Jacob M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chakrabarty, Deepto] MIT, Dept Phys, Cambridge, MA 02139 USA. [Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Patruno, A (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. FU NWO-Veni; ERC FX A.P. acknowledges support from an NWO-Veni fellowship. R.W. was partly supported by an ERC starting grant. NR 41 TC 27 Z9 27 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2012 VL 746 IS 2 AR L27 DI 10.1088/2041-8205/746/2/L27 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 896ZT UT WOS:000300611100014 ER PT J AU Winebarger, AR Warren, HP Schmelz, JT Cirtain, J Mulu-Moore, F Golub, L Kobayashi, K AF Winebarger, Amy R. Warren, Harry P. Schmelz, Joan T. Cirtain, Jonathan Mulu-Moore, Fana Golub, Leon Kobayashi, Ken TI DEFINING THE "BLIND SPOT" OF HINODE EIS AND XRT TEMPERATURE MEASUREMENTS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: corona ID X-RAY TELESCOPE; DIFFERENTIAL EMISSION MEASURE; ACTIVE-REGION; PLASMA; LINES; DIAGNOSTICS; LOOPS; FLARE AB Observing high-temperature, low emission measure plasma is key to unlocking the coronal heating problem. With current instrumentation, a combination of EUV spectral data from Hinode Extreme-ultraviolet Imaging Spectrometer (EIS; sensitive to temperatures up to 4 MK) and broadband filter data from Hinode X-ray Telescope (XRT; sensitive to higher temperatures) is typically used to diagnose the temperature structure of the observed plasma. In this Letter, we demonstrate that a "blind spot" exists in temperature-emission measure space for combined Hinode EIS and XRT observations. For a typical active region core with significant emission at 3-4 MK, Hinode EIS and XRT are insensitive to plasma with temperatures greater than similar to 6 MK and emission measures less than similar to 10(27) cm(-5). We then demonstrate that the temperature and emission measure limits of this blind spot depend upon the temperature distribution of the plasma along the line of sight by considering a hypothetical emission measure distribution sharply peaked at 1 MK. For this emission measure distribution, we find that EIS and XRT are insensitive to plasma with emission measures less than similar to 10(26) cm(-5). We suggest that a spatially and spectrally resolved 6-24 angstrom spectrum would improve the sensitivity to these high-temperature, low emission measure plasma. C1 [Winebarger, Amy R.; Cirtain, Jonathan; Mulu-Moore, Fana] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Warren, Harry P.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Schmelz, Joan T.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA. [Golub, Leon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kobayashi, Ken] Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA. RP Winebarger, AR (reprint author), NASA, George C Marshall Space Flight Ctr, VP 62, Huntsville, AL 35812 USA. EM amy.r.winebarger@nasa.gov OI Golub, Leon/0000-0001-9638-3082 NR 23 TC 22 Z9 22 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2012 VL 746 IS 2 AR L17 DI 10.1088/2041-8205/746/2/L17 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 896ZT UT WOS:000300611100004 ER PT J AU Draper, CS Reichle, RH De Lannoy, GJM Liu, Q AF Draper, C. S. Reichle, R. H. De Lannoy, G. J. M. Liu, Q. TI Assimilation of passive and active microwave soil moisture retrievals SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID OPTICAL DEPTH RETRIEVAL; METHODOLOGY AB Near-surface soil moisture observations from the active microwave ASCAT and the passive microwave AMSR-E satellite instruments are assimilated, both separately and together, into the NASA Catchment land surface model over 3.5 years using an ensemble Kalman filter. The impact of each assimilation is evaluated using in situ soil moisture observations from 85 sites in the US and Australia, in terms of the anomaly time series correlation-coefficient, R. The skill gained by assimilating either ASCAT or AMSR-E was very similar, even when separated by land cover type. Over all sites, the mean root-zone R was significantly increased from 0.45 for an open-loop, to 0.55, 0.54, and 0.56 by the assimilation of ASCAT, AMSR-E, and both, respectively. Each assimilation also had a positive impact over each land cover type sampled. For maximum accuracy and coverage it is recommended that active and passive microwave observations be assimilated together. Citation: Draper, C. S., R. H. Reichle, G. J. M. De Lannoy, and Q. Liu (2012), Assimilation of passive and active microwave soil moisture retrievals, Geophys. Res. Lett., 39, L04401, doi: 10.1029/2011GL050655. C1 [Draper, C. S.; Reichle, R. H.; De Lannoy, G. J. M.; Liu, Q.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Draper, C. S.; De Lannoy, G. J. M.] Univ Space Res Assoc, GESTAR, Columbia, MD USA. [De Lannoy, G. J. M.] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium. [Liu, Q.] Sci Applicat Int Corp, Beltsville, MD USA. RP Draper, CS (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA. EM clara.draper@nasa.gov RI Reichle, Rolf/E-1419-2012; Draper, Clara/P-6097-2016 OI Draper, Clara/0000-0002-8299-4939 FU Research Foundation Flanders FX We are grateful to all who contributed to the data sets used in this study. In particular we acknowledge Richard de Jeu and colleagues (VUA), Wolfgang Wagner and colleagues (TU-Wien), and staff at ESA, Monash University, NASA, USDA, and the University of Melbourne. G. De Lannoy is funded by the Research Foundation Flanders. NR 15 TC 74 Z9 74 U1 5 U2 32 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 18 PY 2012 VL 39 AR L04401 DI 10.1029/2011GL050655 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 899MT UT WOS:000300820700001 ER PT J AU Helmboldt, JF Lazio, TJW Intema, HT Dymond, KF AF Helmboldt, J. F. Lazio, T. J. W. Intema, H. T. Dymond, K. F. TI A new technique for spectral analysis of ionospheric TEC fluctuations observed with the Very Large Array VHF system: From QP echoes to MSTIDs SO RADIO SCIENCE LA English DT Article ID NIGHTTIME MIDLATITUDE IONOSPHERE; SPORADIC-E EXPERIMENT; INSTABILITY AB We have used a relatively long, contiguous VHF observation of a bright cosmic radio source (Cygnus A) with the Very Large Array (VLA) through the nighttime, midlatitude ionosphere to demonstrate the phenomena observable with this instrument. In a companion paper, we showed that the VLA can detect fluctuations in total electron content (TEC) with amplitudes of <= 10(-3) TECU and can measure TEC gradients with a precision of about 2 x 10(-4) TECU km(-1). We detail two complementary techniques for producing spectral analysis of these TEC gradient measurements. The first is able to track individual waves with wavelengths of about half the size of the array (similar to 20 km) or more. This technique was successful in detecting and characterizing many medium-scale traveling ionospheric disturbances (MSTIDs) seen intermittently throughout the night and has been partially validated using concurrent GPS measurements. Smaller waves are also seen with this technique at nearly all times, many of which move in similar directions as the detected MSTIDs. The second technique allows for the detection and statistical description of the properties of groups of waves moving in similar directions with wavelengths as small as 5 km. Combining the results of both spectral techniques, we found a class of intermediate and small scale waves which are likely the quasi-periodic (QP) echoes that have been observed to occur within sporadic-E (E-s) layers. We find two distinct populations of these waves. The members of one population are coincident in time with MSTIDs and are consistent with being generated within E-s layers by the E-F coupling instability. The other population seems more influenced by the neutral wind, similar to the predominant types of QP echoes found by the Sporadic-E Experiments over Kyushu (SEEK). We have also found that the spectra of background (i.e., isotropic) fluctuations can be interpreted as the sum of two turbulent components with maximum scales of about 300 km and 10 km. C1 [Helmboldt, J. F.; Dymond, K. F.] USN, Res Lab, Washington, DC 20375 USA. [Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA. [Intema, H. T.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Helmboldt, JF (reprint author), USN, Res Lab, Code 7213,4555 Overlook Ave SW, Washington, DC 20375 USA. EM joe.helmboldt@nrl.navy.mil; joseph.lazio@jpl.nasa.gov; hintema@nrao.edu; kenneth.dymond@nrl.navy.mil RI Helmboldt, Joseph/C-8105-2012; Intema, Huib/D-1438-2012; OI Intema, Huib/0000-0002-5880-2730; Dymond, Kenneth/0000-0001-8060-9016 FU National Aeronautics and Space Administration FX The authors would like to thank the referees for useful comments and suggestions. Basic research in astronomy at the Naval Research Laboratory is supported by 6.1 base funding. The VLA was operated by the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. 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 26 TC 17 Z9 17 U1 1 U2 5 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 FEB 18 PY 2012 VL 47 AR RS0L02 DI 10.1029/2011RS004787 PG 21 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA 899PE UT WOS:000300827500001 ER PT J AU Robertson, K Furukawa, Y Underwood, A Black, L Liu, JL AF Robertson, Kelly Furukawa, Yoko Underwood, Alison Black, Lindsay Liu, Jinny L. TI Deletion of the Hoc and Soc capsid proteins affects the surface and cellular uptake properties of bacteriophage T4 derived nanoparticles SO BIOCHEMICAL AND BIOPHYSICAL RESEARCH COMMUNICATIONS LA English DT Article DE T4 NPs; Hoc; Soc; Zeta potentials; Cellular uptake ID MOLECULAR ARCHITECTURE; HEAD; PARTICLES; PHAGE-T4; DELIVERY; DOMAINS AB Recently the use of engineered viral scaffolds in biotechnology and medical applications has been increasing dramatically. T4 phage capsid derived nanoparticles (NPs) have potential advantages as sensors and in biotechnology. These applications require that the physical properties and cellular uptake of these NPs be understood. In this study we used a T4 deletion mutant to investigate the effects of removing both the Hoc and Soc proteins from the capsid surface on T4 tailless NPs. The surface charge, zeta potential, size, and cellular uptake efficiencies for both the T4 NP and T4 Delta Hoc Delta Soc NP mutant were measured and compared using dynamic light scattering and flow cytometry and significant differences were detected. Published by Elsevier Inc. C1 [Robertson, Kelly; Liu, Jinny L.] USN, Res Lab, Ctr Bio Mol Sci & Engn, Washington, DC 20375 USA. [Furukawa, Yoko] USN, Res Lab, Seafloor Sci Branch, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. [Black, Lindsay] Univ Maryland, Sch Med, Dept Biochem, Baltimore, MD 21230 USA. RP Liu, JL (reprint author), USN, Res Lab, Ctr Bio Mol Sci & Engn, 4555 Overlook Ave SW, Washington, DC 20375 USA. EM jinny.liu@nrl.navy.mil RI Furukawa, Yoko/B-3099-2013 FU NRL FX We thank Drs. Patricia Legler and Stella North for their comments on the manuscript. This work is supported by NRL 6.2 base program. The opinions expressed here are those of authors and do not represent those of the US Navy, the US Department of Defense, or the US government. NR 21 TC 4 Z9 4 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0006-291X J9 BIOCHEM BIOPH RES CO JI Biochem. Biophys. Res. Commun. PD FEB 17 PY 2012 VL 418 IS 3 BP 537 EP 540 DI 10.1016/j.bbrc.2012.01.061 PG 4 WC Biochemistry & Molecular Biology; Biophysics SC Biochemistry & Molecular Biology; Biophysics GA 900XL UT WOS:000300925300017 PM 22285187 ER PT J AU Jensen, AA Thompson, AM Schmidlin, FJ AF Jensen, Anders A. Thompson, Anne M. Schmidlin, F. J. TI Classification of Ascension Island and Natal ozonesondes using self-organizing maps SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPICAL SOUTH-ATLANTIC; TROPOSPHERIC OZONE MAXIMUM; MARINE BOUNDARY-LAYER; DEEP CONVECTION; WAVE-ONE; TRANSPORT; AFRICA; OCEAN; PACIFIC; TRACE AB Ozone profiles from balloon-borne ozonesondes are used for development of satellite algorithms and in chemistry-climate model initialization, assimilation and evaluation. An important issue in the application of these profiles is how best to treat variations where varying photochemical and dynamical influences can cause the ozone mixing ratio in the tropospheric segments of the profile to change by of a factor of 2-3 within a day. Clustering techniques are an ideal way to approach the statistical classification of profile data and we apply self-organizing maps to tropical tropospheric SHADOZ data, hypothesizing that the data will sort according to various influences on ozone, namely anthropogenic sources like biomass burning, meteorological conditions, and stratospheric or extra-tropical intrusions. Self-organizing maps, that use a learning algorithm to reveal the most prominent features of a data set according to a specified number of clusters, have been determined for the 1998-2009 SHADOZ profiles over Ascension Island (512 profiles, 7.98 degrees S, 14.42 degrees W) and Natal, Brazil (425 profiles, 5.42 degrees S, 35.38 degrees W). The 2 x 2 self-organizing map, which creates 4 clusters, reveals that deviations from the average ozone in the free troposphere include both increased ozone resulting from seasonal biomass burning in Africa and locally reduced ozone brought about by convective lifting of unpolluted boundary-layer air. Expanding to a 4 x 4 self-organizing map shows how biomass burning influences the yearly cycle of tropospheric ozone at Ascension Island and captures the seasonality of ozone at both Ascension Island and Natal. Comparing Ascension Island and Natal using a 4 x 4 self-organizing map at each site reveals similarities in mid-tropospheric ozone, but shows differences in lower-tropospheric ozone due to Ascension Island being closer to African biomass burning and more affected by descent from the mean Walker circulation, with less convective activity, than Natal. C1 [Jensen, Anders A.; Thompson, Anne M.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Schmidlin, F. J.] NASA, Wallops Flight Facil, Goddard Space Flight Ctr, Wallops Isl, VA 23337 USA. RP Jensen, AA (reprint author), Penn State Univ, Dept Meteorol, 413 Walker Bldg, University Pk, PA 16802 USA. EM amt16@psu.edu RI Thompson, Anne /C-3649-2014 OI Thompson, Anne /0000-0002-7829-0920 FU Earth and Environmental Systems Institute (EESI) through Pennsylvania State University; NASA SHADOZ [NNX09AJ23G] FX This research was supported by the Earth and Environmental Systems Institute (EESI) Environmental Scholar fund through Pennsylvania State University and the NASA SHADOZ grant NNX09AJ23G for which M. J. Kurylo and K. W. Jucks are thanked. We are grateful to the years of excellent sounding data from Russell Yon (Ascension Island), Neusa M. Paes Leme and Francisco DaSilva (INPE, Brazil). Conversations with Chris Nowotarski were exceptionally helpful. NR 56 TC 11 Z9 11 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 17 PY 2012 VL 117 AR D04302 DI 10.1029/2011JD016573 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 899NE UT WOS:000300821900002 ER PT J AU Gomez, RM Nedoluha, GE Neal, HL McDermid, IS AF Gomez, R. Michael Nedoluha, Gerald E. Neal, Helen L. McDermid, I. Stuart TI The fourth-generation Water Vapor Millimeter-Wave Spectrometer SO RADIO SCIENCE LA English DT Article ID MIDDLE ATMOSPHERE; RADIOMETER AB For 20 years the Naval Research Laboratory has been making continuous water vapor profile measurements at 22.235 GHz with the Water Vapor Millimeter-Wave Spectrometer (WVMS) instruments, with the program expanding from one to three instruments in the first 6 years. Since the initial deployments there have been gradual improvements in the instrument design which have improved data quality and reduced maintenance requirements. Recent technological developments have made it possible to entirely redesign the instrument and improve not only the quality of the measurements but also the capability of the instrument. We present the fourth-generation instrument now operating at Table Mountain, California, which incorporates the most recent advances in microwave radiometry. This instrument represents the most significant extension of our measurement capability to date, enabling us to measure middle atmospheric water vapor from similar to 26-80 km. C1 [Gomez, R. Michael; Nedoluha, Gerald E.] USN, Remote Sensing Div, Res Lab, Washington, DC 20375 USA. [Neal, Helen L.] Computat Phys Inc, Springfield, VA 22151 USA. [McDermid, I. Stuart] Jet Prop Lab, Table Mt Facil, Wrightwood, CA 92397 USA. RP Gomez, RM (reprint author), USN, Remote Sensing Div, Res Lab, Code 7227,4555 Overlook Ave SW, Washington, DC 20375 USA. EM mike.gomez@nrl.navy.mil FU Mauna Loa Observatory; NASA; Naval Research Laboratory; staff at the Table Mountain Facility FX We wish to thank the staff at the Table Mountain Facility and the Mauna Loa Observatory for their assistance and support. This work is sponsored by NASA under the Upper Atmosphere Research Program and the Naval Research Laboratory. NR 12 TC 3 Z9 3 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 J9 RADIO SCI JI Radio Sci. PD FEB 16 PY 2012 VL 47 AR RS1010 DI 10.1029/2011RS004778 PG 11 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA 899PC UT WOS:000300827300001 ER PT J AU Helmboldt, JF Lazio, TJW Intema, HT Dymond, KF AF Helmboldt, J. F. Lazio, T. J. W. Intema, H. T. Dymond, K. F. TI High-precision measurements of ionospheric TEC gradients with the Very Large Array VHF system SO RADIO SCIENCE LA English DT Article AB We have used a relatively long, contiguous VHF observation of a bright cosmic radio source (Cygnus A) with the Very Large Array (VLA) to demonstrate the capability of this instrument to study the ionosphere. This interferometer, and others like it, can observe ionospheric total electron content (TEC) fluctuations on a much wider range of scales than is possible with many other instruments. We have shown that with a bright source, the VLA can measure differential TEC values between pairs of antennas (delta TEC) with a precision of 3 x 10(-4) TECU. Here, we detail the data reduction and processing techniques used to achieve this level of precision. In addition, we demonstrate techniques for exploiting these high-precision delta TEC measurements to compute the TEC gradient observed by the array as well as small-scale fluctuations within the TEC gradient surface. A companion paper details specialized spectral analysis techniques used to characterize the properties of wave-like fluctuations within this data. C1 [Helmboldt, J. F.; Dymond, K. F.] USN, Res Lab, Washington, DC 20375 USA. [Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA. [Intema, H. T.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Helmboldt, JF (reprint author), USN, Res Lab, Code 7213,4555 Overlook Ave SW, Washington, DC 20375 USA. EM joe.helmboldt@nrl.navy.mil; joseph.lazio@jpl.nasa.gov; hintema@nrao.edu; kenneth.dymond@nrl.navy.mil RI Helmboldt, Joseph/C-8105-2012; Intema, Huib/D-1438-2012 OI Intema, Huib/0000-0002-5880-2730 FU 6.1 base funding; National Aeronautics and Space Administration FX The authors would like to thank the referees for useful comments and suggestions. Basic research in astronomy at the Naval Research Laboratory is supported by 6.1 base funding. The VLA was operated by the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. 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 16 TC 10 Z9 10 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 J9 RADIO SCI JI Radio Sci. PD FEB 16 PY 2012 VL 47 AR RS0K02 DI 10.1029/2011RS004883 PG 13 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA 899PC UT WOS:000300827300002 ER PT J AU Liu, DY Jolliff, BL Zeigler, RA Korotev, RL Wan, YS Xie, HQ Zhang, YH Dong, CY Wang, W AF Liu, Dunyi Jolliff, Bradley L. Zeigler, Ryan A. Korotev, Randy L. Wan, Yushan Xie, Hangqiang Zhang, Yuhai Dong, Chunyan Wang, Wei TI Comparative zircon U-Pb geochronology of impact melt breccias from Apollo 12 and lunar meteorite SaU 169, and implications for the age of the Imbrium impact SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE SHRIMP U-Pb analysis; impact-melt breccia; Apollo 12; SaU 169; Imbrium; Moon ID PROSPECTOR GAMMA-RAY; DECAY CONSTANTS; EVOLUTION; CATACLYSM; HISTORY; ORIGIN; MOON; GEOCHEMISTRY; SPECTROMETER; STRATIGRAPHY AB The ages of zircons from high-Th impact-melt breccias (IMBs) from meteorite Sayh al Uhaymir (SaU) 169 and from rock fragments in soil samples from Apollo 12 have been determined using the SHRIMP-II ion microprobe. The IMBs are very similar to each other in chemistry, mineralogy and texture, and the zircons from the KREEP-rich (high-Th) crystalline impact melt have similar U and Th contents and identical ages, within uncertainties, of 3920 +/- 13 (2 sigma) Ma (SaU 169) and 3914 +/- 7 (2 sigma) Ma (Apollo 12). The age results support the idea that the high-Th IMBs (Apollo 12 and SaU 169) formed in the same impact event. The similarity of composition and age suggest that SaU 169 and the high-Th IMB fragments of Apollo 12 originated from the same area of the Procellarum KREEP Terrane. We interpret the age of zircon grains in the Apollo 12 high-Th IMB as a precise and direct determination of the age of the Imbrium impact. This age is significantly older than the commonly cited age of 3.85 Ga but is similar to recent determinations from SIMS U-Pb dating of Apollo 14 apatite grains and with anticipated revision of ages by Ar-40-Ar-39 and Rb-87-Sr-86. The present zircon Pb-207-Pb-206 age is the first direct zircon age determination of the Imbrium impact event from an Apollo sample. Previous measurements of zircon ages of Apollo IMBs have recorded events pre-dating the Imbrium basin-forming event (C) 2011 Elsevier B.V. All rights reserved. C1 [Jolliff, Bradley L.; Zeigler, Ryan A.; Korotev, Randy L.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Jolliff, Bradley L.; Zeigler, Ryan A.; Korotev, Randy L.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Liu, Dunyi; Wan, Yushan; Xie, Hangqiang; Zhang, Yuhai; Dong, Chunyan; Wang, Wei] Chinese Acad Geol Sci, Inst Geol, Beijing SHRIMP Ctr, Beijing, Peoples R China. [Zeigler, Ryan A.] NASA, ARES Acquisit & Curat, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Jolliff, BL (reprint author), Washington Univ, Dept Earth & Planetary Sci, 1 Brookings Dr, St Louis, MO 63130 USA. EM blj@wustl.edu FU NASA [NNG04GG10G]; Ministry of Science and Technology of China [2009IM030800]; McDonnell Center for the Space Sciences FX We thank NASA for support through grant NNG04GG10G (RLK). We also acknowledge the Ministry of Science and Technology of China for support through grant 2009IM030800. We are grateful for support from the McDonnell Center for the Space Sciences, which enabled BLJ and RAZ to visit the SHRIMP-II lab in Beijing and provided seed funds for this collaboration. We thank Beda Hoffman and the Natural History Museum of Bern for providing the SaU 169 samples for analysis. We thank R. T. Pidgeon for assistance during preparation of the manuscript. The manuscript was greatly improved by comments from reviews by Marc Norman and an anonymous reviewer. NR 46 TC 28 Z9 29 U1 3 U2 17 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD FEB 15 PY 2012 VL 319 BP 277 EP 286 DI 10.1016/j.epsl.2011.12.014 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 913WW UT WOS:000301909100029 ER PT J AU Kokkila, SI Bera, PP Francisco, JS Lee, TJ AF Kokkila, Sara I. Bera, Partha P. Francisco, Joseph S. Lee, Timothy J. TI A group increment scheme for infrared absorption intensities of greenhouse gases SO JOURNAL OF MOLECULAR STRUCTURE LA English DT Article DE IR intensities; ab initio calculations; Additivity models; Global warming molecules; Hydrofluorocarbons; Hydrofluoroethers ID GLOBAL WARMING POTENTIALS; GAUSSIAN BASIS FUNCTIONS; FIRST-ROW ATOMS; HYDROFLUOROETHERS HFES; MOLECULAR CALCULATIONS; RADIATIVE EFFICIENCY; HYDROFLUOROCARBONS; ALTERNATIVES AB A molecule's absorption in the atmospheric infrared (IR) window (IRW) is an indicator of its efficiency as a greenhouse gas. A model for estimating the absorption of a fluorinated molecule within the IRW was developed to assess its radiative impact. This model will be useful in comparing different hydrofluorocarbons and hydrofluoroethers contribution to global warming. The absorption of radiation by greenhouse gases, in particular hydrofluoroethers and hydrofluorocarbons, was investigated using ab initio quantum mechanical methods. Least squares regression techniques were used to create a model based on this data. The placement and number of fluorines in the molecule were found to affect the absorption in the IR window and were incorporated into the model. Several group increment models are discussed. An additive model based on one-carbon groups is found to work satisfactorily in predicting the ab initio calculated vibrational intensities. (C) 2011 Elsevier B.V. All rights reserved. C1 [Bera, Partha P.; Lee, Timothy J.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. [Kokkila, Sara I.] Coll St Benedict, St Joseph, MN 56374 USA. [Kokkila, Sara I.] St Johns Univ, St Joseph, MN 56374 USA. [Francisco, Joseph S.] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA. [Francisco, Joseph S.] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA. RP Lee, TJ (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA. EM Timothy.J.Lee@nasa.gov RI Lee, Timothy/K-2838-2012; Bera, Partha /K-8677-2012; OI Kokkila Schumacher, Sara/0000-0002-2338-4815 FU NASA Ames Research Center; NASA FX This paper is dedicated to Professor Boris Galabov on the occasion of his 70th birthday, who has made seminal contributions to the study of IR intensities. SIK gratefully acknowledges an Undergraduate Student Research Program (USRP) summer fellowship at the NASA Ames Research Center. PPB gratefully acknowledges a NASA Postdoctoral Program Fellowship award. Helpful conversations with Dr. Jeff Cuzzi are gratefully acknowledged. NR 32 TC 1 Z9 1 U1 3 U2 14 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-2860 J9 J MOL STRUCT JI J. Mol. Struct. PD FEB 15 PY 2012 VL 1009 SI SI BP 89 EP 95 DI 10.1016/j.molstruc.2011.11.048 PG 7 WC Chemistry, Physical SC Chemistry GA 905ZY UT WOS:000301315900013 ER PT J AU Lin, ZW Adams, JH Barghouty, AF Randeniya, SD Tripathi, RK Watts, JW Yepes, PP AF Lin, Z. W. Adams, J. H., Jr. Barghouty, A. F. Randeniya, S. D. Tripathi, R. K. Watts, J. W. Yepes, P. P. TI Comparisons of several transport models in their predictions in typical space radiation environments SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Transport code; Space radiation; Radiation shielding; Solar particle events; Galactic cosmic rays ID ACCURATE UNIVERSAL PARAMETERIZATION; ABSORPTION CROSS-SECTIONS; CODE AB We have used several transport codes to calculate dose and dose equivalent values as well as the particle spectra behind a slab or inside a spherical shell shielding in typical space radiation environments. Two deterministic codes, HZETRN and UPROP, and two Monte Carlo codes, FLUKA and Geant4, are included. A soft solar particle event, a hard solar particle event, and a solar minimum galactic cosmic rays environment are considered; and the shielding material is either aluminum or polyethylene. We find that the dose values and particle spectra from HZETRN are in general rather consistent with Geant4 except for neutrons. The dose equivalent values from HZETRN and Geant4 are not far from each other, but the HZETRN values behind shielding are often lower than the Geant4 values. Results from FLUKA and Geant4 are mostly consistent for considered cases. However, results from the legacy code UPROP are often quite different from the other transport codes, partly due to its non-consideration of neutrons. Comparisons for the spherical shell geometry exhibit the same qualitative features as for the slab geometry. In addition, results from both deterministic and Monte Carlo transport codes show that the dose equivalent inside the spherical shell decreases from the center to the inner surface and this decrease is large for solar particle events; consistent with an earlier study based on deterministic radiation transport results. This study demonstrates both the consistency and inconsistency among these transport models in their typical space radiation predictions; further studies will be required to pinpoint the exact physics modules in these models that cause the differences and thus may be improved. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Lin, Z. W.] E Carolina Univ, Dept Phys, Greenville, NC 27858 USA. [Adams, J. H., Jr.; Barghouty, A. F.; Watts, J. W.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Randeniya, S. D.] Univ Texas MD Anderson Canc Ctr, Houston, TX 77030 USA. [Tripathi, R. K.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Watts, J. W.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA. [Yepes, P. P.] Rice Univ, Dept Phys, Houston, TX 77005 USA. RP Lin, ZW (reprint author), E Carolina Univ, Dept Phys, C-209 Howell Sci Complex, Greenville, NC 27858 USA. EM linz@ecu.edu; James.h.adams@nasa.gov; Abdulnasser.F.Barghouty@nasa.gov; kdrandeniya@mdanderson.org; Ram.K.Tripathi@nasa.gov; yepes@rice.edu FU NASA [NNM07AC99P] FX Z.W.L. gratefully acknowledges support provided under NASA Contract No. NNM07AC99P. NR 25 TC 11 Z9 11 U1 0 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD FEB 15 PY 2012 VL 49 IS 4 BP 797 EP 806 DI 10.1016/j.asr.2011.11.025 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 905YO UT WOS:000301312300018 ER PT J AU Sayer, AM Hsu, NC Bettenhausen, C Ahmad, Z Holben, BN Smirnov, A Thomas, GE Zhang, J AF Sayer, A. M. Hsu, N. C. Bettenhausen, C. Ahmad, Z. Holben, B. N. Smirnov, A. Thomas, G. E. Zhang, J. TI SeaWiFS Ocean Aerosol Retrieval (SOAR): Algorithm, validation, and comparison with other data sets SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OPTICAL DEPTH; ATMOSPHERIC CORRECTION; DATA-ASSIMILATION; SPECTRAL RADIANCES; MODIS; SATELLITE; AERONET; LAND; DUST; REFLECTANCE AB The Sea-viewing Wide Field-of-view Sensor (SeaWiFS) provides a well-calibrated 13-year (1997-2010) record of top-of-atmosphere radiance, suitable for use in retrieval of atmospheric aerosol optical depth (AOD). This paper presents and validates a SeaWiFS Ocean Aerosol Retrieval (SOAR) algorithm, which retrieves the AOD at 550 nm and the partition of aerosol particle volume between fine and coarse modes. The algorithm has been applied over water to the whole SeaWiFS record. The data set includes quality flags to identify those retrievals suitable for quantitative use. SOAR has been validated against Aerosol Robotic Network (AERONET) and Maritime Aerosol Network (MAN) data and found to compare well (correlation 0.86 at 550 nm and 0.88 at 870 nm for AERONET, and 0.87 at 550 nm and 0.85 at 870 nm for MAN, using recommended quality control settings). These comparisons are used to identify the typical level of uncertainty on the AOD, estimated as 0.03 + 15% at 550 nm and 0.03 + 10% at 870 nm. The data set also includes the (A) over circle ngstrom exponent, although as expected this is noisy for low aerosol loadings (correlation 0.50; 0.78 for points where the AOD at 550 nm is 0.3 or more). Retrieved AOD is compared with colocated observations from other satellite sensors; regional and seasonal patterns are found to be common between all data sets, and differences generally linked to factors such as cloud screening and retrieval assumptions. Citation: Sayer, A. M., N. C. Hsu, C. Bettenhausen, Z. Ahmad, B. N. Holben, A. Smirnov, G. E. Thomas, and J. Zhang (2012), SeaWiFS Ocean Aerosol Retrieval (SOAR): Algorithm, validation, and comparison with other data sets, J. Geophys. Res., 117, D03206, doi:10.1029/2011JD016599. C1 [Sayer, A. M.; Hsu, N. C.; Bettenhausen, C.; Ahmad, Z.; Holben, B. N.; Smirnov, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Thomas, G. E.] Univ Oxford, Oxford OX1 3PU, England. [Zhang, J.] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA. [Sayer, A. M.] Univ Space Res Assoc, Columbia, MD USA. [Bettenhausen, C.] Sci Syst & Applicat Inc, Lanham, MD USA. [Ahmad, Z.] Sci & Data Syst Inc, Silver Spring, MD USA. [Smirnov, A.] Sigma Space Corp, Lanham, MD USA. RP Sayer, AM (reprint author), Univ Space Res Assoc, Columbia, MD USA. EM andrew.sayer@nasa.gov RI Smirnov, Alexander/C-2121-2009; Sayer, Andrew/H-2314-2012; Hsu, N. Christina/H-3420-2013 OI Smirnov, Alexander/0000-0002-8208-1304; Sayer, Andrew/0000-0001-9149-1789; FU NASA FX This work was supported by a grant from the NASA MEaSUREs program, managed by Martha Maiden. SeaWiFS level 1a data, the SeaDAS software, and NCEP meteorological fields were obtained from the SeaWiFS Ocean Biology Processing Group data distribution service. GlobAerosol was an ESA Data User Element project. The Naval Research Laboratory are thanked for the DA-MODIS data. MODIS data were obtained from the NASA LAADS, and MISR from the NASA Langley ASDC. The AERONET and MAN PIs are thanked for the creation and maintenance of the Sun photometer data records. The authors thank M. Chin, T. Diehl, R. A. Kahn, R. C. Levy, S. Mattoo, L. A. Remer, and Q. Tan for helpful discussions and comments on the manuscript. The authors acknowledge the detailed and constructive comments of three anonymous reviewers, whose suggestions strengthened the manuscript. NR 71 TC 28 Z9 28 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 FEB 15 PY 2012 VL 117 AR D03206 DI 10.1029/2011JD016599 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 899MY UT WOS:000300821200001 ER PT J AU Xiong, S Briggs, MS Connaughton, V Fishman, GJ Tierney, D Fitzpatrick, G Foley, S Guiriec, S Holzworth, RH Hutchins, ML AF Xiong, S. Briggs, M. S. Connaughton, V. Fishman, G. J. Tierney, D. Fitzpatrick, G. Foley, S. Guiriec, S. Holzworth, R. H. Hutchins, M. L. TI Location prediction of electron TGFs SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID GAMMA-RAY FLASHES; RUNAWAY BREAKDOWN; SPRITES; THUNDERSTORM; AIR AB Terrestrial Gamma-ray Flashes (TGFs) are brief pulses of energetic radiation that correlate with thunderstorms and lightning. Most TGFs are observed as gamma-ray pulses; less frequently they can be observed as electrons and positrons that travel along the geomagnetic field line from the source to the detector. In this paper we predict where electron TGFs should be observed by tracing geomagnetic field lines from likely TGF sources and determining the intersections with satellite orbits. TGF source locations are based upon lightning maps by the Lightning Imaging Sensor (LIS) and the Optical Transient Detector (OTD). Predictions are made both for existing spacecraft with instruments observing TGFs and for other orbits. We compare the predictions to the locations of TGFs that have been observed as electron TGFs. 12 of the 13 known electron TGFs are within the predicted high-rate regions. Based on the predicted location maps of electron TGFs, we find that electron TGFs should sometimes be observed above areas with low lightning activity and that electron TGFs are best observed at low altitudes (below approximately 1000 km). C1 [Fishman, G. J.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Tierney, D.; Fitzpatrick, G.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Foley, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Holzworth, R. H.; Hutchins, M. L.] Univ Washington, Seattle, WA 98195 USA. [Xiong, S.; Briggs, M. S.; Connaughton, V.; Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. RP Xiong, S (reprint author), NSSTC, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM shaolin.xiong@uah.edu FU NASA in the United States; BMWi/DLR in Germany; Fermi Guest Investigator Program FX We thank the reviewers for their comments that improved this paper. The Fermi GBM Collaboration acknowledges support for GBM development, operations, and data analysis from NASA in the United States and from BMWi/DLR in Germany. This work was supported in part by the Fermi Guest Investigator Program. The v2.2 gridded satellite lightning data were produced by the NASA LIS/OTD Science Team (Principal Investigator, Hugh J. Christian, NASA / Marshall Space Flight Center) and are available from the Global Hydrology Resource Center (http://ghrc.msfc.nasa.gov). The authors wish to thank the World Wide Lightning Location Network (http://wwlln.net), a collaboration among over 50 universities and institutions, for providing the lightning location data used in this paper. The authors appreciate David M. Smith for helpful comments. SF acknowledges the support of the Irish Research Council for Science, Engineering and Technology, cofunded by Marie Curie Actions under FP7. NR 31 TC 3 Z9 3 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD FEB 15 PY 2012 VL 117 AR A02309 DI 10.1029/2011JA017085 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 899OH UT WOS:000300825100001 ER PT J AU Mishchenko, MI Dlugach, JM AF Mishchenko, Michael I. Dlugach, Janna M. TI Adhesion of mineral and soot aerosols can strongly affect their scattering and absorption properties SO OPTICS LETTERS LA English DT Article ID T-MATRIX; RADIATIVE PROPERTIES; PARTICLES; HYGROSCOPICITY; MORPHOLOGY AB We use the numerically exact superposition T-matrix method to compute the optical cross sections and the Stokes scattering matrix for polydisperse mineral aerosols (modeled as homogeneous spheres) covered with a large number of much smaller soot particles. These results are compared with the Lorenz-Mie results for a uniform external mixture of mineral and soot aerosols. We show that the effect of soot particles adhering to large mineral particles can be to change the extinction and scattering cross sections and the asymmetry parameter quite substantially. The effect on the phase function and degree of linear polarization can be equally significant. (C) 2012 Optical Society of America C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Dlugach, Janna M.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine. 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 FU NASA; National Academy of Sciences of Ukraine FX We thank Ping Yang and an anonymous referee for constructive reviews. This research was partly funded by the NASA Radiation Sciences Program managed by Hal Maring and by the NASA Remote Sensing Theory Program managed by Lucia Tsaoussi. We also acknowledge support from the National Academy of Sciences of Ukraine under the Main Astronomical Observatory GRAPE/GPU/GRID Computing Cluster Project. NR 19 TC 7 Z9 7 U1 1 U2 13 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 FEB 15 PY 2012 VL 37 IS 4 BP 704 EP 706 PG 3 WC Optics SC Optics GA 898AF UT WOS:000300706500087 PM 22344154 ER PT J AU Weng, QH Quattrochi, DA Carlson, TN AF Weng, Qihao Quattrochi, Dale A. Carlson, Toby N. TI Remote sensing of urban environments: Special issue Preface SO REMOTE SENSING OF ENVIRONMENT LA English DT Editorial Material C1 [Weng, Qihao] Indiana State Univ, Ctr Urban & Environm Change, Terre Haute, IN 47809 USA. [Quattrochi, Dale A.] NASA, George C Marshall Space Flight Ctr, Redstone Arsenal, AL USA. [Carlson, Toby N.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. RP Weng, QH (reprint author), Indiana State Univ, Ctr Urban & Environm Change, Terre Haute, IN 47809 USA. EM qweng@indstate.edu OI Weng, Qihao/0000-0002-2498-0934 NR 12 TC 2 Z9 2 U1 1 U2 18 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD FEB 15 PY 2012 VL 117 BP 1 EP 2 DI 10.1016/j.rse.2011.08.005 PG 2 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 894WX UT WOS:000300459300001 ER PT J AU Roberts, DA Quattrochi, DA Hulley, GC Hook, SJ Green, RO AF Roberts, Dar A. Quattrochi, Dale A. Hulley, Glynn C. Hook, Simon J. Green, Robert O. TI Synergies between VSWIR and TIR data for the urban environment: An evaluation of the potential for the Hyperspectral Infrared Imager (HyspIRI) Decadal Survey mission SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE HyspIRI; Urban remote sensing; Spectral Mixture Analysis; Land surface temperature; Spectroscopy ID SPECTRAL MIXTURE ANALYSIS; LAND-SURFACE TEMPERATURE; IMAGING SPECTROMETER AVIRIS; SENSIBLE HEAT-FLUX; IMPERVIOUS SURFACE; WATER-VAPOR; MULTISENSOR DATA; VEGETATION; EMISSIVITY; REFLECTANCE AB This study provides an introduction to the HyspIRI mission a National Research Council "Decadal Survey" mission that combines a 213 channel visible, near-infrared and shortwave infrared (VSWIR) imaging spectrometer with an 8 channel multispectral thermal infrared (TIR) instrument and evaluates some of its potential in urban science. Potential synergies between VSWIR and TIR data are explored using analogous airborne data acquired over the Santa Barbara metropolitan region in June, 2008. These data were analyzed at both their native spatial resolutions (7.5 m VSWIR and 15 m TIR), and aggregated 60 m spatial resolution similar to HyspIRI. A spectral library of dominant urban materials (e.g., grass, trees, soil, roof types, roads) was developed from field and airborne-measured spectra using Multiple-Endmember Spectral Mixture Analysis (MESMA) and used to map fractions of impervious, soil, green vegetation (CV, e.g., trees, lawn) and non-photosynthetic vegetation (NPV). Land Surface Temperature (LST) and emissivity were also retrieved from the airborne data. Co-located pixels from the VSWIR and TIR airborne data were used to generate reflectance/emissivity spectra for a subset of urban materials. MESMA was used to map GV, NPV, soil and impervious fractions at the different spatial resolutions and compare the fractional estimates across spatial scales. Important surface energy parameters, including albedo, vegetation cover fraction, broadband emissivity and surface temperature were also determined for and evaluated for 14 urban and natural land-cover classes in the region. Fractions were validated using 1 m digital photography. Fractions for GV and NPV were highly correlated with validation fractions at all spatial scales, producing a near 1:1 relationship but with a <10% overestimate of CV from MESMA. Similar, high correlations were observed for impervious surfaces, although impervious was significantly underestimated in most urban areas and soil overestimated. Comparison of fractions across scales showed high correlation between CV and NPV at 7.5 and 60 m resolution, suggesting that HyspIRI will provide accurate measures of these two measures in urban areas. An inverse relationship between vegetation cover and LST was observed. Albedo proved to be highly variable and poorly correlated with LST. Broadband emissivity was far less variable with high emissivity surfaces (similar to 0.95) including vegetation, water and asphalt, and low emissivity surfaces (<0.95) including selected roof types, beach sands and senesced grasslands. Residential and commercial areas showed a general pattern of increasing LST with increasing impervious fraction with the highest impervious fractions mapped in commercial areas, roads and roofs. Fine scale spatial structure in cover fractions and LST demonstrated important departures from a simple inverse relationship between CV and LST, even at 60 m. The results demonstrate the utility of HyspIRI data for urban studies and provide an insight of what will be possible on a global scale when HyspIRI data become available. (C) 2011 Elsevier Inc. All rights reserved. C1 [Roberts, Dar A.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA. [Quattrochi, Dale A.] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35812 USA. [Hulley, Glynn C.; Hook, Simon J.; Green, Robert O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Roberts, DA (reprint author), Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA. EM dar@geog.ucsb.edu FU NASA [NNX07AC89G, NNX11AE44G] FX We wish to thank Michael Toomey and Eliza Bradley for their assistance in translating polygons from Google Earth to ENVI vector files. We wish to thank the Jet Propulsion Laboratory for providing radiometrically calibrated, orthorectified AVIRIS and MASTER data. AVIRIS/MASTER data analyzed in this study were acquired as part of the NASA North American Carbon Program (NACP) for research grant NNX07AC89G, Remote-Sensing methane emissions: field-validation with Seepage from marine, urban, and submerged-city sources. The analysis was partially supported by a NASA HyspIRI Preparatory Grant, NNX11AE44G. A portion of this work was carried out at the Jet Propulsion Laboratory/California Institute of Technology, Pasadena, California, under contract with NASA We also wish to thank the reviewers for constructive comments. NR 65 TC 79 Z9 81 U1 9 U2 79 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD FEB 15 PY 2012 VL 117 BP 83 EP 101 DI 10.1016/j.rse.2011.07.021 PG 19 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 894WX UT WOS:000300459300008 ER PT J AU Moore, TS Dowell, MD Franz, BA AF Moore, Timothy S. Dowell, Mark D. Franz, Bryan A. TI Detection of coccolithophore blooms in ocean color satellite imagery: A generalized approach for use with multiple sensors SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Ocean color; Classification; Coccolithophores; Optical water types ID PHYTOPLANKTON FUNCTIONAL-GROUPS; SEA-SURFACE DISTRIBUTION; LATE AUSTRAL SUMMER; SOUTHERN-OCEAN; EMILIANIA-HUXLEYI; ATLANTIC-OCEAN; VARIABILITY; DYNAMICS; ALGORITHM; SECTOR AB A generalized coccolithophore bloom classifier has been developed for use with ocean color imagery. The bloom classifier was developed using extracted satellite reflectance data from SeaWiFS images screened by the default bloom detection mask. In the current application, we extend the optical water type (OWT) classification scheme by adding a new coccolithophore bloom class formed from these extracted reflectances. Based on an in situ coccolithophore data set from the North Atlantic, the detection levels with the new scheme were between 1,500 and 1,800 coccolithophore cells/mL and 43,000 and 78,000 liths/mL The detected bloom area using the OWT method was an average of 1.75 times greater than the default bloom detector based on a collection of SeaWiFS 1 km imagery. The versatility of the scheme is shown with SeaWiFS, MODIS Aqua, CZCS and MERIS imagery at the 1 km scale. The OWT scheme was applied to the daily global SeaWiFS imagery mission data set (years 1997-2010). Based on our results, average annual coccolithophore bloom area was more than two times greater in the southern hemisphere compared to the northern hemisphere with values of 2.00 x 10(6) km(2) and 0.75 x 10(6) km(2), respectively. The new algorithm detects larger bloom areas in the Southern Ocean compared to the default algorithm, and our revised global annual average of 2.75 x 10(6) km(2) is dominated by contributions from the Southern Ocean. (C) 2011 Elsevier Inc. All rights reserved. C1 [Moore, Timothy S.] Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA. [Dowell, Mark D.] European Commiss, JRC, Inst Environm & Sustainabil, I-21027 Ispra, VA, Italy. [Franz, Bryan A.] NASA, Goddard Space Flight Ctr, Ocean Biol Proc Grp, Greenbelt, MD 20771 USA. RP Moore, TS (reprint author), Univ New Hampshire, Ocean Proc Anal Lab, Morse Hall, Durham, NH 03824 USA. EM timothy.moore@unh.edu; mark.dowell@jrc.ec.europa.eu; bryan.a.franz@nasa.gov RI Franz, Bryan/D-6284-2012 OI Franz, Bryan/0000-0003-0293-2082 FU NASA [NNX08AG80A] FX This work was supported by NASA grant NNX08AG80A. Thanks to Tim Smyth for providing the North Atlantic in situ data set that added significantly to the work. The authors thank the anonymous reviewers for their time in providing helpful comments and suggestions. NR 45 TC 29 Z9 30 U1 5 U2 35 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD FEB 15 PY 2012 VL 117 BP 249 EP 263 DI 10.1016/j.rse.2011.10.001 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 894WX UT WOS:000300459300021 ER PT J AU Wang, ZS Schaaf, CB Chopping, MJ Strahler, AH Wang, JD Roman, MO Rocha, AV Woodcock, CE Shuai, YM AF Wang, Zhuosen Schaaf, Crystal B. Chopping, Mark J. Strahler, Alan H. Wang, Jindi Roman, Miguel O. Rocha, Adrian V. Woodcock, Curtis E. Shuai, Yanmin TI Evaluation of Moderate-resolution Imaging Spectroradiometer (MODIS) snow albedo product (MCD43A) over tundra SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE MODIS standard and daily Albedo product; Snow; High latitude tundra; Spatial representativeness ID LAND-SURFACE ALBEDO; REFLECTANCE DISTRIBUTION FUNCTION; RADIATION MEASUREMENT PROGRAM; IN-SITU MEASUREMENTS; BIDIRECTIONAL REFLECTANCE; CLIMATE MODEL; NADIR REFLECTANCE; BOREAL FORESTS; NORTH-AMERICA; BRDF MODELS AB This study assesses the MODIS standard Bidirectional Reflectance Distribution Function (BRDF)/Albedo product, and the daily Direct Broadcast BRDF/Albedo algorithm at tundra locations under large solar zenith angles and high anisotropic diffuse illumination and multiple scattering conditions. These products generally agree with ground-based albedo measurements during the snow cover period when the Solar Zenith Angle (SZA) is less than 70 degrees. An integrated validation strategy, including analysis of the representativeness of the surface heterogeneity, is performed to decide whether direct comparisons between field measurements and 500-m satellite products were appropriate or if the scaling of finer spatial resolution airborne or spaceborne data was necessary. Results indicate that the Root Mean Square Errors (RMSEs) are less than 0.047 during the snow covered periods for all MCD43 albedo products at several Alaskan tundra areas. The MCD43 1-day daily albedo product is particularly well suited to capture the rapidly changing surface conditions during the spring snow melt. Results also show that a full expression of the blue sky albedo is necessary at these large SZA snow covered areas because of the effects of anisotropic diffuse illumination and multiple scattering. In tundra locations with dark residue as a result of fire, the MODIS albedo values are lower than those at the unburned site from the start of snowmelt. (C) 2011 Elsevier Inc. All rights reserved. C1 [Wang, Zhuosen; Schaaf, Crystal B.; Strahler, Alan H.; Woodcock, Curtis E.] Boston Univ, Ctr Remote Sensing, Dept Geog & Environm, Boston, MA 02215 USA. [Wang, Zhuosen; Wang, Jindi] Beijing Normal Univ, State Key Lab Remote Sensing Sci, Ctr Remote Sensing, Beijing 100875, Peoples R China. [Wang, Zhuosen; Wang, Jindi] Beijing Normal Univ, Beijing Key Lab Remote Sensing Environm & Digital, GIS Geog Coll, Beijing 100875, Peoples R China. [Chopping, Mark J.] Montclair State Univ, Dept Earth & Environm Studies, Montclair, NJ USA. [Roman, Miguel O.] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab Code 619, Greenbelt, MD 20771 USA. [Rocha, Adrian V.] Marine Biol Lab, Ctr Ecosyst, Woods Hole, MA 02543 USA. [Shuai, Yanmin] Earth Resources Technol Inc, Laurel, MD 20707 USA. [Schaaf, Crystal B.] Univ Massachusetts, Boston, MA 02125 USA. RP Wang, ZS (reprint author), Boston Univ, Ctr Remote Sensing, Dept Geog & Environm, Boston, MA 02215 USA. EM wangzhs@bu.edu RI Shuai, Yanmin/G-1329-2012; Rocha, Adrian/B-6504-2013; Roman, Miguel/D-4764-2012 OI Roman, Miguel/0000-0003-3953-319X FU NASA [NNX09AL03G, NNX08AE94A, NNX11AD58G]; NSF [OPP-0856853, DEB-0423385]; National Natural Science Foundation of China [40871163] FX This research was supported by NASA awards NNX09AL03G, NNX08AE94A, and NNX11AD58G, NSF grants OPP-0856853 and DEB-0423385, National Natural Science Foundation of China (40871163). The MODIS data were obtained from the NASA Distributed Active Archive Centers (DAACs). The Landsat data were obtained from the USGS Earth Resources Observation and Science (EROS) Center. We also thank Dr. Ellsworth Dutton for providing the ARM ground data. NR 98 TC 44 Z9 51 U1 1 U2 22 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 FEB 15 PY 2012 VL 117 BP 264 EP 280 DI 10.1016/j.rse.2011.10.002 PG 17 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 894WX UT WOS:000300459300022 ER PT J AU Goossens, S Ishihara, Y Matsumoto, K Sasaki, S AF Goossens, Sander Ishihara, Yoshiaki Matsumoto, Koji Sasaki, Sho TI Local lunar gravity field analysis over the South Pole-Aitken basin from SELENE farside tracking data SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MASS ANOMALIES; PROSPECTOR; MISSION; KAGUYA; LINE; MOON; CLEMENTINE; RESOLUTION; GANYMEDE; SPHERE AB We present a method with which we determined the local lunar gravity field model over the South Pole-Aitken (SPA) basin on the farside of the Moon by estimating adjustments to a global lunar gravity field model using SELENE tracking data. Our adjustments are expressed in localized functions concentrated over the SPA region in a spherical cap with a radius of 45 degrees centered at (191.1 degrees E, 53.2 degrees S), and the resolution is equivalent to a 150th degree and order spherical harmonics expansion. The new solution over SPA was used in several applications of geophysical analysis. It shows an increased correlation with high-resolution lunar topography in the frequency band l = 40-70, and admittance values are slightly different and more leveled when compared to other, global gravity field models using the same data. The adjustments expressed in free-air anomalies and differences in Bouguer anomalies between the local solution and the a priori global solution correlate with topographic surface features. The Moho structure beneath the SPA basin is slightly modified in our solution, most notably at the southern rim of the Apollo basin and around the Zeeman crater. C1 [Goossens, Sander; Ishihara, Yoshiaki; Matsumoto, Koji; Sasaki, Sho] Natl Astron Observ Japan, RISE Project, Oshu, Iwate 0230861, Japan. [Goossens, Sander] NASA, Goddard Space Flight Ctr, CRESST Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Goossens, Sander] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA. RP Goossens, S (reprint author), Natl Astron Observ Japan, RISE Project, 2-12 Hoshigaoka, Oshu, Iwate 0230861, Japan. EM sander.j.goossens@nasa.gov; ishihara@miz.nao.ac.jp; matumoto@miz.nao.ac.jp; sho@miz.nao.ac.jp RI Ishihara, Yoshiaki/A-8499-2011; Goossens, Sander/K-2526-2015; OI Goossens, Sander/0000-0002-7707-1128; Ishihara, Yoshiaki/0000-0002-0375-6300 FU Noriyuki Namiki (PERC, Chiba Institute of Technology, Japan); Takahiro Iwata (ISAS/JAXA, Japan); Japan Society for the Promotion of Science [20244073] FX We thank the Planetary Geodynamics Laboratory of NASA/GSFC for providing the GEODYN II/SOLVE software, and we are especially grateful to David Rowlands and Frank Lemoine for discussions concerning the software. We thank Mark Wieczorek for comments on the manuscript, particularly those concerning the localization procedures. The localization transformations applied in this work make extensive use of his SHTOOLS library, which is freely available from "http://www.ipgp.fr/similar to wieczor/SHTOOLS/SHTOOLS.html". We also acknowledge support from Noriyuki Namiki (PERC, Chiba Institute of Technology, Japan) and Takahiro Iwata (ISAS/JAXA, Japan). Two anonymous reviewers are thanked for their comments which helped improve this manuscript. All figures were generated with the free Generic Mapping Tools (GMT) software [Wessel and Smith, 1991]. This work was supported by Grant-in-Aid for Scientific Research (to S. S.) (grant 20244073) from the Japan Society for the Promotion of Science. NR 39 TC 2 Z9 2 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB 14 PY 2012 VL 117 AR E02005 DI 10.1029/2011JE003831 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 899OR UT WOS:000300826100001 ER PT J AU Schoepp-Cothenet, B van Lis, R Philippot, P Magalon, A Russell, MJ Nitschke, W AF Schoepp-Cothenet, Barbara van Lis, Robert Philippot, Pascal Magalon, Axel Russell, Michael J. Nitschke, Wolfgang TI The ineluctable requirement for the trans-iron elements molybdenum and/or tungsten in the origin of life SO SCIENTIFIC REPORTS LA English DT Article ID MULTIPLE SEQUENCE ALIGNMENT; OXIDATION-STATE; EVOLUTION; PROTEIN; ENVIRONMENT; ATMOSPHERE; TOOLS AB An evolutionary tree of key enzymes from the Complex-Iron-Sulfur-Molybdoenzyme (CISM) superfamily distinguishes "ancient" members, i.e. enzymes present already in the last universal common ancestor (LUCA) of prokaryotes, from more recently evolved subfamilies. The majority of the presented subfamilies and, as a consequence, the Molybdo-enzyme superfamily as a whole, appear to have existed in LUCA. The results are discussed with respect to the nature of bioenergetic substrates available to early life and to problems arising from the low solubility of molybdenum under conditions of the primordial Earth. C1 [Schoepp-Cothenet, Barbara; van Lis, Robert; Nitschke, Wolfgang] Univ Aix Marseille, CNRS, Lab Bioenerget & Ingn Prot BIP, Marseille, France. [Magalon, Axel] Univ Aix Marseille, CNRS, LCB, Marseille, France. [Philippot, Pascal] IPGP, Paris, France. [Russell, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Nitschke, W (reprint author), Univ Aix Marseille, CNRS, Lab Bioenerget & Ingn Prot BIP, Marseille, France. EM nitschke@imm.cnrs.fr OI Nitschke, Wolfgang/0000-0003-2084-3032 FU National Aeronautics and Space Administration FX MJR'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 31 TC 29 Z9 29 U1 2 U2 32 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD FEB 13 PY 2012 VL 2 AR 263 DI 10.1038/srep00263 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 896PQ UT WOS:000300582000002 PM 22355775 ER PT J AU Samanta, A Knyazikhin, Y Xu, L Dickinson, RE Fu, R Costa, MH Saatchi, SS Nemani, RR Myneni, RB AF Samanta, Arindam Knyazikhin, Yuri Xu, Liang Dickinson, Robert E. Fu, Rong Costa, Marcos H. Saatchi, Sassan S. Nemani, Ramakrishna R. Myneni, Ranga B. TI Seasonal changes in leaf area of Amazon forests from leaf flushing and abscission SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID SPECTRAL VEGETATION INDEXES; LAND-SURFACE; TROPICAL FOREST; SOUTH-AMERICA; RAIN-FOREST; DRY SEASON; WET SEASON; MODIS; PHENOLOGY; CLIMATE AB A large increase in near-infrared (NIR) reflectance of Amazon forests during the light-rich dry season and a corresponding decrease during the light-poor wet season has been observed in satellite measurements. This increase has been variously interpreted as seasonal change in leaf area resulting from net leaf flushing in the dry season or net leaf abscission in the wet season, enhanced photosynthetic activity during the dry season from flushing new leaves and as change in leaf scattering and absorption properties between younger and older leaves covered with epiphylls. Reconciling these divergent views using theory and observations is the goal of this article. The observed changes in NIR reflectance of Amazon forests could be due to similar, but small, changes in NIR leaf albedo (reflectance plus transmittance) resulting from the exchange of older leaves for newer ones, but with the total leaf area unchanged. However, this argument ignores accumulating evidence from ground-based reports of higher leaf area in the dry season than the wet season, seasonal changes in litterfall and does not satisfactorily explain why NIR reflectance of these forests decreases in the wet season. More plausibly, the increase in NIR reflectance during the dry season and the decrease during the wet season would result from changes in both leaf area and leaf optical properties. Such change would be consistent with known phenological behavior of tropical forests, ground-based reports of seasonal changes in leaf area, litterfall, leaf optical properties and fluxes of evapotranspiration, and thus, would reconcile the various seemingly divergent views. C1 [Samanta, Arindam] Atmospher & Environm Res Inc, Lexington, MA 02421 USA. [Samanta, Arindam; Knyazikhin, Yuri; Xu, Liang; Myneni, Ranga B.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. [Dickinson, Robert E.; Fu, Rong] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA. [Costa, Marcos H.] Univ Fed Vicosa, BR-36570000 Vicosa, MG, Brazil. [Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nemani, Ramakrishna R.] NASA, Biospher Sci Branch, AMES Res Ctr, Moffett Field, CA 94035 USA. RP Samanta, A (reprint author), Atmospher & Environm Res Inc, Lexington, MA 02421 USA. EM arindam.sam@gmail.com RI Xu, Liang/D-1247-2013; Myneni, Ranga/F-5129-2012 FU NASA Earth Science Enterprise FX This work was supported by the NASA Earth Science Enterprise. NR 57 TC 27 Z9 27 U1 0 U2 27 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 EI 2169-8961 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD FEB 11 PY 2012 VL 117 AR G01015 DI 10.1029/2011JG001818 PG 13 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 891UT UT WOS:000300242800003 ER PT J AU Silver, BJ Raymond, R Sigman, DM Prokopeko, M Lollar, BS Lacrampe-Couloume, G Fogel, ML Pratt, LM Lefticariu, L Onstott, TC AF Silver, Bianca J. Raymond, R. Sigman, Daniel M. Prokopeko, Masha Lollar, Barbara Sherwood Lacrampe-Couloume, Georges Fogel, Marilyn L. Pratt, Lisa M. Lefticariu, Liliana Onstott, T. C. TI The origin of NO3- and N-2 in deep subsurface fracture water of South Africa SO CHEMICAL GEOLOGY LA English DT Article DE N isotopes; Deep; Subsurface microbial ecosystems; Radiolysis; N cycle ID WITWATERSRAND BASIN; ISOTOPIC COMPOSITION; AQUEOUS-SOLUTIONS; STABLE-ISOTOPE; HIGH-PRESSURE; NOBLE-GASES; FRESH-WATER; NITROGEN; NITRATE; GROUNDWATER AB Deep (>0.8 km depth) fracture water with residence time estimates on the order of several Ma from the Witwatersrand Basin, South Africa contains up to 40 mu M of NO3-, up to 50 mM N-2 (90 times air saturation at surface) and 1 to -400 mu M NH3/NH4+ To determine whether the oxidized N species were introduced by mining activity, by recharge of paleometeoric water, or by subsurface geochemical processes, we undertook N and 0 isotopic analyses of N species from fracture water, mining water, pore water, fluid inclusion leachate and whole rock cores. The NO2-, NO3- and NH3/NH4+ concentrations of the pore water and fluid inclusion leachate recovered from the low porosity quartzite, shale and metavolcanic units were similar to 10(4) times that of the fracture water. The delta N-15-NO3- and delta O-18-NO3- of the pore water and fluid inclusion leachate, however, overlapped that of the fracture water with the delta N-15-NO3- ranging from 2 to 7 parts per thousand and the delta N-18-NO3- ranging from 20 to 50 parts per thousand. The delta N-15-NO3- of the mining water ranged from 0 to 16 parts per thousand and its delta N-18-NO3- from 0 to 14 parts per thousand making the mining water NO3- isotopically distinct from that of the fracture, pore and fluid inclusion water. The delta N-15-N-2 of the fracture water and the delta N-15-N from the cores ranged from -5 to 10 parts per thousand and overlapped the delta N-15-NO3-. The delta N-15-NO4+ of the fracture water and pore water NH3/NH4+ ranged from -15 to 4 parts per thousand. Although the NO3- concentrations in the pore water and fluid inclusions were high, mass balance calculations indicate that NO3- accounts for <= 10% of the total rock N, whereas NH3/NH4+ trapped in fluid inclusions or NH4+ present in phyllosilicates account for >= 90% of the total N. Based on these findings, the fluid inclusion NO3- appears to be the source of the pore water and fracture water NO3- rather than paleometeoric recharge or mining contamination. Irradiation experiments indicate that radiolytic oxidation of NH3 to NO3- can explain the fluid inclusion NO3- concentrations and, perhaps, its isotopic composition, but only if the NO3- did not attain isotopic equilibrium with the hydrothermal fluid 2 billion years ago. The delta N-15-N, delta N-15-N-2 and delta N-15-NO4+ suggest that the reduction of N-2 to NH4+ also must have occurred in the Witwatersrand Basin in order to explain the abundance of NH4+ throughout the strata. Although the depleted NH3- concentrations in the fracture water relative to the pore water are consistent with microbial NH3- reduction, further analyses will be required to determine the relative importance of biological processes in the subsurface N cycle and whether a complete subsurface N cycle exists. (C) 2011 Elsevier B.V. All rights reserved. C1 [Silver, Bianca J.; Raymond, R.; Sigman, Daniel M.; Onstott, T. C.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Silver, Bianca J.] ARCADISUS Inc, Cranbury, NJ 08512 USA. [Prokopeko, Masha] Univ So Calif, Dept Earth Sci, Los Angeles, CA 90089 USA. [Lollar, Barbara Sherwood; Lacrampe-Couloume, Georges] Univ Toronto, Dept Geol, Toronto, ON M5S 3B1, Canada. [Fogel, Marilyn L.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20005 USA. [Lefticariu, Liliana] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. [Lefticariu, Liliana] So Illinois Univ, Dept Geol, Carbondale, IL 62901 USA. [Silver, Bianca J.; Raymond, R.; Lollar, Barbara Sherwood; Lacrampe-Couloume, Georges; Fogel, Marilyn L.; Pratt, Lisa M.; Lefticariu, Liliana; Onstott, T. C.] Indiana Univ, IPTAI, NASA Astrobiol Inst, Bloomington, IN USA. RP Onstott, TC (reprint author), Princeton Univ, Dept Geosci, Guyot Hall, Princeton, NJ 08544 USA. EM Bianca.silver@arcadis-us.com; prokopen@usc.edu; bslollar@chem.utoronto.ca; m.fogel@gl.ciw.edu; prattl@indiana.edu; tullis@princeton.edu RI Sigman, Daniel/A-2649-2008; Fogel, Marilyn/M-2395-2015 OI Sigman, Daniel/0000-0002-7923-1973; Fogel, Marilyn/0000-0002-1176-3818 FU NASA Astrobiology Institute [NNA04CC03A]; National Science Foundation [EAR-9978267]; NSERC; Canada Research Chair Funds FX This work was supported by the NASA Astrobiology Institute through award NNA04CC03A to the IPTAI Team co-directed by LMP and TCO, by National Science Foundation LExEn Program grant EAR-9978267 to TCO and by the NSERC Discovery and Accelerator Programs and Canada Research Chair Funds to BSL. We are indebted to Colin Ralston and Walter Seymore of Evander Au Mine (Harmony Gold Mining Co. Ltd.) and Arnand vanHeerden of Kloof Au Mine (Gold Fields Ltd.) for logistical support in acquiring the cores for this study. We also are grateful to the comments from two reviewers which greatly improved the manuscript. NR 77 TC 12 Z9 12 U1 1 U2 37 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2541 J9 CHEM GEOL JI Chem. Geol. PD FEB 10 PY 2012 VL 294 BP 51 EP 62 DI 10.1016/j.chemgeo.2011.11.017 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 944ON UT WOS:000304213800005 ER PT J AU Horesh, A Kulkarni, SR Fox, DB Carpenter, J Kasliwal, MM Ofek, EO Quimby, R Gal-Yam, A Cenko, B de Bruyn, AG Kamble, A Wijers, RAMJ van der Horst, AJ Kouveliotou, C Podsiadlowski, P Sullivan, M Maguire, K Howell, DA Nugent, PE Gehrels, N Law, NM Poznanski, D Shara, M AF Horesh, Assaf Kulkarni, S. R. Fox, Derek B. Carpenter, John Kasliwal, Mansi M. Ofek, Eran O. Quimby, Robert Gal-Yam, Avishay Cenko, Bradley de Bruyn, A. G. Kamble, Atish Wijers, Ralph A. M. J. van der Horst, Alexander J. Kouveliotou, Chryssa Podsiadlowski, Philipp Sullivan, Mark Maguire, Kate Howell, D. Andrew Nugent, Peter E. Gehrels, Neil Law, Nicholas M. Poznanski, Dovi Shara, Michael TI EARLY RADIO AND X-RAY OBSERVATIONS OF THE YOUNGEST NEARBY TYPE Ia SUPERNOVA PTF 11kly (SN 2011fe) SO ASTROPHYSICAL JOURNAL LA English DT Article DE radio continuum: general; supernovae: general; X-rays: general ID SYMBIOTIC-STAR PROGENITOR; WHITE-DWARF MODELS; RS-OPHIUCHI; EMISSION; NOVAE; EXPLOSION; EVOLUTION; BINARIES; CHANNEL; SWIFT AB On 2011 August 24 (UT) the Palomar Transient Factory (PTF) discovered PTF11kly (SN 2011fe), the youngest and most nearby Type Ia supernova (SN Ia) in decades. We followed this event up in the radio (centimeter and millimeter bands) and X-ray bands, starting about a day after the estimated explosion time. We present our analysis of the radio and X-ray observations, yielding the tightest constraints yet placed on the pre-explosion mass-loss rate from the progenitor system of this supernova. We find a robust limit of (M)over dot less than or similar to 10(-8)(w/100 km s (1)) M-circle dot yr(-1) from sensitive X-ray non-detections, as well as a similar limit from radio data, which depends, however, on assumptions about microphysical parameters. We discuss our results in the context of single-degenerate models for SNe Ia and find that our observations modestly disfavor symbiotic progenitor models involving a red giant donor, but cannot constrain systems accreting from main-sequence or sub-giant stars, including the popular supersoft channel. In view of the proximity of PTF11kly and the sensitivity of our prompt observations, we would have to wait for a long time (a decade or longer) in order to more meaningfully probe the circumstellar matter of SNe Ia. C1 [Horesh, Assaf; Kulkarni, S. R.; Carpenter, John; Kasliwal, Mansi M.; Ofek, Eran O.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Fox, Derek B.] Penn State Univ, Eberly Coll Sci, University Pk, PA 16802 USA. [Kasliwal, Mansi M.] Carnegie Inst Sci, Pasadena, CA 91101 USA. [Ofek, Eran O.; Gal-Yam, Avishay] Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Quimby, Robert] Univ Tokyo, IPMU, Kashiwa, Chiba, Japan. [Cenko, Bradley] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [de Bruyn, A. G.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [de Bruyn, A. G.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AA Groningen, Netherlands. [Kamble, Atish; Wijers, Ralph A. M. J.] Univ Wisconsin, Ctr Gravitat & Cosmol, Milwaukee, WI 53211 USA. [van der Horst, Alexander J.] Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA. [Kouveliotou, Chryssa] NASA, Space Sci Off, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Podsiadlowski, Philipp; Sullivan, Mark; Maguire, Kate] Univ Oxford, Dept Phys Astrophys, Oxford OX1 3RH, England. [Howell, D. Andrew] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Howell, D. Andrew] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Law, Nicholas M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Poznanski, Dovi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Shara, Michael] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. RP Horesh, A (reprint author), CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. RI Horesh, Assaf/O-9873-2016; OI Horesh, Assaf/0000-0002-5936-1156; Wijers, Ralph/0000-0002-3101-1808; Sullivan, Mark/0000-0001-9053-4820 FU NSF [AST-0908886, AST-1008353]; NASA [NNH07ZDA001-GLAST]; Israeli Science Foundation; BSF; Hubble Fellowship; Carnegie-Princeton Fellowship; Netherlands Organization for Scientific Research (NWO); Gary & Cynthia Bengier; Richard & Rhoda Goldman Fund; NASA/Swift [NNX10AI21G, GO-7100028]; TABASGO Foundation FX We thank the CARMA and EVLA staff for promptly scheduling this target of opportunity. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We thank the ASTRON Radio Observatory for the generous and swift allocation of observing time. PTF is a fully automated, wide-field survey aimed at a systematic exploration of explosions and variable phenomena in optical wavelengths. The participating institutions are Caltech, Columbia University, Weizmann Institute of Science, Lawrence Berkeley Laboratory, University of Oxford, and University of California at Berkeley. The program is centered on a 12K x 8K, 7.8 square degree CCD array (CFH12K) re-engineered for the 1.2 m Oschin Telescope at the Palomar Observatory by Caltech Optical Observatories. Photometric follow-up is undertaken by the automated Palomar 1.5 m telescope. Research at Caltech is supported by grants from NSF and NASA. The Weizmann PTF partnership is supported in part by the Israeli Science Foundation via grants to A. G. Weizmann-Caltech Collaboration is supported by a grant from the BSF to A. G. and S. R. K. A. G. further acknowledges the Lord Sieff of Brimpton Foundation. M. M. K. acknowledges support from a Hubble Fellowship and Carnegie-Princeton Fellowship. We thank the ASTRON Radio Observatory for the generous and swift allocation of observing time. The Westerbork Synthesis Radio Telescope is operated by ASTRON (Netherlands Foundation for Radio Astronomy) with support from the Netherlands Organization for Scientific Research (NWO). A.J.v.d.H. was supported by NASA grant NNH07ZDA001-GLAST. S. B. C. acknowledges generous financial assistance from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, NASA/Swift grants NNX10AI21G and GO-7100028, the TABASGO Foundation, and NSF grant AST-0908886. A. K. is partially supported by NSF award AST-1008353. NR 54 TC 72 Z9 72 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 AR 21 DI 10.1088/0004-637X/746/1/21 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300021 ER PT J AU Kumar, P Cho, KS Bong, SC Park, SH Kim, YH AF Kumar, Pankaj Cho, K. -S. Bong, S. -C. Park, Sung-Hong Kim, Y. H. TI INITIATION OF CORONAL MASS EJECTION AND ASSOCIATED FLARE CAUSED BY HELICAL KINK INSTABILITY OBSERVED BY SDO/AIA SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: atmosphere; Sun: coronal mass ejections (CMEs); Sun: filaments, prominences; Sun: flares; Sun: magnetic topology; Sun: particle emission ID UNSTABLE FLUX ROPES; MAGNETIC-FIELDS; BALLOONING INSTABILITY; NUMERICAL SIMULATIONS; TORUS INSTABILITY; DRIVEN EVOLUTION; SOLAR CORONA; MODEL; ERUPTION; LOOP AB In this paper, we present multiwavelength observations of helical kink instability as a trigger of a coronal mass ejection (CME) which occurred in active region NOAA 11163 on 2011 February 24. The CME was associated with an M3.5 limb flare. High-resolution observations from the Solar Dynamics Observatory/Atmospheric Imaging Assembly suggest the development of helical kink instability in the erupting prominence, which implies a flux rope structure of the magnetic field. A brightening starts below the apex of the prominence with its slow rising motion (similar to 100 km s (1)) during the activation phase. A bright structure, indicative of a helix with similar to 3-4 turns, was transiently formed at this position. The corresponding twist of similar to 6 pi-8 pi is sufficient to generate the helical kink instability in a flux rope according to recently developed models. A slowly rising blob structure was subsequently formed at the apex of the prominence, and a flaring loop was observed near the footpoints. Within 2 minutes, a second blob was formed in the northern prominence leg. The second blob erupts (like a plasmoid ejection) with the detachment of the northern prominence leg, and flare intensity maximizes. The first blob at the prominence apex shows rotational motion in the counterclockwise direction in the plane of sky, interpreted as the unwinding motion of a helix, and it also erupts to give the CME. RHESSI hard X-ray (HXR) sources show the two footpoint sources and a loop-top source during the flare. We found RHESSI HXR flux, soft X-ray flux derivative, and CME acceleration in the low corona correlate well, which is in agreement with the standard flare model (CSHKP). We also discuss the possible role of ballooning as well as torus instabilities in driving the CME. We conclude that the CME and flare were triggered by the helical kink instability in a flux rope and accelerated mainly by the torus instability. C1 [Kumar, Pankaj; Cho, K. -S.; Bong, S. -C.; Park, Sung-Hong; Kim, Y. H.] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea. [Cho, K. -S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cho, K. -S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Kumar, P (reprint author), Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea. EM pankaj@kasi.re.kr RI Park, Sung-Hong/K-1578-2014 OI Park, Sung-Hong/0000-0001-9149-6547 NR 68 TC 36 Z9 36 U1 2 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 AR 67 DI 10.1088/0004-637X/746/1/67 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300067 ER PT J AU Metzger, BD Berger, E AF Metzger, B. D. Berger, E. TI WHAT IS THE MOST PROMISING ELECTROMAGNETIC COUNTERPART OF A NEUTRON STAR BINARY MERGER? SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; gravitational waves; stars: neutron; surveys ID GAMMA-RAY BURSTS; COMPACT OBJECT MERGERS; GRAVITATIONAL-WAVE OBSERVATIONS; EXTENDED EMISSION; HOST GALAXY; R-PROCESS; OPTICAL AFTERGLOW; STANDARD SIRENS; LIGHT CURVES; SCIENCE RUN AB The final inspiral of double neutron star and neutron-star-black-hole binaries are likely to be detected by advanced networks of ground-based gravitational wave (GW) interferometers. Maximizing the science returns from such a discovery will require the identification of an electromagnetic counterpart. Here we critically evaluate and compare several possible counterparts, including short-duration gamma-ray bursts (SGRBs), "orphan" optical and radio afterglows, and day-long optical transients powered by the radioactive decay of heavy nuclei synthesized in the merger ejecta ("kilonovae"). We assess the promise of each counterpart in terms of four "Cardinal Virtues": detectability, high fraction, identifiability, and positional accuracy. Taking into account the search strategy for typical error regions of tens of square degrees, we conclude that SGRBs are the most useful to confirm the cosmic origin of a few GW events, and to test the association with neutron star mergers. However, for the more ambitious goal of localizing and obtaining redshifts for a large sample of GW events, kilonovae are instead preferred. Off-axis optical afterglows are detectable for at most tens of percent of events, while radio afterglows are promising only for energetic relativistic ejecta in a high-density medium. Our main recommendations are: (1) an all-sky gamma-ray satellite is essential for temporal coincidence detections, and for GW searches of gamma-ray-triggered events; (2) the Large Synoptic Survey Telescope should adopt a one-day cadence follow-up strategy, ideally with 0.5 hr per pointing to cover GW error regions; and (3) radio searches should focus on the relativistic case, which requires observations for a few months. C1 [Metzger, B. D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Metzger, BD (reprint author), NASA, Washington, DC 20546 USA. FU NASA [PF9-00065, NAS8-03060]; Chandra Xray Center; National Science Foundation [AST-1107973] FX We thank Hendrik van Eerten and Andrew MacFadyen for producing and maintaining their online library of afterglow light curves. We thank Ehud Nakar for providing theoretical light curves of supernova shock breakout. We thank S. Nissanke and R. O'Shaughnessy for helpful discussions and information. B. D. M. is supported by NASA through Einstein Postdoctoral Fellowship grant No. PF9-00065 awarded by the Chandra Xray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. E. B. acknowledges support for this work from the National Science Foundation through grant AST-1107973. NR 118 TC 211 Z9 212 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 DI 10.1088/0004-637X/746/1/48 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300048 ER PT J AU Millea, M Dore, O Dudley, J Holder, G Knox, L Shaw, L Song, YS Zahn, O AF Millea, M. Dore, O. Dudley, J. Holder, G. Knox, L. Shaw, L. Song, Y-S. Zahn, O. TI MODELING EXTRAGALACTIC FOREGROUNDS AND SECONDARIES FOR UNBIASED ESTIMATION OF COSMOLOGICAL PARAMETERS FROM PRIMARY COSMIC MICROWAVE BACKGROUND ANISOTROPY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; cosmology: observations; cosmology: theory; distance scale; large-scale structure of universe ID ZELDOVICH POWER SPECTRUM; SOUTH-POLE TELESCOPE; STAR-FORMING GALAXIES; HIGH-FREQUENCY; PATCHY REIONIZATION; POLARIZATION; CMB; SIMULATIONS; CLUSTERS; IMPACT AB Using the latest physical modeling and constrained by the most recent data, we develop a phenomenological parameterized model of the contributions to intensity and polarization maps at millimeter wavelengths from external galaxies and Sunyaev-Zeldovich effects. We find such modeling to be necessary for estimation of cosmological parameters from Planck data. For example, ignoring the clustering of the infrared background would result in a bias in ns of 7s in the context of an eight-parameter cosmological model. We show that the simultaneous marginalization over a full foreground model can eliminate such biases, while increasing the statistical uncertainty in cosmological parameters by less than 20%. The small increases in uncertainty can be significantly reduced with the inclusion of higher-resolution ground-based data. The multi-frequency analysis we employ involves modeling 46 total power spectra and marginalization over 17 foreground parameters. We show that we can also reduce the data to a best estimate of the cosmic microwave background power spectra, with just two principal components (with constrained amplitudes) describing residual foreground contamination. C1 [Millea, M.; Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Dore, O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dore, O.] CALTECH, Pasadena, CA 91125 USA. [Dudley, J.; Holder, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Song, Y-S.] Korea Inst Adv Study, Seoul 130722, South Korea. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA. RP Millea, M (reprint author), Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. FU National Aeronautics and Space Administration; Yale University; NSF [AST-1009811, 0709498] FX We benefited from conversations with A. Challinor, J. Dunkley, G. Efstathiout, F. Finelli, S. Gratton, W. Holzapfel, C. Reichardt, D. Scott, G. Ziemann, and G. de Zotti. 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. L. S. acknowledges the support of Yale University and NSF grant AST-1009811. L. K. and M. M. acknowledge support from NSF grant 0709498. NR 77 TC 16 Z9 16 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 AR 4 DI 10.1088/0004-637X/746/1/4 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300004 ER PT J AU Suzuki, N Rubin, D Lidman, C Aldering, G Amanullah, R Barbary, K Barrientos, LF Botyanszki, J Brodwin, M Connolly, N Dawson, KS Dey, A Doi, M Donahue, M Deustua, S Eisenhardt, P Ellingson, E Faccioli, L Fadeyev, V Fakhouri, HK Fruchter, AS Gilbank, DG Gladders, MD Goldhaber, G Gonzalez, AH Goobar, A Gude, A Hattori, T Hoekstra, H Hsiao, E Huang, X Ihara, Y Jee, MJ Johnston, D Kashikawa, N Koester, B Konishi, K Kowalski, M Linder, EV Lubin, L Melbourne, J Meyers, J Morokuma, T Munshi, F Mullis, C Oda, T Panagia, N Perlmutter, S Postman, M Pritchard, T Rhodes, J Ripoche, P Rosati, P Schlegel, DJ Spadafora, A Stanford, SA Stanishev, V Stern, D Strovink, M Takanashi, N Tokita, K Wagner, M Wang, L Yasuda, N Yee, HKC AF Suzuki, N. Rubin, D. Lidman, C. Aldering, G. Amanullah, R. Barbary, K. Barrientos, L. F. Botyanszki, J. Brodwin, M. Connolly, N. Dawson, K. S. Dey, A. Doi, M. Donahue, M. Deustua, S. Eisenhardt, P. Ellingson, E. Faccioli, L. Fadeyev, V. Fakhouri, H. K. Fruchter, A. S. Gilbank, D. G. Gladders, M. D. Goldhaber, G. Gonzalez, A. H. Goobar, A. Gude, A. Hattori, T. Hoekstra, H. Hsiao, E. Huang, X. Ihara, Y. Jee, M. J. Johnston, D. Kashikawa, N. Koester, B. Konishi, K. Kowalski, M. Linder, E. V. Lubin, L. Melbourne, J. Meyers, J. Morokuma, T. Munshi, F. Mullis, C. Oda, T. Panagia, N. Perlmutter, S. Postman, M. Pritchard, T. Rhodes, J. Ripoche, P. Rosati, P. Schlegel, D. J. Spadafora, A. Stanford, S. A. Stanishev, V. Stern, D. Strovink, M. Takanashi, N. Tokita, K. Wagner, M. Wang, L. Yasuda, N. Yee, H. K. C. CA Supernova Cosmology Project TI THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. V. IMPROVING THE DARK- ENERGY CONSTRAINTS ABOVE z > 1 AND BUILDING AN EARLY-TYPE-HOSTED SUPERNOVA SAMPLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; distance scale; supernovae: general ID DIGITAL SKY SURVEY; COLOR-MAGNITUDE RELATION; HIGH-REDSHIFT SUPERNOVAE; PROBE WMAP OBSERVATIONS; LASER ADAPTIVE OPTICS; IA LIGHT CURVES; ADVANCED CAMERA; GALAXY CLUSTERS; LEGACY SURVEY; COSMOLOGICAL CONSTRAINTS AB We present Advanced Camera for Surveys, NICMOS, and Keck adaptive-optics-assisted photometry of 20 Type Ia supernovae (SNe Ia) from the Hubble Space Telescope (HST) Cluster Supernova Survey. The SNe Ia were discovered over the redshift interval 0.623 < z < 1.415. Of these SNe Ia, 14 pass our strict selection cuts and are used in combination with the world's sample of SNe Ia to derive the best current constraints on dark energy. Of our new SNe Ia, 10 are beyond redshift z = 1, thereby nearly doubling the statistical weight of HST-discovered SNe Ia beyond this redshift. Our detailed analysis corrects for the recently identified correlation between SN Ia luminosity and host galaxy mass and corrects the NICMOS zero point at the count rates appropriate for very distant SNe Ia. Adding these SNe improves the best combined constraint on dark-energy density,rho(DE)(z), at redshifts 1.0 < z < 1.6 by 18% (including systematic errors). For a flat. CDM universe, we find Omega(A) = 0.729 +/- 0.014 (68% confidence level (CL) including systematic errors). For a flat wCDM model, we measure a constant dark-energy equation-of-state parameter w = -1.013(-0.073)(+0.068) (68% CL). Curvature is constrained to similar to 0.7% in the owCDM model and to similar to 2% in a model in which dark energy is allowed to vary with parameters w(0) and w(a). Further tightening the constraints on the time evolution of dark energy will require several improvements, including high-quality multi-passband photometry of a sample of several dozenz > 1 SNe Ia. We describe how such a sample could be efficiently obtained by targeting cluster fields with WFC3 on board HST. The updated supernova Union2.1 compilation of 580 SNe is available at http://supernova.lbl.gov/Union. C1 [Suzuki, N.; Rubin, D.; Aldering, G.; Barbary, K.; Faccioli, L.; Fakhouri, H. K.; Goldhaber, G.; Hsiao, E.; Huang, X.; Linder, E. V.; Meyers, J.; Perlmutter, S.; Ripoche, P.; Schlegel, D. J.; Spadafora, A.; Strovink, M.] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Suzuki, N.; Rubin, D.; Amanullah, R.; Barbary, K.; Botyanszki, J.; Faccioli, L.; Fakhouri, H. K.; Goldhaber, G.; Gude, A.; Hsiao, E.; Huang, X.; Linder, E. V.; Meyers, J.; Munshi, F.; Perlmutter, S.; Pritchard, T.; Ripoche, P.; Strovink, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Lidman, C.] Australian Astron Observ, Epping, NSW 1710, Australia. [Amanullah, R.; Goobar, A.] AlbaNova, Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden. [Barrientos, L. F.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile. [Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Connolly, N.] Hamilton Coll, Dept Phys, Clinton, NY 13323 USA. [Dawson, K. S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Dey, A.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Doi, M.; Ihara, Y.; Morokuma, T.; Tokita, K.] Univ Tokyo, Grad Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Donahue, M.; Johnston, D.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Deustua, S.; Fruchter, A. S.; Panagia, N.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Eisenhardt, P.; Rhodes, J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ellingson, E.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Fadeyev, V.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 94064 USA. [Gilbank, D. G.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Gladders, M. D.; Koester, B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Goobar, A.; Stanishev, V.] Stockholm Univ, Albanova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden. [Gude, A.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Hattori, T.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Hoekstra, H.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Jee, M. J.; Lubin, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Johnston, D.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Kashikawa, N.; Morokuma, T.; Takanashi, N.] Natl Astron Observ Japan, Tokyo 1818588, Japan. [Koester, B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Konishi, K.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Kowalski, M.] Univ Bonn, Inst Phys, Bonn, Germany. [Melbourne, J.; Rhodes, J.] CALTECH, Div Phys Math & Astron, Caltech Opt Observ, Pasadena, CA 91125 USA. [Munshi, F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Mullis, C.] Wachovia Corp, Winston Salem, NC 27101 USA. [Oda, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Pritchard, T.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Rosati, P.] ESO, D-85748 Garching, Germany. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Stanishev, V.] Inst Super Tecn, CENTRA Ctr Multidisciplinar Astrofis, P-1049001 Lisbon, Portugal. [Wagner, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Wang, L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Yasuda, N.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan. [Yee, H. K. C.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Suzuki, N (reprint author), EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. EM nsuzuki@lbl.gov; rubind@berkeley.edu; clidman@aao.gov.au RI Kowalski, Marek/G-5546-2012; Yasuda, Naoki/A-4355-2011; Stanishev, Vallery/M-8930-2013; Perlmutter, Saul/I-3505-2015; OI Stanishev, Vallery/0000-0002-7626-1181; Perlmutter, Saul/0000-0002-4436-4661; Strovink, Mark/0000-0001-7020-7769; Meyers, Joshua/0000-0002-2308-4230; Hoekstra, Henk/0000-0002-0641-3231 FU NASA from the Space Telescope Science Institute [GO-10496]; AURA, Inc., under NASA [NAS 5-26555]; Director, Office of Science, Office of High Energy and Nuclear Physics, of the U.S. Department of Energy [AC02-05CH11231]; JSPS [20040003]; U.S. Department of Energy by Lawrence Livermore National Laboratory [W-7405-Eng-48, DE-AC52-07NA27344]; Japan Society for the Promotion of Science; Netherlands Organization for Scientific Research (WO); Marie Curie International Reintegration Grant FX Financial support for this work was provided by NASA through program GO-10496 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. This work was also supported in part by the Director, Office of Science, Office of High Energy and Nuclear Physics, of the U.S. Department of Energy under contract No. AC02-05CH11231, as well as a JSPS core-to-core program "International Research Network for Dark Energy" and by JSPS research grant 20040003. Support for M.B. was provided by the W. M. Keck Foundation. The work of S.A.S. was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory in part under Contract W-7405-Eng-48 and in part under contract DE-AC52-07NA27344. The work of P.E., J.R., and D.S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. T.M. and Y.I. have been financially supported by the Japan Society for the Promotion of Science through its Research Fellowship. H.H. acknowledges support from a VIDI grant from the Netherlands Organization for Scientific Research (WO) and a Marie Curie International Reintegration Grant. N.S., C.L., and S.P. wish to thank the support and hospitality of the Aspen Center for Physics, where much of this paper was written. We thank Jay Anderson, L. E. Bergeron, Ralph Bohlin, Roelof de Jong, Anton Koekemoer, Jennifer Mack, Bahram Mobasher, Adam Riess, Kenneth Sembach, and ACS and NICMOS teams at the Space Telescope Science Institute for their advice on the HST data calibration. We also thank Alex Conley for calibration discussions. Finally, we thank our referee, who carefully read our paper and gave valuable feedback. NR 117 TC 673 Z9 678 U1 1 U2 38 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 AR 85 DI 10.1088/0004-637X/746/1/85 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300085 ER PT J AU Teodoro, M Damineli, A Arias, JI de Araujo, FX Barba, RH Corcoran, MF Fernandes, MB Fernandez-Lajus, E Fraga, L Gamen, RC Gonzalez, JF Groh, JH Marshall, JL McGregor, PJ Morrell, N Nicholls, DC Parkin, ER Pereira, CB Phillips, MM Solivella, GR Steiner, JE Stritzinger, M Thompson, I Torres, CAO Torres, MAP Herencia, MIZ AF Teodoro, M. Damineli, A. Arias, J. I. de Araujo, F. X. Barba, R. H. Corcoran, M. F. Borges Fernandes, M. Fernandez-Lajus, E. Fraga, L. Gamen, R. C. Gonzalez, J. F. Groh, J. H. Marshall, J. L. McGregor, P. J. Morrell, N. Nicholls, D. C. Parkin, E. R. Pereira, C. B. Phillips, M. M. Solivella, G. R. Steiner, J. E. Stritzinger, M. Thompson, I. Torres, C. A. O. Torres, M. A. P. Zevallos Herencia, M. I. TI He II lambda 4686 IN eta CARINAE: COLLAPSE OF THE WIND-WIND COLLISION REGION DURING PERIASTRON PASSAGE SO ASTROPHYSICAL JOURNAL LA English DT Article DE line: profiles; stars: early-type; stars: individual (eta Carinae); stars: massive ID BINARY V444 CYGNI; X-RAY MINIMUM; COLLIDING-WINDS; SPECTROSCOPIC EVENT; EMISSION-LINES; HD 5980; RADIO-EMISSION; THETA-CARINAE; LIGHT-CURVE; SYSTEM AB The periodic spectroscopic events in eta Carinae are now well established and occur near the periastron passage of two massive stars in a very eccentric orbit. Several mechanisms have been proposed to explain the variations of different spectral features, such as an eclipse by the wind-wind collision (WWC) boundary, a shell ejection from the primary star or accretion of its wind onto the secondary. All of them have problems explaining all the observed phenomena. To better understand the nature of the cyclic events, we performed a dense monitoring of eta Carinae with five Southern telescopes during the 2009 low-excitation event, resulting in a set of data of unprecedented quality and sampling. The intrinsic luminosity of the He II lambda 4686 emission line (L similar to 310 L-circle dot) just before periastron reveals the presence of a very luminous transient source of extreme UV radiation emitted in the WWC region. Clumps in the primary's wind probably explain the flare-like behavior of both the X-ray and He II lambda 4686 light curves. After a short-lived minimum, He II lambda 4686 emission rises again to a new maximum, when X-rays are still absent or very weak. We interpret this as a collapse of the WWC onto the "surface" of the secondary star, switching off the hard X-ray source and diminishing the WWC shock cone. The recovery from this state is controlled by the momentum balance between the secondary's wind and the clumps in the primary's wind. C1 [Teodoro, M.; Damineli, A.; Steiner, J. E.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508900 Sao Paulo, Brazil. [Arias, J. I.] Univ La Serena, Dept Fis, La Serena, Chile. [de Araujo, F. X.; Borges Fernandes, M.; Pereira, C. B.; Zevallos Herencia, M. I.] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil. [Barba, R. H.; Gonzalez, J. F.] Consejo Nacl Invest Cient & Tecn, ICATE, San Juan, Argentina. [Corcoran, M. F.] CRESST, Greenbelt, MD 20771 USA. [Corcoran, M. F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Fernandez-Lajus, E.; Gamen, R. C.; Solivella, G. R.] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, La Plata, BA, Argentina. [Fraga, L.] So Observ Astrophys Res, La Serena, Chile. [Groh, J. H.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [McGregor, P. J.; Nicholls, D. C.; Parkin, E. R.] RSAA, Mt Stromlo Observ, Weston, ACT 2611, Australia. [Morrell, N.; Phillips, M. M.] Observ Carnegie Inst Washington, Las Campanas Observ, La Serena, Chile. [Stritzinger, M.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Thompson, I.] Observ Carnegie Inst, Pasadena, CA 91101 USA. [Torres, C. A. O.] Lab Nacl Astrofis, BR-37504364 Bairro Das Nacoes, Itajuba, Brazil. [Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Teodoro, M (reprint author), Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Rua Matao 1226,Cidade Univ, BR-05508900 Sao Paulo, Brazil. EM mairan@astro.iag.usp.br RI Borges Fernandes, Marcelo/K-6210-2016; Pereira, Claudio/L-3199-2016; Damineli, Augusto/D-8210-2012; 7, INCT/H-6207-2013; Teodoro, Mairan/H-9123-2013; Astrofisica, Inct/H-9455-2013; Damineli, Augusto/P-8829-2016; Barba, Rodolfo/P-4649-2014; Gamen, Roberto/A-1728-2015 OI Damineli, Augusto/0000-0002-7978-2994; Damineli, Augusto/0000-0002-7978-2994; Barba, Rodolfo/0000-0003-1086-1579; FU FAPESP [05/00190-8, 09/08013-9]; CNPq; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq-Brazil); NASA; Chandra [G07-8022A, G08-9018A, G09-0016A, GO0-11039A]; RXTE Guest Observer facility at NASA/GSFC FX We thank the referee for questions and suggestions that led to a clarification of the ideas discussed in this paper. M. T., A. D., and J.E.S. are grateful to the Brazilian agencies FAPESP and CNPq for continuous financial support. M. T. is supported through grants FAPESP 05/00190-8 and 09/08013-9. M. B. F. acknowledges Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq-Brazil) for the post-doctoral grant. M. F. C. gratefully acknowledges support from NASA and Chandra via grants G07-8022A, G08-9018A, G09-0016A, and GO0-11039A, along with continued aid from the RXTE Guest Observer facility at NASA/GSFC. Calculations were performed with version 07.02 of Cloudy, last described by Ferland et al. (1998). This research has made use of NASA's Astrophysics Data System. In addition, 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. NR 86 TC 18 Z9 18 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 AR 73 DI 10.1088/0004-637X/746/1/73 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300073 ER PT J AU Tessenyi, M Ollivier, M Tinetti, G Beaulieu, JP du Foresto, VC Encrenaz, T Micela, G Swinyard, B Ribas, I Aylward, A Tennyson, J Swain, MR Sozzetti, A Vasisht, G Deroo, P AF Tessenyi, M. Ollivier, M. Tinetti, G. Beaulieu, J. P. du Foresto, V. Coude Encrenaz, T. Micela, G. Swinyard, B. Ribas, I. Aylward, A. Tennyson, J. Swain, M. R. Sozzetti, A. Vasisht, G. Deroo, P. TI CHARACTERIZING THE ATMOSPHERES OF TRANSITING PLANETS WITH A DEDICATED SPACE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: planetary systems; planets and satellites: atmospheres; stars: late-type; stars: low-mass ID EXOPLANET HD 209458B; UPSILON ANDROMEDAE B; HOT NEPTUNE GJ436B; LOW-MASS STARS; EXTRASOLAR PLANET; TRANSMISSION SPECTRUM; MU-M; ECCENTRIC EXOPLANETS; EMISSION-SPECTRUM; DAYSIDE SPECTRUM AB Exoplanetary science is one of the fastest evolving fields of today's astronomical research, continuously yielding unexpected and surprising results. Ground-based planet-hunting surveys, together with dedicated space missions such as Kepler and CoRoT, are delivering an ever-increasing number of exoplanets, over 690, and ESA's Gaia mission will escalate the exoplanetary census into the several thousands. The next logical step is the characterization of these new worlds. What is their nature? Why are they as they are? Use of the Hubble Space Telescope and Spitzer Space Telescope to probe the atmospheres of transiting hot, gaseous exoplanets has opened perspectives unimaginable even just 10 years ago, demonstrating that it is indeed possible with current technology to address the ambitious goal of characterizing the atmospheres of these alien worlds. However, these successful measurements have also shown the difficulty of understanding the physics and chemistry of these exotic environments when having to rely on a limited number of observations performed on a handful of objects. To progress substantially in this field, a dedicated facility for exoplanet characterization, able to observe a statistically significant number of planets over time and a broad spectral range will be essential. Additionally, the instrument design ( e. g., detector performances, photometric stability) will be tailored to optimize the extraction of the astrophysical signal. In this paper, we analyze the performance and tradeoffs of a 1.2/1.4 m space telescope for exoplanet transit spectroscopy from the visible to the mid-IR. We present the signal-to-noise ratio as a function of integration time and stellar magnitude/spectral type for the acquisition of spectra of planetary atmospheres for a variety of scenarios: hot, warm, and temperate planets orbiting stars ranging in spectral type from hot F-to cooler M-dwarfs. Our results include key examples of known planets (e. g., HD 189733b, GJ 436b, GJ 1214b, and Cancri 55 e) and simulations of plausible terrestrial and gaseous planets, with a variety of thermodynamical conditions. We conclude that even most challenging targets, such as super-Earths in the habitable zone of late-type stars, are within reach of an M-class, space-based spectroscopy mission. C1 [Tessenyi, M.; Tinetti, G.; Swinyard, B.; Aylward, A.; Tennyson, J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Tessenyi, M.; Beaulieu, J. P.] Univ Paris 06, Inst Astrophys Spatiale, CNRS, UMR7095, Paris, France. [Ollivier, M.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Ollivier, M.] CNRS, UMR 8617, IAS, UMR8617, F-91405 Orsay, France. [du Foresto, V. Coude; Encrenaz, T.] LESIA, Observ Paris, Meudon, France. [Micela, G.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Swinyard, B.] STFC Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Ribas, I.] CSIC IEEC, Inst Ciencies Espai, Bellaterra 08193, Spain. [Swain, M. R.; Vasisht, G.; Deroo, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sozzetti, A.] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, TO, Italy. RP Tessenyi, M (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. RI Tennyson, Jonathan/I-2222-2012; Ribas, Ignasi/M-2134-2014; OI Tennyson, Jonathan/0000-0002-4994-5238; Ribas, Ignasi/0000-0002-6689-0312; Micela, Giuseppina/0000-0002-9900-4751; Sozzetti, Alessandro/0000-0002-7504-365X; Tinetti, Giovanna/0000-0001-6058-6654 NR 71 TC 24 Z9 24 U1 1 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 FEB 10 PY 2012 VL 746 IS 1 AR 45 DI 10.1088/0004-637X/746/1/45 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300045 ER PT J AU Todorov, KO Deming, D Knutson, HA Burrows, A Sada, PV Cowan, NB Agol, E Desert, JM Fortney, JJ Charbonneau, D Laughlin, G Langton, J Showman, AP Lewis, NK AF Todorov, Kamen O. Deming, Drake Knutson, Heather A. Burrows, Adam Sada, Pedro V. Cowan, Nicolas B. Agol, Eric Desert, Jean-Michel Fortney, Jonathan J. Charbonneau, David Laughlin, Gregory Langton, Jonathan Showman, Adam P. Lewis, Nikole K. TI WARM SPITZER OBSERVATIONS OF THREE HOT EXOPLANETS: XO-4b, HAT-P-6b, AND HAT-P-8b SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; techniques: photometric ID INFRARED-EMISSION SPECTRUM; SECONDARY ECLIPSE PHOTOMETRY; EXTRASOLAR PLANET; THERMAL EMISSION; TEMPERATURE INVERSION; HD 189733B; TRANSITING PLANET; GIANT PLANETS; LIGHT CURVES; F-STAR AB We analyze Warm Spitzer/Infrared Array Camera observations of the secondary eclipses of three planets, XO-4b, HAT-P-6b, and HAT-P-8b. We measure secondary eclipse amplitudes at 3.6 mu m and 4.5 mu m for each target. XO-4b exhibits a stronger eclipse depth at 4.5 mu m than at 3.6 mu m, which is consistent with the presence of a temperature inversion. HAT-P-8b shows a stronger eclipse amplitude at 3.6 mu m and is best described by models without a temperature inversion. The eclipse depths of HAT-P-6b can be fitted with models with a small or no temperature inversion. We consider our results in the context of a postulated relationship between stellar activity and temperature inversion and a relationship between irradiation level and planet dayside temperature, as discussed by Knutson et al. and Cowan & Agol, respectively. Our results are consistent with these hypotheses, but do not significantly strengthen them. To measure accurate secondary eclipse central phases, we require accurate ephemerides. We obtain primary transit observations and supplement them with publicly available observations to update the orbital ephemerides of the three planets. Based on the secondary eclipse timing, we set upper boundaries for e cos(omega) for HAT-P-6b, HAT-P-8b, and XO-4b and find that the values are consistent with circular orbits. C1 [Todorov, Kamen O.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Deming, Drake] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Knutson, Heather A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Sada, Pedro V.] Univ Monterrey, Dept Math & Phys, Monterrey, Mexico. [Cowan, Nicolas B.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Desert, Jean-Michel; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fortney, Jonathan J.; Laughlin, Gregory] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 USA. [Showman, Adam P.; Lewis, Nikole K.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Todorov, Kamen O.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. RP Todorov, KO (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. RI Agol, Eric/B-8775-2013; OI Agol, Eric/0000-0002-0802-9145; Fortney, Jonathan/0000-0002-9843-4354; Todorov, Kamen/0000-0002-9276-8118; Charbonneau, David/0000-0002-9003-484X FU NASA through JPL/Caltech; NASA; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium 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 through an award issued by JPL/Caltech. 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. We thank the anonymous referee for a careful review of this paper. NR 51 TC 29 Z9 30 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 AR 111 DI 10.1088/0004-637X/746/1/111 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300111 ER PT J AU Su, Y Dennis, BR Holman, GD Wang, TJ Chamberlin, PC Savage, S Veronig, A AF Su, Yang Dennis, Brian R. Holman, Gordon D. Wang, Tongjiang Chamberlin, Phillip C. Savage, Sabrina Veronig, Astrid TI OBSERVATIONS OF A TWO-STAGE SOLAR ERUPTIVE EVENT (SEE): EVIDENCE FOR SECONDARY HEATING SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: coronal mass ejections (CMEs); Sun: flares; Sun: UV radiation; Sun: X-rays, gamma rays ID FLARES; ARCADE AB We present RHESSI, SDO/AIA, SOHO/LASCO, STEREO, and GOES observations of a partially occulted solar eruptive event that occurred at the southwest limb on 2011 March 8. The GOES X-ray light curve shows two peaks separated by almost 2 hr that we interpret as two stages of a single event associated with the delayed eruption of a coronal mass ejection (CME). A hot flux rope formed during the first stage and continued expanding and rising throughout the event. The speed of the flux rope decreased from similar to 120 to 14 km s(-1) during the decay phase of the first stage and increased again during the second stage to become the CME with a speed of similar to 516 km s(-1). RHESSI and GOES data analyses show that the plasma temperature reached over 20 MK in the first stage, then decreased to similar to 10 MK and increased to 15 MK in the second stage. This event provides clear evidence for a secondary heating phase. The enhanced EUV and X-ray emission came from the high corona (similar to 60 arcsec above the limb) in the second stage, similar to 40 arcsec higher than the site of the initial flare emission. STEREO-A on-disk observations indicate that the post-flare loops during this stage were of larger scale sizes and spatially distinct from those in the first stage. C1 [Su, Yang; Dennis, Brian R.; Holman, Gordon D.; Wang, Tongjiang; Chamberlin, Phillip C.; Savage, Sabrina] NASA, Goddard Space Flight Ctr, Solar Phys Lab Code 671, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Su, Yang; Wang, Tongjiang] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Su, Yang; Veronig, Astrid] Graz Univ, Inst Phys, A-8010 Graz, Austria. RP Su, Y (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab Code 671, Heliophys Sci Div, Greenbelt, MD 20771 USA. EM yang.su@uni-graz.at RI Dennis, Brian/C-9511-2012; Chamberlin, Phillip/C-9531-2012; Holman, Gordon/C-9548-2012; Veronig, Astrid/B-8422-2009; Su, Yang/J-5381-2014 OI Chamberlin, Phillip/0000-0003-4372-7405; FU NASA at The Catholic University of America [NNG06GB96A]; European Community [263086]; NASA [NNX08AE44G, NNX10AN10G] FX We thank the referee for providing valuable comments and help in improving this paper. We acknowledge the critical support provided by Kim Tolbert and Richard Schwartz and their help with the IDL RHESSI data analysis software and the SSW procedures. We are grateful to Frederick C. Bruhweiler for managing the NASA Grant NNG06GB96A at The Catholic University of America, through which one of us (Y.S.) was funded. This work is also supported in part by the European Community Framework Programme 7, "High Energy Solar PhysicsData in Europe (HESPE)," grant agreement No. 263086. The work of T.W. was supported by NASA grants NNX08AE44G and NNX10AN10G. NR 12 TC 13 Z9 13 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 10 PY 2012 VL 746 IS 1 AR L5 DI 10.1088/2041-8205/746/1/L5 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892ZD UT WOS:000300323500005 ER PT J AU Wessels, V Gangopadhyay, AK Sahu, KK Hyers, RW Canepari, SM Rogers, JR Kramer, MJ Goldman, AI Robinson, D Lee, JW Morris, JR Kelton, KF AF Wessels, V. Gangopadhyay, A. K. Sahu, K. K. Hyers, R. W. Canepari, S. M. Rogers, J. R. Kramer, M. J. Goldman, A. I. Robinson, D. Lee, J. W. Morris, J. R. Kelton, K. F. TI Reply to "Comment on 'Rapid chemical and topological ordering in supercooled liquid Cu46Zr54'" SO PHYSICAL REVIEW B LA English DT Editorial Material ID BULK METALLIC-GLASS; HEMISPHERICAL TOTAL EMISSIVITY; CU-ZR ALLOYS; THERMOPHYSICAL PROPERTIES; UNDERCOOLED LIQUID; FORMING LIQUID; NONCONTACT MEASUREMENTS; HIGH-TEMPERATURES; THERMODYNAMICS; KINETICS AB The criticisms of Harvey and Gheribi (HG) are directed towards supporting evidence for ordering in supercooled Cu46Zr54 liquid from specific heat measurements and molecular dynamics simulations, not on the direct evidence that came from x-ray diffraction studies. In this reply, we demonstrate that the unique features observed in the specific heat [Cp(T)] are not artifacts of any specific assumptions, as suggested by HG. We have furnished additional details of the MD simulations and clarified related issues raised by HG. The basic conclusions, however, remain unchanged. C1 [Wessels, V.; Gangopadhyay, A. K.; Sahu, K. K.; Kelton, K. F.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Hyers, R. W.; Canepari, S. M.] Univ Massachusetts, Dept Mech Engn, Amherst, MA 01003 USA. [Rogers, J. R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Kramer, M. J.; Goldman, A. I.; Robinson, D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kramer, M. J.; Goldman, A. I.; Robinson, D.] US DOE, Ames Lab, Ames, IA 50011 USA. [Robinson, D.] Argonne Natl Lab, Argonne, IL 60439 USA. [Sahu, K. K.] Swiss Fed Inst Technol, Dept Mat, CH-8046 Zurich, Switzerland. [Lee, J. W.; Morris, J. R.] Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA. RP Wessels, V (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA. RI Morris, J/I-4452-2012 OI Morris, J/0000-0002-8464-9047 NR 38 TC 2 Z9 2 U1 1 U2 14 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD FEB 10 PY 2012 VL 85 IS 6 AR 066102 DI 10.1103/PhysRevB.85.066102 PG 5 WC Physics, Condensed Matter SC Physics GA 889QB UT WOS:000300087200005 ER PT J AU Oskin, ME Arrowsmith, JR Corona, AH Elliott, AJ Fletcher, JM Fielding, EJ Gold, PO Garcia, JJG Hudnut, KW Liu-Zeng, J Teran, OJ AF Oskin, Michael E. Arrowsmith, J. Ramon Hinojosa Corona, Alejandro Elliott, Austin J. Fletcher, John M. Fielding, Eric J. Gold, Peter O. Gonzalez Garcia, J. Javier Hudnut, Ken W. Liu-Zeng, Jing Teran, Orlando J. TI Near-Field Deformation from the El Mayor-Cucapah Earthquake Revealed by Differential LIDAR SO SCIENCE LA English DT Article ID 1999 HECTOR MINE; SURFACE RUPTURE; SLIP DISTRIBUTION; BAJA-CALIFORNIA; LAGUNA-SALADA; FAULT; MEXICO; IRAN; CHINA; ZONE AB Large [moment magnitude (M-w) >= 7] continental earthquakes often generate complex, multifault ruptures linked by enigmatic zones of distributed deformation. Here, we report the collection and results of a high-resolution (>= nine returns per square meter) airborne light detection and ranging (LIDAR) topographic survey of the 2010 M-w 7.2 El Mayor-Cucapah earthquake that produced a 120-kilometer-long multifault rupture through northernmost Baja California, Mexico. This differential LIDAR survey completely captures an earthquake surface rupture in a sparsely vegetated region with pre-earthquake lower-resolution (5-meter-pixel) LIDAR data. The postevent survey reveals numerous surface ruptures, including previously undocumented blind faults within thick sediments of the Colorado River delta. Differential elevation changes show distributed, kilometer-scale bending strains as large as similar to 10(3) microstrains in response to slip along discontinuous faults cutting crystalline bedrock of the Sierra Cucapah. C1 [Oskin, Michael E.; Elliott, Austin J.; Gold, Peter O.] Univ Calif Davis, Dept Geol, Davis, CA 95618 USA. [Arrowsmith, J. Ramon] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Hinojosa Corona, Alejandro; Fletcher, John M.; Gonzalez Garcia, J. Javier; Teran, Orlando J.] Ctr Invest Cient & Educ Super Ensenada, Ensenada 22860, Baja California, Mexico. [Fielding, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hudnut, Ken W.] US Geol Survey, Pasadena, CA 91106 USA. [Liu-Zeng, Jing] China Earthquake Adm, Inst Geol, Natl Key Lab Earthquake Dy nam, Beijing 100029, Peoples R China. RP Oskin, ME (reprint author), Univ Calif Davis, Dept Geol, 1 Shields Ave, Davis, CA 95618 USA. EM meoskin@ucdavis.edu RI Liu-Zeng, Jing/F-8582-2011; Hudnut, Kenneth/B-1945-2009; Hinojosa-Corona, Alejandro/L-5422-2015; Fielding, Eric/A-1288-2007; OI Hudnut, Kenneth/0000-0002-3168-4797; Hinojosa-Corona, Alejandro/0000-0002-2282-337X; Fielding, Eric/0000-0002-6648-8067; Elliott, Austin/0000-0001-5924-7268 FU NSF RAPID [EAR-1039168, 1039147]; NSF [EAR-0106924]; U.S. Geological Survey [02HQAG0008]; Consejo Nacional de Ciencia y Tecnologia [CB-2007-81463]; NASA's Earth Surface and Interior Focus Area FX LIDAR data acquisition supported by an NSF RAPID grant (EAR-1039168 and 1039147), with additional support from the Southern California Earthquake Center (supported by NSF-EAR-0106924 and U.S. Geological Survey grant 02HQAG0008) and Consejo Nacional de Ciencia y Tecnologia (grant CB-2007-81463). Part of this research was supported by NASA's Earth Surface and Interior Focus Area and performed at the Jet Propulsion Laboratory, California Institute of Technology. Y. Fialko, D. Sandwell, J. Galetzka, and A. Gonzalez assisted with Global Positioning System data acquisition and processing. C. Crosby, D. Haddad, O. Kreylos, A. Morelan, and T. Sato provided editorial and computational assistance. The National Center for Airborne Laser Mapping gathered and processed the postevent LIDAR data, distributed at OpenTopography (http://opentopography.org/id/OTLAS.122010.32611.1). We thank INEGI for granting access to the pre-event LIDAR data used for this study. Pre-event LIDAR digital elevation model and derived elevation difference data for the Sierra Cucapah rupture zone are available in the supporting online material. NR 29 TC 77 Z9 83 U1 0 U2 44 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 10 PY 2012 VL 335 IS 6069 BP 702 EP 705 DI 10.1126/science.1213778 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 889AY UT WOS:000300047100048 PM 22323817 ER PT J AU Abbasi, R Abdou, Y Abu-Zayyad, T Ackermann, M Adams, J Aguilar, JA Ahlers, M Allen, MM Altmann, D Andeen, K Auffenberg, J Bai, X Baker, M Barwick, SW Bay, R Alba, JLB Beattie, K Beatty, JJ Bechet, S Becker, JK Becker, KH Benabderrahmane, ML BenZvi, S Berdermann, J Berghaus, P Berley, D Bernardini, E Bertrand, D Besson, DZ Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bose, D Boser, S Botner, O Brown, AM Buitink, S Caballero-Mora, KS Carson, M Chirkin, D Christy, B Clevermann, F Cohen, S Colnard, C Cowen, DF Silva, AHC D'Agostino, MV Danninger, M Daughhetee, J Davis, JC De Clercq, C Degner, T Demirors, L Descamps, F Desiati, P de Vries-Uiterweerd, G DeYoung, T Diaz-Velez, JC Dierckxsens, M Dreyer, J Dumm, JP Dunkman, M Eisch, J Ellsworth, RW Engdegard, O Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feintzeig, J Feusels, T Filimonov, K Finley, C Fischer-Wasels, T Fox, BD Franckowiak, A Franke, R Gaisser, TK Gallagher, J Gerhardt, L Gladstone, L Glusenkamp, T Goldschmidt, A Goodman, JA Gora, D Grant, D Griesel, T Gross, A Grullon, S Gurtner, M Ha, C Ismail, AH Hallgren, A Halzen, F Han, K Hanson, K Heinen, D Helbing, K Hellauer, R Hickford, S Hill, GC Hoffman, KD Hoffmann, B Homeier, A Hoshina, K Huelsnitz, W Hulss, JP Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobi, E Jacobsen, J Japaridze, GS Johansson, H Kampert, KH Kappes, A Karg, T Karle, A Kenny, P Kiryluk, J Kislat, F Klein, SR Kohne, JH Kohnen, G Kolanoski, H Kopke, L Kopper, S Koskinen, DJ Kowalski, M Kowarik, T Krasberg, M Kroll, G Kurahashi, N Kuwabara, T Labare, M Laihem, K Landsman, H Larson, MJ Lauer, R Lunemann, J Madsen, J Marotta, A Maruyama, R Mase, K Matis, HS Meagher, K Merck, M Meszaros, P Meures, T Miarecki, S Middell, E Milke, N Miller, J Montaruli, T Morse, R Movit, SM Nahnhauer, R Nam, JW Naumann, U Nygren, DR Odrowski, S Olivas, A Olivo, M O'Murchadha, A Panknin, S Paul, L de los Heros, CP Petrovic, J Piegsa, A Pieloth, D Porrata, R Posselt, J Price, CC Price, PB Przybylski, GT Rawlins, K Redl, P Resconi, E Rhode, W Ribordy, M Richman, M Rodrigues, JP Rothmaier, F Rott, C Ruhe, T Rutledge, D Ruzybayev, B Ryckbosch, D Sander, HG Santander, M Sarkar, S Schatto, K Schmidt, T Schonwald, A Schukraft, A Schultes, A Schulz, O Schunck, M Seckel, D Semburg, B Seo, SH Sestayo, Y Seunarine, S Silvestri, A Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stezelberger, T Stokstad, RG Stossl, A Strahler, EA Strom, R Stuer, M Sullivan, GW Swillens, Q Taavola, H Taboada, I Tamburro, A Tepe, A Ter-Antonyan, S Tilav, S Toale, PA Toscano, S Tosi, D van Eijndhoven, N Vandenbroucke, J Van Overloop, A van Santen, J Vehring, M Voge, M Walck, C Waldenmaier, T Wallraff, M Walter, M Weaver, C Wendt, C Westerhoff, S Whitehorn, N Wiebe, K Wiebusch, CH Williams, DR Wischnewski, R Wissing, H Wolf, M Wood, TR Woschnagg, K Xu, C Xu, DL Xu, XW Yanez, JP Yodh, G Yoshida, S Zarzhitsky, P Zoll, M AF Abbasi, R. Abdou, Y. Abu-Zayyad, T. Ackermann, M. Adams, J. Aguilar, J. A. Ahlers, M. Allen, M. M. Altmann, D. Andeen, K. Auffenberg, J. Bai, X. Baker, M. Barwick, S. W. Bay, R. Alba, J. L. Bazo Beattie, K. Beatty, J. J. Bechet, S. Becker, J. K. Becker, K. -H. Benabderrahmane, M. L. BenZvi, S. Berdermann, J. Berghaus, P. Berley, D. Bernardini, E. Bertrand, D. Besson, D. Z. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bose, D. Boeser, S. Botner, O. Brown, A. M. Buitink, S. Caballero-Mora, K. S. Carson, M. Chirkin, D. Christy, B. Clevermann, F. Cohen, S. Colnard, C. Cowen, D. F. Silva, A. H. Cruz D'Agostino, M. V. Danninger, M. Daughhetee, J. Davis, J. C. De Clercq, C. Degner, T. Demiroers, L. Descamps, F. Desiati, P. de Vries-Uiterweerd, G. DeYoung, T. Diaz-Velez, J. C. Dierckxsens, M. Dreyer, J. Dumm, J. P. Dunkman, M. Eisch, J. Ellsworth, R. W. Engdegard, O. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feintzeig, J. Feusels, T. Filimonov, K. Finley, C. Fischer-Wasels, T. Fox, B. D. Franckowiak, A. Franke, R. Gaisser, T. K. Gallagher, J. Gerhardt, L. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Goodman, J. A. Gora, D. Grant, D. Griesel, T. Gross, A. Grullon, S. Gurtner, M. Ha, C. Ismail, A. Haj Hallgren, A. Halzen, F. Han, K. Hanson, K. Heinen, D. Helbing, K. Hellauer, R. Hickford, S. Hill, G. C. Hoffman, K. D. Hoffmann, B. Homeier, A. Hoshina, K. Huelsnitz, W. Huelss, J. -P. Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jacobi, E. Jacobsen, J. Japaridze, G. S. Johansson, H. Kampert, K. -H. Kappes, A. Karg, T. Karle, A. Kenny, P. Kiryluk, J. Kislat, F. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koepke, L. Kopper, S. Koskinen, D. J. Kowalski, M. Kowarik, T. Krasberg, M. Kroll, G. Kurahashi, N. Kuwabara, T. Labare, M. Laihem, K. Landsman, H. Larson, M. J. Lauer, R. Luenemann, J. Madsen, J. Marotta, A. Maruyama, R. Mase, K. Matis, H. S. Meagher, K. Merck, M. Meszaros, P. Meures, T. Miarecki, S. Middell, E. Milke, N. Miller, J. Montaruli, T. Morse, R. Movit, S. M. Nahnhauer, R. Nam, J. W. Naumann, U. Nygren, D. R. Odrowski, S. Olivas, A. Olivo, M. O'Murchadha, A. Panknin, S. Paul, L. de los Heros, C. Perez Petrovic, J. Piegsa, A. Pieloth, D. Porrata, R. Posselt, J. Price, C. C. Price, P. B. Przybylski, G. T. Rawlins, K. Redl, P. Resconi, E. Rhode, W. Ribordy, M. Richman, M. Rodrigues, J. P. Rothmaier, F. Rott, C. Ruhe, T. Rutledge, D. Ruzybayev, B. Ryckbosch, D. Sander, H. -G. Santander, M. Sarkar, S. Schatto, K. Schmidt, T. Schoenwald, A. Schukraft, A. Schultes, A. Schulz, O. Schunck, M. Seckel, D. Semburg, B. Seo, S. H. Sestayo, Y. Seunarine, S. Silvestri, A. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stezelberger, T. Stokstad, R. G. Stoessl, A. Strahler, E. A. Strom, R. Stueer, M. Sullivan, G. W. Swillens, Q. Taavola, H. Taboada, I. Tamburro, A. Tepe, A. Ter-Antonyan, S. Tilav, S. Toale, P. A. Toscano, S. Tosi, D. van Eijndhoven, N. Vandenbroucke, J. Van Overloop, A. van Santen, J. Vehring, M. Voge, M. Walck, C. Waldenmaier, T. Wallraff, M. Walter, M. Weaver, Ch. Wendt, C. Westerhoff, S. Whitehorn, N. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wischnewski, R. Wissing, H. Wolf, M. Wood, T. R. Woschnagg, K. Xu, C. Xu, D. L. Xu, X. W. Yanez, J. P. Yodh, G. Yoshida, S. Zarzhitsky, P. Zoll, M. CA IceCube Collaboration TI OBSERVATION OF ANISOTROPY IN THE GALACTIC COSMIC-RAY ARRIVAL DIRECTIONS AT 400 TeV WITH ICECUBE SO ASTROPHYSICAL JOURNAL LA English DT Article DE astroparticle physics; cosmic rays; neutrinos ID MAGNETOHYDRODYNAMIC TURBULENCE; INTERSTELLAR-MEDIUM; MAGNETIC-FIELD; MILAGRO; DIFFUSION; ORIGIN AB In this paper we report the first observation in the Southern hemisphere of an energy dependence in the Galactic cosmic-ray anisotropy up to a few hundred TeV. This measurement was performed using cosmic-ray-induced muons recorded by the partially deployed IceCube observatory between 2009 May and 2010 May. The data include a total of 33 x 10(9) muon events with a median angular resolution of similar to 3 degrees. A sky map of the relative intensity in arrival direction over the Southern celestial sky is presented for cosmic-ray median energies of 20 and 400 TeV. The same large-scale anisotropy observed at median energies around 20 TeV is not present at 400 TeV. Instead, the high-energy sky map shows a different anisotropy structure including a deficit with a post-trial significance of -6.3 sigma. This anisotropy reveals a new feature of the Galactic cosmic-ray distribution, which must be incorporated into theories of the origin and propagation of cosmic rays. C1 [Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Price, C. C.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Ackermann, M.; Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Silva, A. H. Cruz; Franke, R.; Gluesenkamp, T.; Gora, D.; Han, K.; Jacobi, E.; Kislat, F.; Lauer, R.; Middell, E.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Tosi, D.; Walter, M.; Wischnewski, R.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany. [Adams, J.; Brown, A. M.; Gross, A.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Allen, M. M.; Caballero-Mora, K. S.; Cowen, D. F.; DeYoung, T.; Dunkman, M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Larson, M. J.; Meszaros, P.; Rutledge, D.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Altmann, D.; Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Heinen, D.; Hoffmann, B.; Huelss, J. -P.; Laihem, K.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Auffenberg, J.; Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Kopper, S.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Bai, X.; Berghaus, P.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bai, X.; Berghaus, P.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Miarecki, S.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Beattie, K.; Gerhardt, L.; Goldschmidt, A.; Kiryluk, J.; 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. [Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Davis, J. C.; Rott, 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. [Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Meures, T.; Petrovic, J.; Swillens, Q.] Univ Libre Brussels, Sci Fac CP230, B-1050 Brussels, Belgium. [Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany. [Berley, D.; Blaufuss, E.; Christy, B.; Ellsworth, R. W.; 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. [Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Bose, D.; Buitink, S.; De Clercq, C.; Labare, M.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Boeser, S.; Degner, T.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Stueer, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; de los Heros, C. Perez; Strom, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Clevermann, F.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany. [Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany. [Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] So Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Grant, D.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Huelsnitz, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Montaruli, T.] Dipartimento Fis, Sez INFN, I-70126 Bari, Italy. [Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Ismail, A. Haj; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium. [Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. RP Abbasi, R (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. RI Taavola, Henric/B-4497-2011; Tjus, Julia/G-8145-2012; Wiebusch, Christopher/G-6490-2012; Tamburro, Alessio/A-5703-2013; Auffenberg, Jan/D-3954-2014; Botner, Olga/A-9110-2013; Hallgren, Allan/A-8963-2013; Koskinen, David/G-3236-2014; Kowalski, Marek/G-5546-2012; Aguilar Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011 OI Perez de los Heros, Carlos/0000-0002-2084-5866; Taavola, Henric/0000-0002-2604-2810; Buitink, Stijn/0000-0002-6177-497X; Benabderrahmane, Mohamed Lotfi/0000-0003-4410-5886; Wiebusch, Christopher/0000-0002-6418-3008; Carson, Michael/0000-0003-0400-7819; Auffenberg, Jan/0000-0002-1185-9094; Koskinen, David/0000-0002-0514-5917; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952 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; National Science and Engineering Research Council of 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); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus; 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; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland; EU; Capes Foundation, Ministry of Education of Brazil 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; National Science and Engineering Research Council of 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), 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; Japan Society for Promotion of Science (JSPS); and the Swiss National Science Foundation (SNSF), Switzerland. A. Gross acknowledges support by the EU Marie Curie OIF Program; J. P. Rodrigues acknowledges support by the Capes Foundation, Ministry of Education of Brazil. NR 36 TC 70 Z9 71 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 DI 10.1088/0004-637X/746/1/33 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300033 ER PT J AU Camilo, F Kerr, M Ray, PS Ransom, SM Johnston, S Romani, RW Parent, D DeCesar, ME Harding, AK Donato, D Parkinson, PMS Ferrara, EC Freire, PCC Guillemot, L Keith, M Kramer, M Wood, KS AF Camilo, F. Kerr, M. Ray, P. S. Ransom, S. M. Johnston, S. Romani, R. W. Parent, D. DeCesar, M. E. Harding, A. K. Donato, D. Parkinson, P. M. Saz Ferrara, E. C. Freire, P. C. C. Guillemot, L. Keith, M. Kramer, M. Wood, K. S. TI PSR J2030+3641: RADIO DISCOVERY AND GAMMA-RAY STUDY OF A MIDDLE-AGED PULSAR IN THE NOW IDENTIFIED FERMI-LAT SOURCE 1FGL J2030.0+3641 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: stars; pulsars: individual (PSR J2030+3641) ID LARGE-AREA TELESCOPE; BLIND FREQUENCY SEARCHES; MILLISECOND PULSARS; MAGNETIC-FIELD; LIGHT CURVES; SLOT GAPS; EMISSION; POLARIZATION; ACCELERATION; RADIATION AB In a radio search with the Green Bank Telescope of three unidentified low Galactic latitude Fermi Large Area Telescope (LAT) sources, we have discovered the middle-aged pulsar J2030+3641 associated with 1FGL J2030.0+3641 (2FGL J2030.0+3640). Following the detection of gamma-ray pulsations using a radio ephemeris, we have obtained a phase-coherent timing solution based on gamma-ray and radio pulse arrival times which spans the entire Fermi mission. With a rotation period of 0.2 s, a spin-down luminosity of 3 x 10(34) erg s(-1), and a characteristic age of 0.5 Myr, PSR J2030+3641 is a middle-aged neutron star with spin parameters similar to those of the exceedingly gamma-ray-bright and radio-undetected Geminga. Its gamma-ray flux is 1% that of Geminga, primarily because of its much larger distance, as suggested by the large integrated column density of free electrons, DM = 246 pc cm(-3). We fit the gamma-ray light curve, along with limited radio polarimetric constraints, to four geometrical models of magnetospheric emission, and while none of the fits have high significance some are encouraging and suggest that further refinements of these models may be worthwhile. We argue that not many more non-millisecond radio pulsars may be detected along the Galactic plane that are responsible for LAT sources, but that modified methods to search for gamma-ray pulsations should be productive-PSR J2030+3641 would have been found blindly in gamma rays if only >= 0.8 GeV photons had been considered, owing to its relatively flat spectrum and location in a region of high soft background. C1 [Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kerr, M.; Romani, R. W.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Kerr, M.; Romani, R. W.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Ray, P. S.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Johnston, S.; Keith, M.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Parent, D.] George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA. [DeCesar, M. E.; Harding, A. K.; Donato, D.; Ferrara, E. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Donato, D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Donato, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Donato, D.] CRESST, Greenbelt, MD 20771 USA. [Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Freire, P. C. C.; Guillemot, L.; Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kramer, M.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. RP Camilo, F (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. EM fernando@astro.columbia.edu; kerrm@stanford.edu; Paul.Ray@nrl.navy.mil RI Saz Parkinson, Pablo Miguel/I-7980-2013; OI Ray, Paul/0000-0002-5297-5278; Ransom, Scott/0000-0001-5799-9714 FU NASA [PF0-110073, NAS8-03060] FX The GBT is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. 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 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. Support for this work was provided by NASA through Einstein Postdoctoral Fellowship Award Number PF0-110073 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. NR 54 TC 11 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 DI 10.1088/0004-637X/746/1/39 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300039 ER PT J AU Geissler, K Metchev, SA Pham, A Larkin, JE McElwain, M Hillenbrand, LA AF Geissler, Kerstin Metchev, Stanimir A. Pham, Alfonse Larkin, James E. McElwain, Michael Hillenbrand, Lynne A. TI A SUBSTELLAR COMMON PROPER-MOTION COMPANION TO THE PLEIAD HII 1348 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: visual; brown dwarfs; instrumentation: adaptive optics; stars: individual (Cl Melotte 22 1348); stars: low-mass ID LOW-MASS STARS; INTEGRAL FIELD SPECTROGRAPH; ADAPTIVE OPTICS SYSTEM; BROWN DWARF BINARIES; OPEN CLUSTERS; EVOLUTIONARY MODELS; WIDE BINARIES; GIANT PLANETS; LITHIUM TEST; T-DWARFS AB We announce the identification of a proper-motion companion to the star Hii 1348, a K5V member of the Pleiades open cluster. The existence of a faint point source 1.'' 1 away from Hii 1348 was previously known from adaptive optics imaging by Bouvier et al. However, because of a high likelihood of background star contamination and in the absence of follow-up astrometry, Bouvier et al. tentatively concluded that the candidate companion was not physically associated with Hii 1348. We establish the proper-motion association of the pair from adaptive optics imaging with the Palomar 5 m telescope. Adaptive optics spectroscopy with the integral field spectrograph OSIRIS on the Keck 10 m telescope reveals that the companion has a spectral type of M8 +/- 1. According to substellar evolution models, the M8 spectral type resides within the substellar mass regime at the age of the Pleiades. The primary itself is a known double-lined spectroscopic binary, which makes the resolved companion, Hii 1348B, the least massive and widest component of this hierarchical triple system and the first substellar companion to a stellar primary in the Pleiades. C1 [Geissler, Kerstin; Metchev, Stanimir A.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Pham, Alfonse] Indiana Univ, Ctr Explorat Energy & Matter, Bloomington, IN 47408 USA. [Larkin, James E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [McElwain, Michael] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Lab Exoplanets & Stellar Astrophys, Greenbelt, MD 20771 USA. [Hillenbrand, Lynne A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Geissler, K (reprint author), SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. EM geissler@mail.astro.sunysb.edu FU Spitzer Fellowship Program [1273192] FX Partial support for S. A. M. was provided through the Spitzer Fellowship Program under award 1273192. The authors also wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. NR 55 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 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 DI 10.1088/0004-637X/746/1/44 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300044 ER PT J AU Luna, M Karpen, JT DeVore, CR AF Luna, M. Karpen, J. T. DeVore, C. R. TI FORMATION AND EVOLUTION OF A MULTI-THREADED SOLAR PROMINENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: filaments; prominences; Sun: magnetic topology ID MAGNETIC-FIELD; CORONAL LOOPS; THERMAL NONEQUILIBRIUM; QUIESCENT PROMINENCES; ALPHA FILTERGRAMS; ACTIVE-REGION; FILAMENT; DYNAMICS; FLOWS; MODEL AB We investigate the process of formation and subsequent evolution of prominence plasma in a filament channel and its overlying arcade. We construct a three-dimensional time-dependent model of an intermediate quiescent prominence suitable to be compared with observations. We combine the magnetic field structure of a three-dimensional sheared double arcade with one-dimensional independent simulations of many selected flux tubes, in which the thermal nonequilibrium process governs the plasma evolution. We have found that the condensations in the corona can be divided into two populations: threads and blobs. Threads are massive condensations that linger in the flux tube dips. Blobs are ubiquitous small condensations that are produced throughout the filament and overlying arcade magnetic structure, and rapidly fall to the chromosphere. The threads are the principal contributors to the total mass, whereas the blob contribution is small. The total prominence mass is in agreement with observations, assuming reasonable filling factors of order 0.001 and a fixed number of threads. The motion of the threads is basically horizontal, while blobs move in all directions along the field. We have generated synthetic images of the whole structure in an Ha proxy and in two EUV channels of the Atmospheric Imaging Assembly instrument on board Solar Dynamics Observatory, thus showing the plasma at cool, warm, and hot temperatures. The predicted differential emission measure of our system agrees very well with observations in the temperature range log T = 4.6-5.7. We conclude that the sheared-arcade magnetic structure and plasma behavior driven by thermal nonequilibrium fit the abundant observational evidence well for typical intermediate prominences. C1 [Luna, M.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA. [Luna, M.] NASA, Space Weather Lab, GSFC, Greenbelt, MD 20771 USA. [DeVore, C. R.] USN, Res Lab, Washington, DC 20375 USA. RP Luna, M (reprint author), NASA, CRESST, GSFC, Greenbelt, MD 20771 USA. RI DeVore, C/A-6067-2015; Karpen, Judith/E-1484-2012 OI DeVore, C/0000-0002-4668-591X; FU University of Maryland at College Park; people of CRESST; NASA through NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center; ISSI FX This work has been supported by the NASA Heliophysics SR&T program. M. L. also acknowledges support from the University of Maryland at College Park and the people of CRESST. 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. All of us are grateful to our colleagues on international teams on solar prominences hosted by the International Space Science Institute (ISSI) in Bern, Switzerland, especially team leader N. Labrosse, and acknowledge the support of ISSI, where this work has been presented. Finally, we thank J. A. Klimchuk, T. A. Kucera, S. R. Habbal, and K. K. Reeves for helpful discussions. NR 63 TC 39 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 FEB 10 PY 2012 VL 746 IS 1 DI 10.1088/0004-637X/746/1/30 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300030 ER PT J AU Weisskopf, MC Elsner, RF Kolodziejczak, JJ O'Dell, SL Tennant, AF AF Weisskopf, Martin C. Elsner, Ronald F. Kolodziejczak, Jeffery J. O'Dell, Stephen L. Tennant, Allyn F. TI UNRAVELING THE GEOMETRY OF THE CRAB NEBULA's "INNER RING" SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (Crab Nebula) ID PULSAR WIND NEBULAE; ORIGIN; TORUS AB Chandra images of the Crab Nebula resolve the detailed structure of its "inner ring," possibly a termination shock where pulsar-accelerated relativistic particles begin to emit X radiation. Analysis of these images finds that the center of the ellipse-presumably a circular ring in projection-lies about 0.'' 9 (10 light days at 2 kpc) from the pulsar's image, at a position angle of about 300 degrees (east of north). This analysis also measures properties of the ellipse: the position angle of the semi-major axis is about 210 degrees (east of north); the aspect ratio is 0.49. In a simple-albeit, not unique-de-projection of the observed geometry, a circular ring is centered on the axis of symmetry of the pulsar wind nebula. This ring is not equatorial but rather lies near + 4.degrees 5 latitude in pulsar-centered coordinates. Alternative geometries are briefly discussed. C1 [Weisskopf, Martin C.; Elsner, Ronald F.; Kolodziejczak, Jeffery J.; O'Dell, Stephen L.; Tennant, Allyn F.] NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Weisskopf, MC (reprint author), NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. OI O'Dell, Stephen/0000-0002-1868-8056 NR 15 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 DI 10.1088/0004-637X/746/1/41 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300041 ER PT J AU Tokar, RL Johnson, RE Thomsen, MF Sittler, EC Coates, AJ Wilson, RJ Crary, FJ Young, DT Jones, GH AF Tokar, R. L. Johnson, R. E. Thomsen, M. F. Sittler, E. C. Coates, A. J. Wilson, R. J. Crary, F. J. Young, D. T. Jones, G. H. TI Detection of exospheric O-2(+) at Saturn's moon Dione SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ION-CYCLOTRON WAVES; PLASMA; RHEA; MAGNETOSPHERE; SATELLITES; TETHYS AB During a close pass of Cassini through the plasma wake of Saturn's moon Dione on April 7, 2010 the Cassini Plasma Spectrometer (CAPS) detected molecular oxygen ions (O-2(+)) on pick up ring velocity distributions, thus providing the first in situ detection of a neutral exosphere surrounding the icy moon. The density of O-2(+) determined from the CAPS data ranges from 0.01 to 0.09 /cm(3) and is used to estimate the exosphere O-2 radial column density, obtaining the range 0.9 to 7 x 10(11)/cm(2). CAPS was unable to directly detect pick up H2O+ from the exosphere but the observations can be used to set an upper limit to their density of similar to 10 times the O-2(+) density. Citation: Tokar, R. L., R. E. Johnson, M. F. Thomsen, E. C. Sittler, A. J. Coates, R. J. Wilson, F. J. Crary, D. T. Young, and G. H. Jones (2012), Detection of exospheric O-2(+) at Saturn's moon Dione, Geophys. Res. Lett., 39, L03105, doi:10.1029/2011GL050452. C1 [Tokar, R. L.; Thomsen, M. F.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Johnson, R. E.] Univ Virginia, Charlottesville, VA 22904 USA. [Sittler, E. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Coates, A. J.; Jones, G. H.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Wilson, R. J.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Crary, F. J.; Young, D. T.] SW Res Inst, San Antonio, TX 78229 USA. [Jones, G. H.] UCL Birkbeck, Ctr Planetary Sci, London, England. RP Tokar, RL (reprint author), Los Alamos Natl Lab, Mail Stop D466, Los Alamos, NM 87545 USA. EM rlt@lanl.gov RI Wilson, Rob/C-2689-2009; Jones, Geraint/C-1682-2008; Coates, Andrew/C-2396-2008; OI Wilson, Rob/0000-0001-9276-2368; Coates, Andrew/0000-0002-6185-3125; Jones, Geraint/0000-0002-5859-1136 FU JPL [1243218]; Southwest Research Institute; UK Science and Technology Facilities Council (STFC); ESA via UK Space Agency; CAPS-ELS science by STFC; STFC FX The authors wish to thank Krishan Khurana for helpful conversations regarding the Cassini Dione observations. The work of U.S. co-authors was supported by JPL contracts 1243218 with Southwest Research Institute. We acknowledge support of the CAPS ELS operations and software team by the UK Science and Technology Facilities Council (STFC, to 2010) and by ESA via UK Space Agency (from 2011), and support of CAPS-ELS science by STFC. GHJ is supported by an STFC Advanced Fellowship. Cassini is managed by the Jet Propulsion Laboratory for NASA. NR 23 TC 20 Z9 20 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 9 PY 2012 VL 39 AR L03105 DI 10.1029/2011GL050452 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 891UB UT WOS:000300241000004 ER PT J AU He, H Li, C Loughner, CP Li, ZQ Krotkov, NA Yang, K Wang, L Zheng, YF Bao, XD Zhao, GQ Dickerson, RR AF He, Hao Li, Can Loughner, Christopher P. Li, Zhanqing Krotkov, Nickolay A. Yang, Kai Wang, Lei Zheng, Youfei Bao, Xiangdong Zhao, Guoqiang Dickerson, Russell R. TI SO2 over central China: Measurements, numerical simulations and the tropospheric sulfur budget SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LONG-RANGE TRANSPORT; POLLUTION CONTROL POLICIES; AIR-QUALITY BENEFITS; PEARL RIVER-DELTA; DRY DEPOSITION; INTEX-B; EAST-ASIA; PART I; HOMOGENEOUS OXIDATION; AIRCRAFT MEASUREMENTS AB SO2 in central China was measured in situ from an aircraft and remotely using the Ozone Monitoring Instrument (OMI) from the Aura satellite; results were used to develop a numerical tool for evaluating the tropospheric sulfur budget - sources, sinks, transformation and transport. In April 2008, measured ambient SO2 concentrations decreased from similar to 7 ppbv near the surface to similar to 1 ppbv at 1800 m altitude (an effective scale height of similar to 800 m), but distinct SO2 plumes were observed between 1800 and 4500 m, the aircraft's ceiling. These free tropospheric plumes play a major role in the export of SO2 and in the accuracy of OMI retrievals. The mean SO2 column contents from aircraft measurements (0.73 DU, Dobson Units) and operational OMI SO2 products (0.63 +/- 0.26 DU) were close. The OMI retrievals were well correlated with in situ measurements (r = 0.84), but showed low bias (slope = 0.54). A new OMI retrieval algorithm was tested and showed improved agreement and bias (r = 0.87, slope = 0.86). The Community Multiscale Air Quality (CMAQ) model was used to simulate sulfur chemistry, exhibiting reasonable agreement (r = 0.62, slope = 1.33) with in situ SO2 columns. The mean CMAQ SO2 loading over central and eastern China was 54 kT, similar to 30% more than the estimate from OMI SO2 products, 42 kT. These numerical simulations, constrained by observations, indicate that similar to 50% (35 to 61%) of the anthropogenic sulfur emissions were transported downwind, and the overall lifetime of tropospheric SO2 was 38 +/- 7 h. C1 [He, Hao; Li, Zhanqing; Yang, Kai; Dickerson, Russell R.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Bao, Xiangdong; Zhao, Guoqiang] Henan Meteorol Bur, Zhengzhou 450003, Peoples R China. [Li, Can; Loughner, Christopher P.; Krotkov, Nickolay A.; Yang, Kai] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Li, Can; Loughner, Christopher P.; Li, Zhanqing; Dickerson, Russell R.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Wang, Lei; Zheng, Youfei] Nanjing Univ Informat Sci Technol, Nanjing 210044, Jiangsu, Peoples R China. [Li, Zhanqing] Beijing Normal Univ, State Key Lab Earth Surface Proc & Resource, GCESS, Beijing 100875, Peoples R China. [Dickerson, Russell R.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. RP He, H (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. EM russ@atmos.umd.edu RI Dickerson, Russell/F-2857-2010; Li, Can/F-6867-2011; Krotkov, Nickolay/E-1541-2012; He, Hao/E-4771-2015; Li, Zhanqing/F-4424-2010; OI Dickerson, Russell/0000-0003-0206-3083; Krotkov, Nickolay/0000-0001-6170-6750; Li, Zhanqing/0000-0001-6737-382X; Loughner, Christopher/0000-0002-3833-2014 FU NASA [NNX08AH71G]; DOE [DESC0007171]; UMD FX We thank Qiang Zhang at Tsinghua University for the discussion on the application of INTEX-B emission inventory. We thank R. J. Salawitch for helpful comments. This work was supported by NASA (NNX08AH71G), DOE (DESC0007171) and UMD. NR 80 TC 32 Z9 32 U1 3 U2 38 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 9 PY 2012 VL 117 AR D00K37 DI 10.1029/2011JD016473 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 891QJ UT WOS:000300231400005 ER PT J AU Kwok, R Cunningham, GF Manizade, SS Krabill, WB AF Kwok, R. Cunningham, G. F. Manizade, S. S. Krabill, W. B. TI Arctic sea ice freeboard from IceBridge acquisitions in 2009: Estimates and comparisons with ICESat SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID LASER ALTIMETER MEASUREMENTS; AIRBORNE LASER; SHEET; RADAR AB During the spring of 2009, the Airborne Topographic Mapper (ATM) system on the IceBridge mission acquired cross-basin surveys of surface elevations of Arctic sea ice. In this paper, the total freeboard derived from four similar to 2000 km transects are examined and compared with those from the 2009 ICESat campaign. Total freeboard, the sum of the snow and ice freeboards, is the elevation of the air-snow interface above the local sea surface. Prior to freeboard retrieval, signal dependent range biases are corrected. With data from a near co-incident outbound and return track on 21 April, we show that our estimates of the freeboard are repeatable to within similar to 4 cm but dependent locally on the density and quality of sea surface references. Overall difference between the ATM and ICESat freeboards for the four transects is 0.7 (8.5) cm (quantity in bracket is standard deviation), with a correlation of 0.78 between the data sets of one hundred seventy-eight 50 km averages. This establishes a level of confidence in the use of ATM freeboards to provide regional samplings that are consistent with ICESat. In early April, mean freeboards are 41 cm and 55 cm over first year and multiyear sea ice (MYI), respectively. Regionally, the lowest mean ice freeboard (28 cm) is seen on 5 April where the flight track sampled the large expanse of seasonal ice in the western Arctic. The highest mean freeboard (71 cm) is seen in the multiyear ice just west of Ellesmere Island from 21 April. The relatively large unmodeled variability of the residual sea surface resolved by ATM elevations is discussed. C1 [Kwok, R.; Cunningham, G. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Manizade, S. S.] NASA, Wallops Flight Facil, URS Corp, Wallops Isl, VA 23337 USA. [Krabill, W. B.] NASA, Goddard Space Flight Ctr, Lab Hydrospher Proc, Wallops Isl, VA 23337 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 OI Kwok, Ron/0000-0003-4051-5896 FU National Aeronautics and Space Administration FX We thank Ron Lindsay and another reviewer for providing valuable comments that have contributed to improvements of our manuscript. The QuikSCAT data were provided by the Physical Oceanography DAAC at the Jet Propulsion Laboratory, Pasadena, California. The IceBridge data were provided by the National Snow and Ice Data Center. 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 11 TC 14 Z9 14 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD FEB 9 PY 2012 VL 117 AR C02018 DI 10.1029/2011JC007654 PN 2012 PG 14 WC Oceanography SC Oceanography GA 893AY UT WOS:000300328800005 ER PT J AU Parks, GK Lee, E McCarthy, M Goldstein, M Fu, SY Cao, JB Canu, P Lin, N Wilber, M Dandouras, I Reme, H Fazakerley, A AF Parks, G. K. Lee, E. McCarthy, M. Goldstein, M. Fu, S. Y. Cao, J. B. Canu, P. Lin, N. Wilber, M. Dandouras, I. Reme, H. Fazakerley, A. TI Entropy Generation across Earth's Collisionless Bow Shock SO PHYSICAL REVIEW LETTERS LA English DT Article ID GYRATING IONS; ELECTRON; DISTRIBUTIONS AB Earth's bow shock is a collisionless shock wave but entropy has never been directly measured across it. The plasma experiments on Cluster and Double Star measure 3D plasma distributions upstream and downstream of the bow shock allowing calculation of Boltzmann's entropy function H and his famous H theorem, dH/dt <= 0. The collisionless Boltzmann (Vlasov) equation predicts that the total entropy does not change if the distribution function across the shock becomes nonthermal, but it allows changes in the entropy density. Here, we present the first direct measurements of entropy density changes across Earth's bow shock and show that the results generally support the model of the Vlasov analysis. These observations are a starting point for a more sophisticated analysis that includes 3D computer modeling of collisionless shocks with input from observed particles, waves, and turbulences. C1 [Parks, G. K.; Lin, N.; Wilber, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Lee, E.] Kyung Hee Univ, Sch Space Res, Yongin, South Korea. [McCarthy, M.] Univ Washington, Seattle, WA 98195 USA. [Goldstein, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fu, S. Y.] Peking Univ, Inst Space Phys & Appl Technol, Beijing 100871, Peoples R China. [Cao, J. B.] Beihang Univ, Space Sci Inst, Sch Aeronaut, Beijing, Peoples R China. [Canu, P.] Ecole Polytech, Plasma Phys Lab, F-75230 Paris, France. [Dandouras, I.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Reme, H.] IRAP, CNRS, Toulouse 4, France. [Fazakerley, A.] UCL, MSSL, London, England. RP Parks, GK (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM parks@ssl.berkeley.edu RI Lee, Ensang/E-2356-2013; Fu, Suiyan/E-9178-2013; OI Dandouras, Iannis/0000-0002-7121-1118 FU NASA [NNX07AP96G]; WCU through NRF; MEST of Korea [R31-10016] FX The research at UC Berkeley is funded by NASA Grant No. NNX07AP96G and at Kyung Hee University by the WCU program through NRF funded by MEST of Korea (Grant No. R31-10016). NR 15 TC 4 Z9 4 U1 0 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD FEB 9 PY 2012 VL 108 IS 6 AR 061102 DI 10.1103/PhysRevLett.108.061102 PG 4 WC Physics, Multidisciplinary SC Physics GA 889VA UT WOS:000300101500003 PM 22401049 ER PT J AU Fressin, F Torres, G Rowe, JF Charbonneau, D Rogers, LA Ballard, S Batalha, NM Borucki, WJ Bryson, ST Buchhave, LA Ciardi, DR Desert, JM Dressing, CD Fabrycky, DC Ford, EB Gautier, TN Henze, CE Holman, MJ Howard, A Howell, SB Jenkins, JM Koch, DG Latham, DW Lissauer, JJ Marcy, GW Quinn, SN Ragozzine, D Sasselov, DD Seager, S Barclay, T Mullally, F Seader, SE Still, M Twicken, JD Thompson, SE Uddin, K AF Fressin, Francois Torres, Guillermo Rowe, Jason F. Charbonneau, David Rogers, Leslie A. Ballard, Sarah Batalha, Natalie M. Borucki, William J. Bryson, Stephen T. Buchhave, Lars A. Ciardi, David R. Desert, Jean-Michel Dressing, Courtney D. Fabrycky, Daniel C. Ford, Eric B. Gautier, Thomas N., III Henze, Christopher E. Holman, Matthew J. Howard, Andrew Howell, Steve B. Jenkins, Jon M. Koch, David G. Latham, David W. Lissauer, Jack J. Marcy, Geoffrey W. Quinn, Samuel N. Ragozzine, Darin Sasselov, Dimitar D. Seager, Sara Barclay, Thomas Mullally, Fergal Seader, Shawn E. Still, Martin Twicken, Joseph D. Thompson, Susan E. Uddin, Kamal TI Two Earth-sized planets orbiting Kepler-20 SO NATURE LA English DT Article ID TRANSITING PLANET; BLEND SCENARIOS; MULTIPLE SYSTEM; GIANT IMPACTS; CANDIDATES; VALIDATION; EXOPLANETS; COMPANION AB Since the discovery of the first extrasolar giant planets around Sun-like stars(1,2), evolving observational capabilities have brought us closer to the detection of true Earth analogues. The size of an exoplanet can be determined when it periodically passes in front of (transits) its parent star, causing a decrease in starlight proportional to its radius. The smallest exoplanet hitherto discovered(3) has a radius 1.42 times that of the Earth's radius (R-circle plus), and hence has 2.9 times its volume. Here we report the discovery of two planets, one Earth-sized (1.03 R-circle plus) and the other smaller than the Earth (0.87 R-circle plus), orbiting the star Kepler-20, which is already known to host three other, larger, transiting planets(4). The gravitational pull of the new planets on the parent star is too small to measure with current instrumentation. We apply a statistical method to show that the likelihood of the planetary interpretation of the transit signals is more than three orders of magnitude larger than that of the alternative hypothesis that the signals result from an eclipsing binary star. Theoretical considerations imply that these planets are rocky, with a composition of iron and silicate. The outer planet could have developed a thick water vapour atmosphere. C1 [Fressin, Francois; Torres, Guillermo; Charbonneau, David; Ballard, Sarah; Desert, Jean-Michel; Dressing, Courtney D.; Holman, Matthew J.; Latham, David W.; Quinn, Samuel N.; Ragozzine, Darin; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rowe, Jason F.; Borucki, William J.; Bryson, Stephen T.; Henze, Christopher E.; Howell, Steve B.; Koch, David G.; Lissauer, Jack J.; Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rogers, Leslie A.; Seager, Sara] MIT, Dept Phys, Cambridge, MA 02139 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Howard, Andrew; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Jenkins, Jon M.; Mullally, Fergal; Seader, Shawn E.; Twicken, Joseph D.; Thompson, Susan E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Uddin, Kamal] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. RP Fressin, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ffressin@cfa.harvard.edu RI Ragozzine, Darin/C-4926-2013; OI Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Charbonneau, David/0000-0002-9003-484X; Barclay, Thomas/0000-0001-7139-2724; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. NR 28 TC 93 Z9 93 U1 7 U2 53 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 9 PY 2012 VL 482 IS 7384 BP 195 EP 198 DI 10.1038/nature10780 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 888HI UT WOS:000299994100033 PM 22186831 ER PT J AU Zwart, SR Jessup, JM Ji, JP Smith, SM AF Zwart, Sara R. Jessup, J. Milburn Ji, Jiuping Smith, Scott M. TI Saturation Diving Alters Folate Status and Biomarkers of DNA Damage and Repair SO PLOS ONE LA English DT Article ID RED-CELL MASS; NUTRITIONAL-STATUS; BODY IRON; BED REST; CANCER; DIVE; HUMANS; NEOCYTOLYSIS; GAMMA-H2AX; DISEASE AB Exposure to oxygen-rich environments can lead to oxidative damage, increased body iron stores, and changes in status of some vitamins, including folate. Assessing the type of oxidative damage in these environments and determining its relationships with changes in folate status are important for defining nutrient requirements and designing countermeasures to mitigate these effects. Responses of humans to oxidative stressors were examined in participants undergoing a saturation dive in an environment with increased partial pressure of oxygen, a NASA Extreme Environment Mission Operations mission. Six participants completed a 13-d saturation dive in a habitat 19 m below the ocean surface near Key Largo, FL. Fasting blood samples were collected before, twice during, and twice after the dive and analyzed for biochemical markers of iron status, oxidative damage, and vitamin status. Body iron stores and ferritin increased during the dive (P < 0.001), with a concomitant decrease in RBC folate (P < 0.001) and superoxide dismutase activity (P < 0.001). Folate status was correlated with serum ferritin (Pearson r = -0.34, P < 0.05). Peripheral blood mononuclear cell poly(ADP-ribose) increased during the dive and the increase was significant by the end of the dive (P < 0.001); gamma-H2AX did not change during the mission. Together, the data provide evidence that when body iron stores were elevated in a hyperoxic environment, a DNA damage repair response occurred in peripheral blood mononuclear cells, but double-stranded DNA damage did not. In addition, folate status decreases quickly in this environment, and this study provides evidence that folate requirements may be greater when body iron stores and DNA damage repair responses are elevated. C1 [Zwart, Sara R.] Univ Space Res Assoc, Houston, TX USA. [Jessup, J. Milburn; Ji, Jiuping] Natl Canc Inst, Bethesda, MD USA. [Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Zwart, SR (reprint author), Univ Space Res Assoc, Houston, TX USA. EM sara.zwart-1@nasa.gov FU NASA FX This study was supported by the NASA Human Research Program Human Health and Countermeasures Element. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 31 TC 8 Z9 9 U1 0 U2 6 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 7 PY 2012 VL 7 IS 2 AR e31058 DI 10.1371/journal.pone.0031058 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 917MF UT WOS:000302180600027 PM 22347427 ER PT J AU Gorham, PW Allison, P Baughman, BM Beatty, JJ Belov, K Besson, DZ Bevan, S Binns, WR Chen, C Chen, P Clem, JM Connolly, A Detrixhe, M De Marco, D Dowkontt, PF DuVernois, M Grashorn, EW Hill, B Hoover, S Huang, M Israel, MH Javaid, A Liewer, KM Matsuno, S Mercurio, BC Miki, C Mottram, M Nam, J Nichol, RJ Palladino, K Romero-Wolf, A Ruckman, L Saltzberg, D Seckel, D Shang, RY Varner, GS Vieregg, AG Wang, Y AF Gorham, P. W. Allison, P. Baughman, B. M. Beatty, J. J. Belov, K. Besson, D. Z. Bevan, S. Binns, W. R. Chen, C. Chen, P. Clem, J. M. Connolly, A. Detrixhe, M. De Marco, D. Dowkontt, P. F. DuVernois, M. Grashorn, E. W. Hill, B. Hoover, S. Huang, M. Israel, M. H. Javaid, A. Liewer, K. M. Matsuno, S. Mercurio, B. C. Miki, C. Mottram, M. Nam, J. Nichol, R. J. Palladino, K. Romero-Wolf, A. Ruckman, L. Saltzberg, D. Seckel, D. Shang, R. Y. Varner, G. S. Vieregg, A. G. Wang, Y. TI Observational constraints on the ultrahigh energy cosmic neutrino flux from the second flight of the ANITA experiment (vol 82, 022004, 2010) SO PHYSICAL REVIEW D LA English DT Correction C1 [Gorham, P. W.; Allison, P.; DuVernois, M.; Hill, B.; Matsuno, S.; Miki, C.; Romero-Wolf, A.; Ruckman, L.; Varner, G. S.] Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA. [Baughman, B. M.; Beatty, J. J.; Grashorn, E. W.; Mercurio, B. C.; Palladino, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Belov, K.; Hoover, S.; Saltzberg, D.; Vieregg, A. G.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Besson, D. Z.; Detrixhe, M.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Bevan, S.; Connolly, A.; Mottram, M.; Nichol, R. J.] UCL, Dept Phys & Astron, London, England. [Binns, W. R.; Dowkontt, P. F.; Israel, M. H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Chen, C.; Chen, P.; Huang, M.; Nam, J.; Shang, R. Y.; Wang, Y.] Natl Taiwan Univ, Dept Phys, Taipei 10617, Taiwan. [Clem, J. M.; De Marco, D.; Javaid, A.; Seckel, D.] Univ Delaware, Dept Phys, Newark, DE 19716 USA. [Liewer, K. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gorham, PW (reprint author), Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA. RI Vieregg, Abigail/D-2287-2012; Belov, Konstantin/D-2520-2013; Beatty, James/D-9310-2011 OI Beatty, James/0000-0003-0481-4952 NR 4 TC 32 Z9 32 U1 0 U2 7 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD FEB 6 PY 2012 VL 85 IS 4 AR 049901 DI 10.1103/PhysRevD.85.049901 PG 2 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 887QM UT WOS:000299943600013 ER PT J AU Osterstrom, FF Nielsen, OJ Andersen, MPS Wallington, TJ AF Osterstrom, Freja From Nielsen, Ole John Andersen, Mads P. Sulbaek Wallington, Timothy J. TI Atmospheric chemistry of CF3CH2OCH3: Reaction with chlorine atoms and OH radicals, kinetics, degradation mechanism and global warming potential SO CHEMICAL PHYSICS LETTERS LA English DT Article ID STRATOSPHERIC OZONE; HYDROFLUOROCARBONS; AIR; HYDROFLUOROETHERS; ACETYLENE; SERIES; ETHERS; 295-K AB FTIR smog chamber techniques were used to measure k(Cl + CF3CH2OCH3) = (2.28 +/- 0.44) x 10(-11) and k(OH + CF3CH2OCH3) = (4.9 +/- 1.3) x 10(-13) cm(3) molecule(-1) s(-1) in 700 Torr total pressure of air at 296 +/- 2 K. The atmospheric lifetime of CF3CH2OCH3 is estimated at 25 days. Reaction of Cl atoms with CF3CH2OCH3 proceeds 79 +/- 4% at the -CH3 group and 22 +/- 2% at the -CH2- group. Reaction with OH radicals proceeds 55 +/- 5% at the -CH3 group yielding CF3CH2OCHO and 45 +/- 5% at the -CH2- group yielding COF2 and CH3OCHO as primary oxidation products. The infrared spectrum of CF3CH(O)OCH3 was measured and a global warming potential GWP(100) = 8 was estimated. The atmospheric chemistry and environmental impact of CF3CH2OCH3 is discussed in context of the use of hydrofluoroethers as CFC substitutes. (C) 2011 Elsevier B. V. All rights reserved. C1 [Osterstrom, Freja From; Nielsen, Ole John] Univ Copenhagen, Dept Chem, Copenhagen Ctr Atmospher Res, DK-2100 Copenhagen, Denmark. [Andersen, Mads P. Sulbaek] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wallington, Timothy J.] Ford Motor Co, Syst Analyt & Environm Sci Dept, Dearborn, MI 48121 USA. RP Osterstrom, FF (reprint author), Univ Copenhagen, Dept Chem, Copenhagen Ctr Atmospher Res, Univ Pk 5, DK-2100 Copenhagen, Denmark. EM frejafrom@adslhome.dk RI Sulbaek Andersen, Mads/C-4708-2008; Nielsen, Ole/B-9988-2011; Osterstrom, Freja From/E-8646-2015 OI Sulbaek Andersen, Mads/0000-0002-7976-5852; Nielsen, Ole/0000-0002-0088-3937; Osterstrom, Freja From/0000-0003-4125-3365 FU Danish Natural Science Research Council; Villum Kann Rasmussen Foundation; EUROCHAMP2; National Aeronautics and Space Administration FX The authors thank the Danish Natural Science Research Council, the Villum Kann Rasmussen Foundation and EUROCHAMP2, for financial support. We thank S. P. Sander (JPL) for helpful discussions. This work was performed partly at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. M. P. S. A. is supported by an appointment to the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. NR 20 TC 7 Z9 7 U1 0 U2 32 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD FEB 6 PY 2012 VL 524 BP 32 EP 37 DI 10.1016/j.cplett.2011.12.047 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 879GL UT WOS:000299317600006 ER PT J AU Doeringer, D Eldering, A Boone, CD Abad, GG Bernath, PF AF Doeringer, D. Eldering, A. Boone, C. D. Abad, G. Gonzalez Bernath, P. F. TI Observation of sulfate aerosols and SO2 from the Sarychev volcanic eruption using data from the Atmospheric Chemistry Experiment (ACE) SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID INFRARED TRANSMISSION MEASUREMENTS; VERTICAL PROFILES; PINATUBO AEROSOL; OPTICAL-CONSTANTS; EFFECTIVE RADIUS; SURFACE-AREA; EL-CHICHON; SAGE-II; INSTRUMENT; VOLUME AB Infrared spectra measured by the Atmospheric Chemistry Experiment Fourier Transform Spectrometer (ACE-FTS) on the SCISAT satellite were used to analyze the Sarychev volcanic aerosol after the eruption in June 2009. Evidence of the Sarychev eruptions was first detected in July 2009 from enhanced SO2 concentrations and atmospheric extinction. By February 2010, the atmosphere had returned to pre-Sarychev conditions. In July 2009, the volcanic plume was found between 8.5 km and 17.5 km in altitude at mid-and high latitudes (55 degrees N-70 degrees N). The first SO2 and sulfate aerosol retrievals carried out using the infrared solar occultation spectra recorded with the ACE-FTS are presented here. The size distribution parameters, the aerosol volume slant column and the composition of the sulfate aerosol were obtained by using a least squares algorithm. The maximum volume slant column of the aerosols was found to be 850 mu m(3) cm(-3) km, which results in an approximate aerosol loading of 3 mu m(3) cm(-3). One month after the eruption, the composition of the aerosols providing the best-fit is a 75% sulfuric acid-water solution with an effective radius (R-eff) of 0.1-0.3 mu m. C1 [Doeringer, D.] Univ York, Dept Phys, York YO10 5DD, N Yorkshire, England. [Boone, C. D.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. [Eldering, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Abad, G. Gonzalez; Bernath, P. F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Eldering, A.] Univ Calif Los Angeles, Dept Atmospher Sci, Los Angeles, CA 90024 USA. RP Doeringer, D (reprint author), Univ York, Dept Phys, York YO10 5DD, N Yorkshire, England. EM dd557@york.ac.uk RI Bernath, Peter/B-6567-2012; OI Bernath, Peter/0000-0002-1255-396X; Gonzalez Abad, Gonzalo/0000-0002-8090-6480 FU Canadian Space Agency; UK Natural Environment Research Council (NERC) through the National Centre for Earth Observation (NCEO); NASA FX The ACE mission is funded primarily by the Canadian Space Agency. Some funding was provided by the UK Natural Environment Research Council (NERC) through the National Centre for Earth Observation (NCEO). Work at the Jet Propulsion Laboratory, California Institute of Technology was carried out under contract with NASA. NR 36 TC 15 Z9 15 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 FEB 4 PY 2012 VL 117 AR D03203 DI 10.1029/2011JD016556 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 887WB UT WOS:000299961100001 ER PT J AU Hurley, DM Gladstone, GR Stern, SA Retherford, KD Feldman, PD Pryor, W Egan, AF Greathouse, TK Kaufmann, DE Steffl, AJ Parker, JW Miles, PF Horvath, D Davis, MW Versteeg, MH Slater, DC Hendrix, AR Hibbitts, CA Ernst, CM Vervack, RJ Grieves, GA AF Hurley, Dana M. Gladstone, G. Randall Stern, S. Alan Retherford, Kurt D. Feldman, Paul D. Pryor, Wayne Egan, Anthony F. Greathouse, Thomas K. Kaufmann, David E. Steffl, Andrew J. Parker, Joel William Miles, Paul F. Horvath, David Davis, Michael W. Versteeg, Maarten H. Slater, David C. Hendrix, Amanda R. Hibbitts, Charles A. Ernst, Carolyn M. Vervack, Ronald J., Jr. Grieves, Gregory A. TI Modeling of the vapor release from the LCROSS impact: 2. Observations from LAMP SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LUNAR RADIOMETER OBSERVATIONS; WATER; ICE; VOLATILES; DEPOSITS; SURFACES; MISSION; MERCURY; PLUME; MOON AB Using a Monte Carlo model, we analyze the evolution of the vapor plume emanating from the Lunar Crater Observation and Sensing Satellite (LCROSS) impact into Cabeus as seen by the Lyman Alpha Mapping Project (LAMP), a far-ultraviolet (FUV) imaging spectrograph onboard the Lunar Reconnaissance Orbiter. The best fit to the data utilizes a bulk velocity between 3.0 and 4.0 km/s. The fits to the light curve comprised of Hg, Ca, and Mg are not strongly dependent on the temperature. In contrast, the best fit to the light curve from H-2 and CO corresponds to a 500 K thermal velocity distribution. The LAMP field of view primarily encounters particles released at low angles to the horizontal and misses fast moving particles released at more vertical angles. The isotropic model suggests that 117 +/- 16 kg H-2, 41 +/- 3 kg CO, 16 +/- 1 kg Ca, 12.4 +/- 0.8 kg Hg, and 3.8 +/- 0.3 kg Mg are released by the LCROSS impact. Additional errors could arise from an anisotropic plume, which cannot be distinguished with LAMP data. Mg and Ca are likely incompletely volatilized owing to their high vapor temperatures. The highly volatile components (H-2 and CO) might derive from a greater mass of material. To agree with predicted abundances by weight of 0.047%, 0.023%, 11%, 0.28% and 3.4% for H-2, CO, Ca, Hg, and Mg, respectively, the species would be released from 250,000 kg, 180,000 kg, 140 kg, 4400 kg, and 110 kg of regolith, respectively. This is consistent with the relative volatility of these species. C1 [Hurley, Dana M.; Hibbitts, Charles A.; Ernst, Carolyn M.; Vervack, Ronald J., Jr.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA. [Gladstone, G. Randall; Retherford, Kurt D.; Greathouse, Thomas K.; Miles, Paul F.; Horvath, David; Davis, Michael W.; Versteeg, Maarten H.; Slater, David C.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78238 USA. [Stern, S. Alan; Egan, Anthony F.; Kaufmann, David E.; Steffl, Andrew J.; Parker, Joel William] SW Res Inst, Space Sci & Engn Div, Boulder, CO 80302 USA. [Feldman, Paul D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Pryor, Wayne] Cent Arizona Coll, Dept Sci, Coolidge, AZ 85128 USA. [Hendrix, Amanda R.] CALTECH, Jet Prop Lab, Planetary Sci Sect, Pasadena, CA 91109 USA. [Grieves, Gregory A.] Georgia Inst Technol, Sch Chem, Atlanta, GA 30332 USA. RP Hurley, DM (reprint author), Johns Hopkins Univ, Appl Phys Lab, Dept Space, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM dana.hurley@jhuapl.edu RI Ernst, Carolyn/I-4902-2012; Hurley, Dana/F-4488-2015; Vervack, Ronald/C-2702-2016; Hibbitts, Charles/B-7787-2016; OI Hurley, Dana/0000-0003-1052-1494; Vervack, Ronald/0000-0002-8227-9564; Hibbitts, Charles/0000-0001-9089-4391; Retherford, Kurt/0000-0001-9470-150X; Greathouse, Thomas/0000-0001-6613-5731 FU NASA Lunar Reconnaissance Orbiter; NASA Lunar Science Institute [NNA09DB31A] FX This work was supported by NASA Lunar Reconnaissance Orbiter and by the NASA Lunar Science Institute through grant NNA09DB31A. We thank the referees and editors for helpful comments. NR 36 TC 9 Z9 9 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB 4 PY 2012 VL 117 AR E00H07 DI 10.1029/2011JE003841 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 887UQ UT WOS:000299956700001 ER PT J AU Xia, YL Mitchell, K Ek, M Sheffield, J Cosgrove, B Wood, E Luo, LF Alonge, C Wei, HL Meng, J Livneh, B Lettenmaier, D Koren, V Duan, QY Mo, K Fan, Y Mocko, D AF Xia, Youlong Mitchell, Kenneth Ek, Michael Sheffield, Justin Cosgrove, Brian Wood, Eric Luo, Lifeng Alonge, Charles Wei, Helin Meng, Jesse Livneh, Ben Lettenmaier, Dennis Koren, Victor Duan, Qingyun Mo, Kingtse Fan, Yun Mocko, David TI Continental-scale water and energy flux analysis and validation for the North American Land Data Assimilation System project phase 2 (NLDAS-2): 1. Intercomparison and application of model products SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SURFACE PARAMETERIZATION SCHEMES; LATITUDE HYDROLOGICAL PROCESSES; CONTERMINOUS UNITED-STATES; SOUTHERN GREAT-PLAINS; MESOSCALE ETA-MODEL; TORNE-KALIX BASIN; RIVER-BASIN; PILPS PHASE-2(E); PRECIPITATION; SIMULATION AB Results are presented from the second phase of the multiinstitution North American Land Data Assimilation System (NLDAS-2) research partnership. In NLDAS, the Noah, Variable Infiltration Capacity, Sacramento Soil Moisture Accounting, and Mosaic land surface models (LSMs) are executed over the conterminous U.S. (CONUS) in realtime and retrospective modes. These runs support the drought analysis, monitoring and forecasting activities of the National Integrated Drought Information System, as well as efforts to monitor large-scale floods. NLDAS-2 builds upon the framework of the first phase of NLDAS (NLDAS-1) by increasing the accuracy and consistency of the surface forcing data, upgrading the land surface model code and parameters, and extending the study from a 3-year (1997-1999) to a 30-year (1979-2008) time window. As the first of two parts, this paper details the configuration of NLDAS-2, describes the upgrades to the forcing, parameters, and code of the four LSMs, and explores overall model-to-model comparisons of land surface water and energy flux and state variables over the CONUS. Focusing on model output rather than on observations, this study seeks to highlight the similarities and differences between models, and to assess changes in output from that seen in NLDAS-1. The second part of the two-part article focuses on the validation of model-simulated streamflow and evaporation against observations. The results depict a higher level of agreement among the four models over much of the CONUS than was found in the first phase of NLDAS. This is due, in part, to recent improvements in the parameters, code, and forcing of the NLDAS-2 LSMs that were initiated following NLDAS-1. However, large inter-model differences still exist in the northeast, Lake Superior, and western mountainous regions of the CONUS, which are associated with cold season processes. In addition, variations in the representation of sub-surface hydrology in the four LSMs lead to large differences in modeled evaporation and subsurface runoff. These issues are important targets for future research by the land surface modeling community. Finally, improvement from NLDAS-1 to NLDAS-2 is summarized by comparing the streamflow measured from U. S. Geological Survey stream gauges with that simulated by four NLDAS models over 961 small basins. C1 [Xia, Youlong; Mitchell, Kenneth; Ek, Michael; Wei, Helin; Meng, Jesse] NOAA, Environm Modeling Ctr, Natl Ctr Environm & Predict, Camp Springs, MD 20746 USA. [Xia, Youlong; Wei, Helin; Meng, Jesse] NCEP EMC, IMSG, Camp Springs, MD USA. [Sheffield, Justin; Wood, Eric] Princeton Univ, Dept Environm & Civil Engn, Princeton, NJ 08544 USA. [Cosgrove, Brian; Koren, Victor] NOAA, Off Hydrol Dev, Natl Weather Serv, Silver Spring, MD 20910 USA. [Luo, Lifeng] Michigan State Univ, Dept Geog, E Lansing, MI 48824 USA. [Alonge, Charles] AWS Truewind LLC, Albany, NY 12205 USA. [Livneh, Ben; Lettenmaier, Dennis] Univ Washington, Dept Environm & Civil Engn, Seattle, WA 98195 USA. [Duan, Qingyun] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China. [Mo, Kingtse] NOAA, Climate Predict Ctr, Natl Ctr Environm & Predict, Camp Springs, MD 20746 USA. [Fan, Yun] NOAA, Natl Weather Serv, Off Sci & Technol, Silver Spring, MD 20910 USA. [Mocko, David] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20715 USA. [Mocko, David] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20715 USA. RP Xia, YL (reprint author), NOAA, Environm Modeling Ctr, Natl Ctr Environm & Predict, 5200 Auth Rd, Camp Springs, MD 20746 USA. EM Youlong.Xia@noaa.gov RI lettenmaier, dennis/F-8780-2011; Duan, Qingyun/C-7652-2011; Livneh, Ben/I-2939-2015 OI lettenmaier, dennis/0000-0003-3317-1327; Duan, Qingyun/0000-0001-9955-1512; FU NOAA/CPO/CPPA FX This work was supported by the NOAA/CPO/CPPA core project. NR 59 TC 196 Z9 197 U1 2 U2 52 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 3 PY 2012 VL 117 AR D03109 DI 10.1029/2011JD016048 PG 27 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 887VW UT WOS:000299960500001 ER PT J AU Czaja, AD Johnson, CM Yamaguchi, KE Beard, BL AF Czaja, Andrew D. Johnson, Clark M. Yamaguchi, Kosei E. Beard, Brian L. TI Comment on "Abiotic Pyrite Formation Produces a Large Fe Isotope Fractionation" SO SCIENCE LA English DT Editorial Material ID BLACK-SEA; IRON; SEDIMENTS; EARTH C1 [Czaja, Andrew D.; Johnson, Clark M.; Beard, Brian L.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Czaja, Andrew D.; Johnson, Clark M.; Yamaguchi, Kosei E.; Beard, Brian L.] NASA, Astrobiol Inst, Washington, DC USA. [Yamaguchi, Kosei E.] Toho Univ, Dept Chem, Funabashi, Chiba 2748510, Japan. RP Czaja, AD (reprint author), Univ Wisconsin, Dept Geosci, 1215 W Dayton St, Madison, WI 53706 USA. EM aczaja@geology.wisc.edu NR 15 TC 6 Z9 7 U1 1 U2 20 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 3 PY 2012 VL 335 IS 6068 DI 10.1126/science.1211804 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 885HI UT WOS:000299769200024 PM 22301304 ER PT J AU Fassett, CI Head, JW Kadish, SJ Mazarico, E Neumann, GA Smith, DE Zuber, MT AF Fassett, C. I. Head, J. W. Kadish, S. J. Mazarico, E. Neumann, G. A. Smith, D. E. Zuber, M. T. TI Lunar impact basins: Stratigraphy, sequence and ages from superposed impact crater populations measured from Lunar Orbiter Laser Altimeter (LOLA) data SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LATE HEAVY BOMBARDMENT; INNER SOLAR-SYSTEM; CATACLYSM IMPACTORS; ORIGIN; CONSTRAINTS; MOON; SATURATION; CHRONOLOGY; MISSION; EARTH AB Impact basin formation is a fundamental process in the evolution of the Moon and records the history of impactors in the early solar system. In order to assess the stratigraphy, sequence, and ages of impact basins and the impactor population as a function of time, we have used topography from the Lunar Orbiter Laser Altimeter (LOLA) on the Lunar Reconnaissance Orbiter (LRO) to measure the superposed impact crater size-frequency distributions for 30 lunar basins (D >= 300 km). These data generally support the widely used Wilhelms sequence of lunar basins, although we find significantly higher densities of superposed craters on many lunar basins than derived by Wilhelms (50% higher densities). Our data also provide new insight into the timing of the transition between distinct crater populations characteristic of ancient and young lunar terrains. The transition from a lunar impact flux dominated by Population 1 to Population 2 occurred before the mid-Nectarian. This is before the end of the period of rapid cratering, and potentially before the end of the hypothesized Late Heavy Bombardment. LOLA-derived crater densities also suggest that many Pre-Nectarian basins, such as South Pole-Aitken, have been cratered to saturation equilibrium. Finally, both crater counts and stratigraphic observations based on LOLA data are applicable to specific basin stratigraphic problems of interest; for example, using these data, we suggest that Serenitatis is older than Nectaris, and Humboldtianum is younger than Crisium. Sample return missions to specific basins can anchor these measurements to a Pre-Imbrian absolute chronology. C1 [Fassett, C. I.; Head, J. W.; Kadish, S. J.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Mazarico, E.; Neumann, G. A.; Smith, D. E.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Smith, D. E.; Zuber, M. T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Fassett, C. I.] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. RP Fassett, CI (reprint author), Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. EM cfassett@mtholyoke.edu RI Neumann, Gregory/I-5591-2013; Mazarico, Erwan/N-6034-2014; OI Neumann, Gregory/0000-0003-0644-9944; Mazarico, Erwan/0000-0003-3456-427X; Fassett, Caleb/0000-0001-9155-3804 FU Lunar Reconnaissance Orbiter Project; Lunar Orbiter Laser Altimeter team [NNX09AM54G] FX We would like to thank Clark Chapman, Matija Cuk and Stephanie Werner for detailed reviews that helped improve the manuscript. Thanks are extended to the Lunar Reconnaissance Orbiter Project and the Lunar Orbiter Laser Altimeter team for funding (NNX09AM54G) to JWH. NR 60 TC 33 Z9 34 U1 0 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB 2 PY 2012 VL 117 AR E00H06 DI 10.1029/2011JE003951 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 887UM UT WOS:000299956200001 ER PT J AU Johnson, LF Trout, TJ AF Johnson, Lee F. Trout, Thomas J. TI Satellite NDVI Assisted Monitoring of Vegetable Crop Evapotranspiration in California's San Joaquin Valley SO REMOTE SENSING LA English DT Article DE crop coefficient; water use; NDVI; Landsat; fractional cover ID WATER-USE; VEGETATION INDEX; SEMIARID REGION; SHADED AREA; COEFFICIENTS; REFLECTANCE; CANOPY; WHEAT; CORN; ALGORITHM AB Reflective bands of Landsat-5 Thematic Mapper satellite imagery were used to facilitate the estimation of basal crop evapotranspiration (ETcb), or potential crop water use, in San Joaquin Valley fields during 2008. A ground-based digital camera measured green fractional cover (Fc) of 49 commercial fields planted to 18 different crop types (row crops, grains, orchard, vineyard) of varying maturity over 11 Landsat overpass dates. Landsat L1T terrain-corrected images were transformed to surface reflectance and converted to normalized difference vegetation index (NDVI). A strong linear relationship between NDVI and Fc was observed (r(2) = 0.96, RMSE = 0.062). The resulting regression equation was used to estimate Fc for crop cycles of broccoli, bellpepper, head lettuce, and garlic on nominal 7-9 day intervals for several study fields. Prior relationships developed by weighing lysimeter were used to transform Fc to fraction of reference evapotranspiration, also known as basal crop coefficient (Kcb). Measurements of grass reference evapotranspiration from the California Irrigation Management Information System were then used to calculate ETcb for each overpass date. Temporal profiles of Fc, Kcb, and ETcb were thus developed for the study fields, along with estimates of seasonal water use. Daily ETcb retrieval uncertainty resulting from error in satellite-based Fc estimation was <0.5 mm/d, with seasonal uncertainty of 6-10%. Results were compared with FAO-56 irrigation guidelines and prior lysimeter observations for reference. C1 [Johnson, Lee F.] Calif State Univ, Div Sci & Environm Policy, Seaside, CA 93955 USA. [Johnson, Lee F.] NASA, Div Earth Sci, Ames Res Ctr, Moffett Field, CA 94035 USA. [Trout, Thomas J.] USDA ARS, Water Management Res Unit, Ft Collins, CO 80526 USA. RP Johnson, LF (reprint author), Calif State Univ, Div Sci & Environm Policy, Seaside, CA 93955 USA. EM Lee.F.Johnson@nasa.gov; Thomas.Trout@ars.usda.gov OI Trout, Thomas/0000-0003-1896-9170 FU California Dept. Water Resources; NASA's Applied Sciences Program FX Field support was provided by Jim Gartung (USDA-ARS). LEDAPS atmospheric correction processing was facilitated by the NASA Ames Ecological Forecasting Lab. We are grateful for cooperation of commercial growers at Tanimura & Antle, Red Rock Ranch, Britz, Terranova, and Harris Farms. The project was funded by the California Dept. Water Resources. LJ received additional support through NASA's Applied Sciences Program. NR 35 TC 30 Z9 30 U1 3 U2 26 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD FEB PY 2012 VL 4 IS 2 BP 439 EP 455 DI 10.3390/rs4020439 PG 17 WC Remote Sensing SC Remote Sensing GA 978PL UT WOS:000306756400006 ER PT J AU Coustenis, A Atreya, S Castillo, J Coll, P Mueller-Wodarg, I Spilker, L AF Coustenis, A. Atreya, S. Castillo, J. Coll, P. Mueller-Wodarg, I. Spilker, L. TI Surfaces, atmospheres and magnetospheres of the outer planets and their satellites and ring systems: Part VII Preface SO PLANETARY AND SPACE SCIENCE LA English DT Editorial Material C1 [Coustenis, A.] LESIA, Paris Meudon Observ, F-92195 Meudon, France. [Atreya, S.] Univ Michigan, Ann Arbor, MI 48109 USA. [Castillo, J.] CALTECH, JPL, Pasadena, CA 91125 USA. [Coll, P.] Univ Paris 07, LISA, Univ Paris Est Creteil, Creteil, France. [Mueller-Wodarg, I.] Univ London Imperial Coll Sci Technol & Med, London, England. [Spilker, L.] Jet Prop Lab, Pasadena, CA USA. [Coll, P.] Hop Henri Mondor, CNRS, F-94010 Creteil, France. RP Coustenis, A (reprint author), LESIA, Paris Meudon Observ, F-92195 Meudon, France. RI Mueller-Wodarg, Ingo/M-9945-2014 OI Mueller-Wodarg, Ingo/0000-0001-6308-7826 NR 0 TC 1 Z9 1 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD FEB PY 2012 VL 61 IS 1 SI SI BP 1 EP 2 DI 10.1016/j.pss.2011.12.014 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971IY UT WOS:000306198800001 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 Saturn's magnetosphere interaction with Titan for T9 encounter: 3D hybrid modeling and comparison with CAPS observations SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Ionospheres; Atmospheres; Induced magnetospheres; Magnetic barrier; Alfven wing; Plasma modeling ID PLASMA ENVIRONMENT; SOLAR-WIND; MHD MODEL; SIMULATION; IONS; SPECTROMETER; IONOSPHERE; ATOMS; COMET; SHOCK AB Global dynamics of ionized and neutral gases in the environment of Titan plays an important role in the interaction of Saturn's magnetosphere with Titan. Several hybrid simulations of this problem have already been done (Brecht et al., 2000; Kallio et al., 2004; Modolo et al., 2007a; Simon et al., 2007a, 2007b; Modolo and Chanteur, 2008). Observational data from CAPS for the 19 encounter (Sittler et al., 2009) indicates an absence of 0 heavy ions in the upstream that change the models of interaction which were discussed in current publications (Kallio et al., 2004; Modolo et al., 2007a; Simon et al., 2007a, 20076; Ma et al., 2007; Szego et al., 2007). Further analysis of the CAPS data shows very low density or even an absence of H+ ions in upstream. In this paper we discuss two models of the interaction of Saturn's magnetosphere with Titan: (A) high density of H ions in the upstream flow (0.1 cm(-3)), and (B) low density of H+ ions in the upstream flow (0.02 cm(-3)). The hybrid model employs a fluid description for electrons and neutrals, whereas a particle approach is used for ions. We also take into account charge-exchange and photoionization processes and solve self-consistently for electric and magnetic fields. The model atmosphere includes exospheric H+, H-2(+), N-2(+) and CH4+ pickup ion production as well as an immobile background ionosphere and a shell distribution for active ionospheric ions (M-i=28 amu). The hybrid model allows us to account for the realistic anisotropic ion velocity distribution that cannot be done in fluid simulations with isotropic temperatures. Our simulation shows an asymmetry of the ion density distribution and the magnetic field, including the formation of Alfven wing-like structures. The results of the ion dynamics in Titan's environment are compared with Cassini T9 encounter data (CAPS). (C) 2011 Elsevier Ltd. All rights reserved. C1 [Lipatov, A. S.; Sittler, E. C., Jr.; Hartle, R. E.; Cooper, J. F.; Simpson, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lipatov, A. S.] Univ Maryland Baltimore Cty, Goddard Planetary & Heliophys Inst, Baltimore, MD 21228 USA. [Lipatov, A. S.] Russian Acad Sci, AA Dorodnitsyn Comp Ctr, Moscow 119991, Russia. [Lipatov, A. S.] Moscow Inst Phys & Technol, Fac Problems Phys & Power Engn, Moscow, Russia. RP Lipatov, AS (reprint author), NASA, Goddard Space Flight Ctr, Code 673,Bldg 21,Room 247,8800 Greenbelt Rd, 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 [08-CDAP08-0043]; GPHI/(GEST Center) UMBC [900-37-172, 670-90-315]; NASA GSFC [900-37-172, 670-90-315]; NASA Ames Advanced Supercomputing (NAS) Division [SMD-09-1124, SMD-10-1517] 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). A.S.L. was also supported in part by the Grants/Tasks 900-37-172 and 670-90-315 between the GPHI/(GEST Center) UMBC and NASA GSFC. Computational resources were provided by the NASA Ames Advanced Supercomputing (NAS) Division (Projects SMD-09-1124 and SMD-10-1517). The authors thank the referees for fruitful comments. NR 42 TC 5 Z9 5 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD FEB PY 2012 VL 61 IS 1 SI SI BP 66 EP 78 DI 10.1016/j.pss.2011.08.017 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971IY UT WOS:000306198800008 ER PT J AU Stephan, K Jaumann, R Wagner, R Clark, RN Cruikshank, DP Giese, B Hibbitts, CA Roatsch, T Matz, KD Brown, RH Filacchione, G Cappacioni, F Scholten, F Buratti, BJ Hansen, GB Nicholson, PD Baines, KH Nelson, RM Matson, DL AF Stephan, Katrin Jaumann, Ralf Wagner, Roland Clark, Roger N. Cruikshank, Dale P. Giese, Bernd Hibbitts, Charles A. Roatsch, Thomas Matz, Klaus-Dieter Brown, Robert H. Filacchione, Gianrico Cappacioni, Fabrizio Scholten, F. Buratti, Bonnie J. Hansen, Gary B. Nicholson, Phil D. Baines, Kevin H. Nelson, Robert M. Matson, Dennis L. TI The Saturnian satellite Rhea as seen by Cassini VIMS SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Rhea; Icy satellites; Spectroscopy; Surfaces; Cassini/VIMS ID OUTER SOLAR-SYSTEM; E-RING; ENCELADUS SURFACE; IMAGING SCIENCE; ICY SATELLITES; MAGNETOSPHERE; SPECTROMETER; IAPETUS; PARTICLES; DYNAMICS AB Since the arrival of the Cassini spacecraft at Saturn in June 2004, the Visual and Infrared Mapping Spectrometer has obtained new spectral data of the icy satellites of Saturn in the spectral range from 0.35 to 5.2 mu m. Numerous flybys were performed at Saturn's second largest satellite Rhea, providing a nearly complete coverage with pixel-ground resolutions sufficient to analyze variations of spectral properties across Rhea's surface in detail. We present an overview of the VIMS observations obtained so far, as well as the analysis of the spectral properties identified in the VIMS spectra and their variations across its surface compared with spatially highly resolved Cassini ISS images and digital elevation models. Spectral variations measured across Rhea's surface are similar to the variations observed in the VIMS observations of its neighbor Dione, implying similar processes causing or at least inducing their occurrence. Thus, magnetospheric particles and dust impacting onto the trailing hemisphere appear to be responsible for the concentration of dark rocky/organic material and minor amounts of CO2 in the cratered terrain on the trailing hemisphere. Despite the prominent spectral signatures of Rhea's fresh impact crater Inktomi, radiation effects were identified that also affect the H2O ice-rich cratered terrain of the leading hemisphere. The concentration of H2O ice in the vicinity of steep tectonic scarps near 270 degrees W and geologically fresh impact craters implies that Rhea exhibits an icy crust at least in the upper few kilometers. Despite the evidence for past tectonic events, no indications of recent endogenically powered processes could be identified in the Cassini data. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Stephan, Katrin; Jaumann, Ralf; Wagner, Roland; Giese, Bernd; Roatsch, Thomas; Matz, Klaus-Dieter; Scholten, F.] DLR, Inst Planetary Res, D-12489 Berlin, Germany. [Jaumann, Ralf] Free Univ Berlin, FR Planetol & Fernerkundung, D-12249 Berlin, Germany. [Clark, Roger N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA. [Cruikshank, Dale P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hibbitts, Charles A.] JHU Appl Phys Lab, Laurel, MD USA. [Brown, Robert H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Filacchione, Gianrico; Cappacioni, Fabrizio] INAF IASF, Rome, Italy. [Buratti, Bonnie J.; Nelson, Robert M.; Matson, Dennis L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hansen, Gary B.] Univ Washington, Seattle, WA 98195 USA. [Nicholson, Phil D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Baines, Kevin H.] Univ Wisconsin, SSEC, Madison, WI 53706 USA. RP Stephan, K (reprint author), DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany. EM Katrin.Stephan@dlr.de RI Hibbitts, Charles/B-7787-2016; OI Hibbitts, Charles/0000-0001-9089-4391; Filacchione, Gianrico/0000-0001-9567-0055 FU DLR; Helmholtz Alliance 'Planetary evolution and Life' FX We gratefully acknowledge the many years of work of the entire Cassini team that allowed these data to be obtained. We want to thank E. Hoffmann for his support with the data processing. This work has been partly supported by DLR and the Helmholtz Alliance 'Planetary evolution and Life'. NR 88 TC 17 Z9 17 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD FEB PY 2012 VL 61 IS 1 SI SI BP 142 EP 160 DI 10.1016/j.pss.2011.07.019 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971IY UT WOS:000306198800016 ER PT J AU Orton, GS Fletcher, LN Liu, JJ Schneider, T Yanamandra-Fisher, PA de Pater, I Edwards, M Geballe, TR Hammel, HB Fujiyoshi, T Encrenaz, T Pantin, E Mousis, O Fuse, T AF Orton, Glenn S. Fletcher, Leigh N. Liu, Junjun Schneider, Tapio Yanamandra-Fisher, Padma A. de Pater, Imke Edwards, Michelle Geballe, Thomas R. Hammel, Heidi B. Fujiyoshi, Takuya Encrenaz, Therese Pantin, Eric Mousis, Olivier Fuse, Tetsuharu TI Recovery and characterization of Neptune's near-polar stratospheric hot spot SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Neptune; Stratosphere; Temperature; Dynamics; Radiative heating ID MIDINFRARED IMAGER; JUPITER; TEMPERATURES; SPECTROMETER; ATMOSPHERE AB Images of Neptune obtained in 2006 at ESO's Very Large Telescope (Orton et al., 2007, Astronomy & Astrophysics 473, L5) revealed a near-polar hot spot near 70 degrees S latitude that was detectable in filters sampling both stratospheric methane (7 mu m) and ethane (similar to 12 mu m) emission. Such a feature was not present in 2003 Keck and 2005 Gemini North observations, which showed only a general warming trend toward Neptune's pole that was longitudinally homogeneous. Because of the paucity of longitudinal sampling in the 2003,2005 and 2006 images, it was not clear whether the failure to see this phenomenon in 2003 and 2005 was simply the result of insufficient longitudinal sampling or whether the phenomenon was truly variable in time. To unravel these two possibilities, we made follow-up observations on large telescopes that were capable of resolving Neptune at thermal-infrared wavelengths: Gemini South in 2007 and 2010 using the T-ReCS instrument, Subaru in 2008 using the COMICS instrument and VLT in 2008 and 2009 using the VISIR instrument. Two serendipitous T-ReCS images of Neptune were also obtained in 2007 using a broad N-band (8-14 mu m) filter, whose radiance is dominated by stratospheric emission from both methane and ethane. The feature was recovered (i) in 2007 with T-ReCS in the broad N-band image and (ii) in 2008 with COMICS in a 12.5-mu m image. However, T-ReCS observations in 2010 that covered up to 250 degrees of longitude did not show evidence of an off-polar hot spot. Although we have not definitively ruled out the possibility that various observers have simply missed a semi-permanent feature, it seems statistically very unlikely to be the case. With only 3 sightings in 13 independent observing epochs, it is likely that the phenomenon is ephemeral in time. A possible origin for the phenomenon is a large planetary wave that is dynamically confined to the high-latitude regions characterized by prograde zonal winds. It may be episodically excited by dynamical activity deeper in the atmosphere. This must be coupled with mixing near the poles that destroys or at least substantially attenuates the hot spot over the south pole that leads to an appearance of the typical polar stratospheric hot spot being offset in latitude. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Orton, Glenn S.; Yanamandra-Fisher, Padma A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fletcher, Leigh N.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [Liu, Junjun; Schneider, Tapio] CALTECH, Pasadena, CA 91125 USA. [de Pater, Imke] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Edwards, Michelle] Gemini Observ, La Serena, Chile. [Geballe, Thomas R.] Gemini Observ, Hilo, HI 96720 USA. [Hammel, Heidi B.] Space Sci Inst, Ridgefield, CT 06877 USA. [Fujiyoshi, Takuya] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Encrenaz, Therese] Observ Paris, LESIA, F-92195 Meudon, France. [Pantin, Eric] Ctr Etud Atom, F-91190 Gif Sur Yvette, France. [Mousis, Olivier] Univ Franche Comte, CNRS UMR 6213, Inst UTINAM, Observ Sci Univers THETA, F-25010 Besancon, France. [Fuse, Tetsuharu] Natl Inst Informat & Commun Technol, Kashima Space Res Ctr, Ibaraki 3148501, Japan. RP Orton, GS (reprint author), CALTECH, Jet Prop Lab, MS 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Glenn.Orton@jpl.nasa.gov RI Fletcher, Leigh/D-6093-2011; Schneider, Tapio /A-7038-2014 OI Fletcher, Leigh/0000-0001-5834-9588; Schneider, Tapio /0000-0001-5687-2287 FU NSF [AST-0908575]; University of Oxford; David and Lucile Packard Fellowship; NASA [NNX10AQ05G]; National Astronomical Observatory of Japan; Gemini Observatory; National Science Foundation (United States); Science and Technology Facilities Council (United Kingdom); National Research Council (Canada); CONICYT (Chile); Australian Research Council (Australia); Ministrio da Cinica e Tecnologia (Brazil); Ministerio de Cienica, Tecnologia e Innovacin Productiva (Argentina); European Southern Observatory telescopes [081C-0496, 083C-0163]; Subaru Telescope [S08-032]; Gemini North Telescope [GN-2007B-A-105]; Gemini South Telescope [GS-2007B-Q-47, GS-2010B-A-42] FX We thank Erich Karkoschka for helpful comments. Orton and Yanamandra-Fisher conducted a portion of this research at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. They thank Mark Hofstadter, the Principal Investigator of the relevant program, for this support. De Pater was supported by NSF Grant AST-0908575. Fletcher was supported by a Glasstone Science Fellowship at the University of Oxford. Schneider and Liu acknowledge support by a David and Lucile Packard Fellowship and by the NASA Outer Planets Research Program (Grant NNX10AQ05G). Fujiyoshi and Fuse were supported by the National Astronomical Observatory of Japan. Edwards and Geballe were supported by the Gemini Observatory, on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministrio da Cinica e Tecnologia (Brazil) and Ministerio de Cienica, Tecnologia e Innovacin Productiva (Argentina). The simulations on which Fig. 5 is based were performed on Caltech's Division of Geological and Planetary Sciences Dell cluster.; The new results presented in this paper were based, in part, on observations made at the European Southern Observatory telescopes, in programs 081C-0496(A) and 083C-0163(A) and (B), obtained from the ESO/ST-ECF Science Archive Facility; on data collected at Subaru Telescope in program ID S08-032, which is operated by the National Astronomical Observatory of Japan: and on data obtained from the Gemini North Telescope in program GN-2007B-A-105 and the Gemini South Telescope in programs GS-2007B-Q-47, GS-2010B-A-42, which are operated by the Association of Universities for Research in Astronomy. (C) 2010. All rights reserved. NR 25 TC 7 Z9 7 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD FEB PY 2012 VL 61 IS 1 SI SI BP 161 EP 167 DI 10.1016/j.pss.2011.06.013 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971IY UT WOS:000306198800017 ER PT J AU Hepp, AF AF Hepp, Aloysius F. TI Untitled SO MATERIALS SCIENCE IN SEMICONDUCTOR PROCESSING LA English DT Editorial Material C1 NASA Glenn Res Ctr, Cleveland, OH USA. RP Hepp, AF (reprint author), NASA Glenn Res Ctr, Cleveland, OH USA. EM matscisemiproc@gmail.com NR 0 TC 0 Z9 0 U1 1 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1369-8001 J9 MAT SCI SEMICON PROC JI Mater. Sci. Semicond. Process PD FEB PY 2012 VL 15 IS 1 BP 1 EP 1 DI 10.1016/j.mssp.2012.03.016 PG 1 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA 956TL UT WOS:000305111900001 ER PT J AU Ramsey, BD Gaskin, JA Elsner, RF Chen, W Carini, GA De Geronimo, G Keister, J Li, S Li, Z Siddons, DP Smith, G AF Ramsey, B. D. Gaskin, J. A. Elsner, R. F. Chen, W. Carini, G. A. De Geronimo, G. Keister, J. Li, S. Li, Z. Siddons, D. P. Smith, G. TI A low-power, radiation-resistant, Silicon-Drift-Detector array for extraterrestrial element mapping SO JOURNAL OF INSTRUMENTATION LA English DT Article DE Solid state detectors; X-ray detectors and telescopes ID ICY GALILEAN SATELLITES; X-RAY SPECTROMETERS; CMOS TECHNOLOGIES; EUROPAS OCEAN; SURFACE; ORIGIN; TORUS AB We are developing a modular Silicon Drift Detector (SDD) X-Ray Spectrometer (XRS) for measuring the abundances of light surface elements (C to Fe) fluoresced by ambient radiation on remote airless bodies. The value of fluorescence spectrometry for surface element mapping is demonstrated by its inclusion on three recent lunar missions and by exciting new data that have recently been announced from the Messenger Mission to Mercury. The SDD-XRS instrument that we have been developing offers excellent energy resolution and an order of magnitude lower power requirement than conventional CCDs, making much higher sensitivities possible with modest spacecraft resources. In addition, it is significantly more radiation resistant than x-ray CCDs and therefore will not be subject to the degradation that befell recent lunar instruments. In fact, the intrinsic radiation resistance of the SDD makes it applicable even to the harsh environment of the Jovian system where it can be used to map the light surface elements of Europa. In this paper, we first discuss our element-mapping science-measurement goals. We then derive the necessary instrument requirements to meet these goals and discuss our current instrument development status with respect to these requirements. C1 [Ramsey, B. D.; Gaskin, J. A.; Elsner, R. F.] NASA, MSFC, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. [Chen, W.; Carini, G. A.; De Geronimo, G.; Keister, J.; Li, S.; Li, Z.; Siddons, D. P.; Smith, G.] Brookhaven Natl Lab, Upton, NY 11973 USA. RP Ramsey, BD (reprint author), NASA, MSFC, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. EM Brian.Ramsey@nasa.gov NR 42 TC 3 Z9 3 U1 0 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-0221 J9 J INSTRUM JI J. Instrum. PD FEB PY 2012 VL 7 AR C02013 DI 10.1088/1748-0221/7/02/C02013 PG 14 WC Instruments & Instrumentation SC Instruments & Instrumentation GA 941CQ UT WOS:000303940900013 ER PT J AU Andrews, RJ AF Andrews, Russell J. TI Nanotechnology and Drug Delivery: Getting There is Only Half of the Challenge! (Commentary) SO CNS & NEUROLOGICAL DISORDERS-DRUG TARGETS LA English DT Editorial Material ID CARBON; STIMULATION; ADENOSINE C1 NASA, Ames Res Ctr, Ames Associate Smart Syst & Nanotechnol, Moffett Field, CA 94035 USA. RP Andrews, RJ (reprint author), NASA, Ames Res Ctr, Ames Associate Smart Syst & Nanotechnol, Moffett Field, CA 94035 USA. EM rja@russelljandrews.org NR 10 TC 3 Z9 3 U1 0 U2 0 PU BENTHAM SCIENCE PUBL LTD PI SHARJAH PA EXECUTIVE STE Y26, PO BOX 7917, SAIF ZONE, 1200 BR SHARJAH, U ARAB EMIRATES SN 1871-5273 J9 CNS NEUROL DISORD-DR JI CNS Neurol. Disord.-Drug Targets PD FEB PY 2012 VL 11 IS 1 BP 96 EP 97 PG 2 WC Neurosciences; Pharmacology & Pharmacy SC Neurosciences & Neurology; Pharmacology & Pharmacy GA 934MW UT WOS:000303449400011 PM 22380465 ER PT J AU Breger, M Hareter, M Endl, M Kuschnig, R Weiss, WW Matthews, JM Guenther, DB Moffat, AFJ Rowe, JF Rucinski, SM Sasselov, D AF Breger, M. Hareter, M. Endl, M. Kuschnig, R. Weiss, W. W. Matthews, J. M. Guenther, D. B. Moffat, A. F. J. Rowe, J. F. Rucinski, S. M. Sasselov, D. TI Delta Scuti stars in the Praesepe cluster observed by the MOST satellite SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE delta Scuti stars; open clusters and associations: individual (Praesepe); stars: individual (BS Cnc, BT Cnc, EP Cnc, HD 73872); stars: oscillations; techniques: photometric ID STACC 1998 CAMPAIGN; BT CANCRI; F-STARS; PHOTOMETRY; SPACE; VARIABILITY; PULSATION AB The Praesepe cluster contains a number of delta Sct and gamma Dor pulsators. Asteroseismology of cluster stars is simplified by the common distance, age and stellar abundances. Since asteroseismology requires a large number of known frequencies, the small pulsation amplitudes of these stars require space satellite campaigns. The present study utilizes photometric MOST satellite measurements in order to determine the pulsation frequencies of two evolved (EP Cnc, BT Cnc) and two main-sequence (BS Cnc, HD 73872) delta Sct stars in the Praesepe cluster. The frequency analysis of the 2008 and 2009 data detected up to 34 frequencies per star with most amplitudes in the submillimag range. In BS Cnc, two modes showed strong amplitude variability between 2008 and 2009. The frequencies ranged from 0.76 to 41.7 cd(-1). After considering the different evolutionary states and mean stellar densities of these four stars, the differences and large ranges in frequency remain. (C) 2012 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Breger, M.; Hareter, M.; Endl, M.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Breger, M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rowe, J. F.] NASA Ames Res Pk, Moffett Field, CA 94035 USA. [Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Breger, M (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria. EM michel.breger@univie.ac.at FU Austrian Fonds zur Forderung der wissenschaftlichen Forschung [P 21830-N16, P 22691-N16] FX This investigation has been supported by the Austrian Fonds zur Forderung der wissenschaftlichen Forschung through projects P 21830-N16 and P 22691-N16. NR 31 TC 6 Z9 6 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2012 VL 333 IS 2 BP 131 EP 137 DI 10.1002/asna.201111640 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932TH UT WOS:000303312900005 ER PT J AU Nessel, JA Acosta, RJ AF Nessel, James A. Acosta, Roberto J. TI Predicting Sparse Array Performance From Two-Element Interferometer Data SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE Arrays; phase noise; propagation measurements; sparse array antennas ID WATER-VAPOR; TURBULENCE; SPECTRUM AB Widely distributed (sparse) ground-based antenna arrays are being considered for deep space communications applications with the development of the proposed Next Generation Deep Space Network. However, atmospheric-induced phase fluctuations can impose daunting restrictions on the performance of such an array, particularly during transmit and particularly at Ka-band frequencies, which have yet to be successfully resolved. In this paper, an analysis of the uncompensated performance of a sparse antenna array, in terms of its directivity and pattern degradation, is performed utilizing real data. The theoretical derivation for array directivity degradation is validated with interferometric measurements (for a 2-element array) recorded at Goldstone, CA, from May 2007-May 2008. With the validity of the model established, an arbitrary 27-element array geometry is defined at Goldstone, CA, to ascertain its theoretical performance in the presence of phase fluctuations based on the measured data. Therein, a procedure in which array directivity performance can be determined based on site-specific interferometric measurements is established. It is concluded that a combination of compact array geometry and atmospheric compensation is necessary to minimize array loss impact for deep space communications. C1 [Nessel, James A.; Acosta, Roberto J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Nessel, JA (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM james.a.nessel@nasa.gov; roberto.j.acosta@nasa.gov FU NASA's Space Communications and Navigation (SCaN) under the Space Operations Mission Directorate (SOMD) FX Manuscript received September 02, 2010; revised March 14, 2011; accepted June 04, 2011. Date of publication October 21, 2011; date of current version February 03, 2012. This work was supported in part by NASA's Space Communications and Navigation (SCaN) Program under the Space Operations Mission Directorate (SOMD). NR 19 TC 1 Z9 1 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-926X J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD FEB PY 2012 VL 60 IS 2 BP 886 EP 894 DI 10.1109/TAP.2011.2173110 PN 2 PG 9 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 924VV UT WOS:000302720300019 ER PT J AU Ajello, M Baldini, L Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Berenji, B Bloom, ED Bonamente, E Borgland, AW Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cecchi, C Charles, E Chekhtman, A Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S de Angelis, A de Palma, F Dermer, CD Silva, EDE Drell, PS Drlica-Wagner, A Enoto, T Favuzzi, C Fegan, SJ Ferrara, EC Fukazawa, Y Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Graham, P Grenier, IA Guiriec, S Gustafsson, M Hadasch, D Hayashida, M Hughes, RE Johnson, AS Kamae, T Katagiri, H Kataoka, J Knodlseder, J Kuss, M Lande, J Latronico, L Lionetto, AM Longo, F Loparco, F Lovellette, MN Lubrano, P Mazziotta, MN Michelson, PF Mitthumsiri, W Mizuno, T Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Norris, JP Nuss, E Ohsugi, T Okumura, A Orlando, E Ormes, JF Ozaki, M Paneque, D Pesce-Rollins, M Pierbattista, M Piron, F Pivato, G Raino, S Razzano, M Ritz, S Roth, M Parkinson, PMS Scargle, JD Schalk, TL Sgro, C Siskind, EJ Spandre, G Spinelli, P Suson, DJ Tajima, H Takahashi, H Tanaka, T Thayer, JG Thayer, JB Tibaldo, L Tinivella, M Torres, DF Troja, E Uchiyama, Y Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Winer, BL Wood, KS Wood, M Yang, Z Zimmer, S AF Ajello, M. Baldini, L. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Berenji, B. Bloom, E. D. Bonamente, E. Borgland, A. W. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cecchi, C. Charles, E. Chekhtman, A. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. de Angelis, A. de Palma, F. Dermer, C. D. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Enoto, T. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Fukazawa, Y. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Graham, P. Grenier, I. A. Guiriec, S. Gustafsson, M. Hadasch, D. Hayashida, M. Hughes, R. E. Johnson, A. S. Kamae, T. Katagiri, H. Kataoka, J. Knoedlseder, J. Kuss, M. Lande, J. Latronico, L. Lionetto, A. M. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Mazziotta, M. N. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Norris, J. P. Nuss, E. Ohsugi, T. Okumura, A. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Pesce-Rollins, M. Pierbattista, M. Piron, F. Pivato, G. Raino, S. Razzano, M. Ritz, S. Roth, M. Parkinson, P. M. Saz Scargle, J. D. Schalk, T. L. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Suson, D. J. Tajima, H. Takahashi, H. Tanaka, T. Thayer, J. G. Thayer, J. B. Tibaldo, L. Tinivella, M. Torres, D. F. Troja, E. Uchiyama, Y. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Winer, B. L. Wood, K. S. Wood, M. Yang, Z. Zimmer, S. TI Limits on large extra dimensions based on observations of neutron stars with the Fermi-LAT SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE extra dimensions; gravity; neutron stars; core-collapse supernovas ID LARGE-AREA TELESCOPE; EGRET; CATALOG AB We present limits for the compactification scale in the theory of Large Extra Dimensions (LED) proposed by Arkani-Hamed, Dimopoulos, and Dvali. We use 11 months of data from the Fermi Large Area Telescope (Fermi-LAT) to set gamma ray flux limits for 6 gamma-ray faint neutron stars (NS). To set limits on LED we use the model of Hannestad and Raffelt (HR) that calculates the Kaluza-Klein (KK) graviton production in supernova cores and the large fraction subsequently gravitationally bound around the resulting NS. The predicted decay of the bound KK gravitons to gamma gamma should contribute to the flux from NSs. Considering 2 to 7 extra dimensions of the same size in the context of the HR model, we use Monte Carlo techniques to calculate the expected differential flux of gamma-rays arising from these KK gravitons, including the effects of the age of the NS, graviton orbit, and absorption of gamma-rays in the magnetosphere of the NS. We compare our Monte Carlo-based differential flux to the experimental differential flux using maximum likelihood techniques to obtain our limits on LED. Our limits are more restrictive than past EGRET-based optimistic limits that do not include these important corrections. Additionally, our limits are more stringent than LHC based limits for 3 or fewer LED, and comparable for 4 LED. We conclude that if the effective Planck scale is around a TeV, then for 2 or 3 LED the compactification topology must be more complicated than a torus. C1 [Ajello, M.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Enoto, T.; Glanzman, T.; Godfrey, G.; Graham, P.; Hayashida, M.; Hughes, R. E.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Orlando, E.; Paneque, D.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Ajello, M.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Enoto, T.; Glanzman, T.; Godfrey, G.; Graham, P.; Hayashida, M.; Hughes, R. E.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Orlando, E.; Paneque, D.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] INFN Sez Pisa, I-56127 Pisa, Italy. [Barbiellini, G.; Longo, F.] INFN Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Gustafsson, M.; Tibaldo, L.] INFN Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Pivato, G.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.] INFN Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [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.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; 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.; Monte, C.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.] Ecole Polytech, Lab Leprince Ringuet, CNRS IN2P3, Palaiseau, France. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Casandjian, J. M.; Grenier, I. A.; Pierbattista, M.] CEA IRFU CNRS Univ Paris Diderot, Lab AIM, Serv Astrophys, CEA Saclay, F-91191 Gif Sur Yvette, France. [Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA. [Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS IN2P3, F-34095 Montpellier 05, France. [Conrad, J.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Yang, Z.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Conrad, J.] Royal Swedish Acad Sci Res, Stockholm, Sweden. [Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Grp Collegato Udine, INFN Sez Trieste, I-33100 Udine, Italy. [Dermer, C. D.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ferrara, E. C.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fukazawa, Y.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res CSPAR, Huntsville, AL 35899 USA. [Hughes, R. E.] Kyoto Univ, Dept Astron, Grad Sch Sci, Sakyo Ku, Kyoto 6068502, Japan. [Johnson, A. S.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Katagiri, H.] Ibaraki Univ, Coll Sci, Bunkyo Ku, Mito, Ibaraki 3108512, Japan. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France. [Latronico, L.] INFN Sezioine Torino, I-10125 Turin, Italy. [Lionetto, A. M.; Morselli, A.; Vitale, V.] INFN Sez Roma Tor Vergata, I-00133 Rome, Italy. [Lionetto, A. M.; Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Razzano, M.; Ritz, S.; Parkinson, P. M. Saz; Schalk, T. L.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Razzano, M.; Ritz, S.; Parkinson, P. M. Saz; Schalk, T. L.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Siskind, E. J.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Troja, E.] NASA Postdoctoral Program, Oak Ridge, TN USA. [Vianello, G.] Consorzio Interuniv Fis Spaziale CIFS, I-10133 Turin, Italy. [Torres, D. F.] Inst Catalana Recerca & Estudis Avancats ICREA, Barcelona, Spain. RP Ajello, M (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. EM bijanb@alumni.stanford.edu; bberenji@uci.edu; johann.cohen-tanugi@lupm.in2p3.fr RI Orlando, E/R-5594-2016; Do, Changwoo/A-9670-2011; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Ozaki, Masanobu/K-1165-2013; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; OI Do, Changwoo/0000-0001-8358-8417; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Graham, Peter/0000-0002-1600-1601; De Angelis, Alessandro/0000-0002-3288-2517; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Bastieri, Denis/0000-0002-6954-8862; Pesce-Rollins, Melissa/0000-0003-1790-8018; Giroletti, Marcello/0000-0002-8657-8852; Cutini, Sara/0000-0002-1271-2924; Berenji, Bijan/0000-0002-4551-772X 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; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France 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.; 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 28 TC 2 Z9 2 U1 0 U2 7 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 FEB PY 2012 IS 2 AR 012 DI 10.1088/1475-7516/2012/02/012 PG 25 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 904EE UT WOS:000301176000013 ER PT J AU Bae, SY Korniski, R Ream, A Shahinian, H Manohara, HM AF Bae, Sam Y. Korniski, Ron Ream, Allen Shahinian, Hrayr Manohara, Harish M. TI New technique of three-dimensional imaging through a 3-mm single lens camera SO OPTICAL ENGINEERING LA English DT Article DE 3-D imaging; stereo endoscope; multispectral imaging; minimally invasive neurosurgery; skull base surgery; spectral illumination band (SIB); complementary multi-bandpass filters AB We present a technique for imaging full-color 3-D images with a single camera in this paper. Unlike a typical 3-D-imaging system comprising two independent cameras each contributing one viewpoint, the technique presented here creates two viewpoints using a single-lens camera with a bipartite filter whose bandpass characteristics are complementary to each other. The bipartite filter divides the camera's limiting aperture into two spatially separated apertures or viewpoints that alternately image an object field using filter-passband matched, time-sequenced illumination. This technique was applied to construct a 3-D camera to image scenes at a working distance of 10 mm. We evaluated the effectiveness of the 3-D camera in generating stereo images using statistical comparison of the depth resolutions achieved by the 3-D camera and a similar 2D camera arrangement. The comparison showed that the complementary filters produce effective stereopsis at prescribed working distances. (C) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.OE.51.2.021106] C1 [Bae, Sam Y.; Korniski, Ron; Manohara, Harish M.] CALTECH, Jet Prop Lab, Pasadena, CA 90041 USA. [Bae, Sam Y.] Univ Calif Los Angeles, Los Angeles, CA USA. [Ream, Allen] Montana State Univ, Bozeman, MT 59717 USA. [Shahinian, Hrayr] SUNY Stony Brook, Skull Base Inst, Los Angeles, CA USA. RP Bae, SY (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 90041 USA. EM ybae@jpl.nasa.gov FU Skull Base Institute of Los Angeles, California; National Aeronautics and Space Administration FX This research was carried out under funding from the Skull Base Institute of Los Angeles, California. We thank Mr. Victor White and Dr. Kirill Scheglov who inspired us to conduct this research. We are grateful to Dr. Pantazis Mouroulis at JPL whose constructive comments helped shape this work. We also thank Mr. Robert Kowalczyk of JPL for his assistance in the laboratory. Mr. Sam Bae gives special thanks to Professor Harold Monbouquette of UCLA for his support and guidance of the project for his PhD work at UCLA. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Government sponsorship acknowledged. NR 18 TC 5 Z9 5 U1 0 U2 7 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 J9 OPT ENG JI Opt. Eng. PD FEB PY 2012 VL 51 IS 2 AR 021106 DI 10.1117/1.OE.51.2.021106 PG 7 WC Optics SC Optics GA 925RS UT WOS:000302779500008 ER PT J AU Dove, A Heldmann, J McKay, C Toon, OB AF Dove, Adrienne Heldmann, Jennifer McKay, Christopher Toon, Owen B. TI Physics of a Thick Seasonal Snowpack with Possible Implications for Snow Algae SO ARCTIC ANTARCTIC AND ALPINE RESEARCH LA English DT Article ID SURFACE-ENERGY EXCHANGES; ALPINE SITE; TEMPERATURES; BALANCE; MODEL; RADIATION; MOISTURE; CLIMATE; REGION; COVER AB Instrumentation to study snowpack in situ was deployed in Lassen Volcanic National Park (LVNP), California, in an area of deep seasonal snow accumulation and known snow algal bloom recurrence. included in the instrumentation were 11 temperature sensors, evenly spaced up to 2 m above the ground, which provided (1) temperature data within the snowpack when buried, and (2) estimates of snowpack height during accumulation and ablation periods. Beginning in April, moisture sensors measured a strong increase of snowpack liquid water content to greater than 15% by volume; this high melt content is usually coincident with the start of runoff from the snowpack. Snow depth profiles showed a rapid ablation of the final 2 m of the snowpack over about 23 days beginning in late June. SNTHERM numerical modeling confirmed that solar radiation was the dominant energy term throughout the melt season. By modeling a variety of snowpack parameters, such as albedo and initial snow density, we determined that the date of snow loss is the most sensitive observable that can be used to constrain the modeled parameters. These data sets from LVNP can also be applied to knowledge of snow algae lifecycles in deep snow to help understand whether the availability of light, water, or both controls the onset of snow algae germination at the base of a thick snowpack. Data and modeling indicate that meltwater was present throughout the snowpack beginning in March and runoff is initiated in April, when the snowpack was still several meters deep. However, significant levels of light did not penetrate to the soil until June, when the snow was less than 2 m deep. C1 [Dove, Adrienne; Toon, Owen B.] Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Heldmann, Jennifer; McKay, Christopher] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Mountain View, CA 94035 USA. RP Dove, A (reprint author), Atmospher & Space Phys Lab, 1234 Innovat Dr, Boulder, CO 80303 USA. EM adrienne.dove@colorado.edu FU NASA FX This work was funded through the NASA Planetary Geology and Geophysics Program and a NASA Graduate Student Research Program Fellowship. We gratefully acknowledge the machine shop at NASA Ames Research Center for building the equipment stands, Lassen Volcanic National Park for access and permits for the site, Steve Zachary for invaluable help and guidance at the park, and the many field hands who have assisted in data collection over several field seasons. Additionally, we would like to thank the anonymous reviewers for their detailed comments and suggestions, which greatly improved the manuscript. NR 42 TC 2 Z9 2 U1 1 U2 13 PU INST ARCTIC ALPINE RES PI BOULDER PA UNIV COLORADO, BOULDER, CO 80309 USA SN 1523-0430 J9 ARCT ANTARCT ALP RES JI Arct. Antarct. Alp. Res. PD FEB PY 2012 VL 44 IS 1 BP 36 EP 49 DI 10.1657/1938-4246-44.1.36 PG 14 WC Environmental Sciences; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 918SO UT WOS:000302271600005 ER PT J AU Wohl, CJ Atkins, BM Belcher, MA Connell, JW AF Wohl, Christopher J. Atkins, Brad M. Belcher, Marcus A. Connell, John W. TI Synthesis, characterization, topographical modification, and surface properties of copoly(imide siloxane)s SO HIGH PERFORMANCE POLYMERS LA English DT Article DE polyimide; siloxane; abhesion; lunar dust; superhydrophobicity ID BLOCK-COPOLYMERS; PHASE-SEPARATION; LUNAR DUST; BLENDS AB Novel copoly(imide siloxane)s were synthesized from commercially available aminopropyl terminated siloxane oligomers, aromatic dianhydrides, and diamines. This synthetic approach produced copolymers with well-defined siloxane blocks linked with imide units in a random fashion. The copoly(amide acid)s were characterized by solution viscosity and subsequently used to cast thin films followed by thermal imidization in an inert atmosphere. Thin films were characterized using contact angle goniometry, attenuated total reflection Fourier transform infrared spectroscopy, confocal and optical microscopy, and tensile testing. Adhesion of micron-sized particles was determined quantitatively using a sonication device. The polydimethylsiloxane moieties lowered the copolymer surface energy due to migration of siloxane moieties to the film's surface, resulting in a notable reduction in particle adhesion. A further reduction in particle adhesion was achieved by introducing topographical features on a scale of several to tens of microns by a laser ablation technique. C1 [Wohl, Christopher J.; Atkins, Brad M.; Connell, John W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Belcher, Marcus A.] Natl Inst Aerosp, Hampton, VA USA. RP Wohl, CJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM christopher.j.wohl@nasa.gov FU NASA Langley Research Center FX The authors would like to thank Dr Jeffrey A. Hinkley, NASA Langley Research Center, for scientific discussion. This work was funded through the NASA Langley Research Center's Creative and Innovative Research Fund. NR 31 TC 10 Z9 12 U1 3 U2 17 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0954-0083 J9 HIGH PERFORM POLYM JI High Perform. Polym. PD FEB PY 2012 VL 24 IS 1 SI SI BP 40 EP 49 DI 10.1177/0954008311431113 PG 10 WC Polymer Science SC Polymer Science GA 918YR UT WOS:000302288100006 ER PT J AU Gao, Y Zhou, N Yang, F Cui, Y Kovarik, L Hatcher, N Noebe, R Mills, MJ Wang, Y AF Gao, Y. Zhou, N. Yang, F. Cui, Y. Kovarik, L. Hatcher, N. Noebe, R. Mills, M. J. Wang, Y. TI P-phase precipitation and its effect on martensitic transformation in (Ni,Pt)Ti shape memory alloys SO ACTA MATERIALIA LA English DT Article DE Coherent precipitate; Elastic interaction; Nucleation; Aging effect; Phase field simulation ID CRYSTAL NI-AL; TI-NI; MICROSTRUCTURAL DEVELOPMENT; ORDERED INTERMETALLICS; COMPUTER-SIMULATION; START TEMPERATURES; FIELD SIMULATION; GROWTH-KINETICS; STRESS LEVELS; EVOLUTION AB A new precipitate phase named P-phase has recently been identified in (Ni,Pt)Ti high temperature shape memory alloys. In order to understand the roles played by the fine coherent P-phase precipitates in determining the martensitic transformation temperature (M-s), strength of the B2 matrix phase, dimensional stability and shape memory effect of the alloys, a phase field model of P-phase precipitation is developed. Model inputs, including lattice parameters, precipitate matrix orientation relationship, elastic constants and free energy data, are obtained from experimental characterization, ab initio calculations and thermodynamic databases. Through computer simulations, the shape and spatial distribution of the P-phase precipitates, as well as the compositional and stress fields around them, are quantitatively determined. On this basis, the elastic interaction energy between the P-phase precipitates and a martenstic nucleus is calculated. It is found that both the chemical non-uniformity and stress field associated with the P-phase precipitates are in favor of the martensitic transformation. Their relative contributions to the increase in M-s temperature are quantified as a function of aging time and the result seems to agree with the experimental measurements. The shape and spatial distribution of the P-phase precipitates predicted by the simulations also agree well with experimental observations. (C) 2011 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Gao, Y.; Zhou, N.; Yang, F.; Cui, Y.; Kovarik, L.; Mills, M. J.; Wang, Y.] Ohio State Univ, Dept Mat Sci & Engn, Columbus, OH 43210 USA. [Hatcher, N.] Ruhr Univ Bochum, Interdisciplinary Ctr Adv Mat Simulat, Bochum, Germany. [Noebe, R.] NASA, Glen Res Ctr, Cleveland, OH 44135 USA. RP Wang, Y (reprint author), Ohio State Univ, Dept Mat Sci & Engn, 2041 Coll Rd,477 Watts Hall, Columbus, OH 43210 USA. EM wang.363@osu.edu RI Zhou, Ning/B-2624-2010; Wang, Yunzhi/B-2557-2010; Hatcher, Nicholas/H-6450-2013; Mills, Michael/I-6413-2013; Kovarik, Libor/L-7139-2016 OI Hatcher, Nicholas/0000-0001-7130-1618; FU NASA; Supersonics Project (Dale Hopkins, API); NSF [DMRI008349]; US Department of Energy, Office of Basic Energy Sciences [DE-SC0001258] FX This work was supported by the NASA Fundamental Aeronautics Program, Supersonics Project (Dale Hopkins, API), NSF under grant DMRI008349 (YW) and US Department of Energy, Office of Basic Energy Sciences under grant DE-SC0001258 (YG, FY and MJM). NR 55 TC 22 Z9 23 U1 4 U2 58 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6454 EI 1873-2453 J9 ACTA MATER JI Acta Mater. PD FEB PY 2012 VL 60 IS 4 BP 1514 EP 1527 DI 10.1016/j.actamat.2011.11.043 PG 14 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 914YK UT WOS:000301989500008 ER PT J AU Mao, Z Booth-Morrison, C Sudbrack, CK Martin, G Seidman, DN AF Mao, Zugang Booth-Morrison, Christopher Sudbrack, Chantal K. Martin, Georges Seidman, David N. TI Kinetic pathways for phase separation: An atomic-scale study in Ni-Al-Cr alloys SO ACTA MATERIALIA LA English DT Article DE Nickel-based superalloys; Kinetic pathways; Atom probe tomography; Lattice kinetic Monte Carlo; Nanostructures ID INITIO MOLECULAR-DYNAMICS; TOTAL-ENERGY CALCULATIONS; MONTE-CARLO SIMULATIONS; WAVE BASIS-SET; AB-INITIO; PROBE TOMOGRAPHY; MULTICOMPONENT ALLOYS; TEMPORAL EVOLUTION; SOLID-SOLUTIONS; LIQUID-METALS AB The kinetic pathways involved in the formation of gamma'(Ll(2) structure)-precipitates during aging of concentrated Ni-Al-Cr alloys at 873 K, for three distinct alloy compositions, are studied experimentally by atom probe tomography, and computationally with lattice kinetic Monte Carlo (LKMC) simulations using parameters deduced from first-principles calculations of cohesive energies, and from experimental diffusion data. It is found that the compositional evolution of the gamma'-precipitate phase does not follow the predictions of a classical mean-field model for coarsening of precipitates in ternary alloys. LKMC simulations reveal that long-range vacancy solute binding plays a key role during the early stages of gamma'-precipitation. With the aid of Monte Carlo techniques using the parameters employed in the LKMC simulations, we compute the diffusion matrix in the terminal solid-solutions and demonstrate that key features of the observed kinetic pathways are the result of kinetic couplings among the diffusional fluxes. The latter are controlled by the long-range vacancy-solute binding energies. It is concluded that, because it neglects flux couplings, the classical mean-field approach to phase separation for a ternary alloy, despite its many qualitatively correct predictions, fails to describe quantitatively the true kinetic pathways that lead to phase separation in concentrated metallic alloys. (C) 2011 Published by Elsevier Ltd. on behalf of Acta Materialia Inc. C1 [Mao, Zugang; Booth-Morrison, Christopher; Sudbrack, Chantal K.; Martin, Georges; Seidman, David N.] Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA. [Sudbrack, Chantal K.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA. [Martin, Georges] Cabinet Haut Commissaire, Commissariat Energie Atom, F-91191 Gif Sur Yvette, France. [Seidman, David N.] Northwestern Univ, Ctr Atom Probe Tomog NUCAPT, Evanston, IL 60208 USA. RP Seidman, DN (reprint author), Northwestern Univ, Dept Mat Sci & Engn, 2220 Campus Dr, Evanston, IL 60208 USA. EM d-seidman@northwestern.edu RI Seidman, David/B-6697-2009 FU National Science Foundation (NSF) [DMR-0241928]; NSF-MRI [DMR 0420532]; ONR-DURIP [N00014-0400798, N00014-0610539] FX This research was sponsored by the National Science Foundation (NSF) under Grant DMR-0241928, Dr. A.J. Ardell, grant monitor. Alloys were processed at NASA Glenn Research Center courtesy of Dr. Ronald Noebe. APT measurements were performed at the Northwestern University Center for Atom Probe Tomography (NUCAPT). The LEAP tomograph was purchased with initial funding from the NSF-MRI (DMR 0420532, Dr. Charles Bouldin, grant officer) and ONR-DURIP (N00014-0400798, Dr. Julie Christodoulou, grant officer) programs. Additionally, the LEAP tomograph was enhanced with picosecond laser pulsing with funding from the ONR-DURIP (N00014-0610539, J. Christodoulou, grant officer). We wish to thank Prof. Pascal Bellon for discussions, Prof. Dieter Isheim for managing NUCAPT, Dr. Stephen M. Foiles for his grand canonical Monte Carlo code, and Dr. Carelyn Campbell for diffusivity databases. NR 58 TC 18 Z9 18 U1 5 U2 43 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6454 J9 ACTA MATER JI Acta Mater. PD FEB PY 2012 VL 60 IS 4 BP 1871 EP 1888 DI 10.1016/j.actamat.2011.10.046 PG 18 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 914YK UT WOS:000301989500042 ER PT J AU Marko, P Nance, H Dawson-Guynn, K AF Marko, Peter Nance, Holly Dawson-Guynn, Kimberly TI Seafood mislabeling: a response to Mariani SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Letter ID FISH C1 [Marko, Peter] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. [Nance, Holly] Florida Atlantic Univ, Harbor Branch Oceanog Inst, Ft Pierce, FL USA. [Dawson-Guynn, Kimberly] NOAA, Natl Seafood Inspect Lab, Natl Marine Fisheries Serv, Pascagoula, MS USA. RP Marko, P (reprint author), Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. EM pmarko@clemson.edu NR 6 TC 0 Z9 0 U1 0 U2 11 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1540-9295 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD FEB PY 2012 VL 10 IS 1 BP 10 EP 11 DI 10.1890/12.WB.002 PG 2 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 913GG UT WOS:000301864000013 ER PT J AU Knuth, MA Johnson, JB Hopkins, MA Sullivan, RJ Moore, JM AF Knuth, M. A. Johnson, J. B. Hopkins, M. A. Sullivan, R. J. Moore, J. M. TI Discrete element modeling of a Mars Exploration Rover wheel in granular material SO JOURNAL OF TERRAMECHANICS LA English DT Article DE Mars Exploration Rover; Discrete element method; Triaxial test; Lunar regolith simulant AB Three-dimensional discrete element method (DEM) simulations were developed for the Mars Exploration Rover (MER) mission to investigate: (1) rover wheel interactions with martian regolith; and (2) regolith deformation in a geotechnical triaxial strength cell (GTSC). These DEM models were developed to improve interpretations of laboratory and in situ rover data, and can simulate complicated regolith conditions. A DEM simulation was created of a laboratory experiment that involved a MER wheel digging into lunar regolith simulant. Sinkage and torques measured in the experiment were compared with those predicted numerically using simulated particles of increasing shape complexity (spheres, ellipsoids, and poly-ellipsoids). GTSC simulations, using the same model regolith used in the MER simulations, indicate a peak friction angle of approximately 37-38 degrees compared to internal friction angles of 36.5-37.7 degrees determined from the wheel digging experiments. Density of the DEM regolith was 1820 kg/m(3) compared to 1660 kg/m(3) for the lunar simulant used in the wheel digging experiment indicating that the number of grain contacts and grain contact resistance determined bulk strength in the DEM simulations, not density. An improved correspondence of DEM and actual test regolith densities is needed to simulate the evolution of regolith properties as density changes. Published by Elsevier Ltd. on behalf of ISTVS. C1 [Knuth, M. A.; Hopkins, M. A.] USA, Engineer Res & Dev Ctr, Cold Reg Res & Engn Lab, Hanover, NH 03755 USA. [Johnson, J. B.] Univ Alaska Fairbanks, Inst No Engn, Fairbanks, AK 99775 USA. [Sullivan, R. J.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Moore, J. M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Knuth, MA (reprint author), USA, Engineer Res & Dev Ctr, Cold Reg Res & Engn Lab, 72 Lyme Rd, Hanover, NH 03755 USA. EM Margaret.A.Knuth@usace.army.mil; jbjohnson5@alaska.edu; Mark.A.Hopkins@usace.army.mil; rjs33@cornell.edu; jeffmoore@nasa.gov FU NASA Lunar Science Institute; NASA's Kennedy Space Center; NASA MERPS [NNH05ZDA001N] FX This work was supported by the NASA Lunar Science Institute supported project "Scientific Exploration Potential of the Lunar Poles", NASA's Kennedy Space Center Technology Development project "Lunar regolith mechanical properties, the NASA's Mars Fundamental Research Program project "The relationship between the physical and mechanical properties of Mars soils and their simulation", and the NASA Mars Exploration Rover Program-NNH05ZDA001N-MERPS project "Physical and geologic Investigations of the surface materials along the MER traverses. NR 23 TC 20 Z9 21 U1 1 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4898 J9 J TERRAMECHANICS JI J. Terramech. PD FEB PY 2012 VL 49 IS 1 BP 27 EP 36 DI 10.1016/j.terra.2011.09.003 PG 10 WC Engineering, Environmental SC Engineering GA 913TO UT WOS:000301900500003 ER PT J AU Braverman, AJ Fetzer, EJ Kahn, BH Manning, EM Oliphant, RB Teixeira, JP AF Braverman, Amy J. Fetzer, Eric J. Kahn, Brian H. Manning, Evan M. Oliphant, Robert B. Teixeira, Joao P. TI Massive Dataset Analysis for NASA's Atmospheric Infrared Sounder SO TECHNOMETRICS LA English DT Article DE Climate change; Data compression; Data reduction; Remote sensing; Quantization ID CONSTRAINED VECTOR QUANTIZATION AB The National Aeronautics and Space Administration's (NASA) Atmospheric Infrared Sounder (AIRS) has been collecting large quantities of remote sensing data about the vertical structure of temperature, water vapor, and clouds in the Earth's atmosphere since its launch aboard the Aqua spacecraft in mid2002. These data are both global and high resolution, so they are uniquely able to provide distributional information about second- and higher-order interactions that are at the heart of understanding climate processes. However, these data are so large and complex that the structures of interest are not directly accessible without some form of data reduction, and data reduction is particularly problematic because of the way the data are staged and stored. Thus, AIRS data pose a classic problem in the analysis of modern massive datasets: how to quantify and understand global distributional relationships in datasets that are impossible to work with except in small pieces? Our approach is to hierarchically reduce the data in a way that preserves distributional characteristics across subsets formed by stratifying on intuitively meaningful variables. By exploring how distributions change as functions of the stratification variables, we gain insight into processes generating the data. In this article, we describe our implementation of methodology first proposed in two earlier papers. Here, we have operationalized the algorithm and demonstrated that it is both practical within the NASA data processing pipeline, and leads to important scientific insights that are only possible when massive datasets are reduced in a way that respects the structure of multivariate distributions. C1 [Braverman, Amy J.; Fetzer, Eric J.; Kahn, Brian H.; Manning, Evan M.; Oliphant, Robert B.; Teixeira, Joao P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Braverman, AJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Amy.Braverman@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this article was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The NCEP Reanalysis Pressure level data are provided by the NOAA/OAR/ESRL PSD, Boulder, CO. NR 15 TC 2 Z9 2 U1 0 U2 1 PU AMER STATISTICAL ASSOC PI ALEXANDRIA PA 732 N WASHINGTON ST, ALEXANDRIA, VA 22314-1943 USA SN 0040-1706 J9 TECHNOMETRICS JI Technometrics PD FEB PY 2012 VL 54 IS 1 BP 1 EP 15 DI 10.1080/00401706.2012.650504 PG 15 WC Statistics & Probability SC Mathematics GA 914QZ UT WOS:000301967900001 ER PT J AU Wong, AR Toftul, A Polzin, KA Pearson, JB AF Wong, Andrea R. Toftul, Alexandra Polzin, Kurt A. Pearson, J. Boise TI Non-contact thrust stand calibration method for repetitively pulsed electric thrusters SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID PERFORMANCE AB A thrust stand calibration technique for use in testing repetitively pulsed electric thrusters for in-space propulsion has been developed and tested using a modified hanging pendulum thrust stand. In the implementation of this technique, current pulses are applied to a solenoid to produce a pulsed magnetic field that acts against a permanent magnet mounted to the thrust stand pendulum arm. The force on the magnet is applied in this non-contact manner, with the entire pulsed force transferred to the pendulum arm through a piezoelectric force transducer to provide a time-accurate force measurement. Modeling of the pendulum arm dynamics reveals that after an initial transient in thrust stand motion the quasi-steady average deflection of the thrust stand arm away from the unforced or "zero" position can be related to the average applied force through a simple linear Hooke's law relationship. Modeling demonstrates that this technique is universally applicable except when the pulsing period is increased to the point where it approaches the period of natural thrust stand motion. Calibration data were obtained using a modified hanging pendulum thrust stand previously used for steady-state thrust measurements. Data were obtained for varying impulse bit at constant pulse frequency and for varying pulse frequency. The two data sets exhibit excellent quantitative agreement with each other. The overall error on the linear regression fit used to determine the calibration coefficient was roughly %. (C) 2012 American Institute of Physics. [doi:10.1063/1.3680557] C1 [Wong, Andrea R.; Toftul, Alexandra; Polzin, Kurt A.; Pearson, J. Boise] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Wong, AR (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM kurt.a.polzin@nasa.gov FU NASA FX We appreciate the continued management support of Mr. Jim Martin and Ms. Mary Beth Koelbl and the continued academic affairs support of Ms. Mona Miller and Ms. Tina Haymaker. We gratefully acknowledge the contributions and support during the course of this effort by Tommy Reid, Doug Galloway, Ashley Hallock, Derek Mayer, Adam Kimberlin, and Kevin Bonds. This program was supported under NASA's Advanced In-Space Propulsion program managed by Dr. Michael LaPointe. NR 8 TC 2 Z9 2 U1 0 U2 4 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD FEB PY 2012 VL 83 IS 2 AR 025103 DI 10.1063/1.3680557 PN 1 PG 7 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 909LS UT WOS:000301566600053 PM 22380121 ER PT J AU Meador, MAB Malow, EJ Silva, R Wright, S Quade, D Vivod, SL Guo, HQ Guo, J Cakmak, M AF Meador, Mary Ann B. Malow, Ericka J. Silva, Rebecca Wright, Sarah Quade, Derek Vivod, Stephanie L. Guo, Haiquan Guo, Jiao Cakmak, Miko TI Mechanically Strong, Flexible Polyimide Aerogels Cross-Linked with Aromatic Triamine SO ACS APPLIED MATERIALS & INTERFACES LA English DT Article DE aerogel; polyimide; cross-linking; nanoporous materials; high temperature insulation ID MODIFIED SILICA AEROGELS; TEMPERATURE POLYMERS; ELASTIC PROPERTIES; LAYERS AB Polyimide gels are produced by cross-linking anhydride capped polyamic acid oligomers with aromatic triamine in solution and chemically imidizing. The gels are then supercritically dried to form nanoporous polyimide aerogels with densities as low as 0.14 g/cm(3) and surface areas as high as 512 m(2)/g. To understand the effect of the polyimide backbone on properties, aerogels from several combinations of diamine and dianhydride, and formulated oligomer chain length are examined. Formulations made from 2,2'-dimethylbenzidine as the diamine shrink the least but have among the highest compressive modulus. Formulations made using 4,4'-oxydianiline or 2,2'dimethylbenzidine can be fabricated into continuous thin films using a roll to roll casting process. The films are flexible enough to be rolled or folded back on themselves and recover completely without cracking or flaking, and have tensile strengths of 4-9 MPa. Finally, the highest onset of decomposition (above 600 degrees C) of the polyimide aerogels was obtained using p-phenylene diamine as the backbone diamine with either dianhydride studied. All of the aerogels are suitable candidates for high-temperature insulation with glass transition temperatures ranging from 270-340 degrees C and onsets of decomposition from 460-610 degrees C. C1 [Meador, Mary Ann B.; Malow, Ericka J.; Silva, Rebecca; Wright, Sarah; Vivod, Stephanie L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Quade, Derek; Guo, Haiquan] Ohio Aerosp Inst, Cleveland, OH 44142 USA. [Guo, Jiao; Cakmak, Miko] Univ Akron, Akron, OH 44325 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; Third Frontier Program of the State of Ohio FX We thank the NASA Fundamental Aeronautics Program (Hypersonics) for financial support of this research. In addition, we thank Dan Schieman (ARSC) for helium pycnometry measurements and thermal analysis, Linda McCorkle (Ohio Aerospace Institute) for SEM images, and Anna Palczer for nitrogen sorption measurements. We also thank the Third Frontier Program of the State of Ohio for funding the construction of the roll to roll film manufacturing line. NR 34 TC 75 Z9 81 U1 25 U2 156 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 FEB PY 2012 VL 4 IS 2 BP 536 EP 544 DI 10.1021/am2014635 PG 9 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA 897IW UT WOS:000300644500007 PM 22233638 ER PT J AU Lin, Y Bunker, CE Fernando, KAS Connell, JW AF Lin, Yi Bunker, Christopher E. Fernando, K. A. Shiral Connell, John W. TI Aqueously Dispersed Silver Nanoparticle-Decorated Boron Nitride Nanosheets for Reusable, Thermal Oxidation-Resistant Surface Enhanced Raman Spectroscopy (SERS) Devices SO ACS APPLIED MATERIALS & INTERFACES LA English DT Article DE boron nitride nanosheets; nanometal decoration; reusable; SERS; wet transfer ID CARBON NANOTUBES; GRAPHENE OXIDE; METAL NANOPARTICLES; PHOTOCATALYTIC REDUCTION; ANCHORING SEMICONDUCTOR; SCATTERING; FILM; GOLD; LAYER; NANORIBBONS AB The impurity-free aqueous dispersions of boron nitride nanosheets (BNNS) allowed the facile preparation of silver (Ag) nanoparticle-decorated BNNS by chemical reduction of an Ag salt with hydrazine. in the presence of BNNS. The resultant Ag BNNS nanohybrids remained dispersed in water, allowing convenient subsequent solution processing. By using substrate transfer techniques, Ag BNNS nanohybrid thin film coatings on quartz substrates were prepared and evaluated as reusable surface enhanced Raman spectroscopy (SERS) sensors that were robust against repeated solvent washing. In addition, because ofthe unique thermal oxidation-resistant properties of the BNNS, the sensor devices may be readily recycled by short-duration high temperature air oxidation to remove residual analyte molecules in repeated runs. The limiting factor associated with the thermal oxidation recycling process was the Ostwald ripening effect of Ag nanostructures. C1 [Lin, Yi] Natl Inst Aerosp, Hampton, VA 23666 USA. [Bunker, Christopher E.] USAF, Prop Directorate, Res Lab, Wright Patterson AFB, OH 45433 USA. [Fernando, K. A. Shiral] Univ Dayton, Res Inst, Nanotechnol Grp, Dayton, OH 45433 USA. [Connell, John W.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. RP Lin, Y (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. EM yi.lin-1@nasa.gov; christopher.bunker@wpafb.af.mil; john.w.connell@nasa.gov NR 64 TC 64 Z9 65 U1 7 U2 144 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1944-8244 J9 ACS APPL MATER INTER JI ACS Appl. Mater. Interfaces PD FEB PY 2012 VL 4 IS 2 BP 1110 EP 1117 DI 10.1021/am201747d PG 8 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA 897IW UT WOS:000300644500088 PM 22280102 ER PT J AU Vadrevu, KP Ellicott, E Giglio, L Badarinath, KVS Vermote, E Justice, C Lau, WKM AF Vadrevu, Krishna Prasad Ellicott, Evan Giglio, Louis Badarinath, K. V. S. Vermote, Eric Justice, Chris Lau, William K. M. TI Vegetation fires in the himalayan region - Aerosol load, black carbon emissions and smoke plume heights SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Vegetation fires; Biomass burnt; Emissions; India ID SATELLITE-OBSERVATIONS; INJECTION HEIGHTS; OPTICAL DEPTH; MODIS; ALGORITHM; CALIPSO; INDIA; LIDAR AB In this study, we investigate the potential of multi-satellite datasets for quantifying the biomass burning emissions from the Himalayan region. A variety of satellite products were used for characterizing fire events including active fire counts, burnt areas, aerosol optical depth (AOD) variations, aerosol index and smoke plume heights. Results from the MODerate-resolution Imaging Spectroradiometer (MODIS) fire product suggest March June as the major fire season with the peak during the April. An average of 3908 fire counts per year were recorded with sixty four percent of the fires occurring in the low elevation areas in the Himalayan Region. We estimate average burnt areas of 1129 sq. km, with the black carbon emissions of 431 Mg, per year. The mean AOD (2005-2010) was 0.287 +/- 0.105 (one sigma) with peak values in May. Correlation analysis between the fire counts and AOD resulted in a Pearson correlation coefficient of 0.553; the correlation between the FRP and AOD is relatively weaker (r = 0.499). Planetary boundary layer height retrieved from the Modern Era Retrospective-Analysis For Research And Applications (MERRA) product suggests typical PBL height of 1000-1200 m during the April-May peak biomass burning season. Cloud-Aerosol Lidar Orthogonal Polarisation (CALIOP) retrievals show the extent of smoke plume heights beyond the planetary boundary layer during the peak biomass burning month of April. However, comparison of fires in the Himalayan region with other regions and comparisons to aerosol index data from the Ozone Monitoring Instrument (OM!) suggest smoke plumes reaching less than 3 km. Our results on fires and smoke plume height relationships provide valuable information for addressing aerosol transport in the region. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Vadrevu, Krishna Prasad; Ellicott, Evan; Giglio, Louis; Vermote, Eric; Justice, Chris] Univ Maryland, Dept Geog, College Pk, MD 20740 USA. [Badarinath, K. V. S.] Natl Remote Sensing Ctr, Atmospher Sci Sect, Hyderabad 500625, Andhra Pradesh, India. [Lau, William K. M.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Vadrevu, KP (reprint author), Univ Maryland, Dept Geog, College Pk, MD 20740 USA. EM krisvkp@yahoo.com RI Vermote, Eric/K-3733-2012; Lau, William /E-1510-2012; OI Lau, William /0000-0002-3587-3691; Vadrevu, Krishna/0000-0003-4407-5605 FU NASA [NNX10AU77G] FX We thank product developers of MODIS active fires and burnt areas in addition to ATSR, MERIS, MERRA, OMI and CALIPSO datasets. This research was supported by NASA grant NNX10AU77G. NR 47 TC 40 Z9 40 U1 4 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD FEB PY 2012 VL 47 BP 241 EP 251 DI 10.1016/j.atmosenv.2011.11.009 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 903XY UT WOS:000301157700027 ER PT J AU Stenger, MB Evans, JM Knapp, CF Lee, SMC Phillips, TR Perez, SA Moore, AD Paloski, WH Platts, SH AF Stenger, Michael B. Evans, Joyce M. Knapp, Charles F. Lee, Stuart M. C. Phillips, Tiffany R. Perez, Sondra A. Moore, Alan D., Jr. Paloski, William H. Platts, Steven H. TI Artificial gravity training reduces bed rest-induced cardiovascular deconditioning SO EUROPEAN JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE Cardiovascular regulation; Neuroendocrine; Spectral power; Hypergravity; Peak oxygen consumption ID POWER SPECTRAL-ANALYSIS; HEAD-DOWN TILT; ORTHOSTATIC INTOLERANCE; SPACE-FLIGHT; EXERCISE PERFORMANCE; DURATION SPACEFLIGHT; ARTERIAL-PRESSURE; MAXIMAL EXERCISE; UPRIGHT EXERCISE; AMBULATORY MEN AB We studied 15 men (8 treatment, 7 control) before and after 21 days of 6 head-down tilt to determine whether daily, 1-h exposures to 1.0 G(z) (at the heart) artificial gravity (AG) would prevent bed rest-induced cardiovascular deconditioning. Testing included echocardiographic analysis of cardiac function, plasma volume (PV), aerobic power (VO(2)pk) and cardiovascular and neuroendocrine responses to 80 degrees head-up tilt (HUT). Data collected during HUT were ECG, stroke volume (SV), blood pressure (BP) and blood for catecholamines and vasoactive hormones. Heart rate (HR), cardiac output (CO), total peripheral resistance, and spectral power of BP and HR were calculated. Bed rest decreased PV, supine and HUT SV, and indices of cardiac function in both groups. Although PV was decreased in control and AG after bed rest, AG attenuated the decrease in orthostatic tolerance [pre- to post-bed rest change; control: -11.8 +/- 2.0, AG: -6.0 +/- 2.8 min (p = 0.012)] and VO(2)pk [pre- to post-bed rest change; control: -0.39 +/- 0.11, AG: -0.17 +/- 0.06 L/min (p = 0.041)]. AG prevented increases in pre-tilt levels of plasma renin activity [pre- to post-bed rest change; control: 1.53 +/- 0.23, AG: -0.07 +/- 0.34 ng/mL/h (p = 0.001)] and angiotensin II [pre- to post-bed rest change; control: 3.00 +/- 1.04, AG: -0.63 +/- 0.81 pg/mL (p = 0.009)] and increased HUT aldosterone [post-bed rest; control: 107 +/- 30 pg/mL, AG: 229 +/- 68 pg/mL (p = 0.045)] and norepinephrine [post-bed rest; control: 453 +/- 107, AG: 732 +/- 131 pg/mL (p = 0.003)]. We conclude that AG can mitigate some aspects of bed rest-induced cardiovascular deconditioning, including orthostatic intolerance and aerobic power. Mechanisms of improvement were not cardiac-mediated, but likely through improved sympathetic responsiveness to orthostatic stress. C1 [Stenger, Michael B.; Lee, Stuart M. C.; Phillips, Tiffany R.; Perez, Sondra A.; Moore, Alan D., Jr.] NASA, Lyndon B Johnson Space Ctr, Cardiovasc Lab, Wyle Integrated Sci & Engn Grp, Houston, TX 77058 USA. [Evans, Joyce M.; Knapp, Charles F.] Univ Kentucky, Ctr Biomed Engn, Lexington, KY 40506 USA. [Paloski, William H.; Platts, Steven H.] NASA JSC, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. [Paloski, William H.] Univ Houston, Dept Hlth & Human Performance, Houston, TX 77204 USA. RP Stenger, MB (reprint author), NASA, Lyndon B Johnson Space Ctr, Cardiovasc Lab, Wyle Integrated Sci & Engn Grp, Houston, TX 77058 USA. EM michael.b.stenger@nasa.gov FU UTMB GCRC; NASA; NIH [M01 RR 0073] FX The authors gratefully acknowledge the support of the UTMB GCRC nursing staff, the Short Radius Centrifuge team, the subjects who participated in the study and JSC Cardiovascular Laboratory team members that participated in data collection and reduction, particularly Christine Ribeiro, Shang-Jin Shi, Ph.D., Timothy Matz, David Martin, and Natalia Arzeno-Gonzalez. We would also like to thank Alan Feiveson, Ph.D., for statistical support. This study was supported by the NASA Human Research Program, and conducted at the NIH-funded [M01 RR 0073] GCRC at UTMB, Galveston, TX. NR 63 TC 17 Z9 18 U1 0 U2 14 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1439-6319 J9 EUR J APPL PHYSIOL JI Eur. J. Appl. Physiol. PD FEB PY 2012 VL 112 IS 2 BP 605 EP 616 DI 10.1007/s00421-011-2005-1 PG 12 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA 909LZ UT WOS:000301567300021 PM 21626041 ER PT J AU Pe'er, A Zhang, BB Ryde, F McGlynn, S Zhang, B Preece, RD Kouveliotou, C AF Pe'er, Asaf Zhang, Bin-Bin Ryde, Felix McGlynn, Sinead Zhang, Bing Preece, Robert D. Kouveliotou, Chryssa TI The connection between thermal and non-thermal emission in gamma-ray bursts: general considerations and GRB090902B as a case study SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE plasmas; radiation mechanisms: thermal; radiative transfer; scattering; gamma-ray burst: general ID INTERNAL SHOCK MODEL; HIGH-ENERGY EMISSION; SELF-COMPTON EMISSION; SCALE MAGNETIC-FIELDS; PROMPT EMISSION; X-RAY; SYNCHROTRON EMISSION; PHOTOSPHERIC EMISSION; PHYSICAL PARAMETERS; SPECTRAL PROPERTIES AB Photospheric (thermal) emission is inherent to the gamma-ray burst (GRB) 'fireball' model. We show here that inclusion of this component in the analysis of the GRB prompt emission phase naturally explains some of the prompt GRB spectra seen by the Fermi satellite over its entire energy band. The sub-MeV peak is explained as multicolour blackbody emission, and the high-energy tail, extending up to the GeV band, results from roughly similar contributions of synchrotron emission, synchrotron self-Compton and Comptonization of the thermal photons by energetic electrons originating after dissipation of the kinetic energy above the photosphere. We show how this analysis method results in a complete, self-consistent picture of the physical conditions at both emission sites of the thermal and non-thermal radiation. We study the connection between the thermal and non-thermal parts of the spectrum, and show how the values of the free model parameters are deduced from the data. We demonstrate our analysis method on GRB090902B: we deduce a Lorentz factor in the range 920 <= eta <= 1070, photospheric radius r(ph) similar or equal to 7.2-8.4 x 10(11) cm and dissipation radius r(gamma) >= 3.5-4.1 x 10(15) cm. By comparison to afterglow data, we deduce that a large fraction epsilon(d) approximate to 85-95 per cent of the kinetic energy is dissipated, and that a large fraction, similar to equipartition of this energy, is carried by the electrons and the magnetic field. This high value of epsilon(d) questions the 'internal shock' scenario as the main energy dissipation mechanism for this GRB. C1 [Pe'er, Asaf] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Pe'er, Asaf] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zhang, Bin-Bin; Zhang, Bing] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. [Ryde, Felix; McGlynn, Sinead] Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Preece, Robert D.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. RP Pe'er, A (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM apeer@cfa.harvard.edu RI Zhang, Binbin/C-9035-2013; OI Zhang, Binbin/0000-0003-2002-116X; Preece, Robert/0000-0003-1626-7335 FU Space Telescope Science Institute; Fermi grant [31014]; Swedish National Space Board FX This research was supported by the Riccardo Giacconi Fellowship award of the Space Telescope Science Institute, and Fermi grant award #31014. FR acknowledges financial support by the Swedish National Space Board. AP wishes to thank Dale Frail, Jeremy Schnittman, Andy Fruchter, Kuntal Misra, Zeljka Bosnjak, Mario Livio and Kailash Sahu for useful discussions. NR 98 TC 52 Z9 52 U1 0 U2 5 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 420 IS 1 BP 468 EP 482 DI 10.1111/j.1365-2966.2011.20052.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905PL UT WOS:000301284600053 ER PT J AU Ackermann, M Ajello, M Allafort, A Baldini, L Ballet, J Barbiellini, G Bastieri, D Belfiore, A Bellazzini, R Berenji, B Blandford, RD Bloom, ED Bonamente, E Borgland, AW Bottacini, E Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cecchi, C Chekhtman, A Ciprini, S Claus, R Cohen-Tanugi, J de Angelis, A de Palma, F Dermer, CD Silva, EDE Drell, PS Dumora, D Favuzzi, C Fegan, SJ Focke, WB Fortin, P Fukazawa, Y Fusco, P Gargano, F Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Guillemot, L Guiriec, S Hadasch, D Hanabata, Y Harding, AK Hayashida, M Hayashi, K Hays, E Johannesson, G Johnson, AS Kamae, T Katagiri, H Kataoka, J Kerr, M Knodlseder, J Kuss, M Lande, J Latronico, L Lee, SH Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Martin, P Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mitthumsiri, W Mizuno, T Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Naumann-Godo, M Nolan, PL Norris, JP Nuss, E Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Ozaki, M Paneque, D Parent, D Pesce-Rollins, M Pierbattista, M Piron, F Porter, TA Raino, S Rando, R Razzano, M Reimer, O Reposeur, T Ritz, S Parkinson, PMS Sgro, C Siskind, EJ Smith, PD Spinelli, P Strong, AW Takahashi, H Tanaka, T Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Torres, DF Tosti, G Tramacere, A Troja, E Uchiyama, Y Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Yang, Z Zimmer, S Bontemps, S AF Ackermann, M. Ajello, M. Allafort, A. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Belfiore, A. Bellazzini, R. Berenji, B. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Bottacini, E. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cecchi, C. Chekhtman, A. Ciprini, S. Claus, R. Cohen-Tanugi, J. de Angelis, A. de Palma, F. Dermer, C. D. do Couto e Silva, E. Drell, P. S. Dumora, D. Favuzzi, C. Fegan, S. J. Focke, W. B. Fortin, P. Fukazawa, Y. Fusco, P. Gargano, F. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Guillemot, L. Guiriec, S. Hadasch, D. Hanabata, Y. Harding, A. K. Hayashida, M. Hayashi, K. Hays, E. Johannesson, G. Johnson, A. S. Kamae, T. Katagiri, H. Kataoka, J. Kerr, M. Knoedlseder, J. Kuss, M. Lande, J. Latronico, L. Lee, S. -H. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Martin, P. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Naumann-Godo, M. Nolan, P. L. Norris, J. P. Nuss, E. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Parent, D. Pesce-Rollins, M. Pierbattista, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, O. Reposeur, T. Ritz, S. Parkinson, P. M. Saz Sgro, C. Siskind, E. J. Smith, P. D. Spinelli, P. Strong, A. W. Takahashi, H. Tanaka, T. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Torres, D. F. Tosti, G. Tramacere, A. Troja, E. Uchiyama, Y. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Yang, Z. Zimmer, S. Bontemps, S. TI The cosmic-ray and gas content of the Cygnus region as measured in gamma-rays by the Fermi Large Area Telescope SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; ISM: clouds; cosmic rays; gamma rays: ISM ID BLIND FREQUENCY SEARCHES; GALACTIC PLANE SURVEY; MILKY-WAY; SUPERNOVA REMNANT; INFRARED-EMISSION; MOLECULAR CLOUDS; DARK GAS; OUTER GALAXY; X-RAY; H-I AB Context. The Cygnus region hosts a giant molecular-cloud complex that actively forms massive stars. Interactions of cosmic rays with interstellar gas and radiation fields make it shine at gamma-ray energies. Several gamma-ray pulsars and other energetic sources are seen in this direction. Aims. In this paper we analyze the gamma-ray emission measured by the Fermi Large Area Telescope (LAT) in the energy range from 100 MeV to 100 GeV in order to probe the gas and cosmic-ray content on the scale of the whole Cygnus complex. The gamma-ray emission on the scale of the central massive stellar clusters and from individual sources is addressed elsewhere. Methods. The signal from bright pulsars is greatly reduced by selecting photons in their off-pulse phase intervals. We compare the diffuse gamma-ray emission with interstellar gas maps derived from radio/mm-wave lines and visual extinction data. A general model of the region, including other pulsars and gamma-ray sources, is sought. Results. The integral HI emissivity above 100 MeV averaged over the whole Cygnus complex amounts to [2.06 +/- 0.11 (stat.) (+0.15)(-0.84) (syst.)] x 10(-26) photons s(-1) sr(-1) H-atom(-1), where the systematic error is dominated by the uncertainty on the HI opacity to calculate its column densities. The integral emissivity and its spectral energy distribution are both consistent within the systematics with LAT measurements in the interstellar space near the solar system. The average X-CO = N(H-2)/W-CO ratio is found to be [1.68 +/- 0.05 (stat.) (+0.87)(-0.10) (H I opacity)] x 10(20) molecules cm(-2) (K km s(-1))(-1), consistent with other LAT measurements in the Local Arm. We detect significant gamma-ray emission from dark neutral gas for a mass corresponding to similar to 40% of what is traced by CO. The total interstellar mass in the Cygnus complex inferred from its gamma-ray emission amounts to 8 (+5)(-1) x 10(6) M-circle dot at a distance of 1.4 kpc. Conclusions. Despite the conspicuous star formation activity and high masses of the interstellar clouds, the cosmic-ray population in the Cygnus complex averaged over a few hundred parsecs is similar to that of the local interstellar space. C1 [Ackermann, M.; Ajello, M.; Allafort, A.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Allafort, A.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.; Tibaldo, L.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA,IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Belfiore, A.; Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, 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.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [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.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Fortin, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain. [Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA. [Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France. [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.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Dumora, D.; Lott, B.; Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Fukazawa, Y.; Hanabata, Y.; Hayashi, K.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Harding, A. K.; Hays, E.; McEnery, J. E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Katagiri, H.] Ibaraki Univ, Coll Sci, Bunkyo Ku, Mito, Ibaraki 3108512, Japan. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, UPS, OMP, IRAP, Toulouse, France. [Lee, S. -H.] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan. [Martin, P.; Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.] 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. [Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Parent, D.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Torres, D. F.] ICREA, Barcelona, Spain. [Tramacere, A.; Vianello, G.] CIFS, I-10133 Turin, Italy. [Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. [Troja, E.] NASA, Postdoctoral Program, Greenbelt, MD 20771 USA. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, S-10691 Stockholm, Sweden. [Yang, Z.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, S-10691 Stockholm, Sweden. [Bontemps, S.] Univ Bordeaux, CNRS, INSU, Lab Astrophys Bordeaux, Floirac, France. RP Ackermann, M (reprint author), Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. EM isabelle.grenier@cea.fr; luigi.tibaldo@pd.infn.it RI Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; Hays, Elizabeth/D-3257-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Tosti, Gino/E-9976-2013; Saz Parkinson, Pablo Miguel/I-7980-2013; Ozaki, Masanobu/K-1165-2013; Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Rando, Riccardo/M-7179-2013; Loparco, Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; OI Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Loparco, Francesco/0000-0002-1173-5673; Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Giordano, Francesco/0000-0002-8651-2394; De Angelis, Alessandro/0000-0002-3288-2517; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; Rando, Riccardo/0000-0001-6992-818X FU National Aeronautics and Space Administration; Department of Energy in the US; 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; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; Natural Sciences and Engineering Research Council of Canada 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 US, 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. We made use of data from the Canadian Galactic Plane Survey (CGPS). CGPS is a Canadian project with international partners. The Dominion Radio Astrophysical Observatory is operated as a national facility by the National Research Council of Canada. The CGPS is supported by a grant from the Natural Sciences and Engineering Research Council of Canada. We thank T. M. Dame for providing the moment-masked CO data. NR 72 TC 17 Z9 17 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR A71 DI 10.1051/0004-6361/201117539 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100071 ER PT J AU Blanchard, JM Lovell, JEJ Ojha, R Kadler, M Dickey, JM Edwards, PG AF Blanchard, J. M. Lovell, J. E. J. Ojha, R. Kadler, M. Dickey, J. M. Edwards, P. G. TI High resolution rapid response observations of compact radio sources with the Ceduna Hobart Interferometer (CHI) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation: interferometers; galaxies: jets; quasars: general; galaxies: active; galaxies: nuclei; gamma rays: galaxies ID ACTIVE GALACTIC NUCLEI; SCINTILLATION-INDUCED VARIABILITY; VLBI; QUASARS; JETS; CAPABILITIES; TELESCOPE; BLAZARS; OBJECTS AB Context. Frequent, simultaneous observations across the electromagnetic spectrum are essential to the study of a range of astrophysical phenomena including active galactic nuclei. A key tool of such studies is the ability to observe an object when it flares i.e. exhibits a rapid and significant increase in its flux density. Aims. We describe the specific observational procedures and the calibration techniques that have been developed and tested to create a single baseline radio interferometer that can rapidly observe a flaring object. This is the only facility that is dedicated to rapid high resolution radio observations of an object south of -30 degrees declination. An immediate application is to provide rapid contemporaneous radio coverage of AGN flaring at gamma-ray frequencies detected by the Fermi Gamma-ray Space Telescope. Methods. A single baseline interferometer, the Ceduna Hobart Interferometer (CHI), was formed with radio telescopes in Hobart, Tasmania and Ceduna, South Australia. A software correlator was set up at the University of Tasmania to correlate these data. Results. Measurements of the flux densities of flaring objects can be made using our observing strategy within half an hour of a triggering event. These observations can be calibrated with amplitude errors better than 15%. Lower limits to the brightness temperatures of the sources can also be calculated using CHI. C1 [Blanchard, J. M.; Lovell, J. E. J.; Dickey, J. M.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Blanchard, J. M.; Edwards, P. G.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Kadler, M.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Ojha, R.] Catholic Univ Amer, Dept Phys, IACS, Washington, DC 20064 USA. [Kadler, M.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Kadler, M.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte, D-96049 Bamberg, Germany. [Kadler, M.] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany. [Kadler, M.] Univ Space Res Assoc, Columbia, MD 21044 USA. RP Blanchard, JM (reprint author), Univ Tasmania, Sch Math & Phys, Private Bag 37, Hobart, Tas 7001, Australia. EM jayb@utas.edu.au RI Dickey, John/C-6156-2013; OI Dickey, John/0000-0002-6300-7459; Kadler, Matthias/0000-0001-5606-6154 FU NASA through Fermi Guest Investigator [NNH09ZDA001N, 31263]; NASA at the Goddard Space Flight Center FX We are extremely grateful to Simon Ellingsen of the University of Tasmania for providing the V255 PKS B1934-638 data essential to the proper calibration of CHI. This research was funded in part by NASA through Fermi Guest Investigator grant NNH09ZDA001N (proposal number 31263). This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This research has made use of data from the NASA/IPAC Extragalactic Database (NED, operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration); and the SIMBAD database (operated at CDS, Strasbourg, France). This research has made use of NASA's Astrophysics Data System. This research has made use of the United States Naval Observatory (USNO) Radio Reference Frame Image Database (RRFID). NR 30 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 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR A150 DI 10.1051/0004-6361/201117593 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100150 ER PT J AU Farinelli, R Ceccobello, C Romano, P Titarchuk, L AF Farinelli, R. Ceccobello, C. Romano, P. Titarchuk, L. TI Numerical solution of the radiative transfer equation: X-ray spectral formation from cylindrical accretion onto a magnetized neutron star SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: numerical; X-rays: binaries; radiative transfer; magnetic fields ID CONVERGING FLUID-FLOW; COMPTONIZATION MODEL; DOMINATED SHOCK; BLACK-HOLES; POWER-LAW; SCATTERING; BINARIES; PULSARS; INDEX; BULK AB Context. Predicting the emerging X-ray spectra in several astrophysical objects is of great importance, in particular when the observational data are compared with theoretical models. This requires developing numerical routines for the solution of the radiative equation according to the expected physical conditions of the systems under study. Aims. We have developed an algorithm solving the radiative transfer equation in the Fokker-Planck approximation when both thermal and bulk Comptonization take place. The algorithm is essentially a relaxation method, where stable solutions are obtained when the system has reached its steady-state equilibrium. Methods. We obtained the solution of the radiative transfer equation in the two-dimensional domain defined by the photon energy E and optical depth of the system tau using finite-differences for the partial derivatives, and imposing specific boundary conditions for the solutions. We treated the case of cylindrical accretion onto a magnetized neutron star. Results. We considered a blackbody seed spectrum of photons with exponential distribution across the accretion column and for an accretion where the velocity reaches its maximum at the stellar surface and at the top of the accretion column, respectively. In both cases higher values of the electron temperature and of the optical depth tau produce flatter and harder spectra. Other parameters contributing to the spectral formation are the steepness of the vertical velocity profile, the albedo at the star surface, and the radius of the accretion column. The latter parameter modifies the emerging spectra in a specular way for the two assumed accretion profiles. Conclusions. The algorithm has been implemented in the xspec package for X-ray spectral fitting and is specifically dedicated to the physical framework of accretion at the polar cap of a neutron star with a high magnetic field (greater than or similar to 10(12) G). This latter case is expected to be typical of accreting systems such as X-ray pulsars and supergiant fast X-ray transients. C1 [Farinelli, R.; Romano, P.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-90146 Palermo, Italy. [Farinelli, R.; Ceccobello, C.; Titarchuk, L.] Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy. [Titarchuk, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Farinelli, R (reprint author), Ist Astrofis Spaziale & Fis Cosm, INAF, Via U La Malfa 153, I-90146 Palermo, Italy. EM farinelli@ifc.inaf.it FU [ASI-INAF I/009/10/0] FX We acknowledge financial contribution from the agreement ASI-INAF I/009/10/0. NR 14 TC 15 Z9 15 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR A67 DI 10.1051/0004-6361/201118008 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100067 ER PT J AU Guelbenzu, AN Klose, S Kruhler, T Greiner, J Rossi, A Kann, DA Olivares, F Rau, A Afonso, PMJ Elliott, J Filgas, R Yoldas, AK McBreen, S Nardini, M Schady, P Schmidl, S Sudilovsky, V Updike, AC Yoldas, A AF Guelbenzu, A. Nicuesa Klose, S. Kruehler, T. Greiner, J. Rossi, A. Kann, D. A. Olivares, F. Rau, A. Afonso, P. M. J. Elliott, J. Filgas, R. Yoldas, A. Kuepcue McBreen, S. Nardini, M. Schady, P. Schmidl, S. Sudilovsky, V. Updike, A. C. Yoldas, A. TI The late-time afterglow of the extremely energetic short burst GRB 090510 revisited SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: individual: GRB 090510 ID GAMMA-RAY BURSTS; OPTICAL AFTERGLOWS; HOST GALAXIES; EMISSION; SWIFT; ORIGIN; GROND; FERMI AB Context. The Swift discovery of the short burst GRB 090510 has raised considerable attention mainly because of two reasons: first, it had a bright optical afterglow, and second it is among the most energetic events detected so far within the entire GRB population (long plus short). The afterglow of GRB 090510 was observed with Swift/UVOT and Swift/XRT and evidence of a jet break around 1.5 ks after the burst has been reported in the literature, implying that after this break the optical and X-ray light curve should fade with the same decay slope. Aims. As noted by several authors, the post-break decay slope seen in the UVOT data is much shallower than the steep decay in the X-ray band, pointing to a (theoretically hard to understand) excess of optical flux at late times. We assess here the validity of this peculiar behavior. Methods. We reduced and analyzed new afterglow light-curve data obtained with the multichannel imager GROND. These additional g' r' i' z data were then combined with the UVOT and XRT data to study the behavior of the afterglow at late times more stringently. Results. Based on the densely sampled data set obtained with GROND, we find that the optical afterglow of GRB 090510 did indeed enter a steep decay phase starting around 22 ks after the burst. During this time the GROND optical light curve is achromatic, and its slope is identical to the slope of the X-ray data. In combination with the UVOT data this implies that a second break must have occurred in the optical light curve around 22 ks post burst, which, however, has no obvious counterpart in the X-ray band, contradicting the interpretation that this could be another jet break. Conclusions. The GROND data provide the missing piece of evidence that the optical afterglow of GRB 090510 did follow a post-jet break evolution at late times. The break seen in the optical light curve around 22 ks in combination with its missing counterpart in the X-ray band could be due to the passage of the injection frequency across the optical bands, as already theoretically proposed in the literature. This is possibly the first time that this passage has been clearly seen in an optical afterglow. In addition, our results imply that there is no more evidence for an excess of flux in the optical bands at late times. C1 [Guelbenzu, A. Nicuesa; Klose, S.; Rossi, A.; Kann, D. A.; Schmidl, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Kruehler, T.; Greiner, J.; Olivares, F.; Rau, A.; Afonso, P. M. J.; Elliott, J.; Filgas, R.; Nardini, M.; Schady, P.; Sudilovsky, V.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kruehler, T.] Tech Univ Munich, D-85748 Garching, Germany. [Kruehler, T.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Afonso, P. M. J.] Amer River Coll, Dept Phys & Astron, Sacramento, CA 95841 USA. [Yoldas, A. Kuepcue; Yoldas, A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [McBreen, S.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Updike, A. C.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Updike, A. C.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA. [Updike, A. C.] NASA, Observat Cosmol Lab, GSFC, Greenbelt, MD 20771 USA. [Updike, A. C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Guelbenzu, AN (reprint author), Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany. EM ana@tls-tautenburg.de RI Rossi, Andrea/N-4674-2015; OI Rossi, Andrea/0000-0002-8860-6538; Kruehler, Thomas/0000-0002-8682-2384 FU MPE; DFG [SA 2001/2-1, SA 2001/1-1]; DAAD; Leibniz-Prize (DFG) [HA 1850/28-1]; [DFG K1 766/16-1] FX A.N.G., D.A.K., and S.K. acknowledge support by grant DFG K1 766/16-1. A.N.G., A.R., D.A.K., and A.U. are grateful for travel funding support through the MPE. T.K. acknowledges funding by the DFG cluster of excellence "Origin and Structure of the Universe", F.O.E. funding of his Ph.D. through the DAAD, M.N. support by DFG grant SA 2001/2-1 and P.S. by DFG grant SA 2001/1-1. Part of the funding for GROND (both hardware and personnel) was generously granted by the Leibniz-Prize to G. Hasinger (DFG grant HA 1850/28-1). This work made use of data supplied by the UK Swift science data center at the University of Leicester. We thank the referee for a rapid reply and a careful reading of the manuscript. NR 38 TC 12 Z9 12 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR L7 DI 10.1051/0004-6361/201118416 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100160 ER PT J AU Kunneriath, D Eckart, A Vogel, SN Teuben, P Muzic, K Schodel, R Garcia-Marin, M Moultaka, J Staguhn, J Straubmeier, C Zensus, JA Valencia, M Karas, V AF Kunneriath, D. Eckart, A. Vogel, S. N. Teuben, P. Muzic, K. Schoedel, R. Garcia-Marin, M. Moultaka, J. Staguhn, J. Straubmeier, C. Zensus, J. A. Valencia-S, M. Karas, V. TI The Galactic centre mini-spiral in the mm-regime SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; black hole physics; Galaxy: nucleus; radio continuum: general; Galaxy: center ID SAGITTARIUS-A-ASTERISK; DUST-EMBEDDED SOURCES; NUCLEAR STAR CLUSTER; MASSIVE BLACK-HOLE; CENTRAL PARSEC; SGR-A; IONIZED-GAS; INFRARED OBSERVATIONS; CIRCUMNUCLEAR DISK; SPECTROSCOPY AB Context. The mini-spiral is a feature of the interstellar medium in the central similar to 2 pc of the Galactic center. It is composed of several streamers of dust and ionised and atomic gas with temperatures between a few 100 K to 10(4) K. There is evidence that these streamers are related to the so-called circumnuclear disk of molecular gas and are ionized by photons from massive, hot stars in the central parsec. Aims. We attempt to constrain the emission mechanisms and physical properties of the ionized gas and dust of the mini-spiral region with the help of our multiwavelength data sets. Methods. Our observations were carried out at 1.3 mm and 3 mm with the mm interferometric array CARMA in California in March and April 2009, with the MIR instrument VISIR at ESO's VLT in June 2006, and the NIR Br gamma with VLT NACO in August 2009. Results. We present high resolution maps of the mini-spiral, and obtain a spectral index of 0.5 +/- 0.25 for Sgr A*, indicating an inverted synchrotron spectrum. We find electron densities within the range 0.8-1.5 x 10(4) cm(-3) for the mini-spiral from the radio continuum maps, along with a dust mass contribution of similar to 0.25 M-circle dot from the MIR dust continuum, and extinctions ranging from 1.8-3 at 2.16 mu m in the Br gamma line. Conclusions. We observe a mixture of negative and positive spectral indices in our 1.3 mm and 3 mm observations of the extended emission of the mini-spiral, which we interpret as evidence that there are a range of contributions to the thermal free-free emission by the ionized gas emission and by dust at 1.3 mm. C1 [Kunneriath, D.; Eckart, A.; Garcia-Marin, M.; Straubmeier, C.; Zensus, J. A.; Valencia-S, M.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Kunneriath, D.; Eckart, A.; Zensus, J. A.; Valencia-S, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kunneriath, D.; Karas, V.] Acad Sci Czech Republic, Inst Astron, Prague 14100, Czech Republic. [Vogel, S. N.; Teuben, P.; Staguhn, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Muzic, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Schoedel, R.] CSIC, Inst Astrofis Andalucia, Madrid 18008, Spain. [Moultaka, J.] Univ Toulouse, LATT, CNRS, F-31400 Toulouse, France. [Staguhn, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Staguhn, J.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Kunneriath, D (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM devaky@astro.cas.cz RI Schoedel, Rainer/D-4751-2014; Karas, Vladimir/C-1559-2013; Kunneriath, Devaky/G-8513-2014 OI Schoedel, Rainer/0000-0001-5404-797X; Karas, Vladimir/0000-0002-5760-0459; FU Ministerio de Ciencia y Innovacion of the government of Spain; German federal department for education and research ( BMBF) [50OS0502, 50OS0801]; COST Action [MP0905]; PECS [98040] FX D. Kunneriath and M. Valencia-S. are members of the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the MPIfR and the Universities of Bonn and Cologne. R.S. acknowledges support by the Ramon y Cajal programme by the Ministerio de Ciencia y Innovacion of the government of Spain. Macarena Garcia-Marin is supported by the German federal department for education and research (BMBF) under the project numbers: 50OS0502 and 50OS0801. Part of this work was supported by the COST Action MP0905: Black Holes in a violent Universe and PECS project No. 98040. This research has made use of NASA's Astrophysics Data System. NR 50 TC 10 Z9 10 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR A127 DI 10.1051/0004-6361/201117676 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100127 ER PT J AU Kylafis, ND Contopoulos, I Kazanas, D Christodoulou, DM AF Kylafis, N. D. Contopoulos, I. Kazanas, D. Christodoulou, D. M. TI Formation and destruction of jets in X-ray binaries SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: neutron; accretion, accretion disks; black holes physics; X-rays: binaries; magnetic fields ID BLACK-HOLE BINARIES; ADVECTION-DOMINATED ACCRETION; NEUTRON-STAR; HARD STATE; LOW/HARD STATE; COSMIC BATTERY; AQUILA X-1; MILLISECOND PULSAR; MHD SIMULATIONS; RADIO-EMISSION AB Context. Neutron-star and black-hole X-ray binaries (XRBs) exhibit radio jets, whose properties depend on the X-ray spectral state and history of the source. In particular, black-hole XRBs emit compact, steady radio jets when they are in the so-called hard state. These jets become eruptive as the sources move toward the soft state, disappear in the soft state, and then re-appear when the sources return to the hard state. The jets from neutron-star X-ray binaries are typically weaker radio emitters than the black-hole ones at the same X-ray luminosity and in some cases radio emission is detected in the soft state. Aims. Significant phenomenology has been developed to describe the spectral states of neutron-star and black-hole XRBs, and there is general agreement about the type of the accretion disk around the compact object in the various spectral states. We investigate whether the phenomenology describing the X-ray emission on one hand and the jet appearance and disappearance on the other can be put together in a consistent physical picture. Methods. We consider the so-called Poynting-Robertson cosmic battery (PRCB), which has been shown to explain in a natural way the formation of magnetic fields in the disks of AGNs and the ejection of jets. We investigate whether the PRCB can also explain the formation, destruction, and variability of jets in XRBs. Results. We find excellent agreement between the conditions under which the PRCB is efficient (i.e., the type of the accretion disk) and the emission or destruction of the radio jet. Conclusions. The disk-jet connection in XRBs can be explained in a natural way using the PRCB. C1 [Kylafis, N. D.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Kylafis, N. D.] Inst Theoret & Computat Phys, Iraklion 71003, Crete, Greece. [Kylafis, N. D.] Fdn Res & Technol Hellas, Iraklion 71110, Crete, Greece. [Contopoulos, I.] Acad Athens, Res Ctr Astron, Athens 11527, Greece. [Kazanas, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Christodoulou, D. M.] Univ Massachusetts Lowell, Dept Math Sci, Lowell, MA 01854 USA. RP Kylafis, ND (reprint author), Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. EM kylafis@physics.uoc.gr RI Kylafis, Nikolaos/C-4555-2011 OI Kylafis, Nikolaos/0000-0003-0928-0996 FU EU [39965]; EU REGPOT [206469] FX This research has been supported in part by EU Marie Curie project No. 39965, and EU REGPOT project number 206469. N.D.K. thanks Tomaso Belloni for providing hardness-intensity data of GX 339-4 during various outbursts and Michiel van der Klis and Dimitrios Psaltis for useful discussions concerning millisecond pulsars. I.C. thanks Maxim Lyutikov, Ramesh Narayan, Roman Shcherbakov, and Sasha Tchekhovskoy for discussions concerning accretion disks and the PRCB. NR 76 TC 11 Z9 11 U1 0 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR A5 DI 10.1051/0004-6361/201117052 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100005 ER PT J AU Martins, F Escolano, C Wade, GA Donati, JF Bouret, JC AF Martins, F. Escolano, C. Wade, G. A. Donati, J. F. Bouret, J. C. CA MiMeS Collaboration TI Observational effects of magnetism in O stars: surface nitrogen abundances SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: massive; stars: atmospheres; stars: fundamental parameters; stars: abundances; stars: magnetic field ID DRIVEN STELLAR WINDS; THETA(1) ORIONIS-C; VLT-FLAMES SURVEY; B-TYPE STARS; MASSIVE STARS; DIFFERENTIAL ROTATION; DYNAMICAL SIMULATIONS; LINE SPECTROSCOPY; MAGELLANIC-CLOUD; LUMINOUS STARS AB Aims. We investigate the surface nitrogen content of the six magnetic O stars known to date as well as of the early B-type star tau Sco. We compare these abundances to predictions of evolutionary models to isolate the effects of magnetic field on the transport of elements in stellar interiors. Methods. We conduct a quantitative spectroscopic analysis of the sample stars with state-of-the-art atmosphere models. We rely on high signal-to-noise ratio, high resolution optical spectra obtained with ESPADONS at CFHT and NARVAL at TBL. Atmosphere models and synthetic spectra are computed with the code CMFGEN. Values of N/H together with their uncertainties are determined and compared to predictions of evolutionary models. Results. We find that the magnetic stars can be divided into two groups: one with stars displaying no N enrichment (one object); and one with stars most likely showing extra N enrichment (5 objects). For one star (Theta(1) Ori C) no robust conclusion can be drawn due to its young age. The star with no N enrichment is the one with the weakest magnetic field, possibly of dynamo origin. It might be a star having experienced strong magnetic braking under the condition of solid body rotation, but its rotational velocity is still relatively large. The five stars with high N content were probably slow rotators on the zero age main sequence, but they have surface N/H typical of normal O stars, indicating that the presence of a (probably fossil) magnetic field leads to extra enrichment. These stars may have a strong differential rotation inducing shear mixing. Our results should be viewed as a basis on which new theoretical simulations can rely to better understand the effect of magnetism on the evolution of massive stars. C1 [Martins, F.; Escolano, C.] CNRS, LUPM UMR 5299, F-34095 Montpellier 05, France. [Martins, F.; Escolano, C.] Univ Montpellier 2, F-34095 Montpellier 05, France. [Wade, G. A.] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada. [Donati, J. F.] CNRS, IRAP UMR 5277, F-31400 Toulouse, France. [Donati, J. F.] Univ Toulouse 3, F-31400 Toulouse, France. [Escolano, C.; Bouret, J. C.] CNRS, LAM UMR 6110, F-13388 Marseille 13, France. [Escolano, C.; Bouret, J. C.] Univ Aix Marseille 1, F-13388 Marseille 13, France. [Bouret, J. C.] NASA GSFC, Greenbelt, MD 20771 USA. RP Martins, F (reprint author), CNRS, LUPM UMR 5299, Pl Eugene Bataillon, F-34095 Montpellier 05, France. EM fabrice.martins@univ-montp2.fr FU Natural Science and Engineering Research Council of Canada FX We thank the referee, Jo Puls, for valuable comments and for suggesting to add the star tau Sco to our sample. Many thanks to John Hillier for making his code CMFGEN available and for constant help with it. G. A. W. acknowledges Discovery Grant support from the Natural Science and Engineering Research Council of Canada. NR 67 TC 22 Z9 22 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR A29 DI 10.1051/0004-6361/201118039 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100029 ER PT J AU Masson, S Demoulin, P Dasso, S Klein, KL AF Masson, S. Demoulin, P. Dasso, S. Klein, K. -L. TI The interplanetary magnetic structure that guides solar relativistic particles SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE solar-terrestrial relations; Sun: heliosphere; methods: data analysis ID CORONAL MASS EJECTIONS; ADVANCED COMPOSITION EXPLORER; COSMIC-RAY EVENT; ENERGETIC PARTICLES; CURRENT SHEETS; RELEASE TIMES; KEV ELECTRONS; FLUX ROPE; ACCELERATION; PROTONS AB Context. Relating in-situ measurements of relativistic solar particles to their parent activity in the corona requires understanding the magnetic structures that guide them from their acceleration site to the Earth. Relativistic particle events are observed at times of high solar activity, when transient magnetic structures such as interplanetary coronal mass ejections (ICMEs) often shape the interplanetary magnetic field (IMF). They may introduce interplanetary paths that are longer than nominal, and magnetic connections rooted far from the nominal Parker spiral. Aims. We present a detailed study of the IMF configurations during ten relativistic solar particle events of the 23rd activity cycle to elucidate the actual IMF configuration that guides the particles to the Earth, where they are measured by neutron monitors. Methods. We used magnetic field (MAG) and plasma parameter measurements (SWEPAM) from the ACE spacecraft and determined the interplanetary path lengths of energetic particles through a modified version of the velocity dispersion analysis based on energetic particle measurements with SoHO/ERNE. Results. We find that the majority (7/10) of the events is detected in the vicinity of an ICME. Their interplanetary path lengths are found to be longer (1.5-2.6 AU) than those of the two events propagating in the slow solar wind (1.3 AU). The longest apparent path length is found in an event within the fast solar wind, probably caused by enhanced pitch angle scattering. The derived path lengths imply that the first energetic and relativistic protons are released at the Sun at the same time as electron beam emitting type III radio bursts. Conclusions. The timing of the first high-energy particle arrival on Earth is mainly determined by the type of IMF in which the particles propagate. Initial arrival times are as expected from Parker's model in the slow solar wind, and significantly longer in or near transient structures such as ICMEs. C1 [Masson, S.; Demoulin, P.; Klein, K. -L.] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92190 Meudon, France. [Dasso, S.] CONICET UBA, Inst Astron & Fis Espacio, Buenos Aires, DF, Argentina. [Dasso, S.] UBA, Fac Ciencias Exactas & Nat, Dept Fis, Buenos Aires, DF, Argentina. RP Masson, S (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM sophie.masson@nasa.gov OI Demoulin, Pascal/0000-0001-8215-6532 FU ECOS-Sud [A08U01]; Abdus Salam International Centre for Theoretical Physics (ICTP); Delegation Generale pour l'Armement (DGA); NASA; European Commission through the FP6 SOLAIRE Network [MTRN-CT-2006-035484]; [UBACyT 20020090100264]; [PIP 11220090100825/10]; [PICT-2007-00856] FX The authors gratefully acknowledge R. Wimmer-Schweingruber and A. Balogh for helpful discussions on the contents of this paper. This research has made use of NASA's Space Physics Data Facility (SPDF). We thank the ACE instrument teams and their respective principal investigators, namely N. F. Ness (ACE/MAG) and D. J. McComas (ACE/SWEPAM). The authors acknowledge financial support from ECOS-Sud through their cooperative science program (No. A08U01). This work was partially supported by the Argentinean grants: UBACyT 20020090100264 (UBA), PIP 11220090100825/10 (CONICET), and PICT-2007-00856 (ANPCyT). S. D. acknowledges support from the Abdus Salam International Centre for Theoretical Physics (ICTP), as provided in the frame of his regular associateship. S. D. is member of the Carrera del Investigador Cientifico, CONICET. The work of S. M. is funded by a fellowship of Delegation Generale pour l'Armement (DGA). S. M. thank the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA for financial support. Financial support by the European Commission through the FP6 SOLAIRE Network (MTRN-CT-2006-035484) is gratefully acknowledged. We thank E. Valtonen for his very helpful assistance with the ERNE data. NR 58 TC 17 Z9 17 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR A32 DI 10.1051/0004-6361/201118145 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100032 ER PT J AU Rau, A Schady, P Greiner, J Salvato, M Ajello, M Bottacini, E Gehrels, N Afonso, PMJ Elliott, J Filgas, R Kann, DA Klose, S Kruhler, T Nardini, M Guelbenzu, AN Olivares, F Rossi, A Sudilovsky, V Updike, AC Hartmann, DH AF Rau, A. Schady, P. Greiner, J. Salvato, M. Ajello, M. Bottacini, E. Gehrels, N. Afonso, P. M. J. Elliott, J. Filgas, R. Kann, D. A. Klose, S. Kruehler, T. Nardini, M. Guelbenzu, A. Nicuesa Olivares E, F. Rossi, A. Sudilovsky, V. Updike, A. C. Hartmann, D. H. TI BL Lacertae objects beyond redshift 1.3-UV-to-NIR photometry and photometric redshift for Fermi/LAT blazars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: distances and redshifts; techniques: photometric; BL Lacertae objects: general ID LARGE-AREA TELESCOPE; OPTICAL VARIABILITY; CAMPAIGN; CATALOG; MISSION; STARS; GROND AB Context. Observations of the.-ray sky with Fermi led to significant advances towards understanding blazars, the most extreme class of active galactic nuclei. A large fraction of the population detected by Fermi is formed by BL Lacertae (BL Lac) objects, whose sample has always suffered from a severe redshift incompleteness due to the quasi-featureless optical spectra. Aims. Our goal is to provide a significant increase of the number of confirmed high-redshift BL Lac objects contained in the 2 LAC Fermi/LAT cataloge. Methods. For 103 Fermi/LAT blazars, photometric redshifts using spectral energy distribution fitting have been obtained. The photometry includes 13 broad-band filters from the far ultraviolet to the near-IR observed with Swift/UVOT and the multi-channel imager GROND at the MPG/ESO 2.2 m telescope. Data have been taken quasi-simultaneously and the remaining source-intrinsic variability has been corrected for. Results. We release the UV-to-near-IR 13-band photometry for all 103 sources and provide redshift constraints for 75 sources without previously known redshift. Out of those, eight have reliable photometric redshifts at z greater than or similar to 1.3, while for the other 67 sources we provide upper limits. Six of the former eight are BL Lac objects, which quadruples the sample of confirmed high-redshift BL Lac. This includes three sources with redshifts higher than the previous record for BL Lac, including CRATES J0402-2615, with the best-fit solution at z approximate to 1.9. C1 [Rau, A.; Schady, P.; Greiner, J.; Afonso, P. M. J.; Elliott, J.; Filgas, R.; Kruehler, T.; Nardini, M.; Olivares E, F.; Sudilovsky, V.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Salvato, M.] Max Planck Inst Plasma Phys & Excellence Cluster, D-85748 Garching, Germany. [Salvato, M.; Kruehler, T.] Tech Univ Munich, D-85748 Garching, Germany. [Ajello, M.; Bottacini, E.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Ajello, M.; Bottacini, E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Ajello, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Afonso, P. M. J.] Amer River Coll, Phys & Astron Dpt, Sacramento, CA 95841 USA. [Kann, D. A.; Klose, S.; Guelbenzu, A. Nicuesa; Rossi, A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Kruehler, T.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Nardini, M.] Univ Milano Bicocca, I-20126 Milan, Italy. [Updike, A. C.] Dickinson Coll, Dept Phys & Astron, Carlisle, PA 17013 USA. [Hartmann, D. H.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. RP Rau, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. EM arau@mpe.mpg.de RI Gehrels, Neil/D-2971-2012; OI Kruehler, Thomas/0000-0002-8682-2384 FU DFG [HA 1850/28-1, Kl 766/16-1, SA 2001/2-1, SA 2001/1-1]; German Deutsche Forschungsgemeinschaft, DFG [FKZ HA 1850/28-1]; DFG cluster of excellence Origin and Structure of the Universe; European Commission; DARK: The Dark Cosmology Centre; Danish National Research Foundation; Deutscher Akademischer Austausch-Dienst (DAAD); BLANCEFLOR Boncompagni-Ludovisi, ne Bildt foundation; MPE FX We thank the referee for the valuable comments. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). M. S. acknowledges support by the German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize (FKZ HA 1850/28-1). T. K. acknowledges support by the DFG cluster of excellence Origin and Structure of the Universe, by the European Commission under the Marie Curie Intra-European Fellowship Programme), as well as the DARK: The Dark Cosmology Centre, funded by the Danish National Research Foundation. F.O.E. acknowledges funding of his Ph.D. through the Deutscher Akademischer Austausch-Dienst (DAAD). S. K., D. A. K. and A.N.G acknowledge support by DFG grant Kl 766/16-1. ARossi acknowledges support from the BLANCEFLOR Boncompagni-Ludovisi, ne Bildt foundation. M.N. acknowledges support by DFG grant SA 2001/2-1. P. S. acknowledges support by DFG grant SA 2001/1-1. A. C. U., A.N.G., D. A. K. and ARossi are grateful for travel funding support through MPE. We also acknowledge the use of the TOPCAT tool (Taylor 2005). NR 41 TC 33 Z9 33 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR A26 DI 10.1051/0004-6361/201118159 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100026 ER PT J AU Riviere-Marichalar, P Menard, F Thi, WF Kamp, I Montesinos, B Meeus, G Woitke, P Howard, C Sandell, G Podio, L Dent, WRF Mendigutia, I Pinte, C White, GJ Barrado, D AF Riviere-Marichalar, P. Menard, F. Thi, W. F. Kamp, I. Montesinos, B. Meeus, G. Woitke, P. Howard, C. Sandell, G. Podio, L. Dent, W. R. F. Mendigutia, I. Pinte, C. White, G. J. Barrado, D. TI Detection of warm water vapour in Taurus protoplanetary discs by Herschel SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; protoplanetary disks; astrobiology; molecular data; line: identification ID CIRCUMSTELLAR DISKS; STATISTICAL-METHODS; ORGANIC-MOLECULES; ASTRONOMICAL DATA; FORMING REGION; SPITZER SURVEY; UPPER LIMITS; STARS; H2O; EXCITATION AB Line spectra of 68 Taurus T Tauri stars were obtained with the Herschel-PACS (Photodetector Array Camera and Spectrometer) instrument as part of the GASPS (GAS evolution in Protoplanetary Systems) survey of protoplanetary discs. A careful examination of the linescans centred on the [OI] 63.18 mu m fine-structure line unveiled a line at 63.32 mu m in some of these spectra. We identify this line with the 8(18) -> 7(07) transition of ortho-water. It is detected confidently (i.e., > 3 sigma) in eight sources, i.e., similar to 24% of the sub-sample with gas-rich discs. Several statistical tests were used to search for correlations with other disc and stellar parameters such as line fluxes of [OI] 6300 angstrom and 63.18 mu m; X-ray luminosity and continuum levels at 63 mu m and 850 mu m. Correlations are found between the water line fluxes and the [OI] 63.18 mu m line luminosity, the dust continuum, and possibly with the stellar X-ray luminosity. This is the first time that this line of warm water vapour has been detected in protoplanetary discs. We discuss its origins, in particular whether it comes from the inner disc and/or disc surface or from shocks in outflows and jets. Our analysis favours a disc origin, with the observed water vapour line produced within 2-3 AU from the central stars, where the gas temperature is of the order of 500-600 K. C1 [Riviere-Marichalar, P.; Montesinos, B.; Mendigutia, I.; Barrado, D.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Villanueva De La Canada 28691, Spain. [Menard, F.; Thi, W. F.; Pinte, C.] UJF Grenoble 1, CNRS INSU, Inst Planetol & Astrophys IPAG, UMR 5274, F-38041 Grenoble, France. [Kamp, I.; Podio, L.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Meeus, G.] Univ Autonoma Madrid, Fac Ciencias, Dep Fis Teor, E-28049 Madrid, Spain. [Woitke, P.] Univ Vienna, Dept Astron, A-1180 Vienna, Austria. [Woitke, P.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Woitke, P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Howard, C.; Sandell, G.] NASA, SOFIA USRA, Ames Res Ctr, Washington, DC USA. [Dent, W. R. F.] ALMA, Santiago, Chile. [White, G. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [White, G. J.] Rutherford Appleton Lab, Didcot OX11 OQL, Oxon, England. [Barrado, D.] Ctr Astron Hispano Aleman, Calar Alto Observ, Almeria 04004, Spain. RP Riviere-Marichalar, P (reprint author), CSIC INTA, Dept Astrofis, Ctr Astrobiol, POB 78, Villanueva De La Canada 28691, Spain. EM riviere@cab.inta-csic.es RI Barrado Navascues, David/C-1439-2017; Montesinos, Benjamin/C-3493-2017; OI Barrado Navascues, David/0000-0002-5971-9242; Montesinos, Benjamin/0000-0002-7982-2095; Mendigutia, Ignacio/0000-0002-0233-5328 FU Spanish grants [AYA 2010-21161-C02-02, CDS2006-00070, PRICIT-S2009/ESP-1496]; ANR [ANR-07-BLAN-0221, ANR-2010-JCJC-0504-01]; CNES; PNPS of CNRS/INSU; Millennium Science Initiative (ICM) of the Chilean ministry of Economy [P10-022-F]; EC [PERG06-GA-2009-256513] FX We thank the anonymous referee for a constructive report that helped to improve the paper. This research has been funded by Spanish grants AYA 2010-21161-C02-02, CDS2006-00070 and PRICIT-S2009/ESP-1496. In France we thank ANR (contracts ANR-07-BLAN-0221 and ANR-2010-JCJC-0504-01); CNES; PNPS of CNRS/INSU. The Millennium Science Initiative (ICM) of the Chilean ministry of Economy (Nucleus P10-022-F) and an EC-FP7 grant (PERG06-GA-2009-256513) are also acknowledged. NR 32 TC 33 Z9 33 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR L3 DI 10.1051/0004-6361/201118448 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100156 ER PT J AU Tilling, I Woitke, P Meeus, G Mora, A Montesinos, B Riviere-Marichalar, P Eiroa, C Thi, WF Isella, A Roberge, A Martin-Zaidi, C Kamp, I Pinte, C Sandell, G Vacca, WD Menard, F Mendigutia, I Duchene, G Dent, WRF Aresu, G Meijerink, R Spaans, M AF Tilling, I. Woitke, P. Meeus, G. Mora, A. Montesinos, B. Riviere-Marichalar, P. Eiroa, C. Thi, W. -F. Isella, A. Roberge, A. Martin-Zaidi, C. Kamp, I. Pinte, C. Sandell, G. Vacca, W. D. Menard, F. Mendigutia, I. Duchene, G. Dent, W. R. F. Aresu, G. Meijerink, R. Spaans, M. TI Gas modelling in the disc of HD 163296 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE circumstellar matter; astrochemistry; stars: pre-main sequence; protoplanetary disks; stars: fundamental parameters; line: formation ID HERBIG-AE STARS; PRE-MAIN-SEQUENCE; FINE-STRUCTURE EXCITATION; NEAR-INFRARED EMISSION; PROTOPLANETARY DISKS; CIRCUMSTELLAR DUST; YOUNG STARS; ROTATIONAL-EXCITATION; BETA-PICTORIS; GROUND-STATE AB We present detailed model fits to observations of the disc around the Herbig Ae star HD 163296. This well-studied object has an age of similar to 4Myr, with evidence of a circumstellar disc extending out to similar to 540AU. We use the radiation thermo-chemical disc code ProDiMo to model the gas and dust in the circumstellar disc of HD 163296, and attempt to determine the disc properties by fitting to observational line and continuum data. These include new Herschel/PACS observations obtained as part of the open-time key program GASPS (GAS in Protoplanetary Systems), consisting of a detection of the [Oi] 63 mu m line and upper limits for several other far infrared lines. We complement this with continuum data and ground-based observations of the (CO)-C-12 3-2, 2-1 and (CO)-C-13 J = 1-0 line transitions, as well as an upper limit for the H-2 0-0 S(1) transition. We explore the effects of stellar ultraviolet variability and dust settling on the line emission, and on the derived disc properties. Our fitting efforts lead to derived gas/dust ratios in the range 9-100, depending on the assumptions made. We note that the line fluxes are sensitive in general to the degree of dust settling in the disc, with an increase in line flux for settled models. This is most pronounced in lines which are formed in the warm gas in the inner disc, but the low excitation molecular lines are also affected. This has serious implications for attempts to derive the disc gas mass from line observations. We derive fractional PAH abundances between 0.007 and 0.04 relative to ISM levels. Using a stellar and UV excess input spectrum based on a detailed analysis of observations, we find that the all observations are consistent with the previously assumed disc geometry. C1 [Tilling, I.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Woitke, P.] Univ Vienna, Dept Astron, A-1180 Vienna, Austria. [Woitke, P.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Woitke, P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Meeus, G.; Eiroa, C.] Univ Autonoma Madrid, Fac Ciencias, Dep Fisica Teor, E-28049 Madrid, Spain. [Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain. [Montesinos, B.; Riviere-Marichalar, P.; Mendigutia, I.] INTA CSIC, CAB, Ctr Astrobiol, Dept Astrofis, Madrid 28691, Spain. [Thi, W. -F.; Martin-Zaidi, C.; Pinte, C.; Menard, F.; Duchene, G.] UJF Grenoble 1, CNRS INSU, Inst Planetol Astrophys IPAG, UMR 5274, F-38041 Grenoble, France. [Isella, A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Roberge, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kamp, I.; Aresu, G.; Spaans, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Sandell, G.; Vacca, W. D.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Dent, W. R. F.] ESO ALMA, Santiago, Chile. [Meijerink, R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Tilling, I (reprint author), Univ Edinburgh, Royal Observ, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. EM it@roe.ac.uk RI Roberge, Aki/D-2782-2012; Montesinos, Benjamin/C-3493-2017; OI Roberge, Aki/0000-0002-2989-3725; Montesinos, Benjamin/0000-0002-7982-2095; Mendigutia, Ignacio/0000-0002-0233-5328 NR 98 TC 35 Z9 35 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR A20 DI 10.1051/0004-6361/201116919 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100020 ER PT J AU Verdini, A Grappin, R Velli, M AF Verdini, A. Grappin, R. Velli, M. TI Coronal heating in coupled photosphere-chromosphere-coronal systems: turbulence and leakage SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: numerical; Sun: corona; magnetohydrodynamics (MHD); turbulence; Sun: transition region; waves ID FLUCTUATING ENERGY-STORAGE; MHD TURBULENCE; SHELL MODELS; LOOPS; MAGNETOHYDRODYNAMICS; DYNAMICS; CASCADE AB Context. Coronal loops act as resonant cavities for low-frequency fluctuations that are transmitted from the deeper layers of the solar atmosphere. These fluctuations are amplified in the corona and lead to the development of turbulence that in turn is able to dissipate the accumulated energy, thus heating the corona. However, trapping is not perfect, because some energy leaks down to the chromosphere on a long timescale, limiting the turbulent heating. Aims. We consider the combined effects of turbulence and energy leakage from the corona to the photosphere in determining the turbulent energy level and associated heating rate in models of coronal loops, which include the chromosphere and transition region. Methods. We use a piece-wise constant model for the Alfven speed in loops and a reduced MHD-shell model to describe the interplay between turbulent dynamics in the direction perpendicular to the mean field and propagation along the field. Turbulence is sustained by incoming fluctuations that are equivalent, in the line-tied case, to forcing by the photospheric shear flows. While varying the turbulence strength, we systematically compare the average coronal energy level and dissipation in three models with increasing complexity: the classical closed model, the open corona, and the open corona including chromosphere (or three-layer model), with the last two models allowing energy leakage. Results. We find that (i) leakage always plays a role. Even for strong turbulence, the dissipation time never becomes much lower than the leakage time, at least in the three-layer model; therefore, both the energy and the dissipation levels are systematically lower than in the line-tied model; (ii) in all models, the energy level is close to the resonant prediction, i. e., assuming an effective turbulent correlation time longer than the Alfven coronal crossing time; (iii) the heating rate is close to the value given by the ratio of photospheric energy divided by the Alfven crossing time; (iv) the coronal spectral range is divided in two: an inertial range with 5/3 spectral slope, and a large-scale peak where nonlinear couplings are inhibited by trapped resonant modes; (v) in the realistic three-layer model, the two-component spectrum leads to a global decrease in damping equal to Kolmogorov damping reduced by a factor u(rms)/V-a(c) where V-a(c) is the coronal Alfven speed. C1 [Verdini, A.] Royal Observ Belgium, Solar Terr Ctr Excellence SIDC, Brussels, Belgium. [Grappin, R.] Observ Paris, LUTH, Meudon, France. [Grappin, R.] Ecole Polytech, LPP, Palaiseau, France. [Velli, M.] CALTECH, JPL, Pasadena, CA 91125 USA. RP Verdini, A (reprint author), Royal Observ Belgium, Solar Terr Ctr Excellence SIDC, Brussels, Belgium. EM verdini@oma.be FU Belgian Federal Science Policy Office through the ESA-PRODEX; National Aeronautics and Space Administration FX We benefited from useful discussions with G. Belmont. A. V. acknowledges support from the Belgian Federal Science Policy Office through the ESA-PRODEX program. The research described in this paper was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 19 TC 15 Z9 15 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR A70 DI 10.1051/0004-6361/201118046 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100070 ER PT J AU Yong, A Hough, SE Iwahashi, J Braverman, A AF Yong, Alan Hough, Susan E. Iwahashi, Junko Braverman, Amy TI A Terrain-Based Site-Conditions Map of California with Implications for the Contiguous United States SO BULLETIN OF THE SEISMOLOGICAL SOCIETY OF AMERICA LA English DT Article ID SHEAR-WAVE VELOCITY; SEISMIC GROUND-MOTION; SAN-FRANCISCO-BAY; SATELLITE DATA; LOCAL GEOLOGY; EARTHQUAKE; AMPLIFICATION; LANDFORM; TOPOGRAPHY; REGION AB We present an approach based on geomorphometry to predict material properties and characterize site conditions using the V-S30 parameter (time-averaged shear-wave velocity to a depth of 30 m). Our framework consists of an automated terrain classification scheme based on taxonomic criteria (slope gradient, local convexity, and surface texture) that systematically identifies 16 terrain types from 1-km spatial resolution (30 arcsec) Shuttle Radar Topography Mission digital elevation models (SRTM DEMs). Using 853 V-S30 values from California, we apply a simulation-based statistical method to determine the mean V-S30 for each terrain type in California. We then compare the V-S30 values with models based on individual proxies, such as mapped surface geology and topographic slope, and show that our systematic terrain-based approach consistently performs better than semiempirical estimates based on individual proxies. To further evaluate our model, we apply our California-based estimates to terrains of the contiguous United States. Comparisons of our estimates with 325 V-S30 measurements outside of California, as well as estimates based on the topographic slope model, indicate our method to be statistically robust and more accurate. Our approach thus provides an objective and robust method for extending estimates of V-S30 for regions where in situ measurements are sparse or not readily available. C1 [Yong, Alan; Hough, Susan E.] US Geol Survey, Pasadena, CA 91106 USA. [Iwahashi, Junko] Geospatial Informat Author Japan, Tsukuba, Ibaraki, Japan. [Braverman, Amy] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Yong, A (reprint author), US Geol Survey, 525 S Wilson Ave, Pasadena, CA 91106 USA. EM yong@usgs.gov NR 84 TC 22 Z9 22 U1 0 U2 3 PU SEISMOLOGICAL SOC AMER PI ALBANY PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA SN 0037-1106 J9 B SEISMOL SOC AM JI Bull. Seismol. Soc. Amer. PD FEB PY 2012 VL 102 IS 1 BP 114 EP 128 DI 10.1785/0120100262 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 897BC UT WOS:000300614700010 ER PT J AU Zaitchik, BF Simane, B Habib, S Anderson, MC Ozdogan, M Foltz, JD AF Zaitchik, Benjamin F. Simane, Belay Habib, Shahid Anderson, Martha C. Ozdogan, Mutlu Foltz, Jeremy D. TI Building Climate Resilience in the Blue Nile/Abay Highlands: A Role for Earth System Sciences SO INTERNATIONAL JOURNAL OF ENVIRONMENTAL RESEARCH AND PUBLIC HEALTH LA English DT Review DE climate change; adaptation; resilience; land degradation; erosion ID ETHIOPIAN HIGHLANDS; MODEL ANALYSIS; VARIABILITY; PRECIPITATION; EROSION; NILE; CONSERVATION; DEGRADATION; INFORMATION; PRODUCTS AB The Blue Nile (Abay) Highlands of Ethiopia are characterized by significant interannual climate variability, complex topography and associated local climate contrasts, erosive rains and erodible soils, and intense land pressure due to an increasing population and an economy that is almost entirely dependent on smallholder, low-input agriculture. As a result, these highland zones are highly vulnerable to negative impacts of climate variability. As patterns of variability and precipitation intensity alter under anthropogenic climate change, there is concern that this vulnerability will increase, threatening economic development and food security in the region. In order to overcome these challenges and to enhance sustainable development in the context of climate change, it is necessary to establish climate resilient development strategies that are informed by best-available Earth System Science (ESS) information. This requirement is complicated by the fact that climate projections for the Abay Highlands contain significant and perhaps irreducible uncertainties. A critical challenge for ESS, then, is to generate and to communicate meaningful information for climate resilient development in the context of a highly uncertain climate forecast. Here we report on a framework for applying ESS to climate resilient development in the Abay Highlands, with a focus on the challenge of reducing land degradation. C1 [Zaitchik, Benjamin F.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21210 USA. [Simane, Belay] Univ Addis Ababa, Coll Dev Studies, Addis Ababa, Ethiopia. [Habib, Shahid] NASA, Goddard Space Flight Ctr, Off Appl Sci, Greenbelt, MD 20770 USA. [Anderson, Martha C.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA. [Ozdogan, Mutlu; Foltz, Jeremy D.] Univ Wisconsin, Madison, WI 53706 USA. RP Zaitchik, BF (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21210 USA. EM zaitchik@jhu.edu; simaneb@yahoo.com; shahid.habib@nasa.gov; martha.anderson@ars.usda.gov; ozdogon@wisc.edu; jdfoltz@wisc.edu RI Zaitchik, Benjamin/B-9461-2013; Brooks, Katya/J-4975-2014; Anderson, Martha/C-1720-2015; OI Anderson, Martha/0000-0003-0748-5525; Ozdogan, Mutlu/0000-0002-1707-3375 FU Johns Hopkins University; Addis Ababa University; NASA [NNX09AT61G] FX The authors thank the Johns Hopkins University Global Water Program and Addis Ababa University for providing funds for the workshop in Bahir Dar. All 70+ workshop participants are also acknowledged for their contribution to the ideas presented in this paper. Nile LDAS Research results presented here were supported by NASA Applied Sciences grant NNX09AT61G. NR 71 TC 11 Z9 11 U1 5 U2 42 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 1660-4601 J9 INT J ENV RES PUB HE JI Int. J. Environ. Res. Public Health PD FEB PY 2012 VL 9 IS 2 BP 435 EP 461 DI 10.3390/ijerph9020435 PG 27 WC Environmental Sciences; Public, Environmental & Occupational Health SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health GA 898DE UT WOS:000300714800007 PM 22470302 ER PT J AU Gabb, T AF Gabb, Tim TI Advances in Superalloys SO JOM LA English DT Editorial Material C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Gabb, T (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM timothy.p.gabb@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1047-4838 J9 JOM-US JI JOM PD FEB PY 2012 VL 64 IS 2 BP 239 EP 240 DI 10.1007/s11837-012-0240-5 PG 2 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing SC Materials Science; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing GA 902LQ UT WOS:000301040000009 ER PT J AU Bunderson, LD Van de Water, P Luvall, J Levetin, E AF Bunderson, L. D. Van de Water, P. Luvall, J. Levetin, E. TI When Is It Safe To Go Outside? Nighttime Juniper Pollen Concentrations In Texas, Oklahoma, And New Mexico SO JOURNAL OF ALLERGY AND CLINICAL IMMUNOLOGY LA English DT Meeting Abstract CT Annual Meeting of the American-Academy-of-Allergy-Asthma-and-Immunology (AAAAI) CY MAR 02-06, 2012 CL Orlando, FL SP Amer Acad Allergy Asthma & Immunol (AAAAI) C1 [Bunderson, L. D.; Levetin, E.] Univ Tulsa, Tulsa, OK 74104 USA. [Van de Water, P.] Calif State Univ Fresno, Fresno, CA 93740 USA. [Luvall, J.] NASA, Huntsville, AL USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU MOSBY-ELSEVIER PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010-1710 USA SN 0091-6749 J9 J ALLERGY CLIN IMMUN JI J. Allergy Clin. Immunol. PD FEB PY 2012 VL 129 IS 2 SU S BP AB92 EP AB92 PG 1 WC Allergy; Immunology SC Allergy; Immunology GA 903QL UT WOS:000301133400349 ER PT J AU Levetin, E Bunderson, L Van de Water, P Luvall, J AF Levetin, E. Bunderson, L. Van de Water, P. Luvall, J. TI Is Red-Berry Juniper an Overlooked Fall Allergen in the Southwest? SO JOURNAL OF ALLERGY AND CLINICAL IMMUNOLOGY LA English DT Meeting Abstract CT Annual Meeting of the American-Academy-of-Allergy-Asthma-and-Immunology (AAAAI) CY MAR 02-06, 2012 CL Orlando, FL SP Amer Acad Allergy Asthma & Immunol (AAAAI) C1 [Levetin, E.; Bunderson, L.] Univ Tulsa, Tulsa, OK 74104 USA. [Van de Water, P.] Calif State Univ Fresno, Fresno, CA 93740 USA. [Luvall, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU MOSBY-ELSEVIER PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010-1710 USA SN 0091-6749 J9 J ALLERGY CLIN IMMUN JI J. Allergy Clin. Immunol. PD FEB PY 2012 VL 129 IS 2 SU S BP AB91 EP AB91 PG 1 WC Allergy; Immunology SC Allergy; Immunology GA 903QL UT WOS:000301133400345 ER PT J AU Van de Water, PK Bunderson, L Luvall, J Levetin, E AF Van de Water, P. K. Bunderson, L. Luvall, J. Levetin, E. TI Urban Heat And Humidity Islands And The Preferential Deposition Of Airborne Pollen SO JOURNAL OF ALLERGY AND CLINICAL IMMUNOLOGY LA English DT Meeting Abstract CT Annual Meeting of the American-Academy-of-Allergy-Asthma-and-Immunology (AAAAI) CY MAR 02-06, 2012 CL Orlando, FL SP Amer Acad Allergy Asthma & Immunol (AAAAI) C1 [Van de Water, P. K.] Calif State Univ Fresno, Fresno, CA 93740 USA. [Bunderson, L.; Levetin, E.] Univ Tulsa, Tulsa, OK 74104 USA. [Luvall, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. NR 0 TC 0 Z9 0 U1 0 U2 4 PU MOSBY-ELSEVIER PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010-1710 USA SN 0091-6749 J9 J ALLERGY CLIN IMMUN JI J. Allergy Clin. Immunol. PD FEB PY 2012 VL 129 IS 2 SU S BP AB19 EP AB19 PG 1 WC Allergy; Immunology SC Allergy; Immunology GA 903QL UT WOS:000301133400075 ER PT J AU Tapiador, FJ Turk, FJ Petersen, W Hou, AY Garcia-Ortega, E Machado, LAT Angelis, CF Salio, P Kidd, C Huffman, GJ de Castro, M AF Tapiador, Francisco J. Turk, F. J. Petersen, Walt Hou, Arthur Y. Garcia-Ortega, Eduardo Machado, Luiz A. T. Angelis, Carlos F. Salio, Paola Kidd, Chris Huffman, George J. de Castro, Manuel TI Global precipitation measurement: Methods, datasets and applications SO ATMOSPHERIC RESEARCH LA English DT Review DE Precipitation Regional Climate Models (RCM); Global Climate Models (GCM); Quantitative Precipitation Estimation (QPE); Global Precipitation Measurement (GPM) mission ID RAINDROP SIZE DISTRIBUTION; SATELLITE RAINFALL ESTIMATION; VARIATIONAL DATA ASSIMILATION; ENSEMBLE KALMAN FILTER; PROBABILITY-DISTRIBUTION FUNCTIONS; DIFFERENT CLIMATIC REGIMES; SMALL-SCALE VARIABILITY; DUAL-POLARIZED RADAR; SPACE-TIME CLIMATE; PASSIVE MICROWAVE AB This paper explores the many aspects of precipitation measurement that are relevant to providing an accurate global assessment of this important environmental parameter. Methods discussed include ground data, satellite estimates and numerical models. First, the methods for measuring, estimating, and modeling precipitation are discussed. Then, the most relevant datasets gathering precipitation information from those three sources are presented. The third part of the paper illustrates a number of the many applications of those measurements and databases, namely hydropower, data assimilation and validation of Regional Climate Models (RCM). The aim of the paper is to organize the many links and feedbacks between precipitation measurement, estimation and modeling, indicating the uncertainties and limitations of each technique in order to identify areas requiring further attention, and to show the limits within which datasets can be used. Special emphasis is put on the central role of the upcoming Global Precipitation Measurement (GPM) mission in precipitation science. (C) 2011 Elsevier B.V. All rights reserved. C1 [Tapiador, Francisco J.; de Castro, Manuel] UCLM, Dept Environm Sci, Toledo, Spain. [Turk, F. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Petersen, Walt] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. [Hou, Arthur Y.; Kidd, Chris; Huffman, George J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Garcia-Ortega, Eduardo] Univ Leon, Dept Phys, E-24071 Leon, Spain. [Salio, Paola] Univ Buenos Aires, FCEN, Dept Ciencias Atmosfera & Oceanos, Buenos Aires, DF, Argentina. [Kidd, Chris] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Huffman, George J.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Tapiador, FJ (reprint author), UCLM, Dept Environm Sci, Toledo, Spain. EM francisco.tapiador@uclm.es; joseph.turk@jpl.nasa.gov; walt.petersen@nasa.gov; arthur.y.hou@nasa.gov; eduardo.garcia@unileon.es; luiz.machado@cptec.inpe.br; angelis@cptec.inpe.br; salio@cima.fcen.uba.ar; chris.kidd@nasa.gov; george.j.huffman@nasa.gov; manuel.castro@uclm.es RI Garcia-Ortega, Eduardo/A-7088-2012; Hou, Arthur/D-8578-2012; Huffman, George/F-4494-2014; Kidd, Christopher/H-9910-2014; Measurement, Global/C-4698-2015; Machado, Luiz/C-4314-2012 OI Garcia-Ortega, Eduardo/0000-0002-6414-3081; Huffman, George/0000-0003-3858-8308; Machado, Luiz/0000-0002-8243-1706 FU CENIT PROMETEO (MICCIN); JCCM [PPII10-0162-554]; National Aeronautics and Space Administration; JCyL [LE176A11-2]; EU [EVK2-CT-2001-00132, 505539]; DoE; EPA; NOAA; NSF; [CGL2010-20787-C02-01]; [CGL2010-20787-C02-02] FX The work of FTJ (Tapiador) has been funded through projects CGL2010-20787-C02-01, CGL2010-20787-C02-02, CENIT PROMETEO (MICCIN), and PPII10-0162-554 (JCCM). The contributions from FJT (Turk) were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. EGO acknowledges research project LE176A11-2 (JCyL). GJH and WP acknowledge the NASA PMM (Dr. Ramesh Kakar) and GPM Programs for funding support. FJT (Tapiador), FJT (Turk), WP, AYH, LATM, CFA, PS, and GJH are current Principal Investigators in the Precipitation Measurement Missions (PMM, GPM + TRMM) science team. PRUDENCE project was funded by the EU FP5 (Contract no. EVK2-CT-2001-00132). The ENSEMBLES data used in this work was funded by the EU FP6 (Contract no. 505539). NAR-CAPP is funded by the DoE, EPA, NOAA and NSF. The CMAP, CPC, CRU, GPCC, GPCP and TRMM data providers are also gratefully acknowledged. NR 155 TC 91 Z9 94 U1 9 U2 80 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0169-8095 J9 ATMOS RES JI Atmos. Res. PD FEB PY 2012 VL 104 BP 70 EP 97 DI 10.1016/j.atmosres.2011.10.021 PG 28 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 898JS UT WOS:000300739300003 ER PT J AU Palmsten, ML Holman, RA AF Palmsten, Margaret L. Holman, Robert A. TI Laboratory investigation of dune erosion using stereo video SO COASTAL ENGINEERING LA English DT Article DE Stereo imaging; Dune erosion; Wave runup; Remote sensing ID SCALE; IMPACT; RUNUP; COAST AB Simple parameterizations of dune erosion are necessary for forecasting erosion potential prior to an oncoming storm. Dune erosion may be parameterized in terms of the elevation of the total water level (composed of surge, tide, and wave runup) above the dune base and period of exposure of the dune to waves. In this work, we test several versions of this model using observations from a large wave tank experiment designed to model a storm hydrograph, and we develop a new method for acquiring the appropriate data with confidence intervals using stereo video techniques. The stereo method results in observations of dune morphology at higher spatial and temporal resolutions than traditional survey methods allow. Resolution of the stereo technique was 0.1 m in the horizontal and 0.04 m in the vertical, and errors in stereo observations were on the order of 0.02 to 0.08 m (1 to 2 pixels) when compared with surveys. A new method was developed to estimate confidence intervals on stereo observations. When the unchanging dune top was repeatedly sampled, the new confidence intervals encompassed 2 standard deviations of scatter about the mean dune surface 98% of the time. Observations from the stereo method were used to quantify wave runup and dune erosion. We tested a variety of runup statistics based on a Gaussian distribution of swash properties, and found that the most predictive statistic for dune erosion was the 16% exceedance elevation above the dune base, lower than the often used 2% exceedance value. We found that the parameterization of runup was sensitive to the definition of beach slope and that the most accurate beach slope for predicting runup was through the region of the beach profile defined by the mean water level plus one standard deviation of swash. The dune base retreated along a relatively constant trajectory that was a half of the initial beach slope. Finally, a simple model for dune erosion was tested and found to reproduce 64% of the observed variance in dune erosion rate given known forcing at the dune and 49% of the observed variance in dune erosion rate given parameterized forcing. Integrating the simple model over time, 93% of the observed dune retreat distance was reproduced given offshore forcing. (C) 2011 Elsevier B.V. All rights reserved. C1 [Palmsten, Margaret L.] USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. [Palmsten, Margaret L.; Holman, Robert A.] Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. RP Palmsten, ML (reprint author), USN, Res Lab, Stennis Space Ctr, Code 7430, Stennis Space Ctr, MS 39529 USA. EM margaret.palmsten.ctr@nrlssc.navy.mil FU Oregon Sea Grant; United States Geological Survey; Office of Naval Research FX The authors would like to thank Linden Clarke for early development of the stereo code, John Stanley for his hard work on this and other Argus projects, and Peter Ruggiero and Tim Maddux for data collection and project development. This work was completed with funding from the Oregon Sea Grant, the United States Geological Survey, and the Office of Naval Research. NR 28 TC 11 Z9 15 U1 1 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-3839 J9 COAST ENG JI Coast. Eng. PD FEB PY 2012 VL 60 BP 123 EP 135 DI 10.1016/j.coastaleng.2011.09.003 PG 13 WC Engineering, Civil; Engineering, Ocean SC Engineering GA 900WF UT WOS:000300921700011 ER PT J AU Chopping, M North, M Chen, JQ Schaaf, CB Blair, JB Martonchik, JV Bull, MA AF Chopping, Mark North, Malcolm Chen, Jiquan Schaaf, Crystal B. Blair, J. Bryan Martonchik, John V. Bull, Michael A. TI Forest Canopy Cover and Height From MISR in Topographically Complex Southwestern US Landscapes Assessed With High Quality Reference Data SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Biomass; canopy; forestry; lidar; modeling; multiangle; topography ID REMOTE-SENSING DATA; ANGLE SPECTRAL DATA; BIDIRECTIONAL REFLECTANCE; NORTH-AMERICA; UNITED-STATES; ABOVEGROUND BIOMASS; CONIFER FOREST; TREE MORTALITY; MODEL; INVERSION AB This study addresses the retrieval of spatially contiguous canopy cover and height estimates in southwestern US forests via inversion of a geometric-optical (GO) model against surface bidirectional reflectance factor (BRF) estimates from the Multi-angle Imaging SpectroRadiometer (MISR). Model inversion can provide such maps if good estimates of the background bidirectional reflectance distribution function (BRDF) are available. The study area is in the Sierra National Forest in the Sierra Nevada of California. Tree number density, mean crown radius, and fractional cover reference estimates were obtained via analysis of QuickBird 0.6 m spatial resolution panchromatic imagery using the CANopy Analysis with Panchromatic Imagery (CANAPI) algorithm, while RH50, RH75 and RH100 (50%, 75%, and 100% energy return) height data were obtained from the NASA Laser Vegetation Imaging Sensor (LVIS), a full waveform light detection and ranging (lidar) instrument. These canopy parameters were used to drive a modified version of the simple GO model (SGM), accurately reproducing patterns of MISR 672 nm band surface reflectance (mean RMSE = 0.011, mean R-2 = 0.82, N = 1048). Cover and height maps were obtained through model inversion against MISR 672 nm reflectance estimates on a 250 m grid. The free parameters were tree number density and mean crown radius. RMSE values with respect to reference data for the cover and height retrievals were 0.05 and 6.65 m, respectively, with R-2 of 0.54 and 0.49. MISR can thus provide maps of forest cover and height in areas of topographic variation although refinements are required to improve retrieval precision. C1 [Chopping, Mark] Montclair State Univ, Dept Earth & Environm Studies, Montclair, NJ 07043 USA. [North, Malcolm] US Forest Serv, USDA, Pacific SW Res Stn, Davis, CA 95618 USA. [Chen, Jiquan] Univ Toledo, Dept Environm Sci, Toledo, OH 43560 USA. [Schaaf, Crystal B.] Univ Massachusetts, Dept Environm Earth & Ocean Sci, Boston, MA 02125 USA. [Blair, J. Bryan] NASA, Goddard Space Flight Ctr, Laser Remote Sensing Lab, Greenbelt, MD 20771 USA. [Martonchik, John V.; Bull, Michael A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chopping, M (reprint author), Montclair State Univ, Dept Earth & Environm Studies, Montclair, NJ 07043 USA. EM chopping@pegasus.montclair.edu; mnorth@ucdavis.edu; jiquan.chen@utoledo.edu; crystal.schaaf@umb.edu; james.b.blair@nasa.gov; john.v.martonchik@jpl.nasa.gov; michael.a.bull@jpl.nasa.gov RI Chen, Jiquan/D-1955-2009; Khachadourian, Diana/C-8513-2012; Blair, James/D-3881-2013; Beckley, Matthew/D-4547-2013 FU National Aeronautics and Space Administration [NNX08AE71G, NNX11AF90G]; University of Maryland, College Park FX This work was supported by National Aeronautics and Space Administration Grant NNX08AE71G and Grant NNX11AF90G.; The authors acknowledge the LVIS team for use of the LVIS data. They thank Xiaohong Chopping for informed comment; Sawahiko Shimada (Agricultural University of Tokyo) for assistance with large-scale BRDF model inversions; and Joseph Youn and Michael Stoppay (Computer Operations for Research and Education, College of Science and Mathematics, Montclair State University) for computing support. They also thank the two anonymous reviewers for their insights on the original manuscript. The MISR data were obtained from the NASA Langley Atmospheric Science Data Center. LVIS data sets were provided by the Laser Vegetation Imaging Sensor (LVIS) team in the Laser Remote Sensing Branch at NASA Goddard Space Flight Center, with support from the University of Maryland, College Park. NR 50 TC 15 Z9 15 U1 2 U2 29 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD FEB PY 2012 VL 5 IS 1 SI SI BP 44 EP 58 DI 10.1109/JSTARS.2012.2184270 PG 15 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 899VK UT WOS:000300844400005 ER PT J AU Rahul, PRC Bhawar, RL Salvekar, PS Devara, PCS Jiang, JH AF Rahul, P. R. C. Bhawar, Rohini L. Salvekar, P. S. Devara, P. C. S. Jiang, Jonathan H. TI Evidence of Atmospheric Brown Clouds Over India During the 2009 Drought Year SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Aerosols; clouds; greenhouse gases; satellites ID MONSOON; CLIMATE; VARIABILITY; ABSORPTION; POLLUTION; RAIN AB Using Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) satellite derived vertical profiles (Total Attenuated Backscatter at 532 nm, Depolarization Ratios at 532 nm, Vertical Feature Mask, monthly mean vertical aerosol and extinction variability), monthly precipitation anomalies from National Centers for Environmental Prediction-Climate Prediction Center (NCEP-CPC) and NCEP wind anomalies; we report the presence of Atmospheric Brown Clouds (ABCs) over India (65 degrees E-95 degrees E; 8 degrees N-35 degrees N) during the summer monsoon of 2009. CALIPSO data revealed the persistent presence of a massive aerosol plume till 4 Km above sea level; this plume persisted for over 7 months (March through September 2009) over India and was loaded with anthropogenic aerosols like sulphates, black carbon products from biomass burning and fossil fuel combustion. The CALIPSO vertical profiles, NCEP-CPC monthly precipitation anomalies and NCEP monthly wind anomalies corroborate the presence of aerosol plume. C1 [Rahul, P. R. C.; Salvekar, P. S.; Devara, P. C. S.] Indian Inst Trop Meteorol, Pune 411008, Maharashtra, India. [Bhawar, Rohini L.; Jiang, Jonathan H.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA. RP Rahul, PRC (reprint author), Indian Inst Trop Meteorol, Pune 411008, Maharashtra, India. FU CALTECH Jet Propulsion Laboratory; NASA FX This work was supported by the CALTECH Jet Propulsion Laboratory, sponsored by NASA. NR 21 TC 4 Z9 4 U1 0 U2 11 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD FEB PY 2012 VL 5 IS 1 SI SI BP 236 EP 241 DI 10.1109/JSTARS.2011.2170554 PG 6 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 899VK UT WOS:000300844400022 ER PT J AU Tarabalka, Y Tilton, JC Benediktsson, JA Chanussot, J AF Tarabalka, Yuliya Tilton, James C. Benediktsson, Jon Atli Chanussot, Jocelyn TI A Marker-Based Approach for the Automated Selection of a Single Segmentation From a Hierarchical Set of Image Segmentations SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Classification; hierarchical segmentation; hyperspectral images; marker selection ID HYPERSPECTRAL DATA; SPATIAL CLASSIFICATION; EXTRACTION; NETWORKS AB The Hierarchical SEGmentation (HSEG) algorithm, which combines region object finding with region object clustering, has given good performances for multi-and hyperspectral image analysis. This technique produces at its output a hierarchical set of image segmentations. The automated selection of a single segmentation level is often necessary. We propose and investigate the use of automatically selected markers for this purpose. In this paper, a novel Marker-based HSEG (M-HSEG) method for spectral-spatial classification of hyperspectral images is proposed. Two classification-based approaches for automatic marker selection are adapted and compared for this purpose. Then, a novel constrained marker-based HSEG algorithm is applied, resulting in a spectral-spatial classification map. Three different implementations of the M-HSEG method are proposed and their performances in terms of classification accuracies are compared. The experimental results, presented for three hyperspectral airborne images, demonstrate that the proposed approach yields accurate segmentation and classification maps, and thus is attractive for remote sensing image analysis. C1 [Tarabalka, Yuliya; Tilton, James C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Benediktsson, Jon Atli] Univ Iceland, Fac Elect & Comp Engn, IS-107 Reykjavik, Iceland. [Chanussot, Jocelyn] Grenoble Inst Technol INPG, Grenoble Images Speech Signals & Automat Lab GIPS, F-38402 St Martin Dheres, France. RP Tarabalka, Y (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM yuliya.tarabalka@nasa.gov; james.c.tilton@nasa.gov; benedikt@hi.is; jocelyn.chanussot@gipsa-lab.grenoble-inp.fr RI Benediktsson, Jon/F-2861-2010 OI Benediktsson, Jon/0000-0003-0621-9647 FU NASA FX This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 38 TC 41 Z9 42 U1 2 U2 18 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD FEB PY 2012 VL 5 IS 1 SI SI BP 262 EP 272 DI 10.1109/JSTARS.2011.2173466 PG 11 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 899VK UT WOS:000300844400025 ER PT J AU Hamilton, DR Sargsyan, AE Garcia, K Ebert, DJ Whitson, PA Feiveson, AH Alferova, IV Dulchavsky, SA Matveev, VP Bogomolov, VV Duncan, JM AF Hamilton, Douglas R. Sargsyan, Ashot E. Garcia, Kathleen Ebert, Douglas J. Whitson, Peggy A. Feiveson, Alan H. Alferova, Irina V. Dulchavsky, Scott A. Matveev, Vladimir P. Bogomolov, Valery V. Duncan, J. Michael TI Cardiac and vascular responses to thigh cuffs and respiratory maneuvers on crewmembers of the International Space Station SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE microgravity; echocardiography; astronaut; occlusion cuffs; cardiac function ID CENTRAL VENOUS-PRESSURE; HEAD-DOWN TILT; CLINICAL ULTRASOUND ABOARD; CARDIOVASCULAR-SYSTEM; MICROGRAVITY; FLIGHT; WEIGHTLESSNESS; VOLUME; ECHOCARDIOGRAPHY; COUNTERMEASURES AB Hamilton DR, Sargsyan AE, Garcia K, Ebert DJ, Whitson PA, Feiveson AH, Alferova IV, Dulchavsky SA, Matveev VP, Bogomolov VV, Duncan JM. Cardiac and vascular responses to thigh cuffs and respiratory maneuvers on crewmembers of the International Space Station. J Appl Physiol 112: 454-462, 2012. First published September 8, 2011; doi: 10.1152/japplphysiol.00557.2011.-Background: the transition to microgravity eliminates the hydrostatic gradients in the vascular system. The resulting fluid redistribution commonly manifests as facial edema, engorgement of the external neck veins, nasal congestion, and headache. This experiment examined the responses to modified Valsalva and Mueller maneuvers measured by cardiac and vascular ultrasound (ECHO) in a baseline steady state and under the influence of thigh occlusion cuffs available as a countermeasure device (Braslet cuffs). Methods: nine International Space Station crewmember subjects (expeditions 16-20) were examined in 15 experiment sessions 101 +/- 46 days after launch (mean +/- SD; 33-185). Twenty-seven cardiac and vascular parameters were obtained with/without respiratory maneuvers before and after tightening of the Braslet cuffs (162 parameter states/session). Quality of cardiac and vascular ultrasound examinations was assured through remote monitoring and guidance by investigators from the NASA Telescience Center in Houston, TX, and the Mission Control Center in Korolyov, Moscow region, Russia. Results: 14 of 81 conditions (27 parameters measured at baseline, Valsalva, and Mueller maneuver) were significantly different when the Braslet was applied. Seven of 27 parameters were found to respond differently to respiratory maneuvers depending on the presence or absence of thigh compression. Conclusions: acute application of Braslet occlusion cuffs causes lower extremity fluid sequestration and exerts commensurate measurable effects on cardiac performance in microgravity. Ultrasound techniques to measure the hemodynamic effects of thigh cuffs in combination with respiratory maneuvers may serve as an effective tool in determining the volume status of a cardiac or hemodynamically compromised patient at the "microgravity bedside." C1 [Hamilton, Douglas R.; Sargsyan, Ashot E.; Garcia, Kathleen; Ebert, Douglas J.] Wyle Integrated Sci & Engn, Houston, TX USA. [Whitson, Peggy A.; Feiveson, Alan H.; Duncan, J. Michael] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Alferova, Irina V.] Russian Acad Sci, Inst Biomed Problems, Moscow, Russia. [Dulchavsky, Scott A.] Henry Ford Hosp, Detroit, MI 48202 USA. [Matveev, Vladimir P.; Bogomolov, Valery V.] Yuri A Gagarin Cosmonaut Training Ctr, Star City, Russia. RP Hamilton, DR (reprint author), 1290 Hercules Dr, Houston, TX 77058 USA. EM dhamilton@wylehou.com FU NASA [NAS9-02078] FX Primary funding for this project was provided by the Exploration Medical Capability element of NASA's Human Research Program through the Bioastronautics Contract to Wyle Integrated Science and Engineering Group (NAS9-02078). NR 52 TC 8 Z9 9 U1 0 U2 9 PU AMER PHYSIOLOGICAL SOC PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA SN 8750-7587 J9 J APPL PHYSIOL JI J. Appl. Physiol. PD FEB PY 2012 VL 112 IS 3 BP 454 EP 462 DI 10.1152/japplphysiol.00557.2011 PG 9 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA 894DX UT WOS:000300408300017 PM 21903875 ER PT J AU Burns, JO Lazio, J Bale, S Bowman, J Bradley, R Carilli, C Furlanetto, S Harker, G Loeb, A Pritchard, J AF Burns, Jack O. Lazio, J. Bale, S. Bowman, J. Bradley, R. Carilli, C. Furlanetto, S. Harker, G. Loeb, A. Pritchard, J. TI Probing the first stars and black holes in the early Universe with the Dark Ages Radio Explorer (DARE) SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Cosmology: first stars; dark ages; reionization; Radio lines: general; Instrumentation: detectors ID REIONIZATION EPOCH; HIGH-REDSHIFT; ARRAY; CONSTRAINTS; GALAXIES; PARTICLE; BURSTS; NOISE; MHZ AB A concept for a new space-based cosmology mission called the Dark Ages Radio Explorer (DARE) is presented in this paper. DARE's science objectives include: (1) When did the first stars form? (2) When did the first accreting black holes form? (3) When did Reionization begin? (4) What surprises does the end of the Dark Ages hold (e.g., Dark Matter decay)? DARE will use the highly-redshifted hyperfine 21-cm transition from neutral hydrogen to track the formation of the first luminous objects by their impact on the intergalactic medium during the end of the Dark Ages and during Cosmic Dawn (redshifts z = 11-35). It will measure the sky-averaged spin temperature of neutral hydrogen at the unexplored epoch 80-420 million years after the Big Bang, providing the first evidence of the earliest stars and galaxies to illuminate the cosmos and testing our models of galaxy formation. DARE's approach is to measure the expected spectral features in the sky-averaged, redshifted 21-cm signal over a radio bandpass of 40-120 MHz. DARE orbits the Moon for a mission lifetime of 3 years and takes data above the lunar farside, the only location in the inner solar system proven to be free of human-generated radio frequency interference and any significant ionosphere. The science instrument is composed of a low frequency radiometer, including electrically-short, tapered, bi-conical dipole antennas, a receiver, and a digital spectrometer. The smooth frequency response of the antennas and the differential spectral calibration approach using a Markov Chain Monte Carlo technique will be applied to detect the weak cosmic 21-cm signal in the presence of the intense solar system and Galactic foreground emissions. (C) 2011 COSPA R. Published by Elsevier Ltd. All rights reserved. C1 [Burns, Jack O.; Harker, G.] Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Burns, Jack O.; Lazio, J.; Bale, S.; Bowman, J.; Bradley, R.; Carilli, C.; Furlanetto, S.; Harker, G.; Loeb, A.; Pritchard, J.] NASA, Ames Res Ctr, Lunar Sci Inst, Moffett Field, CA 94035 USA. [Lazio, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bale, S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bowman, J.] Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA. [Bradley, R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Carilli, C.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Furlanetto, S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Loeb, A.; Pritchard, J.] Ctr Astrophys, Cambridge, MA 02138 USA. RP Burns, JO (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, 593 UCB, Boulder, CO 80309 USA. EM jack.burns@colorado.edu RI Bale, Stuart/E-7533-2011; Harker, Geraint/C-4885-2012; OI Bale, Stuart/0000-0002-1989-3596; Harker, Geraint/0000-0002-7894-4082; Pritchard, Jonathan/0000-0003-4127-5353 FU NASA Ames Research Center (ARC); Lunar University Network for Astro-physics Research (LUNAR); NLSI [NNA09DB30A] FX The authors would like to thank the management of the NASA Ames Research Center (ARC) for their strong support and investment in the DARE concept, especially ARC Director P. Worden along with P. Klupar, B.J. Jaroux, as well as NASA Lunar Science Institute (NLSI) Director Y. Pendleton and NLSI Deputy Director G. Schmidt. We are particularly grateful to L. Webster, J. Bauman, H. Sanchez, D. Santiago, T. Soderman, and J. Baer at ARC, as well as I. O'Dwyer, A. Tanner, and R. Jarnot at JPL. We would like to acknowledge Ball Aerospace and, especially, L. Hardaway for their investment of resources and effort on the DARE concept. This concept was conceived and supported by the Lunar University Network for Astro-physics Research (LUNAR) (http://lunar.colorado.edu), headquartered at the University of Colorado Boulder, funded by the NLSI via Cooperative Agreement NNA09DB30A. Part of this research was conducted at that the Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration. NR 48 TC 62 Z9 62 U1 1 U2 8 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD FEB 1 PY 2012 VL 49 IS 3 BP 433 EP 450 DI 10.1016/j.asr.2011.10.014 PG 18 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 892DA UT WOS:000300265700001 ER PT J AU Ruzmaikin, A Aumann, HH AF Ruzmaikin, Alexander Aumann, Hartmut H. TI Decadal variability of tropical Pacific temperature in relation to solar cycles SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Climate decadal variability; Solar cycles ID SEA-SURFACE TEMPERATURE; AIR-TEMPERATURE; OUTPUT AB We use the 8-year long satellite temperature data (2002-2010) from Atmospheric Infra Red Sounder (AIRS) and Atmospheric Microwave Sounding Unit (AMSU) on the Aqua satellite to identify temperature trends in the troposphere and low stratosphere over the Nino 3.4 region of the Tropical Pacific Ocean in the most recent 11-year solar cycle. Employing more extended sea surface temperature (SST) data for five solar cycles (1950-2009) in this region we show that the satellite trends reflect a typical decrease of the sea surface temperature (SST) in the Nino 3.4 region in the declining phase of the solar cycle. The magnitude of the SST decrease depends on the solar cycle and ranges between 0.07 K/yr and 0.27 K/yr for the last five solar cycles. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Ruzmaikin, Alexander; Aumann, Hartmut H.] Jet Prop Lab, Pasadena, CA 91109 USA. RP Ruzmaikin, A (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Alexander.Ruzmaikin@jpl.nasa.gov FU Jet Propulsion Laboratory of the California Institute of Technology under National Aeronautics and Space Administration FX This work was supported in part by the Jet Propulsion Laboratory of the California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank two reviewers for helpful critical comments. NR 23 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD FEB 1 PY 2012 VL 49 IS 3 BP 572 EP 578 DI 10.1016/j.asr.2011.11.010 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 892DA UT WOS:000300265700017 ER PT J AU Schlappi, B Altwegg, K Riesen, T Rubin, M AF Schlaeppi, Bernhard Altwegg, Kathrin Riesen, Timm Rubin, Martin TI An underestimated onboard generated recoil force contributing to the Pioneer anomaly SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Pioneer anomaly; Spacecraft outgassing; Spacecraft contamination AB The Pioneer anomaly, an unexpected acceleration of the Pioneer 10 and 11 spacecraft of similar to 8.5 x 10(-10) ms(-2) directed towards the inner Solar System, has been of great interest for the physics community during the past decade: considered explanations range from new physical concepts to conventional mechanism. It is shown that non-isotropic outgassing of the complete spacecraft structure is comparable in magnitude and direction to the effect and should be considered as a significant contribution to the anomalous acceleration. Although gas leaks from e.g. the propulsion system and propulsive mass loss mechanism have been discarded as possible explanations for the anomaly, the arguments used against such mechanisms do not apply to global outgassing from the spacecraft. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Schlaeppi, Bernhard; Altwegg, Kathrin] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Riesen, Timm] NASA Astrobiol Inst, Inst Astron, Honolulu, HI 96822 USA. [Rubin, Martin] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Schlappi, B (reprint author), Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland. EM schlaeppi@space.unibe.ch RI Rubin, Martin/I-7777-2013 OI Rubin, Martin/0000-0001-6549-3318 FU Swiss National Science Foundation; JPL under NASA [1266313, NMO710889]; National Aeronautics and Space Administration through the NASA Astrobiology Institute through the Office of Space Science [NNA09-DA77A] FX Work at the University of Bern was funded by the Swiss National Science Foundation. The work at the University of Michigan was supported by JPL subcontract 1266313 under NASA prime contract NMO710889. 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. NR 17 TC 4 Z9 4 U1 0 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD FEB 1 PY 2012 VL 49 IS 3 BP 579 EP 585 DI 10.1016/j.asr.2011.10.016 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 892DA UT WOS:000300265700018 ER PT J AU Martinez, O Sankar, B Haftka, R Blosser, ML AF Martinez, Oscar Sankar, Bhavani Haftka, Raphael Blosser, Max L. TI Two-Dimensional Orthotropic Plate Analysis for an Integral Thermal Protection System SO AIAA JOURNAL LA English DT Article ID CORE SANDWICH PANELS AB This paper is concerned with homogenization of a corrugated-core sandwich panel, which is a candidate structure for integrated thermal protection systems for space vehicles. The focus is on determining the local stresses in an integrated thermal protection system panel subjected to mechanical and thermal loads. A micromechanical method is developed to homogenize the sandwich panel as an equivalent orthotropic plate. Mechanical and thermal loads are applied to the equivalent thick plate, and the resulting plate deformations were obtained through a shear deformable plate theory. The two-dimensional plate deformations are used to obtain local integrated thermal protection system stresses through reverse homogenization. In addition, simple beam models are used to obtain local facesheet deformations and stress. The local stresses and deflections computed using the analytical method were compared with those from a detailed finite element analysis of the integrated thermal protection system. For the integrated thermal protection system examples considered in this paper, the maximum error in stresses and deflections is less than 5%. This was true for both mechanical and thermal loads acting on the integrated thermal protection system. C1 [Blosser, Max L.] NASA, Langley Res Ctr, Met & Thermal Struct Branch, Struct Concepts & Mech Branch, Hampton, VA 23681 USA. [Martinez, Oscar; Sankar, Bhavani; Haftka, Raphael] Univ Florida, Dept Mech & Aerosp Engn, Gainesville, FL 32611 USA. RP Martinez, O (reprint author), Engn Sci Contract Grp, Houston, TX USA. OI Sankar, Bhavani/0000-0002-4556-1982 FU NASA under the Constellation University FX This research is sponsored by a NASA grant under the Constellation University Institutes Project. The program manager is Claudia Mayer at NASA John H. Glenn Research Center at Lewis Field. NR 20 TC 13 Z9 17 U1 0 U2 9 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD FEB PY 2012 VL 50 IS 2 BP 387 EP 398 DI 10.2514/1.J051172 PG 12 WC Engineering, Aerospace SC Engineering GA 882TO UT WOS:000299587000012 ER PT J AU Kelley, CA Poole, JA Tazaz, AM Chanton, JP Bebout, BM AF Kelley, Cheryl A. Poole, Jennifer A. Tazaz, Amanda M. Chanton, Jeffrey P. Bebout, Brad M. TI Substrate Limitation for Methanogenesis in Hypersaline Environments SO ASTROBIOLOGY LA English DT Article DE Carbon isotopes; Methane; Evaporites; Guerrero Negro; Life in extreme environments ID CARBON-ISOTOPE FRACTIONATION; MICROBIAL MATS; METHANOSARCINA-BARKERI; EVAPORATION PONDS; BAJA-CALIFORNIA; GUERRERO-NEGRO; DIVERSITY; METHANE; SEDIMENTS; SULFATE AB Motivated by the increasingly abundant evidence for hypersaline environments on Mars and reports of methane in its atmosphere, we examined methanogenesis in hypersaline ponds in Baja California Sur, Mexico, and in northern California, USA. Methane-rich bubbles trapped within or below gypsum/halite crusts have delta C-13 values near -40 parts per thousand. Methane with these relatively high isotopic values would typically be considered thermogenic; however, incubations of crust samples resulted in the biological production of methane with similar isotopic composition. A series of measurements aimed at understanding the isotopic composition of methane in hypersaline systems was therefore undertaken. Methane production rates, as well as the concentrations and isotopic composition of the particulate organic carbon (POC), were measured. Methane production was highest from microbial communities living within gypsum crusts, whereas POC content at gypsum/halite sites was low, generally less than 1% of the total mass. The isotopic composition of the POC ranged from -26 parts per thousand to -10 parts per thousand. To determine the substrates used by the methanogens, C-13-labeled methylamines, methanol, acetate, and bicarbonate were added to individual incubation vials, and the methane produced was monitored for C-13 content. The main substrates used by the methanogens were the noncompetitive substrates, the methylamines, and methanol. When unlabeled trimethylamine (TMA) was added to incubating gypsum/halite crusts in increasing concentrations, the isotopic composition of the methane produced became progressively lower; the lowest methane delta C-13 values occurred when the most TMA was added (1000 mu M final concentration). This decrease in the isotopic composition of the methane produced with increasing TMA concentrations, along with the high in situ methane delta C-13 values, suggests that the methanogens within the crusts are operating at low substrate concentrations. It appears that substrate limitation is decreasing isotopic fractionation during methanogenesis, which results in these abnormally high biogenic methane delta C-13 values. C1 [Kelley, Cheryl A.; Poole, Jennifer A.] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. [Tazaz, Amanda M.; Chanton, Jeffrey P.] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA. [Bebout, Brad M.] NASA Ames Res Ctr, Exobiol Branch, Moffett Field, CA USA. RP Kelley, CA (reprint author), Univ Missouri, Dept Geol Sci, 101 Geol Sci Bldg, Columbia, MO 65211 USA. EM kelleyc@missouri.edu RI Kelley, Cheryl/K-9392-2015 FU NASA; University of Missouri's Research Board and Council FX We would like to thank Adrienne Frisbee and Angela Detweiler for assistance in the field and lab, and the Exportadora de Sal de C.V. and the U.S. Fish and Wildlife Service for allowing continued access to the study sites. Financial support from the NASA Exobiology program and the University of Missouri's Research Board and Council is gratefully acknowledged. NR 43 TC 16 Z9 17 U1 1 U2 19 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD FEB PY 2012 VL 12 IS 2 BP 89 EP 97 DI 10.1089/ast.2011.0703 PG 9 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 895UW UT WOS:000300523100001 PM 22248383 ER PT J AU Crisler, JD Newville, TM Chen, F Clark, BC Schneegurt, MA AF Crisler, J. D. Newville, T. M. Chen, F. Clark, B. C. Schneegurt, M. A. TI Bacterial Growth at the High Concentrations of Magnesium Sulfate Found in Martian Soils SO ASTROBIOLOGY LA English DT Article DE Analogue; Mars; Planetary protection; Salts; Life in extreme environments ID SPACECRAFT-ASSEMBLY FACILITY; RED HALOPHILIC BACTERIA; DEAD-SEA HALOBACTERIUM; GREAT SALT PLAINS; DEINOCOCCUS-RADIODURANS; CLEAN ROOMS; DESICCATION TOLERANCE; RADIATION-RESISTANT; IONIZING-RADIATION; VIKING SPACECRAFT AB The martian surface environment exhibits extremes of salinity, temperature, desiccation, and radiation that would make it difficult for terrestrial microbes to survive. Recent evidence suggests that martian soils contain high concentrations of MgSO4 minerals. Through warming of the soils, meltwater derived from subterranean ice-rich regolith may exist for an extended period of time and thus allow the propagation of terrestrial microbes and create significant bioburden at the near surface of Mars. The current report demonstrates that halotolerant bacteria from the Great Salt Plains (GSP) of Oklahoma are capable of growing at high concentrations of MgSO4 in the form of 2 M solutions of epsomite. The epsotolerance of isolates in the GSP bacterial collection was determined, with 35% growing at 2 M MgSO4. There was a complex physiological response to mixtures of MgSO4 and NaCl coupled with other environmental stressors. Growth also was measured at 1 M concentrations of other magnesium and sulfate salts. The complex responses may be partially explained by the pattern of chaotropicity observed for high-salt solutions as measured by agar gelation temperature. Select isolates could grow at the high salt concentrations and low temperatures found on Mars. Survival during repetitive freeze-thaw or drying-rewetting cycles was used as other measures of potential success on the martian surface. Our results indicate that terrestrial microbes might survive under the high-salt, low-temperature, anaerobic conditions on Mars and present significant potential for forward contamination. Stringent planetary protection requirements are needed for future life-detection missions to Mars. C1 [Crisler, J. D.; Newville, T. M.; Schneegurt, M. A.] Wichita State Univ, Dept Biol Sci, Wichita, KS 67260 USA. [Chen, F.] NASA, Planetary Protect Grp, Jet Prop Lab, Pasadena, CA USA. [Clark, B. C.] Space Sci Inst, Boulder, CO USA. RP Schneegurt, MA (reprint author), Wichita State Univ, Dept Biol Sci, 1845 Fairmount, Wichita, KS 67260 USA. EM mark.schneegurt@wichita.edu FU NASA EPSCoR (KNEP); NASA ROSES; NIH NCRR KINBRE FX The authors appreciate the contributions of Leela Bhattarai, Todd Caton, Amy Gray, Roger Kern, Evan Moody, Hieu Nguyen, Ashley Peppers, and Noah Schneegurt. Awards from Kansas NASA EPSCoR (KNEP), NASA ROSES, and NIH NCRR KINBRE supported this work. NR 68 TC 13 Z9 13 U1 1 U2 33 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD FEB PY 2012 VL 12 IS 2 BP 98 EP 106 DI 10.1089/ast.2011.0720 PG 9 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 895UW UT WOS:000300523100002 PM 22248384 ER PT J AU Summers, DP Basa, RCB Khare, B Rodoni, D AF Summers, David P. Basa, Ranor C. B. Khare, Bishun Rodoni, David TI Abiotic Nitrogen Fixation on Terrestrial Planets: Reduction of NO to Ammonia by FeS SO ASTROBIOLOGY LA English DT Article DE Nitrogen fixation; Mars; Earth; Terrestrial; Abiotic; Prebiotic; Nitrogen; Planetary habitability; Biosignatures ID MERIDIANI-PLANUM; EARLY EARTH; OPPORTUNITY ROVER; OXIDATION-STATE; EARLY MARS; ATMOSPHERE; NITRITE; WATER; SPECTROSCOPY; ENVIRONMENT AB Understanding the abiotic fixation of nitrogen and how such fixation can be a supply of prebiotic nitrogen is critical for understanding both the planetary evolution of, and the potential origin of life on, terrestrial planets. As nitrogen is a biochemically essential element, sources of biochemically accessible nitrogen, especially reduced nitrogen, are critical to prebiotic chemistry and the origin of life. Loss of atmospheric nitrogen can result in loss of the ability to sustain liquid water on a planetary surface, which would impact planetary habitability and hydrological processes that shape the surface. It is known that NO can be photochemically converted through a chain of reactions to form nitrate and nitrite, which can be subsequently reduced to ammonia. Here, we show that NO can also be directly reduced, by FeS, to ammonia. In addition to removing nitrogen from the atmosphere, this reaction is particularly important as a source of reduced nitrogen on an early terrestrial planet. By converting NO directly to ammonia in a single step, ammonia is formed with a higher product yield (similar to 50%) than would be possible through the formation of nitrate/nitrite and subsequent conversion to ammonia. In conjunction with the reduction of NO, there is also a catalytic disproportionation at the mineral surface that converts NO to NO2 and N2O. The NO2 is then converted to ammonia, while the N2O is released back in the gas phase, which provides an abiotic source of nitrous oxide. C1 [Summers, David P.] NASA, Carl Sagan Ctr, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Basa, Ranor C. B.; Rodoni, David] Foothill Coll, Los Altos, CA USA. RP Summers, DP (reprint author), NASA, Carl Sagan Ctr, SETI Inst, Ames Res Ctr, Mail Stop 239-4, Moffett Field, CA 94035 USA. EM David.P.Summers@nasa.gov FU NASA Astrobiology Institute [NNA04CC05A]; Exobiology Program FX The authors would like to thank the NASA Astrobiology Institute (NNA04CC05A) and Exobiology Program for support. NR 42 TC 11 Z9 12 U1 3 U2 28 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD FEB PY 2012 VL 12 IS 2 BP 107 EP 114 DI 10.1089/ast.2011.0646 PG 8 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 895UW UT WOS:000300523100003 PM 22283408 ER PT J AU Gleeson, DF Pappalardo, RT Anderson, MS Grasby, SE Mielke, RE Wright, KE Templeton, AS AF Gleeson, Damhnait F. Pappalardo, R. T. Anderson, M. S. Grasby, S. E. Mielke, R. E. Wright, K. E. Templeton, A. S. TI Biosignature Detection at an Arctic Analog to Europa SO ASTROBIOLOGY LA English DT Article DE Europa; Biosignatures; Life detection; Analog; Biomineralization ID INORGANIC SULFUR-COMPOUNDS; NEAR-EDGE SPECTROSCOPY; ELEMENTAL SULFUR; MORPHOLOGICAL BIOSIGNATURES; FILAMENTOUS SULFUR; RAMAN-SPECTROSCOPY; SUBSURFACE OCEAN; SURFACE MATERIAL; CRYSTAL-GROWTH; DEATH-VALLEY AB The compelling evidence for an ocean beneath the ice shell of Europa makes it a high priority for astrobiological investigations. Future missions to the icy surface of this moon will query the plausibly sulfur-rich materials for potential indications of the presence of life carried to the surface by mobile ice or partial melt. However, the potential for generation and preservation of biosignatures under cold, sulfur-rich conditions has not previously been investigated, as there have not been suitable environments on Earth to study. Here, we describe the characterization of a range of biosignatures within potentially analogous sulfur deposits from the surface of an Arctic glacier at Borup Fiord Pass to evaluate whether evidence for microbial activities is produced and preserved within these deposits. Optical and electron microscopy revealed microorganisms and extracellular materials. Elemental sulfur (S-0), the dominant mineralogy within field samples, is present as rhombic and needle-shaped mineral grains and spherical mineral aggregates, commonly observed in association with extracellular polymeric substances. Orthorhombic alpha-sulfur represents the stable form of S-0, whereas the monoclinic (needle-shaped) gamma-sulfur form rosickyite is metastable and has previously been associated with sulfide-oxidizing microbial communities. Scanning transmission electron microscopy showed mineral deposition on cellular and extracellular materials in the form of submicron-sized, needle-shaped crystals. X-ray diffraction measurements supply supporting evidence for the presence of a minor component of rosickyite. Infrared spectroscopy revealed parts-per-million level organics in the Borup sulfur deposits and organic functional groups diagnostic of biomolecules such as proteins and fatty acids. Organic components are below the detection limit for Raman spectra, which were dominated by sulfur peaks. These combined investigations indicate that sulfur mineral deposits may contain identifiable biosignatures that can be stabilized and preserved under low-temperature conditions. Borup Fiord Pass represents a useful testing ground for instruments and techniques relevant to future astrobiological exploration at Europa. C1 [Gleeson, Damhnait F.; Pappalardo, R. T.; Anderson, M. S.; Mielke, R. E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Grasby, S. E.] Geol Survey Canada, Calgary, AB T2L 2A7, Canada. [Wright, K. E.; Templeton, A. S.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. RP Gleeson, DF (reprint author), Ctr Astrobiol CSIC INTA, Madrid 28850, Spain. EM damhnait.gleeson@sciops.esa.int OI Grasby, Stephen/0000-0002-3910-4443; TEMPLETON, ALEXIS/0000-0002-9670-0647 FU NASA; NASA Astrobiology Institute; American Philosophical Society; David and Lucile Packard Foundation; Caltech postdoctoral program; Jupiter Europa Orbiter Project FX We acknowledge the assistance of Benoit Beauchamp at the Arctic Institute of North America, Calgary, Canada, and Kennda Lynch at the Colorado School of Mines. Portions of this work were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA, and were also funded in part by the NASA Astrobiology Institute Director's Discretionary Fund. We also acknowledge financial support from the Lewis and Clark Fund of the American Philosophical Society, the David and Lucile Packard Foundation, the Caltech postdoctoral program, and the Jupiter Europa Orbiter Project. We also wish to thank our anonymous reviewers, with whose help this manuscript has been considerably streamlined and improved overall. NR 84 TC 7 Z9 8 U1 2 U2 50 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD FEB PY 2012 VL 12 IS 2 BP 135 EP 150 DI 10.1089/ast.2010.0579 PG 16 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 895UW UT WOS:000300523100006 PM 22283368 ER PT J AU Ackermann, M Ajello, M Allafort, A Atwood, WB Baldini, L Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Bhat, PN Blandford, RD Bonamente, E Borgland, AW Bregeon, J Briggs, MS Brigida, M Bruel, P Buehler, R Burgess, JM Buson, S Caliandro, GA Cameron, RA Casandjian, JM Cecchi, C Charles, E Chekhtman, A Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Connaughton, V Conrad, J Cutini, S Dennis, BR de Palma, F Dermer, CD Digel, SW Silva, EDE Drell, PS Drlica-Wagner, A Dubois, R Favuzzi, C Fegan, SJ Ferrara, EC Fortin, P Fukazawa, Y Fusco, P Gargano, F Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grillo, L Grove, JE Gruber, D Guiriec, S Hadasch, D Hayashida, M Hays, E Horan, D Iafrate, G Johannesson, G Johnson, AS Johnson, WN Kamae, T Kippen, RM Knodlseder, J Kuss, M Lande, J Latronico, L Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Mazziotta, MN McEnery, JE Meegan, C Mehault, J Michelson, PF Mitthumsiri, W Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Murphy, R Naumann-Godo, M Nuss, E Nymark, T Ohno, M Ohsugi, T Okumura, A Omodei, N Orlando, E Paciesas, WS Panetta, JH Parent, D Pesce-Rollins, M Petrosian, V Pierbattista, M Piron, F Pivato, G Poon, H Porter, TA Preece, R Raino, S Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Ritz, S Sbarra, C Schwartz, RA Sgro, C Share, GH Siskind, EJ Spinelli, P Takahashi, H Tanaka, T Tanaka, Y Thayer, JB Tibaldo, L Tinivella, M Tolbert, AK Tosti, G Troja, E Uchiyama, Y Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V von Kienlin, A Waite, AP Wilson-Hodge, C Wood, DL Wood, KS Yang, Z AF Ackermann, M. Ajello, M. Allafort, A. Atwood, W. B. Baldini, L. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Bhat, P. N. Blandford, R. D. Bonamente, E. Borgland, A. W. Bregeon, J. Briggs, M. S. Brigida, M. Bruel, P. Buehler, R. Burgess, J. M. Buson, S. Caliandro, G. A. Cameron, R. A. Casandjian, J. M. Cecchi, C. Charles, E. Chekhtman, A. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Connaughton, V. Conrad, J. Cutini, S. Dennis, B. R. de Palma, F. Dermer, C. D. Digel, S. W. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Dubois, R. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Fortin, P. Fukazawa, Y. Fusco, P. Gargano, F. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grillo, L. Grove, J. E. Gruber, D. Guiriec, S. Hadasch, D. Hayashida, M. Hays, E. Horan, D. Iafrate, G. Johannesson, G. Johnson, A. S. Johnson, W. N. Kamae, T. Kippen, R. M. Knoedlseder, J. Kuss, M. Lande, J. Latronico, L. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Mazziotta, M. N. McEnery, J. E. Meegan, C. Mehault, J. Michelson, P. F. Mitthumsiri, W. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Murphy, R. Naumann-Godo, M. Nuss, E. Nymark, T. Ohno, M. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Paciesas, W. S. Panetta, J. H. Parent, D. Pesce-Rollins, M. Petrosian, V. Pierbattista, M. Piron, F. Pivato, G. Poon, H. Porter, T. A. Preece, R. Raino, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Ritz, S. Sbarra, C. Schwartz, R. A. Sgro, C. Share, G. H. Siskind, E. J. Spinelli, P. Takahashi, H. Tanaka, T. Tanaka, Y. Thayer, J. B. Tibaldo, L. Tinivella, M. Tolbert, A. K. Tosti, G. Troja, E. Uchiyama, Y. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. von Kienlin, A. Waite, A. P. Wilson-Hodge, C. Wood, D. L. Wood, K. S. Yang, Z. TI FERMI DETECTION OF gamma-RAY EMISSION FROM THE M2 SOFT X-RAY FLARE ON 2010 JUNE 12f SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; Sun: flares; Sun: particle emission; Sun: X-rays, gamma rays ID ACCELERATED-PARTICLE INTERACTIONS; LARGE-AREA TELESCOPE; HIGH-ENERGY-NEUTRON; SOLAR-FLARES; BURST MONITOR; ELECTRONS; SPECTROSCOPY; CALIBRATION; ABUNDANCES; COMPTON AB The Geostationary Operational Environmental Satellite (GOES) M2-class solar flare, SOL2010-06-12T00: 57, was modest in many respects yet exhibited remarkable acceleration of energetic particles. The flare produced an similar to 50 s impulsive burst of hard X-and gamma-ray emission up to at least 400 MeV observed by the Fermi Gamma-ray Burst Monitor and Large Area Telescope experiments. The remarkably similar hard X-ray and high-energy gamma-ray time profiles suggest that most of the particles were accelerated to energies greater than or similar to 300 MeV with a delay of similar to 10 s from mildly relativistic electrons, but some reached these energies in as little as similar to 3 s. The gamma-ray line fluence from this flare was about 10 times higher than that typically observed from this modest GOES class of X-ray flare. There is no evidence for time-extended >100 MeV emission as has been found for other flares with high-energy gamma-rays. C1 [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Glanzman, T.; Godfrey, G.; Grillo, L.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Panetta, J. H.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Ajello, M.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Glanzman, T.; Godfrey, G.; Grillo, L.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Panetta, J. H.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Atwood, W. B.; Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Barbiellini, G.; Iafrate, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.; Sbarra, C.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Pivato, G.; Poon, H.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Bhat, P. N.; Briggs, M. S.; Burgess, J. M.; Connaughton, V.; Guiriec, S.; Paciesas, W. S.; Preece, R.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [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.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; 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.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Fortin, P.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain. [Casandjian, J. M.; Naumann-Godo, M.; Pierbattista, M.] Univ Paris Diderot, La AIM, CEA IRFU, CNRS,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA. [Cutini, S.] ASI, Sci Data Ctr, I-00044 Rome, Italy. [Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3, Montpellier, France. [Conrad, J.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Nymark, T.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Dennis, B. R.; Ferrara, E. C.; Hays, E.; McEnery, J. E.; Schwartz, R. A.; Tolbert, A. K.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Murphy, R.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Fukazawa, Y.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Gruber, D.; Orlando, E.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Iafrate, G.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Lott, B.] Univ Bordeaux 1, CNRS, IN2P3, CEN Bordeaux Gradignan, F-33175 Gradignan, France. [McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Share, G. H.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Meegan, C.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Nymark, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Ohno, M.; Okumura, A.; Tanaka, Y.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Parent, D.; Razzaque, S.] George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 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. [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. [Wilson-Hodge, C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM michael.briggs@nasa.gov; dgruber@mpe.mpg.de; francesco.longo@trieste.infn.it; nicola.omodei@gmail.com; gerald.share@nrl.navy.mil RI Dennis, Brian/C-9511-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Morselli, Aldo/G-6769-2011; Gargano, Fabio/O-8934-2015; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Rando, Riccardo/M-7179-2013; Johnson, Neil/G-3309-2014; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Orlando, E/R-5594-2016 OI lubrano, pasquale/0000-0003-0221-4806; giglietto, nicola/0000-0002-9021-2888; Morselli, Aldo/0000-0002-7704-9553; Gargano, Fabio/0000-0002-5055-6395; Reimer, Olaf/0000-0001-6953-1385; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; FU K. A. Wallenberg Foundation; Fermi GI program FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation.; We thank the referee for suggesting a more detailed examination of the delay between the hard X-ray bremsstrahlung and >30 MeV emission observed by LAT. 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.; Co-authors Briggs, Murphy, Schwartz, Share, and Tolbert were partially funded by the Fermi GI program to conduct the joint spectroscopic studies presented in this paper. NR 45 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 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 144 DI 10.1088/0004-637X/745/2/144 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800042 ER PT J AU Borucki, WJ Koch, DG Batalha, N Bryson, ST Rowe, J Fressin, F Torres, G Caldwell, DA Christensen-Dalsgaard, J Cochran, WD DeVore, E Gautier, TN Geary, JC Gilliland, R Gould, A Howell, SB Jenkins, JM Latham, DW Lissauer, JJ Marcy, GW Sasselov, D Boss, A Charbonneau, D Ciardi, D Kaltenegger, L Doyle, L Dupree, AK Ford, EB Fortney, J Holman, MJ Steffen, JH Mullally, F Still, M Tarter, J Ballard, S Buchhave, LA Carter, J Christiansen, JL Demory, BO Desert, JM Dressing, C Endl, M Fabrycky, D Fischer, D Haas, MR Henze, C Horch, E Howard, AW Isaacson, H Kjeldsen, H Johnson, JA Klaus, T Kolodziejczak, J Barclay, T Li, J Meibom, S Prsa, A Quinn, SN Quintana, EV Robertson, P Sherry, W Shporer, A Tenenbaum, P Thompson, SE Twicken, JD Van Cleve, J Welsh, WF Basu, S Chaplin, W Miglio, A Kawaler, SD Arentoft, T Stello, D Metcalfe, TS Verner, GA Karoff, C Lundkvist, M Lund, MN Handberg, R Elsworth, Y Hekker, S Huber, D Bedding, TR Rapin, W AF Borucki, William J. Koch, David G. Batalha, Natalie Bryson, Stephen T. Rowe, Jason Fressin, Francois Torres, Guillermo Caldwell, Douglas A. Christensen-Dalsgaard, Jorgen Cochran, William D. DeVore, Edna Gautier, Thomas N., III Geary, John C. Gilliland, Ronald Gould, Alan Howell, Steve B. Jenkins, Jon M. Latham, David W. Lissauer, Jack J. Marcy, Geoffrey W. Sasselov, Dimitar Boss, Alan Charbonneau, David Ciardi, David Kaltenegger, Lisa Doyle, Laurance Dupree, Andrea K. Ford, Eric B. Fortney, Jonathan Holman, Matthew J. Steffen, Jason H. Mullally, Fergal Still, Martin Tarter, Jill Ballard, Sarah Buchhave, Lars A. Carter, Josh Christiansen, Jessie L. Demory, Brice-Olivier Desert, Jean-Michel Dressing, Courtney Endl, Michael Fabrycky, Daniel Fischer, Debra Haas, Michael R. Henze, Christopher Horch, Elliott Howard, Andrew W. Isaacson, Howard Kjeldsen, Hans Johnson, John Asher Klaus, Todd Kolodziejczak, Jeffery Barclay, Thomas Li, Jie Meibom, Soren Prsa, Andrej Quinn, Samuel N. Quintana, Elisa V. Robertson, Paul Sherry, William Shporer, Avi Tenenbaum, Peter Thompson, Susan E. Twicken, Joseph D. Van Cleve, Jeffrey Welsh, William F. Basu, Sarbani Chaplin, William Miglio, Andrea Kawaler, Steven D. Arentoft, Torben Stello, Dennis Metcalfe, Travis S. Verner, Graham A. Karoff, Christoffer Lundkvist, Mia Lund, Mikkel N. Handberg, Rasmus Elsworth, Yvonne Hekker, Saskia Huber, Daniel Bedding, Timothy R. Rapin, William TI Kepler-22b: A 2.4 EARTH-RADIUS PLANET IN THE HABITABLE ZONE OF A SUN-LIKE STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: fundamental parameters; stars: individual (Kepler-22, KIC 10593626) ID MAIN-SEQUENCE STARS; TRANSIT TIMING VARIATIONS; INITIAL CHARACTERISTICS; TERRESTRIAL PLANETS; ASTEROSEISMIC DATA; FALSE POSITIVES; SPACE-TELESCOPE; BLEND SCENARIOS; MULTIPLE SYSTEM; CADENCE DATA AB A search of the time-series photometry from NASA's Kepler spacecraft reveals a transiting planet candidate orbiting the 11th magnitude G5 dwarf KIC 10593626 with a period of 290 days. The characteristics of the host star are well constrained by high-resolution spectroscopy combined with an asteroseismic analysis of the Kepler photometry, leading to an estimated mass and radius of 0.970 +/- 0.060 M-circle dot and 0.979 +/- 0.020 R-circle dot. The depth of 492 +/- 10 ppm for the three observed transits yields a radius of 2.38 +/- 0.13 Re for the planet. The system passes a battery of tests for false positives, including reconnaissance spectroscopy, high-resolution imaging, and centroid motion. A full BLENDER analysis provides further validation of the planet interpretation by showing that contamination of the target by an eclipsing system would rarely mimic the observed shape of the transits. The final validation of the planet is provided by 16 radial velocities (RVs) obtained with the High Resolution Echelle Spectrometer on Keck I over a one-year span. Although the velocities do not lead to a reliable orbit and mass determination, they are able to constrain the mass to a 3 sigma upper limit of 124 M-circle plus, safely in the regime of planetary masses, thus earning the designation Kepler-22b. The radiative equilibrium temperature is 262 K for a planet in Kepler-22b's orbit. Although there is no evidence that Kepler-22b is a rocky planet, it is the first confirmed planet with a measured radius to orbit in the habitable zone of any star other than the Sun. C1 [Borucki, William J.; Klaus, Todd] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. [Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Rowe, Jason; Caldwell, Douglas A.; DeVore, Edna; Jenkins, Jon M.; Doyle, Laurance; Mullally, Fergal; Tarter, Jill; Christiansen, Jessie L.; Li, Jie; Quintana, Elisa V.; Tenenbaum, Peter; Thompson, Susan E.; Twicken, Joseph D.; Van Cleve, Jeffrey] SETI Inst, Mountain View, CA 94043 USA. [Fressin, Francois; Torres, Guillermo; Geary, John C.; Latham, David W.; Sasselov, Dimitar; Charbonneau, David; Dupree, Andrea K.; Holman, Matthew J.; Ballard, Sarah; Desert, Jean-Michel; Dressing, Courtney; Meibom, Soren; Quinn, Samuel N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans; Arentoft, Torben; Karoff, Christoffer; Lundkvist, Mia; Lund, Mikkel N.; Handberg, Rasmus] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Christensen-Dalsgaard, Jorgen] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Cochran, William D.; Endl, Michael; Robertson, Paul] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Gautier, Thomas N., III; Johnson, John Asher] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Marcy, Geoffrey W.; Howard, Andrew W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Boss, Alan] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Ciardi, David] CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Kaltenegger, Lisa] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Fortney, Jonathan; Fabrycky, Daniel] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Steffen, Jason H.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Still, Martin; Barclay, Thomas] Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Carter, Josh; Demory, Brice-Olivier] MIT, Cambridge, MA 02139 USA. [Fischer, Debra; Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Kolodziejczak, Jeffery] MSFC, Huntsville, AL 35805 USA. [Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Sherry, William] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Shporer, Avi] Las Cumbres Observ, Goleta, CA 93117 USA. [Chaplin, William; Miglio, Andrea; Verner, Graham A.; Elsworth, Yvonne; Hekker, Saskia] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50014 USA. [Stello, Dennis; Huber, Daniel; Bedding, Timothy R.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Metcalfe, Travis S.] White Dwarf Res Corp, Boulder, CO 80301 USA. [Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Rapin, William] Ctr Spatial Toulouse, Ctr Natl Etud Spatiales, F-31401 Toulouse, France. RP Borucki, WJ (reprint author), NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. EM William.J.Borucki@nasa.gov RI Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015; OI Caldwell, Douglas/0000-0003-1963-9616; Howard, Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; Bedding, Timothy/0000-0001-5943-1460; Metcalfe, Travis/0000-0003-4034-0416; Ciardi, David/0000-0002-5741-3047; Karoff, Christoffer/0000-0003-2009-7965; Demory, Brice-Olivier/0000-0002-9355-5165; Basu, Sarbani/0000-0002-6163-3472; /0000-0001-6545-639X; Lund, Mikkel Norup/0000-0001-9214-5642; Fischer, Debra/0000-0003-2221-0861; Handberg, Rasmus/0000-0001-8725-4502; Kawaler, Steven/0000-0002-6536-6367; Fabrycky, Daniel/0000-0003-3750-0183; Lundkvist, Mia Sloth/0000-0002-8661-2571; Bedding, Tim/0000-0001-5222-4661 FU NASA's Science Mission Directorate; W. M. Keck Foundation; NASA; NASA through JPL/Caltech; National Center for Atmospheric Research; National Science Foundation; Netherlands Organisation for Scientific Research (NWO) FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. 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 Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Some of the observations were made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Additional support for this work was also received from National Center for Atmospheric Research which is sponsored by the National Science Foundation. The authors thank the many people who gave so generously of their time to make this Mission a success. S. H. acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO). NR 83 TC 139 Z9 139 U1 13 U2 60 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 120 DI 10.1088/0004-637X/745/2/120 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800018 ER PT J AU Hammer, DM Hornschemeier, AE Salim, S Smith, R Jenkins, L Mobasher, B Miller, N Ferguson, H AF Hammer, D. M. Hornschemeier, A. E. Salim, S. Smith, R. Jenkins, L. Mobasher, B. Miller, N. Ferguson, H. TI DEEP ULTRAVIOLET LUMINOSITY FUNCTIONS AT THE INFALL REGION OF THE COMA CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Coma); galaxies: dwarf; galaxies: luminosity function, mass function; ultraviolet: galaxies ID EARLY-TYPE GALAXIES; HUBBLE-SPACE-TELESCOPE; STAR-FORMATION RATES; DIGITAL SKY SURVEY; DWARF ELLIPTIC GALAXIES; HICKSON COMPACT-GROUPS; STELLAR POPULATIONS; NEARBY CLUSTERS; VIRGO CLUSTER; REDSHIFT SURVEY AB We have used deep GALEX observations at the infall region of the Coma cluster to measure the faintest ultraviolet (UV) luminosity functions (LFs) presented for a rich galaxy cluster thus far. The Coma UV LFs are measured to M-UV = -10.5 in the GALEX FUV and NUV bands, or 3.5 mag fainter than previous studies, and reach the dwarf early-type galaxy population in Coma for the first time. The Schechter faint-end slopes (alpha approximate to -1.39 in both GALEX bands) are shallower than reported in previous Coma UV LF studies owing to a flatter LF at faint magnitudes. A Gaussian-plus-Schechter model provides a slightly better parameterization of the UV LFs resulting in a faint-end slope of alpha approximate to -1.15 in both GALEX bands. The two-component model gives faint-end slopes shallower than alpha = -1 (a turnover) for the LFs constructed separately for passive and star-forming galaxies. The UV LFs for star-forming galaxies show a turnover at M-UV approximate to -14 owing to a deficit of dwarf star-forming galaxies in Coma with stellar masses below M-* = 10(8) M-circle dot. A similar turnover is identified in recent UV LFs measured for the Virgo cluster suggesting this may be a common feature of local galaxy clusters, whereas the field UV LFs continue to rise at faint magnitudes. We did not identify an excess of passive galaxies as would be expected if the missing dwarf star-forming galaxies were quenched inside the cluster. In fact, the LFs for both dwarf passive and star-forming galaxies show the same turnover at faint magnitudes. We discuss the possible origin of the missing dwarf star-forming galaxies in Coma and their expected properties based on comparisons to local field galaxies. C1 [Hammer, D. M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Hammer, D. M.; Hornschemeier, A. E.; Jenkins, L.] NASA GSFC, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Salim, S.] Indiana Univ, Dept Astron, Bloomington, IN 47404 USA. [Smith, R.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Mobasher, B.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Miller, N.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Ferguson, H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Hammer, DM (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. OI Jenkins, Leigh/0000-0001-9464-0719; Salim, Samir/0000-0003-2342-7501 FU GALEX [05-GALEX05-0046]; Alfred P. Sloan Foundation; NASA; NSF; DoE; Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We thank the anonymous referee for their detailed comments and suggestions that have improved this paper. We thank R. Marzke and members of the Coma Hectospec team for their work on the redshift catalog, and M. Colless for providing an updated version of the GMP catalog redshifts. We are grateful for the LF data shared by A. Boselli, M. Treyer, and M. Blanton, and assistance with the GALEV software by R. Kotulla. We thank T. Heckman for commenting on an early draft and A. Basu-Zych, P. Tzanavaris, and B. Lehmer for helpful science discussion. This research was partially supported by the GALEX Cycle 2 grant 05-GALEX05-0046 (PI: A. E. Hornschemeier). GALEX is a NASA Small Explorer, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. Funding for the creation and distribution of the SDSS Archive has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, NASA, the NSF, DoE, Monbukagakusho, Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. This study made use of the NASA Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory (Caltech), under contract with NASA. NR 119 TC 4 Z9 4 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 177 DI 10.1088/0004-637X/745/2/177 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800075 ER PT J AU Joyce, CJ Smith, CW Isenberg, PA Gary, SP Murphy, N Gray, PC Burlaga, LF AF Joyce, Colin J. Smith, Charles W. Isenberg, Philip A. Gary, S. Peter Murphy, Neil Gray, Perry C. Burlaga, Leonard F. TI OBSERVATION OF BERNSTEIN WAVES EXCITED BY NEWBORN INTERSTELLAR PICKUP IONS IN THE SOLAR WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; magnetic fields; turbulence; waves ID PROTON-BEAM GENERATION; MAGNETIC-FIELD; COMETARY ENVIRONMENT; OUTER HELIOSHEATH; WHISTLER WAVES; ULF WAVES; INSTABILITIES; FLUCTUATIONS; EXCITATION; TURBULENCE AB A recent examination of 1.9 s magnetic field data recorded by the Voyager 2 spacecraft in transit to Jupiter revealed several instances of strongly aliased spectra suggestive of unresolved high-frequency magnetic fluctuations at 4.4 AU. A closer examination of these intervals using the highest resolution data available revealed one clear instance of wave activity at spacecraft frame frequencies from 0.2 to 1 Hz. Using various analysis techniques, we have characterized these fluctuations as Bernstein mode waves excited by newborn interstellar pickup ions. We can find no other interpretation or source consistent with the observations, but this interpretation is not without questions. In this paper, we report a detailed analysis of the waves, including their frequency and polarization, that supports our interpretation. C1 [Joyce, Colin J.; Smith, Charles W.; Isenberg, Philip A.] Univ New Hampshire, Dept Phys, Ctr Space Sci, Durham, NH 03824 USA. [Gary, S. Peter] Los Alamos Natl Lab, Los Alamos, NM USA. [Murphy, Neil] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Burlaga, Leonard F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. RP Joyce, CJ (reprint author), Univ New Hampshire, Dept Phys, Ctr Space Sci, Durham, NH 03824 USA. EM cjl46@unh.edu; Charles.Smith@unh.edu; Phil.Isenberg@unh.edu; pgary@lanl.gov; Neil.Murphy@jpl.nasa.gov; Perry.Gray@dtra.mil; lburlagahsp@verizon.net FU NASA [NNX07AH75G]; NSF [ATM0635863]; Caltech [44A1085631] 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. 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. C.J.J. was an undergraduate in the Physics program at UNH at the time this work was performed and is now a graduate student working within that same program. Perry Gray died unexpectedly just two weeks after this paper was first submitted to the journal. He was a bright and creative scientist who made lifelong friends everywhere he went. He will be greatly missed by friends and colleagues alike. NR 36 TC 10 Z9 10 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 112 DI 10.1088/0004-637X/745/2/112 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800010 ER PT J AU Suchy, S Furst, F Pottschmidt, K Caballero, I Kreykenbohm, I Wilms, J Markowitz, A Rothschild, RE AF Suchy, Slawomir Fuerst, Felix Pottschmidt, Katja Caballero, Isabel Kreykenbohm, Ingo Wilms, Joern Markowitz, Alex Rothschild, Richard E. TI BROADBAND SPECTROSCOPY USING TWO SUZAKU OBSERVATIONS OF THE HMXB GX 301-2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (GX 301-2); stars: magnetic field; X-rays: binaries; X-rays: stars ID PULSE PHASE SPECTROSCOPY; CYCLOTRON LINE ENERGY; X-RAY PULSARS; VELA X-1; ORBITAL CYCLE; NEUTRON-STARS; LIGHT-CURVE; 1A 1118-61; GX-301-2; HERCULES-X-1 AB We present the analysis of two Suzaku observations of GX 301-2 at two orbital phases after the periastron passage. Variations in the column density of the line-of-sight absorber are observed, consistent with accretion from a clumpy wind. In addition to a cyclotron resonance scattering feature (CRSF), multiple fluorescence emission lines were detected in both observations. The variations in the pulse profiles and the CRSF throughout the pulse phase have a signature of a magnetic dipole field. Using a simple dipole model we calculated the expected magnetic field values for different pulse phases and were able to extract a set of geometrical angles, loosely constraining the dipole geometry in the neutron star. From the variation of the CRSF width and energy, we found a geometrical solution for the dipole, making the inclination consistent with previously published values. C1 [Suchy, Slawomir; Markowitz, Alex; Rothschild, Richard E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Fuerst, Felix; Kreykenbohm, Ingo; Wilms, Joern] Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany. [Fuerst, Felix; Kreykenbohm, Ingo; Wilms, Joern] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. [Pottschmidt, Katja] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Pottschmidt, Katja] CRESST, Greenbelt, MD 20771 USA. [Caballero, Isabel] Univ Paris 07, CEA Saclay, DSM IRFU SAp UMR AIM 7158, CNRS CEA, Gif Sur Yvette, France. RP Suchy, S (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM ssuchy@ucsd.edu RI Wilms, Joern/C-8116-2013; Kreykenbohm, Ingo/H-9659-2013; XRAY, SUZAKU/A-1808-2009 OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803; FU NASA [NAS5-30720, NNX08AX83G]; DLR [50 OR 0808]; DAAD; French Space Agency CNES through CNRS FX S.S. acknowledges support by NASA contract NAS5-30720 and grant NNX08AX83G. F. F. is supported by DLR grant 50 OR 0808 and via a DAAD Fellowship. I. C. acknowledges financial support from the French Space Agency CNES through CNRS. 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). NR 52 TC 18 Z9 19 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 124 DI 10.1088/0004-637X/745/2/124 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800022 ER PT J AU Thejappa, G MacDowall, RJ Bergamo, M AF Thejappa, G. MacDowall, R. J. Bergamo, M. TI EMISSION PATTERNS OF SOLAR TYPE III RADIO BURSTS: STEREOSCOPIC OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: coronal mass ejections (CMEs); Sun: flares; Sun: radio radiation ID CORONAL SCATTERING; PLASMA; DIRECTIVITY; RADIOBURSTS; SPACECRAFT; REFRACTION; WAVES; WIND AB Simultaneous observations of solar type III radio bursts obtained by the STEREO A, B, and WIND spacecraft at low frequencies from different vantage points in the ecliptic plane are used to determine their directivity. The heliolongitudes of the sources of these bursts, estimated at different frequencies by assuming that they are located on the Parker spiral magnetic field lines emerging from the associated active regions into the spherically symmetric solar atmosphere, and the heliolongitudes of the spacecraft are used to estimate the viewing angle, which is the angle between the direction of the magnetic field at the source and the line connecting the source to the spacecraft. The normalized peak intensities at each spacecraft R-j = I-j/Sigma I-j (the subscript j corresponds to the spacecraft STEREO A, B, and WIND), which are defined as the directivity factors are determined using the time profiles of the type III bursts. It is shown that the distribution of the viewing angles divides the type III bursts into: (1) bursts emitting into a very narrow cone centered around the tangent to the magnetic field with angular width of similar to 2 degrees and (2) bursts emitting into a wider cone with angular width spanning from similar to-100 degrees to similar to 100 degrees. The plots of the directivity factors versus the viewing angles of the sources from all three spacecraft indicate that the type III emissions are very intense along the tangent to the spiral magnetic field lines at the source, and steadily fall as the viewing angles increase to higher values. The comparison of these emission patterns with the computed distributions of the ray trajectories indicate that the intense bursts visible in a narrow range of angles around the magnetic field directions probably are emitted in the fundamental mode, whereas the relatively weaker bursts visible to a wide range of angles are probably emitted in the harmonic mode. C1 [Thejappa, G.; Bergamo, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [MacDowall, R. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Thejappa, G (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM thejappa.golla@nasa.gov; Robert.MacDowall@nasa.gov; mbergamo@umd.edu RI MacDowall, Robert/D-2773-2012 FU NASA [NNX08AO02G, NNX09AB19G] FX The research of T. G. is supported by the NASA Grants NNX08AO02G and NNX09AB19G. The SWAVES instruments include contributions from the Observatoire of Paris, University of Minnesota, University of California, Berkeley, and NASA/GSFC. NR 29 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 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 187 DI 10.1088/0004-637X/745/2/187 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800085 ER PT J AU Winter, LM Veilleux, S McKernan, B Kallman, TR AF Winter, Lisa M. Veilleux, Sylvain McKernan, Barry Kallman, T. R. TI THE SWIFT BURST ALERT TELESCOPE DETECTED SEYFERT 1 GALAXIES: X-RAY BROADBAND PROPERTIES AND WARM ABSORBERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATIONS; LINE RADIO GALAXIES; ULTRA-FAST OUTFLOWS; BLACK-HOLE MASS; INTRINSIC ABSORPTION; SPECTRAL PROPERTIES; SUZAKU OBSERVATION; COMPTON REFLECTION; SOFT EXCESS AB We present results from an analysis of the broadband, 0.3-195 keV, X-ray spectra of 48 Seyfert 1-1.5 sources detected in the very hard X-rays with the Swift Burst Alert Telescope (BAT). This sample is selected in an all-sky survey conducted in the 14-195 keV band. Therefore, our sources are largely unbiased toward both obscuration and host galaxy properties. Our detailed and uniform model fits to Suzaku/BAT and XMM-Newton/BAT spectra include the neutral absorption, direct power-law, reflected emission, soft excess, warm absorption, and narrow Fe I K alpha emission properties for the entire sample. We significantly detect O VII and O VIII edges in 52% of our sample. The strength of these detections is strongly correlated with the neutral column density measured in the spectrum. Among the strongest detections, X-ray grating and UV observations, where available, indicate outflowing material. The ionized column densities of sources with O VII and O VIII detections are clustered in a narrow range with N-warm similar to 10(21) cm(-2), while sources without strong detections have column densities of ionized gas an order of magnitude lower. Therefore, we note that sources without strong detections likely have warm ionized outflows present but at low column densities that are not easily probed with current X-ray observations. Sources with strong complex absorption have a strong soft excess, which may or may not be due to difficulties in modeling the complex spectra of these sources. Still, the detection of a flat Gamma similar to 1 and a strong soft excess may allow us to infer the presence of strong absorption in low signal-to-noise active galactic nucleus spectra. Additionally, we include a useful correction from the Swift BAT luminosity to bolometric luminosity, based on a comparison of our spectral fitting results with published spectral energy distribution fits from 33 of our sources. C1 [Winter, Lisa M.] Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [McKernan, Barry] CUNY, Dept Sci, Borough Manhattan Community Coll, New York, NY 10007 USA. [McKernan, Barry] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [McKernan, Barry] CUNY, Grad Ctr, New York, NY 10016 USA. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Winter, LM (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, UCB 391, Boulder, CO 80309 USA. RI XRAY, SUZAKU/A-1808-2009; OI Winter, Lisa/0000-0002-3983-020X FU NASA [NNX09AV60G]; NASA through Space Telescope Science Institute [HST-HF-51263.01-A]; Association of Universities for Research in Astronomy, Incorporated, under NASA [NAS5-26555] FX L.M.W. acknowledges CU undergraduate student Tatiana Taylor for assistance with the initial data reductions. Also, we gratefully acknowledge support from NASA grant NNX09AV60G for Suzaku guest observer observations and NASA grant HST-HF-51263.01-A, through a Hubble Fellowship from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This work utilizes observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has made use of data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center. NR 100 TC 38 Z9 39 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 107 DI 10.1088/0004-637X/745/2/107 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800005 ER PT J AU Polyakov, IV Walsh, JE Kwok, R AF Polyakov, Igor V. Walsh, John E. Kwok, Ronald TI Recent Changes of Arctic Multiyear Sea Ice Coverage and the Likely Causes SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Editorial Material ID OCEAN; AMPLIFICATION; THICKNESS C1 [Polyakov, Igor V.; Walsh, John E.] Univ Alaska Fairbanks, Int Arctic Res Ctr, Fairbanks, AK 99775 USA. [Kwok, Ronald] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Polyakov, IV (reprint author), Univ Alaska Fairbanks, Int Arctic Res Ctr, POB 757335, Fairbanks, AK 99775 USA. EM igor@iarc.uaf.edu RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 NR 32 TC 46 Z9 50 U1 2 U2 32 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD FEB PY 2012 VL 93 IS 2 BP 145 EP 151 DI 10.1175/BAMS-D-11-00070.1 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 897FP UT WOS:000300632200004 ER PT J AU Evans, C Archambault, HRM Cordeira, JM Fritz, C Galarneau, TJ Gjorgjievska, S Griffin, KS Johnson, A Komaromi, WA Monette, S Muradyan, P Murphy, B Riemer, M Sears, J Stern, D Tang, B Thompson, S AF Evans, Clark Archambault, Heathe R. M. Cordeira, Jason M. Fritz, Cody Galarneau, Thomas J., Jr. Gjorgjievska, Saska Griffin, Kyle S. Johnson, Alexandria Komaromi, William A. Monette, Sarah Muradyan, Paytsar Murphy, Brian Riemer, Michael Sears, John Stern, Daniel Tang, Brian Thompson, Segayle TI THE PRE-DEPRESSION INVESTIGATION OF CLOUD-SYSTEMS IN THE TROPICS (PREDICT) FIELD CAMPAIGN Perspectives of Early Career Scientists SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID CYCLOGENESIS; OPPORTUNITIES; CYCLONES; WAVES C1 [Evans, Clark; Tang, Brian] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Archambault, Heathe R. M.; Cordeira, Jason M.; Griffin, Kyle S.] SUNY Albany, Albany, NY 12222 USA. [Fritz, Cody] Univ Illinois, Urbana, IL USA. [Galarneau, Thomas J., Jr.] Univ Colorado, CIRES, Boulder, CO 80309 USA. [Gjorgjievska, Saska] New Mexico Inst Min & Technol, Socorro, NM 87801 USA. [Johnson, Alexandria; Muradyan, Paytsar; Murphy, Brian] Purdue Univ, W Lafayette, IN 47907 USA. [Komaromi, William A.] Univ Miami, Coral Gables, FL 33124 USA. [Monette, Sarah; Sears, John] Univ Wisconsin, Madison, WI USA. [Riemer, Michael] Johannes Gutenberg Univ Mainz, Mainz, Germany. [Stern, Daniel] Penn State Univ, State Coll, PA USA. [Thompson, Segayle] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Evans, C (reprint author), Univ Wisconsin, Dept Math Sci, POB 413, Milwaukee, WI 53201 USA. EM evans36@uwm.edu RI Riemer, Michael/C-5491-2009 FU PREDICT; NCAR's Earth Observing Laboratory; NASA [NNG09HG031]; NSF [ATM-1016095]; NOAA GOES-R [NA06NES4400002, 144PH46] FX The ECSs involved in PREDICT are indebted to their respective advisors and mentors for enabling their participation during the field campaign. In addition, these experiences and this manuscript would not have been possible were it not for the support of the PREDICT principal investigators and the staff of NCAR's Earth Observing Laboratory. Contributions from Kathleen Legg, Peggy Lemone, Steve Williams, and Ed Zipser were instrumental in formulating the discussion of the roles ECSs played during GATE. Development of the dividing streamline product was supported in part by NASA through Grant NNG09HG031, and its implementation was aided by discussions with and assistance from Kayo Ide, Mike Montgomery, Scott Braun, Mark Boothe, and Saurabh Barve. The participation of author Fritz was supported in part by NSF Grant ATM-1016095. The participation of author Monette was supported in part by NOAA GOES-R Proving Ground Program Contract No. NA06NES4400002, Fund 144PH46. NR 17 TC 4 Z9 4 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD FEB PY 2012 VL 93 IS 2 BP 173 EP 187 DI 10.1175/BAMS-D-11-00024.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 897FP UT WOS:000300632200006 ER PT J AU Holdeman, JD Clisset, JR Moder, JP AF Holdeman, James D. Clisset, James R. Moder, Jeffrey P. TI Spreadsheet calculations of jets in crossflow: opposed rows of inline and staggered round holes SO HEAT AND MASS TRANSFER LA English DT Article ID MULTIPLE JETS; ORIFICES AB The objective of this study was to demonstrate and analyze empirical model results for jet-in-crossflow configurations which are typical in gas turbine combustors. Calculations in this paper, for opposed rows of round holes in both inline and staggered arrangements, were made with an Excel(A (R)) spreadsheet implementation of a NASA-developed empirical model for the mean conserved scalar field. Results for cases of opposed rows of jets with the orifices on one side shifted by half the orifice spacing shows that staggering can improve the mixing, particularly for cases that would overpenetrate if the orifices were in an aligned configuration. For all cases investigated, the dimensionless variance of the mixture fraction decreased significantly with increasing downstream distance. The variation between cases at a given downstream location was smaller, but the "best" mixers for opposed rows of jets were found to be inline and staggered arrangements at an orifice spacing that is optimum for inline jets. C1 [Holdeman, James D.; Moder, Jeffrey P.] NASA, Combust Branch, Glenn Res Ctr, Cleveland, OH 44135 USA. [Clisset, James R.] Univ Florida, Gainesville, FL 32611 USA. RP Holdeman, JD (reprint author), NASA, Combust Branch, Glenn Res Ctr, Cleveland, OH 44135 USA. EM jjdholdeman@aol.com NR 9 TC 3 Z9 3 U1 0 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0947-7411 J9 HEAT MASS TRANSFER JI Heat Mass Transf. PD FEB PY 2012 VL 48 IS 2 BP 413 EP 424 DI 10.1007/s00231-011-0913-6 PG 12 WC Thermodynamics; Mechanics SC Thermodynamics; Mechanics GA 889OO UT WOS:000300083200019 ER PT J AU O'Brien, S Kent, NJ Lucitt, M Ricco, AJ McAtamney, C Kenny, D Meade, G AF O'Brien, Sinead Kent, Nigel J. Lucitt, Margaret Ricco, Antonio J. McAtamney, Colm Kenny, Dermot Meade, Gerardene TI Effective Hydrodynamic Shaping of Sample Streams in a Microfluidic Parallel-Plate Flow-Assay Device: Matching Whole Blood Dynamic Viscosity SO IEEE TRANSACTIONS ON BIOMEDICAL ENGINEERING LA English DT Article DE Arterial shear rate; dynamic viscosity; hydrodynamic focusing; parallel-plate flow chamber; platelets ID VON-WILLEBRAND-FACTOR; THROMBUS FORMATION; GLOBAL ASSESSMENT; ADHESION; ENDOTHELIUM; HEMOSTASIS; MECHANISMS; SELECTIN; CELLS; VWF AB We report the development of an aqueous buffer system tailored to the fluidic and hemodynamic requirements of our recently reported microfluidic platelet dynamic assay device, which uses hydrodynamic focusing to "shape" a blood sample into a thin flowing layer adjacent to its protein-functionalized surface. By matching the dynamic viscosity of whole blood (3.13 +/- 0.08 mPa.s, from healthy donors), the selected buffer minimizes interfacial fluid mixing and better controls shear rate within the device, permitting platelet/protein-surface interaction assays with as little as 50 mu L of whole blood. Buffers containing the viscosity-enhancing components bovine serum albumin (BSA), gelofusine/glycine, or histopaque (Ficoll gradient solution) were found not to activate platelets when incubated with blood at concentrations up to 50%, as assessed by flow cytometry quantitation of P-selectin expression and alpha IIb beta(3) activation. In contrast, glycerol-based buffer activated platelets (two-fold increase in P-selectin levels) at concentrations as low as 10% by volume. BSA- and gelofusine/glycine-based buffers were problematic in preparation and use, and therefore, were not used beyond initial characterization. The histopaque solution selected as the best choice for flow studies stabilizes sample contact with the device's thrombogenic surface, does not activate platelets, and does not interfere with the action of agonists added to deliberately activate platelets. C1 [O'Brien, Sinead; Lucitt, Margaret; Kenny, Dermot; Meade, Gerardene] Royal Coll Surgeons Ireland, Biomed Diagnost Inst, Dublin 2, Ireland. [Kent, Nigel J.; Ricco, Antonio J.; McAtamney, Colm] Dublin City Univ, Biomed Diagnost Inst, Dublin 9, Ireland. [Kent, Nigel J.] Dublin Inst Technol, Coll Engn & Built Environm, Biomed Devices & Assist Technol Res Grp, Dublin 1, Ireland. [Ricco, Antonio J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Meade, G (reprint author), Royal Coll Surgeons Ireland, Biomed Diagnost Inst, Dublin 2, Ireland. EM sineadobrien2@rcsi.ie; nigel.kent@dcu.ie; LUCITTM@tcd.ie; ajricco@stanford.edu; colm.mcatamney@dcu.ie; dkenny@rcsi.ie; gmeade@rcsi.ie RI Kenny, Dermot/C-3898-2012; Ricco, Antonio/A-5273-2010; OI Ricco, Antonio/0000-0002-2355-4984 FU Science Foundation Ireland [10/CE/B1821] FX Manuscript received February 11, 2011; revised August 8, 2011; accepted September 14, 2011. Date of publication October 19, 2011; date of current version January 20, 2012. This work was supported by the Science Foundation Ireland under Grant No. 10/CE/B1821.1 Asterisk indicates corresponding author. NR 35 TC 2 Z9 2 U1 1 U2 21 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9294 J9 IEEE T BIO-MED ENG JI IEEE Trans. Biomed. Eng. PD FEB PY 2012 VL 59 IS 2 BP 374 EP 382 DI 10.1109/TBME.2011.2172607 PG 9 WC Engineering, Biomedical SC Engineering GA 895PF UT WOS:000300507800010 PM 22020664 ER PT J AU Bradford, AL Weller, DW Punt, AE Ivashchenko, YV Burdin, AM VanBlaricom, GR Brownell, RL AF Bradford, Amanda L. Weller, David W. Punt, Andre E. Ivashchenko, Yulia V. Burdin, Alexander M. VanBlaricom, Glenn R. Brownell, Robert L., Jr. TI Leaner leviathans: body condition variation in a critically endangered whale population SO JOURNAL OF MAMMALOGY LA English DT Article DE density-independence; energy reserves; environmental variability; fitness; Okhotsk Sea; ordinal logistic regression; photo-identification; western gray whales ID ESCHRICHTIUS-ROBUSTUS; NUTRITIONAL CONDITION; GRAY WHALE; CONDITION INDEXES; SAKHALIN ISLAND; HIGH AGREEMENT; FAT CONDITION; ATLANTIC FIN; POLAR BEARS; LOW KAPPA AB The role of environmental limitation and density-dependent regulation in shaping populations is debated in ecology. Populations at low densities may offer an unobstructed view of basic environmental and physiological interactions that impact individual fitness and thus population productivity. The energy reserves of an organism are reflected in its body condition, a measure linking individual fitness and the environment. From 1997 to 2007, we monitored the critically endangered western gray whale (Eschrichtius robustus) population on its primary summer feeding ground off the northeastern coast of Sakhalin Island, Russia. This effort resulted in a large data set of photo-identification images from 5,007 sightings of 168 individual whales that we used to visually assess western gray whale body condition. We quantified temporal variation in the resulting 1,539 monthly body condition determinations with respect to observations of reproductive status and sex. Western gray whale body condition varied annually, and we identified years of significantly better (2004) and worse ((999, 2006, and 2007) body condition. This study is the 1st to track the within-season body condition of individual whales. Body condition improved significantly as the summer progressed, although results suggest that not all whales replenish their energy stores by the end of the season. The body condition of lactating females was significantly worse than that of other whales at all times and was most often determined to be compromised. The body condition of their weaning calves exhibited no temporal variation and was consistently good. It is possible lactating females provide an energetic buffer to their offspring at the expense of their own body condition and future reproductive success. Findings from the analysis establish a foundation for quantifying links between western gray whale body condition, demographic parameters, and environmental conditions; and provide a baseline for monitoring individual and population condition of an ecosystem sentinel species in a changing environment. Overall, this study highlights the presence of density-independent environmental and physiological mechanisms that affect the abundance and growth of populations. C1 [Weller, David W.] NOAA, Protected Resources Div, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla, CA 92037 USA. [Ivashchenko, Yulia V.] Seastar Sci, Yaroslavl 150033, Russia. [Bradford, Amanda L.] Russian Acad Sci, Far E Branch, Kamchatka Branch, Pacific Inst Geog, Petropavlovsk Kamchatski 683024, Russia. [Brownell, Robert L., Jr.] NOAA, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Pacific Grove, CA 93950 USA. [Bradford, Amanda L.; Punt, Andre E.; VanBlaricom, Glenn R.] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA. RP Bradford, AL (reprint author), NOAA, Protected Species Div, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, 1601 Kapiolani Blvd,Suite 1000, Honolulu, HI 96814 USA. EM alb992@u.washington.edu OI Punt, Andre/0000-0001-8489-2488 FU University of Washington; Alaska Sea Life Center; Exxon Neftegas Limited; International Fund for Animal Welfare; International Whaling Commission; United States Marine Mammal Commission; Texas A&M University at Galveston; National Fish and Wildlife Foundation; United States National Marine Fisheries Service; Ocean Park Conservation Foundation; Sakhalin Energy Investment Company; School of Aquatic and Fishery Sciences at the University of Washington; United States Environmental Protection Agency; Washington Cooperative Fish and Wildlife Research Unit FX We thank the many individuals who have provided field assistance over the years, especially S. Blokhin, H. W. Kim, A. Lang, S. Rickards, and G. Tsidulko. Participants in the 2006 NOAA Large Whale Health Assessment Workshop contributed valuable feedback on the body condition assessment protocol. N. Ellis, P. Heagerty, and R. Christensen offered useful advice on the statistical analysis. The edits of W. Perrin and 2 anonymous reviewers improved the manuscript. Support for ALB was funded in part by a grant from the Washington Sea Grant Program, University of Washington, pursuant to National Oceanic and Atmospheric Administration Graduate Fellowship Program in Population Dynamics and Marine Resource Economics. The views expressed herein are those of the authors and do not necessarily reflect the views of National Oceanic and Atmospheric Administration or any of its subagencies. Support and funding for the Russia United States western gray whale research project were provided (in alphabetical order) by Alaska Sea Life Center, Exxon Neftegas Limited, the International Fund for Animal Welfare, the International Whaling Commission, the United States Marine Mammal Commission, the Marine Mammal Research Program at Texas A&M University at Galveston, the National Fish and Wildlife Foundation, the United States National Marine Fisheries Service, Ocean Park Conservation Foundation, Sakhalin Energy Investment Company, the School of Aquatic and Fishery Sciences at the University of Washington, the United States Environmental Protection Agency, and the Washington Cooperative Fish and Wildlife Research Unit. The project was conducted as part of the Marine Mammal Project under Area V: Protection of Nature and the Organization of Reserves within the United States Russia Agreement on Cooperation in the Field of Environmental Protection. NR 83 TC 14 Z9 15 U1 2 U2 26 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD FEB PY 2012 VL 93 IS 1 BP 251 EP 266 DI 10.1644/11-MAMM-A-091.1 PG 16 WC Zoology SC Zoology GA 896VE UT WOS:000300598700023 ER PT J AU Villanueva, GL Mumma, MJ Bonev, BP Novak, RE Barber, RJ DiSanti, MA AF Villanueva, G. L. Mumma, M. J. Bonev, B. P. Novak, R. E. Barber, R. J. DiSanti, M. A. TI Water in planetary and cometary atmospheres: H2O/HDO transmittance and fluorescence models SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Planetary atmospheres; Water; Comets; Mars; Fluorescence ID MOLECULAR SPECTROSCOPIC DATABASE; THERMAL EMISSION SPECTROMETER; INFRARED SOLAR SPECTRA; C/1996 B2 HYAKUTAKE; COMPUTED LINE LIST; DEUTERATED WATER; ENERGY-LEVELS; ISOTOPIC CO2; ANNUAL CYCLE; HALF-WIDTHS AB We developed a modern methodology to retrieve water (H2O) and deuterated water (HDO) in planetary and cometary atmospheres, and constructed an accurate spectral database that combines theoretical and empirical results. On the basis of a greatly expanded set of spectroscopic parameters, we built a full non-resonance cascade fluorescence model and computed fluorescence efficiencies for H2O (500 million lines) and HDO (700 million lines). The new line list was also integrated into an advanced terrestrial radiative transfer code (LBLRTM) and adapted to the CO2 rich atmosphere of Mars, for which we adopted the complex Robert-Bonamy formalism for line shapes. We retrieved water and D/H in the atmospheres of Mars, comet C/2007 W1 (Boattini), and Earth by applying the new formalism to spectra obtained with the high-resolution spectrograph NIRSPEC/Keck II atop Mauna Kea (Hawaii). The new model accurately describes the complex morphology of the water bands and greatly increases the accuracy of the retrieved abundances (and the D/H ratio in water) with respect to previously available models. The new model provides improved agreement of predicted and measured intensities for many H2O lines already identified in comets, and it identifies several unassigned cometary emission lines as new emission lines of H2O. The improved spectral accuracy permits retrieval of more accurate rotational temperatures and production rates for cometary water. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Villanueva, G. L.; Mumma, M. J.; Bonev, B. P.; DiSanti, M. A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Villanueva, G. L.; Bonev, B. P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Novak, R. E.] Iona Coll, Dept Phys, New Rochelle, NY 10801 USA. [Barber, R. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. RP Villanueva, GL (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Mailstop 690-3, Greenbelt, MD 20771 USA. EM Geronimo.Villanueva@nasa.gov RI mumma, michael/I-2764-2013 FU NASA [08-PAST08-0034, 08-PATM08-0031, RTOP 344-32-07, RTOP 344-53-51]; NSF [AST-0807939]; NSF-RUI [AST-0805540] FX GLV acknowledges support from NASA's Planetary Astronomy Program (08-PAST08-0034) and NASA's Planetary Atmospheres Program (08-PATM08-0031). NASA's Planetary Astronomy Program (RTOP 344-32-07) and NASA's Astrobiology Program (RTOP 344-53-51) supported MJM. BPB acknowledges support from the NSF Astronomy and Astrophysics Research Grants Program (AST-0807939). NSF-RUI supported REN through Grant (AST-0805540). We thank Dr. Alan Tokunaga and Alain Khayat for assisting with the acquisition of Mars data in 2010, Dr. Robert Gamache for assisting with the application of his Robert-Bonamy algorithm, and Dr. Jonathan Tennyson and Dr. Iouli Gordon for providing critical assistance in the interpretation of the HITEMP and SELP databases. We greatly acknowledge the valuable insights of the reviewers that led us to an improved manuscript. We thank the staff of the W.M. Keck Observatory (operated as a scientific partnership among CalTech, UCLA, and NASA) for their exceptional support throughout our long Mars and cometary observing Programs. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 88 TC 30 Z9 30 U1 0 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD FEB PY 2012 VL 113 IS 3 BP 202 EP 220 DI 10.1016/j.jqsrt.2011.11.001 PG 19 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 896SK UT WOS:000300591500001 ER PT J AU Roseboom, IG Ivison, RJ Greve, TR Amblard, A Arumugam, V Auld, R Aussel, H Bethermin, M Blain, A Bock, J Boselli, A Brisbin, D Buat, V Burgarella, D Castro-Rodriguez, N Cava, A Chanial, P Chapin, E Chapman, S Clements, DL Conley, A Conversi, L Cooray, A Dowell, CD Dunlop, JS Dwek, E Eales, S Elbaz, D Farrah, D Franceschini, A Glenn, J Griffin, M Halpern, M Hatziminaoglou, E Ibar, E Isaak, K Lagache, G Levenson, L Lu, N Madden, S Maffei, B Mainetti, G Marchetti, L Marsden, G Morrison, G Mortier, AMJ Nguyen, HT O'Halloran, B Oliver, SJ Omont, A Page, MJ Panuzzo, P Papageorgiou, A Pearson, CP Perez-Fournon, I Pohlen, M Rawlings, JI Raymond, G Rigopoulou, D Rizzo, D Rodighiero, G Rowan-Robinson, M Schulz, B Scott, D Seymour, N Shupe, DL Smith, AJ Stevens, JA Symeonidis, M Trichas, M Tugwell, KE Vaccari, M Valtchanov, I Vieira, JD Viero, MP Vigroux, L Wardlow, J Wang, L Wright, G Xu, CK Zemcov, M AF Roseboom, I. G. Ivison, R. J. Greve, T. R. Amblard, A. Arumugam, V. Auld, R. Aussel, H. Bethermin, M. Blain, A. Bock, J. Boselli, A. Brisbin, D. Buat, V. Burgarella, D. Castro-Rodriguez, N. Cava, A. Chanial, P. Chapin, E. Chapman, S. Clements, D. L. Conley, A. Conversi, L. Cooray, A. Dowell, C. D. Dunlop, J. S. Dwek, E. Eales, S. Elbaz, D. Farrah, D. Franceschini, A. Glenn, J. Griffin, M. Halpern, M. Hatziminaoglou, E. Ibar, E. Isaak, K. Lagache, G. Levenson, L. Lu, N. Madden, S. Maffei, B. Mainetti, G. Marchetti, L. Marsden, G. Morrison, G. Mortier, A. M. J. Nguyen, H. T. O'Halloran, B. Oliver, S. J. Omont, A. Page, M. J. Panuzzo, P. Papageorgiou, A. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Rawlings, J. I. Raymond, G. Rigopoulou, D. Rizzo, D. Rodighiero, G. Rowan-Robinson, M. Schulz, B. Scott, Douglas Seymour, N. Shupe, D. L. Smith, A. J. Stevens, J. A. Symeonidis, M. Trichas, M. Tugwell, K. E. Vaccari, M. Valtchanov, I. Vieira, J. D. Viero, M. P. Vigroux, L. Wardlow, J. Wang, L. Wright, G. Xu, C. K. Zemcov, M. TI The Herschel Multi-tiered Extragalactic Survey: SPIRE-mm photometric redshifts SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: high-redshift - galaxies: statistics - submillimetre: galaxies ID DEEP-FIELD-SOUTH; GOODS-N FIELD; FAR-INFRARED PROPERTIES; BRIGHTEST SUBMILLIMETER SOURCE; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMATION HISTORY; FAINT RADIO GALAXIES; MU-M OBSERVATIONS; LABOCA SURVEY; MIDINFRARED COUNTERPARTS AB We investigate the potential of submmmm and submmmmradio photometric redshifts using a sample of mm-selected sources as seen at 250, 350 and 500 mu m by the SPIRE instrument on Herschel. From a sample of 63 previously identified mm sources with reliable radio identifications in the Great Observatories Origins Deep Survey North and Lockman Hole North fields, 46 (73 per cent) are found to have detections in at least one SPIRE band. We explore the observed submm/mm colour evolution with redshift, finding that the colours of mm sources are adequately described by a modified blackbody with constant optical depth tau=(/nu0)beta, where beta=+1.8 and nu 0=c/100 mu m. We find a tight correlation between dust temperature and IR luminosity. Using a single model of the dust temperature and IR luminosity relation, we derive photometric redshift estimates for the 46 SPIRE-detected mm sources. Testing against the 22 sources with known spectroscopic or good quality optical/near-IR photometric redshifts, we find submm/mm photometric redshifts offer a redshift accuracy of vertical bar Delta z vertical bar/(1+z)= 0.16 (=0.51). Including constraints from the radiofar-IR correlation, the accuracy is improved to vertical bar Delta z vertical bar/(1+z)=0.15 (=0.45). We estimate the redshift distribution of mm-selected sources finding a significant excess at z > 3 when compared to similar to 850 mu m selected samples. C1 [Roseboom, I. G.; Farrah, D.; Oliver, S. J.; Smith, A. J.; Wang, L.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Roseboom, I. G.; Ivison, R. J.; Dunlop, J. S.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.; Arumugam, V.; Ibar, E.; Wright, G.] UK Astron Technol Ctr, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Greve, T. R.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Amblard, A.; Cooray, A.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Auld, R.; Eales, S.; Griffin, M.; Isaak, K.; Papageorgiou, A.; Pohlen, M.; Raymond, G.] Cardiff Univ, Cardiff Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aussel, H.; Bethermin, M.; Chanial, P.; Elbaz, D.; Madden, S.; Panuzzo, P.] Univ Paris Diderot, Lab AIM Paris Saclay, CE Saclay, CEA,DSM,Irfu,CNRS, F-91191 Gif Sur Yvette, France. [Bock, J.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Boselli, A.; Buat, V.; Burgarella, D.] Univ Aix Marseille, CNRS, Lab Astrophys Marseille, OAMP, F-13388 Marseille 13, France. [Brisbin, D.] Cornell Univ, Ithaca, NY 14853 USA. [Castro-Rodriguez, N.; Cava, A.; Perez-Fournon, I.] Inst Astrofis Canarias IAC, E-38200 Tenerife, Spain. [Castro-Rodriguez, N.; Cava, A.; Perez-Fournon, I.] Univ La Laguna ULL, Dept Astrofis, E-38205 Tenerife, Spain. [Chapin, E.; Halpern, M.; Marsden, G.; Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Chapman, S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Clements, D. L.; Mortier, A. M. J.; O'Halloran, B.; Rizzo, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Conversi, L.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Dwek, E.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Franceschini, A.; Mainetti, G.; Marchetti, L.; Rodighiero, G.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Hatziminaoglou, E.] ESO, D-85748 Garching, Germany. [Lagache, G.] Univ Paris 11, Inst Astrophys Spatiale IAS, F-91405 Orsay, France. [Lu, N.; Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, Infrared Proc & Anal Ctr, JPL, Pasadena, CA 91125 USA. [Maffei, B.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Morrison, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Morrison, G.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Omont, A.; Vigroux, L.] UPMC Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. [Page, M. J.; Rawlings, J. I.; Seymour, N.; Symeonidis, M.; Tugwell, K. E.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Pearson, C. P.; Rigopoulou, D.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Rigopoulou, D.] Univ Oxford, Oxford OX1 3RH, England. [Stevens, J. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Trichas, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Roseboom, IG (reprint author), Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. EM igr@roe.ac.uk RI Dwek, Eli/C-3995-2012; amblard, alexandre/L-7694-2014; Wardlow, Julie/C-9903-2015; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017; OI amblard, alexandre/0000-0002-2212-5395; Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275; Scott, Douglas/0000-0002-6878-9840; Marchetti, Lucia/0000-0003-3948-7621; Seymour, Nicholas/0000-0003-3506-5536; Bethermin, Matthieu/0000-0002-3915-2015; Rodighiero, Giulia/0000-0002-9415-2296 FU Science and Technology Facilities Council [ST/F002858/1]; Royal Society; European Research Council; Italian Space Agency (ASI) [I/005/07/0]; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA) FX LW and SJO were supported by the Science and Technology Facilities Council (ST/F002858/1).; JSD acknowledges the support of the Royal Society via a Wolfson Research Merit award, and the support of the European Research Council via the award of an Advanced Grant.; AF, GM, LM and MV were supported by the Italian Space Agency (ASI Herschel Science Contract I/005/07/0).; SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada), NAOC (China), CEA, LAM(France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UK ATC, University of Sussex (UK), Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA (USA). NR 89 TC 63 Z9 63 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 419 IS 4 BP 2758 EP 2773 DI 10.1111/j.1365-2966.2011.19827.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 873XZ UT WOS:000298920600002 ER PT J AU Fischer, DA Schwamb, ME Schawinski, K Lintott, C Brewer, J Giguere, M Lynn, S Parrish, M Sartori, T Simpson, R Smith, A Spronck, J Batalha, N Rowe, J Jenkins, J Bryson, S Prsa, A Tenenbaum, P Crepp, J Morton, T Howard, A Beleu, M Kaplan, Z vanNispen, N Sharzer, C DeFouw, J Hajduk, A Neal, JP Nemec, A Schuepbach, N Zimmermann, V AF Fischer, Debra A. Schwamb, Megan E. Schawinski, Kevin Lintott, Chris Brewer, John Giguere, Matt Lynn, Stuart Parrish, Michael Sartori, Thibault Simpson, Robert Smith, Arfon Spronck, Julien Batalha, Natalie Rowe, Jason Jenkins, Jon Bryson, Steve Prsa, Andrej Tenenbaum, Peter Crepp, Justin Morton, Tim Howard, Andrew Beleu, Michele Kaplan, Zachary vanNispen, Nick Sharzer, Charlie DeFouw, Justin Hajduk, Agnieszka Neal, Joe P. Nemec, Adam Schuepbach, Nadine Zimmermann, Valerij TI Planet Hunters: the first two planet candidates identified by the public using the Kepler public archive data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: individual: KIC 10905746; stars: individual: KIC 6185331; planetary systems ID CHROMOSPHERIC ACTIVITY; Y-2 ISOCHRONES; STARS; SEARCH; DWARF; KECK AB Planet Hunters is a new citizen science project designed to engage the public in an exoplanet search using NASA Kepler public release data. In the first month after launch, users identified two new planet candidates which survived our checks for false positives. The follow-up effort included analysis of Keck HIRES spectra of the host stars, analysis of pixel centroid offsets in the Kepler data and adaptive optics imaging at Keck using NIRC2. Spectral synthesis modelling coupled with stellar evolutionary models yields a stellar density distribution, which is used to model the transit orbit. The orbital periods of the planet candidates are 9.8844 +/- 0.0087 d (KIC 10905746) and 49.7696 +/- 0.000 39 d (KIC 6185331), and the modelled planet radii are 2.65 and 8.05 R-circle plus. The involvement of citizen scientists as part of Planet Hunters is therefore shown to be a valuable and reliable tool in exoplanet detection. C1 [Fischer, Debra A.; Brewer, John; Giguere, Matt; Sartori, Thibault; Spronck, Julien; Beleu, Michele; Kaplan, Zachary; vanNispen, Nick; Sharzer, Charlie] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Schwamb, Megan E.; Schawinski, Kevin] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Schwamb, Megan E.; Schawinski, Kevin] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Lintott, Chris; Lynn, Stuart; Simpson, Robert; Smith, Arfon] Oxford Astrophys, Oxford OX1 3RH, England. [Lintott, Chris; Parrish, Michael; Smith, Arfon] Adler Planetarium, Chicago, IL 60605 USA. [Sartori, Thibault] Ecole Normale Super, F-75230 Paris 05, France. [Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Jenkins, Jon; Tenenbaum, Peter] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Crepp, Justin; Morton, Tim] CALTECH, Det Astrophys, Pasadena, CA 91125 USA. [Howard, Andrew] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Fischer, DA (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA. EM debra.fischer@yale.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Smith, Arfon/0000-0002-3957-2474; Brewer, John/0000-0002-9873-1471; Schawinski, Kevin/0000-0001-5464-0888; Fischer, Debra/0000-0003-2221-0861 FU Yale University; NASA [10-OUTRCH.210-0001, PF9-00069, NAS8-03060, NAS5-26555]; NSF [AST-100325]; Leverhulme Trust; National Aeronautics and Space Administration; NASA Office of Space Science [NNX09AF08G] FX DAF acknowledges funding support from Yale University and support from the NASA Supplemental Outreach Award, 10-OUTRCH.210-0001. DAF thanks the Yale Keck TAC for telescope time used to obtain data for this paper. MES is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-100325. Support for the work of KS was provided by NASA through Einstein Postdoctoral Fellowship grant number PF9-00069, issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. The Zooniverse is supported by The Leverhulme Trust. We gratefully acknowledge the dedication and achievements of Kepler Science Team and all those who contributed to the success of the mission. We acknowledge use of public release data served by the NASA/IPAC/NExScI Star and Exoplanet Database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We particularly thank the organizers (Charles Beichman, Dawn Gelino and Carolyn Brinkman) and lecturers (David Ciardi, Stephen Kane and Kaspar von Braun) at the 2010 July Sagan Summer Workshop for providing information and guidance that led to the inspiration for the Planet Hunters site. The Kepler public release data is primarily hosted by the Multimission Archive (MAST) at the Space Telescope Science Institute (STScI) 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. This research has made use of NASA's Astrophysics Data System Bibliographic Services. NR 27 TC 50 Z9 50 U1 1 U2 13 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 419 IS 4 BP 2900 EP 2911 DI 10.1111/j.1365-2966.2011.19932.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 873XZ UT WOS:000298920600013 ER PT J AU Balona, LA Lenz, P Antoci, V Bernabei, S Catanzaro, G Daszynska-Daszkiewicz, J Di Criscienzo, M Grigahcene, A Handler, G Kurtz, DW Marconi, M Molenda-Zakowicz, J Moya, A Nemec, JM Pigulski, A Pricopi, D Ripepi, V Smalley, B Suarez, JC Suran, M Hall, JR Kinemuchi, K Klaus, TC AF Balona, L. A. Lenz, P. Antoci, V. Bernabei, S. Catanzaro, G. Daszynska-Daszkiewicz, J. Di Criscienzo, M. Grigahcene, A. Handler, G. Kurtz, D. W. Marconi, M. Molenda-Zakowicz, J. Moya, A. Nemec, J. M. Pigulski, A. Pricopi, D. Ripepi, V. Smalley, B. Suarez, J. C. Suran, M. Hall, J. R. Kinemuchi, K. Klaus, T. C. TI Kepler observations of the high-amplitude d Scuti star V2367 Cyg SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: individual: V2367 Cyg; stars: oscillations; stars: variables: delta Scuti ID STELLAR EVOLUTION CALCULATIONS; DELTA-SCUTI; VARIABLE-STARS; INITIAL CHARACTERISTICS; CLASSICAL CEPHEIDS; INSTABILITY STRIP; PETERSEN DIAGRAMS; ROTATING STARS; PERIOD RATIOS; CADENCE DATA AB We analyse Kepler observations of the high-amplitude d Scuti (HADS) star V2367 Cyg (KIC 9408694). The variations are dominated by a mode with frequency f1= 5.6611 d-1. Two other independent modes with f2= 7.1490 d-1 and f3= 7.7756 d-1 have amplitudes an order of magnitude smaller than f1. Nearly all the light variation is due to these three modes and their combination frequencies, but several hundred other frequencies of very low amplitude are also present. The amplitudes of the principal modes may vary slightly with time. The star has twice the projected rotational velocity of any other HADS star, which makes it unusual. We find a correlation between the phases of the combination frequencies and their pulsation frequencies, which is not understood. Since modes of highest amplitude in HADS stars are normally radial modes, we assumed that this would also be true in this star. However, attempts to model the observed frequencies as radial modes without mode interaction were not successful. For a star with such a relatively high rotational velocity, it is important to consider the effect of mode interaction. Indeed, when this was done, we were able to obtain a model in which a good match with f1 and f2 is obtained, with f1 being the fundamental radial mode. C1 [Balona, L. A.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Lenz, P.; Handler, G.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Antoci, V.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Bernabei, S.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Catanzaro, G.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Daszynska-Daszkiewicz, J.; Molenda-Zakowicz, J.; Pigulski, A.] Uniwersytet Wroclawski, Inst Astron, PL-51622 Wroclaw, Poland. [Di Criscienzo, M.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Grigahcene, A.] Univ Porto, Fac Ciencias, Ctr Astrofis, P-4150762 Oporto, Portugal. [Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Marconi, M.; Ripepi, V.] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy. [Moya, A.] Dept Astrofis, Madrid 28691, Spain. [Nemec, J. M.] Camosun Coll, Dept Phys & Astron, Victoria, BC V8P 5J2, Canada. [Pricopi, D.; Suran, M.] Acad Romana, Astron Inst, Bucharest, Romania. [Smalley, B.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Suarez, J. C.] Inst Astrofis Andalucia CSIC, Granada, Spain. [Hall, J. R.; Kinemuchi, K.; Klaus, T. C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. RP Balona, LA (reprint author), S African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa. EM lab@saao.ac.za RI Suarez, Juan Carlos/C-1015-2009; OI Suarez, Juan Carlos/0000-0003-3649-8384; Antoci, Victoria/0000-0002-0865-3650; Marconi, Marcella/0000-0002-1330-2927 FU NASA's Science Mission Directorate; South African Astronomical Observatory; Polish MNiSW [N N203 379 636, N N203 302635]; Polish grant [N N203 405139]; Austrian Fonds zur Forderung der wissenschaftlichen Forschung [P20526-N16]; Astro-Madrid [CAMS2009/ESP-1496]; Spanish grant [ESP2007-65475-C02-02, AYA 2010-21161-C02-02, CSD2006-00070] FX The authors wish to thank the Kepler team for their generosity in allowing the data to be released to the Kepler Asteroseismic Science Consortium ahead of public release and for their outstanding efforts which have made these results possible. Funding for the Kepler mission is provided by NASA's Science Mission Directorate.; LAB wishes to thank the South African Astronomical Observatory for financial support. PL acknowledges partial financial support from the Polish MNiSW grant N N203 379 636; AP acknowledges the Polish MNiSzW grant N N203 302635 and JM-Z acknowledges the Polish grant N N203 405139. VA and GH were supported by the Austrian Fonds zur Forderung der wissenschaftlichen Forschung under grant P20526-N16. AM acknowledges the funding of Astro-Madrid (CAMS2009/ESP-1496) and the Spanish grants ESP2007-65475-C02-02, AYA 2010-21161-C02-02 and CSD2006-00070. NR 63 TC 12 Z9 12 U1 0 U2 8 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 419 IS 4 BP 3028 EP 3038 DI 10.1111/j.1365-2966.2011.19939.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 873XZ UT WOS:000298920600022 ER PT J AU Miller, NA O'Steen, R Yen, S Kuntz, KD Hammer, D AF Miller, Neal A. O'Steen, Richard Yen, Steffi Kuntz, K. D. Hammer, Derek TI Using the XMM-Newton Optical Monitor to Study Cluster Galaxy Evolution SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID DIGITAL-SKY-SURVEY; STAR-FORMATION RATES; COLOR-MAGNITUDE DIAGRAM; DATA RELEASE; STELLAR POPULATIONS; DUST ATTENUATION; LOCAL UNIVERSE; RICH CLUSTERS; SDSS FILTERS; MILKY-WAY AB We explore the application of XMM-Newton Optical Monitor (XMM-OM) ultraviolet (UV) data to study galaxy evolution. Our sample is constructed as the intersection of all Abell clusters with z < 0.05 and having archival XMM-OM data in either the UVM2 or UVW1 filters, plus optical and UV photometry from the Sloan Digital Sky Survey and GALEX, respectively. The 11 resulting clusters include 726 galaxies with measured redshifts, 520 of which have redshifts placing them within their parent Abell clusters. We develop procedures for manipulating the XMM-OM images and measuring galaxy photometry from them, and we confirm our results via comparison with published catalogs. Color-magnitude diagrams (CMDs) constructed using the XMM-OM data along with SDSS optical data show promise for evolutionary studies, with good separation between red and blue sequences and real variation in the width of the red sequence that is likely indicative of differences in star formation history. This is particularly true for UVW1 data, as the relative abundance of data collected using this filter and its depth make it an attractive choice. Available tools that use stellar synthesis libraries to fit the UV and optical photometric data may also be used, thereby better describing star formation history within the past billion years and providing estimates of total stellar mass that include contributions from young stars. Finally, color-color diagrams that include XMM-OM UV data appear useful to the photometric identification of both extragalactic and stellar sources. C1 [Miller, Neal A.; Yen, Steffi] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [O'Steen, Richard] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Kuntz, K. D.; Hammer, Derek] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Kuntz, K. D.; Hammer, Derek] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. RP Miller, NA (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM nmiller@astro.umd.edu FU NASA [NNX09AC76G]; ESA member states; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; Japanese Monbukagakusho; Max Planck Society FX N.A.M. gratefully acknowledges the support for this work, which was provided by NASA Astrophysics Data Analysis Program grant NNX09AC76G. We thank Antonio Talavera for his excellent work with XMM-OM calibration and the confirmation of an exposure time error for A2063, and we thank the anonymous referee for insightful comments that have improved the analysis and discussion. 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 and the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The analysis in this article was based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and NASA. Funding for the Sloan Digital Sky Survey (SDSS) has been provided by the Alfred P. Sloan Foundation, the participating institutions, the National Aeronautics and Space Administration, the National Science Foundation, the US Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. 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. NR 51 TC 1 Z9 1 U1 0 U2 0 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 FEB PY 2012 VL 124 IS 912 BP 95 EP 113 DI 10.1086/664187 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897IB UT WOS:000300641300001 ER PT J AU Patel, ZS Grugan, KD Rustgi, AK Cucinotta, FA Huff, JL AF Patel, Zarana S. Grugan, Katharine D. Rustgi, Anil K. Cucinotta, Francis A. Huff, Janice L. TI Ionizing Radiation Enhances Esophageal Epithelial Cell Migration and Invasion Through a Paracrine Mechanism Involving Stromal-Derived Hepatocyte Growth Factor SO RADIATION RESEARCH LA English DT Article ID PANCREATIC-CANCER CELLS; TUMOR MICROENVIRONMENT; IN-VITRO; BREAST-CANCER; MET; FIBROBLASTS; CARCINOMA; INTERLEUKIN-8; METASTASIS; ACTIVATION AB Esophageal cancer is the sixth leading cause of cancer death worldwide and the seventh leading cause of cancer death in the U.S. male population. Ionizing radiation exposure is a risk factor for development of esophageal squamous cell carcinoma, a histological subtype of esophageal cancer that is highly aggressive and is associated with poor patient prognosis. This study investigated the effects of ionizing radiation on the microenvironment and intercellular communication as it relates to esophageal carcinogenesis. We demonstrate that normal esophageal epithelial cells exhibited increased migration and invasion when cultured in the presence of irradiated stromal fibroblasts or with conditioned medium derived from irradiated stromal fibroblasts. Cytokine antibody arrays and ELISAs were used to identify hepatocyte growth factor (HGF) as an abundant protein that is secreted by esophageal fibroblasts at twofold increased levels in culture medium after gamma irradiation. Reverse transcription qPCR analysis confirmed an approximately 50% increase in mRNA levels for HGF at 1 h in irradiated fibroblasts compared to unirradiated controls. Recombinant HGF stimulated increased wound healing, migration and invasion of esophageal epithelial cells, while blocking antibodies against HGF significantly decreased migration and invasion of epithelial cells in coculture with irradiated fibroblasts. Since HGF is known to direct cell migration, invasion and metastasis in a variety of tissues, including the esophagus, its modulation by ionizing radiation may have important implications for nontargeted pathways that influence radiation carcinogenesis in the esophagus. (C) 2012 by Radiation Research Society C1 [Cucinotta, Francis A.; Huff, Janice L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Patel, Zarana S.; Huff, Janice L.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA. [Grugan, Katharine D.; Rustgi, Anil K.] Univ Penn, Div Gastroenterol, Dept Med, Abramson Canc Ctr, Philadelphia, PA 19104 USA. [Grugan, Katharine D.; Rustgi, Anil K.] Univ Penn, Div Gastroenterol, Dept Genet, Abramson Canc Ctr, Philadelphia, PA 19104 USA. [Grugan, Katharine D.] Centocor R&D, Radnor, PA 19087 USA. RP Huff, JL (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,Mail Code SK-SRPE-B37, Houston, TX 77058 USA. EM janice.l.huff@nasa.gov FU NASA [NNJ06HG25A]; American Cancer Society; NIH/NDDK [P30-DK050306]; NIH/NRSA [F32DK-082149-01]; NIH/NCI [P01-CA098101] FX This work was supported by a grant from NASA NNJ06HG25A (JLH), NIH/NCI P01-CA098101 (AKR), American Cancer Society Research Professorship (AKR), NIH/NDDK P30-DK050306 (Cell Culture Core), and NIH/NRSA F32DK-082149-01 (KDG). NR 52 TC 6 Z9 6 U1 1 U2 9 PU RADIATION RESEARCH SOC PI LAWRENCE PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA SN 0033-7587 J9 RADIAT RES JI Radiat. Res. PD FEB PY 2012 VL 177 IS 2 BP 200 EP 208 DI 10.1667/RR2790.1 PG 9 WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology, Nuclear Medicine & Medical Imaging GA 896AR UT WOS:000300538300007 PM 22077339 ER PT J AU Pucci, S Poletto, G Sterling, AC Romoli, M AF Pucci, Stefano Poletto, Giannina Sterling, Alphonse C. Romoli, Marco TI SOLAR POLAR X-RAY JETS AND MULTIPLE BRIGHT POINTS: EVIDENCE FOR SYMPATHETIC ACTIVITY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: activity; Sun: corona ID IMAGING SPECTROMETER; CORONAL HOLES; TELESCOPE; HINODE AB We present an analysis of X-ray bright points (BPs) and X-ray jets observed by Hinode/X-Ray Telescope on 2007 November 2-4, within the solar northern polar coronal hole. After selecting small subregions that include several BPs, we followed their brightness evolution over a time interval of a few hours, when several jets were observed. We find that most of the jets occurred in close temporal association with brightness maxima in multiple BPs: more precisely, most jets are closely correlated with the brightening of at least two BPs. We suggest that the jets result from magnetic connectivity changes that also induce the BP variability. We surmise that the jets and implied magnetic connectivity we describe are small-scale versions of the active-region-scale phenomenon, whereby flares and eruptions are triggered by interacting bipoles. C1 [Pucci, Stefano; Romoli, Marco] Univ Florence, Dept Phys & Astron, Florence, Italy. [Poletto, Giannina] INAF Arcetri Astrophys Observ, Florence, Italy. [Sterling, Alphonse C.] Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. RP Pucci, S (reprint author), Univ Florence, Dept Phys & Astron, Florence, Italy. EM stpucci@arcetri.astro.it RI Romoli, Marco/H-6859-2012 FU ASI [I/023/09/0]; NASA's Science Mission Directorate FX We thank R. Moore for useful discussions and the anonymous referee for his/her constructive comments to the Letter. S.P. and G.P. acknowledge support from ASI I/023/09/0. A.C.S. was supported by funding from NASA's Science Mission Directorate through the Solar Physics SR&T and the LWS TR&T programs. Hinode is a Japanese mission developed and launched by ISAS/JAXA, collaborating with NAOJ as a domestic partner, NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). NR 18 TC 3 Z9 3 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 1 PY 2012 VL 745 IS 2 AR L31 DI 10.1088/2041-8205/745/2/L31 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 891PJ UT WOS:000300228800016 ER PT J AU Rezgui, S Wilcox, EP Lee, P Carts, MA Label, K Nguyen, V Telecco, N McCollum, J AF Rezgui, Sana Wilcox, Edward P. Lee, Poongyeub Carts, Martin A. Label, Kenneth Victor Nguyen Telecco, Nicola McCollum, John TI Investigation of Low Dose Rate and Bias Conditions on the Total Dose Tolerance of a CMOS Flash-Based FPGA SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE Annealing; CMOS; floating gate devices; low-dose rate tests; reprogrammable flash-based FPGAs; TID ID GATE; MEMORIES AB TID test results of CMOS Flash-based FPGAs in gamma-rays are presented. The use of realistic low dose-rates and oriented bias-conditions are shown to extend the FPGA TID tolerance. Implications to qualification methods and to most of the new CMOS technologies are noted. C1 [Rezgui, Sana; Wilcox, Edward P.; Victor Nguyen; Telecco, Nicola; McCollum, John] Microsemi Corp, Mountain View, CA 94043 USA. [Wilcox, Edward P.] MEI Technol NASA GSFC, Greenbelt, MD 20771 USA. [Carts, Martin A.] Radiat Effects & Anal Grp, Greenbelt, MD 20771 USA. [Label, Kenneth] NASA GSFC, Greenbelt, MD 20771 USA. RP Rezgui, S (reprint author), Microsemi Corp, Mountain View, CA 94043 USA. EM sana.rezgui@microsemi.com; ted.wilcox@nasa.gov; poongyeub.lee@microsemi.com; martin.a.carts@nasa.gov; ken.label@nasa.gov; victor.nguyen@microsemi.com; nicola.telecco@microsemi.com; john.mc-collum@microsemi.com FU NASA EEE Parts and Packaging (NEPP) FX Manuscript received July 23, 2011; revised September 18, 2011, October 10, 2011, October 15, 2011, and November 25, 2011; accepted November 28, 2011. Date of publication January 31, 2012; date of current version February 10, 2012. This work was supported by NASA EEE Parts and Packaging (NEPP) Program. NR 16 TC 3 Z9 4 U1 1 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD FEB PY 2012 VL 59 IS 1 BP 134 EP 143 DI 10.1109/TNS.2011.2179316 PN 2 PG 10 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 894JN UT WOS:000300423100001 ER PT J AU Cho, MG Cooke, D Ferguson, D Garrett, HB Hilgers, A Lai, ST Roussel, JF Wheelock, A AF Cho, Mengu Cooke, David Ferguson, Dale Garrett, Henry B. Hilgers, Alain Lai, Shu T. Roussel, Jean-Francois Wheelock, Adrian TI Special Issue on Spacecraft Charging Technology 2012 SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Editorial Material C1 [Cho, Mengu] Kyushu Inst Technol, Kitakyushu, Fukuoka 8048550, Japan. [Cooke, David; Ferguson, Dale; Wheelock, Adrian] USAF, Res Lab, Albuquerque, NM 87117 USA. [Garrett, Henry B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hilgers, Alain] ESA, NL-2200 AG Noordwijk, Netherlands. [Lai, Shu T.] MIT, Space Prop Lab, Cambridge, MA 02139 USA. [Roussel, Jean-Francois] Off Natl Etud & Rech Aerosp, F-31055 Toulouse, France. RP Cho, MG (reprint author), Kyushu Inst Technol, Kitakyushu, Fukuoka 8048550, Japan. NR 0 TC 0 Z9 0 U1 1 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD FEB PY 2012 VL 40 IS 2 SI SI BP 138 EP 138 DI 10.1109/TPS.2011.2180452 PN 1 PG 1 WC Physics, Fluids & Plasmas SC Physics GA 894LS UT WOS:000300428800001 ER PT J AU Garrett, HB Katz, I Jun, I Kim, W Whittlesey, AC Evans, RW AF Garrett, Henry. B. Katz, Ira Jun, Insoo Kim, Wousik Whittlesey, Albert C. Evans, Robin W. TI The Jovian Charging Environment and Its Effects-A Review SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Review DE Aurora; internal electrostatic discharge (IESD); Jupiter; space plasma; spacecraft charging; vxB ID JUPITER AB Several space missions are being considered for Jupiter. These range from the recently launched Juno mission to possible joint NASA and ESA missions to Europa and Ganymede. Although the direct effects of radiation dose are normally considered the most pressing design issue for these missions, spacecraft charging, through surface charging, vxB, and, more importantly, internal charging, is also a key design concern. This paper reviews the current state of understanding of the jovian charging environment including the background plasma, high-energy electrons, and magnetic field. In conjunction with these environments, we will also review the range of effects to be expected in response to these environments. These effects need to be carefully considered in parallel with radiation effects in the design of the planned missions if they are to survive in the extremely challenging jovian environment. C1 [Garrett, Henry. B.; Katz, Ira; Jun, Insoo; Kim, Wousik; Whittlesey, Albert C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Evans, Robin W.] Mori Associates, Montrose, CA 91020 USA. RP Garrett, HB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM henry.b.garrett@jpl.nasa.gov; ira.katz@jpl.nasa.gov; insoo.jun@jpl.nasa.gov; wousik.kim@jpl.nasa.gov; albert.whittlesey@jpl.nasa.gov; robin.w.evans@jpl.nasa.gov FU National Aeronautics and Space Administration FX Copyright 2011. All rights reserved. We would like to acknowledge our many colleagues who have contributed to this effort. Of particular note are our two colleagues Drs. Robb Frederickson and N. J. Stevens who made fundamental contributions to our field. Their loss is greatly regretted. The research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 20 TC 2 Z9 2 U1 0 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 EI 1939-9375 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD FEB PY 2012 VL 40 IS 2 SI SI BP 144 EP 154 DI 10.1109/TPS.2011.2171369 PN 1 PG 11 WC Physics, Fluids & Plasmas SC Physics GA 894LS UT WOS:000300428800003 ER PT J AU Mandell, MJ Davis, VA Davis, GT Maurer, RH Herrmann, C AF Mandell, Myron J. Davis, V. A. Davis, G. T. Maurer, R. H. Herrmann, C. TI Photoemission Driven Charging in Tenuous Plasma SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Article DE Photoemission; spacecraft charging ID LONG-TERM; SPACECRAFT; SURFACE; PROBE; DENSITY; CLUSTER; PLATE AB In the cold, tenuous plasma commonly encountered in magnetospheric and interplanetary orbits, and in the case of scientific satellites with nearly all surfaces effectively conducting, surface charging is driven by photoemission current. The differential potential of the few insulating surfaces, such as lenses or insulating grout between solar cells, can be positive or negative depending on the photoemissivity of the material. We analyze this effect for spacecraft like those of the Magnetospheric MultiScale and the Radiation Belt Storm Probes missions. This paper develops a simple theory for the potentials of sunlit insulators, focusing on insulators that make up a small part of a large conductive surface. The shape of the photoemission spectrum places an absolute limit of about 12 V of positive differential charging on sunlit insulators. For small insulating surfaces, the conventional assumption-that the photoelectronsthat cannot energetically escape return to their surface of origin-is not valid because the photoelectron trajectory path length is large compared with the surface dimension. We describe a theory that accounts for photoelectron transport between small insulators and the surrounding conductive area. These calculations are done both for the case that the insulator has photoemission similar to the conductive area and for the case that the photoemission is far less, as is the case for many insulators. If the insulator has photoemission current density similar to that of a conductor, we predict positive differential potentials of about 2 V at low chassis potential and negligible differential at high chassis potential. In the opposite case that the insulator photoemission is low, we predict no differential at low chassis potentials and negative differential potentials of up to several volts at high chassis potential. C1 [Mandell, Myron J.; Davis, V. A.] Sci Applicat Int Corp, San Diego, CA 92121 USA. [Davis, G. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Maurer, R. H.; Herrmann, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Mandell, MJ (reprint author), Sci Applicat Int Corp, San Diego, CA 92121 USA. EM Myron.j.mandell@saic.com; victoria.a.davis@saic.com; victoria.a.davis@saic.com; Richard.Maurer@jhuapl.edu; Carl.Herrman@jhuapl.edu RI NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 FU Johns Hopkins University Applied Physics Laboratory; ADNET Systems, Inc. FX This research was carried out under contracts with the Johns Hopkins University Applied Physics Laboratory and ADNET Systems, Inc. NR 19 TC 2 Z9 2 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD FEB PY 2012 VL 40 IS 2 SI SI BP 209 EP 216 DI 10.1109/TPS.2011.2179675 PN 1 PG 8 WC Physics, Fluids & Plasmas SC Physics GA 894LS UT WOS:000300428800010 ER PT J AU Davis, VA Mandell, MJ Baker, NR Brown-Hayes, M Davis, GT Maurer, RH Herrmann, C AF Davis, V. A. Mandell, M. J. Baker, N. R. Brown-Hayes, M. Davis, G. T. Maurer, R. H. Herrmann, C. TI Surface-Charging Analysis of the Radiation Belt Storm Probe and Magnetospheric MultiScale Spacecraft SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Article DE Aeorspace simulation; electric field measurements; plasma measurements; spacecraft charging; space environment effects; space-plasma environment; space plasma interactions ID GEOSYNCHRONOUS ORBIT AB The Radiation Belt Storm Probes (RBSPs) are a pair of satellites to be launched in 2012 into 500 x 30 600 km 10 degrees-inclination orbits. The Magnetospheric MultiScale (MMS) mission spacecraft are a set of four satellites to be launched in 2014 into 1300 x 70 000 km (1.2 x 12 Re) 28 degrees-inclination orbits. The apogee will be boosted to 150 000 km (25 Re) during the mission. The spacecraft of both missions will measure magnetic and electric fields and the charged-particle distribution. As measurements of low-energy plasma and of electric fields are sensitive to surface potentials, stringent requirements for electrostatic cleanliness are imposed on both spacecraft designs. We present a surface-charging analysis of the RBSP and MMS spacecraft designs. The resulting chassis and differential potentials are used to estimate spacecraft-generated effects on the measurements and the risk of arcing. C1 [Davis, V. A.; Mandell, M. J.; Baker, N. R.; Brown-Hayes, M.] Sci Applicat Int Corp, San Diego, CA 92121 USA. [Davis, G. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Maurer, R. H.; Herrmann, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Davis, VA (reprint author), Sci Applicat Int Corp, San Diego, CA 92121 USA. RI NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 FU Johns Hopkins University Applied Physics Laboratory; ADNET Systems, Inc. FX This research was carried out under contracts with the Johns Hopkins University Applied Physics Laboratory and ADNET Systems, Inc. NR 17 TC 5 Z9 6 U1 0 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD FEB PY 2012 VL 40 IS 2 SI SI BP 262 EP 273 DI 10.1109/TPS.2011.2178615 PN 1 PG 12 WC Physics, Fluids & Plasmas SC Physics GA 894LS UT WOS:000300428800016 ER PT J AU Charro, M Sanmartin, JR Bombardelli, C Sanchez-Torres, A Lorenzini, EC Garrett, HB Evans, RW AF Charro, Mario Sanmartin, Juan R. Bombardelli, Claudio Sanchez-Torres, Antonio Lorenzini, Enrico C. Garrett, Henry B. Evans, Robin W. TI A Proposed Two-Stage Two-Tether Scientific Mission at Jupiter SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Article DE Bare tether; plasma applications; power generation ID ELECTRODYNAMIC TETHER; ENVIRONMENT; CONSTRAINTS AB A two-stage mission to place a spacecraft (SC) below the Jovian radiation belts, using a spinning bare tether with plasma contactors at both ends to provide propulsion and power, is proposed. Capture by Lorentz drag on the tether, at the periapsis of a barely hyperbolic equatorial orbit, is followed by a sequence of orbits at near-constant periapsis, drag finally bringing the SC down to a circular orbit below the halo ring. Although increasing both tether heating and bowing, retrograde motion can substantially reduce accumulated dose as compared with prograde motion, at equal tether-to-SC mass ratio. In the second stage, the tether is cut to a segment one order of magnitude smaller, with a single plasma contactor, making the SC to slowly spiral inward over several months while generating large onboard power, which would allow multiple scientific applications, including in situ study of Jovian grains, auroral sounding of upper atmosphere, and space-and time-resolved observations of surface and subsurface. C1 [Charro, Mario; Sanmartin, Juan R.; Bombardelli, Claudio; Sanchez-Torres, Antonio] Univ Politecn Madrid, E-28040 Madrid, Spain. [Lorenzini, Enrico C.] Univ Padua, I-35122 Padua, Italy. [Garrett, Henry B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Evans, Robin W.] Mori Associates, Rockville, MD 20852 USA. RP Charro, M (reprint author), Univ Politecn Madrid, E-28040 Madrid, Spain. EM mario.charro@upm.es; juanr.sanmartin@upm.es; claudio.bombardelli@upm.es; antonio.sanchezt@upm.es; enrico.lorenzini@unipd.it; henry.b.garrett@jpl.nasa.gov; robin.w.evans@jpl.nasa.gov RI Sanchez-Torres, Antonio/P-6978-2015 OI Sanchez-Torres, Antonio/0000-0001-5110-5724 FU Spanish Ministerio de Ciencia y Tecnologia [AYA2008-04769]; National Aeronautics and Space Administration FX Manuscript received March 15, 2011; revised August 2, 2011; accepted September 26, 2011. Date of publication November 9, 2011; date of current version February 10, 2012. This work was supported by the Spanish Ministerio de Ciencia y Tecnologia under Grant AYA2008-04769.; The research described in this paper by H. B. Garrett was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 16 TC 6 Z9 6 U1 1 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD FEB PY 2012 VL 40 IS 2 SI SI BP 274 EP 281 DI 10.1109/TPS.2011.2172637 PN 1 PG 8 WC Physics, Fluids & Plasmas SC Physics GA 894LS UT WOS:000300428800017 ER PT J AU Hoang, B Wong, FK Corey, RL Gardiner, G Funderburk, VV Gahart, RL Wright, KH Schneider, TA Vaughn, JA AF Hoang, Bao Wong, Frankie K. Corey, Ronald L. Gardiner, George Funderburk, Victor V. Gahart, Richard L. Wright, Kenneth H., Jr. Schneider, Todd A. Vaughn, Jason A. TI Combined Space Environmental Exposure Test of Multijunction GaAs/Ge Solar Array Coupons SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Article DE Combined environmental space exposure; electrostatic discharge (ESD); multijunction GaAs/Ge solar array; spacecraft charging AB The purpose of this test program is to understand the changes and degradation of the space solar array panel components, including its electrostatic discharge (ESD) mitigation design features in their integrated form, after multiple years (up to 15) of simulated Earth geosynchronous (GEO) space environment. A set of multijunction GaAs/Ge solar array test coupons was subjected to five-year increments of combined environmental exposure tests. These tests consisted of the following: simulated ultraviolet (UV) radiation, ESD, electron/proton particle radiation, thermal cycling, and simulated ion thruster exposures. The solar radiation simulation was produced using a mercury-xenon lamp with wavelengths in the UV spectrum ranging from 230 to 400 nm. The ESD test was performed in the inverted-gradient mode using a low-energy electron (3-6 keV) beam exposure. The ESD test also included a simulated panel coverglass flashover for the primary arc event. The electron/proton radiation exposure included 1.0-MeV electrons, 100-keV electrons, and 40-keV protons. Thermal cycling included simulated transient Earth eclipse for satellites in geosynchronous orbit. With the increasing use of ion thruster engines on many satellites, the combined environmental exposure test also included ion thruster exposure to determine the impact on solar array performance, as well as the ion thruster interaction to ESD events. Before and after each increment of combined environmental exposures, the coupons underwent visual inspection using high power magnification and electrical tests that included characterization by large-area pulse solar simulator, dark I-V, insulation resistance, and electroluminescence. This paper discusses the test objective, test methodologies, and preliminary results after five and ten years of simulated combined environmental exposure tests. C1 [Hoang, Bao] Space Syst Loral, Solar Array Deployable Grp, Palo Alto, CA USA. [Wright, Kenneth H., Jr.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Schneider, Todd A.; Vaughn, Jason A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Gardiner, George] Space Syst Loral, Radiat Effects & ESD Anal & Tests, Motorola GED, Palo Alto, CA USA. [Gardiner, George] Space Syst Loral, Space Environm Dept, Palo Alto, CA USA. RP Hoang, B (reprint author), Space Syst Loral, Solar Array Deployable Grp, Palo Alto, CA USA. EM hoang.bao@ssd.loral.com; wong.frankie@ssd.loral.com; corey.ron@ssd.loral.com; gardiner.george@ssd.loral.com; funderburk.vic@ssd.loral.com; gahart.richard@ssd.loral.com; ken.wright@uah.edu; todd.schneider@nasa.gov; jason.a.vaughn@nasa.gov NR 8 TC 5 Z9 5 U1 0 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD FEB PY 2012 VL 40 IS 2 SI SI BP 324 EP 333 DI 10.1109/TPS.2011.2174161 PN 1 PG 10 WC Physics, Fluids & Plasmas SC Physics GA 894LS UT WOS:000300428800024 ER PT J AU Wright, KH Schneider, TA Vaughn, JA Hoang, B Funderburk, VV Wong, FK Gardiner, G AF Wright, Kenneth H., Jr. Schneider, Todd A. Vaughn, Jason A. Hoang, Bao Funderburk, Victor V. Wong, Frankie K. Gardiner, George TI Electrostatic Discharge Testing of Multijunction Solar Array Coupons After Combined Space Environmental Exposures SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Article DE Electrostatic discharges (ESDs); environmental testing; photovoltaic cell testing AB A set of multijunction GaAs/Ge solar array test coupons provided by Space Systems/Loral was subjected to a sequence of five-year increments of combined space environmental exposure tests. The test coupons capture an integrated design intended for use in a geosynchronous (GEO) space environment. A key component of this test campaign is performing electrostatic discharge (ESD) tests in the inverted gradient mode. The protocol of the ESD tests is based on the ISO standard for ESD testing on solar array panels [ISO-11221]. The test schematic in the ISO reference has been modified with Space System/Loral designed circuitry to better simulate the on-orbit operational conditions of its solar array design. Part of the modified circuitry is to simulate a solar array panel coverglass flashover discharge. All solar array coupons used in the test campaign consist of four cells constructed to form two strings. The ESD tests are performed at the beginning-of-life (BOL) and at each five-year environmental exposure point. The space environmental exposure sequence consists of ultraviolet radiation, electron/proton particle radiation, thermal cycling, and xenon ion thruster plume erosion. This paper discusses the coverglass flashover simulation, the ESD test setup, and the importance of the electrical test design in simulating the on-orbit operational conditions. Results from fifth-year testing are compared to the baseline ESD characteristics determined at the BOL condition. C1 [Wright, Kenneth H., Jr.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Schneider, Todd A.; Vaughn, Jason A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Hoang, Bao; Gardiner, George] Space Syst Loral, Solar Array Deployable Grp, Palo Alto, CA USA. [Wong, Frankie K.; Gardiner, George] Space Syst Loral, Space Environm Dept, Palo Alto, CA USA. [Gardiner, George] Space Syst Loral, Motorola GED, Radiat Effects & ESD Anal & Tests, Palo Alto, CA USA. RP Wright, KH (reprint author), Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. EM Ken.Wright@uah.edu; todd.a.schneider@nasa.gov; jason.a.vaughn@nasa.gov; Hoang.Bao@ssd.loral.com; funderbv@ssd.loral.com; Wong.Frankie@ssd.loral.com; Gardiner.George@ssd.loral.com FU NASA/Marshall Space Flight Center [SAA8-084200]; Space Systems/Loral; NASA; University of Alabama-Huntsville [NNM11AA01A] FX Manuscript received April 6, 2011; revised September 30, 2011; accepted October 23, 2011. Date of publication December 13, 2011; date of current version February 10, 2012. The work at the NASA/Marshall Space Flight Center is performed under Space Act Agreement (SAA8-084200) with Space Systems/Loral. The work of K. H. Wright was supported by NASA through a Cooperative Agreement with the University of Alabama-Huntsville (NNM11AA01A). NR 17 TC 11 Z9 12 U1 1 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 EI 1939-9375 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD FEB PY 2012 VL 40 IS 2 SI SI BP 334 EP 344 DI 10.1109/TPS.2011.2174447 PN 1 PG 11 WC Physics, Fluids & Plasmas SC Physics GA 894LS UT WOS:000300428800025 ER PT J AU Vayner, B Galofaro, JT AF Vayner, Boris Galofaro, Joel T. TI Inception and Prevention of Sustained Discharges on Solar Arrays SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Article DE Arc discharges; photovoltaic space power systems; plasma properties; solar power generation; vacuum arcs ID PLASMA; ARCS; ENVIRONMENT; TESTS; ORBIT AB Sustained arc between adjacent cells is certainly a catastrophic event that results in significant loss in the power delivered to spacecraft systems. In order to prevent this kind of discharges, the threshold magnitudes of voltage and current should be determined in ground tests and compared with respective operational parameters. It is necessary to demonstrate that the results of ground tests depend on solar array designs but do not depend on the simulated environment and the electrical circuitry arrangement. A thorough analysis of about 20 tests performed in different laboratories has been conducted in this work. Sustained arc current thresholds were established for a variety of solar array designs and confronted with well-known magnitudes for vacuum arcs. If both voltage and string current magnitudes exceed the threshold values, the gaps between adjacent strings can be filled in with insulating material (RTV). Comprehensive ground tests demonstrated a high efficiency of this method. However, the lifetime of modern spacecraft spans for 10-15 years, and aging of RTV due to space radiation and temperature variations may cause critical changes in insulator properties. Thus, it seems reasonable to prepare a sample with RTV-grouted gaps, to undergo it proton fluence and thermal cycling equivalent to a few years in the geosynchronous orbit, and to test the sample against sustained arc inception. This program was also realized in the test described in this paper. C1 [Vayner, Boris] Ohio Aerosp Inst, Cleveland, OH 44142 USA. [Galofaro, Joel T.] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA. RP Vayner, B (reprint author), Ohio Aerosp Inst, Cleveland, OH 44142 USA. EM Boris.V.Vayner@nasa.gov FU New Energy Development Organization (Japan) FX The authors would like to thank D. Scheiman for performing the photovoltaic tests. The authors would also like to thank New Energy Development Organization Grant (Japan) for providing the samples. NR 31 TC 4 Z9 4 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD FEB PY 2012 VL 40 IS 2 SI SI BP 388 EP 393 DI 10.1109/TPS.2011.2177480 PN 1 PG 6 WC Physics, Fluids & Plasmas SC Physics GA 894LS UT WOS:000300428800031 ER PT J AU Comiso, JC AF Comiso, Josefino C. TI Large Decadal Decline of the Arctic Multiyear Ice Cover SO JOURNAL OF CLIMATE LA English DT Article ID SEA-ICE; TEMPERATURE; OSCILLATION; OCEAN; AMPLIFICATION; VARIABILITY; TRENDS; WIND AB The perennial ice area was drastically reduced to 38% of its climatological average in 2007 but recovered slightly in 2008, 2009, and 2010 with the areas being 10%, 24%, and 11% higher than in 2007, respectively. However, trends in extent and area remained strongly negative at -12.2% and -13.5% decade(-1), respectively. The thick component of the perennial ice, called multiyear ice, as detected by satellite data during the winters of 1979-2011 was studied, and results reveal that the multiyear ice extent and area are declining at an even more rapid rate of -15.1% and -17.2% decade(-1), respectively, with a record low value in 2008 followed by higher values in 2009, 2010, and 2011. Such a high rate in the decline of the thick component of the Arctic ice cover means a reduction in the average ice thickness and an even more vulnerable perennial ice cover. The decline of the multiyear ice area from 2007 to 2008 was not as strong as that of the perennial ice area from 2006 to 2007, suggesting a strong role of second-year ice melt in the latter. The sea ice cover is shown to be strongly correlated with surface temperature, which is increasing at about 3 times the global average in the Arctic but appears weakly correlated with the Arctic Oscillation (AO), which controls the atmospheric circulation in the region. An 8-9-yr cycle is apparent in the multiyear ice record, which could explain, in part, the slight recovery in the last 3 yr. C1 NASA, Cryospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Comiso, JC (reprint author), NASA, Cryospher Sci Branch, Goddard Space Flight Ctr, Code 614-1, Greenbelt, MD 20771 USA. EM josefino.c.comiso@nasa.gov FU NASA FX The author is thankful to R. Gersten of RSI/SESDA-2 and L. Stock of SGT, Inc. for excellent programming and analysis support. This paper also benefitted substantially from the valuable comments and suggestions of two anonymous reviewers. This work was funded by NASA's Cryospheric Sciences Program. NR 50 TC 199 Z9 208 U1 15 U2 111 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD FEB PY 2012 VL 25 IS 4 BP 1176 EP 1193 DI 10.1175/JCLI-D-11-00113.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 894HU UT WOS:000300418500007 ER PT J AU Dynys, FW Berger, MH Sehirlioglu, A AF Dynys, Frederick W. Berger, Marie-Helene Sehirlioglu, Alp TI Thermoelectric Properties of Undoped and Doped (Ti0.75Sn0.25)O-2 SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY LA English DT Article ID TIO2-SNO2 SYSTEM; SOLID-SOLUTIONS; ELECTRICAL-PROPERTIES; SEEBECK COEFFICIENT; ALIOVALENT DOPANTS; DECOMPOSITION; TRANSPORT; POWER; PRECIPITATION; CERAMICS AB Thermoelectric properties of undoped and doped (Ti0.75Sn0.25)O-2 were investigated for high-temperature thermoelectric conversion application. Nano-composites were formed by annealing above 1000 degrees C. Outside the spinodal dome, ilmenite-type SnTiO3 precipitated from the rutile structure. Thermoelectric properties were measured in the temperature range from room temperature to 1000 degrees C. (Ti0.75Sn0.25)O-2 was doped with both acceptor and donor dopants. Both undoped and doped (Ti0.75Sn0.25)O-2 exhibit n-type electrical behavior independent of the type of the dopant. The electrical conductivity was enhanced three orders of magnitude by donor doping with Nb2O5 or Ta2O5; achieving a maximum of 546 S/m at 850 degrees C. The increase in electrical conductivity was accompanied by reduction of the absolute Seebeck coefficient. Seebeck coefficient reduction of -600 mu V/K was observed between undoped and 4% Ta2O5 doped samples. The solid solution and doping reduced the thermal conductivity to <4 W/mK, far below the parent materials TiO2 and SnO2. Lattice thermal conductivity decreased with increasing temperature, achieving 1.9 W/mK at 900 degrees C for 4% Ta2O5 doping. No further reduction in thermal conductivity was observed in annealed samples containing nano-sized SnTiO3 precipitates. Dimensionless figure of merit (ZT) attained was <0.1. C1 [Dynys, Frederick W.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Berger, Marie-Helene] MINES ParisTech, Ctr Mat, CNRS, UMR 7633, F-91003 Evry, France. [Sehirlioglu, Alp] Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA. RP Dynys, FW (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM frederick.w.dynys@nasa.gov RI Berger, Marie-Helene/B-9785-2013 NR 26 TC 8 Z9 8 U1 2 U2 65 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-7820 J9 J AM CERAM SOC JI J. Am. Ceram. Soc. PD FEB PY 2012 VL 95 IS 2 BP 619 EP 626 DI 10.1111/j.1551-2916.2011.04794.x PG 8 WC Materials Science, Ceramics SC Materials Science GA 884UA UT WOS:000299733100031 ER PT J AU Sato, Y Suzuki, K Iguchi, T Choi, IJ Kadowaki, H Nakajima, T AF Sato, Yousuke Suzuki, Kentaroh Iguchi, Takamichi Choi, In-Jin Kadowaki, Hiroyuki Nakajima, Teruyuki TI Characteristics of Correlation Statistics between Droplet Radius and Optical Thickness of Warm Clouds Simulated by a Three-Dimensional Regional-Scale Spectral Bin Microphysics Cloud Model SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID BOUNDARY-LAYER CLOUDS; MESOSCALE CELLULAR STRUCTURES; SOLAR-RADIATION MEASUREMENTS; SHALLOW CUMULUS CONVECTION; GENERAL-CIRCULATION MODEL; EFFECTIVE PARTICLE RADIUS; LARGE-EDDY SIMULATIONS; MARINE STRATOCUMULUS; FRACTIONAL CLOUDINESS; CONDENSATION NUCLEI AB Three-dimensional downscaling simulations using a spectral bin microphysics (SBM) model were conducted to investigate the effects of aerosol amount and dynamical stabilities of the atmosphere on the correlation statistics between cloud droplet effective radius (RE) and cloud optical thickness (COT) of warm clouds off the coast of California. The regeneration process of aerosols was implemented into the SBM and was found to be necessary for simulating the satellite-observed microphysical properties of warm clouds by the SBM model used in this study. The results showed that the aerosol amount changed the correlation statistics in a way that changes the cloud particle number concentration, whereas the inversion height of the boundary layer, which is related to the atmospheric stability and the cloud-top height, changed the correlation statistics in a way that changes the liquid water path. These results showed that the dominant mechanisms that control the correlation statistics are similar to those suggested by previous modeling studies based on two-dimensional idealized simulations. On the other hand, the present three-dimensional modeling was also able to simulate some realistic patterns of the correlation statistics, namely, mixtures of characteristic patterns and the "high-heeled" pattern as observed by satellite remote sensing. C1 [Sato, Yousuke; Nakajima, Teruyuki] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba 2778568, Japan. [Sato, Yousuke] Japan Soc Promot Sci, Chiyoda Ku, Tokyo, Japan. [Suzuki, Kentaroh] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Iguchi, Takamichi] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Iguchi, Takamichi] NASA, Goddard Space Flight Ctr, Lab Atmosphere, Greenbelt, MD 20771 USA. [Choi, In-Jin] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea. RP Sato, Y (reprint author), Univ Tokyo, Atmosphere & Ocean Res Inst, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778568, Japan. EM satoy@aori.u-tokyo.ac.jp RI Suzuki, Kentaroh/C-3624-2011; Nakajima, Teruyuki/H-2370-2013; Sato, Yousuke/C-5416-2016 OI Nakajima, Teruyuki/0000-0002-9042-504X; Sato, Yousuke/0000-0002-6857-3783 FU Initiative on Promotion of Supercomputing for Young Researchers, Supercomputing Division, Information Technology Center, The University of Tokyo; JAXA/GCOM-C; JAXA/EarthCARE; MEXT/VL for Climate System Diagnostics; MOE [A-1101]; NIES/GOSAT; MEXT/RECCA/SALSA; Korea Meteorological Administration [RACS 2010-1009]; [22-7893] FX This study is supported by Initiative on Promotion of Supercomputing for Young Researchers, Supercomputing Division, Information Technology Center, The University of Tokyo. A part of authors are supported by projects of JAXA/GCOM-C, JAXA/EarthCARE, MEXT/VL for Climate System Diagnostics, MOE/Global Environment Research Fund A-1101, NIES/GOSAT, and MEXT/RECCA/SALSA. Some authors are supported by Grant-in-Aid for JSPS Fellows 22-7893. One of the authors is supported by the Korea Meteorological Administration Research and Development Program under Grant RACS 2010-1009. We are very grateful to Jorgen. B. Jensen of the National Center for Atmospheric Research/Earth Observation Factory for his valuable comment on an earlier version of this paper. NR 63 TC 3 Z9 3 U1 1 U2 15 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD FEB PY 2012 VL 69 IS 2 BP 484 EP 503 DI 10.1175/JAS-D-11-076.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 885SI UT WOS:000299800700005 ER PT J AU Loeb, NG Lyman, JM Johnson, GC Allan, RP Doelling, DR Wong, T Soden, BJ Stephens, GL AF Loeb, Norman G. Lyman, John M. Johnson, Gregory C. Allan, Richard P. Doelling, David R. Wong, Takmeng Soden, Brian J. Stephens, Graeme L. TI Observed changes in top-of-the-atmosphere radiation and upper-ocean heating consistent within uncertainty SO NATURE GEOSCIENCE LA English DT Article ID EARTHS ENERGY IMBALANCE; GLOBAL UPPER-OCEAN; SYSTEM; BUDGET; ERA AB Global climate change results from a small yet persistent imbalance between the amount of sunlight absorbed by Earth and the thermal radiation emitted back to space(1). An apparent inconsistency has been diagnosed between interannual variations in the net radiation imbalance inferred from satellite measurements and upper-ocean heating rate from in situ measurements, and this inconsistency has been interpreted as 'missing energy' in the system(2). Here we present a revised analysis of net radiation at the top of the atmosphere from satellite data, and we estimate ocean heat content, based on three independent sources. We find that the difference between the heat balance at the top of the atmosphere and upper-ocean heat content change is not statistically significant when accounting for observational uncertainties in ocean measurements(3), given transitions in instrumentation and sampling. Furthermore, variability in Earth's energy imbalance relating to El Nino-Southern Oscillation is found to be consistent within observational uncertainties among the satellite measurements, a reanalysis model simulation and one of the ocean heat content records. We combine satellite data with ocean measurements to depths of 1,800 m, and show that between January 2001 and December 2010, Earth has been steadily accumulating energy at a rate of 0.50 +/- 0.43 Wm(-2) (uncertainties at the 90% confidence level). We conclude that energy storage is continuing to increase in the sub-surface ocean. C1 [Loeb, Norman G.; Doelling, David R.; Wong, Takmeng] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Lyman, John M.] Univ Hawaii Manoa, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA. [Lyman, John M.; Johnson, Gregory C.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [Allan, Richard P.] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England. [Soden, Brian J.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Meteorol & Phys Oceanog, Miami, FL 33149 USA. [Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Loeb, NG (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd, Hampton, VA 23681 USA. EM norman.g.loeb@nasa.gov RI Allan, Richard/B-5782-2008; Johnson, Gregory/I-6559-2012 OI Allan, Richard/0000-0003-0264-9447; Johnson, Gregory/0000-0002-8023-4020 FU NASA Science Mission Directorate; US National Oceanic and Atmospheric Administration (NOAA) Climate Program Office; NOAA Research FX We thank the CERES science, algorithm, and data management teams and the NASA Science Mission Directorate for supporting this research. J.M.L. and G.C.J. were funded by the US National Oceanic and Atmospheric Administration (NOAA) Climate Program Office and NOAA Research. We thank S. Good at the UK Met Office for providing OHCA data from the Hadley Centre. NR 30 TC 123 Z9 128 U1 5 U2 63 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 J9 NAT GEOSCI JI Nat. Geosci. PD FEB PY 2012 VL 5 IS 2 BP 110 EP 113 DI 10.1038/NGEO1375 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 893ZU UT WOS:000300397300013 ER PT J AU Koren, I Altaratz, O Remer, LA Feingold, G Martins, JV Heiblum, RH AF Koren, Ilan Altaratz, Orit Remer, Lorraine A. Feingold, Graham Martins, J. Vanderlei Heiblum, Reuven H. TI Aerosol-induced intensification of rain from the tropics to the mid-latitudes SO NATURE GEOSCIENCE LA English DT Article ID PRECIPITATION; CLOUDS; INVIGORATION; POLLUTION; AMAZON; URBAN AB Atmospheric aerosols affect cloud properties, and thereby the radiation balance of the planet and the water cycle. However, the influence of aerosols on clouds, and in particular on precipitation, is far from understood(1), and seems to depend on factors such as location, season(2) and the spatiotemporal scale of the analysis. Here, we examine the relationship between aerosol abundance and rain rate-a key factor in climate and hydrological processes-using rain data from a satellite-based instrument sensitive to stronger rain rates (Tropical Rainfall Measuring Mission(3), TRMM), aerosol and cloud property data from the Moderate Resolution Imaging Spectroradiometer onboard the Aqua satellite(4,5) and meteorological information from the Global Data Assimilation System(6). We show that for a range of conditions, increases in aerosol abundance are associated with the local intensification of rain rates detected by the TRMM. The relationship is apparent over both the ocean and land, and in the tropics, subtropics and mid-latitudes. Further work is needed to determine how aerosols influence weaker rain rates, not picked up in the analysis. We also find that increases in aerosol levels are associated with a rise in cloud-top height. We suggest that the invigoration of clouds and the intensification of rain rates is a preferred response to an increase in aerosol concentration. C1 [Koren, Ilan; Altaratz, Orit; Heiblum, Reuven H.] Weizmann Inst Sci, Dept Environm Sci, IL-76100 Rehovot, Israel. [Remer, Lorraine A.] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Feingold, Graham] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA. [Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, NASA, JCET,GSFC, Baltimore, MD 21250 USA. RP Koren, I (reprint author), Weizmann Inst Sci, Dept Environm Sci, IL-76100 Rehovot, Israel. EM ilan.koren@weizmann.ac.il RI Feingold, Graham/B-6152-2009; Koren, Ilan/K-1417-2012; Manager, CSD Publications/B-2789-2015 OI Koren, Ilan/0000-0001-6759-6265; FU Israel Science Foundation [1172/10]; Minerva Foundation [780048]; NOAA FX This work was supported in part by the Israel Science Foundation (grant # 1172/10) and the Minerva Foundation (780048). G.F. acknowledges support from NOAA's Climate Goal Program. NR 30 TC 70 Z9 71 U1 3 U2 50 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 J9 NAT GEOSCI JI Nat. Geosci. PD FEB PY 2012 VL 5 IS 2 BP 118 EP 122 DI 10.1038/NGEO1364 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 893ZU UT WOS:000300397300015 ER PT J AU Winter, JM Eltahir, EAB AF Winter, Jonathan M. Eltahir, Elfatih A. B. TI Modeling the hydroclimatology of the midwestern United States. Part 1: current climate SO CLIMATE DYNAMICS LA English DT Article DE Hydrology; Regional climate modeling; Midwestern United States ID CONVECTIVE PARAMETERIZATION; FUTURE CLIMATE; REGCM3; WATER; PRECIPITATION; SENSITIVITY; SIMULATION; REPRESENTATION; VARIABILITY; PREDICTION AB An ensemble of six 22-year numerical experiments was conducted to evaluate the ability of Regional Climate Model version 3 (RegCM3) to simulate the energy and water budgets of the midwestern United States. RegCM3 was run using two surface physics schemes: Integrated Biosphere Simulator (IBIS) and Biosphere-Atmosphere Transfer Scheme 1e (BATS1e), and two convective closure assumptions: Fritsch & Chappell (FC80) and Arakawa & Schubert (AS74). Boundary conditions were provided by the National Centers for Environmental Prediction-Department of Energy Reanalysis 2 dataset and the ECHAM5 general circulation model. A companion paper examines the American Midwest under future climate scenarios. Overall, the model that reproduces the observed seasonal cycles of the midwestern United States climate system best is RegCM3 using IBIS and the AS74 convective closure assumption. IBIS simulates shortwave radiation more accurately, while BATS1e simulates longwave radiation more accurately. Summer two-meter air temperature is overestimated by the combination of IBIS and the FC80 convective closure assumption. All models contain a wet bias and overestimate evapotranspiration during the spring. Total runoff, surface runoff, groundwater runoff, and root zone soil moisture are best simulated by RegCM3 using IBIS and the AS74 convective closure assumption. While BATS1e does capture the seasonal cycle of total runoff, gross errors in the partitioning of total runoff between surface runoff and groundwater runoff exist. The seasonal cycle of root zone soil moisture simulated by RegCM3 using IBIS and the AS74 convective closure assumption is dry, but agrees with observations during the summer. The rest of the models underestimate root zone soil moisture. C1 [Winter, Jonathan M.; Eltahir, Elfatih A. B.] MIT, Cambridge, MA 02139 USA. RP Winter, JM (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM jwinter@mit.edu FU National Science Foundation [EAR-04500341]; Martin Family Fellowship FX We thank the International Centre for Theoretical Physics, the Eltahir group, members of the Ralph M. Parsons Laboratory who aided in this research, our reviewers, and our editor. Individuals who made significant contributions to this work include Jeremy Pal and Marc Marcella. This work was funded by the National Science Foundation (Award EAR-04500341) and the Martin Family Fellowship. NR 37 TC 6 Z9 6 U1 0 U2 9 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 FEB PY 2012 VL 38 IS 3-4 BP 573 EP 593 DI 10.1007/s00382-011-1182-2 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 887BE UT WOS:000299899300009 ER PT J AU Winter, JM Eltahir, EAB AF Winter, Jonathan M. Eltahir, Elfatih A. B. TI Modeling the hydroclimatology of the midwestern United States. Part 2: future climate SO CLIMATE DYNAMICS LA English DT Article DE Hydrology; Regional climate modeling; Climate change; Soil moisture; Midwestern United States ID SUMMER DRYNESS AB An ensemble of six 22-year numerical experiments was conducted to quantify the response of soil moisture to multiple climate change scenarios over the American Midwest. Regional Climate Model version 3 (RegCM3) was run using two surface physics schemes: Integrated Biosphere Simulator (IBIS) and Biosphere-Atmosphere Transfer Scheme 1e (BATS1e); and two convective closure assumptions: Fritsch and Chappell and Arakawa and Schubert. Experiments were forced with a surrogate climate change scenario constructed using the National Centers for Environmental Prediction-Department of Energy Reanalysis 2 dataset and the ECHAM5 A1B climate change scenario. RegCM3-IBIS and RegCM3-BATS1e simulate increased two-meter air temperature and downward longwave radiation throughout the year under both climate change scenarios. While differences in shortwave radiation are relatively small; some model configurations and climate change scenarios produce additional precipitation, evapotranspiration, and total runoff during the spring and summer. Soil moisture is unchanged or increased throughout the growing season as enhanced rainfall offsets greater evaporative demand. Negligible drying in root zone soil moisture is found in all climate change experiments conducted, regardless of surface physics scheme, boundary conditions, or convective closure assumption. C1 [Winter, Jonathan M.; Eltahir, Elfatih A. B.] MIT, Cambridge, MA 02139 USA. RP Winter, JM (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM jwinter@mit.edu FU National Science Foundation [EAR-04500341]; Martin Family Fellowship FX We thank the International Centre for Theoretical Physics, the Eltahir group, members of the Ralph M. Parsons Laboratory who aided in this research, our reviewers, and our editor. Individuals who made significant contributions to this work include Jeremy Pal and Marc Marcella. This work was funded by the National Science Foundation (Award EAR-04500341) and the Martin Family Fellowship. NR 25 TC 4 Z9 4 U1 1 U2 10 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 FEB PY 2012 VL 38 IS 3-4 BP 595 EP 611 DI 10.1007/s00382-011-1183-1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 887BE UT WOS:000299899300010 ER PT J AU Garcia, DB Forman, R Shindo, D AF Garcia, D. B. Forman, R. Shindo, D. TI Experimental evaluation of fatigue crack initiation from corroded hemispherical notches in aerospace structural materials SO FATIGUE & FRACTURE OF ENGINEERING MATERIALS & STRUCTURES LA English DT Article DE aluminium 7075-T7351; D6AC steel; fatigue; corrosion pit; initiation; residual stress ID ALUMINUM-ALLOY; PITTING CORROSION; RESIDUAL-STRESS; LIFE; PROPAGATION; GROWTH; STEEL; LIVES AB A test program was developed and executed to evaluate the influence of corroded hemispherical notches on the fatigue crack initiation process in aluminium 7075-T7351, 4340 steel and D6AC steel. Surface enhancements such as shot peening and laser shock peening were also incorporated as part of the test effort with the intent of assessing any improvements in fatigue performance. The aluminium specimens exhibited a relative insensitivity to the surface enhancements for crack initiation in pits ranging from 0.3 to 2.0 mm, and localized yielding was only a factor for smaller pits operated at an elevated load ratio. Residual stresses created by the surface enhancements as well as localized yielding improved the crack initiation behavior from the base of the pits for both the 4340 and D6AC steel specimens. This behaviour was evident at high and low load ratios. In particular, laser shock peening induced residual stresses produced a significant increase in the crack initiation stress even when localized yielding was not a factor. C1 [Garcia, D. B.] SAIC, Houston, TX 77058 USA. [Forman, R.; Shindo, D.] NASA, JSC, Houston, TX 77058 USA. RP Garcia, DB (reprint author), SAIC, 2450 NASA Pkwy, Houston, TX 77058 USA. EM garciadb1004@hotmail.com FU Department of Transportation/Federal Aviation Administration [DTFACT-08-X-00004]; National Aeronautics and Space Administration [DTFACT-08-X-00004] FX The authors thank the support of Traci Stadtmueller, John Bakuckas, Ph.D. and Cu Nguyen from the FAA William J. Hughes Technical Center. This work was sponsored under the Interagency Agreement, DTFACT-08-X-00004, between the Department of Transportation/Federal Aviation Administration and the National Aeronautics and Space Administration. NR 27 TC 1 Z9 2 U1 1 U2 29 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 8756-758X J9 FATIGUE FRACT ENG M JI Fatigue Fract. Eng. Mater. Struct. PD FEB PY 2012 VL 35 IS 2 BP 122 EP 140 DI 10.1111/j.1460-2695.2011.01599.x PG 19 WC Engineering, Mechanical; Materials Science, Multidisciplinary SC Engineering; Materials Science GA 889CH UT WOS:000300050600004 ER PT J AU Pounder, NL Hogan, RJ Varnai, T Battaglia, A Cahalan, RF AF Pounder, Nicola L. Hogan, Robin J. Varnai, Tamas Battaglia, Alessandro Cahalan, Robert F. TI A Variational Method to Retrieve the Extinction Profile in Liquid Clouds Using Multiple-Field-of-View Lidar SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID GREEN-FUNCTION; PART II; SCATTERING; RADAR; THICKNESS; RETURNS; STORAGE; SCHEME; WATER AB Liquid clouds play a profound role in the global radiation budget, but it is difficult to retrieve their vertical profile remotely. Ordinary narrow-field-of-view (FOV) lidars receive a strong return from such clouds, but the information is limited to the first few optical depths. Wide-angle multiple-FOV lidars can isolate radiation that is scattered multiple times before returning to the instrument, often penetrating much deeper into the cloud than does the single-scattered signal. These returns potentially contain information on the vertical profile of the extinction coefficient but are challenging to interpret because of the lack of a fast radiative transfer model for simulating them. This paper describes a variational algorithm that incorporates a fast forward model that is based on the time-dependent two-stream approximation, and its adjoint. Application of the algorithm to simulated data from a hypothetical airborne three-FOV lidar with a maximum footprint width of 600 m suggests that this approach should be able to retrieve the extinction structure down to an optical depth of around 6 and a total optical depth up to at least 35, depending on the maximum lidar FOV. The convergence behavior of Gauss-Newton and quasi-Newton optimization schemes are compared. Results are then presented from an application of the algorithm to observations of stratocumulus by the eight-FOV airborne Cloud Thickness from Off-Beam Lidar Returns (THOR) lidar. It is demonstrated how the averaging kernel can be used to diagnose the effective vertical resolution of the retrieved profile and, therefore, the depth to which information on the vertical structure can be recovered. This work enables more rigorous exploitation of returns from spaceborne lidar and radar that are subject to multiple scattering than was previously possible. C1 [Pounder, Nicola L.; Hogan, Robin J.] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England. [Varnai, Tamas] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Battaglia, Alessandro] Univ Leicester, Dept Phys & Astron, Earth Observat Sci, Leicester LE1 7RH, Leics, England. [Cahalan, Robert F.] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA. RP Pounder, NL (reprint author), Univ Reading, Dept Meteorol, Earley Gate,POB 243, Reading RG6 6BB, Berks, England. EM n.l.pounder@reading.ac.uk RI Cahalan, Robert/E-3462-2012; Hogan, Robin/M-6549-2016; OI Cahalan, Robert/0000-0001-9724-1270; Hogan, Robin/0000-0002-3180-5157; Battaglia, Alessandro/0000-0001-9243-3484 FU NERC's National Centre for Atmospheric Science [NE/H003894/1]; European Space Agency [22442/09/NL/CT] FX This work benefited from the support of NERC's National Centre for Atmospheric Science (Grant NE/H003894/1) and the European Space Agency (Contract 22442/09/NL/CT). Marta Janiskova and Dong Huang are thanked for useful discussions on adjoint coding and L-curve analysis, respectively. NR 35 TC 6 Z9 6 U1 0 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD FEB PY 2012 VL 51 IS 2 BP 350 EP 365 DI 10.1175/JAMC-D-10-05007.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 889JQ UT WOS:000300070400011 ER PT J AU Leinonen, J Moisseev, D Leskinen, M Petersen, WA AF Leinonen, Jussi Moisseev, Dmitri Leskinen, Matti Petersen, Walter A. TI A Climatology of Disdrometer Measurements of Rainfall in Finland over Five Years with Implications for Global Radar Observations SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID RAINDROP SIZE DISTRIBUTION; POLARIMETRIC RADAR; DISTRIBUTION PARAMETERS; DIFFERENTIAL REFLECTIVITY; POLARIZATION RADAR; DUAL-WAVELENGTH; DOPPLER RADAR; PHASE-SHIFT; DISTRIBUTIONS; MODEL AB To improve the understanding of high-latitude rain microphysics and its implications for the remote sensing of rainfall by ground-based and spaceborne radars, raindrop size measurements have been analyzed that were collected over five years with a Joss-Waldvogel disdrometer located in Jarvenpaa, Finland. The analysis shows that the regional climate is characterized by light rain and small drop size with narrow size distributions and that the mutual relations of drop size distribution parameters differ from those reported at lower latitudes. Radar parameters computed from the distributions demonstrate that the high latitudes are a challenging target for weather radar observations, particularly those employing polarimetric and dual-frequency techniques. Nevertheless, the findings imply that polarimetric ground radars can produce reliable "ground truth" estimates for space observations and identify dual-frequency radars utilizing a W-band channel as promising tools for observing rainfall in the high-latitude climate. C1 [Leinonen, Jussi] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Leinonen, Jussi] Aalto Univ, Dept Appl Phys, Espoo, Finland. [Moisseev, Dmitri; Leskinen, Matti] Univ Helsinki, Dept Phys, Helsinki, Finland. [Petersen, Walter A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Leinonen, J (reprint author), Finnish Meteorol Inst, POB 503, FIN-00101 Helsinki, Finland. EM jussi.leinonen@fmi.fi RI Moisseev, Dmitri/A-3288-2008; Measurement, Global/C-4698-2015; OI Moisseev, Dmitri/0000-0002-4575-0409; Leinonen, Jussi/0000-0002-6560-6316 FU Academy of Finland GPM [128255, 128328]; NASA FX This work was supported by the Academy of Finland GPM Grants 128255 and 128328. Walter A. Petersen acknowledges funding from both the NASA PMM Science Program (Dr. R. Kakar) and the NASA GPM Mission (Drs. A. Hou and M. Schwaller). Jussi Leinonen thanks Dr. V. N. Bringi for valuable discussions about the analysis. NR 43 TC 15 Z9 15 U1 0 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD FEB PY 2012 VL 51 IS 2 BP 392 EP 404 DI 10.1175/JAMC-D-11-056.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 889JQ UT WOS:000300070400014 ER PT J AU Lau, WKM Zhou, YP AF Lau, William K. M. Zhou, Y. P. TI Observed recent trends in tropical cyclone rainfall over the North Atlantic and the North Pacific SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SEA-SURFACE TEMPERATURE; UNITED-STATES; CLIMATOLOGICAL RAINFALL; GLOBAL PRECIPITATION; INTENSITY; CLIMATE; MODEL; SENSITIVITY; PERSPECTIVE; REANALYSIS AB In this study, we use Tropical Rainfall Measurement Mission and Global Precipitation Climatology Project rainfall data together with historical storm track records to examine the trend of tropical cyclone (TC) rainfall in the North Atlantic and the northeast and northwest Pacific during two recent decades (1988-1997 and 1998-2007). We find that there is an approximate linear relationship between TC rain (defined as accumulated total rainfall along storm tracks) and storm intensity as classified by the Saffir-Simpson scheme. During the data period, total TC rain has trended upward at a rate of 23.8% +/- 23.5% per decade over the North Atlantic but downward with a rate of 25.1% +/- 19.7% per decade over the northeast Pacific. Over the northwest Pacific, there is a reduction in TC rain of approximately 20.9% +/- 13.5% per decade, possibly associated with a strong interdecadal-scale oscillation. Storm characteristics such as duration and TC rain energy per storm (EPS) remain unchanged for the North Atlantic and the northeast Pacific. For the northwest Pacific, a 28% +/- 18% reduction in EPS from the first decade (1988-1997) to the second decade (1998-2007) is found with the track data from the Joint Typhoon Warning Center. Analyses of the probability distribution function of TC rain show that there is an overall increase in TC frequency across the entire TC rainfall spectrum over the North Atlantic but an overall decrease for the northeast Pacific. In the northwest Pacific, we find a redistribution in EPS with decreased frequency in heavy-rain storms and increased frequency in light-rain storms. Overall, trends in TC rain in the different ocean basins are consistent with long-term relative changes in the ambient large-scale sea surface temperature and vertical wind shear and, to a lesser extent, tropical cyclone Maximum Potential Intensity. C1 [Lau, William K. M.] NASA, Atmospheres Lab, Div Earth Sci, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zhou, Y. P.] Morgan State Univ, Greenbelt, MD USA. RP Lau, WKM (reprint author), NASA, Atmospheres Lab, Div Earth Sci, Goddard Space Flight Ctr, Code 610, Greenbelt, MD 20771 USA. EM william.k.lau@nasa.gov RI Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 FU Precipitation Measuring Mission, NASA Earth Science Division FX This work is supported by the Precipitation Measuring Mission (R. Kakar, Headquarters Manager), NASA Earth Science Division. The authors thank C. Landsea, M. Shepherd, and another anonymous reviewer for their critical comments on the earlier manuscript. NCEP Reanalysis data are obtained from the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from their Web site at http://www.esrl.noaa.gov/psd/. NR 51 TC 8 Z9 8 U1 2 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 1 PY 2012 VL 117 AR D03104 DI 10.1029/2011JD016510 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 887VQ UT WOS:000299959900005 ER PT J AU Wells, KC Martins, JV Remer, LA Kreidenweis, SM Stephens, GL AF Wells, Kelley C. Martins, J. Vanderlei Remer, Lorraine A. Kreidenweis, Sonia M. Stephens, Graeme L. TI Critical reflectance derived from MODIS: Application for the retrieval of aerosol absorption over desert regions SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SKY RADIANCE MEASUREMENTS; RADIATIVE-TRANSFER; OPTICAL-PROPERTIES; DUST; SCATTERING; SATELLITE; ALGORITHM; SENSITIVITY; ASSESSMENTS; NETWORK AB The determination of aerosol direct radiative forcing over desert regions requires accurate information about the aerosol single-scattering albedo (SSA); however, the brightness of desert surfaces in the visible and near-IR range complicates the retrieval of aerosol optical properties using passive space-based measurements. Here we use the critical reflectance method to retrieve spectral aerosol absorption from space over North Africa, a desert region that is predominantly impacted by absorbing dust and biomass burning aerosol. We examine the sensitivity of the critical reflectance parameter to aerosol physical and optical properties that are representative of the region, and we find that the critical reflectance has low sensitivity to assumptions of aerosol size and refractive index for dust-like particles, except at scattering angles near 180 degrees, which should be avoided with this method. We use our findings to retrieve spectral SSA from critical reflectance derived from Moderate Resolution Imaging Spectroradiometer (MODIS) reflectances in the vicinity of two Aerosol Robotic Network (AERONET) stations: Tamanrasset, in the Algerian Sahara, and Banizoumbou, in the Sahel. We retrieve lower aerosol SSAs at Banizoumbou, which is often impacted by dust-smoke mixtures, and higher SSAs at Tamanrasset, where pure desert dust is the dominant aerosol. Our results generally fall within the AERONET uncertainty envelopes, although at Banizoumbou we retrieve a spectral dependence different from that of AERONET. On the basis of our analysis, we expect to be able to retrieve SSA from critical reflectance for pure dust with an uncertainty of 0.02 and to provide spatial and spectral SSA information that will help reduce current uncertainties in the aerosol radiative forcing over desert regions. C1 [Wells, Kelley C.; Kreidenweis, Sonia M.; Stephens, Graeme L.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Remer, Lorraine A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wells, KC (reprint author), Univ Minnesota, Dept Soil Water & Climate, 439 Borlaug Hall,1991 Upper Buford Cir, St Paul, MN 55108 USA. EM kcw@umn.edu; martins@umbc.edu; Lorraine.a.remer@nasa.gov; sonia@atmos.colostate.edu; stephens@atmos.colostate.edu RI Kreidenweis, Sonia/E-5993-2011 OI Kreidenweis, Sonia/0000-0002-2561-2914 FU Center for Earth-Atmosphere Studies through NASA [NNX08AT77G]; NOAA [NA17RJ1228] FX This work was supported by the Center for Earth-Atmosphere Studies through NASA grant NNX08AT77G, with additional funding from NOAA grant NA17RJ1228. We thank Didier Tanre, Emilio Cuevas-Agullo, and Mohamed Mimouni for their efforts in establishing and maintaining the Banizoumbou and Tamanrasset AERONET sites, and we thank the MODIS team for their efforts in calibration and maintenance of the MODIS instrument and data. We would also like to thank Li Zhu, Tom Eck, Rob Levy, Shana Mattoo, and the anonymous reviewers for their helpful suggestions in developing and revising this work. NR 33 TC 3 Z9 3 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 1 PY 2012 VL 117 AR D03202 DI 10.1029/2011JD016891 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 887VQ UT WOS:000299959900009 ER PT J AU Burchill, JK Clemmons, JH Knudsen, DJ Larsen, M Nicolls, MJ Pfaff, RF Rowland, D Sangalli, L AF Burchill, J. K. Clemmons, J. H. Knudsen, D. J. Larsen, M. Nicolls, M. J. Pfaff, R. F. Rowland, D. Sangalli, L. TI High-latitude E region ionosphere-thermosphere coupling: A comparative study using in situ and incoherent scatter radar observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID NEUTRAL COLLISION FREQUENCY; CHAMP OBSERVATIONS; WAVES; PLASMA; DRAG; PARAMETERS; ATMOSPHERE; DENSITY; MODEL; WIND AB We present in situ and ground-based measurements of the ratio kappa of ion cyclotron angular frequency to ion-neutral momentum transfer collision frequency to investigate ionosphere-thermosphere (IT) coupling in the auroral E region. In situ observations were obtained by NASA sounding rocket 36.234, which was launched into the nightside E region ionosphere at 1229 UT on 19 January 2007 from Poker Flat, AK. The payload carried instrumentation to determine ion drift angle and electric field vectors. Neutral winds were measured by triangulating a chemical tracer released from rocket 41.064 launched two minutes later. kappa is calculated from the rotation of the ion drift angle relative to the E-cross-B drift direction in a frame co-rotating with the payload. Between the altitudes of 118 km and 130 km kappa increases exponentially with a scale height of 9.3 +/- 0.7 km, deviating from an exponential above 130 km. kappa = 1 at an altitude z(0) of 119.9 +/- 0.5 km. The ratio was also estimated from Poker Flat Incoherent Scatter Radar (PFISR) measurements using the rotation of ion velocity with altitude. Exponential fits to the PFISR measurements made during the flight of 41.064 yield z(0) = 115.9 +/- 1.2 km and a scale height of 9.1 +/- 1.0 km. Differences between in situ and ground-based measurements show that the E region atmospheric densities were structured vertically and/or horizontally on scales of 1 km to 10 km. There were no signs of ionospheric structure in ion density or ion temperature below scales of 1 km. The observations demonstrate the accuracy with which the in situ and PFISR data may be used as probes of IT coupling. C1 [Burchill, J. K.; Knudsen, D. J.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Clemmons, J. H.] Aerosp Corp, Space Sci Applicat Lab, El Segundo, CA 90245 USA. [Larsen, M.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Nicolls, M. J.] SRI Int, Ctr Geospace Studies, Menlo Pk, CA 94025 USA. [Pfaff, R. F.; Rowland, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sangalli, L.] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada. RP Burchill, JK (reprint author), Univ Calgary, Dept Phys & Astron, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada. EM burchill@phys.ucalgary.ca RI Rowland, Douglas/F-5589-2012; Larsen, Miguel/A-1079-2013; Pfaff, Robert/F-5703-2012; Nicolls, Michael/N-8680-2013; OI Rowland, Douglas/0000-0003-0948-6257; Pfaff, Robert/0000-0002-4881-9715; Nicolls, Michael/0000-0001-8267-6327; Clemmons, James/0000-0002-5298-5222 FU Canadian Space Agency; Natural Sciences and Engineering Research Council of Canada; NSF [ATM-0608577, ATM-0719808, AGS-1007539]; NASA [NNX07AJ99G] FX This research was supported by the Canadian Space Agency and the Natural Sciences and Engineering Research Council of Canada. Joule II SII development was supported by a contract from the Canadian Space Agency. The authors acknowledge the contributions and expertise of the SII development team, R. B. Hriskevich, J. T. Forshaw, R. M. Thomson, J. G. Aase, and E. P. King, and of the Joule II payload team at the NASA Wallops Flight Facility. PFISR data and collection and analysis was supported by NSF cooperative agreement ATM-0608577, and work at SRI International was supported by NSF grant ATM-0719808. MFL was partially supported under NASA grant NNX07AJ99G and NSF grant AGS-1007539. JKB appreciates valuable discussions with B. Jackel, R. Schunk and J.- P. St.-Maurice. NR 34 TC 5 Z9 6 U1 0 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 FEB 1 PY 2012 VL 117 AR A02301 DI 10.1029/2011JA017175 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 888FR UT WOS:000299989700002 ER PT J AU Vinukollu, RK Sheffield, J Wood, EF Bosilovich, MG Mocko, D AF Vinukollu, Raghuveer K. Sheffield, Justin Wood, Eric F. Bosilovich, Michael G. Mocko, David TI Multimodel Analysis of Energy and Water Fluxes: Intercomparisons between Operational Analyses, a Land Surface Model, and Remote Sensing SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID GENERAL-CIRCULATION MODELS; ASSIMILATION SYSTEM NLDAS; RIVER-BASIN; GLOBAL PRECIPITATION; ECMWF REANALYSIS; ETA-MODEL; RADIATION BUDGET; PART I; BALANCE; CEOP AB Using data from seven global model operational analyses (OA), one land surface model, and various remote sensing retrievals, the energy and water fluxes over global land areas are intercompared for 2003/04. Remote sensing estimates of evapotranspiration (ET) are obtained from three process-based models that use input forcings from multisensor satellites. An ensemble mean (linear average) of the seven operational (mean-OA) models is used primarily to intercompare the fluxes with comparisons performed at both global and basin scales. At the global scale, it is found that all components of the energy budget represented by the ensemble mean of the OA models have a significant bias. Net radiation estimates had a positive bias (global mean) of 234 MJ m(-2) yr(-1) (7.4 W m(-2)) as compared to the remote sensing estimates, with the latent and sensible heat fluxes biased by 470 MJ m(-2) yr(-1) (13.3 W m(-2)) and -367 MJ m(-2) yr(-1) (11.7 W m(-2)), respectively. The bias in the latent heat flux is affected by the bias in the net radiation, which is primarily due to the biases in the incoming shortwave and outgoing longwave radiation and to the nudging process of the operational models. The OA models also suffer from improper partitioning of the surface heat fluxes. Comparison of precipitation (P) analyses from the various OA models, gauge analysis, and remote sensing retrievals showed better agreement than the energy fluxes. Basin-scale comparisons were consistent with the global-scale results, with the results for the Amazon in particular showing disparities between OA and remote sensing estimates of energy fluxes. The biases in the fluxes are attributable to a combination of errors in the forcing from the OA atmospheric models and the flux calculation methods in their land surface schemes. The atmospheric forcing errors are mainly attributable to high shortwave radiation likely due to the underestimation of clouds, but also precipitation errors, especially in water-limited regions. C1 [Vinukollu, Raghuveer K.; Sheffield, Justin; Wood, Eric F.] Princeton Univ, CEE Dept, Princeton, NJ 08544 USA. [Vinukollu, Raghuveer K.] Swiss Re, Armonk, NY USA. [Bosilovich, Michael G.; Mocko, David] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Mocko, David] Sci Applicat Int Corp, Mclean, VA 22102 USA. RP Wood, EF (reprint author), Princeton Univ, CEE Dept, EQUAD Olden St, Princeton, NJ 08544 USA. EM efwood@princeton.edu RI Bosilovich, Michael/F-8175-2012; Houser, Paul/J-9515-2013 OI Houser, Paul/0000-0002-2991-0441 FU NASA [NNG04GQ32G, NNX08AN40A, NNX09AK35G] FX This work was jointly supported by NASA Grants NNG04GQ32G "A Terrestrial Evaporation Data Product Using MODIS Data," NNX08AN40A "Developing Consistent Earth System Data Records for the Global Terrestrial Water Cycle," and NNX09AK35G "Development and Diagnostic Analysis of a Multidecadal Global Evaporation Product." The operational model data for the current study were obtained from the authors of Bosilovich et al. (2009), which is part of the Coordinated Energy and Water Observation Project (CEOP, GEWEX), NASA Langley Research Center Atmospheric Science Data Center, Global Precipitation Climatology Center (GPCC), MEDIAS-France, and the Global River Discharge Center (GRDC). NR 80 TC 11 Z9 11 U1 0 U2 24 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2012 VL 13 IS 1 BP 3 EP 26 DI 10.1175/2011JHM1372.1 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 890IN UT WOS:000300138400001 ER PT J AU Kidd, C Bauer, P Turk, J Huffman, GJ Joyce, R Hsu, KL Braithwaite, D AF Kidd, C. Bauer, P. Turk, J. Huffman, G. J. Joyce, R. Hsu, K. -L. Braithwaite, D. TI Intercomparison of High-Resolution Precipitation Products over Northwest Europe SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID DIRECT 4D-VAR ASSIMILATION; MICROWAVE SOUNDING UNIT; GLOBAL PRECIPITATION; RAINFALL ESTIMATION; PASSIVE MICROWAVE; TROPICAL RAINFALL; PART I; SATELLITE; ALGORITHMS; RETRIEVAL AB Satellite-derived high-resolution precipitation products (HRPP) have been developed to address the needs of the user community and are now available with 0.25 degrees X 0.25 degrees (or less) subdaily resolutions. This paper evaluates a number of commonly available satellite-derived HRPPs covering northwest Europe over a 6-yr period. Precipitation products include the Tropical Rainfall Measuring Mission (TRMM) Multisatellite Precipitation Analysis (TMPA), the Climate Prediction Center (CPC) morphing (CMORPH) technique, the CPC merged microwave technique, the Naval Research Laboratory (NRL) blended technique, and the Precipitation Estimation from Remotely Sensed Information using Artificial Neural Networks (PERSIANN) technique. In addition, the Geosynchronous Operational Environmental Satellite (GOES) precipitation index (GPI) and the European Centre for Medium-Range Weather Forecasting (ECMWF) operational forecast model products are included for comparison. Surface reference data from the European radar network is used as ground truth, supported by the Global Precipitation Climatology Centre (GPCC) precipitation gauge analysis and gauge data over the United Kingdom. Measures of correlation, bias ratio, probability of detection, and false alarm ratio are used to evaluate the products. Results show that satellite products generally exhibit a seasonal cycle in correlation, bias ratio, probability of detection, and false alarm ratio, with poorer statistics during the winter. The ECMWF model also shows a seasonal cycle in the correlation, although the results are poorer during the summer, while the bias ratio, probability of detection, and false alarm ratio are consistent through all seasons. Importantly, all the satellite HRPPs underestimate precipitation over northwest Europe in all seasons. C1 [Kidd, C.; Huffman, G. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20706 USA. [Kidd, C.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Bauer, P.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. [Turk, J.] NASA, Jet Prop Lab, Pasadena, CA USA. [Huffman, G. J.] Sci Syst & Applicat Inc, Lanham, MD USA. [Joyce, R.] NOAA, Natl Ctr Environm Predict, Climate Predict Ctr, Camp Springs, MD USA. [Hsu, K. -L.; Braithwaite, D.] Univ Calif Irvine, Henry Samueli Sch Engn, Irvine, CA USA. RP Kidd, C (reprint author), NASA, Goddard Space Flight Ctr, Code 612-0, Greenbelt, MD 20706 USA. EM chris.kidd@nasa.gov RI Huffman, George/F-4494-2014; Kidd, Christopher/H-9910-2014 OI Huffman, George/0000-0003-3858-8308; NR 59 TC 56 Z9 57 U1 3 U2 42 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2012 VL 13 IS 1 BP 67 EP 83 DI 10.1175/JHM-D-11-042.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 890IN UT WOS:000300138400004 ER PT J AU Mahanama, S Livneh, B Koster, R Lettenmaier, D Reichle, R AF Mahanama, Sartih Livneh, Ben Koster, Randal Lettenmaier, Dennis Reichle, Rolf TI Soil Moisture, Snow, and Seasonal Streamflow Forecasts in the United States SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID LATITUDE HYDROLOGICAL PROCESSES; CATCHMENT-BASED APPROACH; LAND-SURFACE PROCESSES; MESOSCALE ETA-MODEL; TORNE-KALIX BASIN; WESTERN US; PILPS PHASE-2(E); RIVER-BASIN; PREDICTABILITY; SIMULATION AB Land surface model experiments are used to quantify, for a number of U.S. river basins, the contributions (isolated and combined) of soil moisture and snowpack initialization to the skill of seasonal streamflow forecasts at multiple leads and for different start dates. Snow initialization has a major impact on skill during the spring melting season. Soil moisture initialization has a smaller but still statistically significant impact during this season, and in other seasons, its contribution to skill dominates. Realistic soil moisture initialization can contribute to skill at long leads (over 6 months) for certain basins and seasons. Skill levels in all seasons are found to be related to the ratio of initial total water storage (soil water plus snow) variance to the forecast period precipitation variance, allowing estimates of the potential for skill in areas outside the verification basins. C1 [Mahanama, Sartih; Koster, Randal; Reichle, Rolf] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Mahanama, Sartih] Sci Applicat Int Corp, Beltsville, MD USA. [Livneh, Ben; Lettenmaier, Dennis] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA. RP Mahanama, S (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Mail Stop 610-1, Greenbelt, MD 20771 USA. EM sarith.p.mahanama@nasa.gov RI Reichle, Rolf/E-1419-2012; Koster, Randal/F-5881-2012; lettenmaier, dennis/F-8780-2011; Livneh, Ben/I-2939-2015; OI Koster, Randal/0000-0001-6418-6383; lettenmaier, dennis/0000-0003-3317-1327; LIVNEH, BEN/0000-0001-5445-2473 FU NASA FX We thank James Verdin for discussions at the onset of this study. We also thank the providers of the naturalized western streamflow data: U.S. Army Corps of Engineers, Omaha NB office, for the Missouri River basin; U.S. Army Corps of Engineers, Tulsa OK office, for the Arkansas Red River basin; Columbia River Basin Climate Change Scenarios Database for the Columbia River basin; California Data Exchange Commission for the California basins; and U.S. Bureau of Reclamation, Lower Colorado Region, for the Colorado River basin. We further thank Professor Edwin Maurer (Santa Clara University) for his assistance in obtaining naturalized streamflow data for the eastern and central U.S. river basins. Funding for much of this study was provided by NASA's Terrestrial Hydrology Program. NR 41 TC 47 Z9 47 U1 0 U2 23 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2012 VL 13 IS 1 BP 189 EP 203 DI 10.1175/JHM-D-11-046.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 890IN UT WOS:000300138400011 ER PT J AU Tokay, A Ozturk, K AF Tokay, Ali Ozturk, Kurtulus TI An Experimental Study of the Small-Scale Variability of Rainfall SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID TRMM PRECIPITATION RADAR; MEASURING MISSION TRMM; GROUND-VALIDATION; GAUGE MEASUREMENTS; STOCHASTIC-MODEL; FIELD CAMPAIGN; ERRORS; PRODUCTS AB Small-scale variability of rainfall has been studied employing six dual rain gauge sites at Wallops Island, Virginia. The rain gauge sites were separated between 0.4 and 5 km, matching the beamwidth of Tropical Rainfall Measuring Mission (TRMM) and Global Precipitation Measurement (GPM) precipitation radars. During a 2-yr observational period, over 7100 rainy samples were received at 5-min integration. A single gauge did not report as high as 67% of the time when at least one of the other gauges had rainfall in one of the seasons. Since rainfall from one of the six rain gauges is sufficient for the rainy footprint from a satellite, this demonstrates the common occurrence of the partial beamfilling. For the periods where all gauges were reporting rainfall, a single gauge had at most 13% difference from the areal average rainfall in one of the seasons. This suggests that at the spatial scale of 5 km, the variability caused by the rain gradient is relatively less important than the variability arising from a partially tilled footprint. During the passage of frontal systems and tropical cyclones, the beam was filled by rain most of the time and this resulted in relatively higher correlation distances. The correlation distance had a sharp drop off from 45 km in moderately variable rainfall to 3 km in highly variable rainfall and ranged from 5 to 35 km between the different seasons. This demonstrates its highly variable nature. Considering temporal sampling, the monthly rainfall error was 35% and 73% for 3-hourly and twice-daily observations, respectively. C1 [Tokay, Ali] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tokay, Ali] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Ozturk, Kurtulus] Turkish State Meteorol Serv, Ankara, Turkey. RP Tokay, A (reprint author), NASA, Goddard Space Flight Ctr, Code 613-1, Greenbelt, MD 20771 USA. EM ali.tokay-1@nasa.gov RI Measurement, Global/C-4698-2015 FU NASA [NNX07AF45G] FX We thank our senior technician, Paul G. Bashor of Computer Science Corporation, NASA Wallops Flight Facility for his dedicated work on operating the gauge network and reviewing this manuscript. Discussions with Prasun Kundu of the University of Maryland, Baltimore County; S. Joseph Munchak of the University of Maryland, College Park; and Robert Meneghini of NASA Goddard Space Flight Center were very helpful. Thanks to David A. Marks of Science Systems Applications Inc., and Amy J. Houghton of the University of Maryland, Baltimore County for the review. Special thanks to Drs. Emad Habib of the University of Louisiana at Lafayette, Gabriele Villarini of Princeton University, and an anonymous reviewer for their constructive reviews. This work has been conducted during the second author's visit to the NASA GSFC as a GEST fellow. This work is funded through NASA under Grant NNX07AF45G. NR 26 TC 11 Z9 11 U1 1 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2012 VL 13 IS 1 BP 351 EP 365 DI 10.1175/JHM-D-11-014.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 890IN UT WOS:000300138400022 ER PT J AU Lau, WKM Kim, KM AF Lau, William K. M. Kim, Kyu-Myong TI The 2010 Pakistan Flood and Russian Heat Wave: Teleconnection of Hydrometeorological Extremes SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID MID-TROPOSPHERIC CYCLONES; PRECIPITATION; MONSOON; SUMMER AB In this paper, preliminary results are presented showing that the two record-setting extreme events during 2010 summer (i.e., the Russian heat wave-wildfires and Pakistan flood) were physically connected. It is found that the Russian heat wave was associated with the development of an extraordinarily strong and prolonged extratropical atmospheric blocking event in association with the excitation of a large-scale atmospheric Rossby wave train spanning western Russia. Kazakhstan, and the northwestern China Tibetan Plateau region. The southward penetration of upper-level vorticity perturbations in the leading trough of the Rossby wave was instrumental in triggering anomalously heavy rain events over northern Pakistan and vicinity in mid- to late July. Also shown are evidences that the Russian heat wave was amplified by a positive feedback through changes in surface energy fluxes between the atmospheric blocking pattern and an underlying extensive land region with below-normal soil moisture. The Pakistan heavy rain events were amplified and sustained by strong anomalous southeasterly flow along the Himalayan foothills and abundant moisture transport from the Bay of Bengal in connection with the northward propagation of the monsoonal intraseasonal oscillation. C1 [Lau, William K. M.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA. [Kim, Kyu-Myong] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Lau, WKM (reprint author), NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA. EM william.k.lau@nasa.gov RI Kim, Kyu-Myong/G-5398-2014; Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 FU NASA Interdisciplinary Investigation; Tropical Rainfall Measuring Mission (TRMM); Korean Meteorological Administration [RACS_2010-2018] FX This work was supported by the NASA Interdisciplinary Investigation and the Tropical Rainfall Measuring Mission (TRMM). K.-M. Kim was supported by the Korean Meteorological Administration Research and Development Program under Grant RACS_2010-2018. We thank two anonymous reviewers for their critical and detailed review of the paper. NR 21 TC 66 Z9 69 U1 1 U2 24 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2012 VL 13 IS 1 BP 392 EP 403 DI 10.1175/JHM-D-11-016.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 890IN UT WOS:000300138400025 ER PT J AU Seneviratne, SI Koster, RD AF Seneviratne, Sonia I. Koster, Randal D. TI A Revised Framework for Analyzing Soil Moisture Memory in Climate Data: Derivation and Interpretation SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID ATMOSPHERE COUPLING EXPERIMENT; MODELS; IMPACTS; EUROPE; SKILL; GLACE AB A revised framework for the analysis of soil moisture memory characteristics of climate models and observational data is derived from the approach proposed by Koster and Suarez. The resulting equation allows the expression of the month-to-month soil moisture autocorrelation as a function of 1) the initial soil moisture variability, 2) the (atmospheric) forcing variability over the considered time period, 3) the correlation between initial soil moisture and subsequent forcing, 4) the sensitivity of evaporation to soil moisture, and 5) the sensitivity of runoff to soil moisture. A specific new feature is the disentangling of the roles of initial soil moisture variability and forcing variability, which were both (for the latter indirectly) contributing to the seasonality term of the original formulation. In addition, a version of the framework entirely based on explicit equations for the underlying relationships (i.e., independent of soil moisture statistics at the following time step) is proposed. The validity of the derived equation is exemplified with atmospheric general circulation model (AGCM) simulations from the Global Land Atmosphere Coupling Experiment (GLACE). C1 [Seneviratne, Sonia I.] ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland. [Koster, Randal D.] NASA Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Seneviratne, SI (reprint author), ETH, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland. EM sonia.seneviratne@env.ethz.ch RI Koster, Randal/F-5881-2012; Seneviratne, Sonia/G-8761-2011 OI Koster, Randal/0000-0001-6418-6383; Seneviratne, Sonia/0000-0001-9528-2917 NR 19 TC 21 Z9 21 U1 1 U2 26 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X J9 J HYDROMETEOROL JI J. Hydrometeorol. PD FEB PY 2012 VL 13 IS 1 BP 404 EP 412 DI 10.1175/JHM-D-11-044.1 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 890IN UT WOS:000300138400026 ER PT J AU Layton, BE Lynch, B Peter, T Jamieson, B AF Layton, Bradley E. Lynch, Bernard Peter, Thomas Jamieson, Brian TI Red blood cell sorting with a multi-bed microfabricated filter SO JOURNAL OF MICROMECHANICS AND MICROENGINEERING LA English DT Article ID ERYTHROCYTE AGGREGATION; HEART-FAILURE; SEPARATION; FLOW; MICROCHANNEL; MICROSYSTEMS; FLUCTUATIONS; DYNAMICS; SURFACES; ANALYZER AB A microfabricated fluidic chip for sorting red blood cells (RBCs) by size has been designed, fabricated and tested. The performance of the chip has been compared against a flow cytometer using samples from identical populations of cells, and statistically significant (p < 0.0005) differences in the measured cell size distributions were observed. The measurement paradigm reported here differs from previously demonstrated devices such as microfabricated Coulter counters or flow cytometers, in that the analysis is inherently parallel and is thus suitable for high throughput, point-of-care analysis. This study is empirical and semi-quantitative. However, important features of RBC trapping are characterized and indications for improved device design are described. C1 [Layton, Bradley E.] Univ Montana, Dept Appl Comp & Elect, Missoula, MT 59802 USA. [Lynch, Bernard; Jamieson, Brian] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Peter, Thomas] Univ Michigan, Dept Biomed Engn, Ann Arbor, MI 48109 USA. [Jamieson, Brian] Sci & Biomed Microsyst, Columbia, MD 21046 USA. RP Layton, BE (reprint author), Univ Montana, Dept Appl Comp & Elect, 909 S Ave W, Missoula, MT 59802 USA. EM bradley.layton@umontana.edu FU NASA [DDF-05-553] FX This work was supported by NASA DDF-05-553. The authors would like to acknowledge assistance from Ken Class of the University of Maryland for consultation and use of equipment. We also thank Ms Stephanie Sullivan for preliminary protocol development and Dr Kathleen Allen for researching references. Any opinions, findings and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Aeronautics and Space Administration. NR 51 TC 1 Z9 1 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0960-1317 J9 J MICROMECH MICROENG JI J. Micromech. Microeng. PD FEB PY 2012 VL 22 IS 2 AR 025009 DI 10.1088/0960-1317/22/2/025009 PG 7 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Instruments & Instrumentation; Physics, Applied SC Engineering; Science & Technology - Other Topics; Instruments & Instrumentation; Physics GA 887VI UT WOS:000299959000009 ER PT J AU Chatterjee, A Diordieva, I Yumoto, K Globus, RK Bhattacharya, S AF Chatterjee, Anuran Diordieva, Inna Yumoto, Kenji Globus, Ruth K. Bhattacharya, Sharmila TI Protein array profiling of mouse serum, six months post whole body radiation with Fe-56 SO JOURNAL OF TOXICOLOGICAL SCIENCES LA English DT Article DE Proteomic; Microarray; Serum; Mice; Radiation ID SPACE RADIATION; CELLS AB To determine the chronic effects of heavy ion irradiation, an antibody based proteomic microarray technology was applied to monitor alterations in the serum proteome, six months after whole body irradiation of adult male C57B1/6 mice with 0.5 Gray of Fe-56. Out of 507 proteins, irradiation reduced expression of 25 proteins and enhanced expression of 12 proteins in serum (> 5% change relative to sham-irradiated controls). Of the 25 proteins found to be down-regulated, Poly ADP Ribose Polymerase (PARP) was 13% lower in the 0.5Gy mice and among the up-regulated proteins, beta-Tubulin was found to be 10% higher in the 0.5Gy group compared to the sham-irradiated 0Gy controls. Thus, irradiation with a relatively low dose of heavy ions caused persistent and selective changes in serum levels of proteins that are typically intracellular, suggesting chronic genotoxic damage. C1 [Chatterjee, Anuran; Yumoto, Kenji; Globus, Ruth K.; Bhattacharya, Sharmila] NASA, Space Biosci Res Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Diordieva, Inna] Clontech Labs, Mountain View, CA 94035 USA. RP Bhattacharya, S (reprint author), NASA, Space Biosci Res Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. EM sharmila.bhattacharya@nasa.gov FU NASA [NNH104Z-UU005N/RAD2004-0000-0110]; DOE-NASA [DE-SC0001507]; Office of Science (BER), U.S. Department of Energy FX Research was supported by a NASA grant (NNH104Z-UU005N/RAD2004-0000-0110) and a DOE-NASA Interagency Award #DE-SC0001507, supported by the Office of Science (BER), U.S. Department of Energy to RKG. NR 4 TC 1 Z9 1 U1 1 U2 3 PU JAPANESE SOC TOXICOLOGICAL SCIENCES PI TOKYO PA INTERNATIONAL MEDICAL INFORMATION CENTER, SHINANOMACHI RENGAKAN, 35 SHINANO-MACHI, SHINJUKU-KU, TOKYO, 160-0016, JAPAN SN 0388-1350 EI 1880-3989 J9 J TOXICOL SCI JI J. Toxicol. Sci. PD FEB PY 2012 VL 37 IS 1 BP 215 EP 217 PG 3 WC Toxicology SC Toxicology GA 890IX UT WOS:000300139400020 PM 22293426 ER PT J AU Nakashima, D Ushikubo, T Zolensky, ME Kita, NT AF Nakashima, Daisuke Ushikubo, Takayuki Zolensky, Michael E. Kita, Noriko T. TI High precision oxygen three-isotope analyses of anhydrous chondritic interplanetary dust particles SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID EARLY SOLAR NEBULA; CARBONACEOUS CHONDRITES; ISOTOPIC COMPOSITIONS; COMET 81P/WILD-2; SILICATE GRAINS; ION MICROPROBE; CHONDRULES; SYSTEM; ALLENDE; ORIGIN AB Oxygen three-isotope ratios of three anhydrous chondritic interplanetary dust particles (IDPs) were analyzed using an ion microprobe with a 2 mu m small beam. The three anhydrous IDPs show Delta 17O values ranging from -5 parts per thousand to +1 parts per thousand, which overlap with those of ferromagnesian silicate particles from comet Wild 2 and anhydrous porous IDPs. For the first time, internal oxygen isotope heterogeneity was resolved in two IDPs at the level of a few per mil in Delta 17O values. Anhydrous IDPs are loose aggregates of fine-grained silicates (=3 mu m in this study), with only a few coarse-grained silicates (220 mu m in this study). On the other hand, Wild 2 particles analyzed so far show relatively coarse-grained (= few mu m) igneous textures. If anhydrous IDPs represent fine-grained particles from comets, the similar Delta 17O values between anhydrous IDPs and Wild 2 particles may imply that oxygen isotope ratios in cometary crystalline silicates are similar, independent of crystal sizes and their textures. The range of Delta 17O values of the three anhydrous IDPs overlaps also with that of chondrules in carbonaceous chondrites, suggesting a genetic link between cometary dust particles (Wild 2 particles and most anhydrous IDPs) and carbonaceous chondrite chondrules. C1 [Nakashima, Daisuke; Ushikubo, Takayuki; Kita, Noriko T.] Univ Wisconsin, Dept Geosci, WiscSIMS, Madison, WI 53706 USA. [Zolensky, Michael E.] NASA Johnson Space Ctr, Astromat Res & Explorat Sci, Houston, TX 77058 USA. RP Nakashima, D (reprint author), Univ Wisconsin, Dept Geosci, WiscSIMS, Madison, WI 53706 USA. EM naka@geology.wisc.edu RI Kita, Noriko/H-8035-2016 OI Kita, Noriko/0000-0002-0204-0765 FU NASA LARS [NK, NNX09AC30G]; NSF-EAR [0319230, 0744079]; NASA FX Thoughtful comments from T. Stephan, J. Aleon, S. Messenger, and C. Floss improved the quality of this manuscript significantly. The authors thank R. K. Noll for help with FE-SEM observation, P. E. Brown for lending a high magnification objective lens for optical microscope, H. Xu for allowing using a polarizing microscope, and J. Kern for SIMS support. This work is supported by the NASA LARS program (NK, NNX09AC30G). WiscSIMS is partly supported by NSF-EAR (0319230, 0744079). M. Z. was supported by NASA's Cosmochemistry and Laboratory Analysis of Returned Samples Programs. NR 59 TC 9 Z9 9 U1 0 U2 10 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD FEB PY 2012 VL 47 IS 2 BP 197 EP 208 DI 10.1111/j.1945-5100.2011.01319.x PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 887MI UT WOS:000299931200003 ER PT J AU Angel, SM Gomer, NR Sharma, SK Mckay, C AF Angel, S. Michael Gomer, Nathaniel R. Sharma, Shiv K. Mckay, Chris TI Remote Raman Spectroscopy for Planetary Exploration: A Review SO APPLIED SPECTROSCOPY LA English DT Review DE Planetary Raman; Standoff Raman; Astrospectroscopy; Laser-induced breakdown spectroscopy; LABS; Laser-induced fluorescence; LIE; Europa; Enceladus; Astrobiology ID NM LASER-PULSE; STANDOFF DETECTION; SUBSURFACE OCEAN; MINERAL IDENTIFICATION; MARTIAN METEORITE; RADIAL DISTANCE; 100 METERS; RIO-TINTO; SPECTRA; MARS AB In this review, we discuss the current state of standoff Raman spectroscopy as it applies to remote planetary applications, including standoff instrumentation, the technique's ability to identify biologically and geologically important analytes, and the feasibility to make standoff Raman measurements under various planetary conditions. This is not intended to be an exhaustive review of standoff Raman and many excellent papers are not mentioned. Rather it is intended to give the reader a quick review of the types of standoff Raman systems that are being developed and that might be suitable for astrospectroscopy, a look at specific analytes that are of interest for planetary applications, planetary measurement opportunities and challenges that need to be solved, and a brief discussion of the feasibility of making surface and plume planetary Raman measurements from an orbiting spacecraft. C1 [Angel, S. Michael; Gomer, Nathaniel R.] Univ S Carolina, Dept Chem & Biochem, Columbia, SC 29208 USA. [Sharma, Shiv K.] Univ Hawaii, Hawaii Inst Geophys Planetol, Honolulu, HI 96822 USA. [Mckay, Chris] NASA Ames, Moffett Field, CA 94035 USA. RP Angel, SM (reprint author), Univ S Carolina, Dept Chem & Biochem, Columbia, SC 29208 USA. EM angel@chem.sc.edu OI Angel, Stanley/0000-0002-0328-0568 FU NSF [CHE 0526821]; NASA under a MIDDP [NNX08AR10G] FX The authors at USC would like to thank NSF for funding for some of the work presented under CHE 0526821, and additional thanks goes to DOE/Lawrence Livermore National Laboratory for equipment and supplies. The work at the University of Hawaii was supported in part by NASA under a MIDDP grant NNX08AR10G. NR 85 TC 29 Z9 29 U1 10 U2 56 PU SOC APPLIED SPECTROSCOPY PI FREDERICK PA 5320 SPECTRUM DRIVE SUITE C, FREDERICK, MD 21703 USA SN 0003-7028 J9 APPL SPECTROSC JI Appl. Spectrosc. PD FEB PY 2012 VL 66 IS 2 BP 137 EP 150 DI 10.1366/11-06535 PG 14 WC Instruments & Instrumentation; Spectroscopy SC Instruments & Instrumentation; Spectroscopy GA 886KZ UT WOS:000299854600001 PM 22449277 ER PT J AU Oterkus, E Madenci, E Weckner, O Silling, S Bogert, P Tessler, A AF Oterkus, Erkan Madenci, Erdogan Weckner, Olaf Silling, Stewart Bogert, Philip Tessler, Alexander TI Combined finite element and peridynamic analyses for predicting failure in a stiffened composite curved panel with a central slot SO COMPOSITE STRUCTURES LA English DT Article DE Progressive; Failure; Composites; Nonlocal; Peridynamic theory AB This study presents an analysis approach based on a merger of the finite element method and the peridynamic theory. Its validity is established through qualitative and quantitative comparisons against the test results for a stiffened composite curved panel with a central slot under combined internal pressure and axial tension. The predicted initial and final failure loads, as well as the final failure modes, are in close agreement with the experimental observations. This approach demonstrates the capability of the PD approach to assess the durability of complex composite structures. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Oterkus, Erkan; Madenci, Erdogan] Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA. [Weckner, Olaf] Boeing Res & Technol, Seattle, WA 98124 USA. [Silling, Stewart] Sandia Natl Labs, Multiscale Dynam Mat Modeling Dept, Albuquerque, NM 87185 USA. [Bogert, Philip; Tessler, Alexander] NASA Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA. RP Madenci, E (reprint author), Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA. EM oterkus@email.arizona.edu; madenci@email.arizona.edu; Olaf.Weckner@boeing.com; sasilli@sandia.gov; philip.b.bogert@nasa.gov; alexander.tessler-1@nasa.gov NR 10 TC 32 Z9 35 U1 3 U2 26 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0263-8223 J9 COMPOS STRUCT JI Compos. Struct. PD FEB PY 2012 VL 94 IS 3 BP 839 EP 850 DI 10.1016/j.compstruct.2011.07.019 PG 12 WC Materials Science, Composites SC Materials Science GA 882WP UT WOS:000299594900005 ER PT J AU Drossart, P Limaye, SS Smrekar, SA AF Drossart, Pierre Limaye, Sanjay S. Smrekar, Suzanne A. TI Introduction to advances in Venus science special issue SO ICARUS LA English DT Editorial Material C1 [Drossart, Pierre] Observ Paris, LESIA, F-92195 Meudon, France. [Limaye, Sanjay S.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA. [Smrekar, Suzanne A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Drossart, P (reprint author), Observ Paris, LESIA, 5 Pl Jules Janssen, F-92195 Meudon, France. OI Limaye, Sanjay/0000-0001-8659-2104 NR 0 TC 1 Z9 1 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD FEB PY 2012 VL 217 IS 2 SI SI BP 433 EP 433 DI 10.1016/j.icarus.2011.12.017 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878FE UT WOS:000299240100001 ER PT J AU Smrekar, SE Sotin, C AF Smrekar, Suzanne E. Sotin, Christophe TI Constraints on mantle plumes on Venus: Implications for volatile history SO ICARUS LA English DT Article DE Venus, Interior; Volcanism; Thermal histories; Planetary dynamics; Geophysics ID TEMPERATURE-DEPENDENT VISCOSITY; STAGNANT LID CONVECTION; PRANDTL NUMBER FLUID; HIGH-RAYLEIGH-NUMBER; THERMAL-CONVECTION; TERRESTRIAL PLANETS; WATER SOLUBILITY; TOPOGRAPHIC RISES; SPHERICAL-SHELL; EVOLUTION AB The analysis of Venus' gravity field and topography suggests the presence of a small number of deep mantle plumes (similar to 9). This study predicts the number of plumes formed at the core-mantle boundary, their characteristics, and the production of partial melt from adiabatic decompression. Numerical simulations are performed using a 3D spherical code that includes large viscosity variations and internal heating. This study investigates the effect of several parameters including the core-mantle boundary temperature, the amount of internal heating, and the mantle viscosity. The smallest number of plumes is achieved when no internal heating is present. However, scaling Earth's radiogenic heating to Venus suggests a value of similar to 16 TW. Cases with internal heating produce more realistic lid thickness and partial melting, but produce either too many plumes or no plumes if a high mantle temperature precludes the formation of a hot thermal boundary layer. Mantle viscosity must be reduced to at least 10(20) Pa s in order to include significant internal heating and still produce hot plumes. In all cases that predict melting, melting occurs throughout the upper mantle. Only cases with high core temperature (>1700 K) produce dry melting. Over time the upper mantle may have lost significant volatiles. Depending on the water content of the lower mantle, deep plumes may contribute to present-day atmospheric water via volcanic outgassing. Assuming 50 ppm water in mantle, 10 plumes with a buoyancy flux of 500 kg/s continuously erupting for 4 myr will outgas an amount of water on the order of that in the lower atmosphere. A higher level of internal heating than achieved to date, as well as relatively low mantle viscosity, may be required to achieve simulations with similar to 10 plumes and a thinner lid. Alternatively, if the mantle is heating up due to the stagnant lid, the effect is equivalent to having lower rates of internal heating. A temperature increase of 110 K/byr is equivalent to -13 TW. This value along with the internal heating of 3 TW used in this study may represent the approximate heat budget of Venus' mantle. (C) 2011 Elsevier Inc. All rights reserved. C1 [Smrekar, Suzanne E.; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. RP Smrekar, SE (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. EM ssmrekar@jpl.nasa.gov FU JPL RTD; French space agency CNES; NASA FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology. CS acknowledges support by JPL R&TD and by the French space agency CNES through support for his Interdisciplinary Scientist role on Venus Express. S.S. acknowledges support from NASA's Planetary Geology and Geophysics Program and NASA interdisciplinary scientist funding for participation on Venus Express. This paper would not have been possible without help from Gael Choblet with the OEDIPUS code, and was significantly improved thanks to very constructive reviews by Shijie Zhong and Anne Davaille. We thank Linda Elkins-Tanton for discussions on melting and mantle water content. Computing was carried out at both the NASA Ames and JPL supercomputer facilities. We thank the undergraduate interns who have contributed to this work: Brian Anderson, Ryen Lapham, Holly Taylor, Ian Bolliger, and Veronica Burnett. Special thanks go to Timmary (Annie) Bonaccorso and Henry Tom, returning students who persevered though numerous variations on plume counting methods. NR 70 TC 14 Z9 15 U1 1 U2 22 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB PY 2012 VL 217 IS 2 SI SI BP 510 EP 523 DI 10.1016/j.icarus.2011.09.011 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878FE UT WOS:000299240100008 ER PT J AU Cottini, V Ignatiev, NI Piccioni, G Drossart, P Grassi, D Markiewicz, WJ AF Cottini, V. Ignatiev, N. I. Piccioni, G. Drossart, P. Grassi, D. Markiewicz, W. J. TI Water vapor near the cloud tops of Venus from Venus Express/VIRTIS dayside data SO ICARUS LA English DT Article DE Venus; Atmosphere ID MIDDLE ATMOSPHERE; SULFURIC-ACID; THERMODYNAMIC PROPERTIES; MULTIPLE-SCATTERING; RADIATIVE-TRANSFER; MESOSPHERE; POLARIZATION; VENERA-15; ABUNDANCE; SPECTRA AB Observations of the dayside of Venus performed by the high spectral resolution channel (-H) of the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) on board the ESA Venus Express mission have been used to measure the altitude of the cloud tops and the water vapor abundance around this level with a spatial resolution ranging from 100 to 10 km. CO2 and H2O bands between 2.48 and 2.60 mu m are analyzed to determine the cloud top altitude and water vapor abundance near this level. At low latitudes (+/- 40 degrees) mean water vapor abundance is equal to 3 +/- 1 ppm and the corresponding cloud top altitude at 2.5 mu m is equal to 69.5 +/- 2 km. Poleward from middle latitudes the cloud top altitude gradually decreases down to 64 km, while the average H2O abundance reaches its maximum of 5 PPm at 80 degrees of latitude with a large scatter from 1 to 15 ppm. The calculated mass percentage of the sulfuric acid solution in cloud droplets of mode 2 (similar to 1 mu m) particles is in the range 75-83%, being in even more narrow interval of 80-83% in low latitudes. No systematic correlation of the dark UV markings with the cloud top altitude or water vapor has been observed. (C) 2011 Elsevier Inc. All rights reserved. C1 [Cottini, V.] NASA GSFC, Greenbelt, MD 20771 USA. [Cottini, V.; Ignatiev, N. I.; Piccioni, G.] Ist Astrofis Spaziale & Fis Cosm IASF INAF, Rome, Italy. [Ignatiev, N. I.] Russian Acad Sci IKI RAN, Space Res Inst, Moscow, Russia. [Ignatiev, N. I.; Markiewicz, W. J.] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. [Drossart, P.] Observ Paris, LESIA, Meudon, France. [Grassi, D.] Ist Fis Spazio Interplanetario IFSI INAF, Rome, Italy. RP Cottini, V (reprint author), NASA GSFC, Code 693,Bldg 34,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM valeria.cottini@nasa.gov OI Piccioni, Giuseppe/0000-0002-7893-6808; Grassi, Davide/0000-0003-1653-3066 FU Agenzia Spaziale Italiana (ASI); Centre National d'Etudes Spatiales (CNES); Russian Foundation of Basic Research [08-02-01383] FX Venus Express is a mission of the European Space Agency. We thank the Agenzia Spaziale Italiana (ASI) and the Centre National d'Etudes Spatiales (CNES) for the support and funding of the VIRTIS experiment. N.I. was supported by the Russian Foundation of Basic Research Grant 08-02-01383. We gratefully thank all members of the Venus Express project and of the VIRTIS and VMC technical teams. We also thank D.V. Titov, an anonymous referee, and C.A. Nixon for carefully reviewing this manuscript and suggesting several improvements. NR 53 TC 18 Z9 18 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD FEB PY 2012 VL 217 IS 2 SI SI BP 561 EP 569 DI 10.1016/j.icarus.2011.06.018 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878FE UT WOS:000299240100012 ER PT J AU Cotton, DV Bailey, J Crisp, D Meadows, VS AF Cotton, Daniel V. Bailey, Jeremy Crisp, D. Meadows, V. S. TI The distribution of carbon monoxide in the lower atmosphere of Venus SO ICARUS LA English DT Article DE Atmospheres, Chemistry; Atmospheres, Dynamics; Radiative transfer; Spectroscopy; Venus, Atmosphere ID DEEP ATMOSPHERE; NIGHTSIDE; CO; SPECTROSCOPY; TEMPERATURE; TROPOSPHERE; MESOSPHERE; ABUNDANCE; SPECTRA; SURFACE AB We have obtained spatially resolved near-infrared spectroscopy of the Venus nightside on 15 nights over three observing seasons. We use the depth of the CO absorption band at 2.3 mu m to map the two-dimensional distribution of CO across both hemispheres. Radiative transfer models are used to relate the measured CO band depth to the volume mixing ratio of CO. The results confirm previous investigations in showing a general trend of increased CO abundances at around 60 latitude north and south as compared with the equatorial regions. Observations taken over a few nights generally show very similar CO distributions, but significant changes are apparent over longer periods. In past studies it has been assumed that the CO latitudinal variation occurs near 35 km altitude, at which K-band sensitivity to CO is greatest. By modeling the detailed spectrum of the excess CO at high latitudes we show that it occurs at altitudes around 45 km, much higher than has previously been assumed, and that there cannot be significant contribution from levels of 36 km or lower. We suggest that this is most likely due to downwelling of CO-rich gas from the upper atmosphere at these latitudes, with the CO being removed by around 40 km through chemical processes such as the reaction with SO3. (C) 2011 Elsevier Inc. All rights reserved. C1 [Cotton, Daniel V.; Bailey, Jeremy] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Crisp, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Meadows, V. S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Bailey, Jeremy; Crisp, D.; Meadows, V. S.] NASA Astrobiol Inst, Virtual Planetary Lab Lead Team, Washington, DC USA. RP Bailey, J (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. EM j.bailey@unsw.edu.au NR 44 TC 7 Z9 7 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 J9 ICARUS JI Icarus PD FEB PY 2012 VL 217 IS 2 SI SI BP 570 EP 584 DI 10.1016/j.icarus.2011.05.020 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878FE UT WOS:000299240100013 ER PT J AU McGouldrick, K Momary, TW Baines, KH Grinspoon, DH AF McGouldrick, Kevin Momary, Thomas W. Baines, Kevin H. Grinspoon, David H. TI Quantification of middle and lower cloud variability and mesoscale dynamics from Venus Express/VIRTIS observations at 1.74 mu m SO ICARUS LA English DT Article DE Venus, Atmosphere; Atmospheres, Dynamics; Atmospheres, Evolution; Infrared observations; Meteorology ID DARK SIDE; EVOLUTION; CLIMATE; VIRTIS; FEATURES; MISSION; MODEL; HOLES AB We present an analysis of VIRTIS-M-IR observations of 1.74 mu m emission from the nightside of Venus. The 1.74 mu m window in the near infrared spectrum of Venus is an ideal proxy for investigating the evolution of middle and lower cloud deck opacity of Venus because it exhibits good signal to noise due to its brightness, good contrast between bright and dark regions, and few additional sources of extinction beside the clouds themselves. We have analyzed the data from the first 407 orbits (equivalent to 407 Earth days) of the Venus Express mission to determine the magnitude of variability in the 1.74 mu m radiance. We have also performed an analysis of the evolution of individual features over a span of roughly 5-6 h on two successive orbits of Venus Express. We find that the overall 1.74 mu m brightness of Venus has been increasing through the first 407 days of the mission, indicating a gradual diminishing of the cloud coverage and/or thickness, and that the lower latitudes exhibited more variability and more brightening than higher latitudes. We find that individual features evolve with a time scale of about 30 h, consistent with our previous analysis. Analysis of the evolution and motion of the clouds can be used to estimate the mesoscale dynamics within the clouds of Venus. We find that advection alone cannot explain the observed evolution of the features. The measured vorticity and divergence in the vicinity of the features are consistent with evolution under the influence of significant vertical motions likely driven by a radiative dynamical feedback. We measure a zonal wind speed of around 65 m/s, and a meridional wind speed around 2.5 m/s by tracking the motion of the central region of the features. But we also find that the measured wind speeds depend strongly on the points chosen for the wind speed analysis. (C) 2011 Elsevier Inc. All rights reserved. C1 [McGouldrick, Kevin] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. [Momary, Thomas W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Baines, Kevin H.] Univ Wisconsin, Dept Space Sci & Engn, Madison, WI 53706 USA. [Grinspoon, David H.] Denver Museum Nat & Sci, Dept Space Sci, Denver, CO 80205 USA. RP McGouldrick, K (reprint author), Univ Colorado, Lab Atmospher & Space Phys, 1234 Innovat Dr, Boulder, CO 80303 USA. EM kevin.mcgouldrick@lasp.colorado.edu FU National Aeronautics and Space Administration FX We thank two anonymous reviewers for their helpful comments that have led to the improvement of this paper, especially with regard to the analysis of the mesoscale dynamics. We also thank Giuseppe Piccioni, Pierre Drossart, and the VIRTIS team for their work in the preparation of the data from the VIRTIS instrument. A portion of the work described in this paper was carried out at the Jet Propulsion Laboratory, Pasadena, CA, under contract with the National Aeronautics and Space Administration. All authors were supported by NASA in support of ESA's Venus Express mission. NR 46 TC 4 Z9 4 U1 0 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD FEB PY 2012 VL 217 IS 2 SI SI BP 615 EP 628 DI 10.1016/j.icarus.2011.07.009 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878FE UT WOS:000299240100017 ER PT J AU Titov, DV Markiewicz, WJ Ignatiev, NI Song, L Limaye, SS Sanchez-Lavega, A Hesemann, J Almeida, M Roatsch, T Matz, KD Scholten, F Crisp, D Esposito, LW Hviid, SF Jaumann, R Keller, HU Moissl, R AF Titov, Dmitrij V. Markiewicz, Wojciech J. Ignatiev, Nikolay I. Song, Li Limaye, Sanjay S. Sanchez-Lavega, Agustin Hesemann, Jonas Almeida, Miguel Roatsch, Thomas Matz, Klaus-Dieter Scholten, Frank Crisp, David Esposito, Larry W. Hviid, Stubbe F. Jaumann, Ralf Keller, Horst U. Moissl, Richard TI Morphology of the cloud tops as observed by the Venus Express Monitoring Camera SO ICARUS LA English DT Article DE Venus; Cloud morphology; UV imaging; Venus Monitoring Camera ID WINDS; ATMOSPHERE; MISSION; GALILEO; IMAGES; DYNAMICS; PATTERNS; FEATURES; WAVES AB Since the discovery of ultraviolet markings on Venus, their observations have been a powerful tool to study the morphology, motions and dynamical state at the cloud top level. Here we present the results of investigation of the cloud top morphology performed by the Venus Monitoring Camera (VMC) during more than 3 years of the Venus Express mission. The camera acquires images in four narrow-band filters centered at 365, 513, 965 and 1010 nm with spatial resolution from 50 km at apocentre to a few hundred of meters at pericentre. The VMC experiment provides a significant improvement in the Venus imaging as compared to the capabilities of the earlier missions. The camera discovered new cloud features like bright "lace clouds" and cloud columns at the low latitudes, dark polar oval and narrow circular and spiral "grooves" in the polar regions, different types of waves at the high latitudes. The VMC observations revealed detailed structure of the sub-solar region and the afternoon convective wake, the bow-shape features and convective cells, the mid-latitude transition region and the "polar cap". The polar orbit of the satellite enables for the first time nadir viewing of the Southern polar regions and an opportunity to zoom in on the planet. The experiment returned numerous images of the Venus limb and documented global and local brightening events. VMC provided almost continuous monitoring of the planet with high temporal resolution that allowed one to follow changes in the cloud morphology at various scales. We present the in-flight performance of the instrument and focus in particular on the data from the ultraviolet channel, centered at the characteristic wavelength of the unknown UV absorber that yields the highest contrasts on the cloud top. Low latitudes are dominated by relatively dark clouds that have mottled and fragmented appearance clearly indicating convective activity in the sub-solar region. At similar to 50 degrees latitude this pattern gives way to streaky clouds suggesting that horizontal, almost laminar, flow prevails here. Poleward from about 60 degrees S the planet is covered by almost featureless bright polar hood sometimes crossed by dark narrow (similar to 300 km) spiral or circular structures. This global cloud pattern can change on time scales of a few days resulting in global and local "brightening events" when the bright haze can extend far into low latitudes and/or increase its brightness by 30%. Close-up snapshots reveal plenty of morphological details like convective cells, cloud streaks, cumulus-like columns, wave trains. Different kinds of small scale waves are frequently observed at the cloud top. The wave activity is mainly observed in the 65-80 degrees latitude band and is in particular concentrated in the region of Ishtar Terra that suggests their possible orographic origin. The VMC observations have important implications for the problems of the unknown UV absorber, microphysical processes, dynamics and radiative energy balance at the cloud tops. They are only briefly discussed in the paper, but each of them will be the subject of a dedicated study. (C) 2011 Elsevier Inc. All rights reserved. C1 [Titov, Dmitrij V.] ESA ESTEC, NL-2200 AG Noordwijk, Netherlands. [Titov, Dmitrij V.; Markiewicz, Wojciech J.; Ignatiev, Nikolay I.; Song, Li; Hesemann, Jonas; Hviid, Stubbe F.; Keller, Horst U.; Moissl, Richard] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Ignatiev, Nikolay I.] Space Res Inst IKI, Moscow 117997, Russia. [Limaye, Sanjay S.] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI 53706 USA. [Sanchez-Lavega, Agustin] Univ Basque Country, ETSI, Bilbao 48013, Spain. [Almeida, Miguel] SRE OS, ESA ESAC, Madrid 28691, Spain. [Roatsch, Thomas; Matz, Klaus-Dieter; Scholten, Frank; Jaumann, Ralf] Inst Planetary Explorat DLR, D-12489 Berlin, Germany. [Crisp, David] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Esposito, Larry W.] Univ Colorado, LASP, Boulder, CO 80309 USA. RP Titov, DV (reprint author), ESA ESTEC, PB 299, NL-2200 AG Noordwijk, Netherlands. EM Dmitri.Titov@esa.int OI Limaye, Sanjay/0000-0001-8659-2104; Sanchez-Lavega, Agustin/0000-0001-7355-1522 NR 49 TC 48 Z9 48 U1 0 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 J9 ICARUS JI Icarus PD FEB PY 2012 VL 217 IS 2 SI SI BP 682 EP 701 DI 10.1016/j.icarus.2011.06.020 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878FE UT WOS:000299240100023 ER PT J AU Sonnabend, G Krotz, P Schmulling, F Kostiuk, T Goldstein, J Sornig, M Stupar, D Livengood, T Hewagama, T Fast, K Mahieux, A AF Sonnabend, Guido Kroetz, Peter Schmuelling, Frank Kostiuk, Theodor Goldstein, Jeff Sornig, Manuela Stupar, Dusan Livengood, Timothy Hewagama, Tilak Fast, Kelly Mahieux, Arnaud TI Thermospheric/mesospheric temperatures on Venus: Results from ground-based high-resolution spectroscopy of CO2 in 1990/1991 and comparison to results from 2009 and between other techniques SO ICARUS LA English DT Article DE Venus, Atmosphere; Infrared observations; Spectroscopy ID MU-M WAVELENGTH; INFRARED HETERODYNE SPECTROSCOPY; NATURAL LASER-EMISSION; UPPER-ATMOSPHERE; LINE OBSERVATIONS; THERMAL STRUCTURE; WIND VELOCITIES; MARS; THERMOSPHERE; SPECTROMETER AB We report temperatures in Venus' upper mesosphere/lower thermosphere, deduced from reanalyzing very high resolution infrared spectroscopy of CO2 emission lines acquired in 1990 and 1991. Kinetic temperatures at similar to 110 km altitude (0.15 Pa) are derived from the Doppler width of fully-resolved single line profiles measured near 10.4 mu m wavelength using the NASA GSFC Infrared Heterodyne Spectrometer (IRHS) at the NASA IRTF on Mauna Kea, HI, close to Venus inferior conjunction and two Venus solstices. Measured temperatures range from similar to 200 to 240 K with uncertainty typically less than 10 K. Temperatures retrieved from similar measurement in 2009 using the Cologne Tuneable Heterodyne Infrared Spectrometer (THIS) at the NOAO McMath Telescope at Kitt Peak, AZ are 10-20 K lower. Temperatures retrieved more recently from the SOIR instrument on Venus EXpress are consistent with these results when the geometry of observation is accounted for. It is difficult to compare ground-based sub-mm retrievals extrapolated to 110 km due to their much larger field of view, which includes the night side regions not accessible to infrared heterodyne observations. Temperature variability appears to be high on day-to-day as well as longer timescales. Observed short term and long term variability may be attributed to atmospheric dynamics, diurnal variability and changes over solar activity and seasons. The Venus International Reference Atmosphere (VIRA) model predicts cooler temperatures at the sampled altitudes in the lower thermosphere/upper mesosphere and is not consistent with these measurements. (C) 2011 Elsevier Inc. All rights reserved. C1 [Sonnabend, Guido; Kroetz, Peter; Stupar, Dusan] Univ Cologne, Inst Phys, D-50937 Cologne, Germany. [Schmuelling, Frank; Kostiuk, Theodor; Fast, Kelly] NASA GSFC, Greenbelt, MD 20771 USA. [Schmuelling, Frank] DLR, D-53227 Bonn, Germany. [Goldstein, Jeff; Livengood, Timothy] NCESSE, Capital Hts, MD 20791 USA. [Hewagama, Tilak] Univ Maryland, College Pk, MD 20742 USA. [Sornig, Manuela] Rhein Inst Umweltforsch, D-50931 Cologne, Germany. [Mahieux, Arnaud] Belgian Inst Space Aeron, B-1180 Brussels, Belgium. RP Sonnabend, G (reprint author), Univ Cologne, Inst Phys, Zulpicher Str 77, D-50937 Cologne, Germany. EM samstag@ph1.uni-koeln.de RI Hewagama, T/C-8488-2012; Livengood, Timothy/C-8512-2012; Kostiuk, Theodor/A-3077-2014 FU National Aeronautics and Space Administration; Deutsche Forschungsgemeinschaft (DFG) [SO879/1-2]; Belgian Federal Science Policy Office; European Space Agency (ESA, PRODEX) [C90268, 90113, 17645] FX Research at the NASA Infrared Telescope Facility was supported by the National Aeronautics and Space Administration Planetary Astronomy Program. This work was supported by the Deutsche Forschungsgemeinschaft (DFG) through Grant SO879/1-2. We would like to thank the SOIR team, especially Jean-Loup Bertaux, PI of the instrument, and Ann Carine Vandaele, group leader at the Belgian Institute for Space Aeronomy, Brussels. The research program was supported by the Belgian Federal Science Policy Office and the European Space Agency (ESA, PRODEX program, contracts C90268, 90113, and 17645). NR 35 TC 11 Z9 11 U1 2 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD FEB PY 2012 VL 217 IS 2 SI SI BP 856 EP 862 DI 10.1016/j.icarus.2011.07.015 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878FE UT WOS:000299240100038 ER PT J AU Sornig, M Livengood, TA Sonnabend, G Stupar, D Kroetz, P AF Sornig, M. Livengood, T. A. Sonnabend, G. Stupar, D. Kroetz, P. TI Direct wind measurements from November 2007 in Venus' upper atmosphere using ground-based heterodyne spectroscopy of CO2 at 10 mu m wavelength SO ICARUS LA English DT Article DE Venus; Atmospheres, Dynamics; Infrared observations ID INFRARED OBSERVATIONS; GLOBAL CIRCULATION; MARTIAN ATMOSPHERE; THERMAL STRUCTURE; LINE OBSERVATIONS; UPPER MESOSPHERE; EMISSION-LINES; NATURAL LASER; EXPRESS; MARS AB Between November 23 and 28, 2007, the Cologne Tuneable Heterodyne Infrared Spectrometer THIS was installed at the McMath-Pierce Solar Telescope (Kitt Peak, Arizona, USA) to determine zonal wind velocities and to estimate the subsolar-to-antisolar flow. We investigate dynamics in the upper atmosphere of Venus by measuring the Doppler shift of fully-resolved non-LTE CO2 emission lines at 959.3917 cm(-1) (10.423 mu m), which probe a narrow altitude region in Venus' atmosphere around 110 +/- 10 km (similar to 1 mu bar). The results show no significant zonal wind velocity at the equator. An increase with latitude up to 43 +/- 13 m/s at a latitude of 33 degrees N was observed. This confirms the deduction of a minor influence of Venus superrotation at an altitude of 110 km from previous measurements in May 2007 (Sornig et al., 2008). The specific observing geometry enables estimating the maximum cross terminator velocity of the subsolar-to-antisolar flow at 72 +/- 47 m/s. (C) 2011 Elsevier Inc. All rights reserved. C1 [Sornig, M.] Univ Cologne, Rhein Inst Umweltforsch, Abt Planetenforsch, D-50931 Cologne, Germany. [Livengood, T. A.] NASA GSFC, Greenbelt, MD 20771 USA. [Livengood, T. A.] NCESSE, Capital Hts, MD 20791 USA. [Sonnabend, G.; Stupar, D.; Kroetz, P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Sornig, M (reprint author), Univ Cologne, Rhein Inst Umweltforsch, Abt Planetenforsch, Aachener Str 209, D-50931 Cologne, Germany. EM sornig@ph1.uni-koeln.de; timothy.a.livengood@nasa.gov; samstag@ph1.uni-koeln.de; stupar@ph1.uni-koeln.de; kroetz@ph1.uni-koeln.de RI Livengood, Timothy/C-8512-2012 FU Europlanet; Deutsche Forschungsgemeinschaft (DFG) [SO879/1-1] FX This work was supported by Europlanet and the Deutsche Forschungsgemeinschaft (DFG) special Grant SO879/1-1. NR 49 TC 8 Z9 8 U1 2 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD FEB PY 2012 VL 217 IS 2 SI SI BP 863 EP 874 DI 10.1016/j.icarus.2011.03.019 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878FE UT WOS:000299240100039 ER PT J AU Raney, RK Freeman, A Jordan, RL AF Raney, Russell Keith Freeman, Anthony Jordan, Rolando L. TI Improved Range Ambiguity Performance in Quad-Pol SAR SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Ambiguities; circular polarization; hybrid polarity; quadrature polarimetric (quad-pol); synthetic aperture radar (SAR) ID CALIBRATION; ANTENNA AB Conventional quadrature-polarimetric (quad-pol) synthetic aperture radar (SAR) systems operating from space are severely constrained by their limited range of useful incident angles and their reduced swath widths particularly at larger incidence. These limitations are due primarily to relatively severe range ambiguities in the cross-polarized measurement channels. The conventional approach for quad-pol SAR systems uses linear polarizations on both transmit and receive. Range ambiguities can be markedly reduced by adopting hybrid-polarimetric architecture. In this approach, the radar transmits circularly polarized waves but receives on orthogonal linear polarizations. The sense of the circular polarization-left or right-is reversed on alternate transmissions. Hybrid-polarimetric quad-pol architecture leads to hardware that is more readily calibrated because neither receive channel is cross polarized with respect to the transmitted polarization; hence, their mean signal levels are the same. The data provided by a hybrid-polarimetric quad-pol SAR may be transformed into the conventional linearly polarized scattering matrix, thus preserving compatibility with the rich heritage of analysis tools developed for such radars. C1 [Raney, Russell Keith] Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 20723 USA. [Freeman, Anthony; Jordan, Rolando L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Raney, RK (reprint author), Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 20723 USA. EM keith.raney@jhuapl.edu; Anthony.Freeman@jpl.nasa.gov; Rolando.jordan@jpl.nasa.gov FU National Aeronautics and Space Administration FX This work was supported in part by the National Aeronautics and Space Administration. NR 17 TC 10 Z9 13 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD FEB PY 2012 VL 50 IS 2 BP 349 EP 356 DI 10.1109/TGRS.2011.2121075 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 880UJ UT WOS:000299432900003 ER PT J AU Kleidman, RG Smirnov, A Levy, RC Mattoo, S Tanre, D AF Kleidman, Richard G. Smirnov, Alexander Levy, Robert C. Mattoo, Shana Tanre, Didier TI Evaluation and Wind Speed Dependence of MODIS Aerosol Retrievals Over Open Ocean SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Aerosols; remote sensing ID OPTICAL-THICKNESS RETRIEVALS; TROPOSPHERIC AEROSOLS; SIZE DISTRIBUTION; SUN PHOTOMETER; VALIDATION; SATELLITE; PRODUCT; DEPTH; ATLANTIC; SPACE AB The Maritime Aerosol Network (MAN) data set provides high-quality ground truth to validate the Moderate Resolution Imaging Spectroradiometer (MODIS) aerosol product over open ocean. Prior validation of the ocean aerosol product has been limited to coastal and island sites. Comparing MODIS Collection 5 ocean aerosol retrieval products with collocated MAN measurements from ships shows that MODIS is meeting the prelaunch uncertainty estimates for aerosol optical depth (AOD) with 64% and 67% of retrievals at 550 nm and 74% and 78% of retrievals at 870 nm, falling within expected uncertainty for Terra and Aqua, respectively. Angstrom exponent comparisons show a high correlation between MODIS retrievals and shipboard measurements (R = 0.85 for Terra and 0.83 for Aqua), although the MODIS aerosol algorithm tends to underestimate particle size for large particles and overestimate size for small particles, as seen in earlier collections. Prior analysis noted an offset between Terra and Aqua ocean AODs, without concluding which sensor was more accurate. The simple linear regression reported here is consistent with other anecdotal evidence that Aqua agreement with the Aerosol Robotic Network is marginally better. However, we cannot claim based on the current study that the better Aqua comparison is statistically significant. A systematic increase of error as a function of wind speed is noted in both Terra and Aqua retrievals. This wind speed dependence enters the retrieval when winds deviate from the 6-m/s value assumed in the rough ocean surface and white cap parameterizations. Wind speed dependence in the results can be mitigated by using auxiliary National Centers for Environmental Prediction wind speed information in the retrieval process. C1 [Kleidman, Richard G.; Levy, Robert C.; Mattoo, Shana] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Kleidman, Richard G.; Levy, Robert C.; Mattoo, Shana] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smirnov, Alexander] Sigma Space Corp, Lanham, MD 20706 USA. [Smirnov, Alexander] NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tanre, Didier] Univ Lille, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France. RP Kleidman, RG (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM Richard.Kleidman@nasa.gov; Alexander.Smirnov-1@nasa.gov; robert.c.levy@nasa.gov; Shana.Mattoo@nasa.gov; didier.tanre@univ-lille1.fr RI Smirnov, Alexander/C-2121-2009; Levy, Robert/M-7764-2013 OI Smirnov, Alexander/0000-0002-8208-1304; Levy, Robert/0000-0002-8933-5303 FU National Aeronautics and Space Administration [06-EOS/06-1037] FX This work was supported by the National Aeronautics and Space Administration Climate and Radiation Research and Analysis Program managed by H. Maring under Grant 06-EOS/06-1037. NR 47 TC 14 Z9 15 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 FEB PY 2012 VL 50 IS 2 BP 429 EP 435 DI 10.1109/TGRS.2011.2162073 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 880UJ UT WOS:000299432900011 ER PT J AU Colliander, A McDonald, K Zimmermann, R Schroeder, R Kimball, JS Njoku, EG AF Colliander, Andreas McDonald, Kyle Zimmermann, Reiner Schroeder, Ronny Kimball, John S. Njoku, Eni G. TI Application of QuikSCAT Backscatter to SMAP Validation Planning: Freeze/Thaw State Over ALECTRA Sites in Alaska From 2000 to 2007 SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Alaska Ecological Transect (ALECTRA); freeze/thaw state; Quick Scatterometer (QuikSCAT); Soil Moisture Active Passive (SMAP) ID NASA SCATTEROMETER NSCAT; LANDSCAPE; SEASONS; BOREAL; CYCLES; FROZEN; SOIL; SAR AB The mapping of the predominant freeze/thaw state of the landscape is one of the main objectives of the National Aeronautics and Space Administration's proposed Soil Moisture Active Passive (SMAP) mission. This study applies Alaska Ecological Transect (ALECTRA) biophysical network temperature measurements and satellite radar scatterometer data from the Quick Scatterometer (QuikSCAT) to evaluate some of the validation issues regarding the planned SMAP freeze/thaw measurements. Although the QuikSCAT data are acquired at Ku-band frequency, rather than at the L-band frequency of the proposed SMAP instrument, QuikSCAT data do provide a high temporal fidelity over the ALECTRA sites, similar to SMAP. The results of this study show that multiple temperature measurements representative of individual landscape components (soil, snow cover, vegetation, and atmosphere) covering different types of terrain within the satellite field of view are important for understanding the freeze/thaw process and the aggregate radar backscatter response to that process. The backscatter temporal dynamics and relative contribution of the freeze/thaw state of these landscape elements to radar signal vary with land cover, seasonal weather, and climate conditions. C1 [Colliander, Andreas; McDonald, Kyle; Schroeder, Ronny; Njoku, Eni G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [McDonald, Kyle] CUNY City Coll, Dept Earth & Atmospher Sci, New York, NY 10031 USA. [Zimmermann, Reiner] Univ Hohenheim, Inst Bot & Bot Gardens, D-70593 Stuttgart, Germany. [Schroeder, Ronny] CUNY City Coll, Cooperat Remote Sensing Sci & Technol Ctr CREST I, New York, NY 10031 USA. [Kimball, John S.] Univ Montana, Coll Forestry & Conservat, Missoula, MT 59812 USA. RP Colliander, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM andreas.colliander@jpl.nasa.gov; kmcdonald2@ccny.cuny.edu; rzimmerm@uni-hohenheim.de; ronny.schroeder@jpl.nasa.gov; johnk@ntsg.umt.edu; eni.g.njoku@jpl.nasa.gov FU National Aeronautics and Space Administration FX The authors would like to thank T. Linke for his assistance in processing the Alaska Ecological Transect data. The work described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, under a contract with the National Aeronautics and Space Administration. NR 17 TC 10 Z9 10 U1 0 U2 13 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD FEB PY 2012 VL 50 IS 2 BP 461 EP 468 DI 10.1109/TGRS.2011.2174368 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 880UJ UT WOS:000299432900014 ER PT J AU Roberts, JB Robertson, FR Clayson, CA Bosilovich, MG AF Roberts, J. Brent Robertson, Franklin R. Clayson, Carol A. Bosilovich, Michael G. TI Characterization of Turbulent Latent and Sensible Heat Flux Exchange between the Atmosphere and Ocean in MERRA SO JOURNAL OF CLIMATE LA English DT Article ID AIR-SEA FLUXES; BULK AERODYNAMIC ALGORITHMS; WIND STRESS; SURFACE METEOROLOGY; RESPONSE EXPERIMENT; EQUATORIAL PACIFIC; REANALYSIS PROJECT; GLOBAL ENERGY; NCEP-NCAR; ATLANTIC AB Turbulent fluxes of heat and moisture across the atmosphere ocean interface are fundamental components of the earth's energy and water balance. Characterizing both the spatiotemporal variability and the fidelity of these exchanges of heat and moisture is critical to understanding the global water and energy cycle variations, quantifying atmosphere ocean feedbacks, and improving model predictability. This study examines the veracity of the recently completed NASA Modern-Era Retrospective Analysis for Research and Applications (MERRA) product in terms of its turbulent surface fluxes. This assessment employs a large dataset of directly measured turbulent fluxes as well as other turbulent surface flux datasets. The spatial and temporal variability of the surface fluxes are examined in terms of their annual-mean climatologies, their seasonal covariability of near-surface bulk parameters, and their representation of extremes. The impact of data assimilation on the near-surface parameters is assessed through evaluation of the incremental analysis update tendencies. It is found that MERRA turbulent surface fluxes are relatively accurate for typical conditions but have systematically weak vertical gradients in moisture and temperature and a weaker covariability between the near-surface gradients and wind speed than found in observations. This results in an underestimate of the surface latent and sensible heat fluxes over the western boundary current and storm-track regions. The assimilation of observations generally acts to bring MERRA closer to observational products by increasing moisture and temperature near the surface and decreasing the near-surface wind speeds. C1 [Roberts, J. Brent; Robertson, Franklin R.] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35805 USA. [Clayson, Carol A.] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA. [Clayson, Carol A.] Florida State Univ, Inst Geophys Fluid Dynam, Tallahassee, FL 32306 USA. [Bosilovich, Michael G.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Roberts, JB (reprint author), NASA, George C Marshall Space Flight Ctr, Earth Sci Off, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM jason.b.roberts@nasa.gov RI Bosilovich, Michael/F-8175-2012 NR 56 TC 9 Z9 10 U1 1 U2 11 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD FEB 1 PY 2012 VL 25 IS 3 BP 821 EP 838 DI 10.1175/JCLI-D-11-00029.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 885SG UT WOS:000299800500001 ER PT J AU Wiese, DN Nerem, RS Lemoine, FG AF Wiese, D. N. Nerem, R. S. Lemoine, F. G. TI Design considerations for a dedicated gravity recovery satellite mission consisting of two pairs of satellites SO JOURNAL OF GEODESY LA English DT Article DE Time variable gravity; GRACE; Temporal aliasing errors; Constellations; Satellite geodesy ID LOCALIZED SPECTRAL-ANALYSIS; GRACE MEASUREMENTS; CLIMATE EXPERIMENT; FIELD MODELS; GLOBAL OCEAN; VARIABILITY; ASSIMILATION; SYSTEM; SPHERE; TIDES AB Future satellite missions dedicated to measuring time-variable gravity will need to address the concern of temporal aliasing errors; i.e., errors due to high-frequency mass variations. These errors have been shown to be a limiting error source for future missions with improved sensors. One method of reducing them is to fly multiple satellite pairs, thus increasing the sampling frequency of the mission. While one could imagine a system architecture consisting of dozens of satellite pairs, this paper explores the more economically feasible option of optimizing the orbits of two pairs of satellites. While the search space for this problem is infinite by nature, steps have been made to reduce it via proper assumptions regarding some parameters and a large number of numerical simulations exploring appropriate ranges for other parameters. A search space originally consisting of 15 variables is reduced to two variables with the utmost impact on mission performance: the repeat period of both pairs of satellites (shown to be near-optimal when they are equal to each other), as well as the inclination of one of the satellite pairs (the other pair is assumed to be in a polar orbit). To arrive at this conclusion, we assume circular orbits, repeat groundtracks for both pairs of satellites, a 100-km inter-satellite separation distance, and a minimum allowable operational satellite altitude of 290 km based on a projected 10-year mission lifetime. Given the scientific objectives of determining time-variable hydrology, ice mass variations, and ocean bottom pressure signals with higher spatial resolution, we find that an optimal architecture consists of a polar pair of satellites coupled with a pair inclined at 72A degrees, both in 13-day repeating orbits. This architecture provides a 67% reduction in error over one pair of satellites, in addition to reducing the longitudinal striping to such a level that minimal post-processing is required, permitting a substantial increase in the spatial resolution of the gravity field products. It should be emphasized that given different sets of scientific objectives for the mission, or a different minimum allowable satellite altitude, different architectures might be selected. C1 [Wiese, D. N.; Nerem, R. S.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. [Lemoine, F. G.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Wiese, DN (reprint author), Univ Colorado, Colorado Ctr Astrodynam Res, 431 UCB, Boulder, CO 80309 USA. EM wiese@colorado.edu; nerem@colorado.edu; frank.g.lemoine@nasa.gov RI Lemoine, Frank/D-1215-2013 FU National Science Foundation; National Defense Science and Engineering Graduate Fellowship Program; NASA GRACE Science Team investigation [NNX08AH63G] FX This research was funded by the National Science Foundation Graduate Fellowship Program, the National Defense Science and Engineering Graduate Fellowship Program, and the NASA GRACE Science Team investigation (NNX08AH63G). The authors would like to thank NASA Goddard Space Flight Center for providing GEODYN and SOLVEto perform the numerical simulations, along with the NCEP model. We acknowledge Jean-Paul Boy (EOST/University of Strasbourg, France) for providing the ECMWF-derived and MOG-2D-derived datasets in this study to GSFC. Additionally, we thank ESA and the Institute of Astronomical and Physical Geodesy (IAPG) at the Technical University of Munich for providing the ice model used in the simulations. NR 44 TC 20 Z9 22 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 FEB PY 2012 VL 86 IS 2 BP 81 EP 98 DI 10.1007/s00190-011-0493-8 PG 18 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA 881XH UT WOS:000299524800001 ER PT J AU Davis, CJ Davies, JA St Cyr, OC Campbell-Brown, M Skelt, A Kaiser, M Meyer-Vernet, N Crothers, S Lintott, C Smith, A Bamford, S Baeten, EML AF Davis, C. J. Davies, J. A. St Cyr, O. C. Campbell-Brown, M. Skelt, A. Kaiser, M. Meyer-Vernet, Nicole Crothers, S. Lintott, C. Smith, A. Bamford, S. Baeten, E. M. L. TI The distribution of interplanetary dust between 0.96 and 1.04 au as inferred from impacts on the STEREO spacecraft observed by the heliospheric imagers SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Sun: heliosphere; solar-terrestrial relations; meteorites, meteors, meteoroids; zodiacal dust ID METEOR ORBIT RADAR; RADIO; RADIANTS; S/WAVES; MISSION; SECCHI AB The distribution of dust in the ecliptic plane between 0.96 and 1.04 au has been inferred from impacts on the two Solar Terrestrial Relations Observatory (STEREO) spacecraft through observation of secondary particle trails and unexpected off-points in the heliospheric imager (HI) cameras. This study made use of analysis carried out by members of a distributed web-based citizen science project Solar Stormwatch. A comparison between observations of the brightest particle trails and a survey of fainter trails shows consistent distributions. While there is no obvious correlation between this distribution and the occurrence of individual meteor streams at Earth, there are some broad longitudinal features in these distributions that are also observed in sources of the sporadic meteor population. The different position of the HI instrument on the two STEREO spacecraft leads to each sampling different populations of dust particles. The asymmetry in the number of trails seen by each spacecraft and the fact that there are many more unexpected off-points in the HI-B than in HI-A indicates that the majority of impacts are coming from the apex direction. For impacts causing off-points in the HI-B camera, these dust particles are estimated to have masses in excess of 10-17 kg with radii exceeding 0.1 mu m. For off-points observed in the HI-A images, which can only have been caused by particles travelling from the anti-apex direction, the distribution is consistent with that of secondary 'storm' trails observed by HI-B, providing evidence that these trails also result from impacts with primary particles from an anti-apex source. Investigating the mass distribution for the off-points of both HI-A and HI-B, it is apparent that the differential mass index of particles from the apex direction (causing off-points in HI-B) is consistently above 2. This indicates that the majority of the mass is within the smaller particles of this population. In contrast, the differential mass index of particles from the anti-apex direction (causing off-points in HI-A) is consistently below 2, indicating that the majority of the mass is to be found in larger particles of this distribution. C1 [Davis, C. J.; Davies, J. A.; Skelt, A.; Crothers, S.] Rutherford Appleton Lab, RAL Space, Chilton OX11 0DQ, Oxon, England. [Davis, C. J.] Univ Reading, Dept Meteorol, Reading RG6 7BE, Berks, England. [St Cyr, O. C.; Kaiser, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Campbell-Brown, M.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 5B8, Canada. [Skelt, A.] Faringdon Community Coll, Farringdon SN7 7CB, Oxon, England. [Meyer-Vernet, Nicole] Observ Paris, F-92195 Meudon, France. [Lintott, C.; Smith, A.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Lintott, C.; Smith, A.] Adler Planetarium, Chicago, IL 60605 USA. [Bamford, S.] Univ Nottingham, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England. [Baeten, E. M. L.] Zooniverse, Dept Astrophys, Oxford OX1 3RH, England. RP Davis, CJ (reprint author), Rutherford Appleton Lab, RAL Space, Chilton OX11 0DQ, Oxon, England. EM chris.davis@stfc.ac.uk RI Scott, Christopher/H-8664-2012; Bamford, Steven/E-8702-2010; OI Scott, Christopher/0000-0001-6411-5649; Bamford, Steven/0000-0001-7821-7195; Smith, Arfon/0000-0002-3957-2474 FU UK Space Agency; Leverhulme Trust FX The UK STEREO group is supported by funding from the UK Space Agency. Solar Stormwatch is a collaborative project between the Zooniverse team, the Royal Observatory Greenwich and the Science and Technology Facilities Council. The Zooniverse is supported by the Leverhulme Trust. The STEREO heliospheric imagers are supported by the UK Space Agency. STEREO HI data are made available via the UK Solar System Data Centre (www.ukssdc.ac.uk). NR 23 TC 9 Z9 9 U1 0 U2 13 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 420 IS 2 BP 1355 EP 1366 DI 10.1111/j.1365-2966.2011.20125.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880OU UT WOS:000299417600033 ER PT J AU Mandelbaum, R Hirata, CM Leauthaud, A Massey, RJ Rhodes, J AF Mandelbaum, Rachel Hirata, Christopher M. Leauthaud, Alexie Massey, Richard J. Rhodes, Jason TI Precision simulation of ground-based lensing data using observations from space SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; methods: data analysis; techniques: image processing; galaxies: structure ID DIGITAL SKY SURVEY; SPECTROSCOPIC TARGET SELECTION; IMAGE-ANALYSIS COMPETITION; TELESCOPE ADVANCED CAMERA; GALAXY CLUSTERS; DATA RELEASE; GREAT08 CHALLENGE; ELLIPTIC GALAXIES; SHAPE MEASUREMENT; COSMIC SHEAR AB Current and upcoming wide-field, ground-based, broad-band imaging surveys promise to address a wide range of outstanding problems in galaxy formation and cosmology. Several such uses of ground-based data, especially weak gravitational lensing, require highly precise measurements of galaxy image statistics with careful correction for the effects of the point spread function (PSF). In this paper, we introduce the shera (SHEar Reconvolution Analysis) software to simulate ground-based imaging data with realistic galaxy morphologies and observing conditions, starting from space-based data (from the Cosmological Evolution Survey, COSMOS) and accounting for the effects of the space-based PSF. This code simulates ground-based data, optionally with a weak lensing shear applied, in a model-independent way using a general Fourier space formalism. The utility of this pipeline is that it allows for a precise, realistic assessment of systematic errors due to the method of data processing, for example in extracting weak lensing galaxy shape measurements or galaxy radial profiles, given user-supplied observational conditions and real galaxy morphologies. Moreover, the simulations allow for the empirical test of error estimates and determination of parameter degeneracies, via generation of many noise maps. The public release of this software, along with a large sample of cleaned COSMOS galaxy images (corrected for charge transfer inefficiency), should enable upcoming ground-based imaging surveys to achieve their potential in the areas of precision weak lensing analysis, galaxy profile measurement and other applications involving detailed image analysis. C1 [Mandelbaum, Rachel] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Hirata, Christopher M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Leauthaud, Alexie] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Massey, Richard J.] Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mandelbaum, R (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. EM rmandelb@astro.princeton.edu RI Mandelbaum, Rachel/N-8955-2014 OI Mandelbaum, Rachel/0000-0003-2271-1527 FU US National Science Foundation [AST-0807337]; US Department of Energy [DE-FG03-02-ER40701]; Alfred P. Sloan Foundation; David and Lucile Packard Foundation; LBNL; Berkeley Center for Cosmological Physics; STFC [PP/E006450/1]; ERC [MIRG-CT-208994]; NASA FX We thank the referee for many constructive comments about the organization and content of this paper. The authors would also like to thank Jim Gunn, Robert Lupton, Dustin Lang, David Hogg, Michael Blanton, Barney Rowe, Peter Capak, Chiaki Hikage, Uros Seljak and Gary Bernstein for useful conversations about this project, and Eric Huff both for discussing it and giving the software a name. CMH is supported by the US National Science Foundation (AST-0807337), the US Department of Energy (DE-FG03-02-ER40701), the Alfred P. Sloan Foundation, and the David and Lucile Packard Foundation. AL acknowledges support from the Chamberlain Fellowship at LBNL and from the Berkeley Center for Cosmological Physics. RJM is supported by STFC Advanced Fellowship #PP/E006450/1 and ERC grant MIRG-CT-208994. This work was done in part at JPL, run under a contract for NASA by Caltech. NR 83 TC 38 Z9 38 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 420 IS 2 BP 1518 EP 1540 DI 10.1111/j.1365-2966.2011.20138.x PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880OU UT WOS:000299417600046 ER PT J AU Sundqvist, JO Owocki, SP Cohen, DH Leutenegger, MA Townsend, RHD AF Sundqvist, Jon O. Owocki, Stanley P. Cohen, David H. Leutenegger, Maurice A. Townsend, Richard H. D. TI A generalized porosity formalism for isotropic and anisotropic effective opacity and its effects on X-ray line attenuation in clumped O star winds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE line: profiles; radiative transfer; stars: early-type; stars: mass-loss; stars: winds, outflows; X-rays: stars ID DRIVEN STELLAR WINDS; MASS-LOSS RATE; ZETA-PUPPIS; EMISSION; PROFILES; SPECTROSCOPY; INSTABILITY; SIMULATIONS; CONSTRAINTS; ABSORPTION AB We present a generalized formalism for treating the porosity-associated reduction in continuum opacity that occurs when individual clumps in a stochastic medium become optically thick. As in previous work, we concentrate on developing bridging laws between the limits of optically thin and thick clumps. We consider geometries resulting in either isotropic or anisotropic effective opacity, and, in addition to an idealized model in which all clumps have the same local overdensity and scale, we also treat an ensemble of clumps with optical depths set by Markovian statistics. This formalism is then applied to the specific case of boundfree absorption of X-rays in hot star winds, a process not directly affected by clumping in the optically thin limit. We find that the Markov model gives surprisingly similar results to those found previously for the single-clump model, suggesting that porous opacity is not very sensitive to details of the assumed clump distribution function. Further, an anisotropic effective opacity favours escape of X-rays emitted in the tangential direction (the venetian blind effect), resulting in a bump of higher flux close to line centre as compared to profiles computed from isotropic porosity models. We demonstrate how this characteristic line shape may be used to diagnose the clump geometry, and we confirm previous results that for optically thick clumping to significantly influence X-ray line profiles, very large porosity lengths, defined as the mean free path between clumps, are required. Moreover, we present the first X-ray line profiles computed directly from line-driven instability simulations using a 3D patch method, and find that porosity effects from such models also are very small. This further supports the view that porosity has, at most, a marginal effect on X-ray line diagnostics in O stars, and therefore that these diagnostics do indeed provide a good clumping insensitive method for deriving O star mass-loss rates. C1 [Sundqvist, Jon O.; Owocki, Stanley P.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Cohen, David H.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Leutenegger, Maurice A.] NASA, GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Leutenegger, Maurice A.] NASA, GSFC, CRESST, Greenbelt, MD 20771 USA. [Leutenegger, Maurice A.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Townsend, Richard H. D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Sundqvist, JO (reprint author), Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. EM jon@bartol.udel.edu FU NASA ATP [NNX11AC40G]; NASA ADAP [NNX11AD26G] FX This work was supported in part by NASA ATP grant NNX11AC40G. DHC acknowledges support from NASA ADAP grant NNX11AD26G to Swarthmore College. We thank A. Feldmeier for providing the instability simulations discussed in Section 5, and for suggesting the exploration of Markov models discussed in Section 6. NR 35 TC 17 Z9 17 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 FEB PY 2012 VL 420 IS 2 BP 1553 EP 1561 DI 10.1111/j.1365-2966.2011.20141.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880OU UT WOS:000299417600048 ER PT J AU Guan, B Waliser, DE Molotch, NP Fetzer, EJ Neiman, PJ AF Guan, Bin Waliser, Duane E. Molotch, Noah P. Fetzer, Eric J. Neiman, Paul J. TI Does the Madden-Julian Oscillation Influence Wintertime Atmospheric Rivers and Snowpack in the Sierra Nevada? SO MONTHLY WEATHER REVIEW LA English DT Article ID EXTREME PRECIPITATION; CALIFORNIA; SATELLITE; RETRIEVALS; WASHINGTON; REANALYSIS; MOUNTAINS; FREQUENCY; CALJET; FLOODS AB The relationships between the Madden-Julian oscillation (MJO), activities of atmospheric rivers (ARs), and the resulting snowpack accumulation in the California Sierra Nevada, are analyzed based on 13 yr of observations for water years 1998-2010 inclusive. The AR activity, as measured by the number of high-impact ARs, mean per event snow water equivalent (SWE) changes, and the cumulative SWE changes, is shown to be significantly augmented when MJO convection is active over the far western tropical Pacific (phase 6 on the Wheeler-Hendon diagram). The timing of high-impact ARs (early- versus late-winter occurrences) also appears to be regulated by the MJO. Total snow accumulation in the Sierra Nevada (i.e., AR and non-AR accumulation combined) is most significantly increased when MJO convection is active over the eastern Indian Ocean (phase 3), and reduced when MJO convection is active over the Western Hemisphere (phase 8), with the magnitude of the daily anomaly being roughly half the cold-season mean daily snow accumulation over many snow sensor sites. The positive (negative) SWE anomaly is accompanied by a cold (warm) surface air temperature (SAT) anomaly and an onshore (offshore) water vapor flux anomaly. The contrasting SAT anomaly patterns associated with MJO phases 3 and 8, revealed by the in situ observations, are more realistically represented in the Atmospheric Infrared Sounder retrievals than in the European Centre for Medium-Range Weather Forecasts Interim reanalysis. C1 [Guan, Bin; Waliser, Duane E.; Molotch, Noah P.; Fetzer, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA. [Molotch, Noah P.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Neiman, Paul J.] NOAA, Div Phys Sci, Earth Syst Res Lab, Boulder, CO USA. RP Guan, B (reprint author), CALTECH, Jet Prop Lab, M-S 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM bin.guan@jpl.nasa.gov RI Guan, Bin/F-6735-2010; Molotch, Noah/C-8576-2009 FU NASA [NNX08AH18G]; NSF [EAR 1032295]; ARRA; Water Resources Area of the NASA FX This research was supported by NASA Grant NNX08AH18G, NSF Grant EAR 1032295, and by ARRA funds. Additional support was provided by the Water Resources Area of the NASA Applied Sciences Program. Thanks go to K. Weickmann, R. Wood, P. Webster, I.-S. Kang, J. Wallace, and G. Kiladis for helpful discussions and comments; and to F. Ralph for his encouragement. DEW's, EJF's, and BG's contribution, and part of NPM's contribution, 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 38 TC 31 Z9 31 U1 1 U2 26 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 EI 1520-0493 J9 MON WEATHER REV JI Mon. Weather Rev. PD FEB PY 2012 VL 140 IS 2 BP 325 EP 342 DI 10.1175/MWR-D-11-00087.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 886JI UT WOS:000299850300001 ER PT J AU Masson, S Aulanier, G Pariat, E Klein, KL AF Masson, S. Aulanier, G. Pariat, E. Klein, K. -L. TI Interchange Slip-Running Reconnection and Sweeping SEP Beams SO SOLAR PHYSICS LA English DT Article DE Flares: models; Flares: energetic particles; Magnetohydrodynamics ID SOLAR-ENERGETIC PARTICLES; QUASI-SEPARATRIX LAYERS; CURRENT SHEET FORMATION; SOFT-X-RAY; FLUX TUBES; MAGNETIC RECONNECTION; NULL-POINT; INNER HELIOSPHERE; ALFVEN WAVES; FIELD LINES AB We present a new model to explain how particles (solar energetic particles; SEPs), accelerated at a reconnection site that is not magnetically connected to the Earth, could eventually propagate along the well-connected open flux tube. Our model is based on the results of a low-beta resistive magnetohydrodynamics simulation of a three-dimensional line-tied and initially current-free bipole, which is embedded in a non-uniform open potential field. The topology of this configuration is that of an asymmetric coronal null point, with a closed fan surface and an open outer spine. When driven by slow photospheric shearing motions, field lines, initially fully anchored below the fan dome, reconnect at the null point, and jump to the open magnetic domain. This is the standard interchange mode as sketched and calculated in 2D. The key result in 3D is that reconnected open field lines located in the vicinity of the outer spine keep reconnecting continuously, across an open quasi-separatrix layer, as previously identified for non-open-null-point reconnection. The apparent slipping motion of these field lines leads to formation of an extended narrow magnetic flux tube at high altitude. Because of the slip-running reconnection, we conjecture that if energetic particles would be traveling through, or be accelerated inside, the diffusion region, they would be successively injected along continuously reconnecting field lines that are connected farther and farther from the spine. At the scale of the full Sun, owing to the super-radial expansion of field lines below 3 R (aS (TM)), such energetic particles could easily be injected in field lines slipping over significant distances, and could eventually reach the distant flux tube that is well-connected to the Earth. C1 [Masson, S.] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Aulanier, G.; Pariat, E.; Klein, K. -L.] Univ Paris Diderot, Observ Paris, CNRS, LESIA,UPMC, F-92190 Meudon, France. RP Masson, S (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM sophie.masson@nasa.gov FU Direction Generale de l'Armement (DGA); NASA at Goddard Space Flight Center; NASA; European Commission [MTRN-CT-2006-035484] FX The authors thank the referee for helpful comments, which improved the clarity of the paper. The MHD calculations were done on the quadri-core bi-Xeon computers of the Cluster of the Division Informatique de l'Observatoire de Paris (DIO). The work of S.M. is funded by a fellowship of Direction Generale de l'Armement (DGA). S.M. thank the NASA Postdoctoral Program at the Goddard Space Flight Center, administrated by Oak Ridge Associated Universities through a contract with NASA for financial support. Financial support by the European Commission through the FP6 SOLAIRE Network (MTRN-CT-2006-035484) is gratefully acknowledged. NR 50 TC 34 Z9 34 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD FEB PY 2012 VL 276 IS 1-2 BP 199 EP 217 DI 10.1007/s11207-011-9886-3 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YX UT WOS:000299295100012 ER PT J AU Thompson, WT Kliem, B Torok, T AF Thompson, W. T. Kliem, B. Toeroek, T. TI 3D Reconstruction of a Rotating Erupting Prominence SO SOLAR PHYSICS LA English DT Article DE Corona, active; Prominences, active; Coronal mass ejections; Initiation and propagation; Magnetic fields, corona ID CORONAL MASS EJECTION; CURRENT SHEET; FILAMENTS; HINODE; SOHO; TELESCOPE; HELICITY; MISSION; REGION; STEREO AB A bright prominence associated with a coronal mass ejection (CME) was seen erupting from the Sun on 9 April 2008. This prominence was tracked by both the Solar Terrestrial Relations Observatory (STEREO) EUVI and COR1 telescopes, and was seen to rotate about the line of sight as it erupted; therefore, the event has been nicknamed the "Cartwheel CME." The threads of the prominence in the core of the CME quite clearly indicate the structure of a weakly to moderately twisted flux rope throughout the field of view, up to heliocentric heights of 4 solar radii. Although the STEREO separation was 48A degrees, it was possible to match some sharp features in the later part of the eruption as seen in the 304 line in EUVI and in the H alpha-sensitive bandpass of COR1 by both STEREO Ahead and Behind. These features could then be traced out in three-dimensional space, and reprojected into a view in which the eruption is directed toward the observer. The reconstructed view shows that the alignment of the prominence to the vertical axis rotates as it rises up to a leading-edge height of a parts per thousand aEuro parts per thousand 2.5 solar radii, and then remains approximately constant. The alignment at 2.5 solar radii differs by about 115A degrees from the original filament orientation inferred from H alpha and EUV data, and the height profile of the rotation, obtained here for the first time, shows that two thirds of the total rotation are reached within a parts per thousand aEuro parts per thousand 0.5 solar radii above the photosphere. These features are well reproduced by numerical simulations of an unstable moderately twisted flux rope embedded in external flux with a relatively strong shear field component. C1 [Thompson, W. T.] NASA, Adnet Syst Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kliem, B.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Kliem, B.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Toeroek, T.] Univ Paris Diderot, Observ Paris, CNRS, LESIA,UPMC, F-92190 Meudon, France. RP Thompson, WT (reprint author), NASA, Adnet Syst Inc, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA. EM William.T.Thompson@nasa.gov RI Thompson, William/D-7376-2012 FU NASA [NNG06EB68C, NNX08AG44G]; DFG; STFC; European Commission through SOTERIA Network [218816]; NASA HTP; LWS FX We acknowledge the use of data provided by the Global High Resolution Ha Network, and by the SECCHI instruments on the STEREO spacecraft. Magnetic field extrapolations were supplied by the CCMC; special thanks to Lutz Rastaetter and Peter MacNeice for help with the CCMC data. We thank the anonymous referee for a constructive report which led to a deeper consideration of PIL orientation vs. height, and S. Patsourakos for information about his fitting of the CME orientation in the COR2 height range. WTT's work was supported by NASA Grant NNG06EB68C. BK's work was supported by the DFG, the STFC, and by NASA through Grant NNX08AG44G. TT's work was partially supported by the European Commission through the SOTERIA Network (EU FP7 Space Science Project No. 218816) and by the NASA HTP and LWS programs. NR 30 TC 23 Z9 23 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD FEB PY 2012 VL 276 IS 1-2 BP 241 EP 259 DI 10.1007/s11207-011-9868-5 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YX UT WOS:000299295100014 ER PT J AU Sheldon, JE Griffith, PC Peters, F Sheldon, WM Blanton, JO Amft, J Pomeroy, LR AF Sheldon, Joan E. Griffith, Peter C. Peters, Francesc Sheldon, Wade M., Jr. Blanton, Jackson O. Amft, Julie Pomeroy, Lawrence R. TI Southeastern USA continental shelf respiratory rates revisited SO BIOGEOCHEMISTRY LA English DT Article DE Microbial respiration; Southeastern U. S. continental shelf; Dissolved oxygen; Bacteria ID ATMOSPHERIC CO2; UNITED-STATES; WATERS; OCEAN; TRANSPORT; ESTUARINE; MARGINS; GEORGIA; CARBON; OXYGEN AB Respiratory rates on the U. S. southeastern continental shelf have been estimated several times by different investigators, most recently by Jiang et al. (Biogeochemistry 98:101-113, 2010) who report lower mean rates than were found in earlier work and attribute the differences to analytical error in all methods used in earlier studies. The differences are, instead, attributable to the differences in the geographical scope of the studies. The lower estimates of regional organic carbon flux of Jiang et al. (Biogeochemistry 98:101-113, 2010) are a consequence of their extrapolation of data from a small portion of the shelf to the entire South Atlantic Bight. This comment examines the methodologies used as well as the variability of respiratory rates in this region over space and time. C1 [Sheldon, Joan E.; Sheldon, Wade M., Jr.] Univ Georgia, Dept Marine Sci, Athens, GA 30602 USA. [Griffith, Peter C.] NASA Goddard Space Flight Ctr, Sigma Space Corp, Carbon Cycle & Ecosyst Off, Greenbelt, MD 20711 USA. [Peters, Francesc] CSIC, Inst Ciencies Mar, E-08003 Barcelona, Spain. [Blanton, Jackson O.; Amft, Julie] Skidaway Inst Oceanog, Savannah, GA 31411 USA. [Pomeroy, Lawrence R.] Univ Georgia, Inst Ecol, Athens, GA 30602 USA. RP Sheldon, JE (reprint author), Univ Georgia, Dept Marine Sci, Athens, GA 30602 USA. EM jsheldon@uga.edu RI Peters, Francesc/A-6364-2009; Griffith, Peter/I-1392-2016 OI Peters, Francesc/0000-0001-9405-4306; Griffith, Peter/0000-0002-4267-7429 FU National Science Foundation [0620959] FX J. E. Sheldon and W. M. Sheldon, Jr. were supported by the Georgia Coastal Ecosystems Long-Term Ecological Research program (National Science Foundation award number 0620959). NR 29 TC 1 Z9 1 U1 0 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-2563 J9 BIOGEOCHEMISTRY JI Biogeochemistry PD FEB PY 2012 VL 107 IS 1-3 BP 501 EP 506 DI 10.1007/s10533-010-9552-0 PG 6 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 864GV UT WOS:000298226700031 ER PT J AU Yoo, SW Chaudhuri, S Sacksteder, KR Zhang, P Zhu, DL Law, CK AF Yoo, Sean W. Chaudhuri, Swetaprovo Sacksteder, Kurt R. Zhang, Peng Zhu, Delin Law, Chung K. TI Response of spherical diffusion flames subjected to rotation: Microgravity experimentation and computational simulation SO COMBUSTION AND FLAME LA English DT Article DE Rotating spherical diffusion flame ID COMBUSTION; DROPLET AB Microgravity experiments were conducted in the 2.2-s drop tower and zero-gravity facility at NASA-GRC to gain fundamental understanding of the effects of spinning on an otherwise spherical diffusion flame. The flames were generated by injecting either a fuel or an oxidizer mixture from a porous burner to a controlled ambient of either an oxidizer or fuel mixture, respectively. Results show that the polar flame location scales with the angular velocity monotonically as omega(a), where a is greater and smaller than unity for small and large spinning velocities, respectively. On the contrary, the equatorial flame location responds nonmonotonically to increasing spinning velocity: first increasing and then decreasing. The experimental observations agree well with the computational simulation where the simulated results demonstrate that the nonmonotonic response of the equatorial flame location is caused by dilution of the reactant concentration in the outwardly-directed radial flow by the product and inert that are carried by the inwardly-directed polar flow upon traversing the flame segment in the polar region. (C) 2011 The Combustion Institute. Published by Elsevier Inc. All rights reserved. C1 [Yoo, Sean W.; Chaudhuri, Swetaprovo; Zhang, Peng; Zhu, Delin; Law, Chung K.] Princeton Univ, Dept Mech & Aerosp Engn, Princeton, NJ 08544 USA. [Sacksteder, Kurt R.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Chaudhuri, S (reprint author), Princeton Univ, Dept Mech & Aerosp Engn, Princeton, NJ 08544 USA. EM sweto@princeton.edu RI Chaudhuri, Swetaprovo/C-6542-2008; Law, Chung /E-1206-2013; OI Chaudhuri, Swetaprovo/0000-0003-2294-5534; Zhang, Peng/0000-0002-1806-4200; Chaudhuri, Swetaprovo/0000-0003-4109-8633 FU NASA; NASA GSRP FX This work was supported by the NASA Microgravity Combustion Program and a NASA GSRP fellowship program to S.W.Y. The authors would like to acknowledge the assistance of Dr. P. Ferkul, as well as all personnel at the 2.2-second drop tower and Zero-G facility at NASA Glenn Research Center. NR 13 TC 0 Z9 0 U1 0 U2 10 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0010-2180 J9 COMBUST FLAME JI Combust. Flame PD FEB PY 2012 VL 159 IS 2 BP 665 EP 672 DI 10.1016/j.combustflame.2011.07.013 PG 8 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA 875XJ UT WOS:000299068200017 ER PT J AU Simon, TA Ward, WA Boss, AP AF Simon, Tyler A. Ward, William A., Jr. Boss, Alan P. TI Performance analysis of Intel multiprocessors using astrophysics simulations SO CONCURRENCY AND COMPUTATION-PRACTICE & EXPERIENCE LA English DT Article; Proceedings Paper CT Conference on Frontiers of Multicore Computing CY AUG, 2010 CL Univ Maryland, Baltimore County, Catonsville, MD HO Univ Maryland, Baltimore County DE FLASH; performance analysis; multicore ID THERMONUCLEAR FLASHES; REFINEMENT; BENCHMARK; CODE AB This paper provides a performance evaluation and investigation of the astrophysics code FLASH for a variety of Intel multiprocessors. This work was performed at the NASA Center for Computational Sciences (NCCS) on behalf of the Carnegie Institution of Washington (CIW) as a study preliminary to the acquisition of a high-performance computing (HPC) system at the CIW and for the NCCS itself to measure the relative performance of a recently acquired Intel Nehalem-based system against previously installed multicore HPC resources. A brief overview of computer performance evaluation is provided, followed by a description of the systems under test, a description of the FLASH test problem, and the test results. Additionally, the paper characterizes some of the effects of load imbalance imposed by adaptive mesh refinement. Copyright (C) 2012 John Wiley & Sons, Ltd. C1 [Simon, Tyler A.] NASA, Ctr Climate Simulat, Goddard Space Flight Ctr, Greenbelt, MD 20706 USA. [Ward, William A., Jr.] DoD High Performance Comp Modernizat Program, Lorton, VA USA. [Boss, Alan P.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC USA. RP Simon, TA (reprint author), NASA, Ctr Climate Simulat, Goddard Space Flight Ctr, Greenbelt, MD 20706 USA. EM tyler.simon@nasa.gov RI novacescu, florica/B-4503-2011 OI novacescu, florica/0000-0001-5561-4956 NR 28 TC 3 Z9 3 U1 0 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1532-0626 J9 CONCURR COMP-PRACT E JI Concurr. Comput.-Pract. Exp. PD FEB PY 2012 VL 24 IS 2 SI SI BP 155 EP 166 DI 10.1002/cpe.1888 PG 12 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA 877RW UT WOS:000299201000005 ER PT J AU Veraverbeke, S Somers, B Gitas, I Katagis, T Polychronaki, A Goossens, R AF Veraverbeke, S. Somers, B. Gitas, I. Katagis, T. Polychronaki, A. Goossens, R. TI Spectral mixture analysis to assess post-fire vegetation regeneration using Landsat Thematic Mapper imagery: Accounting for soil brightness variation SO INTERNATIONAL JOURNAL OF APPLIED EARTH OBSERVATION AND GEOINFORMATION LA English DT Article DE Fire; Vegetation recovery; Landsat Thematic Mapper; Spectral mixture analysis; MESMA; Segmentation ID 2007 PELOPONNESE WILDFIRES; SANTA-MONICA MOUNTAINS; LEAF-AREA INDEX; BURN SEVERITY; SOUTHERN-CALIFORNIA; HYPERSPECTRAL DATA; ENDMEMBER VARIABILITY; MEDITERRANEAN BASIN; TIME-SERIES; FIRE AB Post-fire vegetation cover is a crucial parameter in rangeland management. This study aims to assess the post-fire vegetation recovery 3 years after the large 2007 Peloponnese (Greece) wildfires. Post-fire recovery landscapes typically are mixed vegetation-substrate environments which makes spectral mixture analysis (SMA) a very effective tool to derive fractional vegetation cover maps. Using a combination of field and simulation techniques this study aimed to account for the impact of background brightness variability on SMA model performance. The field data consisted out of a spectral library of in situ measured reflectance signals of vegetation and substrate and 78 line transect plots. In addition, a Landsat Thematic Mapper (TM) scene was employed in the study. A simple SMA, in which each constituting terrain feature is represented by its mean spectral signature, a multiple endmember SMA (MESMA) and a segmented SMA, which accounts for soil brightness variations by forcing the substrate endmember choice based on ancillary data (lithological map), were applied. In the study area two main spectrally different lithological units were present: relatively bright limestone and relatively dark flysch (sand-siltstone). Although the simple SMA model resulted in reasonable regression fits for the flysch and limestones subsets separately (coefficient of determination R-2 of respectively 0.67 and 0.72 between field and TM data), the performance of the regression model on the pooled dataset was considerably weaker (R-2=0.65). Moreover, the regression lines significantly diverged among the different subsets leading to systematic over-or underestimations of the vegetative fraction depending on the substrate type. MESMA did not solve the endmember variability issue. The MESMA model did not manage to select the proper substrate spectrum on a reliable basis due to the lack of shape differences between the flysch and limestone spectra,. The segmented SMA model which accounts for soil brightness variations minimized the variability problems. Compared to the simple SMA and MESMA models, the segmented SMA resulted in a higher overall correlation (R-2 = 0.70), its regression slope and intercept were more similar among the different substrate types and its resulting regression lines more closely resembled the expected one-one line. This paper demonstrates the improvement of a segmented approach in accounting for soil brightness variations in estimating vegetative cover using SMA. However, further research is required to evaluate the model's performance for other soil types, with other image data and at different post-fire timings. (C) 2011 Elsevier B.V. All rights reserved. C1 [Veraverbeke, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Veraverbeke, S.; Goossens, R.] Univ Ghent, Dept Geog, BE-9000 Ghent, Belgium. [Somers, B.] Flemish Inst Technol Res VITO, Ctr Remote Sensing & Earth Observat Proc TAP, BE-2400 Mol, Belgium. [Gitas, I.; Katagis, T.; Polychronaki, A.] Aristotle Univ Thessaloniki, Lab Forest Management & Remote Sensing, GR-54124 Thessaloniki, Greece. RP Veraverbeke, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,US-91109, Pasadena, CA 91109 USA. EM Sander.S.Veraverbeke@jpl.nasa.gov; ben.somers@vito.be; igitas@for.auth.gr; thkatag@for.auth.gr; anpolych@for.auth.gr; rudi.goossens@ugent.be RI Veraverbeke, Sander/H-2301-2012; Gitas, Ioannis/C-3329-2008 OI Veraverbeke, Sander/0000-0003-1362-5125; Gitas, Ioannis/0000-0003-0056-5629 FU Ghent University; National Aeronautics and Space Administration; Belgian Science Policy Office [SR/67/146] FX The study was financed by the Ghent University special research funds (BOF: Bijzonder Onderzoeksfonds). Part of the work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The contribution of Dr. Ben Somers is funded by the Belgian Science Policy Office in the frame of the STEREO II programme - project VEGEMIX (SR/67/146). NR 78 TC 18 Z9 19 U1 3 U2 40 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0303-2434 J9 INT J APPL EARTH OBS JI Int. J. Appl. Earth Obs. Geoinf. PD FEB PY 2012 VL 14 IS 1 BP 1 EP 11 DI 10.1016/j.jag.2011.08.004 PG 11 WC Remote Sensing SC Remote Sensing GA 871AB UT WOS:000298708900001 ER PT J AU Martin, AM Laporte, D Koga, KT Kawamoto, T Hammouda, T AF Martin, Audrey M. Laporte, Didier Koga, Kenneth T. Kawamoto, Tatsuhiko Hammouda, Tahar TI Experimental Study of the Stability of a Dolomite plus Coesite Assemblage in Contact With Peridotite: Implications for Sediment-Mantle Interaction and Diamond Formation During Subduction SO JOURNAL OF PETROLOGY LA English DT Article DE decarbonation reaction; redox reaction; metastable graphite; metasomatism; ultrahigh-pressure metamorphism ID PRESSURE METAMORPHIC ROCKS; NORTHERN KAZAKSTAN; KOKCHETAV MASSIF; DABIE MOUNTAINS; OCEAN CRUST; 2 CO2; 6 GPA; MAGNESITE; DECARBONATION; KINETICS AB Carbonates carried by oceanic plates-in the form of sediment or alteration products of basalts-are introduced into the mantle by subduction. The high-pressure-high-temperature stability of carbonates in a closed system has been constrained by a number of studies, but the effects of the interactions between subducted carbonates and the surrounding mantle on carbonate stability are poorly known. These interactions may, however, influence the stability depth of the subducted material, the composition of the interaction zone, and the rate of carbon transfer from the slab to the mantle. To determine the exchange mechanisms at the interface between a subducted dolomite + coesite assemblage and the overlying mantle, we performed experiments at 6 GPa and 900 degrees C and 1100 degrees C in a multi-anvil apparatus. In a first series of experiments, we studied the reaction and migration processes operating along the interface between a cylinder of dolomite + coesite and a cylinder of garnet peridotite. In a second series of experiments, homogeneous mixtures of dolomite + coesite and garnet peridotite were equilibrated at high pressure and high temperature to characterize the phase relations as a function of the (dolomite + coesite)/peridotite ratio. We show that the destabilization temperature of a subducted dolomite + coesite assemblage is less than 900 degrees C at 6 GPa when in contact with a garnet lherzolite or a harzburgite. A reaction zone composed mainly of clinopyroxene + magnesite is produced at the interface between dolomite + coesite and peridotite. Carbon-in the form of a fluid or in a carbonatitic melt-also infiltrates the garnet peridotite to form magnesite and clinopyroxene. Moreover, graphite was observed in two experiments. We believe that it was produced by a redox reaction at the interface between dolomite + coesite and iron-bearing silicates in the peridotite. As our experimental conditions are in the stability field of diamond, this suggests a potential mechanism for diamond crystallization from subducted dolomite + coesite in contact with the mantle wedge. C1 [Martin, Audrey M.] NASA, Lyndon B Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA. [Kawamoto, Tatsuhiko] Kyoto Univ, Grad Sch Sci, Inst Geothermal Sci, Beppu, Oita 8740903, Japan. [Martin, Audrey M.; Laporte, Didier; Koga, Kenneth T.; Hammouda, Tahar] IRD, LMV, R163, F-63038 Clermont Ferrand, France. [Martin, Audrey M.; Laporte, Didier; Koga, Kenneth T.; Hammouda, Tahar] CNRS, LMV, UMR 6524, F-63038 Clermont Ferrand, France. [Martin, Audrey M.; Laporte, Didier; Koga, Kenneth T.; Hammouda, Tahar] Univ Clermont Ferrand, Univ Clermont Ferrand 2, Lab Magmas & Volcans, F-63000 Clermont Ferrand, France. RP Martin, AM (reprint author), NASA, Lyndon B Johnson Space Ctr, Mailcode KT, 2101 NASA Pkwy, Houston, TX 77058 USA. EM aud.martin23@gmail.com RI Kawamoto, Tatsuhiko/H-6088-2011; Koga, Kenneth T./D-8170-2017; OI Kawamoto, Tatsuhiko/0000-0002-6989-874X; Koga, Kenneth T./0000-0002-0862-6804; Martin, Audrey/0000-0002-1165-8866 FU JSPS Japan-France; Institut National des Sciences de l'Univers (INSU-CNRS); Centre National de la Recherche Scientifique (INSU National Instrument) FX The exchange visit to JASRI was supported by the JSPS Japan-France integrated action program (SAKURA 2006-2007). This study was supported by the DyETI program of the Institut National des Sciences de l'Univers (INSU-CNRS), through grants to T. Hammouda. The multi-anvil apparatus of Laboratoire Magmas et Volcans is financially supported by the Centre National de la Recherche Scientifique (INSU National Instrument). NR 54 TC 9 Z9 10 U1 0 U2 22 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-3530 J9 J PETROL JI J. Petrol. PD FEB PY 2012 VL 53 IS 2 BP 391 EP 417 DI 10.1093/petrology/egr066 PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 879QW UT WOS:000299348000006 ER PT J AU Jain, A AF Jain, Abhinandan TI Multibody graph transformations and analysis SO NONLINEAR DYNAMICS LA English DT Article DE Multibody dynamics; Simulation ID SPATIAL OPERATOR ALGEBRA; SYSTEM DYNAMICS AB This is the second part of a two-part paper that develops graph theoretic techniques for the topological transformation and analysis of multibody system dynamics. The first part focused on tree systems, and developed systematic and rigorous techniques for the partitioning, aggregation, and substructuring of multibody dynamics models. This second part, uses the aggregation techniques as the foundation to develop the constraint-embedding technique that enables the transformation of the nontree system graphs into tree graphs. This enables the application of a large family of analytical and computational techniques for trees to closed-chain systems. This is illustrated through an extension of the low-order articulated-body forward dynamics algorithm for tree systems to closed-chain systems. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jain, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Abhi.Jain@jpl.nasa.gov FU National Aeronautics and Space Administration; National Institute of Health [RO1GM082896-01A2] FX We would like to acknowledge the many detailed and insightful comments by the anonymous reviewer that have helped us revise and improve this paper. The research described in this paper was performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration.3 This project was also supported in part by Grant Number RO1GM082896-01A2 from the National Institute of Health. NR 17 TC 1 Z9 1 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0924-090X J9 NONLINEAR DYNAM JI Nonlinear Dyn. PD FEB PY 2012 VL 67 IS 3 BP 2153 EP 2170 DI 10.1007/s11071-011-0136-x PG 18 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 876CW UT WOS:000299085800037 PM 22267894 ER PT J AU Nitschke, W Russell, MJ AF Nitschke, Wolfgang Russell, Michael J. TI Redox bifurcations: Mechanisms and importance to life now, and at its origin SO BIOESSAYS LA English DT Article ID METHANOGENIC ARCHAEA; CLOSTRIDIUM-KLUYVERI; ENERGY-CONSERVATION; FERREDOXIN; REDUCTION; NADH; COMPLEX C1 [Nitschke, Wolfgang] CNRS IFR88, Bioenerget & Ingn Prot UPR9036, Marseille, France. [Russell, Michael J.] CALTECH, JPL, Pasadena, CA 91125 USA. RP Nitschke, W (reprint author), CNRS IFR88, Bioenerget & Ingn Prot UPR9036, Marseille, France. EM nitschke@ibsm.cnrs-mrs.fr NR 12 TC 27 Z9 27 U1 4 U2 30 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0265-9247 J9 BIOESSAYS JI Bioessays PD FEB PY 2012 VL 34 IS 2 BP 106 EP 109 DI 10.1002/bies.201100134 PG 4 WC Biochemistry & Molecular Biology; Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics GA 874UL UT WOS:000298983500023 PM 22045626 ER PT J AU Toth, G van der Holst, B Sokolov, IV De Zeeuw, DL Gombosi, TI Fang, F Manchester, WB Meng, X Najib, D Powell, KG Stout, QF Glocer, A Ma, YJ Opher, M AF Toth, Gabor van der Holst, Bart Sokolov, Igor V. De Zeeuw, Darren L. Gombosi, Tamas I. Fang, Fang Manchester, Ward B. Meng, Xing Najib, Dalal Powell, Kenneth G. Stout, Quentin F. Glocer, Alex Ma, Ying-Juan Opher, Merav TI Adaptive numerical algorithms in space weather modeling SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE 65D99 Numerical approximation; 77A05 Magnetohydrodynamics ID CORONAL MASS EJECTIONS; HYPERBOLIC CONSERVATION-LAWS; 3-DIMENSIONAL MHD SIMULATION; NONSYMMETRIC LINEAR-SYSTEMS; SOLAR-WIND; IDEAL MAGNETOHYDRODYNAMICS; PARTICLE-ACCELERATION; ELECTRIC POTENTIALS; MAGNETIC-FIELD; SCHEMES AB Space weather describes the various processes in the Sun-Earth system that present danger to human health and technology. The goal of space weather forecasting is to provide an opportunity to mitigate these negative effects. Physics-based space weather modeling is characterized by disparate temporal and spatial scales as well as by different relevant physics in different domains. A multi-physics system can be modeled by a software framework comprising several components. Each component corresponds to a physics domain, and each component is represented by one or more numerical models. The publicly available Space Weather Modeling Framework (SWMF) can execute and couple together several components distributed over a parallel machine in a flexible and efficient manner. The framework also allows resolving disparate spatial and temporal scales with independent spatial and temporal discretizations in the various models. Several of the computationally most expensive domains of the framework are modeled by the Block-Adaptive Tree Solarwind Roe-type Upwind Scheme (BATS-R-US) code that can solve various forms of the magnetohydrodynamic (MHD) equations, including Hall, semi-relativistic, multi-species and multi-fluid MHD, anisotropic pressure, radiative transport and heat conduction. Modeling disparate scales within BATS-R-US is achieved by a block-adaptive mesh both in Cartesian and generalized coordinates. Most recently we have created a new core for BATS-R-US: the Block-Adaptive Tree Library (BAIL) that provides a general toolkit for creating, load balancing and message passing in a 1,2 or 3 dimensional block-adaptive grid. We describe the algorithms of BATL and demonstrate its efficiency and scaling properties for various problems. BATS-R-US uses several time-integration schemes to address multiple time-scales: explicit time stepping with fixed or local time steps, partially steady-state evolution, point-implicit, semi-implicit, explicit/implicit, and fully implicit numerical schemes. Depending on the application, we find that different time stepping methods are optimal. Several of the time integration schemes exploit the block-based granularity of the grid structure. The framework and the adaptive algorithms enable physics-based space weather modeling and even short-term forecasting. (C) 2011 Elsevier Inc. All rights reserved. C1 [Toth, Gabor; van der Holst, Bart; Sokolov, Igor V.; De Zeeuw, Darren L.; Gombosi, Tamas I.; Fang, Fang; Manchester, Ward B.; Meng, Xing; Najib, Dalal; Powell, Kenneth G.; Stout, Quentin F.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. [Glocer, Alex] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. [Ma, Ying-Juan] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Opher, Merav] Boston Univ, Dept Astron, Boston, MA 02215 USA. RP Toth, G (reprint author), Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. EM gtoth@umich.edu RI Ma, Yingjuan/B-4895-2017; De Zeeuw, Darren/F-3667-2011; van der Holst, Bart/A-3557-2013; Glocer, Alex/C-9512-2012; Manchester, Ward/I-9422-2012; Gombosi, Tamas/G-4238-2011; Toth, Gabor/B-7977-2013; Sokolov, Igor/H-9860-2013; feggans, john/F-5370-2012; Meng, Xing/A-1929-2016 OI Ma, Yingjuan/0000-0003-2584-7091; Stout, Quentin/0000-0002-8047-7348; van der Holst, Bart/0000-0001-5260-3944; Powell, Kenneth/0000-0002-3708-8814; Glocer, Alex/0000-0001-9843-9094; Gombosi, Tamas/0000-0001-9360-4951; Toth, Gabor/0000-0002-5654-9823; Sokolov, Igor/0000-0002-6118-0469; FU NSF [ATM 0642309, ATM-0639336, AGS-1027192, AGS 1023735]; NASA [NNX07AC16G, NNX07AV80G]; AFOSR [FA9550-07-1-0434]; Department of Energy NNSA [DEFC52-08NA28616]; Jet Propulsion Laboratory [DRDA-07-1583]; NASA LWS [NNX09AJ78G]; NSF CAREER [ATM-0747654] FX The heliospheric components of the SWMF are developed as part of the Comprehensive Corona and Heliospheric Model supported by the NSF ATM 0642309 and NASA NNX07AC16G grants. The magnetospheric components are developed as part of the Community-based Whole Magnetospheric Model supported by NSF ATM-0639336 and AFOSR FA9550-07-1-0434 grants. Extension of BATS-R-US to non-ideal MHD was supported by the NASA Applied Information Systems Research Program grant NNX07AV80G. We also acknowledge support from the NSF Cyber-Enabled Discovery and Innovation grant AGS-1027192. The Block Adaptive Tree Library, the radiative transfer and multi-material physics were developed by the Center for Radiative Shock Hydrodynamics supported by the Department of Energy NNSA under the Predictive Science Academic Alliance Program by grant DEFC52-08NA28616. The General Input Parameter Handling Toolkit development was supported by the DRDA-07-1583 grant from the Jet Propulsion Laboratory. Ward Manchester and Fang Fang acknowledge support by the NSF AGS 1023735 and NASA LWS NNX09AJ78G grants. Merav Opher thanks the support of the NSF CAREER Grant ATM-0747654. We thank the NASA Supercomputer Division at Ames and its helpful staff for making it possible to perform many of the simulations presented in this paper. NR 91 TC 168 Z9 170 U1 2 U2 26 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 FEB 1 PY 2012 VL 231 IS 3 SI SI BP 870 EP 903 DI 10.1016/j.jcp.2011.02.006 PG 34 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 868LG UT WOS:000298524200008 ER PT J AU Paranicas, C Roussos, E Krupp, N Kollmann, P Hendrix, AR Cassidy, T Johnson, RE Schenk, P Jones, G Carbary, J Mitchell, DG Dialynas, K AF Paranicas, C. Roussos, E. Krupp, N. Kollmann, P. Hendrix, A. R. Cassidy, T. Johnson, R. E. Schenk, P. Jones, G. Carbary, J. Mitchell, D. G. Dialynas, K. TI Energetic charged particle weathering of Saturn's inner satellites SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Planetary magnetospheres; Saturn; Planetary satellites ID MAGNETOSPHERE; PROTONS; EUROPA; BOMBARDMENT; ALBEDO; RING AB We characterize the relative importance of energetic electrons and protons to the weathering of five of the inner satellites of Saturn. To do this, we present data from the Magnetospheric Imaging Instrument on the Cassini spacecraft, some of which is averaged over the whole mission to date. We also compute averaged proton and electron energy spectra relevant to the distances of these inner satellites. Where data are available, we estimate the power per unit area into a satellite's surface. For electron energy deposition into satellite leading hemispheres, we find the power per unit area is greatest at Mimas and falls off with distance from Saturn. Using fluxes of 1-50 MeV protons detected within the sweeping corridors of Mimas and Enceladus, we find the corresponding deposition would be about 2 x 10(8) and 3.7 x 10(7) eV/cm(2) s. (C) 2011 Elsevier Ltd. All rights C1 [Paranicas, C.; Carbary, J.; Mitchell, D. G.] APL, Laurel, MD 20723 USA. [Roussos, E.; Krupp, N.; Kollmann, P.] MPS, D-37191 Katlenburg Lindau, Germany. [Hendrix, A. R.; Cassidy, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Johnson, R. E.] UVA, Charlottesville, VA 22904 USA. [Schenk, P.] LPI, Houston, TX USA. [Jones, G.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Dialynas, K.] Univ Athens, Athens, Greece. RP Paranicas, C (reprint author), APL, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM chris.paranicas@jhuapl.edu RI Jones, Geraint/C-1682-2008; Paranicas, Christopher/B-1470-2016; Carbary, James/C-2086-2016; Kollmann, Peter/C-2583-2016; OI Jones, Geraint/0000-0002-5859-1136; Paranicas, Christopher/0000-0002-4391-8255; Carbary, James/0000-0003-1781-3078; Kollmann, Peter/0000-0002-4274-9760; Roussos, Elias/0000-0002-5699-0678 NR 28 TC 12 Z9 12 U1 2 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD FEB PY 2012 VL 61 IS 1 SI SI BP 60 EP 65 DI 10.1016/j.pss.2011.02.012 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971IY UT WOS:000306198800007 ER PT J AU Eckman, RS Stackhouse, PW AF Eckman, Richard S. Stackhouse, Paul W., Jr. TI CEOS contributions to informing energy management and policy decision making using space-based Earth observations SO APPLIED ENERGY LA English DT Article; Proceedings Paper CT International Conference on Applied Energy (ICAE) on Energy Solutions for a Sustainable World CY APR 21-23, 2010 CL Singapore, SINGAPORE DE Energy management; Renewable energy resource assessment; Committee on Earth Observation Satellites; Group on Earth Observations; Energy efficiency; Decision support AB Earth observations are playing an increasingly significant role in informing decision making in the energy sector. In renewable energy applications, space-based observations now routinely augment sparse ground-based observations used as input for renewable energy resource assessment applications. As one of the nine Group on Earth Observations (GEO) societal benefit areas, the enhancement of management and policy decision making in the energy sector is receiving attention in activities conducted by the Committee on Earth Observation Satellites (CEOS). CEOS has become the "space arm" for the implementation of the Global Earth Observation System of Systems (GEOSS) vision. It is directly supporting the space-based, near-term tasks articulated in the GEO three-year work plan. This paper describes a coordinated program of demonstration projects conducted by CEOS member agencies and partners to utilize Earth observations to enhance energy management end-user decision support systems. We discuss the importance of engagement with stakeholders and understanding their decision support needs in successfully increasing the uptake of Earth observation products for societal benefit. Several case studies are presented, demonstrating the importance of providing data sets in formats and units familiar and immediately usable by decision makers. These projects show the utility of Earth observations to enhance renewable energy resource assessment in the developing world, forecast space weather impacts on the power grid, and improve energy efficiency in the built environment. Published by Elsevier Ltd. C1 [Eckman, Richard S.; Stackhouse, Paul W., Jr.] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA. [Eckman, Richard S.] NASA Headquarters, Div Earth Sci, Sci Miss Directorate, Washington, DC 20546 USA. RP Eckman, RS (reprint author), NASA, Sci Directorate, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM Richard.S.Eckman@nasa.gov; Paul.W.Stackhouse@nasa.gov NR 13 TC 8 Z9 8 U1 0 U2 5 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0306-2619 J9 APPL ENERG JI Appl. Energy PD FEB PY 2012 VL 90 IS 1 SI SI BP 206 EP 210 DI 10.1016/j.apenergy.2011.03.001 PG 5 WC Energy & Fuels; Engineering, Chemical SC Energy & Fuels; Engineering GA 853KV UT WOS:000297426100032 ER PT J AU Leckey, CAC Rogge, MD Miller, CA Hinders, MK AF Leckey, Cara A. C. Rogge, Matthew D. Miller, Corey A. Hinders, Mark K. TI Multiple-mode Lamb wave scattering simulations using 3D elastodynamic finite integration technique SO ULTRASONICS LA English DT Article DE Lamb waves; Nondestructive evaluation; Simulation ID HELICAL ULTRASONIC TOMOGRAPHY; ALUMINUM-ALLOYS; PROPAGATION; TIME; GEOMETRIES; DAMAGE AB We have implemented three-dimensional (3D) elastodynamic finite integration technique (EFIT) simulations to model Lamb wave scattering for two flaw-types in an aircraft-grade aluminum plate, a rounded rectangle flat-bottom hole and a disbond of the same shape. The plate thickness and flaws explored in this work include frequency-thickness regions where several Lamb wave modes exist and sometimes overlap in phase and/or group velocity. For the case of the flat-bottom hole the depth was incrementally increased to explore progressive changes in multiple-mode Lamb wave scattering due to the damage. The flat-bottom hole simulation results have been compared to experimental data and are shown to provide key insight for this well-defined experimental case by explaining unexpected results in experimental waveforms. For the rounded rectangle disbond flaw, which would be difficult to implement experimentally, we found that Lamb wave behavior differed significantly from the flat-bottom hole flaw. Most of the literature in this field is restricted to low frequency-thickness regions due to difficulties in interpreting data when multiple modes exist. We found that benchmarked 3D EFIT simulations can yield an understanding of scattering behavior for these higher frequency-thickness regions and in cases that would be difficult to set up experimentally. Additionally, our results show that 2D simulations would not have been sufficient for modeling the complicated scattering that occurred. Published by Elsevier B.V. C1 [Leckey, Cara A. C.; Rogge, Matthew D.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Miller, Corey A.; Hinders, Mark K.] Coll William & Mary, Dept Appl Sci, Williamsburg, VA USA. RP Leckey, CAC (reprint author), NASA, Langley Res Ctr, MS 231, Hampton, VA 23681 USA. EM cara.ac.leckey@nasa.gov NR 43 TC 25 Z9 25 U1 0 U2 19 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0041-624X J9 ULTRASONICS JI Ultrasonics PD FEB PY 2012 VL 52 IS 2 BP 193 EP 207 DI 10.1016/j.ultras.2011.08.003 PG 15 WC Acoustics; Radiology, Nuclear Medicine & Medical Imaging SC Acoustics; Radiology, Nuclear Medicine & Medical Imaging GA 852EQ UT WOS:000297335200001 PM 21908011 ER PT J AU Hillers, G Graham, N Campillo, M Kedar, S Landes, M Shapiro, N AF Hillers, G. Graham, N. Campillo, M. Kedar, S. Landes, M. Shapiro, N. TI Global oceanic microseism sources as seen by seismic arrays and predicted by wave action models SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Article DE microseisms; noise seasonality; noise source; seismic noise; wave action models ID NOISE; TOMOGRAPHY; RADIATION; PACIFIC; COASTAL; PHASE; TIME; SEA; HUM AB We analyze global microseism excitation patterns between July 2000 and June 2001. Seismological observations are compared with modeling results to isolate robust activity features of relevant source processes. First, we use observations of microseism source locations estimated by Landes et al. (2010) based on array processing of ambient noise correlations. Second, we construct synthetic activity patterns by coupling sea state estimates derived from wave action models to the excitation theory for microseisms. The overall spatiotemporal evolution of both estimates is characterized by a seasonal character that is associated with strong activity during winter months. The distribution of landmass causes seasonal changes on the Northern Hemisphere (NH) to exceed the variability on the Southern Hemisphere (SH). Our systematic comparison of the two estimates reveals significant microseism excitation along coastlines and in the open ocean. Since coastal reflections are not accounted for in the modeling approach, the consistent mismatch between near-coastal observations and predictions suggests that relevant microseism energy arriving at the networks is generated in these areas. Simultaneously, systematic coincidence away from coastlines verifies the open ocean generation hypothesis. These conclusions are universal and robust with respect to the seismic network locations on the NH. The spatially homogeneous resolution of our synthetics provides a valuable resource for the assessment of the global microseism weather. Similar to previously identified hot spot areas in the North Atlantic, the modeled distributions hypothesize regions of strong localized activity on the SH, which are only partially confirmed by the analyzed data sets. C1 [Hillers, G.; Campillo, M.] Univ Grenoble 1, CNRS, Inst Sci Terre, F-38041 Grenoble 9, France. [Graham, N.] Hydrol Res Ctr, San Diego, CA 92130 USA. [Kedar, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Landes, M.] Commissariat Energie Atom & Energies Renouvelable, Direct Applicat Mil, Dept Ile de France, F-91297 Arpajon, France. [Shapiro, N.] CNRS, UMR7154, Inst Phys Globe Paris, F-75238 Paris, France. RP Hillers, G (reprint author), Univ Grenoble 1, CNRS, Inst Sci Terre, BP 53, F-38041 Grenoble 9, France. EM hillersg@ujf-grenoble.fr RI Shapiro, Nikolai/G-1049-2010; Campillo, Michel/K-6231-2012 OI Shapiro, Nikolai/0000-0002-0144-723X; FU European Research Council [L27507] FX We thank P. Roux for discussions on beamformer resolution. The manuscript benefited from the comments of the Editor, Thorsten Becker, and two anonymous reviewers. This work was supported by the European Research Council (advanced grant Whisper L27507). Most figures were constructed using Generic Mapping Tools (GMT) [Wessel and Smith, 1991]. NR 54 TC 37 Z9 38 U1 1 U2 20 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 JAN 31 PY 2012 VL 13 AR Q01021 DI 10.1029/2011GC003875 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 888GA UT WOS:000299990600001 ER PT J AU Hanna, KLD Wyatt, MB Thomas, IR Bowles, NE Greenhagen, BT Maturilli, A Helbert, J Paige, DA AF Hanna, Kerri L. Donaldson Wyatt, Michael B. Thomas, Ian R. Bowles, Neil E. Greenhagen, Benjamin T. Maturilli, Alessandro Helbert, Joern Paige, David A. TI Thermal infrared emissivity measurements under a simulated lunar environment: Application to the Diviner Lunar Radiometer Experiment SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID REFLECTANCE SPECTRA; SURFACE FEATURES; MOON; SPECTROSCOPY; OLIVINE; ROCK; PLAGIOCLASE; MINERALOGY; SILICATES; PYROXENES AB We present new laboratory thermal infrared emissivity spectra of the major silicate minerals identified on the Moon measured under lunar environmental conditions and evaluate their application to lunar remote sensing data sets. Thermal infrared spectral changes between ambient and lunar environmental conditions are characterized for the first time over the 400 similar to 1700 cm(-1) (6-25 mu m) spectral range for a fine-particulate mineral suite including plagioclase (albite and anorthite), pyroxene (enstatite and augite), and olivine (forsterite). The lunar environment introduces observable effects in thermal infrared emissivity spectra of fine particulate minerals, which include: (1) a shift in the Christiansen feature (CF) position to higher wave numbers (shorter wavelengths), (2) an increase in the overall spectral contrast, and (3) decreases in the spectral contrast of the reststrahlen bands and transparency features. Our new measurements demonstrate the high sensitivity of thermal infrared emissivity spectra to environmental conditions under which they are measured and provide important constraints for interpreting new thermal infrared data sets of the Moon, including the Diviner Lunar Radiometer Experiment onboard NASA's Lunar Reconnaissance Orbiter. Full resolution laboratory mineral spectra convolved to Diviner's three spectral channels show that spectral shape, CF position and band ratios can be used to distinguish between individual mineral groups and lunar lithologies. The integration of the thermal infrared CF position with near infrared spectral parameters allows for robust mineralogical identifications and provides a framework for future integrations of data sets across two different wavelength regimes. C1 [Hanna, Kerri L. Donaldson; Wyatt, Michael B.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Thomas, Ian R.; Bowles, Neil E.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [Greenhagen, Benjamin T.] Jet Prop Lab, Geophys & Planetary Geosci Grp, Pasadena, CA 91109 USA. [Maturilli, Alessandro; Helbert, Joern] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany. [Paige, David A.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Hanna, KLD (reprint author), Brown Univ, Dept Geol Sci, Box 1846, Providence, RI 02912 USA. EM kerri_donaldson_hanna@brown.edu RI Greenhagen, Benjamin/C-3760-2016 OI Helbert, Jorn/0000-0001-5346-9505; FU NASA [NNX08AM75G] FX We would like to extend our appreciation to P. Christensen and Arizona State University for donating the samples used in this study. The authors would also like to thank S. Ruff and an anonymous reviewer for comments and suggestions that have helped to improve the manuscript as well as C. M. Pieters for comments and suggestions that greatly improved the thermal- and near- infrared data integration portion of this manuscript. K. L. Donaldson Hanna and M. B. Wyatt were supported by NASA grant NNX08AM75G. NR 68 TC 7 Z9 7 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JAN 31 PY 2012 VL 117 AR E00H05 DI 10.1029/2011JE003862 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 887UL UT WOS:000299956100001 ER PT J AU Abe, K Fuke, H Haino, S Hams, T Hasegawa, M Horikoshi, A Kim, KC Kusumoto, A Lee, MH Makida, Y Matsuda, S Matsukawa, Y Mitchell, JW Nishimura, J Nozaki, M Orito, R Ormes, JF Sakai, K Sasaki, M Seo, ES Shinoda, R Streitmatter, RE Suzuki, J 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. Kim, K. C. Kusumoto, A. Lee, M. H. Makida, Y. Matsuda, S. Matsukawa, Y. Mitchell, J. W. Nishimura, J. Nozaki, M. Orito, R. Ormes, J. F. Sakai, K. Sasaki, M. Seo, E. S. Shinoda, R. Streitmatter, R. E. Suzuki, J. Tanaka, K. Thakur, N. Yamagami, T. Yamamoto, A. Yoshida, T. Yoshimura, K. TI Measurement of the Cosmic-Ray Antiproton Spectrum at Solar Minimum with a Long-Duration Balloon Flight over Antarctica SO PHYSICAL REVIEW LETTERS LA English DT Article ID BESS-POLAR EXPERIMENT; BLACK-HOLES; SPECTROMETER; PROGRESS; SEARCH; MATTER; FLUX AB The energy spectrum of cosmic-ray antiprotons ((p) over bar 's) from 0.17 to 3.5 GeV has been measured using 7886 (p) over bar 's detected by BESS-Polar II during a long-duration flight over Antarctica near solar minimum in December 2007 and January 2008. This shows good consistency with secondary (p) over bar calculations. Cosmologically primary (p) over bar 's have been investigated by comparing measured and calculated (p) over bar spectra. BESS-Polar II data show no evidence of primary (p) over bar 's from the evaporation of primordial black holes. C1 [Hams, T.; Mitchell, J. W.; Sakai, K.; Sasaki, M.; Streitmatter, R. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Abe, K.; Kusumoto, A.; Matsukawa, Y.; Orito, R.] Kobe Univ, Kobe, Hyogo 6578501, Japan. [Fuke, H.; Yamagami, T.; Yoshida, T.] Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Haino, S.; Hasegawa, M.; Horikoshi, A.; Makida, Y.; Matsuda, S.; Nozaki, M.; Suzuki, J.; Tanaka, K.; Yamamoto, A.; Yoshimura, K.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan. [Kim, K. C.; Lee, M. H.; Seo, E. S.] Univ Maryland, IPST, College Pk, MD 20742 USA. [Nishimura, J.; Sakai, K.; Shinoda, R.; Yamamoto, A.] Univ Tokyo, Bunkyo Ku, Tokyo 1130033, Japan. [Ormes, J. F.; Thakur, N.] Univ Denver, Denver, CO 80208 USA. RP Sakai, K (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Kenichi.Sakai@nasa.gov OI Seo, Eun-Suk/0000-0001-8682-805X FU KAKENHI; MEXT-JSPS; NASA FX The BESS-Polar Collaboration is supported in Japan by the Grant-in-Aid "KAKENHI" for specially promoted and basic researches, MEXT-JSPS, and in the U.S. by NASA. Balloon flight operations were carried out by the NASA Columbia Scientific Balloon Facility and the National Science Foundation United States Antarctic Program. We would like to express our sincere thanks for their continuous professional support. NR 27 TC 43 Z9 43 U1 0 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JAN 31 PY 2012 VL 108 IS 5 AR 051102 DI 10.1103/PhysRevLett.108.051102 PG 5 WC Physics, Multidisciplinary SC Physics GA 886DU UT WOS:000299832900002 PM 22400920 ER PT J AU Park, IH Gangupomu, V Wagner, J Jain, A Vaidehi, N AF Park, In-Hee Gangupomu, Vamshi Wagner, Jeffrey Jain, Abhinandan Vaidehi, Nagarajan TI Structure Refinement of Protein Low Resolution Models using GNEIMO Constrained Dynamics Method SO BIOPHYSICAL JOURNAL LA English DT Meeting Abstract CT 56th Annual Meeting of the Biophysical-Society CY FEB 25-29, 2012 CL San Diego, CA SP Biophys Soc C1 [Park, In-Hee; Gangupomu, Vamshi; Wagner, Jeffrey; Vaidehi, Nagarajan] City Hope Natl Med Ctr, Beckman Res Inst, Duarte, CA USA. [Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0006-3495 J9 BIOPHYS J JI Biophys. J. PD JAN 31 PY 2012 VL 102 IS 3 SU 1 BP 25A EP 25A PG 1 WC Biophysics SC Biophysics GA 179ZF UT WOS:000321561200124 ER PT J AU Moore, JP Rogge, MD AF Moore, Jason P. Rogge, Matthew D. TI Shape sensing using multi-core fiber optic cable and parametric curve solutions SO OPTICS EXPRESS LA English DT Article ID BEND MEASUREMENT; BRAGG GRATINGS AB The shape of a multi-core optical fiber is calculated by numerically solving a set of Frenet-Serret equations describing the path of the fiber in three dimensions. Included in the Frenet-Serret equations are curvature and bending direction functions derived from distributed fiber Bragg grating strain measurements in each core. The method offers advantages over prior art in that it determines complex three-dimensional fiber shape as a continuous parametric solution rather than an integrated series of discrete planar bends. Results and error analysis of the method using a tri-core optical fiber is presented. Maximum error expressed as a percentage of fiber length was found to be 7.2%. 2012 Optical Society of America C1 [Moore, Jason P.; Rogge, Matthew D.] NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Moore, JP (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA. EM jason.p.moore@nasa.gov NR 10 TC 44 Z9 44 U1 10 U2 31 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 JAN 30 PY 2012 VL 20 IS 3 BP 2967 EP 2973 DI 10.1364/OE.20.002967 PG 7 WC Optics SC Optics GA 895ME UT WOS:000300499500103 PM 22330534 ER PT J AU Numata, K Camp, J AF Numata, Kenji Camp, Jordan TI Estimation of frequency noise in semiconductor lasers due to mechanical thermal noise SO PHYSICS LETTERS A LA English DT Article DE Thermal noise; Semiconductor laser ID 1/F NOISE; DEGRADATION; VCSELS AB We evaluate mechanical thermal noise in semiconductor lasers, applying a methodology developed for fixed-spacer cavities for laser frequency stabilization. Our simple model determines an underlying fundamental limit for the frequency noise of free-running semiconductor laser, and provides a framework where the noise may be potentially reduced with improved design. (C) 2012 Elsevier B.V. All rights reserved. C1 [Numata, Kenji; Camp, Jordan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Numata, Kenji] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Numata, K (reprint author), NASA, Goddard Space Flight Ctr, Code 663,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM kenji.numata@nasa.gov NR 40 TC 0 Z9 1 U1 0 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0375-9601 EI 1873-2429 J9 PHYS LETT A JI Phys. Lett. A PD JAN 30 PY 2012 VL 376 IS 6-7 BP 798 EP 802 DI 10.1016/j.physleta.2012.01.013 PG 5 WC Physics, Multidisciplinary SC Physics GA 904AZ UT WOS:000301167300003 ER PT J AU Slavin, JA Anderson, BJ Baker, DN Benna, M Boardsen, SA Gold, RE Ho, GC Imber, SM Korth, H Krimigis, SM McNutt, RL Raines, JM Sarantos, M Schriver, D Solomon, SC Travnicek, P Zurbuchen, TH AF Slavin, James A. Anderson, Brian J. Baker, Daniel N. Benna, Mehdi Boardsen, Scott A. Gold, Robert E. Ho, George C. Imber, Suzanne M. Korth, Haje Krimigis, Stamatios M. McNutt, Ralph L., Jr. Raines, Jim M. Sarantos, Menelaos Schriver, David Solomon, Sean C. Travnicek, Pavel Zurbuchen, Thomas H. TI MESSENGER and Mariner 10 flyby observations of magnetotail structure and dynamics at Mercury SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID STEADY MAGNETOSPHERIC CONVECTION; KELVIN-HELMHOLTZ INSTABILITY; LATITUDE BOUNDARY-LAYER; SOLAR-WIND INTERACTION; MAGNETIC-FIELD; GEOMAGNETIC TAIL; GEOTAIL OBSERVATIONS; EARTHS MAGNETOSPHERE; DISTANT MAGNETOTAIL; NEAR-TAIL AB The first (M1), second (M2), and third (M3) MESSENGER flybys of Mercury traversed the planet's magnetotail from 1.25 to 3.25 R-M downstream of the planet, where R-M is Mercury's radius (2440 km). The encounters took place under northward, southward, and variable-polarity interplanetary magnetic field (IMF), respectively. The magnetic field strength B in Mercury's magnetotail follows a power law decrease with increasing antisunward distance vertical bar X vertical bar, B similar to vertical bar X vertical bar(G), with G varying from -5.4 for northward to -1.6 for southward IMF. Low-latitude boundary layers (LLBLs) containing strong northward magnetic field were detected at the tail flanks during two of the flybys. The observed thickness of the LLBL was similar to 33% and 16% of the radius of the tail during M1 and M3, respectively, but the boundary layer was completely absent during M2. Clear signatures of tail reconnection are evident in the M2 and M3 magnetic field measurements. Plasmoids and traveling compression regions were observed during M2 and M3 with typical durations of similar to 1-3 s, suggesting diameters of similar to 500-1500 km. Overall, the response of Mercury's magnetotail to the steady southward IMF during M2 appeared very similar to steady magnetospheric convection events at Earth, which are believed to be driven by quasi-continuous reconnection. In contrast, the M3 measurements are dominated by tail loading and unloading events that resemble the large-scale magnetic field reconfigurations observed during magnetospheric substorms at Earth. C1 [Slavin, James A.; Boardsen, Scott A.; Imber, Suzanne M.; Sarantos, Menelaos] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Anderson, Brian J.; Gold, Robert E.; Ho, George C.; Korth, Haje; Krimigis, Stamatios M.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Baker, Daniel N.] Univ Colorado, Lab Solar & Atmospher Phys, Boulder, CO 80303 USA. [Benna, Mehdi] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Boardsen, Scott A.; Imber, Suzanne M.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Krimigis, Stamatios M.; Sarantos, Menelaos] Acad Athens, Off Space Res & Technol, Athens, Greece. [Raines, Jim M.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Schriver, David] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Travnicek, Pavel] Acad Sci Czech Republic, Astron Inst, Prague 14131, Czech Republic. RP Slavin, JA (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Code 670-0,Bldg 21,Greenbelt Rd, Greenbelt, MD 20771 USA. RI Benna, Mehdi/F-3489-2012; Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; Sarantos, Menelaos/H-8136-2013; McNutt, Ralph/E-8006-2010; Travnicek, Pavel/G-8608-2014; Ho, George/G-3650-2015 OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166; Ho, George/0000-0003-1093-2066 FU NASA [NASW-00002, NAS5-97271] FX Computational assistance and data visualization support provided by J. Feggans are gratefully acknowledged. We are also pleased to acknowledge stimulating comments and discussions with V. Uritsky. 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. NR 97 TC 36 Z9 36 U1 1 U2 11 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 JAN 28 PY 2012 VL 117 AR A01215 DI 10.1029/2011JA016900 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 884JG UT WOS:000299700300001 ER PT J AU Kim, JW Nunez, JC Siochi, EJ Wise, KE Lin, Y Connell, JW Smith, MW AF Kim, Jae-Woo Nunez, Jennifer Carpena Siochi, Emilie J. Wise, Kristopher E. Lin, Yi Connell, John W. Smith, Michael W. TI In situ mechanical property measurements of amorphous carbon-boron nitride nanotube nanostructures SO NANOTECHNOLOGY LA English DT Article ID STRENGTH; ELECTRON; MODULUS; BUNDLES; FIBERS AB To understand the mechanical properties of amorphous carbon (a-C)/boron nitride nanotube (BNNT) nanostructures, in situ mechanical tests are conducted inside a transmission electron microscope equipped with an integrated atomic force microscope system. The nanotube structure is modified with amorphous carbon deposited by controlled electron beam irradiation. We demonstrate multiple in situ tensile, compressive, and lap shear tests with a-C/BNNT hybrid nanostructures. The tensile strength of the a-C/BNNT hybrid nanostructure is 5.29 GPa with about 90 vol% of a-C. The tensile strength and strain of the end-to-end joint structure with a-C welding is 0.8 GPa and 5.2% whereas the lap shear strength of the side-by-side joint structure with a-C is 0.25 GPa. C1 [Kim, Jae-Woo; Lin, Yi] Natl Inst Aerosp, Hampton, VA 23666 USA. [Nunez, Jennifer Carpena; Siochi, Emilie J.; Wise, Kristopher E.; Connell, John W.; Smith, Michael W.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. RP Kim, JW (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. EM jae-woo.kim-1@nasa.gov RI Kim, Jae-Woo/A-8314-2008 NR 27 TC 4 Z9 4 U1 0 U2 21 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0957-4484 J9 NANOTECHNOLOGY JI Nanotechnology PD JAN 27 PY 2012 VL 23 IS 3 AR 035701 DI 10.1088/0957-4484/23/3/035701 PG 9 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA 877HQ UT WOS:000299168800013 PM 22172920 ER PT J AU Welsh, WF Orosz, JA Carter, JA Fabrycky, DC Ford, EB Lissauer, JJ Prsa, A Quinn, SN Ragozzine, D Short, DR Torres, G Winn, JN Doyle, LR Barclay, T Batalha, N Bloemen, S Brugamyer, E Buchhave, LA Caldwell, C Caldwell, DA Christiansen, JL Ciardi, DR Cochran, WD Endl, M Fortney, JJ Gautier, TN Gilliland, RL Haas, MR Hall, JR Holman, MJ Howard, AW Howell, SB Isaacson, H Jenkins, JM Klaus, TC Latham, DW Li, J Marcy, GW Mazeh, T Quintana, EV Robertson, P Shporer, A Steffen, JH Windmiller, G Koch, DG Borucki, WJ AF Welsh, William F. Orosz, Jerome A. Carter, Joshua A. Fabrycky, Daniel C. Ford, Eric B. Lissauer, Jack J. Prsa, Andrej Quinn, Samuel N. Ragozzine, Darin Short, Donald R. Torres, Guillermo Winn, Joshua N. Doyle, Laurance R. Barclay, Thomas Batalha, Natalie Bloemen, Steven Brugamyer, Erik Buchhave, Lars A. Caldwell, Caroline Caldwell, Douglas A. Christiansen, Jessie L. Ciardi, David R. Cochran, William D. Endl, Michael Fortney, Jonathan J. Gautier, Thomas N., III Gilliland, Ronald L. Haas, Michael R. Hall, Jennifer R. Holman, Matthew J. Howard, Andrew W. Howell, Steve B. Isaacson, Howard Jenkins, Jon M. Klaus, Todd C. Latham, David W. Li, Jie Marcy, Geoffrey W. Mazeh, Tsevi Quintana, Elisa V. Robertson, Paul Shporer, Avi Steffen, Jason H. Windmiller, Gur Koch, David G. Borucki, William J. TI Transiting circumbinary planets Kepler-34 b and Kepler-35 b SO NATURE LA English DT Article ID HIERARCHICAL TRIPLE; ECLIPSING BINARIES; DATA RELEASE; STELLAR; STARS; SYSTEMS; STABILITY; CATALOG AB Most Sun-like stars in the Galaxy reside in gravitationally bound pairs of stars(1,2) (binaries). Although long anticipated(3-8), the existence of a 'circumbinary planet' orbiting such a pair of normal stars was not definitively established until the discovery(9) of the planet transiting (that is, passing in front of) Kepler-16. Questions remained, however, about the prevalence of circumbinary planets and their range of orbital and physical properties. Here we report two additional transiting circumbinary planets: Kepler-34 (AB)b and Kepler-35 (AB)b, referred to here as Kepler-34 b and Kepler-35 b, respectively. Each is a low-density gas-giant planet on an orbit closely aligned with that of its parent stars. Kepler-34 b orbits two Sun-like stars every 289 days, whereas Kepler-35 b orbits a pair of smaller stars (89% and 81% of the Sun's mass) every 131 days. The planets experience large multi-periodic variations in incident stellar radiation arising from the orbital motion of the stars. The observed rate of circumbinary planets in our sample implies that more than similar to 1% of close binary stars have giant planets in nearly coplanar orbits, yielding a Galactic population of at least several million. C1 [Welsh, William F.; Orosz, Jerome A.; Short, Donald R.; Windmiller, Gur] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. [Ford, Eric B.] Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Lissauer, Jack J.; Barclay, Thomas; Batalha, Natalie; Christiansen, Jessie L.; Haas, Michael R.; Howell, Steve B.; Jenkins, Jon M.; Li, Jie; Quintana, Elisa V.; Koch, David G.; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Carter, Joshua A.; Quinn, Samuel N.; Ragozzine, Darin; Torres, Guillermo; Holman, Matthew J.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Quinn, Samuel N.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Doyle, Laurance R.; Caldwell, Douglas A.; Christiansen, Jessie L.; Jenkins, Jon M.; Li, Jie; Quintana, Elisa V.] SETI Inst, Carl Sagan Ctr Study Life Universe, Mountain View, CA 94043 USA. [Barclay, Thomas] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA. [Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Bloemen, Steven] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Brugamyer, Erik; Cochran, William D.; Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Gautier, Thomas N., III] Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Klaus, Todd C.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Mazeh, Tsevi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Shporer, Avi] Las Cumbres Observ, Global Telescope Network, Santa Barbara, CA 93117 USA. [Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. RP Welsh, WF (reprint author), San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA. EM wfw@sciences.sdsu.edu; jacarter@cfa.harvard.edu RI Steffen, Jason/A-4320-2013; Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015; OI Caldwell, Douglas/0000-0003-1963-9616; Howard, Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Barclay, Thomas/0000-0001-7139-2724; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; Kepler Participating Scientist Program; NSF; NASA; STScI; European Research Council under the European Community; Research Council of KU Leuven; FAS Science Division Research Computing Group at Harvard University FX Kepler was selected as the tenth NASA Discovery mission with funding provided by NASA's Science Mission Directorate. We thank the many people who made the Kepler mission a reality. W. F. W., J.A.O., E. B. F., A. P., L. R. D., J.J.F., M.J.H., T. M. and J.H.S. were supported by the Kepler Participating Scientist Program. W. F. W., J.A.O., D. R. S. and G. W. were supported by the NSF. D. C. F. and J.A.C. acknowledge NASA support through Hubble Fellowship grants, awarded by STScI, operated by AURA. J.N.W. was supported by the NASA Origins programme. S. B. acknowledges funding from the European Research Council under the European Community's Seventh Framework Programme (PROSPERITY) and from the Research Council of KU Leuven. Some of the reported computations were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. This Letter is based in part on observations made with the Nordic Optical Telescope (operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias), the W. M. Keck Observatory (operated by the University of California and the California Institute of Technology) and the Hobby-Eberly Telescope (HET; a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximillians-Universitat Munchen, and Georg-August-Universitat Goettingen). NR 22 TC 200 Z9 201 U1 1 U2 17 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 26 PY 2012 VL 481 IS 7382 BP 475 EP U85 DI 10.1038/nature10768 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 881GY UT WOS:000299471800033 PM 22237021 ER PT J AU Trattner, KJ Petrinec, SM Fuselier, SA Omidi, N Sibeck, DG AF Trattner, K. J. Petrinec, S. M. Fuselier, S. A. Omidi, N. Sibeck, D. G. TI Evidence of multiple reconnection lines at the magnetopause from cusp observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID FLUX-TRANSFER EVENTS; LOW-ALTITUDE OBSERVATIONS; SHEET BOUNDARY-LAYER; HIGH-LATITUDE; DAYSIDE RECONNECTION; MAGNETIC-FIELD; MAGNETOSPHERIC CUSP; QUANTITATIVE MODEL; NORTHWARD IMF; ION OUTFLOW AB Recent global hybrid simulations investigated the formation of flux transfer events (FTEs) and their convection and interaction with the cusp. Based on these simulations, we have analyzed several Polar cusp crossings in the Northern Hemisphere to search for the signature of such FTEs in the energy distribution of downward precipitating ions: precipitating ion beams at different energies parallel to the ambient magnetic field and overlapping in time. Overlapping ion distributions in the cusp are usually attributed to a combination of variable ion acceleration during the magnetopause crossing together with the time-of-flight effect from the entry point to the observing satellite. Most "step up" ion cusp structures (steps in the ion energy dispersions) only overlap for the populations with large pitch angles and not for the parallel streaming populations. Such cusp structures are the signatures predicted by the pulsed reconnection model, where the reconnection rate at the magnetopause decreased to zero, physically separating convecting flux tubes and their parallel streaming ions. However, several Polar cusp events discussed in this study also show an energy overlap for parallel-streaming precipitating ions. This condition might be caused by reopening an already reconnected field line, forming a magnetic island (flux rope) at the magnetopause similar to that reported in global MHD and Hybrid simulations. C1 [Trattner, K. J.; Petrinec, S. M.; Fuselier, S. A.] Lockheed Martin Space Syst Co, Adv Technol Ctr, Palo Alto, CA 94304 USA. [Omidi, N.] Solana Sci Inc, Solana Beach, CA 92075 USA. [Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Trattner, KJ (reprint author), Lockheed Martin Space Syst Co, Adv Technol Ctr, 3251 Hanover St,Bldg B255,A022S, Palo Alto, CA 94304 USA. EM karlheinz.j.trattner.dr@lmco.com RI Sibeck, David/D-4424-2012 FU NASA [NNX08AF35G, NNX09AM72G, NNX11AJ09G, NNG05GE15G]; NSF [AGS-1007449] FX We acknowledge the use of the ISTP KP database. Solar wind observations were provided by the Wind Solar Wind Experiment (Wind/SWE) [Ogilvie et al., 1995]. The IMF measurements were provided by the Wind Magnetic Field Instrument (Wind/MFI) [Lepping et al., 1995]. The work at Lockheed Martin was supported by NASA contracts NNX08AF35G, NNX09AM72G, NNX11AJ09G, and NNG05GE15G. N. Omidi acknowledges support from NSF grant AGS-1007449. NR 61 TC 4 Z9 4 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JAN 25 PY 2012 VL 117 AR A01213 DI 10.1029/2011JA017080 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 884IV UT WOS:000299699000002 ER PT J AU Macedo, MN DeFries, RS Morton, DC Stickler, CM Galford, GL Shimabukuro, YE AF Macedo, Marcia N. DeFries, Ruth S. Morton, Douglas C. Stickler, Claudia M. Galford, Gillian L. Shimabukuro, Yosio E. TI Decoupling of deforestation and soy production in the southern Amazon during the late 2000s SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE agriculture; land sparing; extensification; Brazilian Amazon ID LAND-USE CHANGE; BRAZILIAN AMAZON; AGRICULTURAL INTENSIFICATION; FORESTS; CONSEQUENCES; CONSERVATION; EXPANSION; REDD AB From 2006 to 2010, deforestation in the Amazon frontier state of Mato Grosso decreased to 30% of its historical average (1996-2005) whereas agricultural production reached an all-time high. This study combines satellite data with government deforestation and production statistics to assess land-use transitions and potential market and policy drivers associated with these trends. In the forested region of the state, increased soy production from 2001 to 2005 was entirely due to cropland expansion into previously cleared pasture areas (74%) or forests (26%). From 2006 to 2010, 78% of production increases were due to expansion (22% to yield increases), with 91% on previously cleared land. Cropland expansion fell from 10 to 2% of deforestation between the two periods, with pasture expansion accounting for most remaining deforestation. Declining deforestation coincided with a collapse of commodity markets and implementation of policy measures to reduce deforestation. Soybean profitability has since increased to pre-2006 levels whereas deforestation continued to decline, suggesting that antideforestation measures may have influenced the agricultural sector. We found little evidence of direct leakage of soy expansion into cerrado in Mato Grosso during the late 2000s, although indirect land-use changes and leakage to more distant regions are possible. This study provides evidence that reduced deforestation and increased agricultural production can occur simultaneously in tropical forest frontiers, provided that land is available and policies promote the efficient use of already-cleared lands (intensification) while restricting deforestation. It remains uncertain whether government- and industry-led policies can contain deforestation if future market conditions favor another boom in agricultural expansion. C1 [Macedo, Marcia N.; DeFries, Ruth S.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Morton, Douglas C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Galford, Gillian L.] Woods Hole Res Ctr, Falmouth, MA 02540 USA. [Stickler, Claudia M.] Inst Pesquisa Ambiental Amazonia, BR-71503505 Brasilia, DF, Brazil. [Shimabukuro, Yosio E.] Inst Nacl Pesquisas Espaciais, Div Sensoriamento Remoto, BR-12227010 Sao Jose Dos Campos, SP, Brazil. RP DeFries, RS (reprint author), Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. EM rd2402@columbia.edu RI Morton, Douglas/D-5044-2012; Galford, Gillian/K-6240-2012 OI Galford, Gillian/0000-0003-2192-7385 FU National Aeronautics and Space Administration [NNX08AX08H]; Gordon and Betty Moore Foundation; Packard Foundation; National Science Foundation [DEB-0949996, DEB-0743703] FX This manuscript was greatly improved by the constructive comments of Arild Angelsen, Paulo Brando, Victor Gutierrez-Velez, Ramon Lopez, and two anonymous reviewers. We thank Michael Coe, Christopher Neill, and the Instituto de Pesquisa Ambiental da Amazonia for logistical support in the field; and Rebecca de Sa and Darlisson Nunes da Costa for assistance with data collection. This work was funded by National Aeronautics and Space Administration Earth System Science Fellowship NNX08AX08H, The Gordon and Betty Moore Foundation, the Packard Foundation, and National Science Foundation Grants DEB-0949996 and DEB-0743703. NR 42 TC 159 Z9 163 U1 10 U2 122 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 24 PY 2012 VL 109 IS 4 BP 1341 EP 1346 DI 10.1073/pnas.1111374109 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 880NA UT WOS:000299412600068 PM 22232692 ER PT J AU Fritts, DC Janches, D Iimura, H Hocking, WK Bageston, JV Leme, NMP AF Fritts, D. C. Janches, D. Iimura, H. Hocking, W. K. Bageston, J. V. Leme, N. M. P. TI Drake Antarctic Agile Meteor Radar first results: Configuration and comparison of mean and tidal wind and gravity wave momentum flux measurements with Southern Argentina Agile Meteor Radar SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID DIURNAL PROPAGATING TIDE; LATENT-HEAT RELEASE; AMSU-A RADIANCES; JUNE-AUGUST 1999; LOWER THERMOSPHERE; PLANETARY-WAVES; MIDDLE ATMOSPHERE; POKER FLAT; MU RADAR; INTERANNUAL VARIABILITY AB A new generation meteor radar was installed at the Brazilian Antarctic Comandante Ferraz Base (62.1 degrees S) in March 2010. This paper describes the motivations for the radar location, its measurement capabilities, and comparisons of measured mean winds, tides, and gravity wave momentum fluxes from April to June of 2010 and 2011 with those by a similar radar on Tierra del Fuego (53.8 degrees S). Motivations for the radars include the "hotspot" of small-scale gravity wave activity extending from the troposphere into the mesosphere and lower thermosphere (MLT) centered over the Drake Passage, the maximum of the semidiurnal tide at these latitudes, and the lack of other MLT wind measurements in this latitude band. Mean winds are seen to be strongly modulated at planetary wave and longer periods and to exhibit strong coherence over the two radars at shorter time scales as well as systematic seasonal variations. The semidiurnal tide contributes most to the large-scale winds over both radars, with maximum tidal amplitudes during May and maxima at the highest altitudes varying from similar to 20 to >70 ms(-1). In contrast, the diurnal tide and various planetary waves achieve maximum winds of similar to 10 to 20 ms(-1). Monthly mean gravity wave momentum fluxes appear to reflect the occurrence of significant sources at lower altitudes, with relatively small zonal fluxes over both radars, but with significant, and opposite, meridional momentum fluxes below similar to 85 km. These suggest gravity waves propagating away from the Drake Passage at both sites, and may indicate an important source region accounting in part for this "hotspot." C1 [Fritts, D. C.; Iimura, H.] NW Res Associates, Colorado Res Associates Div, Boulder, CO USA. [Janches, D.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Bageston, J. V.; Leme, N. M. P.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [Hocking, W. K.] Univ Western Ontario, Dept Phys, London, ON N6A 3K7, Canada. RP Fritts, DC (reprint author), NW Res Associates, Colorado Res Associates Div, 3380 Mitchell Ln, Boulder, CO USA. EM dave@cora.nwra.com RI Janches, Diego/D-4674-2012 OI Janches, Diego/0000-0001-8615-5166 FU NSF [OPP-0839084, ATM-0634650]; Secretaria for the Interministerial Commission of Sea Resources (SECIRM); Brazilian Antarctic Program (PROANTAR); National Institute for Science and Technology; Antarctic Environmental Research (INCT-APA); ATMANTAR/MCT/CNPq, FAPERJ; FAPESP [2010/06608-2] FX Research described in this paper was performed under NSF grants OPP-0839084 and ATM-0634650. We are especially grateful to the Secretaria for the Interministerial Commission of Sea Resources (SECIRM), the Brazilian Antarctic Program (PROANTAR), the National Institute for Science and Technology, Antarctic Environmental Research (INCT-APA), and the ATMANTAR/MCT/CNPq project, FAPERJ, for their support of this research and visits to Ferraz Station to install and service DrAAMER. We are also very grateful for the valuable assistance of personnel at Estacion Astronomica Rio Grande (EARG) with the operations and maintenance of SAAMER. J. V. Bageston thanks FAPESP for his postdoctorate fellowship under the process number 2010/06608-2. Finally, we are indebted to MARDOC and Genesis Software for working with us to devise a radar configuration that met our measurement objectives. We also acknowledge use of the CEDAR database and the GSWM-09 website at NCAR for GSWM-09 results employed for our comparisons. NR 71 TC 13 Z9 13 U1 0 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JAN 21 PY 2012 VL 117 AR D02105 DI 10.1029/2011JD016651 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 880FN UT WOS:000299390400002 ER PT J AU Wood, EF Roundy, JK Troy, TJ van Beek, R Bierkens, M Blyth, E de Roo, A Doll, P Ek, M Famiglietti, J Gochis, D van de Giesen, N Houser, P Jaffe, P Kollet, S Lehner, B Lettenmaier, DP Peters-Lidard, CD Sivapalan, M Sheffield, J Wade, AJ Whitehead, P AF Wood, Eric F. Roundy, Joshua K. Troy, Tara J. van Beek, Rens Bierkens, Marc Blyth, Eleanor de Roo, Ad Doell, Petra Ek, Mike Famiglietti, James Gochis, David van de Giesen, Nick Houser, Paul Jaffe, Peter Kollet, Stefan Lehner, Bernhard Lettenmaier, Dennis P. Peters-Lidard, Christa D. Sivapalan, Murugesu Sheffield, Justin Wade, Andrew J. Whitehead, Paul TI Reply to comment by Keith J. Beven and Hannah L. Cloke on "Hyperresolution global land surface modeling: Meeting a grand challenge for monitoring Earth's terrestrial water'' SO WATER RESOURCES RESEARCH LA English DT Editorial Material C1 [Wood, Eric F.; Roundy, Joshua K.; Troy, Tara J.; Jaffe, Peter; Sheffield, Justin] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. [van Beek, Rens; Bierkens, Marc] Univ Utrecht, Dept Phys Geog, NL-3508 TC Utrecht, Netherlands. [Blyth, Eleanor] Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England. [de Roo, Ad] European Commiss Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy. [Doell, Petra] Goethe Univ Frankfurt, Inst Phys Geog, D-60054 Frankfurt, Germany. [Ek, Mike] Natl Ctr Environm Protect, Environm Modeling Ctr, Suitland, MD USA. [Famiglietti, James] Univ Calif Irvine, UC Ctr Hydrol Modeling, Irvine, CA 92697 USA. [Gochis, David] Natl Ctr Atmospher Res, Res Applicat Lab, Boulder, CO 80304 USA. [van de Giesen, Nick] Delft Univ Technol, Dept Water Management, NL-2628 CN Delft, Netherlands. [Houser, Paul] George Mason Univ, Dept Geog & GeoInformat Sci, Fairfax, VA 22030 USA. [Kollet, Stefan] Univ Bonn, Inst Meteorol, D-53121 Bonn, Germany. [Lehner, Bernhard] McGill Univ, Dept Geog, Montreal, PQ H3A 2K6, Canada. [Lettenmaier, Dennis P.] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA. [Peters-Lidard, Christa D.] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sivapalan, Murugesu] Univ Illinois, Dept Civil & Environm Engn, Urbana, IL 61801 USA. [Sivapalan, Murugesu] Univ Illinois, Dept Geog, Urbana, IL 61801 USA. [Wade, Andrew J.] Univ Reading, Sch Human & Environm Sci, Reading RG6 6DW, Berks, England. [Whitehead, Paul] Univ Oxford, Sch Geog & Environm, Oxford OX1 3QY, England. RP Wood, EF (reprint author), Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. EM efwood@princeton.edu RI Doll, Petra/A-3784-2009; Sivapalan, Murugesu/A-3538-2008; Blyth, Eleanor/A-4010-2009; van de Giesen, Nick/B-5010-2008; Houser, Paul/J-9515-2013; lettenmaier, dennis/F-8780-2011; Peters-Lidard, Christa/E-1429-2012; Roundy, Joshua/H-9377-2016; van Beek, Rens/B-4904-2014; OI Doll, Petra/0000-0003-2238-4546; Sivapalan, Murugesu/0000-0003-3004-3530; van de Giesen, Nick/0000-0002-7200-3353; Houser, Paul/0000-0002-2991-0441; lettenmaier, dennis/0000-0003-3317-1327; Peters-Lidard, Christa/0000-0003-1255-2876; Roundy, Joshua/0000-0003-0328-3248; van Beek, Rens/0000-0002-4758-108X; Troy, Tara/0000-0001-5366-0633; Wade, Andrew/0000-0002-5296-8350 NR 13 TC 9 Z9 9 U1 3 U2 42 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD JAN 21 PY 2012 VL 48 AR W01802 DI 10.1029/2011WR011202 PG 3 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 880DV UT WOS:000299385800004 ER PT J AU Abbasi, R Abdou, Y Abu-Zayyad, T Adams, J Aguilar, JA Ahlers, M Altmann, D Andeen, K Auffenberg, J Bai, X Baker, M Barwick, SW Bay, R Alba, JLB Beattie, K Beatty, JJ Bechet, S Becker, JK Becker, KH Benabderrahmane, ML BenZvi, S Berdermann, J Berghaus, P Berley, D Bernardini, E Bertrand, D Besson, DZ Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bose, D Boser, S Botner, O Brown, AM Buitink, S Caballero-Mora, KS Carson, M Chirkin, D Christy, B Clem, J Clevermann, F Cohen, S Colnard, C Cowen, DF D'Agostino, MV Danninger, M Daughhetee, J Davis, JC De Clercq, C Demirors, L Denger, T Depaepe, O Descamps, F Desiati, P de Vries-Uiterweerd, G DeYoung, T Diaz-Velez, JC Dierckxsens, M Dreyer, J Dumm, JP Ehrlich, R Eisch, J Ellsworth, RW Engdegard, O Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feintzeig, J Feusels, T Filimonov, K Finley, C Fischer-Wasels, T Foerster, MM Fox, BD Franckowiak, A Franke, R Gaisser, TK Gallagher, J Gerhardt, L Gladstone, L Glusenkamp, T Goldschmidt, A Goodman, JA Gora, D Grant, D Griesel, T Gross, A Grullon, S Gurtner, M Ha, C Hajismail, A Hallgren, A Halzen, F Han, K Hanson, K Heinen, D Helbing, K Herquet, P Hickford, S Hill, GC Hoffman, KD Homeier, A Hoshina, K Hubert, D Huelsnitz, W Hulss, JP Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobsen, J Japaridze, GS Johansson, H Joseph, JM Kampert, KH Kappes, A Karg, T Karle, A Kenny, P Kiryluk, J Kislat, F Klein, SR Kohne, JH Kohnen, G Kolanoski, H Kopke, L Kopper, S Koskinen, DJ Kowalski, M Kowarik, T Krasberg, M Krings, T Kroll, G Kurahashi, N Kuwabara, T Labare, M Lafebre, S Laihem, K Landsman, H Larson, MJ Lauer, R Lunemann, J Madsen, J Majumdar, P Marotta, A Maruyama, R Mase, K Matis, HS Meagher, K Merck, M Meszaros, P Meures, T Middell, E Milke, N Miller, J Montaruli, T Morse, R Movit, SM Nahnhauer, R Nam, JW Naumann, U Niessen, P Nygren, DR Odrowski, S Olivas, A Olivo, M O'Murchadha, A Ono, M Panknin, S Paul, L de los Heros, CP Petrovic, J Piegsa, A Pieloth, D Porrata, R Posselt, J Price, PB Przybylski, GT Rawlins, K Redl, P Resconi, E Rhode, W Ribordy, M Rizzo, A Rodrigues, JP Roth, P Rothmaier, F Rott, C Ruhe, T Rutledge, D Ruzybayev, B Ryckbosch, D Sander, HG Santander, M Sarkar, S Schatto, K Schmidt, T Schonwald, A Schukraft, A Schultes, A Schulz, O Schunck, M Seckel, D Semburg, B Seo, SH Sestayo, Y Seunarine, S Silvestri, A Slipak, A Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stephens, G Stezelberger, T Stokstad, RG Stossl, A Stoyanov, S Strahler, EA Straszheim, T Stur, M Sullivan, GW Swillens, Q Taavola, H Taboada, I Tamburro, A Tepe, A Ter-Antonyan, S Tilav, S Toale, PA Toscano, S Tosi, D Turcan, D van Eijndhoven, N Vandenbroucke, J Van Overloop, A van Santen, J Vehring, M Voge, M Walck, C Waldenmaier, T Wallraff, M Walter, M Weaver, C Wendt, C Westerhoff, S Whitehorn, N Wiebe, K Wiebusch, CH Williams, DR Wischnewski, R Wissing, H Wolf, M Wood, TR Woschnagg, K Xu, C Xu, XW Yodh, G Yoshida, S Zarzhitsky, P Zoll, M AF Abbasi, R. Abdou, Y. Abu-Zayyad, T. Adams, J. Aguilar, J. A. Ahlers, M. Altmann, D. Andeen, K. Auffenberg, J. Bai, X. Baker, M. Barwick, S. W. Bay, R. Alba, J. L. Bazo Beattie, K. Beatty, J. J. Bechet, S. Becker, J. K. Becker, K. -H. Benabderrahmane, M. L. BenZvi, S. Berdermann, J. Berghaus, P. Berley, D. Bernardini, E. Bertrand, D. Besson, D. Z. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bose, D. Boeser, S. Botner, O. Brown, A. M. Buitink, S. Caballero-Mora, K. S. Carson, M. Chirkin, D. Christy, B. Clem, J. Clevermann, F. Cohen, S. Colnard, C. Cowen, D. F. D'Agostino, M. V. Danninger, M. Daughhetee, J. Davis, J. C. De Clercq, C. Demiroers, L. Denger, T. Depaepe, O. Descamps, F. Desiati, P. de Vries-Uiterweerd, G. DeYoung, T. Diaz-Velez, J. C. Dierckxsens, M. Dreyer, J. Dumm, J. P. Ehrlich, R. Eisch, J. Ellsworth, R. W. Engdegard, O. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feintzeig, J. Feusels, T. Filimonov, K. Finley, C. Fischer-Wasels, T. Foerster, M. M. Fox, B. D. Franckowiak, A. Franke, R. Gaisser, T. K. Gallagher, J. Gerhardt, L. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Goodman, J. A. Gora, D. Grant, D. Griesel, T. Gross, A. Grullon, S. Gurtner, M. Ha, C. Hajismail, A. Hallgren, A. Halzen, F. Han, K. Hanson, K. Heinen, D. Helbing, K. Herquet, P. Hickford, S. Hill, G. C. Hoffman, K. D. Homeier, A. Hoshina, K. Hubert, D. Huelsnitz, W. Huelss, J. -P. Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jacobsen, J. Japaridze, G. S. Johansson, H. Joseph, J. M. Kampert, K. -H. Kappes, A. Karg, T. Karle, A. Kenny, P. Kiryluk, J. Kislat, F. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koepke, L. Kopper, S. Koskinen, D. J. Kowalski, M. Kowarik, T. Krasberg, M. Krings, T. Kroll, G. Kurahashi, N. Kuwabara, T. Labare, M. Lafebre, S. Laihem, K. Landsman, H. Larson, M. J. Lauer, R. Luenemann, J. Madsen, J. Majumdar, P. Marotta, A. Maruyama, R. Mase, K. Matis, H. S. Meagher, K. Merck, M. Meszaros, P. Meures, T. Middell, E. Milke, N. Miller, J. Montaruli, T. Morse, R. Movit, S. M. Nahnhauer, R. Nam, J. W. Naumann, U. Niessen, P. Nygren, D. R. Odrowski, S. Olivas, A. Olivo, M. O'Murchadha, A. Ono, M. Panknin, S. Paul, L. de los Heros, C. Perez Petrovic, J. Piegsa, A. Pieloth, D. Porrata, R. Posselt, J. Price, P. B. Przybylski, G. T. Rawlins, K. Redl, P. Resconi, E. Rhode, W. Ribordy, M. Rizzo, A. Rodrigues, J. P. Roth, P. Rothmaier, F. Rott, C. Ruhe, T. Rutledge, D. Ruzybayev, B. Ryckbosch, D. Sander, H. -G. Santander, M. Sarkar, S. Schatto, K. Schmidt, T. Schoenwald, A. Schukraft, A. Schultes, A. Schulz, O. Schunck, M. Seckel, D. Semburg, B. Seo, S. H. Sestayo, Y. Seunarine, S. Silvestri, A. Slipak, A. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stephens, G. Stezelberger, T. Stokstad, R. G. Stoessl, A. Stoyanov, S. Strahler, E. A. Straszheim, T. Stuer, M. Sullivan, G. W. Swillens, Q. Taavola, H. Taboada, I. Tamburro, A. Tepe, A. Ter-Antonyan, S. Tilav, S. Toale, P. A. Toscano, S. Tosi, D. Turcan, D. van Eijndhoven, N. Vandenbroucke, J. Van Overloop, A. van Santen, J. Vehring, M. Voge, M. Walck, C. Waldenmaier, T. Wallraff, M. Walter, M. Weaver, Ch. Wendt, C. Westerhoff, S. Whitehorn, N. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wischnewski, R. Wissing, H. Wolf, M. Wood, T. R. Woschnagg, K. Xu, C. Xu, X. W. Yodh, G. Yoshida, S. Zarzhitsky, P. Zoll, M. TI NEUTRINO ANALYSIS OF THE 2010 SEPTEMBER CRAB NEBULA FLARE AND TIME-INTEGRATED CONSTRAINTS ON NEUTRINO EMISSION FROM THE CRAB USING ICECUBE SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: general; ISM: supernova remnants; neutrinos; pulsars: individual (Crab Pulsar) ID HIGH-ENERGY NEUTRINOS; GAMMA-RAY FLARES; PULSAR WINDS; TELESCOPES; SIGNALS; SYSTEM AB We present the results of a search for high-energy muon neutrinos with the IceCube detector in coincidence with the Crab Nebula flare reported on 2010 September by various experiments. Due to the unusual flaring state of the otherwise steady source we performed a prompt analysis of the 79-string configuration data to search for neutrinos that might be emitted along with the observed. gamma-rays. We performed two different and complementary data selections of neutrino events in the time window of 10 days around the flare. One event selection is optimized for discovery of E-upsilon(2). neutrino spectrum typical of first-order Fermi acceleration. A similar event selection has also been applied to the 40-string data to derive the time-integrated limits to the neutrino emission from the Crab. The other event selection was optimized for discovery of neutrino spectra with softer spectral index and TeV energy cutoffs as observed for various Galactic sources in. gamma-rays. The 90% confidence level (CL) best upper limits on the Crab flux during the 10 day flare are 4.73 x 10(-11) cm(-2) s(-1) TeV-1 for an E-upsilon(2). neutrino spectrum and 2.50 x 10(-10) cm(-2) s(-1) TeV-1 for a softer neutrino spectra of E-upsilon(-2.7), as indicated by Fermi measurements during the flare. In this paper, we also illustrate the impact of the time-integrated limit on the Crab neutrino steady emission. The limit obtained using 375.5 days of the 40-string configuration is compared to existing models of neutrino production from the Crab and its impact on astrophysical parameters is discussed. The most optimistic predictions of some models are already rejected by the IceCube neutrino telescope with more than 90% CL. C1 [Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Hajismail, A.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium. [Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Adams, J.; Brown, A. M.; Gross, A.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Altmann, D.; Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Gluesenkamp, T.; Heinen, D.; Huelss, J. -P.; Krings, T.; Laihem, K.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Auffenberg, J.; Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Kopper, S.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Bai, X.; Berghaus, P.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bai, X.; Berghaus, P.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Franke, R.; Gora, D.; Han, K.; Kislat, F.; Lauer, R.; Majumdar, P.; Middell, E.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Tosi, D.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany. [Beattie, K.; Gerhardt, L.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Davis, J. C.; Rott, 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. [Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Meures, T.; Petrovic, J.; Swillens, Q.] Univ Libre Bruxelles, Sci Fac CP230, B-1050 Brussels, Belgium. [Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany. [Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Roth, P.; Schmidt, T.; Straszheim, T.; Sullivan, G. W.; Turcan, D.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Bose, D.; Buitink, S.; De Clercq, C.; Depaepe, O.; Hubert, D.; Labare, M.; Rizzo, A.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Boeser, S.; Denger, T.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Stuer, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; de los Heros, C. Perez; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Caballero-Mora, K. S.; Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Lafebre, S.; Larson, M. J.; Meszaros, P.; Rutledge, D.; Slipak, A.; Stephens, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Clevermann, F.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany. [Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany. [Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] So Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Grant, D.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Ishihara, A.; Mase, K.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Univ Berlin, Inst Phys, D-12489 Berlin, Germany. [Rawlins, K.] Univ Alaska, Dept Phys & Astron, Anchorage, AK 99508 USA. [Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados. [Toale, P. A.; Williams, D. R.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Montaruli, T.] Univ Bari, Dipartmento Fis, I-70126 Bari, Italy. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Abbasi, R (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. RI Taavola, Henric/B-4497-2011; Sarkar, Subir/G-5978-2011; Wiebusch, Christopher/G-6490-2012; Beatty, James/D-9310-2011; Kowalski, Marek/G-5546-2012; Tamburro, Alessio/A-5703-2013; Hallgren, Allan/A-8963-2013; Botner, Olga/A-9110-2013; Tjus, Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014; Koskinen, David/G-3236-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013 OI Taavola, Henric/0000-0002-2604-2810; Buitink, Stijn/0000-0002-6177-497X; Carson, Michael/0000-0003-0400-7819; Hubert, Daan/0000-0002-4365-865X; Benabderrahmane, Mohamed Lotfi/0000-0003-4410-5886; Sarkar, Subir/0000-0002-3542-858X; Wiebusch, Christopher/0000-0002-6418-3008; Beatty, James/0000-0003-0481-4952; Perez de los Heros, Carlos/0000-0002-2084-5866; Auffenberg, Jan/0000-0002-1185-9094; Koskinen, David/0000-0002-0514-5917; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X FU U.S. National Science Foundation-Office; U.S. National Science Foundation-Physics Division; University of Wisconsin Alumni Research Foundation; Grid Laboratory of Wisconsin (GLOW); Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy; Louisiana Optical Network Initiative (LONI); National Science and Engineering Research Council of Canada; Swedish Research Council; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Deutsche Forschungsgemeinschaft (DFG); Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO; 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; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland; EU; Capes Foundation, Ministry of Education of Brazil; National Energy Research Scientific Computing Center; Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF) 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; National Science and Engineering Research Council of 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), 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; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; A. GroB acknowledges support by the EU Marie Curie OIF Program; J. P. Rodrigues acknowledges support by the Capes Foundation, Ministry of Education of Brazil. NR 43 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 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 45 DI 10.1088/0004-637X/745/1/45 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600045 ER PT J AU Barbary, K Aldering, G Amanullah, R Brodwin, M Connolly, N Dawson, KS Doi, M Eisenhardt, P Faccioli, L Fadeyev, V Fakhouri, HK Fruchter, AS Gilbank, DG Gladders, MD Goldhaber, G Goobar, A Hattori, T Hsiao, E Huang, X Ihara, Y Kashikawa, N Koester, B Konishi, K Kowalski, M Lidman, C Lubin, L Meyers, J Morokuma, T Oda, T Panagia, N Perlmutter, S Postman, M Ripoche, P Rosati, P Rubin, D Schlegel, DJ Spadafora, AL Stanford, SA Strovink, M Suzuki, N Takanashi, N Tokita, K Yasuda, N AF Barbary, K. Aldering, G. Amanullah, R. Brodwin, M. Connolly, N. Dawson, K. S. Doi, M. Eisenhardt, P. Faccioli, L. Fadeyev, V. Fakhouri, H. K. Fruchter, A. S. Gilbank, D. G. Gladders, M. D. Goldhaber, G. Goobar, A. Hattori, T. Hsiao, E. Huang, X. Ihara, Y. Kashikawa, N. Koester, B. Konishi, K. Kowalski, M. Lidman, C. Lubin, L. Meyers, J. Morokuma, T. Oda, T. Panagia, N. Perlmutter, S. Postman, M. Ripoche, P. Rosati, P. Rubin, D. Schlegel, D. J. Spadafora, A. L. Stanford, S. A. Strovink, M. Suzuki, N. Takanashi, N. Tokita, K. Yasuda, N. CA Supernova Cosmology Project TI THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. VI. THE VOLUMETRIC TYPE Ia SUPERNOVA RATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; supernovae: general; white dwarfs ID DIGITAL SKY SURVEY; SUBARU DEEP FIELD; SIMILAR-TO 1; GALAXY CLUSTERS; LEGACY SURVEY; STAR-FORMATION; COSMOLOGICAL CONSTRAINTS; XMMXCS J2215.9-1738; II SUPERNOVAE; LIGHT CURVES AB We present a measurement of the volumetric Type Ia supernova (SN Ia) rate out to z similar or equal to 1.6 from the Hubble Space Telescope Cluster Supernova Survey. In observations spanning 189 orbits with the Advanced Camera for Surveys we discovered 29 SNe, of which approximately 20 are SNe Ia. Twelve of these SNe Ia are located in the foregrounds and backgrounds of the clusters targeted in the survey. Using these new data, we derive the volumetric SN Ia rate in four broad redshift bins, finding results consistent with previous measurements at z greater than or similar to 1 and strengthening the case for an SN Ia rate that is greater than or similar to 0.6 x 10(-4) h(70)(3) yr(-1) Mpc(-3) at z similar to 1 and flattening out at higher redshift. We provide SN candidates and efficiency calculations in a form that makes it easy to rebin and combine these results with other measurements for increased statistics. Finally, we compare the assumptions about host-galaxy dust extinction used in different high-redshift rate measurements, finding that different assumptions may induce significant systematic differences between measurements. C1 [Barbary, K.; Amanullah, R.; Fakhouri, H. K.; Goldhaber, G.; Huang, X.; Meyers, J.; Perlmutter, S.; Rubin, D.; Strovink, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Barbary, K.; Aldering, G.; Dawson, K. S.; Fakhouri, H. K.; Goldhaber, G.; Hsiao, E.; Meyers, J.; Perlmutter, S.; Ripoche, P.; Rubin, D.; Schlegel, D. J.; Spadafora, A. L.; Strovink, M.; Suzuki, N.] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Amanullah, R.; Faccioli, L.; Goobar, A.] Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden. [Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Connolly, N.] Dept Phys, Hamilton Coll, Clinton, NY 13323 USA. [Dawson, K. S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Doi, M.; Ihara, Y.; Morokuma, T.; Tokita, K.] Univ Tokyo, Inst Astron, Grad Sch Sci, Mitaka, Tokyo 1810015, Japan. [Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fadeyev, V.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 94064 USA. [Fruchter, A. S.; Panagia, N.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gilbank, D. G.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Gladders, M. D.; Koester, B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Goobar, A.] Stockholm Univ, Albanova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden. [Hattori, T.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Kashikawa, N.; Morokuma, T.; Takanashi, N.] Univ Tokyo, Inst Ind Sci, Meguro Ku, Tokyo 1538505, Japan. [Koester, B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Konishi, K.; Yasuda, N.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Kowalski, M.] Univ Bonn, Inst Phys, Bonn, Germany. [Lidman, C.] Australian Astron Observ, Epping, NSW 1710, Australia. [Lubin, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95618 USA. [Oda, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Rosati, P.] ESO, D-85748 Garching, Germany. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. RP Barbary, K (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. EM kbarbary@lbl.gov RI Kowalski, Marek/G-5546-2012; Perlmutter, Saul/I-3505-2015; OI Perlmutter, Saul/0000-0002-4436-4661; Strovink, Mark/0000-0001-7020-7769; Meyers, Joshua/0000-0002-2308-4230 FU NASA from Space Telescope Science Institute [GO-10496]; NASA [NAS 5-26555]; Office of Science, Office of High Energy and Nuclear Physics, of the U.S. Department of Energy [AC02-05CH11231]; JSPS [20040003] FX Financial support for this work was provided by NASA through program GO-10496 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. This work was also supported in part by the Director, Office of Science, Office of High Energy and Nuclear Physics, of the U.S. Department of Energy under Contract No. AC02-05CH11231, as well as a JSPS core-to-core program "International Research Network for Dark Energy" and by a JSPS research grant (20040003). The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Finally, this work would not have been possible without the dedicated efforts of the daytime and nighttime support staff at the Cerro Paranal Observatory.; STScI is operated by the association of Universities for Research in Astronomy, Inc., under the NASA contract NAS 5-26555. The observations are associated with program GO-10496. NR 67 TC 15 Z9 15 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 31 DI 10.1088/0004-637X/745/1/31 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600031 ER PT J AU Barbary, K Aldering, G Amanullah, R Brodwin, M Connolly, N Dawson, KS Doi, M Eisenhardt, P Faccioli, L Fadeyev, V Fakhouri, HK Fruchter, AS Gilbank, DG Gladders, MD Goldhaber, G Goobar, A Hattori, T Hsiao, E Huang, X Ihara, Y Kashikawa, N Koester, B Konishi, K Kowalski, M Lidman, C Lubin, L Meyers, J Morokuma, T Oda, T Panagia, N Perlmutter, S Postman, M Ripoche, P Rosati, P Rubin, D Schlegel, DJ Spadafora, AL Stanford, SA Strovink, M Suzuki, N Takanashi, N Tokita, K Yasuda, N AF Barbary, K. Aldering, G. Amanullah, R. Brodwin, M. Connolly, N. Dawson, K. S. Doi, M. Eisenhardt, P. Faccioli, L. Fadeyev, V. Fakhouri, H. K. Fruchter, A. S. Gilbank, D. G. Gladders, M. D. Goldhaber, G. Goobar, A. Hattori, T. Hsiao, E. Huang, X. Ihara, Y. Kashikawa, N. Koester, B. Konishi, K. Kowalski, M. Lidman, C. Lubin, L. Meyers, J. Morokuma, T. Oda, T. Panagia, N. Perlmutter, S. Postman, M. Ripoche, P. Rosati, P. Rubin, D. Schlegel, D. J. Spadafora, A. L. Stanford, S. A. Strovink, M. Suzuki, N. Takanashi, N. Tokita, K. Yasuda, N. CA Supernova Cosmology Project TI THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. II. THE TYPE Ia SUPERNOVA RATE IN HIGH-REDSHIFT GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; supernovae: general; white dwarfs ID DELAY-TIME DISTRIBUTION; DIGITAL SKY SURVEY; INTRACLUSTER PLANETARY-NEBULAE; CORE-COLLAPSE SUPERNOVAE; DIFFUSE OPTICAL LIGHT; IRAC SHALLOW SURVEY; SIMILAR-TO 1; X-RAY; LUMINOSITY FUNCTION; VIRGO-CLUSTER AB We report a measurement of the Type Ia supernova (SN Ia) rate in galaxy clusters at 0.9 < z < 1.46 from the Hubble Space Telescope Cluster Supernova Survey. This is the first cluster SN Ia rate measurement with detected z > 0.9 SNe. Finding 8 +/- 1 cluster SNe Ia, we determine an SN Ia rate of 0.50(-0.19)(+0.23) (stat) (+0.10)(-0.09) (sys) h(70)(2) SNuB (SNuB equivalent to 10(-12) SNe (L-1)circle dot(,B) yr(-1)). In units of stellar mass, this translates to 0.36(-0.13)(+0.16) (stat) (+0.07)(-0.06) (sys) h(70)(2) SNuM (SNuM = 10(-12) SNe M-1 circle dot yr(-1)). This represents a factor of approximate to 5 +/- 2 increase over measurements of the cluster rate at z < 0.2. We parameterize the late-time SN Ia delay time distribution (DTD) with a power law: Psi(t) t(s). Under the approximation of a single-burst cluster formation redshift of z(f) = 3, our rate measurement in combination with lower-redshift cluster SN Ia rates constrains s = -1.41(-0.40)(+0.47), consistent with measurements of the DTD in the field. This measurement is generally consistent with expectations for the "double degenerate" scenario and inconsistent with some models for the "single degenerate" scenario predicting a steeper DTD at large delay times. We check for environmental dependence and the influence of younger stellar populations by calculating the rate specifically in cluster red-sequence galaxies and in morphologically early-type galaxies, finding results similar to the full cluster rate. Finally, the upper limit of one hostless cluster SN Ia detected in the survey implies that the fraction of stars in the intra-cluster medium is less than 0.47 (95% confidence), consistent with measurements at lower redshifts. C1 [Barbary, K.; Amanullah, R.; Fakhouri, H. K.; Goldhaber, G.; Huang, X.; Meyers, J.; Perlmutter, S.; Rubin, D.; Strovink, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Barbary, K.; Aldering, G.; Dawson, K. S.; Faccioli, L.; Fakhouri, H. K.; Goldhaber, G.; Hsiao, E.; Meyers, J.; Perlmutter, S.; Ripoche, P.; Rubin, D.; Schlegel, D. J.; Spadafora, A. L.; Strovink, M.; Suzuki, N.] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Amanullah, R.; Goobar, A.] Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden. [Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Connolly, N.] Hamilton Coll, Dept Phys, Clinton, NY 13323 USA. [Dawson, K. S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Doi, M.; Ihara, Y.; Morokuma, T.; Tokita, K.] Univ Tokyo, Grad Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fadeyev, V.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 94064 USA. [Fruchter, A. S.; Panagia, N.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gilbank, D. G.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Gladders, M. D.; Koester, B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Goobar, A.] Stockholm Univ, Albanova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden. [Hattori, T.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Kashikawa, N.; Morokuma, T.; Takanashi, N.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Koester, B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Konishi, K.; Yasuda, N.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Kowalski, M.] Univ Bonn, Inst Phys, Bonn, Germany. [Lidman, C.] Australian Astron Observ, Epping, NSW 1710, Australia. [Lubin, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95618 USA. [Oda, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Rosati, P.] ESO, D-85748 Garching, Germany. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. RP Barbary, K (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. EM kbarbary@lbl.gov RI Kowalski, Marek/G-5546-2012; Perlmutter, Saul/I-3505-2015; OI Perlmutter, Saul/0000-0002-4436-4661; Strovink, Mark/0000-0001-7020-7769; Meyers, Joshua/0000-0002-2308-4230 FU Japan Society for the Promotion of Science (JSPS) [20040003]; Australian Research Council (ARC); NASA from Space Telescope Science Institute [GO-10496]; Office of Science, Office of High Energy and Nuclear Physics U.S. Department of Energy [AC02-05CH11231]; NASA [NAS 5-26555] FX We thank Eric Bell and DanMaoz for helpful discussion. T. M. is financially supported by the Japan Society for the Promotion of Science (JSPS) through the JSPS Research Fellowship. C. L. is financially supported by the Australian Research Council (ARC) through the ARC Future Fellowship program. Financial support for this work was provided by NASA through program GO-10496 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. This work was also supported in part by the Director, Office of Science, Office of High Energy and Nuclear Physics, of the U.S. Department of Energy under Contract No. AC02-05CH11231, as well as a JSPS core-to-core program "International Research Network for Dark Energy" and by a JSPS research grant (20040003). The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Finally, this work would not have been possible without the dedicated efforts of the daytime and nighttime support staff at the Cerro Paranal Observatory. NR 147 TC 25 Z9 27 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 32 DI 10.1088/0004-637X/745/1/32 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600032 ER PT J AU Folatelli, G Phillips, MM Morrell, N Tanaka, M Maeda, K Nomoto, K Stritzinger, M Burns, CR Hamuy, M Mazzali, P Boldt, L Campillay, A Contreras, C Gonzalez, S Roth, M Salgado, F Freedman, WL Madore, BF Persson, SE Suntzeff, NB AF Folatelli, Gaston Phillips, M. M. Morrell, Nidia Tanaka, Masaomi Maeda, Keiichi Nomoto, Ken'ichi Stritzinger, Maximilian Burns, Christopher R. Hamuy, Mario Mazzali, Paolo Boldt, Luis Campillay, Abdo Contreras, Carlos Gonzalez, Sergio Roth, Miguel Salgado, Francisco Freedman, W. L. Madore, Barry F. Persson, S. E. Suntzeff, Nicholas B. TI UNBURNED MATERIAL IN THE EJECTA OF TYPE Ia SUPERNOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; techniques: spectroscopic ID DELAYED DETONATION MODELS; EARLY SPECTRAL EVOLUTION; PHOTOMETRY DATA RELEASE; WHITE-DWARF MODELS; LIGHT CURVES; EXPLOSION MODELS; ABUNDANCE STRATIFICATION; SN 2004EO; CARBON; PROJECT AB The presence of unburned material in the ejecta of normal Type Ia supernovae (SNe Ia) is investigated using early-time spectroscopy obtained by the Carnegie Supernova Project. The tell-tale signature of pristine material from a C+O white dwarf progenitor star is the presence of carbon, as oxygen is also a product of carbon burning. The most prominent carbon lines in optical spectra of SNe Ia are expected to arise from C II. We find that at least 30% of the objects in the sample show an absorption at approximate to 6300 angstrom which is attributed to C II lambda 6580. An alternative identification of this absorption as Ha is considered to be unlikely. These findings imply a larger incidence of carbon in SNe Ia ejecta than previously noted. We show how observational biases and physical conditions may hide the presence of weak C II lines, and account for the scarcity of previous carbon detections in the literature. This relatively large frequency of carbon detections has crucial implications on our understanding of the explosive process. Furthermore, the identification of the 6300 angstrom absorptions as carbon would imply that unburned material is present at very low expansion velocities, merely approximate to 1000 km s(-1) above the bulk of Si II. Based on spectral modeling, it is found that the detections are consistent with a mass of carbon of 10(-3) to 10(-2) M-circle dot. The presence of this material so deep in the ejecta would imply substantial mixing, which may be related to asymmetries of the flame propagation. Another possible explanation for the carbon absorptions may be the existence of clumps of unburned material along the line of sight. However, the uniformity of the relation between C II and Si II velocities is not consistent with such small-scale asymmetries. The spectroscopic and photometric properties of SNe Ia with and without carbon signatures are compared. A trend toward bluer color and lower luminosity at maximum light is found for objects which show carbon. C1 [Folatelli, Gaston; Tanaka, Masaomi; Maeda, Keiichi; Nomoto, Ken'ichi] Univ Tokyo, IPMU, Kashiwa, Chiba 2778583, Japan. [Folatelli, Gaston; Hamuy, Mario] Univ Chile, Dept Astron, Santiago, Chile. [Phillips, M. M.; Morrell, Nidia; Campillay, Abdo; Gonzalez, Sergio; Roth, Miguel] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Stritzinger, Maximilian] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Stritzinger, Maximilian] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Burns, Christopher R.; Freedman, W. L.; Madore, Barry F.; Persson, S. E.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Mazzali, Paolo] Ist Naz Astrofis Oss Astron, I-35122 Padua, Italy. [Boldt, Luis] Univ Bonn, Argelander Inst Astron, D-53111 Bonn, Germany. [Contreras, Carlos] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Salgado, Francisco] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Madore, Barry F.] CALTECH, Jet Prop Lab, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Suntzeff, Nicholas B.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. RP Folatelli, G (reprint author), Univ Tokyo, IPMU, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan. EM gaston.folatelli@ipmu.jp RI Nomoto, Ken'ichi/A-4393-2011; Hamuy, Mario/G-7541-2016; OI stritzinger, maximilian/0000-0002-5571-1833 FU NSF [AST-0306969, AST-0908886, AST-0607438, AST-1008343]; Danish NSF; World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan; CONICYT [1060808]; Centro de Astrofisica FONDAP [15010003]; Centro BASAL CATA [PFB-06]; Millennium Center for Supernova Science [P06-045-F]; [23740175] FX We are grateful to Wojtek Krzeminski for his dedicated efforts during the CSP campaigns. We also thank Luc Dessart for his useful suggestions, and Joseph Anderson, Francisco Forster, Giuliano Pignata, and the rest of the MCSS team for interesting discussions on the topic of this paper. This material is based upon work supported by NSF under grants AST-0306969, AST-0908886, AST-0607438, and AST-1008343. The Dark Cosmology Centre is funded by the Danish NSF. This research is supported by the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. G. F. acknowledges financial support by Grant-in-Aid for Scientific Research for Young Scientists (23740175). M. H. acknowledges support by CONICYT through grants FONDECYT Regular 1060808, Centro de Astrofisica FONDAP 15010003, Centro BASAL CATA (PFB-06), and by the Millennium Center for Supernova Science (P06-045-F). NR 76 TC 38 Z9 38 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 74 DI 10.1088/0004-637X/745/1/74 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600074 ER PT J AU Fressin, F Torres, G Pont, F Knutson, HA Charbonneau, D Mazeh, T Aigrain, S Fridlund, M Henze, CE Guillot, T Rauer, H AF Fressin, Francois Torres, Guillermo Pont, Frederic Knutson, Heather A. Charbonneau, David Mazeh, Tsevi Aigrain, Suzanne Fridlund, Malcolm Henze, Christopher E. Guillot, Tristan Rauer, Heike TI SPITZER INFRARED OBSERVATIONS AND INDEPENDENT VALIDATION OF THE TRANSITING SUPER- EARTH CoRoT-7 b SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; planetary systems; stars: individual: CoRoT-7; stars: statistics; techniques: photometric ID SPACE-TELESCOPE; EMISSION-SPECTRUM; PLANET CANDIDATES; BLEND SCENARIOS; MULTIPLE SYSTEM; LIGHT CURVES; ARRAY CAMERA; HD 189733B; LOW-MASS; VARIABILITY AB The detection and characterization of the first transiting super-Earth, CoRoT-7 b, has required an unprecedented effort in terms of telescope time and analysis. Although the star does display a radial-velocity signal at the period of the planet, this has been difficult to disentangle from the intrinsic stellar variability and pinning down the velocity amplitude has been very challenging. As a result, the precise value of the mass of the planet-and even the extent to which it can be considered to be confirmed-has been debated in the recent literature, with six mass measurements published so far based on the same spectroscopic observations, ranging from about 2 to 8 Earth masses. Here we report on an independent validation of the planet discovery using one of the fundamental properties of a transit signal: its achromaticity. We observed four transits of CoRoT-7 b at 4.5 mu m and 8.0 mu m with the Infrared Array Camera (IRAC) on board the Spitzer Space Telescope in order to determine whether the depth of the transit signal in the near-infrared is consistent with that observed in the CoRoT bandpass, as expected for a planet. We detected the transit and found an average depth of 0.426 +/- 0.115 mmag at 4.5 mu m, which is in good agreement with the depth of 0.350 +/- 0.011 mmag (ignoring limb darkening) found by CoRoT. The observations at 8.0 mu m did not yield a significant detection. The 4.5 mu m observations place important constraints on the kinds of astrophysical false positives that could mimic the signal. Combining this with additional constraints reported earlier, we performed an exhaustive exploration of possible blend scenarios for CoRoT-7 b using the BLENDER technique. We are able to rule out the vast majority of false positives, and the remaining ones are found to be much less likely than a true transiting planet. We thus validate CoRoT-7 b as a bona fide planet with a very high degree of confidence, independently of any radial-velocity information. Our Spitzer observations have additionally allowed us to significantly improve the ephemeris of the planet, so that future transits should be recoverable well into the next decade. In its warm phase Spitzer is expected to be an essential tool for the validation, along the lines of the present analysis, of transiting planet candidates with shallow signals from CoRoT as well as from the Kepler mission, including potentially rocky planets in the habitable zones of their parent stars. C1 [Fressin, Francois; Torres, Guillermo; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pont, Frederic] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Mazeh, Tsevi] Tel Aviv Univ, Dept Astron & Astrophys, IL-69978 Tel Aviv, Israel. [Aigrain, Suzanne] Univ Oxford, Oxford OX1 3RH, England. [Fridlund, Malcolm] ESTEC ESA, NL-2200 AG Noordwijk, Netherlands. [Henze, Christopher E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Guillot, Tristan] Observ Cote Azur, F-06304 Nice, France. [Rauer, Heike] Deutsch Zentrum Luft & Raumfahrt DLR, D-12489 Berlin, Germany. RP Fressin, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ffressin@cfa.harvard.edu OI Charbonneau, David/0000-0002-9003-484X FU NASA FX We are grateful to the anonymous referee for many very helpful comments and suggestions. 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 contract to NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This research has made use of the facilities at the NASA Advanced Supercomputing Division (NASA Ames Research Center). NR 42 TC 9 Z9 9 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 81 DI 10.1088/0004-637X/745/1/81 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600081 ER PT J AU Gong, Y Cooray, A Silva, M Santos, MG Bock, J Bradford, CM Zemcov, M AF Gong, Yan Cooray, Asantha Silva, Marta Santos, Mario G. Bock, James Bradford, C. Matt Zemcov, Michael TI INTENSITY MAPPING OF THE [C II] FINE STRUCTURE LINE DURING THE EPOCH OF REIONIZATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; diffuse radiation; intergalactic medium; large-scale structure of universe ID 158 MU-M; FAR-INFRARED SPECTROSCOPY; STAR-FORMATION RATE; INTERSTELLAR-MEDIUM; CHEMICAL EVOLUTION; MOLECULAR GAS; GALAXIES; EMISSION; CII; SIMULATIONS AB The atomic C II fine-structure line is one of the brightest lines in a typical star-forming galaxy spectrum with a luminosity similar to 0.1%-1% of the bolometric luminosity. It is potentially a reliable tracer of the dense gas distribution at high redshifts and could provide an additional probe to the era of reionization. By taking into account the spontaneous, stimulated, and collisional emission of the C II line, we calculate the spin temperature and the mean intensity as a function of the redshift. When averaged over a cosmologically large volume, we find that the C II emission from ionized carbon in individual galaxies is larger than the signal generated by carbon in the intergalactic medium. Assuming that the C II luminosity is proportional to the carbon mass in dark matter halos, we also compute the power spectrum of the C II line intensity at various redshifts. In order to avoid the contamination from CO rotational lines at low redshift when targeting a C II survey at high redshifts, we propose the cross-correlation of C II and 21