FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Arab-Sedze, M Heggy, E Bretar, F Berveiller, D Jacquemoud, S AF Arab-Sedze, M. Heggy, E. Bretar, F. Berveiller, D. Jacquemoud, S. TI Quantification of L-band InSAR coherence over volcanic areas using LiDAR and in situ measurements SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Radar coherence; L-band; LiDAR; Volcanic areas; Surface roughness; Radar wave penetration; Vegetation density; Piton de la Fournaise ID GROUND-PENETRATING RADAR; INTERFEROMETRIC RADAR; VEGETATION INDEXES; FOURNAISE VOLCANO; REUNION-ISLAND; PINE FOREST; LASER; DECORRELATION; SURFACE; PITON AB Interferometric Synthetic Aperture Radar (InSAR) is a powerful tool to monitor large-scale ground deformation at active volcanoes. However, vegetation and pyroclastic deposits degrade the radar coherence and therefore the measurement of 3-D surface displacements. In this article, we explore the complementarity between ALOS-PALSAR coherence images, airborne LiDAR data and in situ measurements acquired over the Piton de La Fournaise volcano (Reunion Island, France) to determine the sources of errors that may affect repeat-pass InSAR measurements. We investigate three types of surfaces: terrains covered with vegetation, lava flows (a'a, pahoehoe or slabby pahoehoe lava flows) and pyroclastic deposits (lapilli). To explain the loss of coherence observed over the Dolomieu crater between 2008 and 2009, we first use laser altimetry data to map topographic variations. The LiDAR intensity, which depends on surface reflectance, also provides ancillary information about the potential sources of coherence loss. In addition, surface roughness and rock dielectric properties of each terrain have been determined in situ to better understand how electromagnetic waves interact with such media: rough and porous surfaces, such as the a'a lava flows, produce a higher coherence loss than smoother surfaces, such as the pahoehoe lava flows. Variations in dielectric properties suggest a higher penetration depth in pyroclasts than in lava flows at L-band frequency. Decorrelation over the lapilli is hence mainly caused by volumetric effects. Finally, a map of LAI (Leaf Area Index) produced using SPOT 5 imagery allows us to quantify the effect of vegetation density: radar coherence is negatively correlated with LAI and is unreliable for values higher than 7.5. (C) 2014 Elsevier Inc. All rights reserved. C1 [Arab-Sedze, M.; Jacquemoud, S.] Univ Paris Diderot, Sorbonne Paris Cite, Inst Phys Globe Paris, UMR CNRS 7154, F-75013 Paris, France. [Arab-Sedze, M.] Inst Natl Informat Geog & Forestiere, Lab MATIS, F-94160 St Mande, France. [Heggy, E.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Bretar, F.] Consulat Gen France Shanghai, Serv Sci & Technol, Shanghai 200001, Peoples R China. [Berveiller, D.] Univ Paris 11, AgroParisTech, CNRS, Lab Ecol Systemat & Evolut ESE,UMR 8079, F-91405 Orsay, France. RP Arab-Sedze, M (reprint author), Inst Phys Globe Paris, Batiment Lamarck A,Case 7071, F-75013 Paris, France. EM sedze@ipgp.fr; essam.heggy@jpl.nasa.gov; frederic.bretar@ieee.org; daniel.berveiller@u-psud.fr; jacquemoud@ipgp.fr RI Jacquemoud, Stephane/F-8842-2010 FU CNES; National Aeronautics and Space Administration FX This work was funded by the CNES Terre Ocean Surfaces Continentales Atmosphere (TOSCA) program from 2011 to 2013 in the frame of the DEVOIR (DEformation of active vegetated VOlcanos using Insar and lidaR) project. The Institut national de l'information geographique et forestiere kindly provided the LiDAR data. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank our colleagues from the Observatoire Volcanologique du Piton de la Fournaise (OVPF) for their support during the geophysical survey. NR 63 TC 1 Z9 1 U1 6 U2 21 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD SEP PY 2014 VL 152 BP 202 EP 216 DI 10.1016/j.rse.2014.06.011 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AR2CW UT WOS:000343392200017 ER PT J AU Ramsey, E Rangoonwala, A Chi, ZH Jones, CE Bannister, T AF Ramsey, Elijah, III Rangoonwala, Arnina Chi, Zhaohui Jones, Cathleen E. Bannister, Terri TI Marsh Dieback, loss, and recovery mapped with satellite optical, airborne polarimetric radar, and field data SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Spartina alterniflora marsh dieback; Optical vegetation indexes; NASA UAVSAR; Polarimetric synthetic aperture radar (PoISAR); Coastal wetlands ID SPARTINA-ALTERNIFLORA DIEBACK; COAST SALT MARSHES; LEAF-AREA INDEX; L-BAND; C-BAND; LOUISIANA; REFLECTANCE; VEGETATION; SAR; WETLAND AB Landsat Thematic Mapper and Satellite Pour l'Observation de la Terre (SPOT) satellite based optical sensors, NASA Uninhabited Aerial Vehicle synthetic aperture radar (UAVSAR) polarimetric SAR (PolSAR), and field data captured the occurrence and the recovery of an undetected dieback that occurred between the summers of 2010, 2011, and 2012 in the Spartina alterniflora marshes of coastal Louisiana. Field measurements recorded the dramatic biomass decrease from 2010 to 2011 and a biomass recovery in 2012 dominated by a decrease of live biomass, and the loss of marsh as part of the dieback event. Based on an established relationship, the near-infrared/red vegetation index (VI) and site-specific measurements delineated a contiguous expanse of marsh dieback encompassing 6649.9 ha of 18,2923 ha of S. alterniflora marshes within the study region. PoISAR data were transformed to variables used in biophysical mapping, and of this variable suite, the cross-polarization HV (horizontal send and vertical receive) backscatter was the best single indicator of marsh dieback and recovery. HV backscatter exhibited substantial and significant changes over the dieback and recovery period, tracked measured biomass changes, and significantly correlated with the live/dead biomass ratio. Within the context of regional trends, both HV and VI indicators started higher in pre-dieback marshes and exhibited substantially and statistically higher variability from year to year than that exhibited in the non-dieback marshes. That distinct difference allowed the capturing of the S. altemiflora marsh dieback and recovery; however, these changes were incorporated in a regional trend exhibiting similar but more subtle biomass composition changes. Published by Elsevier Inc. C1 [Ramsey, Elijah, III] US Geol Survey, Natl Wetlands Res Ctr, Lafayette, LA 70506 USA. [Rangoonwala, Arnina] Five Rivers Serv LLC, Colorado Springs, CO 80918 USA. [Chi, Zhaohui; Bannister, Terri] Univ Louisiana Lafayette, CESU, Lafayette, LA 70506 USA. [Jones, Cathleen E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ramsey, E (reprint author), US Geol Survey, Natl Wetlands Res Ctr, 700 Cajundome Blvd, Lafayette, LA 70506 USA. EM ramseye@usgs.gov FU National Aeronautics Space Administration (NASA) [11-TE11-104]; collaboration with the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA FX We thank Francis Fields Jr. of the Apache Louisiana Minerals LLC, a subsidiary of Apache Corporation, for access to their properties. We also thank Ryan Longhenry, Data Management Specialist, U.S. Geological Survey (USGS), Earth Resources Observation and Science (EROS) Center and Carolyn Gacke, contractor Science Applications International Corporation at USGS EROS Center for the help and support in providing the SPOT satellite data. We appreciate the help by Sijan Sapkota of the U.S. Geological Survey for his assistance in developing statistical models. We appreciate the review of the manuscript by John liames, Research Biologist at U.S. Environmental Protection Agency, and Dirk Werle of AERDE Environmental Research, Canada. We also thank the two anonymous reviewers for their exhaustive, judicious and perceptive reviews. Research was supported in part by National Aeronautics Space Administration (NASA) grant #11-TE11-104 and was carried out in collaboration with the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Any use of trade, firm, or product names is for descriptive purposes only and does not imply endorsement by the U.S. Government NR 60 TC 5 Z9 5 U1 4 U2 23 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD SEP PY 2014 VL 152 BP 364 EP 374 DI 10.1016/j.rse.2014.07.002 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AR2CW UT WOS:000343392200029 ER PT J AU Joiner, J Yoshida, Y Vasilkov, A Schaefer, K Jung, M Guanter, L Zhang, Y Garrity, S Middleton, EM Huemmrich, KF Gu, L Marchesini, LB AF Joiner, J. Yoshida, Y. Vasilkov, Ap. Schaefer, K. Jung, M. Guanter, L. Zhang, Y. Garrity, S. Middleton, E. M. Huemmrich, K. F. Gu, L. Marchesini, L. Belelli TI The seasonal cycle of satellite chlorophyll fluorescence observations and its relationship to vegetation phenology and ecosystem atmosphere carbon exchange SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Fluorescence; Vegetation; Fluorescence; Chlorophyll; GOME-2; Gross primary productivity; Light-use efficiency; Flux tower; Growing season; Carbon uptake period; Phenology ID GROSS PRIMARY PRODUCTION; LIGHT-USE EFFICIENCY; DECIDUOUS BROADLEAF FOREST; EDDY-COVARIANCE; UNITED-STATES; MODIS DATA; PHOTOSYNTHETIC EFFICIENCY; RESPONSE PARAMETERS; TOWER MEASUREMENTS; FLUX MEASUREMENTS AB Mapping of terrestrial chlorophyll fluorescence from space has shown potential for providing global measurements related to gross primary productivity (GPP). In particular, space-based fluorescence may provide information on the length of the carbon uptake period. Here, for the first time we test the ability of satellite fluorescence retrievals to track seasonal cycle of photosynthesis as estimated from a diverse set of tower gas exchange measurements from around the world. The satellite fluorescence retrievals are obtained using new observations near the 740 nm emission feature from the Global Ozone Monitoring Experiment 2 (GOME-2) instrument offering the highest temporal and spatial resolution of available global measurements. Because GOME-2 has a large ground footprint (similar to 40 x 80 km(2)) as compared with that of the flux towers and the GOME-2 data require averaging to reduce random errors, we additionally compare with seasonal cycles of upscaled GPP estimated from a machine learning approach averaged over the same temporal and spatial domain as the satellite data surrounding the tower locations. We also examine the seasonality of absorbed photosynthetically-active radiation (AFAR) estimated from satellite measurements. Finally, to assess whether global vegetation models may benefit from the satellite fluorescence retrievals through validation or additional constraints, we examine seasonal cycles of GPP as produced from an ensemble of vegetation models. Several of the data-driven models rely on satellite reflectance-based vegetation parameters to derive estimates of APAR that are used to compute GPP. For forested (especially deciduous broadleaf and mixed forests) and cropland sites, the GOME-2 fluorescence data track the spring onset and autumn shutoff of photosynthesis as delineated by the upscaled GPP estimates. In contrast the reflectance-based indicators and many of the models, particularly those driven by data, tend to overestimate the length of the photosynthetically-active period for these biomes. Satellite fluorescence measurements therefore show potential for improving the seasonal dependence of photosynthesis simulated by global models at similar spatial scales. (C) 2014 Elsevier Inc All rights reserved. C1 [Joiner, J.; Middleton, E. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yoshida, Y.; Vasilkov, Ap.] Sci Syst & Applicat Inc, Lanham, MD USA. [Schaefer, K.] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA. [Jung, M.] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [Guanter, L.; Zhang, Y.] Free Univ Berlin, Berlin, Germany. [Garrity, S.] Los Alamos Natl Lab, Los Alamos, NM 87544 USA. [Huemmrich, K. F.] Univ Maryland Baltimore Cty, JCET, Baltimore, MD 21228 USA. [Gu, L.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [Marchesini, L. Belelli] Vrije Univ Amsterdam, Amsterdam, Netherlands. RP Garrity, S (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87544 USA. EM Joanna.joiner@nasa.gov RI Guanter, Luis/I-1588-2015; Belelli Marchesini, Luca/M-3554-2014; Gu, Lianhong/H-8241-2014; OI Guanter, Luis/0000-0002-8389-5764; Belelli Marchesini, Luca/0000-0001-8408-4675; Gu, Lianhong/0000-0001-5756-8738; Zhang, Yongguang/0000-0001-8286-300X FU NASA Carbon Cycle Science program [NNH1ODA001N]; U.S. Department of Energy, Biological and Environmental Research, Terrestrial Carbon Program [DEFG0204ER63917, DEFG0204ER63911]; CFCAS; NSERC; BIOCAP; Environment Canada; NRCan; CarboEuropeIP; FAOGTOSTCO; iLEAPS; Max Planck Institute for Biogeochemistry; National Science Foundation; University of Tuscia; Wageningen University CALM Group; Universit Laval; U.S. Department of Energy; National Science Foundation (NSF); U.S. Department of Agriculture (USDA); U.S. Department of Energy (DOE); Biological and Environmental Research Program (BER); U.S. DOE, through the Midwestern Center of the National Institute for Global Environmental Change (NIGEC) [DE-FC03-90ER61010]; BER [DE FG02-03ER63624, DE-FG03-01ER63278]; NOAA [NA09OAR4310063]; NASA [NNX10AR63G, NNX11A008A]; NASA Terrestrial Ecology Program [NNX08AI77G]; NSF Biocomplexity Program [EAR-0120630]; Australian Research Council FT [FT1110602]; [DP130101566] FX Funding for this work was provided in part by the NASA Carbon Cycle Science program (NNH1ODA001N). The authors gratefully acknowledge EUMETSAT and the MODIS data processing team for making available the GOME-2 and MODIS data sets, respectively, used here as well as the algorithm development teams. We also thank James Collatz, Randy Kawa, William Cook, Yen-Ben Cheng, Larry Corp, Petya Campbell, Qingyuan Zhang, and Arlindo da Silva for helpful discussions. We are indebted to Philip Durbin for assistance with the GOME-2 satellite data set. We also thank Joshua Fisher and an anonymous reviewer for helpful comments that helped to improve the paper.; This study uses eddy covariance data acquired by the FLUXNET community and in particular by the following networks: AmeriFlux (U.S. Department of Energy, Biological and Environmental Research, Terrestrial Carbon Program (DEFG0204ER63917 and DEFG0204ER63911)) AfriFlux, CarboAfrica, CarboEuropelP, CarboItaly, CarboMont, FluxnetCanada (supported by the CFCAS, NSERC, BIOCAP, Environment Canada, and NRCan), GreenGrass, KoFlux, LBA, NECC, OzFlux, and USCCC. We acknowledge the financial support to the eddy covariance data harmonization provided by the CarboEuropeIP, FAOGTOSTCO, iLEAPS, Max Planck Institute for Biogeochemistry, National Science Foundation, University of Tuscia, Wageningen University CALM Group (Climate change and Adaptive Land and Water Management), Universit Laval and Environment Canada and U.S. Department of Energy and the database development and technical support from the Berkeley Water Center, Lawrence Berkeley National Laboratory, Microsoft Research eScience, Oak Ridge National Laboratory, University of California Berkeley, University of Virginia, and South Dakota State University. Sites in the U.S. also acknowledge support from the National Science Foundation (NSF), U.S. Department of Agriculture (USDA), and the U.S. Department of Energy (DOE). Funding for this research was also provided by the Biological and Environmental Research Program (BER), U.S. DOE, through the Midwestern Center of the National Institute for Global Environmental Change (NIGEC) under Cooperative Agreements DE-FC03-90ER61010, and from the BER under Cooperative Agreements DE FG02-03ER63624 and DE-FG03-01ER63278, NOAA grant NA09OAR4310063, and NASA grants NNX10AR63G and NNX11A008A. Any opinions, findings, and conclusions or recommendations expressed in this publication are those of the authors and do not necessarily reflect the views of the DOE. Access to the MMSF AmeriFlux site is provided by the Indiana Department of Natural Resources, Division of Forestry. The ZA-Kru site was supported by the NASA Terrestrial Ecology Program (Grant # NNX08AI77G) and NSF Biocomplexity Program (Grant # EAR-0120630) through grants to NPH. The OzFlux sites (AU-Wac, AU-Fog, AI-How) were provided by Jason Beringer who was funded under an Australian Research Council FT (FT1110602) and project support from DP130101566. Support for collection and archiving was provided through the Australia Terrestrial Ecosystem Research Network (TERN) (http://www.tem.org.au). NR 123 TC 38 Z9 38 U1 11 U2 78 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD SEP PY 2014 VL 152 BP 375 EP 391 DI 10.1016/j.rse.2014.06.022 PG 17 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AR2CW UT WOS:000343392200030 ER PT J AU Shuai, YM Masek, JG Gao, F Schaaf, CB He, T AF Shuai, Yanmin Masek, Jeffrey G. Gao, Feng Schaaf, Crystal B. He, Tao TI An approach for the long-term 30-m land surface snow-free albedo retrieval from historic Landsat surface reflectance and MODIS-based a priori anisotropy knowledge SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Albedo algorithm; Landsat; MODIS BRDF; Forest disturbance ID BIDIRECTIONAL REFLECTANCE; HEMISPHERICAL REFLECTANCE; DIRECTIONAL REFLECTANCE; ATMOSPHERIC CORRECTION; PARAMETERIZATION SIB2; VEGETATION CANOPIES; FOREST DISTURBANCE; NADIR REFLECTANCE; USE EFFICIENCY; BOREAL FOREST AB Land surface albedo has been recognized by the Global Terrestrial Observing System (GTOS) as an essential climate variable crucial for accurate modeling and monitoring of the Earth's radiative budget. While global climate studies can leverage albedo datasets from MODIS, VIIRS, and other coarse-resolution sensors, many applications in heterogeneous environments can benefit from higher-resolution albedo products derived from Landsat We previously developed a "MODIS-concurrent" approach for the 30-meter albedo estimation which relied on combining post-2000 Landsat data with MODIS Bidirectional Reflectance Distribution Function (BRDF) information. Here we present a "pre-MODIS era" approach to extend 30-m surface albedo generation in time back to the 1980s, through an a priori anisotropy Look-Up Table (LUT) built up from the high quality MCD43A BRDF estimates over representative homogenous regions. Each entry in the LUT reflects a unique combination of land cover, seasonality, terrain information, disturbance age and type, and Landsat optical spectral bands. An initial conceptual WT was created for the Pacific Northwest (PNW) of the United-States and provides BRDF shapes estimated from MODIS observations for undisturbed and disturbed surface types (including recovery trajectories of burned areas and non-fire disturbances). By accepting the assumption of a generally invariant BRDF shape for similar land surface structures as a priori information, spectral white-sky and black-sky albedos are derived through albedo-to-nadir reflectance ratios as a bridge between the Landsat and MODIS scale. A further narrow-to-broadband conversion based on radiative transfer simulations is adopted to produce broadband albedos at visible, near infrared, and shortwave regimes. We evaluate the accuracy of resultant Landsat albedo using available field measurements at forested AmeriFlux stations in the PNW region, and examine the consistency of the surface albedo generated by this approach respectively with that from the "concurrent" approach and the coincident MODIS operational surface albedo products. Using the tower measurements as reference, the derived Landsat 30-m snow-free shortwave broadband albedo yields an absolute accuracy of 0.02 with a root mean square error less than 0.016 and a bias of no more than 0.007. A further cross-comparison over individual scenes shows that the retrieved white sky shortwave albedo from the "pre-MODIS era" LUT approach is highly consistent (R-2 = 0.988, the scene-averaged low RMSE = 0.009 and bias = -0.005) with that generated by the earlier "concurrent" approach. The Landsat albedo also exhibits more detailed landscape texture and a wider dynamic range of albedo values than the coincident 500-m MODIS operational products (MCD43A3), especially in the heterogeneous regions. Collectively, the "pre-MODIS" LUT and "concurrent" approaches provide a practical way to retrieve long-term Landsat albedo from the historic Landsat archives as far back as the 19805, as well as the current Landsat-8 mission, and thus support investigations into the evolution of the albedo of terrestrial biomes at fine resolution. (C) 2014 Elsevier Inc. All rights reserved. C1 [Shuai, Yanmin] Earth Resources Technol Inc, NASA, GSFC, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Gao, Feng] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [Schaaf, Crystal B.] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA. [He, Tao] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. RP Shuai, YM (reprint author), Earth Resources Technol Inc, NASA, GSFC, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA. EM shuaiym@gmail.com RI Masek, Jeffrey/D-7673-2012; He, Tao/H-5130-2012 OI He, Tao/0000-0003-2079-7988 FU NASA Terrestrial Ecology Program via a "Science of Terra/Aqua" [NNX11AG53G]; U.S. Geological Survey (USGS) [G12PC00072]; MODIS team under NASA [NNX12AL38G] FX This study was supported by the NASA Terrestrial Ecology Program via a "Science of Terra/Aqua" grant (#NNX11AG53G) and partly by the U.S. Geological Survey (USGS) Landsat science team grant (G12PC00072). The authors would like to thank AmeriFlux network for providing ground data, the extra help on ground details from Drs. Beverly E. Law, Christoph Thomas, William J. Massman, Sean Burns, and Tilden P. Meyers. We thank the LEDAPS project and USGS for providing Landsat surface reflectance, Dr. Zhuosen Wang and the entire MODIS team under NASA grant NNX12AL38G for the generation of operational MCD43A (V005), the Multi-Resolution Land Characteristics (MRLC) consortium to provide NLCD 2006 dataset, the USDA forest service-RSAC and USGS-EROS for the publish of annual MTBS dataset, and Jet Propulsion Laboratory for the open of SRTM data as well University of Maryland for the further process on SRTM and the generation of NAFD data. NR 97 TC 10 Z9 10 U1 3 U2 36 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD SEP PY 2014 VL 152 BP 467 EP 479 DI 10.1016/j.rse.2014.07.009 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AR2CW UT WOS:000343392200035 ER PT J AU Mannino, A Novak, MG Hooker, SB Hyde, K Aurin, D AF Mannino, Antonio Novak, Michael G. Hooker, Stanford B. Hyde, Kimberly Aurin, Dirk TI Algorithm development and validation of CDOM properties for estuarine and continental shelf waters along the northeastern U.S. coast SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE CDOM; MODIS; SeaWiFS; Chesapeake Bay; Ocean; Remote sensing; Ocean color; Continental shelf; Middle Atlantic Bight; Gulf of Maine; Georges Bank ID DISSOLVED ORGANIC-MATTER; INHERENT OPTICAL-PROPERTIES; MIDDLE ATLANTIC BIGHT; ABSORPTION SPECTRAL SLOPES; OCEAN COLOR ALGORITHMS; CANADIAN BEAUFORT SEA; GLOBAL DISTRIBUTION; MISSISSIPPI RIVER; CHESAPEAKE BAY; CHLOROPHYLL-A AB An extensive set of field measurements have been collected throughout the continental margin of the northeastern U.S. from 2004 to 2011 to develop and validate ocean color satellite algorithms for the retrieval of the absorption coefficient of chromophoric dissolved organic matter (a(CDOM)) and CDOM spectral slopes for the 275:295 nm and 300:600 nm spectral range (S-275:295 and S-300:600). Remote sensing reflectance (R-rs) measurements computed from in-water radiometry profiles along with a(CDOM)(lambda) data are applied to develop several types of algorithms for the SeaWiFS and MODIS-Aqua ocean color satellite sensors, which involve least squares linear regression of a(CDOM)(X) with (1)R-rs band ratios, (2) quasi-analytical algorithm-based (QAA-based) products of total absorption coefficients, (3) multiple R-rs bands within a multiple linear regression (MLR) analysis, and (4) diffuse attenuation coefficient (K-d). The relative error (mean absolute percent difference; MAPD) for the MLR retrievals of a(CDOM)(275), a(CDOM)(355), a(CDOM)(380), a(CDOM)(412) and a(CDOM)(443) for our study region range from 20.4 to 23.9% for MODIS-Aqua and 27.3-30% for SeaWiFS. Because of the narrower range of CDOM spectral slope values, the MAPD for the MLR S-275:295 and S-300:600 algorithms are much lower ranging from 9.9% and 9.1% for SeaWiFS, respectively, and 8.7% and 9.7% for MODIS, respectively. Multi-year, seasonal and spatial MODIS-Aqua and SeaWiFS distributions of Claw, S-275:295 and S-300:600 processed with these algorithms are consistent with field measurements and the processes that impact CDOM levels along the continental shelf of the northeastern U.S. Several satellite data processing factors correlate with higher uncertainty in satellite retrievals of a(CDOM), S-275:295 and S-300.600 within the coastal ocean, including solar zenith angle, sensor viewing angle, and atmospheric products applied for atmospheric corrections. Algorithms that include ultraviolet R-rs bands provide a better fit to field measurements than algorithms without the ultraviolet R-rs bands. This suggests that satellite sensors with ultraviolet capability could provide better retrievals of CDOM. Because of the strong correlations between CDOM parameters and DOM constituents in the coastal ocean, satellite observations of CDOM parameters can be applied to study the distributions, sources and sinks of DOM, which are relevant for understanding the carbon cycle, modeling the Earth system, and to discern how the Earth is changing. Published by Elsevier Inc. C1 [Mannino, Antonio; Hooker, Stanford B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Novak, Michael G.; Aurin, Dirk] NASA, Goddard Space Flight Ctr, SSAI Inc, Greenbelt, MD 20771 USA. [Hyde, Kimberly] NOAA, Northeast Fisheries Serv Ctr, Narragansett, RI 02882 USA. RP Mannino, A (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 616-1, Greenbelt, MD 20771 USA. EM antonio.mannino@nasa.gov RI Hooker, Stanford/E-2162-2012; Mannino, Antonio/I-3633-2014 FU NASA programs; Ocean Biology and Biogeochemistry Program (Climate Variability of the East Coast [CliVEC] project and calibration/validation project); Biodiversity Program; New Investigator Program and Interdisciplinary Science FX Various NASA programs supported the work described in this publication including the Ocean Biology and Biogeochemistry Program (Climate Variability of the East Coast [CliVEC] project and calibration/validation project), Biodiversity Program, New Investigator Program and Interdisciplinary Science. We thank the captains and crews of the RN Delaware II, RN Sharp, RN Gulf Challenger, RN Connecticut, and RN Fay Slover. Our profound gratitude to Jerry Prezioso, Jon Hare, and Harvey Walsh for accommodating our CliVEC project research on NOAA's Northeast Marine Fisheries Service Ecosystem Monitoring (ECO-Mon) cruises. Many thanks to Veronica Lance, Xiaoju Pan, Davide D'Alimonte, Mary Russ, Katherine Filippino, Peter Bernhardt, Jean-Noel Druon, and John Morrow for their assistance on the various research cruises that contributed to this work. We thank Mike Twardowski for organizing and leading the OBB-supported calibration/validation project and cruises in the Hudson River-Estuary and New York Bight region. Ru Morrison kindly invited our group to participate on cruises in the Gulf of Maine and waters surrounding the Martha's Vineyard Coastal Observatory. Thanks to Jay Austin, Eileen Hofmann and John Klinck for planning and/or assistance with the Old Dominion University Chesapeake Bay mouth hydrography transects and data access. We express our sincere gratitude to Chuck McClain and three anonymous reviewers for providing insightful comments on a prior draft of this manuscript that improved the final version of this manuscript. Many thanks to the NASA Goddard Space Flight Center Ocean Biology Processing Group for their efforts in providing high quality MODIS and SeaWiFS satellite data products. NR 98 TC 10 Z9 11 U1 1 U2 29 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD SEP PY 2014 VL 152 BP 576 EP 602 DI 10.1016/j.rse.2014.06.027 PG 27 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AR2CW UT WOS:000343392200043 ER PT J AU Al-Yaari, A Wigneron, JP Ducharne, A Kerr, YH Wagner, W De Lannoy, G Reichle, R Al Bitar, A Dorigo, W Richaume, P Mialon, A AF Al-Yaari, A. Wigneron, J. -P. Ducharne, A. Kerr, Y. H. Wagner, W. De lannoy, G. Reichle, R. Al Bitar, A. Dorigo, W. Richaume, P. Mialon, A. TI Global-scale comparison of passive (SMOS) and active (ASCAT) satellite based microwave soil moisture retrievals with soil moisture simulations (MERRA-Land) SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE SMOS; ASCAT; MERRA-Land; Soil; Moisture; Global; Vegetation; LAI ID AMSR-E; TRIPLE COLLOCATION; ERS SCATTEROMETER; IN-SITU; MODEL; VALIDATION; PRODUCTS; ASSIMILATION; MISSION; CALIBRATION AB Global surface soil moisture (SSM) datasets are being produced based on active and passive microwave satellite observations and simulations from land surface models (LSM). This study investigates the consistency of two global satellite-based SSM datasets based on microwave remote sensing observations from the passive Soil Moisture and Ocean Salinity (SMOS; SMOSL3 version 2.5) and the active Advanced Scatterometer (ASCAT; version TU-Wien-WARP 5.5) with respect to LSM SSM from the MERRA-Land data product. The relationship between the global-scale SSM products was studied during the 2010-2012 period using (1) a time series statistics (considering both original SSM data and anomalies), (2) a space time analysis using Hovmoller diagrams, and (3) a triple collocation error model. The SMOSL3 and ASCAT retrievals are consistent with the temporal dynamics of modeled SSM (correlation R > 0.70 for original SSM) in the transition zones between wet and dry climates, including the Sahel, the Indian subcontinent, the Great Plains of North America, eastern Australia, and southeastern Brazil. Over relatively dense vegetation covers, a better consistency with MERRA-Land was obtained with ASCAT than with SMOSL3. However, it was found that ASCAT retrievals exhibit negative correlation versus MERRA-Land in some arid regions (e.g., the Sahara and the Arabian Peninsula). In terms of anomalies, SMOSL3 better captures the short term SSM variability of the reference dataset (MERRA-Land) than ASCAT over regions with limited radio frequency interference (RFI) effects (e.g., North America, South America, and Australia). The seasonal and latitudinal variations of SSM are relatively similar for the three products, although the MERRA-Land SSM values are generally higher and their seasonal amplitude is much lower than for SMOSL3 and ASCAT. Both SMOSL3 and ASCAT have relatively comparable triple collocation errors with similar spatial error patterns: (i) lowest errors in arid regions (e.g., Sahara and Arabian Peninsula), due to the very low natural variability of soil moisture in these areas, and Central America, and (ii) highest errors over most of the vegetated regions (e.g., northern Australia, India, central Asia, and South America). However, the ASCAT SSM product is prone to larger random errors in some regions (e.g., north-western Africa, Iran, and southern South Africa). Vegetation density was found to be a key factor to interpret the consistency with MERRA-Land between the two remotely sensed products (SMOSL3 and ASCAT) which provides complementary information on SSM. This study shows that both SMOS and ASCAT have thus a potential for data fusion into long-term data records. (C) 2014 British Geological Survey (c) NERC. Published by Elsevier Inc. C1 [Al-Yaari, A.; Wigneron, J. -P.] INRA, UMR ISPA 1391, F-33140 Villenave Dornon, France. [Al-Yaari, A.; Ducharne, A.] Univ Paris 06, CNRS, UMR METIS 7619, Paris, France. [Al-Yaari, A.] Thamar Univ, Fac Sci Appl, Dept Geol, Thamar, Yemen. [Kerr, Y. H.; Al Bitar, A.; Richaume, P.; Mialon, A.] Univ Toulouse 3, CNRS, CNES, IRD,UMR Ctr Etudes Spatiales BIOsphere CESBIO 51, F-31062 Toulouse, France. [Wagner, W.; Dorigo, W.] Vienna Univ Technol, Dept Geodesy & Geoinformat, A-1040 Vienna, Austria. [De lannoy, G.; Reichle, R.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off Code 610 1, Greenbelt, MD 20771 USA. RP Wigneron, JP (reprint author), INRA, UMR ISPA 1391, F-33140 Villenave Dornon, France. EM wigneron@bordeaux.inra.fr RI Reichle, Rolf/E-1419-2012; Al-Yaari, Amen/B-1444-2016; OI Al-Yaari, Amen/0000-0001-7530-6088; Wagner, Wolfgang/0000-0001-7704-6857; Al Bitar, Ahmad/0000-0002-1756-1096 FU TOSCA (Terre Ocean Surfaces Continentales et Atmosphere) CNES program; Islamic Development Bank (IDB); NASA Soil Moisture Active Passive mission FX This research work was funded by the TOSCA (Terre Ocean Surfaces Continentales et Atmosphere) CNES program and the Islamic Development Bank (IDB). Gabrielle De Lannoy and Rolf Reichle were supported by the NASA Soil Moisture Active Passive mission. The authors acknowledge CATDS for the SMOSL3 dataset (http://catds.ifremer.fr) and the Vienna University of Technology (TU-WIEN) for the ASCAT product. SMOS team at CESBIO is thanked for fruitful discussions. Mr Christophe Moisy provided valuable technical assistance. NR 80 TC 38 Z9 39 U1 5 U2 53 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD SEP PY 2014 VL 152 BP 614 EP 626 DI 10.1016/j.rse.2014.07.013 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AR2CW UT WOS:000343392200045 ER PT J AU Franch, B Vermote, EF Claverie, M AF Franch, B. Vermote, E. F. Claverie, M. TI Intercomparison of Landsat albedo retrieval techniques and evaluation against in situ measurements across the US SURFRAD network SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Surface albedo; BRDF; Landsat; MODIS ID BROAD-BAND ALBEDO; BIDIRECTIONAL REFLECTANCE; SURFACE ALBEDO; CLIMATE-CHANGE; MODIS DATA; FEEDBACKS; VARIABILITY; VALIDATION; IMPACTS; FORESTS AB Surface albedo is an essential parameter not only for developing climate models, but also for most energy balance studies. While climate models are usually applied at coarse resolution, the energy balance studies, which are mainly focused on agricultural applications, require a high spatial resolution. In this context Landsat is one of the most used remote sensing sensors. The albedo, estimated through the angular integration of the Bidirectional Reflectance Distribution Function (BRDF), requires an appropriate angular sampling of the surface. However, Landsat sampling characteristics, with nearly constant observation geometry and low illumination variation, prevent from deriving a surface albedo product. In this paper we present an algorithm to derive a Landsat surface albedo based on the BRDF parameters estimated from the MODerate Resolution Imaging Spectroradiometer (MODIS) Climate Modeling Grid (CMG) surface reflectance product (M{O,Y}D09) using the VJB method (Vermote, Justice, & Breon, 2009). We base our method on Landsat unsupervised classification to disaggregate the BRDF parameters to the Landsat spatial resolution. We tested the proposed algorithm over five different sites of the US Surface Radiation (SURFRAD) network and inter-compare our results with Shuai, Masek, Gao, and Schaaf (2011) method, which also provides Landsat albedo. The results show that with the proposed method we can derive the surface albedo with a Root Mean Square Error (RMSE) of 0.015 (7%). This result supposes an improvement of 5% in the RMSE compared to Shuai et al.'s (2011) method (with a RMSE of 0.024, 12%) that is mainly determined by the correction of the negative bias (lower retrieved albedo than in situ data). (C) 2014 Elsevier Inc. All rights reserved. C1 [Franch, B.; Claverie, M.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Franch, B.; Vermote, E. F.; Claverie, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Franch, B (reprint author), NASA, Goddard Space Flight Ctr, Dept Geog Sci, Terr Informat Syst Lab, Mail Code 619,Bldg 32,Room N148A, Greenbelt, MD 20771 USA. EM belen.franchgras@nasa.gov NR 40 TC 11 Z9 11 U1 3 U2 24 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD SEP PY 2014 VL 152 BP 627 EP 637 DI 10.1016/j.rse.2014.07.019 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AR2CW UT WOS:000343392200046 ER PT J AU Free, J AF Free, James TI Conversation with Optimist-in-chief SO AEROSPACE AMERICA LA English DT Editorial Material C1 NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Free, J (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0740-722X J9 AEROSPACE AM JI Aerosp. Am. PD SEP PY 2014 VL 52 IS 8 BP 18 EP 20 PG 3 WC Engineering, Aerospace SC Engineering GA AR0TC UT WOS:000343283200012 ER PT J AU Roland, A AF Roland, Alex TI Arguments That Count: Physics, Computing, and Missile Defense, 1949-2012 SO ISIS LA English DT Book Review C1 [Roland, Alex] Duke Univ, Durham, NC 27706 USA. [Roland, Alex] Natl Aeronaut & Space Adm, Washington, DC USA. RP Roland, A (reprint author), Duke Univ, Durham, NC 27706 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 EI 1545-6994 J9 ISIS JI Isis PD SEP PY 2014 VL 105 IS 3 BP 671 EP 672 PG 4 WC History & Philosophy Of Science SC History & Philosophy of Science GA AQ7PQ UT WOS:000343011900063 ER PT J AU Ning, SA Kroo, I Aftosmis, MJ Nemec, M Kless, JE AF Ning, S. Andrew Kroo, Ilan Aftosmis, Michael J. Nemec, Marian Kless, James E. TI Extended Formation Flight at Transonic Speeds SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT 29th AIAA Applied Aerodynamics Conference CY JUN 27-30, 2011 CL Honolulu, HI SP AIAA ID BIRDS AB Aircraft flown in formation can realize significant reductions in drag by flying in regions of wake upwash. However, most transports fly at transonic speeds where the impact of compressibility on formation flight is not well understood. This study uses an Euler solver to analyze the inviscid aerodynamic forces and moments of transonic wing/body configurations flying in a two-aircraft formation. Formations with large streamwise separation distances (10-50 wingspans) are considered. This work indicates that compressibility-related drag penalties in formation flight may be eliminated by slowing 2-3% below the nominal out-of-formation cruise Mach number, either at fixed lift coefficient or fixed altitude. The latter option has the additional benefit that the aerodynamic performance of the formation improves slightly at higher lift coefficients. Although optimal in-formation lift coefficients are not as high as those estimated by incompressible analyses, modest increases in altitude can yield further improvements in aerodynamic efficiency. Increasing the lateral separation of the aircraft allows for slightly higher cruise speeds in exchange for higher induced drag. For the configurations examined here, a 1-2% reduction in Mach number combined with a lateral spacing increase of 5% span (vertical spacing aligned with the vortex) achieves a total formation drag savings of about 10%. C1 [Ning, S. Andrew; Kroo, Ilan] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA. [Aftosmis, Michael J.] NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA. [Nemec, Marian; Kless, James E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ning, SA (reprint author), Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA. EM andrewning@alumni.stanford.edu OI Ning, Andrew/0000-0003-2190-823X NR 25 TC 1 Z9 1 U1 0 U2 7 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD SEP-OCT PY 2014 VL 51 IS 5 BP 1501 EP 1510 DI 10.2514/1.C032385 PG 10 WC Engineering, Aerospace SC Engineering GA AQ8MS UT WOS:000343080200016 ER PT J AU Guruswamy, GP AF Guruswamy, Guru P. TI Frequency Domain Flutter Boundary Computations Using Navier-Stokes Equations on Superclusters SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT 12th AIAA Aviation Technology, Integration, and Operations (ATIO) Conference / 14th AIAA/ISSMO Multidisciplinary Analysis and Optimization Conference CY SEP 17-19, 2012 CL Indianapolis, IN SP AIAA, ISSMO C1 NASA, Ames Res Ctr, Fundamental Modeling & Simulat Branch, Adv Supercomp Div, Moffett Field, CA 94035 USA. RP Guruswamy, GP (reprint author), NASA, Ames Res Ctr, Fundamental Modeling & Simulat Branch, Adv Supercomp Div, Moffett Field, CA 94035 USA. NR 12 TC 2 Z9 2 U1 0 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD SEP-OCT PY 2014 VL 51 IS 5 BP 1640 EP 1642 DI 10.2514/1.C032126 PG 3 WC Engineering, Aerospace SC Engineering GA AQ8MS UT WOS:000343080200028 ER PT J AU DeHaven, S Wincheski, R Albin, S AF DeHaven, Stanton Wincheski, Russell Albin, Sacharia TI Anthracene Fibers Grown in a Microstructured Optical Fiber for X-ray Detection SO MATERIALS LA English DT Article DE growth from melt; organic compounds; scintillating materials; optical fiber devices ID SINGLE-CRYSTALS; ORGANIC CRYSTALS; ELECTROLUMINESCENCE; PRESSURE; SPECTRA AB Anthracene fibers are grown inside a microstructured quartz matrix to form a multicore optical fiber for X-ray detection. A modified fiber growth method for single crystal anthracene from the melt via the Bridgman-Stockbarger technique is presented. The anthracene fiber is characterized by using spectrophotometry, Raman spectroscopy, and X-ray diffraction. These results show the anthracene grown in fiber has high purity and a crystal structure similar to anthracene grown from liquid, vapor, and melt techniques. As an X-ray detector, the output is 12%-16% efficient between the energy ranges of 40 and 10 keV. The effect of materials and fiber processing are discussed. C1 [DeHaven, Stanton; Wincheski, Russell] NASA Langley Res Ctr, Hampton, VA 23681 USA. [Albin, Sacharia] Norfolk State Univ, Dept Engn, Norfolk, VA 23504 USA. [Albin, Sacharia] Norfolk State Univ, Ctr Biotechnol & Biomed Sci, Norfolk, VA 23504 USA. RP DeHaven, S (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA. EM stanton.l.dehaven@nasa.gov; russell.a.wincheski@nasa.gov; salbin@nsu.edu NR 38 TC 2 Z9 2 U1 2 U2 9 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 1996-1944 J9 MATERIALS JI Materials PD SEP PY 2014 VL 7 IS 9 BP 6291 EP 6303 DI 10.3390/ma7096291 PG 13 WC Materials Science, Multidisciplinary SC Materials Science GA AQ8QS UT WOS:000343095300014 ER PT J AU Westgate, JA Pearce, NJG Gatti, E Achyuthan, H AF Westgate, John A. Pearce, Nicholas J. G. Gatti, Emma Achyuthan, Hema TI Distinction between the Youngest Toba Tuff and Oldest Toba Tuff from northern Sumatra based on the area density of spontaneous fission tracks in their glass shards SO QUATERNARY RESEARCH LA English DT Article DE Volcanic glass shards; Spontaneous fission tracks; Partial track fading; Toba tuffs; Acheulean artifacts; Sumatra; India ID INDIAN SUBCONTINENT; PENINSULAR INDIA; TEPHRA BEDS; AGE; INDONESIA; ERUPTION; SUPERERUPTION; SEDIMENTS; ASH AB Determination of the area density of spontaneous fission tracks (rho(s)) in glass shards of Toba tephra is a reliable way to distinguish between the Youngest Toba Tuff (YTT) and the Oldest Toba Tuff (OTT). The rho(s) values for YTT, uncorrected for partial track fading, range from 70 to 181 tracks/cm(2) with a weighted mean of 108 5 tracks/cm(2), based on 15 samples. Corrected rho(s) values for YTT are in the range of 77-140 tracks/cm(2) with a weighted mean of 113 +/- 8 tracks/cm(2), within the range of uncorrected rho(s) values. No significant difference in rho(s) exists between YTT samples collected from marine and continental depositional settings. The uncorrected rho(s) for OTT is 1567 +/- 114 tracks/cm(2) so that confusion with YTT is unlikely. The rho(s) values of the Toba tephra at Bori, Morgaon, and Gandhigram in northwestern India indicate a YTT identity, in agreement with geochemical data on their glass shards, the presence of multiple glass populations, and a glass fission-track age determination. Therefore, the view of others that OTT is present at these sites - and thereby indicates an early Pleistocene age for the associated Acheulean artifacts - is incorrect. (C) 2014 University of Washington. Published by Elsevier Inc All rights reserved. C1 [Westgate, John A.] Univ Toronto, Dept Earth Sci, Toronto, ON M5S 3B1, Canada. [Pearce, Nicholas J. G.] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3DB, Dyfed, Wales. [Gatti, Emma] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91106 USA. [Achyuthan, Hema] Anna Univ, Dept Geol, Chennai 600025, Tamil Nadu, India. RP Westgate, JA (reprint author), Univ Toronto, Dept Earth Sci, Toronto, ON M5S 3B1, Canada. EM westgate@es.utoronto.ca RI Pearce, Nicholas/B-5295-2009; OI Pearce, Nicholas/0000-0003-3157-9564 FU Natural Sciences and Engineering Research Council of Canada FX Funds provided by the Natural Sciences and Engineering Research Council of Canada are gratefully acknowledged. We thank Craig Chesner (Eastern Illinois University, U.S.A.) and Jinnappa Pattan (CSIR, National Institute of Oceanography, Goa, India) for samples. Significant improvements to the manuscript were made following reviews by M. D. Petraglia (University of Oxford), J. Dodson (Associate Editor), and an anonymous reviewer. NR 34 TC 2 Z9 2 U1 11 U2 18 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0033-5894 EI 1096-0287 J9 QUATERNARY RES JI Quat. Res. PD SEP PY 2014 VL 82 IS 2 BP 388 EP 393 DI 10.1016/j.yqres.2014.07.001 PG 6 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA AQ8LJ UT WOS:000343076700009 ER PT J AU Montanaro, M Lunsford, A Tesfaye, Z Wenny, B Reuter, D AF Montanaro, Matthew Lunsford, Allen Tesfaye, Zelalem Wenny, Brian Reuter, Dennis TI Radiometric Calibration Methodology of the Landsat 8 Thermal Infrared Sensor SO REMOTE SENSING LA English DT Article DE Landsat; TIRS; radiometric calibration AB The science-focused mission of the Landsat 8 Thermal Infrared Sensor (TIRS) requires that it have an accurate radiometric calibration. A calibration methodology was developed to convert the raw output from the instrument into an accurate at-aperture radiance. The methodology is based on measurements obtained during component-level and instrument-level characterization testing. The radiometric accuracy from the pre-flight measurements was estimated to be approximately 0.7%. The calibration parameters determined pre-flight were updated during the post-launch checkout period by utilizing the on-board calibration sources and Earth scene data. These relative corrections were made to adjust for differences between the pre-flight and the on-orbit performance of the instrument, thereby correcting large striping artifacts observed in Earth imagery. Despite this calibration correction, banding artifacts (low frequency variation in the across-track direction) have been observed in certain uniform Earth scenes, but not in other uniform scenes. In addition, the absolute calibration performance determined from vicarious measurements have revealed a time-varying error to the absolute radiance reported by TIRS. These issues were determined to not be caused by the calibration process developed for the instrument. Instead, an investigation has revealed that stray light is affecting the recorded signal from the Earth. The varying optical stray light effect is an ongoing subject of evaluation and investigation, and a correction strategy is being devised that will be added to the calibration process. C1 [Montanaro, Matthew; Tesfaye, Zelalem; Wenny, Brian] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA. [Lunsford, Allen] NASA, Goddard Space Flight Ctr, Catholic Univ Amer, Greenbelt, MD 20771 USA. [Reuter, Dennis] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Montanaro, M (reprint author), NASA, Goddard Space Flight Ctr, Sigma Space Corp, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM matthew.montanaro@nasa.gov; allen.w.lunsford@nasa.gov; zelalem.tesfaye-1@nasa.gov; brian.n.wenny@nasa.gov; dennis.c.reuter@nasa.gov FU NASA [NNG09HP18C] FX The work presented here was funded under NASA Contract NNG09HP18C. NR 12 TC 12 Z9 12 U1 2 U2 15 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD SEP PY 2014 VL 6 IS 9 BP 8803 EP 8821 DI 10.3390/rs6098803 PG 19 WC Remote Sensing SC Remote Sensing GA AQ8QI UT WOS:000343093800040 ER PT J AU Traore, AK Ciais, P Vuichard, N MacBean, N Dardel, C Poulter, B Piao, SL Fisher, JB Viovy, N Jung, M Myneni, R AF Traore, Abdoul Khadre Ciais, Philippe Vuichard, Nicolas MacBean, Natasha Dardel, Cecile Poulter, Benjamin Piao, Shilong Fisher, Joshua B. Viovy, Nicolas Jung, Martin Myneni, Ranga TI 1982-2010 Trends of Light Use Efficiency and Inherent Water Use Efficiency in African vegetation: Sensitivity to Climate and Atmospheric CO2 Concentrations SO REMOTE SENSING LA English DT Article DE inherent water use efficiency; light use efficiency; Africa; trend analysis; atmospheric CO2 effect and climate effects on vegetation ID PHOTOSYNTHETICALLY ACTIVE RADIATION; NET ECOSYSTEM EXCHANGE; TREE-RING DELTA-C-13; CARBON-DIOXIDE; DIFFUSE-RADIATION; FAGUS-SYLVATICA; ARID ECOSYSTEMS; SOLAR-RADIATION; PAST CENTURY; RAIN-FOREST AB Light and water use by vegetation at the ecosystem level, are key components for understanding the carbon and water cycles particularly in regions with high climate variability and dry climates such as Africa. The objective of this study is to examine recent trends over the last 30 years in Light Use Efficiency (LUE) and inherent Water Use Efficiency (iWUE*) for the major biomes of Africa, including their sensitivities to climate and CO2. LUE and iWUE* trends are analyzed using a combination of NOAA-AVHRR NDVI3g and fAPAR3g, and a data-driven model of monthly evapotranspiration and Gross Primary Productivity (based on flux tower measurements and remote sensing fAPAR, yet with no flux tower data in Africa) and the ORCHIDEE (ORganizing Carbon and Hydrology In Dynamic EcosystEms) process-based land surface model driven by variable CO2 and two different gridded climate fields. The iWUE* data product increases by 10%-20% per decade during the 1982-2010 period over the northern savannas (due to positive trend of vegetation productivity) and the central African forest (due to positive trend of vapor pressure deficit). In contrast to the iWUE*, the LUE trends are not statistically significant. The process-based model simulations only show a positive linear trend in iWUE* and LUE over the central African forest. Additionally, factorial model simulations were conducted to attribute trends in iWUE and LUE to climate change and rising CO2 concentrations. We found that the increase of atmospheric CO2 by 52.8 ppm during the period of study explains 30%-50% of the increase in iWUE* and > 90% of the LUE trend over the central African forest. The modeled iWUE* trend exhibits a high sensitivity to the climate forcing and environmental conditions, whereas the LUE trend has a smaller sensitivity to the selected climate forcing. C1 [Traore, Abdoul Khadre; Ciais, Philippe; Vuichard, Nicolas; MacBean, Natasha; Viovy, Nicolas] LSCE IPSL CEA CNRS UVQS, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France. [Dardel, Cecile] CNRS UPS IRD CNES, UMR 5563, Observ Midi Pyrenees, GET, F-31400 Toulouse, France. [Poulter, Benjamin] Montana State Univ, Dept Ecol, Bozeman, MT 59717 USA. [Piao, Shilong] Peking Univ, Coll Urban & Environm Sci, Dept Ecol, Beijing 100871, Peoples R China. [Piao, Shilong] Peking Univ, Key Lab Earth Surface Proc, Minist Educ, Beijing 100871, Peoples R China. [Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jung, Martin] Max Planck Inst Biogeochem, D-52425 Jena, Germany. [Myneni, Ranga] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. RP Traore, AK (reprint author), LSCE IPSL CEA CNRS UVQS, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France. EM traore@lsce.ipsl.fr; philippe.ciais@lsce.ipsl.fr; nicolas.vuichard@lsce.ipsl.fr; Natasha.MacBean@lsce.ipsl.fr; cecile.dardel@gmail.com; benjamin.poulter@montana.edu; slpiao@pku.edu.cn; Joshua.B.Fisher@jpl.nasa.gov; nicolas.viovy@lsce.ipsl.fr; mjung@bgc-jena.mpg.de; ranga.myneni@gmail.com RI Myneni, Ranga/F-5129-2012; MacBean, Natasha/L-2190-2015; Vuichard, Nicolas/A-6629-2011; OI MacBean, Natasha/0000-0001-6797-4836; Poulter, Benjamin/0000-0002-9493-8600 FU European Commission under the 7th Framework Programme (FP7) FX This work is supported by the ClimAfrica project funded by the European Commission under the 7th Framework Programme (FP7). We are grateful to the GIMMS group for sharing the NDVI3g data (we thank Zaichun Zhu and Ranga B. Myneni). Through Martin Jung, we are thankful to the Department Biogeochemical Integration at the Max Planck Institute for Biogeochemistry for providing Monthly gross primary productivity and evapotranspiration deduced from FLUXNET data from the "La-Thuile-2007" synthesis effort. NR 82 TC 6 Z9 6 U1 4 U2 50 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD SEP PY 2014 VL 6 IS 9 BP 8923 EP 8944 DI 10.3390/rs6098923 PG 22 WC Remote Sensing SC Remote Sensing GA AQ8QI UT WOS:000343093800045 ER PT J AU Eom, BH Penanen, K Hahn, I AF Eom, Byeong Ho Penanen, Konstantin Hahn, Inseob TI A cryogen-free ultralow-field superconducting quantum interference device magnetic resonance imaging system SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID MICROTESLA MRI; SQUID; MEG AB Magnetic resonance imaging (MRI) at microtesla fields using superconducting quantum interference device (SQUID) detection has previously been demonstrated, and advantages have been noted. Although the ultralow-field SQUID MRI technique would not need the heavy superconducting magnet of conventional MRI systems, liquid helium required to cool the low-temperature detector still places a significant burden on its operation. We have built a prototype cryocooler-based SQUID MRI system that does not require a cryogen. The SQUID detector and the superconducting gradiometer were cooled down to 3.7 K and 4.3 K, respectively. We describe the prototype design, characterization, a phantom image, and areas of further improvements needed to bring the imaging performance to parity with conventional MRI systems. (C) 2014 AIP Publishing LLC. C1 [Eom, Byeong Ho; Penanen, Konstantin; Hahn, Inseob] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hahn, I (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ihahn@caltech.edu FU National Aeronautics and Space Administration (NASA) FX I.H. gives thanks to Professor D. Goodstein for his support at Caltech. The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). NR 19 TC 1 Z9 1 U1 2 U2 8 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 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD SEP PY 2014 VL 85 IS 9 AR 094302 DI 10.1063/1.4895998 PG 9 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA AQ6HE UT WOS:000342910500046 PM 25273745 ER PT J AU Giorgi, AP Rovzar, C Davis, KS Fuller, T Buermann, W Saatchi, S Smith, TB Silveira, LF Gillespie, TW AF Giorgi, Ana Paula Rovzar, Corey Davis, Kelsey S. Fuller, Trevon Buermann, Wolfgang Saatchi, Sassan Smith, Thomas B. Silveira, Luis Fabio Gillespie, Thomas W. TI Spatial conservation planning framework for assessing conservation opportunities in the Atlantic Forest of Brazil SO APPLIED GEOGRAPHY LA English DT Article DE Brazil; Ecological niche models; Endemic birds; Environmental management; Protected areas; Radar ID BIODIVERSITY CONSERVATION; SPECIES DISTRIBUTIONS; PASSERINE BIRDS; LANDSCAPE; AREAS; PRIORITIZATION; BIOGEOGRAPHY; CHALLENGES; CORRIDORS; DIVERSITY AB Historic rates of habitat change and growing exploitation of natural resources threaten avian biodiversity in the Brazilian Atlantic Forest, a global biodiversity hotspot. We implemented a twostage framework for conservation planning in the Atlantic Forest. First, we used ecological niche modeling to predict the distributions of 23 endemic bird species using 19 climatic metrics and 12 spectral and radar remote sensing metrics. Second, we utilized the principle of complementarity to prioritize new sites to augment the Atlantic Forest's existing reserves. The best predictors of bird distributions were precipitation metrics (the seasonality of rainfall) and radar remote sensing metrics (QSCAT). The existing protected areas do not include 10% of the habitat of each of the 23 endemic species. We propose a more economical set of protected areas by reducing the extent to which new sites duplicate the biodiversity content of existing protected areas. There is a high concordance between the proposed conservation areas that we designed using computerized algorithms and Important Bird Areas prioritized by BirdLife International. Insofar as deforestation in the Atlantic Forest is similar to land conversion in other biodiversity hotspots, our methodology is applicable to conservation efforts elsewhere in the world. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Giorgi, Ana Paula; Rovzar, Corey; Davis, Kelsey S.; Gillespie, Thomas W.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA. [Giorgi, Ana Paula; Fuller, Trevon; Smith, Thomas B.] Univ Calif Los Angeles, Ctr Trop Res, Los Angeles, CA 90095 USA. [Buermann, Wolfgang] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. [Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Silveira, Luis Fabio] Univ Sao Paulo, BR-13418900 Piracicaba, SP, Brazil. RP Gillespie, TW (reprint author), Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA. EM TG@GEOG.UCLA.EDU RI Silveira, Luis/F-8337-2012 OI Silveira, Luis/0000-0003-2576-7657 NR 47 TC 0 Z9 0 U1 2 U2 26 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0143-6228 EI 1873-7730 J9 APPL GEOGR JI Appl. Geogr. PD SEP PY 2014 VL 53 BP 369 EP 376 DI 10.1016/j.apgeog.2014.06.013 PG 8 WC Geography SC Geography GA AQ1GK UT WOS:000342529700032 PM 28210009 ER PT J AU Dutta, P Rathi, M Zheng, N Gao, Y Yao, Y Martinez, J Ahrenkiel, P Selvamanickam, V AF Dutta, P. Rathi, M. Zheng, N. Gao, Y. Yao, Y. Martinez, J. Ahrenkiel, P. Selvamanickam, V. TI High mobility single-crystalline-like GaAs thin films on inexpensive flexible metal substrates by metal-organic chemical vapor deposition SO APPLIED PHYSICS LETTERS LA English DT Article ID COATED CONDUCTORS; CELLS AB We demonstrate heteroepitaxial growth of single-crystalline-like n and p-type doped GaAs thin films on inexpensive, flexible, and light-weight metal foils by metal-organic chemical vapor deposition. Single-crystalline-like Ge thin film on biaxially textured templates made by ion beam assisted deposition on metal foil served as the epitaxy enabling substrate for GaAs growth. The GaAs films exhibited strong (004) preferred orientation, sharp in-plane texture, low grain misorientation, strong photoluminescence, and a defect density of similar to 10(7) cm(-2). Furthermore, the GaAs films exhibited hole and electron mobilities as high as 66 and 300 cm(2)/V-s, respectively. High mobility single-crystalline-like GaAs thin films on inexpensive metal substrates can pave the path for roll-to-roll manufacturing of flexible III-V solar cells for the mainstream photovoltaics market. (C) 2014 AIP Publishing LLC. C1 [Dutta, P.; Rathi, M.; Gao, Y.; Yao, Y.; Selvamanickam, V.] Univ Houston, Dept Mech Engn, Houston, TX 77204 USA. [Zheng, N.; Ahrenkiel, P.] South Dakota Sch Mines & Technol, Dept Nanosci & Nanoengn, Rapid City, SD 57701 USA. [Martinez, J.] NASA, Lyndon B Johnson Space Ctr, Mat Evaluat Lab, Houston, TX 77085 USA. RP Dutta, P (reprint author), Univ Houston, Dept Mech Engn, Houston, TX 77204 USA. EM pdutta2@central.uh.edu NR 25 TC 10 Z9 10 U1 2 U2 30 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD SEP 1 PY 2014 VL 105 IS 9 AR 092104 DI 10.1063/1.4895388 PG 5 WC Physics, Applied SC Physics GA AQ4FX UT WOS:000342749800022 ER PT J AU d'Abzac, FX Czaja, AD Beard, BL Schauer, JJ Johnson, CM AF d'Abzac, Francois-Xavier Czaja, Andrew D. Beard, Brian L. Schauer, James J. Johnson, Clark M. TI Iron Distribution in Size-Resolved Aerosols Generated by UV-Femtosecond Laser Ablation: Influence of Cell Geometry and Implications for In Situ Isotopic Determination by LA-MC-ICP-MS SO GEOSTANDARDS AND GEOANALYTICAL RESEARCH LA English DT Article DE femtosecond laser ablation; aerosols; isotopes; agglomeration; residence time ID PLASMA-MASS-SPECTROMETRY; FE ISOTOPES; ELEMENTAL FRACTIONATION; RATIO DETERMINATION; 266 NM; PARTICLES; SULFIDES; GLASS; NANOSECOND; METEORITES AB The influence of ablation cell geometry (Frames single- and HelEx two-volume cells) and laser wavelength (198 and 266nm) on aerosols produced by femtosecond laser ablation (fs-LA) were evaluated. Morphologies, iron mass distribution (IMD) and Fe-56/Fe-54 ratios of particles generated from magnetite, pyrite, haematite and siderite were studied. The following two morphologies were identified: spherules (10-200nm) and agglomerates (5-10nm). Similarity in IMD and ablation rate at 198 and 266nm indicates similar ablation mechanisms. Fe-56/Fe-54 ratios increased with aerodynamic particle size as a result of kinetic fractionation during laser plasma plume expansion, cooling and aerosol condensation. The HelEx cell produces smaller particles with a larger range of Fe-56/Fe-54 ratios (1.85) than particles from the Frames cell (1.16 parts per thousand), but the bulk aerosol matches the bulk substrate for both cells, demonstrating stoichiometric fs-LA sampling. IMD differences are the result of faster wash out of the HelEx cell allowing less time for agglomeration of small, low- Fe-56 particles with larger, high- Fe-56 particles in the cell. Even with a shorter ablation time, half the total Fe ion intensity, and half the ablation volume, the HelEx cell produced Fe isotope determinations for magnetite that were as precise as the Frames cell, even when the latter included an aerosol-homogenising mixing chamber. The HelEx cell delivered a more constant stream of small particles to the ICP, producing a more stable Fe ion signal (0.7% vs. 1.5% RSE for Fe-56 in a forty-cycle single analysis), constant instrumental mass bias and thus a more precise measurement. C1 [d'Abzac, Francois-Xavier; Czaja, Andrew D.; Beard, Brian L.; Johnson, Clark M.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [d'Abzac, Francois-Xavier; Czaja, Andrew D.; Beard, Brian L.; Johnson, Clark M.] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA. [Czaja, Andrew D.] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA. [Czaja, Andrew D.] Univ Cincinnati, Dept Chem, Cincinnati, OH 45221 USA. [Schauer, James J.] Univ Wisconsin, Environm Chem & Technol Program, Madison, WI 53706 USA. RP d'Abzac, FX (reprint author), Univ Wisconsin, Dept Geosci, 1215W Dayton St, Madison, WI 53706 USA. EM fxdabzac@gmail.com FU NSF [DMR-1121288]; NASA; NASA Astrobiology Institute FX The authors gratefully acknowledge use of facilities and instrumentation supported by the NSF-funded University of Wisconsin Materials Research Science and Engineering Center (DMR-1121288). This study was funded by NSF and NASA grants to C.M.J. and B. L. B., including funding from the NASA Astrobiology Institute. The anonymous reviewers are thanked for their constructive comments. NR 70 TC 7 Z9 7 U1 2 U2 33 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1639-4488 EI 1751-908X J9 GEOSTAND GEOANAL RES JI Geostand. Geoanal. Res. PD SEP PY 2014 VL 38 IS 3 BP 293 EP 309 DI 10.1111/j.1751-908X.2014.00281.x PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ4HQ UT WOS:000342754900005 ER PT J AU Westphal, AJ Anderson, D Butterworth, AL Frank, DR Lettieri, R Marchant, W Von Korff, J Zevin, D Ardizzone, A Campanile, A Capraro, M Courtney, K Criswell, MN Crumpler, D Cwik, R Gray, FJ Hudson, B Imada, G Karr, J Wah, LLW Mazzucato, M Motta, PG Rigamonti, C Spencer, RC Woodrough, SB Santoni, IC Sperry, G Terry, JN Wordsworth, N Yahnke, T Allen, C Ansari, A Bajt, S Bastien, RK Bassim, N Bechtel, HA Borg, J Brenker, FE Bridges, J Brownlee, DE Burchell, M Burghammer, M Changela, H Cloetens, P Davis, AM Doll, R Floss, C Flynn, G Gainsforth, Z Grun, E Heck, PR Hillier, JK Hoppe, P Huth, J Hvide, B Kearsley, A King, AJ Lai, B Leitner, J Lemelle, L Leroux, H Leonard, A Nittler, LR Ogliore, R Ong, WJ Postberg, F Price, MC Sandford, SA Tresseras, JAS Schmitz, S Schoonjans, T Silversmit, G Simionovici, AS Sole, VA Srama, R Stephan, T Sterken, VJ Stodolna, J Stroud, RM Sutton, S Trieloff, M Tsou, P Tsuchiyama, A Tyliszczak, T Vekemans, B Vincze, L Zolensky, ME AF Westphal, Andrew J. Anderson, David Butterworth, Anna L. Frank, David R. Lettieri, Robert Marchant, William Von Korff, Joshua Zevin, Daniel Ardizzone, Augusto Campanile, Antonella Capraro, Michael Courtney, Kevin Criswell, Mitchell N., III Crumpler, Dixon Cwik, Robert Gray, Fred Jacob Hudson, Bruce Imada, Guy Karr, Joel Wah, Lily Lau Wan Mazzucato, Michele Motta, Pier Giorgio Rigamonti, Carlo Spencer, Ronald C. Woodrough, Stephens B. Santoni, Irene Cimmino Sperry, Gerry Terry, Jean-Noel Wordsworth, Naomi Yahnke, Tom, Sr. Allen, Carlton Ansari, Asna Bajt, Sasa Bastien, Ron K. Bassim, Nabil Bechtel, Hans A. Borg, Janet Brenker, Frank E. Bridges, John Brownlee, Donald E. Burchell, Mark Burghammer, Manfred Changela, Hitesh Cloetens, Peter Davis, Andrew M. Doll, Ryan Floss, Christine Flynn, George Gainsforth, Zack Gruen, Eberhard Heck, Philipp R. Hillier, Jon K. Hoppe, Peter Huth, Joachim Hvide, Brit Kearsley, Anton King, Ashley J. Lai, Barry Leitner, Jan Lemelle, Laurence Leroux, Hugues Leonard, Ariel Nittler, Larry R. Ogliore, Ryan Ong, Wei Ja Postberg, Frank Price, Mark C. Sandford, Scott A. Tresseras, Juan-Angel Sans Schmitz, Sylvia Schoonjans, Tom Silversmit, Geert Simionovici, Alexandre S. Sole, Vicente A. Srama, Ralf Stephan, Thomas Sterken, Veerle J. Stodolna, Julien Stroud, Rhonda M. Sutton, Steven Trieloff, Mario Tsou, Peter Tsuchiyama, Akira Tyliszczak, Tolek Vekemans, Bart Vincze, Laszlo Zolensky, Michael E. TI Stardust Interstellar Preliminary Examination I: Identification of tracks in aerogel SO METEORITICS & PLANETARY SCIENCE LA English DT Article AB Here, we report the identification of 69 tracks in approximately 250 cm(2) of aerogel collectors of the Stardust Interstellar Dust Collector. We identified these tracks through Stardust@home, a distributed internet-based virtual microscope and search engine, in which > 30,000 amateur scientists collectively performed >9 x 10(7) searches on approximately 10(6) fields of view. Using calibration images, we measured individual detection efficiency, and found that the individual detection efficiency for tracks > 2.5 mu m in diameter was >0.6, and was >0.75 for tracks >3 mu m in diameter. Because most fields of view were searched >30 times, these results could be combined to yield a theoretical detection efficiency near unity. The initial expectation was that interstellar dust would be captured at very high speed. The actual tracks discovered in the Stardust collector, however, were due to low-speed impacts, and were morphologically strongly distinct from the calibration images. As a result, the detection efficiency of these tracks was lower than detection efficiency of calibrations presented in training, testing, and ongoing calibration. Nevertheless, as calibration images based on low-speed impacts were added later in the project, detection efficiencies for low-speed tracks rose dramatically. We conclude that a massively distributed, calibrated search, with amateur collaborators, is an effective approach to the challenging problem of identification of tracks of hypervelocity projectiles captured in aerogel. C1 [Westphal, Andrew J.; Anderson, David; Butterworth, Anna L.; Lettieri, Robert; Marchant, William; Von Korff, Joshua; Zevin, Daniel; Gainsforth, Zack; Stodolna, Julien] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Frank, David R.; Bastien, Ron K.] NASA JSC, ESCG, Houston, TX USA. [Ardizzone, Augusto] Red Team, Palermo, Italy. [Campanile, Antonella] Red Team, Reggio Emilia, Italy. [Capraro, Michael] Red Team, Riverview, MI USA. [Courtney, Kevin] Red Team, Ballwin, MO USA. [Criswell, Mitchell N., III] Dog Star Observ, Red Team, Pearce, AZ USA. [Crumpler, Dixon] Red Team, Durham, NC USA. [Cwik, Robert] Red Team, Silver City, NM USA. [Gray, Fred Jacob] Red Team, Hampton, SC USA. [Hudson, Bruce] Red Team, Montreal, PQ, Canada. [Imada, Guy] Red Team, Brookings, OR USA. [Karr, Joel] Red Team, Kansas City, MO USA. [Wah, Lily Lau Wan] Red Team, Singapore, Singapore. [Mazzucato, Michele; Motta, Pier Giorgio] Red Team, Florence, Italy. [Rigamonti, Carlo] Red Team, Moncalieri, Italy. [Spencer, Ronald C.] Red Team, Leominster, MA USA. [Woodrough, Stephens B.] Red Team, St Petersburg, FL USA. [Santoni, Irene Cimmino] Red Team, Upper Saddle River, NJ USA. [Sperry, Gerry] Red Team, Tacoma, WA USA. [Terry, Jean-Noel] Red Team, Tarentaise, France. [Wordsworth, Naomi] Red Team, Wycombe, South Buckingha, England. [Yahnke, Tom, Sr.] Red Team, Louis, MO USA. [Allen, Carlton; Zolensky, Michael E.] NASA JSC, ARES, Houston, TX USA. [Ansari, Asna; Hvide, Brit] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Bajt, Sasa] DESY, Hamburg, Germany. [Bassim, Nabil; Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA. [Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA. [Borg, Janet] IAS Orsay, Orsay, France. [Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ, Geosci Inst, Frankfurt, Germany. [Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England. [Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury, Kent, England. [Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France. [Changela, Hitesh] George Washington Univ, Washington, DC 20052 USA. [Davis, Andrew M.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA. [Doll, Ryan; Leonard, Ariel; Nittler, Larry R.; Ong, Wei Ja] Washington Univ, St Louis, MO USA. [Flynn, George] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA. [Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Heck, Philipp R.] Field Museum Nat Hist, Chicago, IL 60605 USA. [Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany. [Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany. [Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England. [King, Ashley J.] Univ Chicago, Chicago, IL 60637 USA. [King, Ashley J.] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA. [Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France. [Leroux, Hugues] Univ Lyon 1, F-69622 Villeurbanne, France. [Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA. [Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium. [Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France. [Srama, Ralf; Sterken, Veerle J.] Univ Stuttgart, IRS, D-70174 Stuttgart, Germany. [Sterken, Veerle J.] TU Braunschweig, IGEP, Braunschweig, Germany. [Sterken, Veerle J.] MPIK, Heidelberg, Germany. [Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Tsuchiyama, Akira] Osaka Univ, Osaka, Japan. RP Westphal, AJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM westphal@ssl.berkeley.edu RI Sans Tresserras, Juan Angel/J-9362-2014; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015; Bajt, Sasa/G-2228-2010; Stroud, Rhonda/C-5503-2008; OI Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner, Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X; Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943 FU NASA [NNX09AC36G, NNH11AQ61I]; Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231]; U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-98CH10886] FX We thank Sean Brennan and Giles Graham for thoughtful comments, and John Bradley for editorial handling. The ISPE consortium gratefully acknowledges the NASA Discovery Program for Stardust, the fourth NASA Discovery mission. AJW, ALB, ZG, RL, DZ, WM, and JVK were supported by NASA grant NNX09AC36G. We thank Steve Boggs for astrophysical soft X-ray spectra. RMS, HCG, and NDB were supported by NASA grant NNH11AQ61I. The Advanced Light Source is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Use of the National Synchrotron Light Source, Brookhaven National Laboratory, was supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DE-AC02-98CH10886. NR 8 TC 12 Z9 12 U1 3 U2 31 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 IS 9 SI SI BP 1509 EP 1521 DI 10.1111/maps.12168 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ6HT UT WOS:000342912100001 ER PT J AU Frank, DR Westphal, AJ Zolensky, ME Gainsforth, Z Butterworth, AL Bastien, RK Allen, C Anderson, D Ansari, A Bajt, S Bassim, N Bechtel, HA Borg, J Brenker, FE Bridges, J Brownlee, DE Burchell, M Burghammer, M Changela, H Cloetens, P Davis, AM Doll, R Floss, C Flynn, G Grun, E Heck, PR Hillier, JK Hoppe, P Hudson, B Huth, J Hvide, B Kearsley, A King, AJ Lai, B Leitner, J Lemelle, L Leroux, H Leonard, A Lettieri, R Marchant, W Nittler, LR Ogliore, R Ong, WJ Postberg, F Price, MC Sandford, SA Tresseras, JAS Schmitz, S Schoonjans, T Silversmit, G Simionovici, AS Sole, VA Srama, R Stephan, T Sterken, VJ Stodolna, J Stroud, RM Sutton, S Trieloff, M Tsou, P Tsuchiyama, A Tyliszczak, T Vekemans, B Vincze, L Von Korff, J Wordsworth, N Zevin, D AF Frank, David R. Westphal, Andrew J. Zolensky, Michael E. Gainsforth, Zack Butterworth, Anna L. Bastien, Ronald K. Allen, Carlton Anderson, David Ansari, Asna Bajt, Sasa Bassim, Nabil Bechtel, Hans A. Borg, Janet Brenker, Frank E. Bridges, John Brownlee, Donald E. Burchell, Mark Burghammer, Manfred Changela, Hitesh Cloetens, Peter Davis, Andrew M. Doll, Ryan Floss, Christine Flynn, George Gruen, Eberhard Heck, Philipp R. Hillier, Jon K. Hoppe, Peter Hudson, Bruce Huth, Joachim Hvide, Brit Kearsley, Anton King, Ashley J. Lai, Barry Leitner, Jan Lemelle, Laurence Leroux, Hugues Leonard, Ariel Lettieri, Robert Marchant, William Nittler, Larry R. Ogliore, Ryan Ong, Wei Ja Postberg, Frank Price, Mark C. Sandford, Scott A. Tresseras, Juan-Angel Sans Schmitz, Sylvia Schoonjans, Tom Silversmit, Geert Simionovici, Alexandre S. Sole, Vicente A. Srama, Ralf Stephan, Thomas Sterken, Veerle J. Stodolna, Julien Stroud, Rhonda M. Sutton, Steven Trieloff, Mario Tsou, Peter Tsuchiyama, Akira Tyliszczak, Tolek Vekemans, Bart Vincze, Laszlo Von Korff, Joshua Wordsworth, Naomi Zevin, Daniel TI Stardust Interstellar Preliminary Examination II: Curating the interstellar dust collector, picokeystones, and sources of impact tracks SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID IRON-NICKEL SULFIDES; RADIATION PRESSURE; COMETARY DUST; AEROGEL; PARTICLES; MISSION; FEATURES; GRAINS; DISKS; FOIL AB We discuss the inherent difficulties that arise during "ground truth" characterization of the Stardust interstellar dust collector. The challenge of identifying contemporary interstellar dust impact tracks in aerogel is described within the context of background spacecraft secondaries and possible interplanetary dust particles and beta-meteoroids. In addition, the extraction of microscopic dust embedded in aerogel is technically challenging. Specifically, we provide a detailed description of the sample preparation techniques developed to address the unique goals and restrictions of the Interstellar Preliminary Exam. These sample preparation requirements and the scarcity of candidate interstellar impact tracks exacerbate the difficulties. We also illustrate the role of initial optical imaging with critically important examples, and summarize the overall processing of the collection to date. C1 [Frank, David R.; Bastien, Ronald K.] NASA Johnson Space Ctr, ESCG, Houston, TX 77058 USA. [Westphal, Andrew J.; Gainsforth, Zack; Butterworth, Anna L.; Anderson, David; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA. [Zolensky, Michael E.; Allen, Carlton] NASA Johnson Space Ctr, ARES, Houston, TX USA. [Ansari, Asna; Davis, Andrew M.; Heck, Philipp R.; Hvide, Brit] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Bajt, Sasa] DESY, Hamburg, Germany. [Bassim, Nabil; Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA. [Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA. [Borg, Janet] IAS Orsay, Orsay, France. [Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany. [Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England. [Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury CT2 7NZ, Kent, England. [Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France. [Changela, Hitesh] George Washington Univ, Washington, DC USA. [Davis, Andrew M.; King, Ashley J.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA. [Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja] Washington Univ, St Louis, MO USA. [Flynn, George] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA. [Gruen, Eberhard; Sterken, Veerle J.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany. [Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany. [Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England. [Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA. [Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France. [Leroux, Hugues] Univ Lille 1, Lille, France. [Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA. [Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Sandford, Scott A.] NASA Ames Res Ctr, Moffett Field, CA USA. [Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium. [Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France. [Srama, Ralf] Univ Stuttgart, IRS, D-70174 Stuttgart, Germany. [Sterken, Veerle J.] TU Braunschweig, IGEP, Braunschweig, Germany. [Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Tsuchiyama, Akira] Osaka Univ, Osaka, Japan. RP Frank, DR (reprint author), NASA Johnson Space Ctr, ESCG, Houston, TX 77058 USA. EM david.r.frank@nasa.gov RI Stroud, Rhonda/C-5503-2008; Sans Tresserras, Juan Angel/J-9362-2014; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015; Bajt, Sasa/G-2228-2010 OI Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943; Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner, Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X; FU NASA [NNX09AC36G, NNH11AQ61I]; Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231]; U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-98CH10886] FX We thank P. Wozniekiewicz and C. Engrand for their thoughtful reviews that greatly improved this manuscript. We also thank the AE John Bradley for his critical input and time and effort spent reviewing the ISPE manuscripts. The ISPE consortium gratefully acknowledges the NASA Discovery Program for Stardust, the fourth NASA Discovery mission. We are thankful for having the privilege of looking after the collection and are gratefully indebted to the 30,000+ dusters who made this possible. AJW, ALB, ZG, RL, DZ, WM and JVK were supported by NASA grant NNX09AC36G. RMS, HCG and NDB were supported by NASA grant NNH11AQ61I. The Advanced Light Source is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Use of the National Synchrotron Light Source, Brookhaven National Laboratory, was supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DE-AC02-98CH10886. NR 40 TC 13 Z9 13 U1 1 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 IS 9 SI SI BP 1522 EP 1547 DI 10.1111/maps.12147 PG 26 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ6HT UT WOS:000342912100002 ER PT J AU Bechtel, HA Flynn, GJ Allen, C Anderson, D Ansari, A Bajt, S Bastien, RK Bassim, N Borg, J Brenker, FE Bridges, J Brownlee, DE Burchell, M Burghammer, M Butterworth, AL Changela, H Cloetens, P Davis, AM Doll, R Floss, C Frank, DR Gainsforth, Z Grun, E Heck, PR Hillier, JK Hoppe, P Hudson, B Huth, J Hvide, B Kearsley, A King, AJ Lai, B Leitner, J Lemelle, L Leroux, H Leonard, A Lettieri, R Marchant, W Nittler, LR Ogliore, R Ong, WJ Postberg, F Price, MC Sandford, SA Tresseras, JAS Schmitz, S Schoonjans, T Silversmit, G Simionovici, AS Sole, VA Srama, R Stadermann, FJ Stephan, T Sterken, VJ Stodolna, J Stroud, RM Sutton, S Trieloff, M Tsou, P Tsuchiyama, A Tyliszczak, T Vekemans, B Vincze, L Von Korff, J Westphal, AJ Wordsworth, N Zevin, D Zolensky, ME AF Bechtel, Hans A. Flynn, George J. Allen, Carlton Anderson, David Ansari, Asna Bajt, Sasa Bastien, Ron K. Bassim, Nabil Borg, Janet Brenker, Frank E. Bridges, John Brownlee, Donald E. Burchell, Mark Burghammer, Manfred Butterworth, Anna L. Changela, Hitesh Cloetens, Peter Davis, Andrew M. Doll, Ryan Floss, Christine Frank, David R. Gainsforth, Zack Gruen, Eberhard Heck, Philipp R. Hillier, Jon K. Hoppe, Peter Hudson, Bruce Huth, Joachim Hvide, Brit Kearsley, Anton King, Ashley J. Lai, Barry Leitner, Jan Lemelle, Laurence Leroux, Hugues Leonard, Ariel Lettieri, Robert Marchant, William Nittler, Larry R. Ogliore, Ryan Ong, Wei Ja Postberg, Frank Price, Mark C. Sandford, Scott A. Tresseras, Juan-Angel Sans Schmitz, Sylvia Schoonjans, Tom Silversmit, Geert Simionovici, Alexandre S. Sole, Vicente A. Srama, Ralf Stadermann, Frank J. Stephan, Thomas Sterken, Veerle J. Stodolna, Julien Stroud, Rhonda M. Sutton, Steven Trieloff, Mario Tsou, Peter Tsuchiyama, Akira Tyliszczak, Tolek Vekemans, Bart Vincze, Laszlo Von Korff, Joshua Westphal, Andrew J. Wordsworth, Naomi Zevin, Daniel Zolensky, Michael E. TI Stardust Interstellar Preliminary Examination III: Infrared spectroscopic analysis of interstellar dust candidates SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID COMET 81P/WILD 2; CONSTRAINTS; ORGANICS; RETURN; LIGHT AB Under the auspices of the Stardust Interstellar Preliminary Examination, picokeystones extracted from the Stardust Interstellar Dust Collector were examined with synchrotron Fourier transform infrared (FTIR) microscopy to establish whether they contained extraterrestrial organic material. The picokeystones were found to be contaminated with varying concentrations and speciation of organics in the native aerogel, which hindered the search for organics in the interstellar dust candidates. Furthermore, examination of the picokeystones prior to and post X-ray microprobe analyses yielded evidence of beam damage in the form of organic deposition or modification, particularly with hard X-ray synchrotron X-ray fluorescence. From these results, it is clear that considerable care must be taken to interpret any organics that might be in interstellar dust particles. For the interstellar candidates examined thus far, however, there is no clear evidence of extraterrestrial organics associated with the track and/or terminal particles. However, we detected organic matter associated with the terminal particle in Track 37, likely a secondary impact from the Al-deck of the sample return capsule, demonstrating the ability of synchrotron FTIR to detect organic matter in small particles within picokeystones from the Stardust interstellar dust collector. C1 [Bechtel, Hans A.; Tyliszczak, Tolek] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA. [Flynn, George J.] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA. [Allen, Carlton; Zolensky, Michael E.] NASA Johnson Space Ctr, ARES, Houston, TX USA. [Anderson, David; Butterworth, Anna L.; Gainsforth, Zack; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Westphal, Andrew J.; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA. [Ansari, Asna; Heck, Philipp R.; Hvide, Brit; King, Ashley J.] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Bajt, Sasa] DESY, Hamburg, Germany. [Bastien, Ron K.; Frank, David R.] NASA Johnson Space Ctr, ESCG, Houston, TX USA. [Bassim, Nabil; Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA. [Borg, Janet] IAS Orsay, Orsay, France. [Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany. [Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England. [Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury, Kent, England. [Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France. [Changela, Hitesh] George Washington Univ, Washington, DC USA. [Davis, Andrew M.; King, Ashley J.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA. [Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja; Stadermann, Frank J.] Washington Univ, St Louis, MO USA. [Gruen, Eberhard; Sterken, Veerle J.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany. [Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany. [Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England. [Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA. [Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France. [Leroux, Hugues] Univ Lille 1, Lille 1, France. [Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA. [Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Postberg, Frank; Srama, Ralf; Sterken, Veerle J.] Univ Stuttgart, Inst Raumfahrtsyst, Stuttgart, Germany. [Sandford, Scott A.] NASA Ames Res Ctr, Moffett Field, CA USA. [Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium. [Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France. [Sterken, Veerle J.] TU Braunschweig, Inst Geophys & Extraterrestr Phys, Braunschweig, Germany. [Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Tsuchiyama, Akira] Osaka Univ, Osaka, Japan. RP Bechtel, HA (reprint author), Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA. EM habechtel@lbl.gov RI Sans Tresserras, Juan Angel/J-9362-2014; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015; Bajt, Sasa/G-2228-2010; Stroud, Rhonda/C-5503-2008; OI Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner, Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X; Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943 FU NASA Laboratory Analysis of Returned Samples research grant [NNX11AE15G]; NASA [NNX09AC36G, NNH11AQ61I]; Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231]; U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-98CH10886] FX The ISPE consortium gratefully acknowledges the NASA Discovery Program for Stardust, the fourth NASA Discovery mission. GJF was supported by a NASA Laboratory Analysis of Returned Samples research grant NNX11AE15G. AJW, ALB, ZG, RL, DZ, WM, and JVK were supported by NASA grant NNX09AC36G. RMS, HCG, and NDB were supported by NASA grant NNH11AQ61I. The ALS is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Use of the NSLS, BNL, was supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DE-AC02-98CH10886. NR 30 TC 6 Z9 6 U1 2 U2 14 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 IS 9 SI SI BP 1548 EP 1561 DI 10.1111/maps.12125 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ6HT UT WOS:000342912100003 ER PT J AU Butterworth, AL Westphal, AJ Tyliszczak, T Gainsforth, Z Stodolna, J Frank, DR Allen, C Anderson, D Ansari, A Bajt, S Bastien, RK Bassim, N Bechtel, HA Borg, J Brenker, FE Bridges, J Brownlee, DE Burchell, M Burghammer, M Changela, H Cloetens, P Davis, AM Doll, R Floss, C Flynn, G Grun, E Heck, PR Hillier, JK Hoppe, P Hudson, B Huth, J Hvide, B Kearsley, A King, AJ Lai, B Leitner, J Lemelle, L Leroux, H Leonard, A Lettieri, R Marchant, W Nittler, LR Ogliore, R Ong, WJ Postberg, F Price, MC Sandford, SA Tresseras, JAS Schmitz, S Schoonjans, T Silversmit, G Simionovici, AS Sole, VA Srama, R Stadermann, FJ Stephan, T Sterken, VJ Stroud, RM Sutton, S Trieloff, M Tsou, P Tsuchiyama, A Vekemans, B Vincze, L Von Korff, J Wordsworth, N Zevin, D Zolensky, ME AF Butterworth, Anna L. Westphal, Andrew J. Tyliszczak, Tolek Gainsforth, Zack Stodolna, Julien Frank, David R. Allen, Carlton Anderson, David Ansari, Asna Bajt, Sasa Bastien, Ron K. Bassim, Nabil Bechtel, Hans A. Borg, Janet Brenker, Frank E. Bridges, John Brownlee, Donald E. Burchell, Mark Burghammer, Manfred Changela, Hitesh Cloetens, Peter Davis, Andrew M. Doll, Ryan Floss, Christine Flynn, George Gruen, Eberhard Heck, Philipp R. Hillier, Jon K. Hoppe, Peter Hudson, Bruce Huth, Joachim Hvide, Brit Kearsley, Anton King, Ashley J. Lai, Barry Leitner, Jan Lemelle, Laurence Leroux, Hugues Leonard, Ariel Lettieri, Robert Marchant, William Nittler, Larry R. Ogliore, Ryan Ong, Wei Ja Postberg, Frank Price, Mark C. Sandford, Scott A. Tresseras, Juan-Angel Sans Schmitz, Sylvia Schoonjans, Tom Silversmit, Geert Simionovici, Alexandre S. Sole, Vicente A. Srama, Ralf Stadermann, Frank J. Stephan, Thomas Sterken, Veerle J. Stroud, Rhonda M. Sutton, Steven Trieloff, Mario Tsou, Peter Tsuchiyama, Akira Vekemans, Bart Vincze, Laszlo Von Korff, Joshua Wordsworth, Naomi Zevin, Daniel Zolensky, Michael E. TI Stardust Interstellar Preliminary Examination IV: Scanning transmission X-ray microscopy analyses of impact features in the Stardust Interstellar Dust Collector SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID NEAR-EDGE STRUCTURE; K-EDGE; ABSORPTION SPECTROSCOPY; MINERALS; AL; XANES; TEMPERATURE; MAGNESIUM; RANGE; MG AB We report the quantitative characterization by synchrotron soft X-ray spectroscopy of 31 potential impact features in the aerogel capture medium of the Stardust Interstellar Dust Collector. Samples were analyzed in aerogel by acquiring high spatial resolution maps and high energy-resolution spectra of major rock-forming elements Mg, Al, Si, Fe, and others. We developed diagnostic screening tests to reject spacecraft secondary ejecta and terrestrial contaminants from further consideration as interstellar dust candidates. The results support an extraterrestrial origin for three interstellar candidates: I1043,1,30 (Orion) is a 3 pg particle with Mg-spinel, forsterite, and an iron-bearing phase. I1047,1,34 (Hylabrook) is a 4 pg particle comprising an olivine core surrounded by low-density, amorphous Mg-silicate and amorphous Fe, Cr, and Mn phases. I1003,1,40 (Sorok) has the track morphology of a high-speed impact, but contains no detectable residue that is convincingly distinguishable from the background aerogel. Twenty-two samples with an anthropogenic origin were rejected, including four secondary ejecta from impacts on the Stardust spacecraft aft solar panels, nine ejecta from secondary impacts on the Stardust Sample Return Capsule, and nine contaminants lacking evidence of an impact. Other samples in the collection included I1029,1,6, which contained surviving solar system impactor material. Four samples remained ambiguous: I1006,2,18, I1044,2,32, and I1092,2,38 were too dense for analysis, and we did not detect an intact projectile in I1044,3,33. We detected no radiation effects from the synchrotron soft X-ray analyses; however, we recorded the effects of synchrotron hard X-ray radiation on I1043,1,30 and I1047,1,34. C1 [Butterworth, Anna L.; Westphal, Andrew J.; Gainsforth, Zack; Stodolna, Julien; Anderson, David; Lettieri, Robert; Marchant, William; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Tyliszczak, Tolek; Bechtel, Hans A.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA. [Frank, David R.; Bastien, Ron K.] NASA JSC, ESCG, Houston, TX USA. [Allen, Carlton; Zolensky, Michael E.] NASA JSC, ARES, Houston, TX USA. [Ansari, Asna; Heck, Philipp R.; Hvide, Brit] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Bajt, Sasa] DESY, Hamburg, Germany. [Bassim, Nabil; Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA. [Borg, Janet] Inst Astrophys Spatiale, Orsay, France. [Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany. [Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England. [Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury, Kent, England. [Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France. [Changela, Hitesh] George Washington Univ, Washington, DC USA. [Davis, Andrew M.; King, Ashley J.; Stephan, Thomas] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja; Stadermann, Frank J.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Flynn, George] SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA. [Gruen, Eberhard; Sterken, Veerle J.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany. [Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany. [Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England. [Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA. [Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France. [Leroux, Hugues] Univ Lille, Lille, France. [Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA. [Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Sandford, Scott A.] NASA Ames Res Ctr, Moffett Field, CA USA. [Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium. [Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France. [Srama, Ralf; Sterken, Veerle J.] Univ Stuttgart, Inst Raumfahrtsyst, D-70174 Stuttgart, Germany. [Sterken, Veerle J.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterrestr Phys, D-38106 Braunschweig, Germany. [Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Tsuchiyama, Akira] Osaka Univ, Osaka, Japan. RP Butterworth, AL (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM annab@ssl.berkeley.edu RI Bajt, Sasa/G-2228-2010; Stroud, Rhonda/C-5503-2008; Sans Tresserras, Juan Angel/J-9362-2014; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015 OI Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943; Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner, Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X FU NASA [NNX09AC36G, NNH11AQ61I]; Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231]; U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-98CH10886] FX The ISPE consortium gratefully acknowledges the NASA Discovery Program for Stardust, the fourth NASA Discovery mission. AJW, ALB, ZG, RL, DZ, WM, and JVK were supported by NASA grant NNX09AC36G. RMS, HCG, and NDB were supported by NASA grant NNH11AQ61I. The ALS is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy, under Contract No. DE-AC02-05CH11231. Use of the National Synchrotron Light Source, Brookhaven National Laboratory, was supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DE-AC02-98CH10886. We appreciate greatly the thorough reviews by one anonymous reviewer, John Bradley, and associate editor, Christian Koeberl. Their contributions improved the manuscript and helped to clarify key findings. We thank Steve Boggs for helpful discussions regarding X-ray dose estimates in the Interstellar Medium, and for providing diffuse X-ray data. We thank the Natural History Museum, London, for providing most of the standards used for acquiring the XANES spectra library in this work. NR 33 TC 12 Z9 12 U1 0 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 IS 9 SI SI BP 1562 EP 1593 DI 10.1111/maps.12220 PG 32 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ6HT UT WOS:000342912100004 ER PT J AU Brenker, FE Westphal, AJ Vincze, L Burghammer, M Schmitz, S Schoonjans, T Silversmit, G Vekemans, B Allen, C Anderson, D Ansari, A Bajt, S Bastien, RK Bassim, N Bechtel, HA Borg, J Bridges, J Brownlee, DE Burchell, M Butterworth, AL Changela, H Cloetens, P Davis, AM Doll, R Floss, C Flynn, G Fougeray, P Frank, DR Gainsforth, Z Grun, E Heck, PR Hillier, JK Hoppe, P Hudson, B Huth, J Hvide, B Kearsley, A King, AJ Lai, B Leitner, J Lemelle, L Leroux, H Leonard, A Lettieri, R Marchant, W Nittler, LR Ogliore, R Ong, WJ Postberg, F Price, MC Sandford, SA Tresseras, JAS Simionovici, AS Sole, VA Srama, R Stadermann, F Stephan, T Sterken, VJ Stodolna, J Stroud, RM Sutton, S Trieloff, M Tsou, P Tsuchiyama, A Tyliszczak, T Von Korff, J Wordsworth, N Zevin, D Zolensky, ME AF Brenker, Frank E. Westphal, Andrew J. Vincze, Laszlo Burghammer, Manfred Schmitz, Sylvia Schoonjans, Tom Silversmit, Geert Vekemans, Bart Allen, Carlton Anderson, David Ansari, Asna Bajt, Sasa Bastien, Ron K. Bassim, Nabil Bechtel, Hans A. Borg, Janet Bridges, John Brownlee, Donald E. Burchell, Mark Butterworth, Anna L. Changela, Hitesh Cloetens, Peter Davis, Andrew M. Doll, Ryan Floss, Christine Flynn, George Fougeray, Patrick Frank, David R. Gainsforth, Zack Gruen, Eberhard Heck, Philipp R. Hillier, Jon K. Hoppe, Peter Hudson, Bruce Huth, Joachim Hvide, Brit Kearsley, Anton King, Ashley J. Lai, Barry Leitner, Jan Lemelle, Laurence Leroux, Hugues Leonard, Ariel Lettieri, Robert Marchant, William Nittler, Larry R. Ogliore, Ryan Ong, Wei Ja Postberg, Frank Price, Mark C. Sandford, Scott A. Tresseras, Juan-Angel Sans Simionovici, Alexandre S. Sole, Vicente A. Srama, Ralf Stadermann, Frank Stephan, Thomas Sterken, Veerle J. Stodolna, Julien Stroud, Rhonda M. Sutton, Steven Trieloff, Mario Tsou, Peter Tsuchiyama, Akira Tyliszczak, Tolek Von Korff, Joshua Wordsworth, Naomi Zevin, Daniel Zolensky, Michael E. TI Stardust Interstellar Preliminary Examination V: XRF analyses of interstellar dust candidates at ESRF ID13 SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID INTERPLANETARY DUST; AEROGEL; OLIVINE AB Here, we report analyses by synchrotron X-ray fluorescence microscopy of the elemental composition of eight candidate impact features extracted from the Stardust Interstellar Dust Collector (SIDC). Six of the features were unambiguous tracks, and two were crater-like features. Five of the tracks are so-called "midnight" tracks-that is, they had trajectories consistent with an origin either in the interstellar dust stream or as secondaries from impacts on the Sample Return Capsule (SRC). In a companion paper reporting synchrotron X-ray diffraction analyses of ISPE candidates, we show that two of these particles contain natural crystalline materials: the terminal particle of track 30 contains olivine and spinel, and the terminal particle of track 34 contains olivine. Here, we show that the terminal particle of track 30, Orion, shows elemental abundances, normalized to Fe, that are close to CI values, and a complex, fine-grained structure. The terminal particle of track 34, Hylabrook, shows abundances that deviate strongly from CI, but shows little fine structure and is nearly homogenous. The terminal particles of other midnight tracks, 29 and 37, had heavy element abundances below detection threshold. A third, track 28, showed a composition inconsistent with an extraterrestrial origin, but also inconsistent with known spacecraft materials. A sixth track, with a trajectory consistent with secondary ejecta from an impact on one of the spacecraft solar panels, contains abundant Ce and Zn. This is consistent with the known composition of the glass covering the solar panel. Neither crater-like feature is likely to be associated with extraterrestrial materials. We also analyzed blank aerogel samples to characterize background and variability between aerogel tiles. We found significant differences in contamination levels and compositions, emphasizing the need for local background subtraction for accurate quantification. C1 [Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, D-60438 Frankfurt, Germany. [Westphal, Andrew J.; Anderson, David; Butterworth, Anna L.; Gainsforth, Zack; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Vincze, Laszlo; Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart] Univ Ghent, Dept Analyt Chem, B-9000 Ghent, Belgium. [Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France. [Ansari, Asna; Hvide, Brit; King, Ashley J.] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Bajt, Sasa] DESY, D-22607 Hamburg, Germany. [Bastien, Ron K.; Frank, David R.] NASA, Lyndon B Johnson Space Ctr, ESCG, Houston, TX 77058 USA. [Bassim, Nabil; Stroud, Rhonda M.] Naval Res Lab, Nanoscale Mat Sect, Washington, DC 20375 USA. [Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94720 USA. [Borg, Janet] IAS Orsay, Orsay, France. [Bridges, John] Univ Leicester, Space Res Ctr, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury CT2 7NR, Kent, England. [Changela, Hitesh] George Washington Univ, Washington, DC 20052 USA. [Davis, Andrew M.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA. [Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja; Stadermann, Frank] Washington Univ, St Louis, MO 63130 USA. [Flynn, George] SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA. [Fougeray, Patrick] Chigy, Burgundy, Chigy, France. [Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Heck, Philipp R.; Hillier, Jon K.; Postberg, Frank] Inst Geowissensch, D-69120 Heidelberg, Germany. [Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany. [Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England. [Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Argonne, IL 60439 USA. [Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France. [Leroux, Hugues] Univ Lille 1, Unite Mat & Transformat UMR 8207, F-59655 Villeneuve Dascq, France. [Nittler, Larry R.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Ogliore, Ryan] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetary Sci, Honolulu, HI 96822 USA. [Sandford, Scott A.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. [Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France. [Srama, Ralf; Sterken, Veerle J.] Univ Stuttgart, Inst Raumfahrtsyst, D-70569 Stuttgart, Germany. [Trieloff, Mario] Inst Geowissensch, D-69120 Heidelberg, Germany. [Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tsuchiyama, Akira] Osaka Univ, Grad Sch Sci, Dept Earth & Planetary Sci, Osaka, Japan. RP Westphal, AJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM westphal@ssl.berkeley.edu RI Bajt, Sasa/G-2228-2010; Stroud, Rhonda/C-5503-2008; Sans Tresserras, Juan Angel/J-9362-2014; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015 OI Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943; Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner, Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X FU NASA [NNX09AC36G, NNH11AQ61I]; Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231]; U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-98CH10886]; German Science Foundation (DFG) FX This manuscript was improved due to the thoughtful comments of John Bradley. The ISPE consortium gratefully acknowledge the NASA Discovery Program for Stardust, the fourth NASA Discovery mission. AJW, ALB, ZG, RL, DZ, WM, and JVK were supported by NASA grant NNX09AC36G. We thank Steve Boggs for astrophysical soft X-ray spectra. RMS, HCG, and NDB were supported by NASA grant NNH11AQ61I. The Advanced Light Source is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Use of the National Synchrotron Light Source, Brookhaven National Laboratory, was supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract no. DE-AC02-98CH10886. We like to thank the ESRF for the allocated beamtime at ID13, instrumental and technical support. FEB and SS were supported by funding of the German Science Foundation (DFG). NR 28 TC 9 Z9 9 U1 1 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 IS 9 SI SI BP 1594 EP 1611 DI 10.1111/maps.12206 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ6HT UT WOS:000342912100005 ER PT J AU Simionovici, AS Lemelle, L Cloetens, P Sole, VA Tresseras, JAS Butterworth, AL Westphal, AJ Gainsforth, Z Stodolna, J Allen, C Anderson, D Ansari, A Bajt, S Bassim, N Bastien, RK Bechtel, HA Borg, J Brenker, FE Bridges, J Brownlee, DE Burchell, M Burghammer, M Changela, H Davis, AM Doll, R Floss, C Flynn, G Frank, DR Grun, E Heck, PR Hillier, JK Hoppe, P Hudson, B Huth, J Hvide, B Kearsley, A King, AJ Lai, B Leitner, J Leonard, A Leroux, H Lettieri, R Marchant, W Nittler, LR Ogliore, R Ong, WJ Postberg, F Price, MC Sandford, SA Schmitz, S Schoonjans, T Silversmit, G Srama, R Stadermann, FJ Stephan, T Sterken, VJ Stroud, RM Sutton, S Trieloff, M Tsou, P Tsuchiyama, A Tyliszczak, T Vekemans, B Vincze, L Von Korff, J Wordsworth, N Zevin, D Zolensky, ME AF Simionovici, Alexandre S. Lemelle, Laurence Cloetens, Peter Sole, Vicente A. Tresseras, Juan-Angel Sans Butterworth, Anna L. Westphal, Andrew J. Gainsforth, Zack Stodolna, Julien Allen, Carlton Anderson, David Ansari, Asna Bajt, Sasa Bassim, Nabil Bastien, Ron K. Bechtel, Hans A. Borg, Janet Brenker, Frank E. Bridges, John Brownlee, Donald E. Burchell, Mark Burghammer, Manfred Changela, Hitesh Davis, Andrew M. Doll, Ryan Floss, Christine Flynn, George Frank, David R. Gruen, Eberhard Heck, Philipp R. Hillier, Jon K. Hoppe, Peter Hudson, Bruce Huth, Joachim Hvide, Brit Kearsley, Anton King, Ashley J. Lai, Barry Leitner, Jan Leonard, Ariel Leroux, Hugues Lettieri, Robert Marchant, William Nittler, Larry R. Ogliore, Ryan Ong, Wei Ja Postberg, Frank Price, Mark C. Sandford, Scott A. Schmitz, Sylvia Schoonjans, Tom Silversmit, Geert Srama, Ralf Stadermann, Frank J. Stephan, Thomas Sterken, Veerle J. Stroud, Rhonda M. Sutton, Steven Trieloff, Mario Tsou, Peter Tsuchiyama, Akira Tyliszczak, Tolek Vekemans, Bart Vincze, Laszlo Von Korff, Joshua Wordsworth, Naomi Zevin, Daniel Zolensky, Michael E. TI Stardust Interstellar Preliminary Examination VI: Quantitative elemental analysis by synchrotron X-ray fluorescence nanoimaging of eight impact features in aerogel SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID COMET 81P/WILD-2; SOLAR-SYSTEM; DUST; GRAINS; CLOUD; GAS AB Hard X-ray, quantitative, fluorescence elemental imaging was performed on the ID22NI nanoprobe and ID22 microprobe beam lines of the European Synchrotron Research facility (ESRF) in Grenoble, France, on eight interstellar candidate impact features in the framework of the NASA Stardust Interstellar Preliminary Examination (ISPE). Three features were unambiguous tracks, and the other five were identified as possible, but not definite, impact features. Overall, we produced an absolute quantification of elemental abundances in the 15 <= Z <= 30 range by means of corrections of the beam parameters, reference materials, and fundamental atomic parameters. Seven features were ruled out as interstellar dust candidates (ISDC) based on compositional arguments. One of the three tracks, I1043,1,30,0,0, contained, at the time of our analysis, two physically separated, micrometer-sized terminal particles, the most promising ISDCs, Orion and Sirius. We found that the Sirius particle was a fairly homogenous Ni-bearing particle and contained about 33 fg of distributed high-Z elements (Z > 12). Orion was a highly heterogeneous Fe-bearing particle and contained about 59 fg of heavy elements located in hundred nanometer phases, forming an irregular mantle that surrounded a low-Z core. X-ray diffraction (XRD) measurements revealed Sirius to be amorphous, whereas Orion contained partially crystalline material (Gainsforth et al. 2014). Within the mantle, one grain was relatively Fe-Ni-Mn-rich; other zones were relatively Mn-Cr-Ti-rich and may correspond to different spinel populations. For absolute quantification purposes, Orion was assigned to a mineralogical assemblage of forsterite, spinel, and an unknown Fe-bearing phase, while Sirius was most likely composed of an amorphous Mg-bearing material with minor Ni and Fe. Owing to its nearly chondritic abundances of the nonvolatile elements Ca, Ti, Co, and Ni with respect to Fe, in combination with the presence of olivine and spinel as inferred from XRD measurements, Orion had a high probability of being extraterrestrial in origin. C1 [Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France. [Lemelle, Laurence] Ecole Normale Super Lyon, CNRS, LGL LJC, F-69364 Lyon, France. [Cloetens, Peter; Sole, Vicente A.; Tresseras, Juan-Angel Sans; Burghammer, Manfred] European Synchrotron Radiat Facil, F-38043 Grenoble, France. [Butterworth, Anna L.; Westphal, Andrew J.; Gainsforth, Zack; Stodolna, Julien; Anderson, David; Lettieri, Robert; Marchant, William; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA. [Allen, Carlton; Bastien, Ron K.; Frank, David R.; Zolensky, Michael E.] NASA JSC, ESCG, Houston, TX USA. [Ansari, Asna; Heck, Philipp R.; Hvide, Brit] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Bajt, Sasa] DESY, Hamburg, Germany. [Bassim, Nabil] Naval Res Lab, Washington, DC USA. [Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA. [Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany. [Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England. [Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Burchell, Mark; Price, Mark C.] Univ Kent, Sch Phys Sci, Canterbury, Kent, England. [Changela, Hitesh] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Davis, Andrew M.; King, Ashley J.; Stephan, Thomas] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja; Stadermann, Frank J.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Flynn, George] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA. [Gruen, Eberhard; Leitner, Jan] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany. [Hoppe, Peter; Huth, Joachim; Sterken, Veerle J.] Max Planck Inst Chem, D-55128 Mainz, Germany. [Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England. [Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA. [Leroux, Hugues] Univ Lille 1, F-59655 Villeneuve Dascq, France. [Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA. [Ogliore, Ryan] Univ Hawaii Manoa, Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Sandford, Scott A.] NASA Ames Res Ctr, Moffett Field, CA USA. [Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium. [Srama, Ralf; Sterken, Veerle J.] Univ Stuttgart, Inst Raumfahrtsyst, D-70174 Stuttgart, Germany. [Sterken, Veerle J.] TU Braunschweig, IGEP, Braunschweig, Germany. [Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA. [Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Tsuchiyama, Akira] Osaka Univ, Dept Earth & Space Sci, Osaka, Japan. RP Simionovici, AS (reprint author), Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France. EM Alexandre.Simionovici@ujf-grenoble.fr RI Sans Tresserras, Juan Angel/J-9362-2014; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015; Bajt, Sasa/G-2228-2010; Stroud, Rhonda/C-5503-2008; OI Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner, Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X; Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943 FU French "Centre National d'Etudes Spatiales" (CNES); NASA FX A. Simionovici and L. Lemelle acknowledge support from the French "Centre National d'Etudes Spatiales" (CNES). The Stardust mission was supported by NASA as the fourth mission in the Discovery program. NR 29 TC 8 Z9 8 U1 0 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 IS 9 SI SI BP 1612 EP 1625 DI 10.1111/maps.12208 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ6HT UT WOS:000342912100006 ER PT J AU Flynn, GJ Sutton, SR Lai, B Wirick, S Allen, C Anderson, D Ansari, A Bajt, S Bastien, RK Bassim, N Bechtel, HA Borg, J Brenker, FE Bridges, J Brownlee, DE Burchell, M Burghammer, M Butterworth, AL Changela, H Cloetens, P Davis, AM Doll, R Floss, C Frank, D Gainsforth, Z Grun, E Heck, PR Hillier, JK Hoppe, P Hudson, B Huth, J Hvide, B Kearsley, A King, AJ Leitner, J Lemelle, L Leroux, H Leonard, A Lettieri, R Marchant, W Nittler, LR Ogliore, R Ong, WJ Postberg, F Price, MC Sandford, SA Tresseras, JAS Schmitz, S Schoonjans, T Silversmit, G Simionovici, A Sole, VA Srama, R Stadermann, FJ Stephan, T Sterken, V Stodolna, J Stroud, RM Trieloff, M Tsou, P Tsuchiyama, A Tyliszczak, T Vekemans, B Vincze, L Von Korff, J Westphal, AJ Wordsworth, N Zevin, D Zolensky, ME AF Flynn, George J. Sutton, Steven R. Lai, Barry Wirick, Sue Allen, Carlton Anderson, David Ansari, Asna Bajt, Sasa Bastien, Ron K. Bassim, Nabil Bechtel, Hans A. Borg, Janet Brenker, Frank E. Bridges, John Brownlee, Donald E. Burchell, Mark Burghammer, Manfred Butterworth, Anna L. Changela, Hitesh Cloetens, Peter Davis, Andrew M. Doll, Ryan Floss, Christine Frank, David Gainsforth, Zack Gruen, Eberhard Heck, Philipp R. Hillier, Jon K. Hoppe, Peter Hudson, Bruce Huth, Joachim Hvide, Brit Kearsley, Anton King, Ashley J. Leitner, Jan Lemelle, Laurence Leroux, Hugues Leonard, Ariel Lettieri, Robert Marchant, William Nittler, Larry R. Ogliore, Ryan Ong, Wei Ja Postberg, Frank Price, Mark C. Sandford, Scott A. Tresseras, Juan-Angel Sans Schmitz, Sylvia Schoonjans, Tom Silversmit, Geert Simionovici, Alexandre Sole, Vicente A. Srama, Ralf Stadermann, Frank J. Stephan, Thomas Sterken, Veerle Stodolna, Julien Stroud, Rhonda M. Trieloff, Mario Tsou, Peter Tsuchiyama, Akira Tyliszczak, Tolek Vekemans, Bart Vincze, Laszlo Von Korff, Joshua Westphal, Andrew J. Wordsworth, Naomi Zevin, Daniel Zolensky, Michael E. TI Stardust Interstellar Preliminary Examination VII: Synchrotron X-ray fluorescence analysis of six Stardust interstellar candidates measured with the Advanced Photon Source 2-ID-D microprobe SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID COMET 81P/WILD-2; SOLAR-SYSTEM; DUST; ABUNDANCES; ELEMENTS AB The NASA Stardust spacecraft exposed an aerogel collector to the interstellar dust passing through the solar system. We performed X-ray fluorescence element mapping and abundance measurements, for elements 19 <= Z <= 30, on six "interstellar candidates," potential interstellar impacts identified by Stardust@Home and extracted for analyses in picokeystones. One, I1044,3,33, showed no element hot-spots within the designated search area. However, we identified a nearby surface feature, consistent with the impact of a weak, high-speed particle having an approximately chondritic (CI) element abundance pattern, except for factor-of-ten enrichments in K and Zn and an S depletion. This hot-spot, containing approximately 10 fg of Fe, corresponds to an approximately 350 nm chondritic particle, small enough to be missed by Stardust@Home, indicating that other techniques may be necessary to identify all interstellar candidates. Only one interstellar candidate, I1004,1,2, showed a track. The terminal particle has large enrichments in S, Ti, Cr, Mn, Ni, Cu, and Zn relative to Fe-normalized CI values. It has high Al/Fe, but does not match the Ni/Fe range measured for samples of Al-deck material from the Stardust sample return capsule, which was within the field-of-view of the interstellar collector. A third interstellar candidate, I1075,1,25, showed an Al-rich surface feature that has a composition generally consistent with the Al-deck material, suggesting that it is a secondary particle. The other three interstellar candidates, I1001,1,16, I1001,2,17, and I1044,2,32, showed no impact features or tracks, but allowed assessment of submicron contamination in this aerogel, including Fe hot-spots having CI-like Ni/Fe ratios, complicating the search for CI-like interstellar/interplanetary dust. C1 [Flynn, George J.] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA. [Sutton, Steven R.; Lai, Barry] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA. [Sutton, Steven R.; Wirick, Sue] Univ Chicago, CARS, Chicago, IL 60637 USA. [Allen, Carlton; Bastien, Ron K.; Frank, David; Zolensky, Michael E.] NASA JSC, ARES, Houston, TX USA. [Anderson, David; Butterworth, Anna L.; Gainsforth, Zack; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Westphal, Andrew J.; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA. [Ansari, Asna; Heck, Philipp R.; Hvide, Brit] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Bajt, Sasa] DESY, Hamburg, Germany. [Bassim, Nabil] Naval Res Lab, Washington, DC USA. [Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA. [Borg, Janet] IAS Orsay, Orsay, France. [Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany. [Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England. [Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury CT2 7NZ, Kent, England. [Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France. [Changela, Hitesh] George Washington Univ, Washington, DC USA. [Davis, Andrew M.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA. [Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja; Stadermann, Frank J.] Washington Univ, St Louis, MO USA. [Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany. [Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany. [Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England. [King, Ashley J.] Univ Chicago, Chicago, IL 60637 USA. [King, Ashley J.] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France. [Leroux, Hugues] Univ Lille 1, UMR CNRS 8008, Lab Struct & Proprietes Etat Solide, F-59655 Villeneuve Dascq, France. [Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA. [Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium. [Simionovici, Alexandre] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France. [Srama, Ralf] Univ Stuttgart, Inst Raumfahrtsyst, D-70174 Stuttgart, Germany. [Sterken, Veerle] Univ Stuttgart, D-70174 Stuttgart, Germany. [Sterken, Veerle] TU Braunschweig, Inst Geophys & Extraterrestrial Phys, Braunschweig, Germany. [Sterken, Veerle] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA. [Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Tsuchiyama, Akira] Osaka Univ, Osaka, Japan. RP Flynn, GJ (reprint author), SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA. EM flynngj@plattsburgh.edu RI Bajt, Sasa/G-2228-2010; Sans Tresserras, Juan Angel/J-9362-2014; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015 OI Burchell, Mark/0000-0002-2680-8943; Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner, Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X FU NASA; NASA Laboratory Analysis of Returned Samples research grant [NNX11AE15G]; U.S. DOE [DE-AC02-06CH11357]; Department of Energy (DOE)-Geosciences [DE-FG02-92ER14244]; DOE [DE-AC02-98CH10886] FX The Stardust interstellar dust collection mission was supported by NASA as the fourth mission in the Discovery program. This analytical work was supported by a NASA Laboratory Analysis of Returned Samples research grant NNX11AE15G (to G. J. F.). Use of the Advanced Photon Source, an Office of Science User Facility operated for the U.S. Department of Energy (DOE) Office of Science by Argonne National Laboratory, was supported by the U.S. DOE under Contract No. DE-AC02-06CH11357. Portions of this work were performed at Beamline X26A, National Synchrotron Light Source (NSLS), Brookhaven National Laboratory. X26A is supported by the Department of Energy (DOE)-Geosciences (DE-FG02-92ER14244 to The University of Chicago-CARS). Use of the NSLS was supported by DOE under Contract No. DE-AC02-98CH10886. NR 20 TC 9 Z9 9 U1 0 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 IS 9 SI SI BP 1626 EP 1644 DI 10.1111/maps.12144 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ6HT UT WOS:000342912100007 ER PT J AU Gainsforth, Z Brenker, FE Simionovici, AS Schmitz, S Burghammer, M Butterworth, AL Cloetens, P Lemelle, L Tresserras, JAS Schoonjans, T Silversmit, G Sole, VA Vekemans, B Vincze, L Westphal, AJ Allen, C Anderson, D Ansari, A Bajt, S Bastien, RK Bassim, N Bechtel, HA Borg, J Bridges, J Brownlee, DE Burchell, M Changela, H Davis, AM Doll, R Floss, C Flynn, G Fougeray, P Frank, D Grun, E Heck, PR Hillier, JK Hoppe, P Hudson, B Huth, J Hvide, B Kearsley, A King, AJ Lai, B Leitner, J Leroux, H Leonard, A Lettieri, R Marchant, W Nittler, LR Ogliore, R Ong, WJ Postberg, F Price, MC Sandford, SA Srama, R Stephan, T Sterken, V Stodolna, J Stroud, RM Sutton, S Trieloff, M Tsou, P Tsuchiyama, A Tyliszczak, T Von Korff, J Zevin, D Zolensky, ME AF Gainsforth, Zack Brenker, Frank E. Simionovici, Alexandre S. Schmitz, Sylvia Burghammer, Manfred Butterworth, Anna L. Cloetens, Peter Lemelle, Laurence Tresserras, Juan-Angel Sans Schoonjans, Tom Silversmit, Geert Sole, Vicente A. Vekemans, Bart Vincze, Laszlo Westphal, Andrew J. Allen, Carlton Anderson, David Ansari, Asna Bajt, Sasa Bastien, Ron K. Bassim, Nabil Bechtel, Hans A. Borg, Janet Bridges, John Brownlee, Donald E. Burchell, Mark Changela, Hitesh Davis, Andrew M. Doll, Ryan Floss, Christine Flynn, George Fougeray, Patrick Frank, David Gruen, Eberhard Heck, Philipp R. Hillier, Jon K. Hoppe, Peter Hudson, Bruce Huth, Joachim Hvide, Brit Kearsley, Anton King, Ashley J. Lai, Barry Leitner, Jan Leroux, Hugues Leonard, Ariel Lettieri, Robert Marchant, William Nittler, Larry R. Ogliore, Ryan Ong, Wei Ja Postberg, Frank Price, Mark C. Sandford, Scott A. Srama, Ralf Stephan, Thomas Sterken, Veerle Stodolna, Julien Stroud, Rhonda M. Sutton, Steven Trieloff, Mario Tsou, Peter Tsuchiyama, Akira Tyliszczak, Tolek Von Korff, Joshua Zevin, Daniel Zolensky, Michael E. TI Stardust Interstellar Preliminary Examination VIII: Identification of crystalline material in two interstellar candidates SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID DUST PARTICLES; ORDER-DISORDER; AEROGEL; DIFFRACTION; GRAINS; DIMENSIONS; COLLECTION; SILICATES; GRAPHITE; OLIVINES AB Using synchrotron-based X-ray diffraction measurements, we identified crystalline material in two particles of extraterrestrial origin extracted from the Stardust Interstellar Dust Collector. The first particle, I1047,1,34 (Hylabrook), consisted of a mosaiced olivine grain approximately 1 mu m in size with internal strain fields up to 0.3%. The unit cell dimensions were a - 4.85 +/- 0.08 angstrom, b - 10.34 +/- 0.16 angstrom, c - 6.08 +/- 0.13 angstrom (2 sigma). The second particle, I1043,1,30 (Orion), contained an olivine grain approximate to 2 mu m in length and > 500 nm in width. It was polycrystalline with both mosaiced domains varying over approximate to 20 degrees and additional unoriented domains, and contained internal strain fields < 1%. The unit cell dimensions of the olivine were a = 4.76 +/- 0.05 angstrom, b = 10.23 +/- 0.10 angstrom, c = 5.99 +/- 0.06 angstrom (2 sigma), which limited the olivine to a forsteritic composition [Fo(65) (2 sigma). Orion also contained abundant spinel nanocrystals of unknown composition, but unit cell dimension a = 8.06 +/- 0.08 angstrom (2 sigma). Two additional crystalline phases were present and remained unidentified. An amorphous component appeared to be present in both these particles based on STXM and XRF results reported elsewhere. C1 [Gainsforth, Zack; Butterworth, Anna L.; Westphal, Andrew J.; Anderson, David; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany. [Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France. [Burghammer, Manfred; Cloetens, Peter; Tresserras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France. [Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France. [Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, Dept Analyt Chem, B-9000 Ghent, Belgium. [Allen, Carlton; Zolensky, Michael E.] NASA JSC, ARES, Houston, TX USA. [Ansari, Asna; Heck, Philipp R.; Hvide, Brit] Field Museum Nat Hist, Chicago, IL 60605 USA. [Bajt, Sasa] DESY, Hamburg, Germany. [Bastien, Ron K.; Frank, David] NASA JSC, ESCG, Houston, TX USA. [Bassim, Nabil; Stroud, Rhonda M.] Naval Res Lab, Washington, DC USA. [Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA. [Borg, Janet] IAS Orsay, Orsay, France. [Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England. [Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Burchell, Mark; Price, Mark C.] Univ Kent, Sch Phys Sci, Canterbury, Kent, England. [Changela, Hitesh] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Davis, Andrew M.; Stephan, Thomas] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Flynn, George; Sterken, Veerle] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA. [Fougeray, Patrick] Chigy, Burgundy, France. [Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany. [Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany. [Kearsley, Anton; King, Ashley J.] Nat Hist Museum, London SW7 5BD, England. [Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA. [Leroux, Hugues] Univ Lille 1, Lille, France. [Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA. [Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Hillier, Jon K.; Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Srama, Ralf; Sterken, Veerle] Univ Stuttgart, IRS, D-70174 Stuttgart, Germany. [Sterken, Veerle] TU Braunschweig, IGEP, Braunschweig, Germany. [Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Tsuchiyama, Akira] Osaka Univ, Osaka, Japan. RP Gainsforth, Z (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM zackg@ssl.berkeley.edu RI Stroud, Rhonda/C-5503-2008; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015; Bajt, Sasa/G-2228-2010 OI Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943; Leitner, Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X; FU NASA [NNX09AC36G]; Office of Science, Office of Basic Energy Sciences, U.S. Department of Energy [DE-AC02-05CH11231] FX Zack Gainsforth, Andrew J. Westphal, Anna L. Butterworth were supported by NASA grant NNX09AC36G. The operations of the Advanced Light Source at Lawrence Berkeley National Laboratory are supported by the Director, Office of Science, Office of Basic Energy Sciences, U.S. Department of Energy under contract number DE-AC02-05CH11231. NR 54 TC 7 Z9 7 U1 0 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 IS 9 SI SI BP 1645 EP 1665 DI 10.1111/maps.12148 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ6HT UT WOS:000342912100008 ER PT J AU Postberg, F Hillier, JK Armes, SP Bugiel, S Butterworth, A Dupin, D Fielding, LA Fujii, S Gainsforth, Z Grun, E Li, YW Srama, R Sterken, V Stodolna, J Trieloff, M Westphal, A Achilles, C Allen, C Ansari, A Bajt, S Bassim, N Bastien, RK Bechtel, HA Borg, J Brenker, F Bridges, J Brownlee, DE Burchell, M Burghammer, M Changela, H Cloetens, P Davis, A Doll, R Floss, C Flynn, G Frank, D Heck, PR Hoppe, P Huss, G Huth, J Kearsley, A King, AJ Lai, B Leitner, J Lemelle, L Leonard, A Leroux, H Lettieri, R Marchant, W Nittler, LR Ogliore, R Ong, WJ Price, MC Sandford, SA Tressaras, JAS Schmitz, S Schoonjans, T Schreiber, K Silversmit, G Simionovici, A Sole, VA Stadermann, F Stephan, T Stroud, RM Sutton, S Tsou, P Tsuchiyama, A Tyliczszak, T Vekemans, B Vincze, L Zevin, D Zolensky, ME AF Postberg, F. Hillier, J. K. Armes, S. P. Bugiel, S. Butterworth, A. Dupin, D. Fielding, L. A. Fujii, S. Gainsforth, Z. Gruen, E. Li, Y. W. Srama, R. Sterken, V. Stodolna, J. Trieloff, M. Westphal, A. Achilles, C. Allen, C. Ansari, A. Bajt, S. Bassim, N. Bastien, R. K. Bechtel, H. A. Borg, J. Brenker, F. Bridges, J. Brownlee, D. E. Burchell, M. Burghammer, M. Changela, H. Cloetens, P. Davis, A. Doll, R. Floss, C. Flynn, G. Frank, D. Heck, P. R. Hoppe, P. Huss, G. Huth, J. Kearsley, A. King, A. J. Lai, B. Leitner, J. Lemelle, L. Leonard, A. Leroux, H. Lettieri, R. Marchant, W. Nittler, L. R. Ogliore, R. Ong, W. J. Price, M. C. Sandford, S. A. Tressaras, J. -A. Sans Schmitz, S. Schoonjans, T. Schreiber, K. Silversmit, G. Simionovici, A. Sole, V. A. Stadermann, F. Stephan, T. Stroud, R. M. Sutton, S. Tsou, P. Tsuchiyama, A. Tyliczszak, T. Vekemans, B. Vincze, L. Zevin, D. Zolensky, M. E. TI Stardust Interstellar Preliminary Examination IX: High-speed interstellar dust analog capture in Stardust flight-spare aerogel SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID COMET 81P/WILD 2; IMPACT FEATURES; MICROPARTICLES; PARTICLES; TRACKS AB The NASA Stardust mission used silica aerogel slabs to slowly decelerate and capture impinging cosmic dust particles for return to Earth. During this process, impact tracks are generated along the trajectory of the particle into the aerogel. It is believed that the morphology and dimensions of these tracks, together with the state of captured grains at track termini, may be linked to the size, velocity, and density of the impacting cosmic dust grain. Here, we present the results of laboratory hypervelocity impact experiments, during which cosmic dust analog particles (diameters of between 0.2 and 0.4 mu m), composed of olivine, orthopyroxene, or an organic polymer, were accelerated onto Stardust flight-spare low-density (approximately 0.01 g cm(-3)) silica aerogel. The impact velocities (3-21 km s(-1)) were chosen to simulate the range of velocities expected during Stardust's interstellar dust (ISD) collection phases. Track lengths and widths, together with the success of particle capture, are analyzed as functions of impact velocity and particle composition, density, and size. Captured terminal particles from low-density organic projectiles become undetectable at lower velocities than those from similarly sized, denser mineral particles, which are still detectable (although substantially altered by the impact process) at 15 km s(-1). The survival of these terminal particles, together with the track dimensions obtained during low impact speed capture of small grains in the laboratory, indicates that two of the three best Stardust candidate extraterrestrial grains were actually captured at speeds much lower than predicted. Track length and diameters are, in general, more sensitive to impact velocities than previously expected, which makes tracks of particles with diameters of 0.4 mu m and below hard to identify at low capture speeds (<10 km s(-1)). Therefore, although captured intact, the majority of the interstellar dust grains returned to Earth by Stardust remain to be found. C1 [Postberg, F.; Bugiel, S.; Li, Y. W.; Srama, R.; Sterken, V.] Univ Stuttgart, Inst Raumfahrtsyst, Stuttgart, Germany. [Postberg, F.; Hillier, J. K.; Trieloff, M.] Heidelberg Univ, Inst Geowissensch, D-69115 Heidelberg, Germany. [Armes, S. P.; Dupin, D.; Fielding, L. A.; Fujii, S.] Univ Sheffield, Dept Chem, Sheffield, S Yorkshire, England. [Bugiel, S.; Gruen, E.; Li, Y. W.; Sterken, V.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Butterworth, A.; Gainsforth, Z.; Stodolna, J.; Westphal, A.; Lettieri, R.; Marchant, W.; Zevin, D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA. [Gruen, E.] Univ Colorado, LASP, Boulder, CO 80309 USA. [Li, Y. W.] Harbin Inst Technol, Sch Mat Sci & Engn, Harbin 150006, Peoples R China. [Sterken, V.] Tech Univ Carolo Wilhelmina Braunschweig, IGEP, D-38106 Braunschweig, Germany. [Achilles, C.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Allen, C.; Bastien, R. K.; Frank, D.; Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. [Ansari, A.; Davis, A.; King, A. J.; Stephan, T.] Univ Chicago, Chicago, IL 60637 USA. [Bajt, S.] DESY, Hamburg, Germany. [Bassim, N.; Changela, H.; Stroud, R. M.] Naval Res Lab, Washington, DC USA. [Bechtel, H. A.; Tyliczszak, T.] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA. [Borg, J.] IAS Orsay, Orsay, France. [Brenker, F.; Schmitz, S.] Univ Frankfurt Main, Inst Geowissensch, Frankfurt, Germany. [Bridges, J.] Univ Leicester, Space Res Ctr, Leicester, Leics, England. [Brownlee, D. E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Burchell, M.; Price, M. C.] Univ Kent, Sch Phys Sci, Canterbury, Kent, England. [Burghammer, M.; Cloetens, P.; Tressaras, J. -A. Sans; Sole, V. A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France. [Changela, H.] George Washington Univ, Washington, DC USA. [Doll, R.; Floss, C.; Leonard, A.; Ong, W. J.; Schreiber, K.; Stadermann, F.] Washington Univ, St Louis, MO USA. [Flynn, G.] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA. [Heck, P. R.] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Hoppe, P.; Huth, J.; Leitner, J.] Max Planck Inst Chem, D-55128 Mainz, Germany. [Huss, G.; Ogliore, R.] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Kearsley, A.] Nat Hist Museum, London SW7 5BD, England. [Lai, B.; Sutton, S.] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA. [Lemelle, L.] Ecole Normale Super Lyon, F-69364 Lyon, France. [Leroux, H.] Univ Lille 1, Lille, France. [Nittler, L. R.] Carnegie Inst Sci, Washington, DC USA. [Sandford, S. A.] NASA Ames Res Ctr, Moffett Field, CA USA. [Schoonjans, T.; Silversmit, G.; Vekemans, B.; Vincze, L.] Univ Ghent, B-9000 Ghent, Belgium. [Simionovici, A.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France. [Tsou, P.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Tsuchiyama, A.] Osaka Univ, Osaka, Japan. RP Postberg, F (reprint author), Univ Stuttgart, Inst Raumfahrtsyst, Stuttgart, Germany. EM postberg@irs.uni-stuttgart.de RI Fielding, Lee/B-8440-2011; Stroud, Rhonda/C-5503-2008; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015; Bajt, Sasa/G-2228-2010; OI Fielding, Lee/0000-0002-4958-1155; Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943; Armes, Steven/0000-0002-8289-6351; Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner, Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X; Fujii, Syuji/0000-0003-2562-9502 FU NASA [NNX09AC36G, NNH11AQ61I]; Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy [DE-AC02- 05CH11231]; U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-98CH10886]; DFG [1385]; Klaus Tschira Stiftung GmbH FX The ISPE consortium gratefully acknowledge the NASA Discovery Program for Stardust, the fourth NASA Discovery mission. AJW, ALB, ZG, RL, DZ, WM and JVK were supported by NASA grant NNX09AC36G. We thank Steve Boggs for astrophysical soft x-ray spectra. RMS, HCG and NDB were supported by NASA grant NNH11AQ61I. The Advanced Light Source is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract No. DE-AC02- 05CH11231. Use of the National Synchrotron Light Source, Brookhaven National Laboratory, was supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DE-AC02-98CH10886.; FP, JKH, RS and MT acknowledge funding by DFG special priority program 1385 "The First 10 Million years of the Solar System" and the support by Klaus Tschira Stiftung GmbH. NR 28 TC 11 Z9 11 U1 2 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 IS 9 SI SI BP 1666 EP 1679 DI 10.1111/maps.12173 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ6HT UT WOS:000342912100009 ER PT J AU Sterken, VJ Westphal, AJ Altobelli, N Grun, E Hillier, JK Postberg, F Srama, R Allen, C Anderson, D Ansari, A Bajt, S Bastien, RS Bassim, N Bechtel, HA Borg, J Brenker, FE Bridges, J Brownlee, DE Burchell, M Burghammer, M Butterworth, AL Changela, H Cloetens, P Davis, AM Doll, R Floss, C Flynn, G Frank, D Gainsforth, Z Heck, PR Hoppe, P Hudson, B Huth, J Hvide, B Kearsley, A King, AJ Lai, B Leitner, J Lemelle, L Leroux, H Leonard, A Lettieri, R Marchant, W Nittler, LR Ogliore, R Ong, WJ Price, MC Sandford, SA Tresseras, JAS Schmitz, S Schoonjans, T Silversmit, G Simionovici, A Sole, VA Stephan, T Stodolna, J Stroud, RM Sutton, S Trieloff, M Tsou, P Tsuchiyama, A Tyliszczak, T Vekemans, B Vincze, L Von Korff, J Wordsworth, N Zevin, D Zolensky, ME AF Sterken, Veerle J. Westphal, Andrew J. Altobelli, Nicolas Gruen, Eberhard Hillier, Jon K. Postberg, Frank Srama, Ralf Allen, Carlton Anderson, David Ansari, Asna Bajt, Sasa Bastien, Ron S. Bassim, Nabil Bechtel, Hans A. Borg, Janet Brenker, Frank E. Bridges, John Brownlee, Donald E. Burchell, Mark Burghammer, Manfred Butterworth, Anna L. Changela, Hitesh Cloetens, Peter Davis, Andrew M. Doll, Ryan Floss, Christine Flynn, George Frank, David Gainsforth, Zack Heck, Philipp R. Hoppe, Peter Hudson, Bruce Huth, Joachim Hvide, Brit Kearsley, Anton King, Ashley J. Lai, Barry Leitner, Jan Lemelle, Laurence Leroux, Hugues Leonard, Ariel Lettieri, Robert Marchant, William Nittler, Larry R. Ogliore, Ryan Ong, Wei Ja Price, Mark C. Sandford, S. A. Tresseras, Juan-Angel Sans Schmitz, Sylvia Schoonjans, Tom Silversmit, Geert Simionovici, Alexandre Sole, Vicente A. Stephan, Thomas Stodolna, Julien Stroud, Rhonda M. Sutton, Steven Trieloff, Mario Tsou, Peter Tsuchiyama, Akira Tyliszczak, Tolek Vekemans, Bart Vincze, Laszlo Von Korff, Joshua Wordsworth, Naomi Zevin, Daniel Zolensky, Michael E. TI Stardust Interstellar Preliminary Examination X: Impact speeds and directions of interstellar grains on the Stardust dust collector SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID RADIATION PRESSURE; SIZE DISTRIBUTION; SAMPLE RETURN; EARTH; HELIOSPHERE; PARTICLES; AEROGEL; MATTER; SARIM AB On the basis of an interstellar dust model compatible with Ulysses and Galileo observations, we calculate and predict the trajectories of interstellar dust (ISD) in the solar system and the distribution of the impact speeds, directions, and flux of ISD particles on the Stardust Interstellar Dust Collector during the two collection periods of the mission. We find that the expected impact velocities are generally low (<10 km s(-1)) for particles with the ratio of the solar radiation pressure force to the solar gravitational force beta > 1, and that some of the particles will impact on the cometary side of the collector. If we assume astronomical silicates for particle material and a density of 2 g cm(-3), and use the Ulysses measurements and the ISD trajectory simulations, we conclude that the total number of (detectable) captured ISD particles may be on the order of 50. In companion papers in this volume, we report the discovery of three interstellar dust candidates in the Stardust aerogel tiles. The impact directions and speeds of these candidates are consistent with those calculated from our ISD propagation model, within the uncertainties of the model and of the observations. C1 [Sterken, Veerle J.] Univ Stuttgart, Inst Raumfahrtsyst, D-70569 Stuttgart, Germany. [Sterken, Veerle J.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extreterr Phys, D-38106 Braunschweig, Germany. [Westphal, Andrew J.; Anderson, David; Butterworth, Anna L.; Gainsforth, Zack; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Altobelli, Nicolas] European Space Agcy, Madrid, Spain. [Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany. [Srama, Ralf] Univ Stuttgart, Inst Raumfahrtsyst, D-70174 Stuttgart, Germany. [Allen, Carlton; Zolensky, Michael E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Ansari, Asna; Hvide, Brit] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Bajt, Sasa] DESY, Hamburg, Germany. [Bastien, Ron S.; Frank, David] NASA, Lyndon B Johnson Space Ctr, Engn & Sci Contract Grp, Houston, TX 77058 USA. [Bassim, Nabil] Naval Res Lab, Washington, DC USA. [Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA. [Borg, Janet] Inst Astrophys Spatiale, Orsay, France. [Brenker, Frank E.] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany. [Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England. [Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Burchell, Mark; Price, Mark C.] Univ Kent, Sch Phys Sci, Canterbury, Kent, England. [Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France. [Changela, Hitesh] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Davis, Andrew M.; Stephan, Thomas] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Flynn, George] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA. [Heck, Philipp R.] Field Museum Nat Hist, Chicago, IL 60605 USA. [Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany. [Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England. [King, Ashley J.] Univ Chicago, Chicago, IL 60637 USA. [King, Ashley J.] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA. [Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France. [Leroux, Hugues] Univ Sci & Tech Lille, Lille, France. [Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA. [Ogliore, Ryan] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Sandford, S. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Schmitz, Sylvia] Univ Frankfurt Main, Inst Geowissensch, Frankfurt, Germany. [Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, Dept Analyt Chem, B-9000 Ghent, Belgium. [Simionovici, Alexandre] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France. [Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA. [Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Tsuchiyama, Akira] Osaka Univ, Dept Earth & Space Sci, Osaka, Japan. RP Sterken, VJ (reprint author), Int Space Sci Inst ISSI, Hallerstr 6, CH-3012 Bern, Switzerland. EM veerle.sterken@issibern.ch RI Sans Tresserras, Juan Angel/J-9362-2014; Bajt, Sasa/G-2228-2010; Stroud, Rhonda/C-5503-2008; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015 OI Sans Tresserras, Juan Angel/0000-0001-9047-3992; Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943; Leitner, Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X FU NASA [NNX09AC36G, NNH11AQ61I]; ESA; Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231]; U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-98CH10886] FX We thank the reviewers and the AE Christian Koeberl, for their thoughtful reviews that greatly improved this manuscript. We also thank the AE John Bradley for his critical input and time and effort spent reviewing the ISPE manuscripts. The ISPE consortium gratefully acknowledge the NASA Discovery Program for Stardust, the fourth NASA Discovery mission. AJW, ALB, ZG, RL, DZ, WM, and JVK were supported by NASA grant NNX09AC36G. RMS, HCG, and NDB were supported by NASA grant NNH11AQ61I. VJS acknowledges support from ESA. The Advanced Light Source is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Use of the National Synchrotron Light Source, Brookhaven National Laboratory, was supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DE-AC02-98CH10886. NR 37 TC 15 Z9 15 U1 0 U2 12 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 IS 9 SI SI BP 1680 EP 1697 DI 10.1111/maps.12219 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ6HT UT WOS:000342912100010 ER PT J AU Stroud, RM Allen, C Ansari, A Anderson, D Bajt, S Bassim, N Bastien, RS Bechtel, HA Borg, J Brenker, FE Bridges, J Brownlee, DE Burchell, M Burghammer, M Butterworth, AL Changela, H Cloetens, P Davis, AM Doll, R Floss, C Flynn, G Frank, DR Gainsforth, Z Grun, E Heck, PR Hillier, JK Hoppe, P Huth, J Hvide, B Kearsley, A King, AJ Kotula, P Lai, B Leitner, J Lemelle, L Leroux, H Leonard, A Lettieri, R Marchant, W Nittler, LR Ogliore, R Ong, WJ Postberg, F Price, MC Sandford, SA Tresseras, JAS Schmitz, S Schoonjans, T Schreiber, K Silversmit, G Simionovici, AS Sole, VA Srama, R Stephan, T Sterken, VJ Stodolna, J Sutton, S Trieloff, M Tsou, P Tsuchiyama, A Tyliszczak, T Vekemans, B Vincze, L Westphal, AJ Von Korff, J Zevin, D Zolensky, ME AF Stroud, Rhonda M. Allen, Carlton Ansari, Asna Anderson, David Bajt, Sasa Bassim, Nabil Bastien, Ron S. Bechtel, Hans A. Borg, Janet Brenker, Frank E. Bridges, John Brownlee, Donald E. Burchell, Mark Burghammer, Manfred Butterworth, Anna L. Changela, Hitesh Cloetens, Peter Davis, Andrew M. Doll, Ryan Floss, Christine Flynn, George Frank, David R. Gainsforth, Zack Gruen, Eberhard Heck, Philipp R. Hillier, Jon K. Hoppe, Peter Huth, Joachim Hvide, Brit Kearsley, Anton King, Ashley J. Kotula, Paul Lai, Barry Leitner, Jan Lemelle, Laurence Leroux, Hugues Leonard, Ariel Lettieri, Robert Marchant, William Nittler, Larry R. Ogliore, Ryan Ong, Wei Jia Postberg, Frank Price, Mark C. Sandford, Scott A. Tresseras, Juan-Angel Sans Schmitz, Sylvia Schoonjans, Tom Schreiber, Kate Silversmit, Geert Simionovici, Alexandre S. Sole, Vicente A. Srama, Ralf Stephan, Thomas Sterken, Veerle J. Stodolna, Julien Sutton, Steven Trieloff, Mario Tsou, Peter Tsuchiyama, Akira Tyliszczak, Tolek Vekemans, Bart Vincze, Laszlo Westphal, Andrew J. Von Korff, Joshua Zevin, Daniel Zolensky, Michael E. TI Stardust Interstellar Preliminary Examination XI: Identification and elemental analysis of impact craters on Al foils from the Stardust Interstellar Dust Collector SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID TRANSMISSION ELECTRON-MICROSCOPY; COMET 81P/WILD 2; ISOTOPIC COMPOSITIONS; ALUMINUM FOILS; RESIDUES; FEATURES; AEROGEL; MORPHOLOGY; MISSION; MATTER AB The Stardust Interstellar Preliminary Examination team analyzed thirteen Al foils from the NASA Stardust interstellar collector tray in order to locate candidate interstellar dust (ISD) grain impacts. Scanning electron microscope (SEM) images reveal that the foils possess abundant impact crater and crater-like features. Elemental analyses of the crater features, with Auger electron spectroscopy, SEM-based energy dispersive X-ray (EDX) spectroscopy, and scanning transmission electron microscope-based EDX spectroscopy, demonstrate that the majority are either the result of impacting debris fragments from the spacecraft solar panels, or intrinsic defects in the foil. The elemental analyses also reveal that four craters contain residues of a definite extraterrestrial origin, either as interplanetary dust particles or ISD particles. These four craters are designated level 2 interstellar candidates, based on the crater shapes indicative of hypervelocity impacts and the residue compositions inconsistent with spacecraft debris. C1 [Stroud, Rhonda M.; Bassim, Nabil; Changela, Hitesh] Naval Res Lab, Mat Sci & Technol Div, Washington, DC 20375 USA. [Allen, Carlton; Zolensky, Michael E.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. [Ansari, Asna; Heck, Philipp R.; Hvide, Brit; Marchant, William] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Anderson, David; Butterworth, Anna L.; Gainsforth, Zack; Lettieri, Robert; Stodolna, Julien; Westphal, Andrew J.; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA. [Bajt, Sasa] DESY, Hamburg, Germany. [Bastien, Ron S.; Frank, David R.] NASA, Lyndon B Johnson Space Ctr, JETS, Houston, TX 77058 USA. [Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA. [Borg, Janet] IAS Orsay, Orsay, France. [Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geowissensch, Frankfurt, Germany. [Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England. [Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury, Kent, England. [Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France. [Changela, Hitesh] George Washington Univ, Washington, DC USA. [Davis, Andrew M.; King, Ashley J.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA. [Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Jia; Schreiber, Kate] Washington Univ, St Louis, MO USA. [Flynn, George] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA. [Gruen, Eberhard; Srama, Ralf] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany. [Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany. [Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England. [Kotula, Paul] Sandia Natl Labs, Albuquerque, NM USA. [Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA. [Lemelle, Laurence] ENS, Lyon, France. [Leroux, Hugues] Univ Sci & Techol Lille, Lille, France. [Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA. [Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Sandford, Scott A.; Vincze, Laszlo] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart] Univ Ghent, B-9000 Ghent, Belgium. [Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France. [Srama, Ralf] TU Braunschweig, IGEP, Braunschweig, Germany. [Sterken, Veerle J.] Univ Stuttgart, IRS, D-70174 Stuttgart, Germany. [Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Tsuchiyama, Akira] Osaka Univ, Osaka, Japan. RP Stroud, RM (reprint author), Naval Res Lab, Mat Sci & Technol Div, Washington, DC 20375 USA. EM stroud@nrl.navy.mil RI Sans Tresserras, Juan Angel/J-9362-2014; Kotula, Paul/A-7657-2011; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015; Bajt, Sasa/G-2228-2010; Stroud, Rhonda/C-5503-2008; OI Sans Tresserras, Juan Angel/0000-0001-9047-3992; Kotula, Paul/0000-0002-7521-2759; Leitner, Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X; Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943 FU NASA [NNH11AQ61I, NNX09AC36G]; NASA Origins of Solar Systems Program; Tawani Foundation; DFG [SPP1385]; Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231]; U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-98CH10886] FX We thank Fred Horz and Martin Lee for constructive reviews. RMS, HCG, and NDB were supported by NASA grant NNH11AQ61I. JW. ALB, ZG, RL, DZ, WM, and JVK were supported by NASA grant NNX09AC36G. SAS acknowledges support from the NASA Origins of Solar Systems Program. PRH, AA, BH were supported by the Tawani Foundation. PH and JL acknowledge support by DFG through SPP1385: the first ten million years of the solar system-a planetary materials approach. The Advanced Light Source is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Use of the National Synchrotron Light Source, Brookhaven National Laboratory, was supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DE-AC02-98CH10886. NR 39 TC 9 Z9 9 U1 2 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 IS 9 SI SI BP 1698 EP 1719 DI 10.1111/maps.12136 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ6HT UT WOS:000342912100011 ER PT J AU Westphal, AJ Bechtel, HA Brenker, FE Butterworth, AL Flynn, G Frank, DR Gainsforth, Z Hillier, JK Postberg, F Simionovici, AS Sterken, VJ Stroud, RM Allen, C Anderson, D Ansari, A Bajt, S Bastien, RK Bassim, N Borg, J Bridges, J Brownlee, DE Burchell, M Burghammer, M Changela, H Cloetens, P Davis, AM Doll, R Floss, C Grun, E Heck, PR Hoppe, P Hudson, B Huth, J Hvide, B Kearsley, A King, AJ Lai, B Leitner, J Lemelle, L Leroux, H Leonard, A Lettieri, R Marchant, W Nittler, LR Ogliore, R Ong, WJ Price, MC Sandford, SA Tresseras, JAS Schmitz, S Schoonjans, T Silversmit, G Sole, VA Srama, R Stadermann, F Stephan, T Stodolna, J Sutton, S Trieloff, M Tsou, P Tsuchiyama, A Tyliszczak, T Vekemans, B Vincze, L Von Korff, J Wordsworth, N Zevin, D Zolensky, ME AF Westphal, Andrew J. Bechtel, Hans A. Brenker, Frank E. Butterworth, Anna L. Flynn, George Frank, David R. Gainsforth, Zack Hillier, Jon K. Postberg, Frank Simionovici, Alexandre S. Sterken, Veerle J. Stroud, Rhonda M. Allen, Carlton Anderson, David Ansari, Asna Bajt, Sasa Bastien, Ron K. Bassim, Nabil Borg, Janet Bridges, John Brownlee, Donald E. Burchell, Mark Burghammer, Manfred Changela, Hitesh Cloetens, Peter Davis, Andrew M. Doll, Ryan Floss, Christine Gruen, Eberhard Heck, Philipp R. Hoppe, Peter Hudson, Bruce Huth, Joachim Hvide, Brit Kearsley, Anton King, Ashley J. Lai, Barry Leitner, Jan Lemelle, Laurence Leroux, Hugues Leonard, Ariel Lettieri, Robert Marchant, William Nittler, Larry R. Ogliore, Ryan Ong, Wei Ja Price, Mark C. Sandford, Scott A. Tresseras, Juan-Angel Sans Schmitz, Sylvia Schoonjans, Tom Silversmit, Geert Sole, Vicente A. Srama, Ralf Stadermann, Frank Stephan, Thomas Stodolna, Julien Sutton, Steven Trieloff, Mario Tsou, Peter Tsuchiyama, Akira Tyliszczak, Tolek Vekemans, Bart Vincze, Laszlo Von Korff, Joshua Wordsworth, Naomi Zevin, Daniel Zolensky, Michael E. TI Final reports of the Stardust Interstellar Preliminary Examination SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ULYSSES DUST DATA AB With the discovery of bona fide extraterrestrial materials in the Stardust Interstellar Dust Collector, NASA now has a fundamentally new returned sample collection, after the Apollo, Antarctic meteorite, Cosmic Dust, Genesis, Stardust Cometary, Hayabusa, and Exposed Space Hardware samples. Here, and in companion papers in this volume, we present the results from the Preliminary Examination of this collection, the Stardust Interstellar Preliminary Examination (ISPE). We found extraterrestrial materials in two tracks in aerogel whose trajectories and morphology are consistent with an origin in the interstellar dust stream, and in residues in four impacts in the aluminum foil collectors. While the preponderance of evidence, described in detail in companion papers in this volume, points toward an interstellar origin for some of these particles, alternative origins have not yet been eliminated, and definitive tests through isotopic analyses were not allowed under the terms of the ISPE. In this summary, we answer the central questions of the ISPE: How many tracks in the collector are consistent in their morphology and trajectory with interstellar particles? How many of these potential tracks are consistent with real interstellar particles, based on chemical analysis? Conversely, what fraction of candidates are consistent with either a secondary or interplanetary origin? What is the mass distribution of these particles, and what is their state? Are they particulate or diffuse? Is there any crystalline material? How many detectable impact craters (> 100 nm) are there in the foils, and what is their size distribution? How many of these craters have analyzable residue that is consistent with extraterrestrial material? And finally, can craters from secondaries be recognized through crater morphology (e.g., ellipticity)? C1 [Westphal, Andrew J.; Butterworth, Anna L.; Gainsforth, Zack; Anderson, David; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA. [Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany. [Flynn, George] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA. [Frank, David R.; Bastien, Ron K.] NASA JSC, ESCG, Houston, TX USA. [Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany. [Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France. [Sterken, Veerle J.] Univ Stuttgart, IRS, D-70174 Stuttgart, Germany. [Sterken, Veerle J.] Tech Univ Carolo Wilhelmina Braunschweig, IGEP, D-38106 Braunschweig, Germany. [Sterken, Veerle J.; Zolensky, Michael E.] MPIK, Heidelberg, Germany. [Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA. [Allen, Carlton] NASA JSC, ARES, Houston, TX USA. [Ansari, Asna; Hvide, Brit] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Bajt, Sasa] DESY, Hamburg, Germany. [Bassim, Nabil] Naval Res Lab, Nanoscale Mat Sect, Washington, DC USA. [Borg, Janet] IAS Orsay, Orsay, France. [Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England. [Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury, Kent, England. [Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France. [Changela, Hitesh] George Washington Univ, Washington, DC USA. [Davis, Andrew M.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA. [Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja; Stadermann, Frank] Washington Univ, St Louis, MO USA. [Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Heck, Philipp R.] Field Museum Nat Hist, Chicago, IL 60605 USA. [Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany. [Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England. [King, Ashley J.] Univ Chicago, Chicago, IL 60637 USA. [King, Ashley J.] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA. [Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France. [Leroux, Hugues] Univ Lille 1, Lille, France. [Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA. [Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium. [Srama, Ralf] Univ Stuttgart, IRS, D-70174 Stuttgart, Germany. [Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Tsuchiyama, Akira] Osaka Univ, Osaka, Japan. RP Westphal, AJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM westphal@ssl.berkeley.edu RI Sans Tresserras, Juan Angel/J-9362-2014; Bajt, Sasa/G-2228-2010; Stroud, Rhonda/C-5503-2008; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015 OI Sans Tresserras, Juan Angel/0000-0001-9047-3992; Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943; Leitner, Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X NR 25 TC 12 Z9 12 U1 3 U2 20 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 IS 9 SI SI BP 1720 EP 1733 DI 10.1111/maps.12221 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ6HT UT WOS:000342912100012 ER PT J AU Nichols, JE Peteet, DM Moy, CM Castaneda, IS McGeachy, A Perez, M AF Nichols, Jonathan E. Peteet, Dorothy M. Moy, Christopher M. Castaneda, Isla S. McGeachy, Alicia Perez, Max TI Impacts of climate and vegetation change on carbon accumulation in a south-central Alaskan peatland assessed with novel organic geochemical techniques SO HOLOCENE LA English DT Article DE carbon cycle; organic geochemistry; paleoclimate; paleoecology; peatlands; stable isotopes ID DELTA-D VALUES; DIALKYL GLYCEROL TETRAETHERS; IONIZATION-MASS-SPECTROMETRY; N-ALKANES; METEORIC PRECIPITATION; ISOTOPIC COMPOSITION; NORTHERN MINNESOTA; OMBROTROPHIC PEAT; MEMBRANE-LIPIDS; WATER-CONTENT AB To constrain the effect of climate and peatland type on carbon accumulation, we reconstructed these parameters from a Holocene-length core of a Sphagnum-dominated peatland near Cordova, AK, USA. We determined peat type using a combination of peat texture and density, macrofossils, distributions of leaf-wax biomarkers, and soil pH reconstructions based on distributions of branched glycerol dialkyl glycerol tetraether lipids (brGDGTs). We produced an independent record of hydroclimate and temperature change using hydrogen isotope ratios of leaf-wax biomarkers and distributions of brGDGTs. Carbon accumulation rates were constrained with 14 AMS C-14 dates from identified macrofossils and ash-free bulk density. In the early Holocene, the site was a shallow pond with evidence for emergent macrophytes, Sphagnum, and algae growing in a warm, moist climate. At 9.2 kyr (1 kyr = 1000 cal. yr BP), the site became a Sphagnum-dominated bog. Under mid-Holocene warm, evaporative climate conditions, the site became sedge-dominated. As climate cooled and effective precipitation increased, Sphagnum was able to gain dominance abruptly at similar to 3.5 kyr. Large changes in the vegetation assemblage and hydrology and climate are contemporaneous with significant changes in the rate of carbon accumulation. Carbon accumulated most rapidly when Sphagnum dominated and effective moisture was high and most slowly when sedges were dominant and conditions were warmer and drier. Estimates of future climate change indicate warmer, more evaporative conditions that, in the past, favored a sedge-dominated environment, suggesting that this peatland and those similar can contribute to a positive feedback to warming by transitioning to less efficient carbon sinks. C1 [Nichols, Jonathan E.; Peteet, Dorothy M.] Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Peteet, Dorothy M.] NASA, Goddard Inst Space Studies, Houston, TX USA. [Moy, Christopher M.] Univ Otago, Dunedin, New Zealand. [Castaneda, Isla S.] Univ Massachusetts, Amherst, MA 01003 USA. [McGeachy, Alicia] Spelman Coll, Atlanta, GA USA. [McGeachy, Alicia] Northwestern Univ, Evanston, IL 60208 USA. [Perez, Max] SUNY Binghamton, Binghamton, NY 13902 USA. RP Nichols, JE (reprint author), Lamont Doherty Earth Observ, 101D Paleomagnetics,61 Route 9W, Palisades, NY 10964 USA. EM jnichols@ldeo.columbia.edu FU US National Science Foundation [ARC-1022979]; Climate Center of the Lamont-Doherty Earth Observatory; NASA Postdoctoral Program; US Geological Survey Mendenhall Postdoctoral Fellowship FX This work is supported by the US National Science Foundation ARC-1022979 and by the Climate Center of the Lamont-Doherty Earth Observatory. JEN and CMM also gratefully acknowledge support from the NASA Postdoctoral Program and the US Geological Survey Mendenhall Postdoctoral Fellowship, respectively. NR 52 TC 6 Z9 7 U1 3 U2 41 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0959-6836 EI 1477-0911 J9 HOLOCENE JI Holocene PD SEP PY 2014 VL 24 IS 9 SI SI BP 1146 EP 1155 DI 10.1177/0959683614540729 PG 10 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA AQ1XO UT WOS:000342578200012 ER PT J AU De Witt, JK Edwards, WB Scott-Pandorf, MM Norcross, JR Gernhardt, ML AF De Witt, John K. Edwards, W. Brent Scott-Pandorf, Melissa M. Norcross, Jason R. Gernhardt, Michael L. TI The preferred walk to run transition speed in actual lunar gravity SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE Biomechanics; Locomotion; Preferred transition speed; Microgravity; Froude number ID DYNAMIC SIMILARITY HYPOTHESIS; REDUCED GRAVITY; HUMAN LOCOMOTION AB Quantifying the preferred transition speed (PTS) from walking to running has provided insight into the underlying mechanics of locomotion. The dynamic similarity hypothesis suggests that the PTS should occur at the same Froude number across gravitational environments. In normal Earth gravity, the PTS occurs at a Froude number of 0.5 in adult humans, but previous reports found the PTS occurred at Froude numbers greater than 0.5 in simulated lunar gravity. Our purpose was to (1) determine the Froude number at the PTS in actual lunar gravity during parabolic flight and (2) compare it with the Froude number at the PTS in simulated lunar gravity during overhead suspension. We observed that Froude numbers at the PTS in actual lunar gravity (1.39 +/- 0.45) and simulated lunar gravity (1.11 +/- 0.26) were much greater than 0.5. Froude numbers at the PTS above 1.0 suggest that the use of the inverted pendulum model may not necessarily be valid in actual lunar gravity and that earlier findings in simulated reduced gravity are more accurate than previously thought. C1 [De Witt, John K.; Scott-Pandorf, Melissa M.; Norcross, Jason R.] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. [Edwards, W. Brent] Univ Calgary, Calgary, AB T2N 1N4, Canada. [Gernhardt, Michael L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP De Witt, JK (reprint author), Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. EM john.k.dewitt@nasa.gov FU Human Health and Countermeasures Element of the National Aeronautics and Space Administration's Human Research Program FX This work was a directed study funded by the Human Health and Countermeasures Element of the National Aeronautics and Space Administration's Human Research Program. NR 12 TC 6 Z9 6 U1 2 U2 9 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 EI 1477-9145 J9 J EXP BIOL JI J. Exp. Biol. PD SEP PY 2014 VL 217 IS 18 BP 3200 EP 3203 DI 10.1242/jeb.105684 PG 4 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AQ0XN UT WOS:000342506100009 PM 25232195 ER PT J AU Lopez, RA Moya, PS Munoz, V Vinas, AF Valdivia, JA AF Lopez, Rodrigo A. Moya, Pablo S. Munoz, Victor Vinas, Adolfo F. Alejandro Valdivia, J. TI Kinetic transverse dispersion relation for relativistic magnetized electron-positron plasmas with Maxwell-Juttner velocity distribution functions SO PHYSICS OF PLASMAS LA English DT Article ID POLARIZED ELECTROMAGNETIC-WAVES; HOT ACCRETION DISKS; PARAMETRIC DECAYS AB We use a kinetic treatment to study the linear transverse dispersion relation for a magnetized isotropic relativistic electron-positron plasma with finite relativistic temperature. The explicit linear dispersion relation for electromagnetic waves propagating along a constant background magnetic field is presented, including an analytical continuation to the whole complex frequency plane for the case of Maxwell-Juttner velocity distribution functions. This dispersion relation is studied numerically for various temperatures. For left-handed solutions, the system presents two branches, the electromagnetic ordinary mode and the Alfven mode. In the low frequency regime, the Alfven branch has two dispersive zones, the normal zone (where partial derivative omega/partial derivative k > 0) and an anomalous zone (where partial derivative x/partial derivative k < 0). We find that in the anomalous zone of the Alfven branch, the electromagnetic waves are damped, and there is a maximum wave number for which the Alfven branch is suppressed. We also study the dependence of the Alfven velocity and effective plasma frequency with the temperature. We complemented the analytical and numerical approaches with relativistic full particle simulations, which consistently agree with the analytical results. (C) 2014 AIP Publishing LLC. C1 [Lopez, Rodrigo A.] Univ Concepcion, Dept Fis, Fac Ciencias Fis & Matemat, Concepcion, Chile. [Moya, Pablo S.; Vinas, Adolfo F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Moya, Pablo S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Munoz, Victor; Alejandro Valdivia, J.] Univ Chile, Fac Ciencias, Dept Fis, Santiago, Chile. [Alejandro Valdivia, J.] CEDENNA, Ctr Desarrollo Nanociencia & Nanotecnol, Santiago, Chile. RP Lopez, RA (reprint author), Univ Concepcion, Dept Fis, Fac Ciencias Fis & Matemat, Concepcion, Chile. RI Moya, Pablo/C-3163-2011; Lopez, Rodrigo/H-7576-2013; Valdivia, Juan/A-3631-2008; Munoz, Victor/A-2255-2008 OI Moya, Pablo/0000-0002-9161-0888; Valdivia, Juan/0000-0003-3381-9904; FU CONICyT through FONDECyT Grant [1110135, 1110729, 1121144, 3140142]; CONICyT-Becas Chile; CEDENNA; NASA-Wind/SWE project FX The authors thank Roberto Navarro for useful discussions. Also, we thank the support of CONICyT through FONDECyT Grant Nos. 1110135 and 1110729 (J.A.V.); No. 1121144 (V.M.) and Postdoctoral Grant No. 3140142. (R.A.L.) We also thank the CONICyT-Becas Chile program by providing financial support for postdoctoral fellow (P.S.M.). We also thank financial support from CEDENNA. A.F.V. would like to thank the NASA-Wind/SWE project for their support. NR 30 TC 6 Z9 6 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD SEP PY 2014 VL 21 IS 9 AR 092107 DI 10.1063/1.4894679 PG 10 WC Physics, Fluids & Plasmas SC Physics GA AQ4JC UT WOS:000342760900014 ER PT J AU Navarro, RE Araneda, J Munoz, V Moya, PS F-Vinas, A Valdivia, JA AF Navarro, Roberto E. Araneda, Jaime Munoz, Victor Moya, Pablo S. F-Vinas, Adolfo Valdivia, Juan A. TI Theory of electromagnetic fluctuations for magnetized multi-species plasmas SO PHYSICS OF PLASMAS LA English DT Article ID PROTON TEMPERATURE ANISOTROPY; QUASI-THERMAL FLUCTUATIONS; SOLAR-WIND; VELOCITY DISTRIBUTIONS; SPACE PLASMAS; IONS; INSTABILITIES; CONSTRAINT; STREAMS; 0.3-AU AB Analysis of electromagnetic fluctuations in plasma provides relevant information about the plasma state and its macroscopic properties. In particular, the solar wind persistently sustains a small but detectable level of magnetic fluctuation power even near thermal equilibrium. These fluctuations may be related to spontaneous electromagnetic fluctuations arising from the discreteness of charged particles. Here, we derive general expressions for the plasma fluctuations in a multi-species plasma following arbitrary distribution functions. This formalism, which generalizes and includes previous works on the subject, is then applied to the generation of electromagnetic fluctuations propagating along a background magnetic field in a plasma of two proton populations described by drifting bi-Maxwellians. (C) 2014 AIP Publishing LLC. C1 [Navarro, Roberto E.; Munoz, Victor; Valdivia, Juan A.] Univ Chile, Fac Ciencias, Dept Fis, Santiago, Chile. [Araneda, Jaime] Univ Concepcion, Dept Fis, Concepcion 4070386, Chile. [Moya, Pablo S.; F-Vinas, Adolfo] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Moya, Pablo S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Valdivia, Juan A.] CEIBA Complejidad, Ctr Estudios Interdisciplinarios Basicos & Aplica, Bogota, Colombia. RP Navarro, RE (reprint author), Univ Chile, Fac Ciencias, Dept Fis, Casilla 653, Santiago, Chile. EM roberto.navarro@ug.uchile.cl RI Moya, Pablo/C-3163-2011; Valdivia, Juan/A-3631-2008; Navarro, Roberto/F-7045-2014; Araneda, Jaime/J-9245-2015; Munoz, Victor/A-2255-2008 OI Moya, Pablo/0000-0002-9161-0888; Valdivia, Juan/0000-0003-3381-9904; Navarro, Roberto/0000-0003-0782-1904; FU FONDECyT [1110135, 1110729, 1130273, 1121144, 1110880]; CONICYT-Becas Chile; CONICyT [21100691]; CEDENNA; NASA's Wind/SWE program FX This project has been financially supported by FONDECyT under contract Nos. 1110135 (J.A.V.), 1110729 (J.A.V.), 1130273 (J.A.V.), 1121144 (V. M.), and 1110880 (J.A). P.S.M thanks a Postdoctoral Fellowship from CONICYT-Becas Chile. R.N. thanks a doctoral fellowship from CONICyT No. 21100691. J.A.V. also thanks to CEDENNA and A.F.V. thanks to NASA's Wind/SWE program for their support. NR 48 TC 11 Z9 11 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD SEP PY 2014 VL 21 IS 9 AR 092902 DI 10.1063/1.4894700 PG 7 WC Physics, Fluids & Plasmas SC Physics GA AQ4JC UT WOS:000342760900069 ER PT J AU Govindarajan, N de Visser, CC Krishnakumar, K AF Govindarajan, Nithin de Visser, Cornelis. C. Krishnakumar, Kalmanje TI A sparse collocation method for solving time-dependent HJB equations using multivariate B-splines SO AUTOMATICA LA English DT Article DE Optimal feedback control; Hamilton-Jacobi-Bellman equation; Adaptive dynamic programming; Splines; Collocation method ID JACOBI-BELLMAN EQUATIONS; NUMERICAL-SOLUTION; NONLINEAR-SYSTEMS AB This paper presents a sparse collocation method for solving the time-dependent Hamilton-Jacobi-Bellman (HJB) equation associated with the continuous-time optimal control problem on a fixed, finite time-horizon with integral cost functional. Through casting the problem in a recursive framework using the value-iteration procedure, the value functions of every iteration step is approximated with a time-varying multivariate simplex B-spline on a certain state domain of interest. In the collocation scheme, the time-dependent coefficients of the spline function are further approximated with ordinary univariate B-splines to yield a discretization for the value function fully in terms of piece-wise polynomials. The B-spline coefficients are determined by solving a sequence of highly sparse quadratic programming problems. The proposed algorithm is demonstrated on a pair of benchmark example problems. Simulation results indicate that the method can yield increasingly more accurate approximations of the value function by refinement of the triangulation. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Govindarajan, Nithin] Delft Univ Technol, Fac Mech Maritime & Mat Engn, Delft Ctr Syst & Control, NL-2628 CD Delft, Netherlands. [de Visser, Cornelis. C.] Delft Univ Technol, Fac Aerosp Engn, Control & Simulat Div, NL-2600 GB Delft, Netherlands. [Krishnakumar, Kalmanje] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. RP Govindarajan, N (reprint author), Delft Univ Technol, Fac Mech Maritime & Mat Engn, Delft Ctr Syst & Control, NL-2628 CD Delft, Netherlands. EM N.Govindarajan@student.tudelft.nl; C.C.deVisser@tudelft.nl; k.krishnakumar@nasa.gov NR 31 TC 1 Z9 1 U1 0 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0005-1098 EI 1873-2836 J9 AUTOMATICA JI Automatica PD SEP PY 2014 VL 50 IS 9 BP 2234 EP 2244 DI 10.1016/j.automatica.2014.07.012 PG 11 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA AQ0NG UT WOS:000342479400003 ER PT J AU Lee, HH Piner, KR Hinton, MG Chang, YJ Kimoto, A Kanaiwa, M Su, NJ Walsh, W Sun, CL DiNardo, G AF Lee, Hui-Hua Piner, Kevin R. Hinton, Michael G. Chang, Yi-Jay Kimoto, Ai Kanaiwa, Minoru Su, Nan-Jay Walsh, William Sun, Chi-Lu DiNardo, Gerard TI Sex-structured population dynamics of blue marlin Makaira nigricans in the Pacific Ocean SO FISHERIES SCIENCE LA English DT Article DE Sexual dimorphism; Sex structure; Age structure; Selectivity; Pacific Ocean; Blue marlin ID STOCK ASSESSMENT MODELS; ISTIOPHORID BILLFISHES; FISHERIES; GROWTH; AGE AB The population dynamics of the blue marlin Makaira nigricans stock in the Pacific Ocean were estimated for 1971-2011 using a fully integrated length-based, age-, and sex-structured model. Fishery-specific catch, size composition, and catch-per-unit of effort were used in the modeling as likelihood components. Estimated dynamics were consistent with a stock that is fully exploited and stable over the last several years. No significant trends in recruitment were noted; however, female blue marlin were estimated to make up a majority of the catch, and historical exploitation has disproportionately changed the age structure of females relative to males. This result is due to differences in assumed life history and estimated selectivity. Changes to important life history parameters that are responsible for the productivity of the stock would potentially change the interpretation of current stock status. C1 [Lee, Hui-Hua; Chang, Yi-Jay; Walsh, William] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96818 USA. [Piner, Kevin R.] NOAA, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla, CA 92037 USA. [Hinton, Michael G.] Interamer Trop Tuna Commiss, La Jolla, CA 92037 USA. [Kimoto, Ai] Natl Res Inst Far Seas Fisheries, Shimizu, Shizuoka 4248633, Japan. [Kanaiwa, Minoru] Tokyo Univ Agr, Abashiri, Hokkaido 0992493, Japan. [Su, Nan-Jay; Sun, Chi-Lu] Natl Taiwan Univ, Inst Oceanog, Taipei 106, Taiwan. [DiNardo, Gerard] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96818 USA. RP Lee, HH (reprint author), Univ Hawaii, Joint Inst Marine & Atmospher Res, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA. EM huihua.lee@noaa.gov; kevin.piner@noaa.gov; mhinton@iattc.org; aikimoto@affrc.go.jp; m3kanaiw@bioindustry.nodai.ac.jp; chilu@ntu.edu.tw; gerard.dinardo@noaa.gov OI Chang, Yi-Jay/0000-0002-7472-4672 NR 26 TC 3 Z9 3 U1 0 U2 8 PU SPRINGER JAPAN KK PI TOKYO PA CHIYODA FIRST BLDG EAST, 3-8-1 NISHI-KANDA, CHIYODA-KU, TOKYO, 101-0065, JAPAN SN 0919-9268 EI 1444-2906 J9 FISHERIES SCI JI Fish. Sci. PD SEP PY 2014 VL 80 IS 5 BP 869 EP 878 DI 10.1007/s12562-014-0762-6 PG 10 WC Fisheries SC Fisheries GA AP6XC UT WOS:000342220700001 ER PT J AU Kelsey, CR Scott, J Lane, A Schwitzer, E West, M Thomas, S Herndon, J Michalski, M Horwitz, M Hennig, T Jones, L AF Kelsey, C. R. Scott, J. Lane, A. Schwitzer, E. West, M. Thomas, S. Herndon, J. Michalski, M. Horwitz, M. Hennig, T. Jones, L. TI Cardiopulmonary Exercise Testing Prior to Myeloablative Allogeneic Stem Cell Transplantation Using Total Body Irradiation: A Feasibility Study SO INTERNATIONAL JOURNAL OF RADIATION ONCOLOGY BIOLOGY PHYSICS LA English DT Meeting Abstract CT 56th Annual Meeting of the American-Society-for-Radiation-Oncology CY SEP 14-17, 2014 CL San Francisco, CA SP Amer Soc Radiat Oncol C1 [Kelsey, C. R.; Lane, A.; Schwitzer, E.; West, M.; Thomas, S.; Herndon, J.; Michalski, M.; Horwitz, M.; Hennig, T.; Jones, L.] Duke Univ, Durham, NC USA. [Scott, J.] NASA, Houston, TX USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0360-3016 EI 1879-355X J9 INT J RADIAT ONCOL JI Int. J. Radiat. Oncol. Biol. Phys. PD SEP 1 PY 2014 VL 90 SU 1 MA 3195 BP S681 EP S681 PG 1 WC Oncology; Radiology, Nuclear Medicine & Medical Imaging SC Oncology; Radiology, Nuclear Medicine & Medical Imaging GA AP8LV UT WOS:000342331402410 ER PT J AU Ditty, JG AF Ditty, James G. TI STERNAL SPINES IN PENAEID POSTLARVAE (DECAPODA: PENAEIDAE): LIFE-PHASE-SPECIFIC AND SYSTEMATICALLY SIGNIFICANT? SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article DE developmental plasticity; Parapenaeus; penaeid diversity; sternal plate shape; sternal spine patterns ID SHRIMP FARFANTEPENAEUS-DUORARUM; EARLY DEVELOPMENTAL-STAGES; INDIAN-OCEAN EXPEDITION; INDO-WEST PACIFIC; GULF-OF-MEXICO; LARVAL DEVELOPMENT; GENUS PENAEUS; CRUSTACEA DECAPODA; RATHBUN DECAPODA; TAXONOMIC VALUE AB Our ability to identify and discriminate postlarvae of penaeids below family level remains poor due to phase brevity and a lack of taxonomic characters. Whether sternal spines are unique and taxonomically significant to postlarvae has not been resolved. I describe number and placement of spines in Parapenaeus sp. Smith, 1885, and a specimen tentatively identified as Xiphopenaeus kroyeri (Heller, 1862) from the Gulf of Mexico; review information for penaeids worldwide; and evaluate the significance of sternal spines as a life-phase specific taxonomic character and to penaeid systematics. To date, sternal spines have been described for 14 of 32 genera and 26 species. Most taxa share one of two common sternal formulas: either 0 + 0 + 0 + 1 + 0, or 0 + 0 + 0 + 1 + 1. Only Metapenaeopsis Bouvier, 1905, and the tentative Xiphopenaeus kroyeri have a pair of spines on at least the first-two sternal plates, and only Metapenaeopsis and Litopenaeus Perez-Farfante, 1969, contain members with different sternal formulas. I suggest that differences among taxa in shape of the sternal plates may be an unrecognized taxonomic character. Sternal spines are not life-phase specific and do not reflect lower-level systematic relationships within Penaeidae regardless of generic nomenclature applied. The unusual length, shape, and reverse orientation of the spine on plate five in species of Parapenaeus, and presence of an elongate ventromedian spine on one or more pleomeres in Parapenaeus and Funchalia Johnson, 1868, supports molecular and morphological data that Penaeidae may be paraphyletic. While generally ineffective as a stand-alone taxonomic character, differences in number, placement, and orientation of sternal spines, i.e., the 'sternal pattern'; knowledge of geographic distributions; and, perhaps differences in sternal plate shape should be included in the suite of characters used to discriminate and identify penaeids during the postlarva phase. C1 Natl Marine Fisheries Serv, Natl Oceanog & Atmospher Adm, Galveston, TX 77551 USA. RP Ditty, JG (reprint author), Natl Marine Fisheries Serv, Natl Oceanog & Atmospher Adm, 4700 Ave U, Galveston, TX 77551 USA. EM Jim.Ditty@NOAA.gov FU NOAA's Southeast Fisheries Science Center FX Thanks to Dr. Antonina dos Santos, Instituto Portugues do Mar e da Atmosfera, Lisbon, Portugal, for providing a postlarva of Melicertus kerathurus collected off Portugal, and to Carley Knight, University of Southern Mississippi and NOAA's Pascagoula Laboratory for myses and postlarvae of Parapenaeus sp. from the Gulf of Mexico. Thanks to Dr. Geoffrey Matthews (retired), formerly of NOAA's Galveston Laboratory, and to Shawn Hillen and Juan Salas of NOAA's Galveston Laboratory who participated in sample collection, and to NOAA's Southeast Fisheries Science Center for funding support Thanks also to Juan Salas for illustrating the sternal pattern for Litopenaeus setiferus, Fatfantepenaeus aztecus, Melicertus kerathurus, Parapenaeus sp. and tentative Xiphopenaeus kroyeri. Images were reproduced by kind permission of the publishers through Rightslink (R): CSIRO Publishing (Marine and Freshwater Research); Oxford University Press (Journal of Plankton Research); Springer (Hydrobiologia) with permission from Springer Science + Business Media; and courtesy of NOAA Fisheries (Fishery Bulletin). Views and opinions expressed here are those of the author and do not necessarily reflect those of NOAA Fisheries. NR 120 TC 0 Z9 0 U1 1 U2 8 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 EI 1937-240X J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD SEP PY 2014 VL 34 IS 5 BP 618 EP 628 DI 10.1163/1937240X-00002261 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AP9IH UT WOS:000342393000010 ER PT J AU Carpenter, JR Markley, FL AF Carpenter, J. Russell Markley, F. Landis TI Wald Sequential Probability Ratio Test for Space Object Conjunction Assessment SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID SATELLITE COLLISION PROBABILITY; AVOIDANCE MANEUVER DECISIONS; ORBIT UNCERTAINTY; TERM ENCOUNTERS; PROPAGATION; RISK AB This paper shows how satellite owners/operators may use sequential estimates of collision probability, along with a prior assessment of the base risk of collision, in a compound hypothesis ratio test to inform decisions concerning collision risk mitigation maneuvers. The compound hypothesis test reduces to a simple probability ratio test, which appears to be a novel result. The test satisfies tolerances related to targeted false alarm and missed detection rates. This result is independent of the method one uses to compute the probability density that one integrates to compute collision probability. A well-established test case from the literature shows that this test yields acceptable results within the constraints of a typical operational conjunction assessment decision timeline. Another example illustrates the use of the test in a practical conjunction assessment scenario based on operations of the International Space Station. C1 [Carpenter, J. Russell] NASA, Goddard Space Flight Ctr, Nav & Mission Design Branch, Greenbelt, MD 20771 USA. [Markley, F. Landis] NASA, Goddard Space Flight Ctr, Attitude Control Syst Engn Branch, Greenbelt, MD 20771 USA. RP Carpenter, JR (reprint author), NASA, Goddard Space Flight Ctr, Nav & Mission Design Branch, Code 595, Greenbelt, MD 20771 USA. NR 33 TC 0 Z9 0 U1 1 U2 4 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD SEP-OCT PY 2014 VL 37 IS 5 BP 1385 EP 1396 DI 10.2514/1.G000478 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA AP7FS UT WOS:000342243800001 ER PT J AU Heath, CM AF Heath, Christopher M. TI Characterization of Swirl-Venturi Lean Direct Injection Designs for Aviation Gas Turbine Combustion SO JOURNAL OF PROPULSION AND POWER LA English DT Article AB Injector geometry, physical mixing, chemical processes, and engine cycle conditions together govern performance, operability, and emission characteristics of aviation gas turbine combustion systems. The present investigation explores swirl-venturi lean direct injection combustor fundamentals, characterizing the influence of key geometric injector parameters on reacting flow physics and emission production trends. In this computational study, a design space exploration was performed using a parameterized swirl-venturi lean direct injector model. From the parametric geometry, 20 three-element lean direct injection combustor sectors were produced and simulated using steady-state Reynolds-averaged Navier-Stokes reacting computations. Species concentrations were solved directly using a reduced 18-step reaction mechanism for Jet A. Turbulence closure was obtained using a nonlinear kappa-epsilon model. Results demonstrate sensitivities of the geometric perturbations on axially averaged flowfield responses. Output variables include axial velocity, turbulent kinetic energy, static temperature, fuel patternation, and minor species mass fractions. Significant trends have been reduced to surrogate model approximations, intended to guide future injector design trade studies and advance aviation gas turbine combustion research. C1 NASA, John H Glenn Res Ctr Lewis Field, Multidisciplinary Design Anal & Optimizat Branch, Cleveland, OH 44135 USA. RP Heath, CM (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Multidisciplinary Design Anal & Optimizat Branch, MS 5-10, Cleveland, OH 44135 USA. FU Supersonics and Fixed Wing Projects of the NASA Fundamental Aeronautics Program FX The author gratefully acknowledges the support of the Supersonics and Fixed Wing Projects of the NASA Fundamental Aeronautics Program. Also, a special thanks to Jonathan Seidel for providing the inspiration for this research; Jeffrey Moder for the numerous enhancements made to the National Combustion Code; and the NASA OpenMDAO development team, especially Justin Gray, for providing software integration assistance. NR 30 TC 1 Z9 1 U1 3 U2 13 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 EI 1533-3876 J9 J PROPUL POWER JI J. Propul. Power PD SEP-OCT PY 2014 VL 30 IS 5 BP 1334 EP 1356 DI 10.2514/1.B35077 PG 23 WC Engineering, Aerospace SC Engineering GA AQ1HG UT WOS:000342531900021 ER PT J AU Agee, CB Muttik, N Ziegler, K Walton, EL Herd, CDK McCubbin, FM Santos, AR Burger, PV Simon, JI Peters, TJ Tappa, MJ Sanborn, ME Yin, QZ AF Agee, C. B. Muttik, N. Ziegler, K. Walton, E. L. Herd, C. D. K. McCubbin, F. M. Santos, A. R. Burger, P. V. Simon, J. I. Peters, T. J. Tappa, M. J. Sanborn, M. E. Yin, Q-Z. TI NEW METEORITE TYPE NWA 8159 AUGITE BASALT: SPECIMEN FROM A PREVIOUSLY UNSAMPLED LOCATION ON MARS? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Agee, C. B.; Muttik, N.; Ziegler, K.; McCubbin, F. M.; Santos, A. R.; Burger, P. V.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Agee, C. B.; Muttik, N.; Ziegler, K.; McCubbin, F. M.; Santos, A. R.; Burger, P. V.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Walton, E. L.; Herd, C. D. K.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2M7, Canada. [Simon, J. I.; Peters, T. J.; Tappa, M. J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Peters, T. J.] LPI, Houston, TX USA. [Tappa, M. J.] JETS Jacobs Technol, Houston, TX USA. [Sanborn, M. E.; Yin, Q-Z.] Univ Calif Davis, Dept Earth & Planetary Sci, Sacramento, CA USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A11 EP A11 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200008 ER PT J AU Bishop, JL Tirsch, D AF Bishop, J. L. Tirsch, D. TI VNIR SPECTRAL PROPERTIES OF MARTIAN METEORITES AND COMPARISON WITH CRISM SPECTRA OF MARS IN THE ISIDIS BASIN REGION SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Bishop, J. L.] SETI Inst, Carl Sagan Ctr, Mountain View, CA USA. [Bishop, J. L.] NASA Ames, Mountain View, CA USA. [Tirsch, D.] German Aerosp Ctr DLR, Inst Planetary Res, Berlin, Germany. EM jbishop@seti.org NR 4 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A42 EP A42 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200039 ER PT J AU Blumenfeld, EH Evans, CA Oshel, ER Liddle, DA Beaulieu, K Zeigler, RA Righter, K Hanna, RD Ketcham, RA AF Blumenfeld, E. H. Evans, C. A. Oshel, E. R. Liddle, D. A. Beaulieu, K. Zeigler, R. A. Righter, K. Hanna, R. D. Ketcham, R. A. TI High-Resolution Imaged-Based 3D Reconstruction Combined with X-Ray CT Data Enables Comprehensive Non-Destructive Documentation and Targeted Research of Astromaterials SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Blumenfeld, E. H.] Hamad bin Khalifa Univ, UCL Qatar, Doha, Qatar. [Evans, C. A.; Zeigler, R. A.; Righter, K.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Oshel, E. R.; Liddle, D. A.; Beaulieu, K.] NASA, Lyndon B Johnson Space Ctr, JETS, Houston, TX 77058 USA. [Hanna, R. D.; Ketcham, R. A.] Univ Texas Austin, Jackson Sch Geosci, UTCT Facil, Austin, TX 78712 USA. EM e.blumenfeld.12@ucl.ac.uk RI Ketcham, Richard/B-5431-2011 OI Ketcham, Richard/0000-0002-2748-0409 NR 3 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A46 EP A46 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200043 ER PT J AU Bottke, WF Swindle, TD Marchi, S Scott, ERD Vokrouhlicky, D Weirich, JR AF Bottke, W. F. Swindle, T. D. Marchi, S. Scott, E. R. D. Vokrouhlicky, D. Weirich, J. R. TI USING METEORITES TO FIND THE AGE OF THE MOON-FORMING EVENT SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID GIANT IMPACT; EARTH C1 [Bottke, W. F.; Marchi, S.] SW Res Inst, Boulder, CO USA. [Bottke, W. F.; Swindle, T. D.; Marchi, S.] NASA, SSERVI, Washington, DC USA. [Swindle, T. D.] Univ Arizona, Tucson, AZ USA. [Scott, E. R. D.] Univ Hawaii, Honolulu, HI 96822 USA. [Vokrouhlicky, D.] Charles Univ Prague, Prague, Czech Republic. [Weirich, J. R.] Univ Western Ontario, London, ON, Canada. EM bottke@boulder.swri.edu NR 7 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A52 EP A52 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200049 ER PT J AU Bridges, JC Schwenzer, SP Leveille, R Westall, F Wiens, RC Mangold, N Bristow, T Edwards, P Berger, G AF Bridges, J. C. Schwenzer, S. P. Leveille, R. Westall, F. Wiens, R. C. Mangold, N. Bristow, T. Edwards, P. Berger, G. TI CLAY AND MAGNETITE FORMATION AT YELLOWKNIFE BAY, MARS. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Bridges, J. C.; Edwards, P.] Univ Leicester, Space Res Ctr, Leicester LE1 7RH, Leics, England. [Schwenzer, S. P.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. [Leveille, R.] McGill Univ, Montreal, PQ, Canada. [Westall, F.] CNRS, Ctr Biophys Mol, F-45071 Orleans, France. [Wiens, R. C.] Los Alamos Natl Lab, Los Alamos, NM 87544 USA. [Mangold, N.] Lab Planetol & Geodynam Nantes, Nantes, France. [Mangold, N.] Univ Nantes, F-44035 Nantes, France. [Bristow, T.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Berger, G.] IRAP Obs Midi Pyrenees, Toulouse, France. EM j.bridges@le.ac.uk RI BERGER, Gilles/F-7118-2016 NR 8 TC 0 Z9 0 U1 0 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A59 EP A59 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200056 ER PT J AU Chennaoui-Aoudjehane, H Larouci, N Jambon, A Mittlefehldt, DW AF Chennaoui-Aoudjehane, H. Larouci, N. Jambon, A. Mittlefehldt, D. W. TI A CLASSIFICATION TABLE FOR ACHONDRITES (2) SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Chennaoui-Aoudjehane, H.; Larouci, N.] Hassan II Univ Casablanca, Fac Sci, Casablanca, Morocco. [Jambon, A.] Univ Paris 06, ISTEP, F-75252 Paris, France. [Mittlefehldt, D. W.] NASA, Astromat Res Off, Johnson Space Ctr, Houston, TX USA. EM chennaoui_h@yahoo.fr NR 6 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A73 EP A73 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200070 ER PT J AU Clemett, SJ Nakamura-Messenger, K Messenger, S AF Clemett, S. J. Nakamura-Messenger, K. Messenger, S. TI MASS SPECTUM IMAGING OF ORGANICS INJECTED INTO STARDUST AEROGEL BY COMETARY IMPACTS. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Clemett, S. J.] ERC Inc JACOBS, Houston, TX 77023 USA. [Nakamura-Messenger, K.; Messenger, S.] NASA, A Robert M Walker Lab Space Sci, Johnson Space Ctr, Houston, TX 77058 USA. EM simon.j.clemett@nasa.gov NR 9 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A76 EP A76 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200073 ER PT J AU Day, JMD Corder, CA Dhaliwal, JK Liu, Y Taylor, LA AF Day, J. M. D. Corder, C. A. Dhaliwal, J. K. Liu, Y. Taylor, L. A. TI The Chelyabinsk fall highly siderophile element abundance and Os-187/Os-188 composition and comparison with ordinary and carbonaceous chondrites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Day, J. M. D.; Corder, C. A.; Dhaliwal, J. K.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Liu, Y.] CALTECH, JPL, Pasadena, CA 91109 USA. [Taylor, L. A.] Univ Tennessee, Plametary Geosci Inst, Knoxville, TN 37996 USA. EM jmdday@ucsd.edu NR 6 TC 0 Z9 0 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A91 EP A91 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200088 ER PT J AU Englert, P Bishop, JL Gibson, EK Patel, S Koeberl, C AF Englert, P. Bishop, J. L. Gibson, E. K. Patel, S. Koeberl, C. TI DON JUAN BASIN, WRIGHT VALLEY, ANTARCTICA: MODEL FOR SURFACE PROCESSES ON MARS. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Englert, P.] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Bishop, J. L.; Patel, S.] SETI Inst, Mountain View, CA USA. [Bishop, J. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gibson, E. K.] Johnson Space Flight Ctr, Houston, TX USA. [Patel, S.] San Jose State Univ, San Jose, CA 95192 USA. [Koeberl, C.] Univ Vienna, Vienna, Austria. EM penglert@hawaii.edu NR 6 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A110 EP A110 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200107 ER PT J AU Fries, M Steele, A AF Fries, M. Steele, A. TI TOWARDS A GENERAL EQUATION FOR THE SURVIVAL OF MICROBES TRANSFERRED BETWEEN SOLAR SYSTEM BODIES. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Fries, M.] NASA, ARES, Johnson Space Ctr, Houston, TX USA. [Steele, A.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. EM marc.d.fries@nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A123 EP A123 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200120 ER PT J AU Fries, M Matson, R Schaefer, J Fries, J Hankey, M Anderson, L AF Fries, Marc Matson, Robert Schaefer, Jacob Fries, Jeffrey Hankey, Mike Anderson, Lindsay TI WORLDWIDE WEATHER RADAR IMAGERY MAY ALLOW SUBSTANTIAL INCREASE IN METEORITE FALL RECOVERY. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Fries, Marc] NASA, ARES, Johnson Space Ctr, Houston, TX USA. [Matson, Robert] Leidos Inc, Reston, VA 20190 USA. [Fries, Jeffrey] USAF Weather Agcy, Weather Grp 1, Offutt AFB, NE 68113 USA. [Hankey, Mike] Amer Meteor Soc, Geneseo, NY 14454 USA. [Anderson, Lindsay] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. EM marc.d.fries@nasa.gov NR 3 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A124 EP A124 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200121 ER PT J AU Hallis, LJ Huss, GR Nagashima, K Taylor, GJ Stoffler, D Smith, CL Lee, MR AF Hallis, L. J. Huss, G. R. Nagashima, K. Taylor, G. J. Stoeffler, D. Smith, C. L. Lee, M. R. TI D/H AND WATER SOURCES IN TISSINT. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Hallis, L. J.; Huss, G. R.; Taylor, G. J.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. [Hallis, L. J.; Huss, G. R.; Nagashima, K.; Taylor, G. J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Stoeffler, D.] Museum Nat Hist, Berlin, Germany. [Smith, C. L.] Nat Hist Museum, London, England. [Hallis, L. J.; Lee, M. R.] Univ Glasgow, Sch Geog & Earth Sci, Glasgow G12 8QQ, Lanark, Scotland. EM Lyd-ia.Hallis@glasgow.ac.uk NR 9 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A153 EP A153 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200150 ER PT J AU Han, JM Brearley, AJ Keller, LP AF Han, Jangmi Brearley, Adrian J. Keller, Lindsay P. TI MICROSTRUCTURES OF HIBONITE FROM AN ALH A77307 (CO3.0) CAI: EVIDENCE FOR EVAPORATIVE LOSS OF CALCIUM. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID METEORITES C1 [Han, Jangmi] LPI, Houston, TX 77058 USA. [Han, Jangmi; Keller, Lindsay P.] NASA, JSC, ARES, Robert M Walker Lab Space Sci, Houston, TX 77058 USA. [Brearley, Adrian J.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. EM jangmi.han@nasa.gov NR 6 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A155 EP A155 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200152 ER PT J AU Hanna, RD Zolensky, M Ketcham, RA Behr, WM Martinez, JE AF Hanna, R. D. Zolensky, M. Ketcham, R. A. Behr, W. M. Martinez, J. E. TI IMPACT-INDUCED CHONDRULE DEFORMATION AND AQUEOUS ALTERATION OF CM2 MURCHISON SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID CARBONACEOUS CHONDRITES C1 [Hanna, R. D.; Ketcham, R. A.; Behr, W. M.] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA. [Zolensky, M.] NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA. [Martinez, J. E.] NASA, Jacobs Technol, Johnson Space Ctr, Houston, TX 77058 USA. EM romy@jsg.utexas.edu RI Ketcham, Richard/B-5431-2011 OI Ketcham, Richard/0000-0002-2748-0409 NR 8 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A156 EP A156 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200153 ER PT J AU Hermalyn, B AF Hermalyn, B. TI EJECTA FROM TARGETS STRONG AND WEAK: EXPERIMENTAL MEASUREMENTS OF STRENGTH CONTROLLED AND STRENGTHLESS CRATERS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Hermalyn, B.] Univ Hawaii, NASA, ARC, Honolulu, HI 96822 USA. EM hermalyn@hawaii.edu NR 3 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A163 EP A163 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200160 ER PT J AU Jones, JH Franz, HB AF Jones, J. H. Franz, H. B. TI CORRELATIONS BETWEEN SURFICIAL SULFUR AND A CRUSTAL ASSIMILATION SIGNATURE IN MARTIAN SHERGOTTITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Jones, J. H.] NASA JSC, KR, Houston, TX 77058 USA. [Franz, H. B.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA. EM john.h.jones@nasa.gov NR 1 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A190 EP A190 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200187 ER PT J AU Kebukawa, Y Zolensky, ME Fries, M Kilcoyne, ALD Rahman, Z Cody, GD AF Kebukawa, Y. Zolensky, M. E. Fries, M. Kilcoyne, A. L. D. Rahman, Z. Cody, G. D. TI DIVERSITY IN C-XANES SPECTRA OBTAINED FROM CARBONACEOUS SOLID INCLUSIONS FROM MONAHANS HALITE. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Kebukawa, Y.] Yokohama Natl Univ, Fac Engn, Yokohama, Kanagawa, Japan. [Zolensky, M. E.; Fries, M.] NASA Johnson Space Ctr, Houston, TX USA. [Kilcoyne, A. L. D.] Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA USA. [Cody, G. D.] Carnegie Inst Sci, Geophys Lab, Washington, DC USA. EM kebukawa@ynu.ac.jp RI Kilcoyne, David/I-1465-2013 NR 3 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A199 EP A199 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200196 ER PT J AU Keller, LP Berger, EL AF Keller, L. P. Berger, E. L. TI SPACE WEATHERING OF OLIVINE IN LUNAR SOILS: A COMPARISON TO ITOKAWA REGOLITH SAMPLES. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Keller, L. P.] NASA JSC, Code KR, Houston, TX 77058 USA. [Berger, E. L.] NASA JSC, Jacobs JETS Contract, GeoControl Syst Inc, Houston, TX 77058 USA. EM Lindsay.P.Keller@nasa.gov NR 3 TC 0 Z9 0 U1 2 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A200 EP A200 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200197 ER PT J AU Keller, LP Needham, AW Messenger, S AF Keller, L. P. Needham, A. W. Messenger, S. TI A FIB/TEM/NANOSIMS STUDY OF A WARK-LOVERING RIM ON AN ALLENDE CAI. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Keller, L. P.; Messenger, S.] NASA JSC, Robert M Walker Lab Space Sci, Code KR, ARES, Houston, TX 77058 USA. [Needham, A. W.] LPI, Houston, TX 77058 USA. EM Lind-say.P.Keller@nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A201 EP A201 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200198 ER PT J AU Liu, Y Howarth, G Young, ED Pernet-Fisher, J Kohl, I Day, JMD Chen, Y Taylor, LA AF Liu, Y. Howarth, G. Young, E. D. Pernet-Fisher, J. Kohl, I. Day, J. M. D. Chen, Y. Taylor, L. A. TI New olivine-phyric shergottites, Larkman Nunatuks (LAR) 12011, 12095, 12240 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Liu, Y.; Chen, Y.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Howarth, G.; Pernet-Fisher, J.; Taylor, L. A.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. [Young, E. D.; Kohl, I.] Univ Calif Los Angeles, Dept Earth Planet & Space Sci, Los Angeles, CA 90095 USA. [Day, J. M. D.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. EM yangliu@jpl.nasa.gov NR 2 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A240 EP A240 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200237 ER PT J AU Ma, C Tschauner, O Beckett, JR Liu, Y Rossman, GR Zuravlev, K Prakapenka, V Dera, P Taylor, LA AF Ma, C. Tschauner, O. Beckett, J. R. Liu, Y. Rossman, G. R. Zuravlev, K. Prakapenka, V. Dera, P. Taylor, L. A. TI TISSINTITE, (Ca,Na,square)AlSi2O6: A SHOCK-INDUCED CLINOPYROXENE IN THE TISSINT METEORITE. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Ma, C.; Beckett, J. R.; Rossman, G. R.] CALTECH, Pasadena, CA 91125 USA. [Tschauner, O.] Univ Nevada, Las Vegas, NV 89154 USA. [Liu, Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zuravlev, K.; Prakapenka, V.] Argonne Natl Lab, Argonne, IL 60439 USA. [Dera, P.] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Taylor, L. A.] Univ Tennessee, Knoxville, TN 37996 USA. NR 4 TC 0 Z9 0 U1 2 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A249 EP A249 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200246 ER PT J AU Matsuno, J Miyake, A Tsuchiyama, A Nakamura-Messenger, K Messenger, S AF Matsuno, J. Miyake, A. Tsuchiyama, A. Nakamura-Messenger, K. Messenger, S. TI NANO-SCALE 3D OBSERVATION OF GEMS GRAINS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID ORIGINS C1 [Matsuno, J.; Miyake, A.; Tsuchiyama, A.] Kyoto Univ, Dept Geol & Mineral, Kyoto 6068501, Japan. [Nakamura-Messenger, K.; Messenger, S.] NASA Johnson Space Ctr, Houston, TX USA. EM jmatsuno@kueps.kyoto-u.ac.jp NR 5 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A267 EP A267 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200264 ER PT J AU McCubbin, FM Tartese, R Santos, AR Domokos, G Muttik, N Szabo, T Vazquez, J Boyce, JW Keller, LP Jerolmack, DJ Anand, M Moser, DE Delhaye, T Shearer, CK Agee, CB AF McCubbin, F. M. Tartese, R. Santos, A. R. Domokos, G. Muttik, N. Szabo, T. Vazquez, J. Boyce, J. W. Keller, L. P. Jerolmack, D. J. Anand, M. Moser, D. E. Delhaye, T. Shearer, C. K. Agee, C. B. TI ALTERATION OF SEDIMENTARY CLASTS IN MARTIAN METEORITE NORTHWEST AFRICA 7034 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [McCubbin, F. M.; Santos, A. R.; Muttik, N.; Shearer, C. K.; Agee, C. B.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Tartese, R.; Anand, M.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. [Domokos, G.; Szabo, T.] Budapest Univ Technol & Econ, Dept Mech Mat & Struct, Budapest, Hungary. [Vazquez, J.] US Geol Survey, Menlo Pk, CA 94025 USA. [Vazquez, J.] Stanford Univ, Stanford USGS Ion Microprobe Lab, Stanford, CA 94305 USA. [Boyce, J. W.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Keller, L. P.] NASA Johnson Space Ctr, Houston, TX 77058 USA. [Jerolmack, D. J.] Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA. [Anand, M.] Nat Hist Museum, Dept Earth Sci, London SW7 5BD, England. [Moser, D. E.] Univ Western Ontario, Dept Earth Sci, London, ON N6A 5B7, Canada. [Delhaye, T.] Univ Rennes 1, Plateforme ONIS NanoSIMS, F-35042 Rennes, France. EM fmccubbi@unm.edu NR 1 TC 1 Z9 1 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A269 EP A269 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200266 ER PT J AU Mikouchi, T Aoyagi, Y Sugiyama, K Yokoyama, Y Goodrich, CA Zolensky, ME AF Mikouchi, T. Aoyagi, Y. Sugiyama, K. Yokoyama, Y. Goodrich, C. A. Zolensky, M. E. TI EXPERIMENTAL CRYSTALLIZATION OF IRON MARTENSITE IN THE ALMAHATA SITTA UREILITE. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID IMPACT C1 [Mikouchi, T.; Aoyagi, Y.] Univ Tokyo, Dept Earth & Planet Sci, Tokyo 1130033, Japan. [Sugiyama, K.; Yokoyama, Y.] Tohoku Univ, Inst Mat Res, Katahira, Miyagi 9808577, Japan. [Goodrich, C. A.] Planet Sci Inst, Tucson, AZ 85719 USA. [Zolensky, M. E.] NASA JSC, ARES, Houston, TX 77058 USA. EM mikou-chi@eps.s.u-tokyo.ac.jp RI Sugiyama, Kazumasa/B-3447-2010 NR 4 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A282 EP A282 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200279 ER PT J AU Mills, RD Simon, JI Wang, J Hauri, EH Alexander, CMO AF Mills, R. D. Simon, J. I. Wang, J. Hauri, E. H. Alexander, C. M. O'D. TI WATER CONTENT OF LUNAR ALKALI FELDSPAR. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID MOON C1 [Mills, R. D.; Simon, J. I.] NASA, Ctr Isotope Cosmochem & Geochronol, ARES, JSC, Houston, TX 77058 USA. [Wang, J.; Hauri, E. H.; Alexander, C. M. O'D.] Carnegie Inst Sci, DTM, Washington, DC 20015 USA. EM rdmills25@gmail.com NR 10 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A284 EP A284 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200281 ER PT J AU Mittlefehldt, DW AF Mittlefehldt, D. W. TI HOWARDITES AND MESOSIDERITES: CONTRASTING POLYMICT BRECCIAS FROM TWO SIMILAR DIFFERENTIATED ASTEROIDS. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID CONSTRAINTS; LITHOLOGIES; HISTORY; CLASTS C1 [Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. EM david.w.mittlefehldt@nasa.gov NR 12 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A285 EP A285 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200282 ER PT J AU Nagao, K Haba, MK Zolensky, M Jenniskens, P Shaddad, MH AF Nagao, K. Haba, M. K. Zolensky, M. Jenniskens, P. Shaddad, M. H. TI NOBLE GASES IN TWO FRAGMENTS OF DIFFERENT LITHOLOGIES FROM THE ALMAHATA SITTA METEORITE. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID ASTEROID 2008 TC3; UREILITE; RECOVERY C1 [Nagao, K.] Univ Tokyo, Geochem Res Ctr, Tokyo 1130033, Japan. [Haba, M. K.] NIPR, Tokyo 1908518, Japan. [Zolensky, M.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. [Jenniskens, P.] SETI Inst, Mountain View, CA 94043 USA. [Shaddad, M. H.] Univ Khartoum, Phys & Astron Dept, Khartoum 11115, Sudan. EM nagao@eqchem.s.u-tokyo.ac.jp NR 12 TC 0 Z9 0 U1 0 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A294 EP A294 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200291 ER PT J AU Nguyen, AN Berger, EL Nakamura-Messenger, K Messenger, S AF Nguyen, A. N. Berger, E. L. Nakamura-Messenger, K. Messenger, S. TI COORDINATED MINERALOGICAL AND ISOTOPIC ANALYSIS OF A COSMIC SYMPLECTITE IDENTIFIED IN A STARDUST TERMINAL PARTICLE. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID TRACKS C1 [Nguyen, A. N.; Berger, E. L.] NASA, Lyndon B Johnson Space Ctr, JETS, Houston, TX 77058 USA. [Nguyen, A. N.; Berger, E. L.; Nakamura-Messenger, K.; Messenger, S.] NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, ARES, Houston, TX 77058 USA. EM lan-anh.n.nguyen@nasa.gov NR 8 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A298 EP A298 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200295 ER PT J AU Nuth, JA Johnson, NM Carayon, A AF Nuth, Joseph A. Johnson, Natasha M. Carayon, Alicia TI MEASURING VOLATILE/SOLID CARBON BRANCHING RATIOS FOR FISCHER-TROPSCH-TYPE REACTIONS. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID SOLAR NEBULA; CHEMISTRY; CATALYSIS C1 [Nuth, Joseph A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Washington, DC USA. [Johnson, Natasha M.; Carayon, Alicia] NASA, Goddard Space Flight Ctr, Astrochem Lab, Washington, DC USA. [Carayon, Alicia] Int Space Univ, Illkirch Graffenstaden, France. EM joseph.a.nuth@nasa.gov RI Johnson, Natasha/E-3093-2012 NR 8 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A301 EP A301 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200298 ER PT J AU Park, J Nyquist, LE Herzog, GF Turrin, BD Lindsay, FN Delaney, JS Swisher, CC Shih, CY Shirai, N Yamaguchi, A AF Park, J. Nyquist, L. E. Herzog, G. F. Turrin, B. D. Lindsay, F. N. Delaney, J. S. Swisher, C. C., III Shih, C. -Y. Shirai, N. Yamaguchi, A. TI Ar-40/Ar-39 AGES OF ANORTHOSITIC LUNAR ROCK 64435 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Park, J.; Herzog, G. F.; Turrin, B. D.; Lindsay, F. N.; Delaney, J. S.; Swisher, C. C., III] Rutgers U, Piscataway, NJ 08854 USA. [Park, J.] LPI, Houston, TX 77058 USA. [Park, J.] Kingsborough Comm Coll, Brooklyn, NY 11235 USA. [Nyquist, L. E.] KR NASA Johnson Space Ctr, Houston, TX 77058 USA. [Shih, C. -Y.] Jacobs, Houston, TX 77258 USA. [Shirai, N.] Tokyo Metropolitan Univ, Hachioji, Tokyo 1920372, Japan. [Yamaguchi, A.] NIPR Tokyo, AMRC, Tokyo 1908518, Japan. NR 9 TC 0 Z9 0 U1 0 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A316 EP A316 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200313 ER PT J AU Povenmire, H Lehrman, N Zolensky, M AF Povenmire, H. Lehrman, N. Zolensky, M. TI THE DUMBBELL, LAYERED INTERNAL SCHLIEREN TEKTITE FROM CHINA SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Povenmire, H.] FL Inst Technol, Indialantic, FL 32903 USA. [Zolensky, M.] NASA JSC, ARES, Houston, TX 77058 USA. EM katiehall@yahoo.com NR 1 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A327 EP A327 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200324 ER PT J AU Rampino, MR AF Rampino, Michael R. TI DISC DARK MATTER IN THE GALAXY AND CYCLES OF EXTRATERRESTRIAL IMPACTS, MASS EXTINCTIONS AND GEOTECTONIC EVENTS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Rampino, Michael R.] NYU, Dept Biol & Environm Studies, New York, NY 10003 USA. [Rampino, Michael R.] NASA, Goddard Inst Space Studies, New York, NY 10027 USA. EM mrr1@nyu.edu NR 0 TC 0 Z9 0 U1 2 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A334 EP A334 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200331 ER PT J AU Sandford, SA Materese, CK Nuevo, M AF Sandford, S. A. Materese, C. K. Nuevo, M. TI FORMATION OF HETEROCYCLES FROM THE UV IRRADIATION OF POLYCYCLIC AROMATIC HYDROCARBONS IN ICES. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID ULTRAVIOLET PHOTOIRRADIATION; NUCLEOBASES; PYRIMIDINE; PHOTOLYSIS; ANALOGS C1 [Sandford, S. A.; Materese, C. K.; Nuevo, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Materese, C. K.] Oak Ridge Associated Univ, Oak Ridge, TN USA. [Nuevo, M.] Bay Area Environm Res Inst, Petaluma, CA USA. EM Scott.A.Sandford@nasa.gov NR 7 TC 0 Z9 0 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A353 EP A353 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200350 ER PT J AU Simon, JI Peters, TJ Tappa, MJ Agee, CB AF Simon, J. I. Peters, T. J. Tappa, M. J. Agee, C. B. TI NORTHWEST AFRICA 8159: AN similar to 2.3 BILLION YEAR OLD MARTIAN OLIVINE-BEARING AUGITE BASALT SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Simon, J. I.; Peters, T. J.; Tappa, M. J.] NASA, Lyndon B Johnson Space Ctr, Ctr Isotope Cosmochem & Geochronol Astromat Res &, Houston, TX 77058 USA. [Peters, T. J.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Tappa, M. J.] JETS Jacobs Technol, Houston, TX 77258 USA. [Agee, C. B.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. EM Justin.I.Simon@NASA.gov NR 4 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A363 EP A363 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200360 ER PT J AU Smith, RL Blake, GA Boogert, ACA Pontoppidan, KM Lockwood, AC AF Smith, R. L. Blake, G. A. Boogert, A. C. A. Pontoppidan, K. M. Lockwood, A. C. TI INVESTIGATING PROTOSTELLAR CARBON RESERVOIRS WITH HIGH-RESOLUTION SPECTROSCOPY TOWARD MASSIVE YOUNG STELLAR OBJECTS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID CO2 C1 [Smith, R. L.] NC Museum Nat Sci, Raleigh, NC USA. [Smith, R. L.] Appalachian State Univ, Boone, NC 28608 USA. [Blake, G. A.; Lockwood, A. C.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Boogert, A. C. A.] NASA Ames, SOFIA USRA, Ames, IA USA. [Pontoppidan, K. M.] Space Telescope Sci Inst, Baltimore, MD USA. EM rachel.smith@naturalsciences.org NR 9 TC 0 Z9 0 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A370 EP A370 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200367 ER PT J AU Steele, A McCubbin, FM Benning, LG Siljestrom, S Cody, GD Goreva, Y Hauri, EH Wang, J Kilcoyne, ALD Grady, M Verchovsky, A Sabbah, H Smith, C Freissinet, C Glavin, DP Burton, AS Fries, MD Blanco, JDR Glamoclija, M Rogers, KL Mikhail, S Zare, RN Wu, Q Ismail, A Dworkin, JP Bhartia, R AF Steele, A. McCubbin, F. M. Benning, L. G. Siljestroem, S. Cody, G. D. Goreva, Y. Hauri, E. H. Wang, J. Kilcoyne, A. L. D. Grady, M. Verchovsky, A. Sabbah, H. Smith, C. Freissinet, C. Glavin, D. P. Burton, A. S. Fries, M. D. Blanco, Rodriguez J. D. Glamoclija, M. Rogers, K. L. Mikhail, S. Zare, R. N. Wu, Q. Ismail, A. Dworkin, J. P. Bhartia, R. TI Hydrothermal Organic Synthesis on Mars: Evidence from the Tissint Meteorite SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Steele, A.; Siljestroem, S.; Cody, G. D.; Glamoclija, M.; Rogers, K. L.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [McCubbin, F. M.] Univ New Mexico, Dept Earth & Planetary Sci, Inst Meteorit, Albuquerque, NM 87131 USA. [Benning, L. G.; Blanco, Rodriguez J. D.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. [Siljestroem, S.] SP Tech Res Inst Sweden, Dept Chem Mat & Surfaces, Boras, Sweden. [Siljestroem, S.; Goreva, Y.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Hauri, E. H.; Wang, J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Kilcoyne, A. L. D.] Adv Light Source, Berkeley, CA USA. [Grady, M.; Verchovsky, A.] Stanford Univ, Ctr Earth Planetary Space & Astron Res, Stanford, CA 94305 USA. [Sabbah, H.; Zare, R. N.; Wu, Q.; Ismail, A.] Stanford Univ, Dept Chem, Stanford, CA 94305 USA. [Sabbah, H.] Univ Toulouse, Toulouse, France. [Sabbah, H.] CNRS, Toulouse, France. [Smith, C.] Nat Hist Museum, Dept Mineral, London, England. [Freissinet, C.; Glavin, D. P.; Dworkin, J. P.] NASA, Goddard Space Flight Ctr, Houston, TX USA. [Burton, A. S.; Fries, M. D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Blanco, Rodriguez J. D.] Univ Copenhagen, Dept Chem, Nanosci Ctr, DK-1168 Copenhagen, Denmark. [Glamoclija, M.] Rutgers State Univ, Dept Earth & Planetary Sci, Piscataway, NJ 08855 USA. [Rogers, K. L.] Rensselaer Polytech Inst, Troy, NY 12181 USA. [Mikhail, S.] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9YL, Midlothian, Scotland. [Ismail, A.] King Abdulaziz Univ, Dept Chem, Rabigh, Saudi Arabia. [Bhartia, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RI Ismail, Ali/I-7595-2012; Glavin, Daniel/D-6194-2012; Kilcoyne, David/I-1465-2013; Dworkin, Jason/C-9417-2012 OI Ismail, Ali/0000-0001-9556-5140; Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997 NR 0 TC 1 Z9 1 U1 1 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A376 EP A376 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200373 ER PT J AU Trivedi, M Smith, HD Sears, DWG AF Trivedi, M. Smith, H. D. Sears, D. W. G. TI DETECTING AND DISTINGUISHING METAMORPHIC GRADIENTS OF UNEQUILIBRATED (TYPE 3) ORDINARY CHONDRITES USING INFRARED REFLECTANCE SPECTRA SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Trivedi, M.; Smith, H. D.; Sears, D. W. G.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. EM Mi-hir.Trivedi17@bcp.org; Heather.d.smith@nasa.gov; derek.sears@nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A403 EP A403 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200400 ER PT J AU Tsuchiyama, A Miyake, A Zolensky, ME Uesugi, K Nakano, T Takeuchi, A Suzuki, Y Yoshida, K AF Tsuchiyama, A. Miyake, A. Zolensky, M. E. Uesugi, K. Nakano, T. Takeuchi, A. Suzuki, Y. Yoshida, K. TI SEARCH FOR FLUID INCLUSIONS IN A CARBONACEOUS CHONDRITE USING A NEW X-RAY MICRO-TOMOGRAPHY TECHNIQUE COMBAINED WITH FIB SAMPLING. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Tsuchiyama, A.; Miyake, A.; Yoshida, K.] Kyoto Univ, Grad Sch Sci, Kyoto 6068501, Japan. [Zolensky, M. E.] NASA, JSC, Houston, TX USA. [Uesugi, K.; Takeuchi, A.; Suzuki, Y.] SPring 8, JASRI, Koto, Hyogo, Japan. [Nakano, T.] GSJ, AIST, Tsukuba, Ibaraki, Japan. NR 4 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A404 EP A404 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200401 ER PT J AU Uesugi, M Tsuchiyama, A Uesugi, K Takeuchi, A Suzuki, Y Park, J Nagao, K Nishiizumi, K Nakashima, D Kita, N Langenhorst, F Keller, L Karouji, Y Nakato, A Yada, T Kumagai, K Okada, T Abe, M AF Uesugi, M. Tsuchiyama, A. Uesugi, K. Takeuchi, A. Suzuki, Y. Park, J. Nagao, K. Nishiizumi, K. Nakashima, D. Kita, N. Langenhorst, F. Keller, L. Karouji, Y. Nakato, A. Yada, T. Kumagai, K. Okada, T. Abe, M. TI CURRENT STATUS OF THE CONSORTIUM STURDY OF THE LARGEST ITOKAWA PARTICLE RA-QD02-0136-01 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Uesugi, M.; Karouji, Y.; Nakato, A.; Yada, T.; Kumagai, K.; Okada, T.; Abe, M.] Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Tokyo, Japan. [Tsuchiyama, A.; Okada, T.; Abe, M.] Kyoto Univ, Kyoto 6068501, Japan. [Uesugi, K.; Takeuchi, A.; Suzuki, Y.] Japan Synchrotron Radiat Inst JASRI, Tokyo, Japan. [Park, J.] Rutgers State Univ, Piscataway, NJ 08855 USA. [Nagao, K.] Univ Tokyo, Tokyo 1138654, Japan. [Nishiizumi, K.] Univ Calif, Oakland, CA USA. [Nakashima, D.] Tohoku Univ, Sendai, Miyagi 980, Japan. [Kita, N.] Univ Wisconsin Madison, Madison, WI USA. [Langenhorst, F.] Univ Jena, D-07745 Jena, Germany. [Keller, L.] NASA, JSC, Houston, TX USA. NR 8 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A409 EP A409 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200406 ER PT J AU Weisberg, MK Zolensky, ME Kimura, M Ebel, DS AF Weisberg, M. K. Zolensky, M. E. Kimura, M. Ebel, D. S. TI THE HIGHLY PRIMITIVE ALH 81189 EH3 CHONDRITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID ENSTATITE CHONDRITES; EARTH C1 [Weisberg, M. K.] Kingsborough Coll CUNY, Dept Phys Sci, Brooklyn, NY 11235 USA. [Weisberg, M. K.; Ebel, D. S.] CUNY, Grad Ctr, New York, NY 10016 USA. [Weisberg, M. K.; Ebel, D. S.] Amer Museum Nat Hist, Dept Earth & Planet Sci, New York, NY 10024 USA. [Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. [Kimura, M.] Ibaraki Univ, Fac Sci, Mito, Ibaraki 3108512, Japan. [Kimura, M.] Natl Inst Polar Res, Tokyo 1908518, Japan. NR 14 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A429 EP A429 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200426 ER PT J AU Wozniakiewicz, PJ Bradley, JP Price, MC Zolensky, ME Ishii, HA Brownlee, DE Russell, SS AF Wozniakiewicz, P. J. Bradley, J. P. Price, M. C. Zolensky, M. E. Ishii, H. A. Brownlee, D. E. Russell, S. S. TI CONTEMPORARY COSMIC DUST ARRIVING AT THE EARTH'S SURFACE: INITIAL RESULTS FROM THE KWAJALEIN MICROMETEORITE COLLECTION. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID ACCRETION RATE C1 [Wozniakiewicz, P. J.; Russell, S. S.] Nat Hist Museum, Dept Earth Sci, London SW7 5BD, England. [Wozniakiewicz, P. J.; Price, M. C.] Univ Kent, Sch Phys Sci, Canterbury CT2 7NH, Kent, England. [Bradley, J. P.; Ishii, H. A.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Brownlee, D. E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. EM p.wozniakiewicz@nhm.ac.uk NR 6 TC 0 Z9 0 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A438 EP A438 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200435 ER PT J AU Yabuta, H Uesugi, M Naraoka, H Ito, M Kilcoyne, D Sandford, SA Kitajima, F Mita, H Takano, Y Yada, T Karouji, Y Ishibashi, Y Okada, T Abe, M AF Yabuta, H. Uesugi, M. Naraoka, H. Ito, M. Kilcoyne, D. Sandford, S. A. Kitajima, F. Mita, H. Takano, Y. Yada, T. Karouji, Y. Ishibashi, Y. Okada, T. Abe, M. TI FUNCTIONAL GROUP COMPOSITIONS OF CARBONACEOUS MATERIALS OF HAYABUSA-RETURNED SAMPLES. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Yabuta, H.] Osaka Univ, Suita, Osaka 565, Japan. [Uesugi, M.; Yada, T.; Karouji, Y.; Ishibashi, Y.; Okada, T.; Abe, M.] JAXA ISAS, Sagamihara, Kanagawa, Japan. [Naraoka, H.; Kitajima, F.] Kyushu Univ, Fukuoka 812, Japan. [Ito, M.; Takano, Y.] JAMSTEC, Yokosuka, Kanagawa, Japan. [Kilcoyne, D.] LBNL, Adv Light Source, Berkeley, CA USA. [Sandford, S. A.] NASA, Ames, IA USA. [Mita, H.] Fukuoka Inst Tech Japan, Fukuoka, Japan. EM hyabuta@ess.sci.osaka-u.ac.jp RI Kilcoyne, David/I-1465-2013 NR 9 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A443 EP A443 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200440 ER PT J AU Zeigler, RA Almeida, NV Sykes, D Smith, CL AF Zeigler, R. A. Almeida, N. V. Sykes, D. Smith, C. L. TI X-RAY MICRO-COMPUTED TOMOGRAPHY OF APOLLO SAMPLES AS A CURATION TECHNIQUE ENABLING BETTER RESEARCH SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Zeigler, R. A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Almeida, N. V.; Smith, C. L.] Nat Hist Museum, Dept Earth Sci, London, England. [Sykes, D.] Nat Hist Museum, Imaging & Anal Ctr, London, England. EM ryan.a.zeigler@nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A450 EP A450 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200447 ER PT J AU Zolensky, M Frank, D AF Zolensky, M. Frank, D. TI SURVIVING HIGH-TEMPERATURE COMPONENTS IN CI CHONDRITES. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Zolensky, M.] NASA, ARES, JSC, Houston, TX 77058 USA. [Frank, D.] ESCG, Houston, TX 77058 USA. EM michael.e.zolensky@nasa.gov NR 3 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2014 VL 49 SU 1 SI SI BP A453 EP A453 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200450 ER PT J AU Morscher, GN Smith, C Maillet, E Baker, C Monsour, R AF Morscher, Gregory N. Smith, Craig Maillet, Emmanuel Baker, Chris Monsour, Rabih TI Electrical resistance monitoring of damage and crack growth in advanced SiC-based ceramic composites SO AMERICAN CERAMIC SOCIETY BULLETIN LA English DT Article ID MATRIX COMPOSITES C1 [Morscher, Gregory N.; Maillet, Emmanuel; Monsour, Rabih] Univ Akron, Akron, OH 44325 USA. [Smith, Craig] NASA, Glenn Res Ctr, Cleveland, OH USA. [Baker, Chris] Bridgestone Amer Tire Operat, Akron, OH USA. RP Morscher, GN (reprint author), Univ Akron, Akron, OH 44325 USA. EM gm33@uakron.edu OI Maillet, Emmanuel/0000-0001-5143-4982 FU ONR [N00014-11-1-0765]; Navy STTR [N68335-13-C-0349]; NASA Glenn Research Center FX ONR Contract No. N00014-11-1-0765 (William Nickerson PI), Navy STTR Contract No. N68335-13-C-0349, and NASA Glenn Research Center funded this work. NR 10 TC 1 Z9 1 U1 0 U2 10 PU AMER CERAMIC SOC PI WESTERVILLE PA 600 N CLEVELAND AVE, WESTERVILLE, OH 43082 USA SN 0002-7812 EI 1945-2705 J9 AM CERAM SOC BULL JI Am. Ceram. Soc. Bull. PD SEP PY 2014 VL 93 IS 7 BP 28 EP 31 PG 4 WC Materials Science, Ceramics SC Materials Science GA AO8OV UT WOS:000341615000019 ER PT J AU Jain, M Jiang, AX Kido, T Takadama, K Mercer, EG Rungta, N Waser, M Wagner, A Burke, J Sofge, D Lawless, W Sridharan, M Hawes, N Hwang, T AF Jain, Manish Jiang, Albert Xin Kido, Takashi Takadama, Keiki Mercer, Eric G. Rungta, Neha Waser, Mark Wagner, Alan Burke, Jennifer Sofge, Don Lawless, William Sridharan, Mohan Hawes, Nick Hwang, Tim TI Reports of the 2014 AAAI Spring Symposium Series SO AI MAGAZINE LA English DT Article AB The Association for the Advancement of Artificial Intelligence was pleased to present the AAAI 2014 Spring Symposium Series, held Monday through Wednesday, March 24-26, 2014. The titles of the eight symposia were Applied Computational Game Theory, Big Data Becomes Personal:, Knowledge into Meaning, Formal Verification and Modeling in Human-Machine Systems, Implementing Selves with Safe Motivational Systems and Self-Improvement, The Intersection of Robust Intelligence and Trust in Autonomous Systems, Knowledge Representation and Reasoning in Robotics, Qualitative Representations for Robots, and Social Hacking and Cognitive Security on the Internet and New Media). This report contains summaries of the symposia, written, in most cases, by the cochairs of the symposium. C1 [Jain, Manish] Virginia Polytech Inst & State Univ, Dept Comp Sci, Blacksburg, VA 24061 USA. [Jiang, Albert Xin] Univ So Calif, Dept Comp Sci, Los Angeles, CA 90089 USA. [Kido, Takashi] Rikengenesis, Yokohama, Kanagawa, Japan. [Takadama, Keiki] Univ Electrocommun, Chofu, Tokyo 182, Japan. [Mercer, Eric G.] Brigham Young Univ, Dept Comp Sci, Provo, UT 84602 USA. [Rungta, Neha] NASA, Ames Res Ctr, Moffett Field, CA USA. [Waser, Mark] Digital Wisdom Inst, New York, NY USA. [Wagner, Alan] Georgia Inst Technol, Georgia Tech Res Inst, Atlanta, GA 30332 USA. [Burke, Jennifer] Boeing Res & Technol, New York, NY USA. [Sofge, Don] Naval Res Lab, Washington, DC USA. [Lawless, William] Pain Coll, Augusta, GA USA. [Sridharan, Mohan] Texas Tech Univ, Lubbock, TX 79409 USA. [Hawes, Nick] Univ Birmingham, Sch Comp Sci, Birmingham B15 2TT, W Midlands, England. [Hwang, Tim] Pacific Social Architecting Corp, New York, NY USA. [Hwang, Tim] Data & Soc Res Inst New York City, New York, NY USA. RP Jain, M (reprint author), Virginia Polytech Inst & State Univ, Dept Comp Sci, Blacksburg, VA 24061 USA. OI Hawes, Nick/0000-0002-7556-6098 NR 0 TC 0 Z9 0 U1 1 U2 6 PU AMER ASSOC ARTIFICIAL INTELL PI MENLO PK PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA SN 0738-4602 J9 AI MAG JI AI Mag. PD FAL PY 2014 VL 35 IS 3 BP 70 EP 76 PG 7 WC Computer Science, Artificial Intelligence SC Computer Science GA AP1DB UT WOS:000341805500008 ER PT J AU Anenberg, SC West, JJ Yu, HB Chin, M Schulz, M Bergmann, D Bey, I Bian, HS Diehl, T Fiore, A Hess, P Marmer, E Montanaro, V Park, R Shindell, D Takemura, T Dentener, F AF Anenberg, Susan C. West, J. Jason Yu, Hongbin Chin, Mian Schulz, Michael Bergmann, Dan Bey, Isabelle Bian, Huisheng Diehl, Thomas Fiore, Arlene Hess, Peter Marmer, Elina Montanaro, Veronica Park, Rokjin Shindell, Drew Takemura, Toshihiko Dentener, Frank TI Impacts of intercontinental transport of anthropogenic fine particulate matter on human mortality SO AIR QUALITY ATMOSPHERE AND HEALTH LA English DT Article DE Health impact assessment; Particulate matter; Long-range transport; Chemical transport modeling ID REGIONAL AIR-QUALITY; MULTIMODEL ASSESSMENT; EMISSION CONTROLS; GLOBAL BURDEN; UNITED-STATES; POLLUTION; AEROSOL; OZONE; EXPOSURE; VISIBILITY AB Fine particulate matter with diameter of 2.5 mu m or less (PM2.5) is associated with premature mortality and can travel long distances, impacting air quality and health on intercontinental scales. We estimate the mortality impacts of 20 % anthropogenic primary PM2.5 and PM2.5 precursor emission reductions in each of four major industrial regions (North America, Europe, East Asia, and South Asia) using an ensemble of global chemical transport model simulations coordinated by the Task Force on Hemispheric Transport of Air Pollution and epidemiologically-derived concentration-response functions. We estimate that while 93-97 % of avoided deaths from reducing emissions in all four regions occur within the source region, 3-7 % (11,500; 95 % confidence interval, 8,800-14,200) occur outside the source region from concentrations transported between continents. Approximately 17 and 13 % of global deaths avoided by reducing North America and Europe emissions occur extraregionally, owing to large downwind populations, compared with 4 and 2 % for South and East Asia. The coarse resolution global models used here may underestimate intraregional health benefits occurring on local scales, affecting these relative contributions of extraregional versus intraregional health benefits. Compared with a previous study of 20 % ozone precursor emission reductions, we find that despite greater transport efficiency for ozone, absolute mortality impacts of intercontinental PM2.5 transport are comparable or greater for neighboring source-receptor pairs, due to the stronger effect of PM2.5 on mortality. However, uncertainties in modeling and concentration-response relationships are large for both estimates. C1 [Anenberg, Susan C.] US EPA, Washington, DC 20460 USA. [West, J. Jason] Univ N Carolina, Chapel Hill, NC USA. [Yu, Hongbin] Univ Maryland, College Pk, MD 20742 USA. [Chin, Mian; Bian, Huisheng; Diehl, Thomas] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Schulz, Michael] Norwegian Meteorol Inst, Oslo, Norway. [Bergmann, Dan] Lawrence Livermore Natl Lab, Livermore, CA USA. [Bey, Isabelle] Swiss Fed Inst Technol, Zurich, Switzerland. [Diehl, Thomas] Univ Space Res Assoc, Columbia, MD USA. [Fiore, Arlene] Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA. [Hess, Peter] Cornell Univ, Dept Biol & Environm Engn, Ithaca, NY USA. [Marmer, Elina] Univ Hamburg, Dept Educ, Hamburg, Germany. [Montanaro, Veronica] Univ Aquila, I-67100 Laquila, Italy. [Park, Rokjin] Seoul Natl Univ, Seoul, South Korea. [Shindell, Drew] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Shindell, Drew] Columbia Earth Inst, New York, NY USA. [Takemura, Toshihiko] Kyushu Univ, Appl Mech Res Inst, Fukuoka 8168580, Japan. [Dentener, Frank] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21020 Ispra, Italy. RP Anenberg, SC (reprint author), US EPA, 1200 Penn Ave NW MC6301A, Washington, DC 20460 USA. EM anenberg.susan@epa.gov RI Yu, Hongbin/C-6485-2008; Takemura, Toshihiko/C-2822-2009; Kyushu, RIAM/F-4018-2015; West, Jason/J-2322-2015; Park, Rokjin/I-5055-2012; Shindell, Drew/D-4636-2012; Schulz, Michael/A-6930-2011; U-ID, Kyushu/C-5291-2016; Chin, Mian/J-8354-2012 OI Yu, Hongbin/0000-0003-4706-1575; Takemura, Toshihiko/0000-0002-2859-6067; West, Jason/0000-0001-5652-4987; Park, Rokjin/0000-0001-8922-0234; Schulz, Michael/0000-0003-4493-4158; FU NASA; US Department of Energy (BER) at LLNL [DE-AC5207NA27344] FX The opinions expressed in this article are the authors' and do not necessarily represent those of their employers, including the USEPA. Model simulations were performed under the UN ECE Task Force on Hemispheric Transport of Air Pollution. H. Y. was supported by the NASA Atmospheric Composition Modeling and Analysis Program administered by R. Eckman. D. B. was supported by the US Department of Energy (BER) at LLNL under contract DE-AC5207NA27344. NR 48 TC 6 Z9 6 U1 7 U2 40 PU SPRINGER INTERNATIONAL PUBLISHING AG PI CHAM PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND SN 1873-9318 EI 1873-9326 J9 AIR QUAL ATMOS HLTH JI Air Qual. Atmos. Health PD SEP PY 2014 VL 7 IS 3 BP 369 EP 379 DI 10.1007/s11869-014-0248-9 PG 11 WC Environmental Sciences SC Environmental Sciences & Ecology GA AO8GP UT WOS:000341592100011 ER PT J AU Hasoglu, MF Abdel-Naby, SA Gatuzz, E Garcia, J Kallman, TR Mendoza, C Gorczyca, TW AF Hasoglu, M. F. Abdel-Naby, Sh. A. Gatuzz, E. Garcia, J. Kallman, T. R. Mendoza, C. Gorczyca, T. W. TI K-SHELL PHOTOABSORPTION OF MAGNESIUM IONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atomic data; atomic processes; ISM: abundances; line: formation ID X-RAY SPECTROSCOPY; PHOTOIONIZATION CROSS-SECTIONS; XMM-NEWTON OBSERVATION; INTERSTELLAR-MEDIUM; FLUORESCENCE YIELDS; ATOMIC OXYGEN; ABSORPTION; CHANDRA; AUGER; ABUNDANCES AB X-ray photoabsorption cross sections have been computed for all magnesium ions with three or more electrons using the R-matrix method. A comparison with other available data for Mg II-Mg x shows good qualitative agreement in the resultant resonance shapes. However, for the lower ionization stages, and for singly ionized Mg II in particular, the previous R-matrix results overestimate the K-edge position due to the neglect of important orbital relaxation effects, and a global shift downward in photon energy of those cross sections is therefore warranted. We have found that the cross sections for Mg I and Mg II are further complicated by the M-shell (n = 3) occupancy. As a result, the treatment of spectator Auger decay of 1s -> np resonances using a method based on multichannel quantum defect theory and an optical potential becomes problematic, making it necessary to implement an alternative, approximate treatment of Auger decay for neutral Mg I. The new cross sections are used to fit the Mg K edge in XMM-Newton spectra of the low-mass X-ray binary GS 1826-238, where most of the interstellar Mg is found to be in ionized form. C1 [Hasoglu, M. F.] Hasan Kalyoncu Univ, Dept Comp Engn, TR-27100 Sahinbey, Gaziantep, Turkey. [Abdel-Naby, Sh. A.] Auburn Univ, Dept Phys, Auburn, AL 36849 USA. [Gatuzz, E.; Mendoza, C.] Inst Venezolano Invest Cient, Ctr Fis, Caracas 1020, Venezuela. [Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mendoza, C.; Gorczyca, T. W.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. RP Hasoglu, MF (reprint author), Hasan Kalyoncu Univ, Dept Comp Engn, TR-27100 Sahinbey, Gaziantep, Turkey. OI Mendoza, Claudio/0000-0002-2854-4806 FU NASA APRA grant [NNX11AF32G] FX This work was supported in part by the NASA APRA grant NNX11AF32G. NR 55 TC 3 Z9 3 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2014 VL 214 IS 1 AR 8 DI 10.1088/0067-0049/214/1/8 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP0TP UT WOS:000341777800008 ER PT J AU Gopalswamy, N Xie, H Akiyama, S Makela, PA Yashiro, S AF Gopalswamy, Nat Xie, Hong Akiyama, Sachiko Makela, Pertti A. Yashiro, Seiji TI Major solar eruptions and high-energy particle events during solar cycle 24 SO EARTH PLANETS AND SPACE LA English DT Article DE Coronal mass ejections; Flares; Ground level enhancement events; Solar energetic particle events ID CORONAL MASS EJECTIONS; II RADIO-BURSTS; GROUND-LEVEL ENHANCEMENT; SPACE WEATHER; PROTON EVENTS; PEAK INTENSITIES; SHOCK FORMATION; NEAR-SUN; VARIABILITY; FLARES AB We report on a study of all major solar eruptions that occurred on the frontside of the Sun during the rise to peak phase of cycle 24 (first 62 months) in order to understand the key factors affecting the occurrence of large solar energetic particle events (SEPs) and ground level enhancement (GLE) events. The eruptions involve major flares with soft X-ray peak flux >= 5.0 x 10(-5) Wm(-2) (i.e., flare size >= M5.0) and accompanying coronal mass ejections (CMEs). The selection criterion was based on the fact that the only front-side GLE in cycle 24 (GLE 71) had a flare size of M5.1. Only approximately 37% of the major eruptions from the western hemisphere resulted in large SEP events. Almost the same number of large SEP events was produced in weaker eruptions (flare size < M5.0), suggesting that the soft X-ray flare is not a good indicator of SEP or GLE events. On the other hand, the CME speed is a good indicator of SEP and GLE events because it is consistently high supporting the shock acceleration mechanism. We found the CME speed, magnetic connectivity to Earth (in longitude and latitude), and ambient conditions as the main factors that contribute to the lack of high-energy particle events during cycle 24. Several eruptions poorly connected to Earth (eastern-hemisphere or behind-the-west-limb events) resulted in very large SEP events detected by the Solar Terrestrial Relations Observatory (STEREO) spacecraft. Some very fast CMEs, likely to have accelerated particles to GeV energies, did not result in a GLE event because of poor latitudinal connectivity. The stringent latitudinal requirement suggests that the highest-energy particles are likely accelerated in the nose part of shocks, while the lower energy particles are accelerated at all parts. There were also well-connected fast CMEs, which did not seem to have accelerated high-energy particles due to possible unfavorable ambient conditions (high Alfven speed, overall reduction in acceleration efficiency in cycle 24). C1 [Gopalswamy, Nat] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Xie, Hong; Akiyama, Sachiko; Makela, Pertti A.; Yashiro, Seiji] Catholic Univ Amer, Washington, DC 20064 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM nat.gopalswamy@nasa.gov OI Gopalswamy, Nat/0000-0001-5894-9954 FU NASA's LWS; LWS TRT FX This work was supported by NASA's LWS and LWS TR&T programs. This work benefitted greatly from the open data policy of NASA. NR 48 TC 20 Z9 20 U1 2 U2 7 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1880-5981 J9 EARTH PLANETS SPACE JI Earth Planets Space PD SEP 1 PY 2014 VL 66 AR 104 DI 10.1186/1880-5981-66-104 PG 15 WC Geosciences, Multidisciplinary SC Geology GA AP6EG UT WOS:000342169800001 ER PT J AU Cartwright, JA Ott, U Mittlefehldt, DW AF Cartwright, J. A. Ott, U. Mittlefehldt, D. W. TI The quest for regolithic howardites. Part 2: Surface origins highlighted by noble gases SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID CALCIUM-RICH ACHONDRITES; CARBONACEOUS CHONDRITE CLASTS; ANCIENT SOLAR-ACTIVITY; PARENT BODY REGOLITH; RAY EXPOSURE AGES; ANGRA-DOS-REIS; BASALTIC ACHONDRITES; ANTARCTIC METEORITES; PRODUCTION-RATES; COSMOGENIC NEON AB We report noble gas data of helium (He), neon (Ne), argon (Ar), krypton (Kr) and xenon (Xe), cosmic ray exposure (CRE) ages and nominal gas retention (K Ar, U Th He) ages for seven howardites (CRE 01400, EET 87513, EET 87518, EET 99400, GRO 95535, GRO 95602, SAN 03472), in continuing research to identify regolithic samples, and better understand the vestan regolith. In our previous work, we found little correlation between suggested regolith parameters of Ni > 300 mu g/g, Al2O3 8-9 wt% and eucrite/diogenite (E:D) ratio of 2:1 (Warren et al., 2009), and trapped solar wind (SW), fractionated solar wind (FSW) or planetary noble gas components (from impacted material) -noble gas indicators of a regolithic origin. Here, we have expanded our data set to include samples outside of these parameters to further explore composition, and the differences in Ni content as indicators for the presence of non-Vesta material. In addition, our sample set includes two potentially paired meteorites from the GRO suite. Finally, in our petrographic studies, the samples selected showed no evidence for carbonaceous chondrite fragments, which should reduce the effect of "contamination" by planetary noble gas components, and will allow us to better identify SW/FSW components, where present. Of the samples studied here, three howardites GRO 95535, GRO 95602 and EET 87513 show evidence for a regolithic origin, with both isotopic and element noble gas ratios clearly pointing to the presence of trapped components similar to SW/FSW or planetary. The two GRO howardites, GRO 95535 and GRO 95602, show similar noble gas ratios to our previously defined SW/FSW dominated regolithic group (LEW 85313 and MET 00423), suggesting a surface origin for these samples. However, interestingly, the GRO samples show vastly different cosmogenic noble gas abundances, and thus different CRE ages, which suggests that they are not paired. For howardite EET 87513, the data hint to the presence of CM-material, with a neon release pattern similar to our defined planetary/FSW dominated regolithic group (CM-rich samples PRA 04401, SCO 06040). Our petrological investigations found no evidence for CM fragments within EET 87513, though a single clast was reported previously (Buchanan et al., 1993). Aside from the Ne release pattern, the remaining noble gas data show more similarity with SW/FSW components. The remaining four howardites CRE 01400, EET 87518, EET 99400, and SAN 03472 and are dominated by cosmogenic noble gases, and show no evidence for a regolithic origin. Our data suggest that a CM-composition is likely present in all samples to some degree, but that this can be overprinted by SW components or cosmogenic components obtained in situ on the vestan surface or during transit to Earth respectively. The presence of CM material is an important parameter for understanding the evolution of Vesta's surface. While we have uncovered three further regolithic howardites (similar to 13 regolithic total, of similar to 41 analysed), further noble gas analysis of HED meteorites is needed to not only determine regolithic origins, but to better characterise the abundance of carbonaceous chondrite material and its effect on the noble gas signatures of such samples. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Cartwright, J. A.; Ott, U.] Max Planck Inst Chem, D-55128 Mainz, Germany. [Cartwright, J. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Ott, U.] Univ West Hungary, H-9700 Szombathely, Hungary. [Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. RP Cartwright, JA (reprint author), CALTECH, Div Geol & Planetary Sci, MC 100-23,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM jac@caltech.edu RI Cartwright, Julia/A-8470-2013 FU National Science Foundation (USA) FX We thank the National Science Foundation (USA) for funding the ANSMET collecting teams that brought back the Antarctic samples studied here, and the Meteorite Working Group, NASA-Johnson Space Center and the National Museum of Natural History (Smithsonian Institution) for allocation of the samples. We are grateful to K. McBride and C. Satterwhite for extraction of the samples used in this work. DWM's participation in this project, and bulk sample major and trace element analyses were funded through NASA's Cosmochemistry Program. NR 111 TC 8 Z9 8 U1 3 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD SEP 1 PY 2014 VL 140 BP 488 EP 508 DI 10.1016/j.gca.2014.05.033 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2SP UT WOS:000341925300031 ER PT J AU Feuerecker, M Crucian, B Salam, AP Rybka, A Kaufmann, I Moreels, M Quintens, R Schelling, G Thiel, M Baatout, S Sams, C Chouker, A AF Feuerecker, Matthias Crucian, Brian Salam, Alex P. Rybka, Ales Kaufmann, Ines Moreels, Marjan Quintens, Roel Schelling, Gustav Thiel, Manfred Baatout, Sarah Sams, Clarence Chouker, Alexander TI Early Adaption to the Antarctic Environment at Dome C: Consequences on Stress-Sensitive Innate Immune Functions SO HIGH ALTITUDE MEDICINE & BIOLOGY LA English DT Article DE adenosine; Antarctica; hormones; hypobaric hypoxia; polymorphonuclear leukocytes (PMNs) ID ADENOSINE A(2A) RECEPTORS; HIGH-ALTITUDE; HEALTHY-VOLUNTEERS; HYPOXIA; CORTISOL; MEGAKARYOCYTOPOIESIS; CATECHOLAMINES; INFLAMMATION; RESPONSES; AFFINITY AB Purpose/Aims: Medical reports of Antarctic expeditions indicate that health is affected under these extreme conditions. The present study at CONCORDIA-Station (Dome C, 3233 m) seeks to investigate the early consequences of confinement and hypobaric hypoxia on the human organism. Methods: Nine healthy male participants were included in this study. Data collection occurred before traveling to Antarctica (baseline), and at 1 week and 1 month upon arrival. Investigated parameters included basic physiological variables, psychological stress tests, cell blood count, stress hormones, and markers of innate immune functions in resting and stimulated immune cells. By testing for the hydrogen peroxide (H2O2) production of stimulated polymorphonuclear leukocytes (PMNs), the effects of the hypoxia-adenosine-sensitive immune modulatory pathways were examined. Results: As compared to baseline data, reduced oxygen saturation, hemoconcentration, and an increase of secreted catecholamines was observed, whereas no psychological stress was seen. Upon stimulation, the activity of PMNs and L-selectin shedding was mitigated after 1 week. Endogenous adenosine concentration was elevated during the early phase. In summary, living conditions at high altitude influence the innate immune system's response. After 1 month, some of the early effects on the human organism were restored. Conclusion: As this early adaptation is not related to psychological stress, the changes observed are likely to be induced by environmental stressors, especially hypoxia. As hypoxia is triggering ATP-catabolism, leading to elevated endogenous adenosine concentrations, this and the increased catecholamine concentration might contribute to the early, but reversible downregulation of innate immune functions. This indicates the slope of innate immune adaptation to hypoxia. C1 [Feuerecker, Matthias; Kaufmann, Ines; Schelling, Gustav; Chouker, Alexander] Univ Munich, Dept Anaesthesiol, Klinikum Grosshadern, Res Grp Stress & Immun, D-81377 Munich, Germany. [Crucian, Brian; Sams, Clarence] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Salam, Alex P.; Rybka, Ales] European Space Agcy, Concordia, Dome, France. [Salam, Alex P.] Univ Oxford, Inst Cognit & Evolutionary Anthropol, London, England. [Moreels, Marjan; Quintens, Roel; Baatout, Sarah] CEN SCK, Belgian Nucl Res Ctr, Radiobiol Unit, B-2400 Mol, Belgium. [Thiel, Manfred] Heidelberg Univ, Fac Med, Dept Anaesthesiol & Intens Care, Mannheim, Germany. [Baatout, Sarah] Univ Ghent, Dept Mol Biotechnol, Ghent, Belgium. RP Chouker, A (reprint author), Univ Munich, Dept Anaesthesiol, Marchioninistr 15, D-81377 Munich, Germany. EM alexander.chouker@med.uni-muenchen.de FU European Space Agency; French (IPEV) polar institute; Italian (PNRA) polar institute; German National Space Program (DLR) [50WB0719/WB0919]; 2 PRODEX/BELSPO/ESA [C90-391, 42-000-90-380]; NASA (JSC) FX The authors are grateful to the support from the European Space Agency (ESA ELIPS 3 and 4 programs), the French (IPEV) and Italian (PNRA) polar institutes, and the German National Space Program (DLR, 50WB0719/WB0919). This research was also financially supported by the 2 PRODEX/BELSPO/ESA contracts (C90-391 and 42-000-90-380) and NASA (JSC). NR 37 TC 2 Z9 4 U1 2 U2 12 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1527-0297 EI 1557-8682 J9 HIGH ALT MED BIOL JI High Alt. Med. Biol. PD SEP PY 2014 VL 15 IS 3 BP 341 EP 348 DI 10.1089/ham.2013.1128 PG 8 WC Biophysics; Public, Environmental & Occupational Health; Sport Sciences SC Biophysics; Public, Environmental & Occupational Health; Sport Sciences GA AP5ZL UT WOS:000342157100009 PM 25099674 ER PT J AU Mukhanov, O Prokopenko, G Romanofsky, R AF Mukhanov, Oleg Prokopenko, Georgy Romanofsky, Robert TI Quantum Sensitivity SO IEEE MICROWAVE MAGAZINE LA English DT Article ID INTERFERENCE FILTERS; MAGNETIC-FIELD; MAGNETOMETERS; SYSTEMS; RADIO C1 [Mukhanov, Oleg; Prokopenko, Georgy] Hypres Inc, Elmsford, NY 10523 USA. [Romanofsky, Robert] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Mukhanov, O (reprint author), Hypres Inc, 175 Clearbrook Rd, Elmsford, NY 10523 USA. EM mukhanov@hypres.com NR 38 TC 11 Z9 11 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1527-3342 EI 1557-9581 J9 IEEE MICROW MAG JI IEEE Microw. Mag. PD SEP-OCT PY 2014 VL 15 IS 6 BP 57 EP 65 DI 10.1109/MMM.2014.2332421 PG 9 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA AP4UX UT WOS:000342075400008 ER PT J AU Scaramuzza, D Achtelik, MC Doitsidis, L Fraundorfer, F Kosmatopoulos, E Martinelli, A Achtelik, MW Chli, M Chatzichristofis, S Kneip, L Gurdan, D Heng, L Lee, GH Lynen, S Meier, L Pollefeys, M Renzaglia, A Siegwart, R Stumpf, JC Tanskanen, P Troiani, C Weiss, S AF Scaramuzza, Davide Achtelik, Michael C. Doitsidis, Lefteris Fraundorfer, Friedrich Kosmatopoulos, Elias Martinelli, Agostino Achtelik, Markus W. Chli, Margarita Chatzichristofis, Savvas Kneip, Laurent Gurdan, Daniel Heng, Lionel Lee, Gim Hee Lynen, Simon Meier, Lorenz Pollefeys, Marc Renzaglia, Alessandro Siegwart, Roland Stumpf, Jan Carsten Tanskanen, Petri Troiani, Chiara Weiss, Stephan TI Vision-Controlled Micro Flying Robots From System Design to Autonomous Navigation and Mapping in GPS-Denied Environments SO IEEE ROBOTICS & AUTOMATION MAGAZINE LA English DT Article ID OPTIMIZATION; ALGORITHMS; QUADROTOR; COVERAGE; SCALE C1 [Scaramuzza, Davide] Univ Zurich, CH-8050 Zurich, Switzerland. [Achtelik, Michael C.; Gurdan, Daniel; Stumpf, Jan Carsten] Ascending Technol GmbH, D-82152 Krailling, Germany. [Doitsidis, Lefteris] Technol Educ Inst Crete, Khania 73100, Greece. [Fraundorfer, Friedrich] Tech Univ Munich, D-80333 Munich, Germany. [Kosmatopoulos, Elias; Chatzichristofis, Savvas] Democritus Univ Thrace, GR-67100 Xanthi, Greece. [Kosmatopoulos, Elias; Chatzichristofis, Savvas] ITI CERTH, Xanthi 67100, Greece. [Martinelli, Agostino] INRIA Grenoble Rhone Alpes, F-38334 Grenoble, France. [Achtelik, Markus W.] ETH, Autonomous Syst Lab, CH-8092 Zurich, Switzerland. [Chli, Margarita] Univ Edinburgh, Edinburgh EH8 9AB, Midlothian, Scotland. [Kneip, Laurent] Australian Natl Univ, Canberra, ACT 0200, Australia. [Heng, Lionel; Lynen, Simon; Meier, Lorenz; Siegwart, Roland; Tanskanen, Petri] ETH, CH-8092 Zurich, Switzerland. [Lee, Gim Hee] ETH, CH-8051 Zurich, Switzerland. [Pollefeys, Marc] ETH, CH-8006 Zurich, Switzerland. [Renzaglia, Alessandro] Univ Minnesota, Minneapolis, MN 55455 USA. [Troiani, Chiara] INRIA Rhone Alpes, F-38334 Grenoble, France. [Weiss, Stephan] NASA Jet Prop Lab, Pasadena, CA 91109 USA. [Weiss, Stephan] CALTECH, Pasadena, CA 91109 USA. RP Scaramuzza, D (reprint author), Univ Zurich, CH-8050 Zurich, Switzerland. EM davide.scaramuzza@ieee.org; michael@achtelik.net; ldoitsidis@chania.teicrete.gr; friedrich.fraundorfer@tum.de; kosmatop@dssl.tuc.gr; agostino.martinelli@inria.fr; markus.achtelik@mavt.ethz.ch; margarita.chli@mavt.ethz.ch; schatzic@ee.duth.gr; laurent.kneip@anu.edu.au; daniel@gurdan.de; hengli@inf.ethz.ch; lgimhee@gmail.com; simon.lynen@mavt.ethz.ch; lm@inf.ethz.ch; marc.pollefeys@inf.ethz.ch; a.renzaglia@gmail.com; rsiegwart@ethz.ch; jan@asctec.de; tpetri@student.ethz.ch; chiara.troiani@inrialpes.fr; stephan.weiss@ieee.org RI Lee, Gim Hee/K-5241-2015; OI Kneip, Laurent/0000-0001-6727-6608 NR 58 TC 35 Z9 35 U1 5 U2 50 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1070-9932 EI 1558-223X J9 IEEE ROBOT AUTOM MAG JI IEEE Robot. Autom. Mag. PD SEP PY 2014 VL 21 IS 3 BP 26 EP 40 DI 10.1109/MRA.2014.2322295 PG 15 WC Automation & Control Systems; Robotics SC Automation & Control Systems; Robotics GA AP4YW UT WOS:000342087700007 ER PT J AU Giangrande, SE Collis, S Theisen, AK Tokay, A AF Giangrande, Scott E. Collis, Scott Theisen, Adam K. Tokay, Ali TI Precipitation Estimation from the ARM Distributed Radar Network during the MC3E Campaign SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID MESOSCALE CONVECTIVE SYSTEMS; DUAL-POLARIZATION RADAR; X-BAND; DIFFERENTIAL PHASE; C-BAND; RAINFALL ESTIMATION; POLARIMETRIC RADAR; WEATHER RADAR; ERROR VARIANCE; PART II AB This study presents radar-based precipitation estimates collected during the 2-month U. S. Department of Energy Atmospheric Radiation Measurement Program (ARM)-NASA Midlatitude Continental Convective Clouds Experiment (MC3E). Emphasis is on the usefulness of radar observations from the C-band and X-band scanning ARM precipitation radars (CSAPR and XSAPR, respectively) for rainfall estimation products to distances within 100 km of the Lamont, Oklahoma, ARM facility. The study utilizes a dense collection of collocated ARM, NASA Global Precipitation Measurement, and nearby surface Oklahoma Mesonet gauge records to evaluate radar-based hourly rainfall products and campaign-optimized methods over individual gauges and for areal rainfall characterizations. Rainfall products are also evaluated against the performance of a regional NWS Weather Surveillance Radar-1988 Doppler (WSR-88D) S-band dual-polarization radar product. Results indicate that the CSAPR system may achieve similar point-and areal-gauge bias and root-mean-square (RMS) error performance to a WSR-88D reference for the variety of MC3E deep convective events sampled. The best campaign rainfall performance was achieved when using radar relations capitalizing on estimates of the specific attenuation from the CSAPR system. The XSAPRs demonstrate limited capabilities, having modest success in comparison with the WSR-88D reference for hourly rainfall accumulations that are under 10mm. All rainfall estimation methods exhibit a reduction by a factor of 1.5-2.5 in RMS errors for areal accumulations over a 15-km(2) NASA dense gauge network, with the smallest errors typically associated with dual-polarization radar methods. C1 [Giangrande, Scott E.] Brookhaven Natl Lab, Div Atmospher Sci, Upton, NY 11973 USA. [Collis, Scott] Argonne Natl Lab, Div Environm Sci, Argonne, IL 60439 USA. [Theisen, Adam K.] Univ Oklahoma, Cooperat Inst Mesoscale Meteorol Studies, Atmospher Radiat Measurement Program, Data Qual Off, Norman, OK 73019 USA. [Tokay, Ali] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. [Tokay, Ali] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Giangrande, SE (reprint author), Brookhaven Natl Lab, Div Atmospher Sci, Bldg 490D,Bell Ave, Upton, NY 11973 USA. EM scott.giangrande@bnl.gov RI Measurement, Global/C-4698-2015; Giangrande, Scott/I-4089-2016 OI Giangrande, Scott/0000-0002-8119-8199 FU Brookhaven Science Associates, LLC [DE-AC02-98CH10886]; U.S. Department of Energy; Climate Science for a Sustainable Energy Future (CSSEF) project of the Earth System Modeling (ESM) program in the DOE Office of Science; U.S. Department of Energy Office of Science, Office of Biological and Environmental Research (OBER) [DE-AC02-06CH11357]; OBER of the DOE as part of the ARM Program; Battelle-Pacific Northwest National Laboratory [206248]; NOAA/Office of Oceanic and Atmospheric Research under U.S. Department of Commerce NOAA-University of Oklahoma [NA11OAR4320072] FX This paper has been authored by employees of Brookhaven Science Associates, LLC, under Contract DE-AC02-98CH10886 with the U.S. Department of Energy. The publisher by accepting the paper for publication acknowledges that the U.S. government retains a nonexclusive, paid-up, irrevocable, worldwide license to publish or reproduce the published form of this paper, or to allow others to do so, for U.S. government purposes. Author Giangrande's work is supported by the Climate Science for a Sustainable Energy Future (CSSEF) project of the Earth System Modeling (ESM) program in the DOE Office of Science. Argonne National Laboratory's work was supported by the U.S. Department of Energy Office of Science, Office of Biological and Environmental Research (OBER), under Contract DE-AC02-06CH11357. The work has been supported by the OBER of the DOE as part of the ARM Program. Adam Theisen's work was supported by Battelle-Pacific Northwest National Laboratory, Contract 206248, and his home institution CIMMS is supported by NOAA/Office of Oceanic and Atmospheric Research under U.S. Department of Commerce NOAA-University of Oklahoma Cooperative Agreement NA11OAR4320072. The authors thank Dr. Alexander Ryzhkov for support on implementation of specific-attenuation-based rainfall methods, associated comments, and considerations. We thank Michael Jensen of BNL, Virendra Ghate of ANL, and Randy Peppler of OU-CIMMS for internal reviews of this manuscript. NR 63 TC 9 Z9 9 U1 1 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD SEP PY 2014 VL 53 IS 9 BP 2130 EP 2147 DI 10.1175/JAMC-D-13-0321.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AP3ZY UT WOS:000342017800003 ER PT J AU Shuman, CA Hall, DK DiGirolamo, NE Mefford, TK Schnaubelt, MJ AF Shuman, Christopher A. Hall, Dorothy K. DiGirolamo, Nicolo E. Mefford, Thomas K. Schnaubelt, Michael J. TI Comparison of Near-Surface Air Temperatures and MODIS Ice-Surface Temperatures at Summit, Greenland (2008-13) SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID POLAR PATHFINDER DATASET; CLOUD DETECTION; ANTARCTIC PLATEAU; ARCTIC SURFACE; ABLATION ZONE; PART II; SHEET; MELT; SATELLITE; CLIMATE AB The stability of the Moderate Resolution Imaging Spectroradiometer (MODIS) ice-surface temperature (IST) product from Terra was investigated for use as a climate-quality data record. The availability of climate-quality air temperature data T-A from a NOAA observatory at Greenland's Summit Station has enabled this high-temporal-resolution study of MODIS ISTs. During a > 5-yr period (July 2008-August 2013), more than 2500 IST values were compared with +/- 3-min-average T-A values from NOAA's primary 2-m temperature sensor. This enabled an expected small offset between air and ice-sheet surface temperatures (T-A > IST) to be investigated over multiple annual cycles. The principal findings of this study show 1) that IST values are slightly colder than the T-A values near freezing but that this offset increases as temperature decreases and 2) that there is a pattern in IST-T-A differences as the solar zenith angle (SoZA) varies annually. This latter result largely explains the progressive offset from the in situ data at colder temperatures but also indicates that the MODIS cloud mask is less accurate approaching and during the polar night. The consistency of the results over each year in this study indicates that MODIS provides a platform for remotely deriving surface temperature data, with the resulting IST data being most compatible with in situ T-A data when the sky is clear and the SoZA is less than similar to 85 degrees. The ongoing development of the IST dataset should benefit from improved cloud filtering as well as algorithm modifications to account for the progressive offset from T-A at colder temperatures. C1 [Shuman, Christopher A.; Schnaubelt, Michael J.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Greenbelt, MD 20771 USA. [Shuman, Christopher A.; DiGirolamo, Nicolo E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hall, Dorothy K.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [DiGirolamo, Nicolo E.] Sci Syst & Applicat Inc, Greenbelt, MD USA. [Mefford, Thomas K.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Mefford, Thomas K.] NOAA, Earth Syst Res Lab, Boulder, CO USA. RP Shuman, CA (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Code 615, Greenbelt, MD 20771 USA. EM christopher.a.shuman@nasa.gov FU NASA's Cryospheric Sciences Program FX The authors thank the support staff at the Greenland Summit Station for helping to provide the in situ data necessary for this study. The TA data were derived from NOAA's Earth System Research Laboratory Global Monitoring Division datasets. NASA's Cryospheric Sciences Program provided funding for the MODIS IST dataset as well as the work performed at NASA Goddard Space Flight Center (GSFC) and at University of Maryland, Baltimore County. Jack Xiong and Brian Wenny of the MODIS Characterization and Support Team at GSFC and George Riggs (Science Systems and Applications, Inc., at GSFC), provided additional insights on the IST data and MODIS products. We thank the editor and three anonymous reviewers for their comments and guidance that improved the final paper. NR 39 TC 5 Z9 5 U1 1 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD SEP PY 2014 VL 53 IS 9 BP 2171 EP 2180 DI 10.1175/JAMC-D-14-0023.1 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AP3ZY UT WOS:000342017800006 ER PT J AU Kelley, OA AF Kelley, Owen A. TI Where the Least Rainfall Occurs in the Sahara Desert, the TRMM Radar Reveals a Different Pattern of Rainfall Each Season SO JOURNAL OF CLIMATE LA English DT Article ID WEST-AFRICA; PRECIPITATION RADAR; CLIMATE-CHANGE; LAND-SURFACE; VARIABILITY; SATELLITE; MODEL; SYSTEMS; OCEAN; CLASSIFICATION AB Some previous studies were unable to detect seasonal organization to the rainfall in the Sahara Desert, while others reported seasonal patterns only in the less-arid periphery of the Sahara. In contrast, the precipitation radar on the Tropical Rainfall Measuring Mission (TRMM) satellite detects four rainy seasons in the part of the Sahara where the TRMM radar saw the least rainfall during a 15-yr period (1998-2012). According to the TRMM radar, approximately 20 degrees-27 degrees N, 22 degrees-32 degrees E is the portion of the Sahara that has the lowest average annual rain accumulation (1-5 mm yr(-1)). Winter (January and February) has light rain throughout this region but more rain to the north over the Mediterranean Sea. Spring (April and May) has heavier rain and has lightning observed by the TRMM Lightning Imaging Sensor (LIS). Summer rain and lightning (July and August) occur primarily south of 23 degrees N. At a maximum over the Red Sea, autumn rain and lightning (October and November) can be heavy in the northeastern portion of the study area, but these storms are unreliable: that is, the TRMM radar detects such storms in only 6 of the 15 years. These four rainy seasons are each separated by a comparatively drier month in the monthly rainfall climatology. The few rain gauges in this arid region broadly agree with the TRMM radar on the seasonal organization of rainfall. This seasonality is reason to reevaluate the idea that Saharan rainfall is highly irregular and unpredictable. C1 [Kelley, Owen A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kelley, Owen A.] George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. RP Kelley, OA (reprint author), NASA, Goddard Space Flight Ctr, Code 610-2, Greenbelt, MD 20771 USA. EM owen.kelley@nasa.gov FU NASA METS-II [NNG10CR16C] FX This work was supported by the NASA METS-II Contract NNG10CR16C. The Precipitation Processing System (PPS) at NASA Goddard Space Flight Center provided computational facilities. The staff of the NASA Goddard Library located hard-to-find documents and datasets. The following people provided suggestions for improving the manuscript: Jeanne Beatty, Michael Chesnes, George Huffman, Genevieve Demos Kelley, Erich Stocker, John Stout, Clifton Sutton, and three anonymous reviewers. NR 85 TC 3 Z9 3 U1 2 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD SEP PY 2014 VL 27 IS 18 BP 6919 EP 6939 DI 10.1175/JCLI-D-14-00145.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AP3NC UT WOS:000341981800005 ER PT J AU Blaber, EA Dvorochkin, N Torres, ML Yousuf, R Burns, BP Globus, RK Almeida, EAC AF Blaber, E. A. Dvorochkin, N. Torres, M. L. Yousuf, R. Burns, B. P. Globus, R. K. Almeida, E. A. C. TI Mechanical unloading of bone in microgravity reduces mesenchymal and hematopoietic stem cell-mediated tissue regeneration SO STEM CELL RESEARCH LA English DT Article ID RED-BLOOD-CELL; EPIDERMAL-GROWTH-FACTOR; OSTEOCLAST DIFFERENTIATION; SPACE-FLIGHT; OSTEOBLAST DIFFERENTIATION; SIMULATED MICROGRAVITY; MUSCULOSKELETAL DISUSE; PRESSURE-GRADIENTS; CANCELLOUS BONE; GENE-EXPRESSION AB Mechanical loading of mammalian tissues is a potent promoter of tissue growth and regeneration, whilst unloading in microgravity can cause reduced tissue regeneration, possibly through effects on stem cell tissue progenitors. To test the specific hypothesis that mechanical unloading alters differentiation of bone marrow mesenchymal and hematopoietic stem cell lineages, we studied cellular and molecular aspects of how bone marrow in the mouse proximal femur responds to unloading in microgravity. Trabecular and cortical endosteal bone surfaces in the femoral head underwent significant bone resorption in microgravity, enlarging the marrow cavity. Cells isolated from the femoral head marrow compartment showed significant down-regulation of gene expression markers for early mesenchymal and hematopoietic differentiation, including FUT1(-6.72), CSF2(-3.30), CD90(-3.33), PTPRC(-2.79), and GDF15(-2.45), but not stem cell markers, such as SOX2. At the cellular level, in situ histological analysis revealed decreased megakaryocyte numbers whilst erythrocytes were increased 2.33 fold. Furthermore, erythrocytes displayed elevated fucosylation and clustering adjacent to sinuses forming the marrow-blood barrier, possibly providing a mechanistic basis for explaining spaceflight anemia. Culture of isolated bone marrow cells immediately after microgravity exposure increased the marrow progenitor's potential for mesenchymal differentiation into in-vitro mineralized bone nodules, and hematopoietic differentiation into osteoclasts, suggesting an accumulation of undifferentiated progenitors during exposure to microgravity. These results support the idea that mechanical unloading of mammalian tissues in microgravity is a strong inhibitor of tissue growth and regeneration mechanisms, acting at the level of early mesenchymal and hematopoietic stem cell differentiation. Published by Elsevier B. V. C1 [Blaber, E. A.; Burns, B. P.] Univ New S Wales, Sch Biotechnol & Bimol Sci, Sydney, NSW, Australia. [Blaber, E. A.; Dvorochkin, N.; Torres, M. L.; Yousuf, R.; Globus, R. K.; Almeida, E. A. C.] NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA. [Torres, M. L.] Santa Clara Univ, Dept Bioengn, Santa Clara, CA 95053 USA. RP Almeida, EAC (reprint author), NASA, Ames Res Ctr, Mail Stop 236-7, Moffett Field, CA 94035 USA. EM e.almeida@nasa.gov OI BURNS, BRENDAN/0000-0002-2962-2597 NR 97 TC 10 Z9 10 U1 1 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1873-5061 EI 1876-7753 J9 STEM CELL RES JI Stem Cell Res. PD SEP PY 2014 VL 13 IS 2 BP 181 EP 201 DI 10.1016/j.scr.2014.05.005 PG 21 WC Cell & Tissue Engineering; Biotechnology & Applied Microbiology; Cell Biology SC Cell Biology; Biotechnology & Applied Microbiology GA AP7WB UT WOS:000342287400001 PM 25011075 ER PT J AU Chen, BY Pinho, ST De Carvalho, NV Baiz, PM Tay, TE AF Chen, B. Y. Pinho, S. T. De Carvalho, N. V. Baiz, P. M. Tay, T. E. TI A floating node method for the modelling of discontinuities in composites SO ENGINEERING FRACTURE MECHANICS LA English DT Article DE Composites; Phantom node method; X-FEM; Multiple cracks; Crack interaction ID FINITE-ELEMENT-METHOD; 3-DIMENSIONAL CRACK INITIATION; FIBER-REINFORCED COMPOSITES; POSTERIORI ERROR ESTIMATION; DEFORMABLE SHALLOW SHELLS; AUTOMATIC MESH GENERATOR; COHESIVE SEGMENTS METHOD; THIN-WALLED STRUCTURES; ANALYSES SGBEM-FEM; LEVEL SETS AB This paper presents a new method suitable for modelling multiple discontinuities within a finite element. The architecture of the proposed method is similar to that of the phantom node method (which is equivalent to XFEM with Heaviside enrichment), and the solution of it is equivalent to local remeshing within the cracked element. The new method shows several advantages over the phantom node method, such as avoiding errors in the mapping of the crack geometry from the physical to the natural space and avoiding performing integrations over only part of an element. Compared to remeshing, the proposed method enables the representation of discontinuities through relatively closed FE codes (such as user-defined elements) without modifying the initial mesh and geometry, thus making it computationally more efficient. Additionally, the proposed method is particularly suited for modelling weak and cohesive discontinuities and for the representation of complex crack networks; it can model multiple plies and interfaces of a composite laminate, and both matrix crack and delamination, within a user-defined element; the information is shared between the plies and interfaces within such an element, allowing the direct implementation of interactive mechanisms. Verification examples show that the floating node method can predict stress intensity factors and crack propagation accurately. An application example shows that the proposed method can predict well the transition from matrix cracking to delamination and the subsequent saturation of matrix crack density in a c ross-ply laminate. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Chen, B. Y.; Tay, T. E.] Natl Univ Singapore, Dept Mech Engn, Singapore 119077, Singapore. [Chen, B. Y.; Pinho, S. T.; Baiz, P. M.] Univ London Imperial Coll Sci Technol & Med, Dept Aeronaut, London SW7 2AZ, England. [De Carvalho, N. V.] NASA, Langley Res Ctr, Natl Inst Aerosp, Hampton, VA 23665 USA. RP Chen, BY (reprint author), Block EA,02-21,9 Engn Dr 1, Singapore 117576, Singapore. EM boyang.chen@nus.edu.sg RI Pinho, Silvestre/B-4618-2012; Chen, Boyang/J-1271-2016; OI Chen, Boyang/0000-0001-7393-4363; Tay, Tong-Earn/0000-0002-2846-1947 FU National University of Singapore FX The first author greatly acknowledges the research scholarship from National University of Singapore. NR 134 TC 15 Z9 15 U1 2 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0013-7944 EI 1873-7315 J9 ENG FRACT MECH JI Eng. Fract. Mech. PD SEP PY 2014 VL 127 BP 104 EP 134 DI 10.1016/j.engfracmech.2014.05.018 PG 31 WC Mechanics SC Mechanics GA AO7SA UT WOS:000341551700010 ER PT J AU Siljestrom, S Freissinet, C Goesmann, F Steininger, H Goetz, W Steele, A Amundsen, H AF Siljestrom, Sandra Freissinet, Caroline Goesmann, Fred Steininger, Harald Goetz, Walter Steele, Andrew Amundsen, Hans CA AMASE11 Team TI Comparison of Prototype and Laboratory Experiments on MOMA GCMS: Results from the AMASE11 Campaign SO ASTROBIOLOGY LA English DT Article DE MOMA; ExoMars; Pyrolysis-GCMS; Derivatization; Svalbard; AMASE ID CHROMATOGRAPHY-MASS-SPECTROMETRY; ALLAN HILLS 84001; MARTIAN METEORITE ALH84001; ROCKNEST AEOLIAN DEPOSIT; MARS-LIKE SOILS; ORGANIC-COMPOUNDS; OMEGA/MARS EXPRESS; DESERT VARNISH; LIFE-DETECTION; FOSSIL LEAVES AB The characterization of any organic molecules on Mars is a top-priority objective for the ExoMars European Space Agency-Russian Federal Space Agency joint mission. The main instrument for organic analysis on the ExoMars rover is the Mars Organic Molecule Analyzer (MOMA). In preparation for the upcoming mission in 2018, different Mars analog samples are studied with MOMA and include samples collected during the Arctic Mars Analog Svalbard Expedition (AMASE) to Svalbard, Norway. In this paper, we present results obtained from two different Mars analog sites visited during AMASE11, Colletthogda and Botniahalvoya. Measurements were performed on the samples during AMASE11 with a MOMA gas chromatograph (GC) prototype connected to a commercial mass spectrometer (MS) and later in home institutions with commercial pyrolysis-GCMS instruments. In addition, derivatization experiments were performed on the samples during AMASE11 and in the laboratory. Three different samples were studied from the Colletthogda that included one evaporite and two carbonate-bearing samples. Only a single sample was studied from the Botniahalvoya site, a weathered basalt covered by a shiny surface consisting of manganese and iron oxides. Organic molecules were detected in all four samples and included aromatics, long-chained hydrocarbons, amino acids, nucleobases, sugars, and carboxylic acids. Both pyrolysis and derivatization indicated the presence of extinct biota by the detection of carboxylic acids in the samples from Colletthogda, while the presence of amino acids, nucleobases, carboxylic acids, and sugars indicated an active biota in the sample from Botniahalvoya. The results obtained with the prototype flight model in the field coupled with repeat measurements with commercial instruments within the laboratory were reassuringly similar. This demonstrates the performance of the MOMA instrument and validates that the instrument will aid researchers in their efforts to answer fundamental questions regarding the speciation and possible source of organic content on Mars. C1 [Siljestrom, Sandra] SP Tech Res Inst Sweden, Dept Chem Mat & Surfaces, S-50115 Boras, Sweden. [Siljestrom, Sandra; Steele, Andrew] Carnegie Inst Sci, Geophys Lab, Washington, DC USA. [Freissinet, Caroline] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Freissinet, Caroline] Oak Ridge Associated Univ, NASA Postdoctoral Program NPP, Oak Ridge, TN USA. [Goesmann, Fred; Steininger, Harald; Goetz, Walter] Max Planck Inst Sonnensyst Forsch, Gottingen, Germany. [Amundsen, Hans] Earth & Planetary Explorat Serv, Oslo, Norway. RP Siljestrom, S (reprint author), SP Tech Res Inst Sweden, Dept Chem Mat & Surfaces, Box 587, S-50115 Boras, Sweden. EM sandra.siljestrom@sp.se FU AMASE by ESA; Deutsches Zentrum fur Luft- und Raumfahrt (DLR) [FKZ: 50QX1001]; MPS; Swedish National Space Board; Deep Carbon Observatory (A. Steele, PI); program of the Geophysical Laboratory, Carnegie Institution of Washington; Swedish National Space Board [121/11]; GSFC; NASA ASTEP (A. Steele, PI) FX The financial support of AMASE by ESA is gratefully acknowledged. The participation of F. G. was supported by Deutsches Zentrum fur Luft- und Raumfahrt (DLR; FKZ: 50QX1001). The participation of S. S. in AMASE11 was supported by MPS and a Swedish National Space Board travel grant. S. S. was further supported by the Deep Carbon Observatory (A. Steele, PI), the postdoctoral fellowship program of the Geophysical Laboratory, Carnegie Institution of Washington, and the Swedish National Space Board (Contract No. 121/11). The participation of C. F. was supported by GSFC. AMASE11 was strongly supported by NASA ASTEP (A. Steele, PI). NR 89 TC 2 Z9 2 U1 5 U2 30 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD SEP PY 2014 VL 14 IS 9 BP 780 EP 797 DI 10.1089/ast.2014.1197 PG 18 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AP1GM UT WOS:000341815900004 PM 25238325 ER PT J AU Heller, R Williams, D Kipping, D Limbach, MA Turner, E Greenberg, R Sasaki, T Bolmont, E Grasset, O Lewis, K Barnes, R Zuluaga, JI AF Heller, Rene Williams, Darren Kipping, David Limbach, Mary Anne Turner, Edwin Greenberg, Richard Sasaki, Takanori Bolmont, Emeline Grasset, Olivier Lewis, Karen Barnes, Rory Zuluaga, Jorge I. TI Formation, Habitability, and Detection of Extrasolar Moons SO ASTROBIOLOGY LA English DT Review DE Astrobiology; Extrasolar planets; Habitability; Planetary science; Tides ID TRANSIT TIMING VARIATIONS; TIME-SERIES PHOTOMETRY; SOLAR-LIKE STARS; GIANT PLANETS; GALILEAN SATELLITES; LIGHT CURVES; SOUTH-POLE; REGULAR SATELLITES; TIDAL DISSIPATION; SUBSURFACE OCEAN AB The diversity and quantity of moons in the Solar System suggest a manifold population of natural satellites exist around extrasolar planets. Of peculiar interest from an astrobiological perspective, the number of sizable moons in the stellar habitable zones may outnumber planets in these circumstellar regions. With technological and theoretical methods now allowing for the detection of sub-Earth-sized extrasolar planets, the first detection of an extrasolar moon appears feasible. In this review, we summarize formation channels of massive exomoons that are potentially detectable with current or near-future instruments. We discuss the orbital effects that govern exomoon evolution, we present a framework to characterize an exomoon's stellar plus planetary illumination as well as its tidal heating, and we address the techniques that have been proposed to search for exomoons. Most notably, we show that natural satellites in the range of 0.1-0.5 Earth mass (i) are potentially habitable, (ii) can form within the circumplanetary debris and gas disk or via capture from a binary, and (iii) are detectable with current technology. C1 [Heller, Rene] McMaster Univ, Dept Phys & Astron, Origins Inst, Hamilton, ON L8S 4M1, Canada. [Williams, Darren] Penn State Erie, Behrend Coll, Sch Sci, Erie, PA USA. [Kipping, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Limbach, Mary Anne; Turner, Edwin] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Limbach, Mary Anne] Princeton Univ, Dept Mech & Aerosp Engn, Princeton, NJ 08544 USA. [Turner, Edwin] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba, Japan. [Greenberg, Richard] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Sasaki, Takanori] Kyoto Univ, Dept Astron, Kyoto, Japan. [Bolmont, Emeline] Univ Bordeaux, LAB, UMR 5804, Floirac, France. [Bolmont, Emeline] CNRS, LAB, UMR 5804, Floirac, France. [Grasset, Olivier] Univ Nantes, CNRS, Nantes, France. [Lewis, Karen] Tokyo Inst Technol, Tokyo 152, Japan. [Barnes, Rory] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Barnes, Rory] NASA, Astrobiol Inst, Virtual Planetary Lab, Lead Team, Washington, DC USA. [Zuluaga, Jorge I.] Univ Antioquia, FACom, FCEN, Inst Fis, Medellin, Colombia. RP Heller, R (reprint author), McMaster Univ, Dept Phys & Astron, Origins Inst, Hamilton, ON L8S 4M1, Canada. EM rheller@physics.mcmaster.ca OI Zuluaga, Jorge I./0000-0002-6140-3116 FU Origins Institute at McMaster University; Canadian Astrobiology Training Program, a Collaborative Research and Training Experience Program - Natural Sciences and Engineering Research Council of Canada (NSERC); Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; Global COE Program, "From the Earth to 'Earths,''' MEXT, Japan; JSPS KAKENHI [24740120]; NSF [AST-1108882]; NASA Astrobiology Institute [NNH05ZDA001C]; CODI/UdeA; World Premier International Research Center Initiative, MEXT, Japan FX The helpful comments of two referees are very much appreciated. We thank Alexis Carlotti, Jill Knapp, Matt Mountain, George Rieke, Dave Spiegel, and Scott Tremaine for useful conversations and Ted Stryk for granting permission to use a reprocessed image of Europa. Rene Heller is supported by the Origins Institute at McMaster University and by the Canadian Astrobiology Training Program, a Collaborative Research and Training Experience Program funded by the Natural Sciences and Engineering Research Council of Canada (NSERC). Darren Williams is a member of the Center for Exoplanets and Habitable Worlds, which is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. Takanori Sasaki was supported by a grant for the Global COE Program, "From the Earth to 'Earths,''' MEXT, Japan, and Grant-in-Aid for Young Scientists (B), JSPS KAKENHI Grant Number 24740120. Rory Barnes acknowledges support from NSF grant AST-1108882 and the NASA Astrobiology Institute's Virtual Planetary Laboratory lead team under cooperative agreement no. NNH05ZDA001C. Jorge I. Zuluaga is supported by CODI/UdeA. This research has been supported in part by World Premier International Research Center Initiative, MEXT, Japan. This work has made use of NASA's Astrophysics Data System Bibliographic Services. NR 261 TC 20 Z9 20 U1 4 U2 24 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD SEP PY 2014 VL 14 IS 9 BP 798 EP 835 DI 10.1089/ast.2014.1147 PG 38 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AP1GM UT WOS:000341815900005 PM 25147963 ER PT J AU Ballard, T Seager, R Smerdon, JE Cook, BI Ray, AJ Rajagopalan, B Kushnir, Y Nakamura, J Henderson, N AF Ballard, Tristan Seager, Richard Smerdon, Jason E. Cook, Benjamin I. Ray, Andrea J. Rajagopalan, Balaji Kushnir, Yochanan Nakamura, Jennifer Henderson, Naomi TI Hydroclimate Variability and Change in the Prairie Pothole Region, the "Duck Factory'' of North America SO EARTH INTERACTIONS LA English DT Article DE North America; Climate change; Hydrologic cycle; Climate variability; Ecosystem effects ID WETLANDS; CLIMATE; VULNERABILITY; SURVIVAL; DROUGHT; DAKOTA; ENSO AB The Prairie Pothole Region (PPR) of the northern Great Plains is a vital ecosystem responsible each year for producing 50%-80% of new recruits to the North American duck population. Climate variability and change can impact the hydrology and ecology of the region with implications for waterfowl populations. The historical relationship between PPR wetlands, duck populations, and seasonal hydroclimate are explored. Model experiments from phase 5 of the Coupled Model Intercomparison Project are used to determine whether a recent wetting trend is due to natural variability or changing climate and how PPR hydroclimate will change into the future. Year-to-year variations in May duck populations, pond numbers, and the Palmer drought severity index are well correlated over past decades. Pond and duck numbers tend to increase in spring following La Nina events, but the correlation is not strong. Model simulations suggest that the strengthening of the precipitation gradient across the PPR over the past century is predominantly due to natural variability and therefore could reverse. Model projections of future climate indicate precipitation will increase across the PPR in all seasons except summer, but this gain for surface moisture is largely offset by increased evapotranspiration because of higher temperatures and increased atmospheric evaporative demand. In summer, the combined effects of warming and precipitation changes indicate seasonal surface drying in the future. The presented hydroclimate analyses produce potential inputs to ecological and hydrological simulations of PPR wetlands to inform risk analysis of how this North American waterfowl habitat will evolve in the future, providing guidance to land managers facing conservation decisions. C1 [Ballard, Tristan] Duke Univ, Durham, NC USA. [Seager, Richard; Smerdon, Jason E.; Kushnir, Yochanan; Nakamura, Jennifer; Henderson, Naomi] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Ray, Andrea J.] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Rajagopalan, Balaji] Univ Colorado, Dept Civil Environm & Architectural Engn, Boulder, CO 80309 USA. RP Seager, R (reprint author), Columbia Univ, Lamont Doherty Earth Observ, 61 Route 9W, Palisades, NY 10964 USA. EM seager@ldeo.columbia.edu RI Smerdon, Jason/F-9952-2011; Cook, Benjamin/H-2265-2012; Rajagopalan, Balaji/A-5383-2013 OI Rajagopalan, Balaji/0000-0002-6883-7240 FU NSF [AGS-1243204]; NOAA [NA08OAR4320912]; Lamont summer undergraduate intern program FX This work was supported by NSF Award AGS-1243204 ("Linking near-term future changes in weather and hydroclimate in western North America to adaptation for ecosystem and water management") and NOAA Award NA08OAR4320912 ("Global decadal hydroclimate variability and change"). We particularly thank Susan Skagen (U.S. Geological Survey), Michael Olson and Richard Nelson (U.S. Fish and Wildlife Service), and Helen Sofaer (Colorado State University) for their careful readings, which led to a more informative and practically useful paper. TB acknowledges the Lamont summer undergraduate intern program for additional support. We thank Haibo Liu for assembling the CMIP5 model database at Lamont. We thank two anonymous reviewers for detailed and thoughtful comments and criticisms. The authors declare no conflicts of interest. NR 36 TC 6 Z9 6 U1 4 U2 43 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1087-3562 J9 EARTH INTERACT JI Earth Interact. PD SEP PY 2014 VL 18 AR 14 DI 10.1175/EI-D-14-0004.1 PG 28 WC Geosciences, Multidisciplinary SC Geology GA AP1GI UT WOS:000341815500001 ER PT J AU Yau, AJ Lenihan, HS Kendall, BE AF Yau, Annie J. Lenihan, Hunter S. Kendall, Bruce E. TI Fishery management priorities vary with self-recruitment in sedentary marine populations SO ECOLOGICAL APPLICATIONS LA English DT Article DE closed population; coral reef fishery; fishing mortality; giant clam; integral projection model; local population; mixed recruitment; Mo'orea, French Polynesia; open population; self-recruitment; small-scale fishery; Tridacna ID CORAL-REEF FISHERIES; GIANT CLAMS; LARVAL CONNECTIVITY; DENSITY-DEPENDENCE; TRIDACNA-CROCEA; MAXIMA; MODEL; GROWTH; SUSTAINABILITY; ARCHIPELAGO AB Fisheries science often uses population models that assume no external recruitment, but nearshore marine populations harvested on small scales of <200 km often exhibit an unknown mix of self-recruitment and recruitment from external sources. Since empirical determination of self-recruitment vs. external recruitment is difficult, we used a modeling approach to examine the sensitivity of fishery management priorities to recruitment assumptions (self [closed], external [open]) in a local population of harvested giant clams (Tridacna maxima) on Mo'orea, French Polynesia. From 2006 to 2010, we measured growth, fecundity, recruitment, and survival (resulting from natural and fishing mortality). We used these data to parameterize both a closed (complete self-recruitment) and an open (no self-recruitment) integral projection model (IPM), and then calculated elasticities of demographic rates (growth, survival, recruitment) to future population abundance in 20 years. The models' lowest projected abundance was 93.4% (95% CI, [86.5%, 101.8%]) of present abundance, if the local population is entirely open and the present level of fishing mortality persists. The population will exhibit self-sustaining dynamics (1 <= lambda <= 1.07) as for a closed population if the ratio of self-recruits per gram of dry gonad is >0.775 (equivalent to 52.85% self-recruitment under present conditions). Elasticity analysis of demographic parameters indicated that future abundance can most effectively be influenced by increasing survival of mid-sized clams (similar to 80-120 mm) if the population is self-sustaining, and by increasing survival of juvenile clams (similar to 40-70 mm) if the population is non-self-sustaining (as for an open population). Our results illustrate that management priorities can vary depending on the amount of self-recruitment in a local population. C1 [Yau, Annie J.; Lenihan, Hunter S.; Kendall, Bruce E.] Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA. RP Yau, AJ (reprint author), NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA. EM annie.yau@noaa.gov RI Kendall, Bruce/C-1871-2008 OI Kendall, Bruce/0000-0003-1782-8106 FU Gump Research Station Pacific Education and Research Laboratories (PEARL) Award; PADI Foundation [317]; Luce Science to Solutions Fellowship; Mo'orea Coral Reef (MCR) Long Term Ecological Research Site; Bren School of Environmental Science and Management; University of California FX This research was supported by grants to A. Yau from the Gump Research Station Pacific Education and Research Laboratories (PEARL) Award, PADI Foundation grant number 317, and the Luce Science to Solutions Fellowship. Additional support came from the Mo'orea Coral Reef (MCR) Long Term Ecological Research Site, the Bren School of Environmental Science and Management, and the University of California. This is a contribution of the MCR LTER Site and Contribution Number 195 of the UC Berkeley Gump Research Station. We thank R. Nisbet and J. Wilson for their input and helpful comments that improved earlier versions of the manuscript. We thank the staff of the Gump Station for their assistance and friendship. We are grateful to T. Adam, A. Brooks, X. Han, K. Seydel, H. Stewart, and K. Walovich for their efforts in collecting shells. Finally, we thank L. Albertson, J. Creason, T. Minter, A. Rivera, S. Shaffiy, and T. Teore for their assistance with fieldwork, all the fishers for their knowledge on pahua fishing and participation in this study, and the Brando Trust, Conservation Tetiaroa, and Pacific Beachcomber for permission to work on Tetiaroa. NR 63 TC 3 Z9 3 U1 1 U2 31 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1051-0761 EI 1939-5582 J9 ECOL APPL JI Ecol. Appl. PD SEP PY 2014 VL 24 IS 6 BP 1490 EP 1504 PG 15 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA AO9YE UT WOS:000341715800018 ER PT J AU Sujidkul, T Smith, CE Ma, ZJ Morscher, GN Xia, ZH AF Sujidkul, Thanyawalai Smith, Craig E. Ma, Zhijun Morscher, Gregory N. Xia, Zhenhai TI Correlating Electrical Resistance Change with Mechanical Damage in Woven SiC/SiC Composites: Experiment and Modeling SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY LA English DT Article ID DEPENDENT MATRIX CRACKING; CERAMIC COMPOSITES; CFRP COMPOSITES; ACCUMULATION; RESISTIVITY; BEHAVIOR; FAILURE AB Silicon carbide (SiC) fiber-reinforced SiC matrix composites are inherently multifunctional materials. In addition to their primary function as a structural material, the electric properties of the SiC/SiC composites could be used for the sensing and monitoring of in situ damage nucleation and evolution. To detect damage and use that information to further predict the useful life of a particular component, it is necessary to establish the relationship between damage and electrical resistance change. Here, two typical SiC/SiC composites, melt infiltrated (MI), and chemical vapor infiltrated (CVI) woven SiC/SiC composites, were tested to establish the relationship between the electrical response and mechanical damage in unload-reload tensile hysteresis tests. Compared to the 55% resistance increase seen for CVI composites, the MI SiC/SiC composites exhibit a maximum resistance change in 450% in response to mechanical loading (damage), which is the highest sensitivity known among various composites. An analytic model accounting for fiber breakage and matrix cracks was developed to link the electrical resistance to mechanical damage in the composites. The predictions from the models agree well with the experimental data for both composites with high and low conductive matrices. The residual resistance change after unloading is also correlated to the loading history by the analytical relationship. This study demonstrates that resistance change is sensitive to damage in a predictable manner and can be used to improve the reliability of damage assessment of SiC/SiC composites. C1 [Sujidkul, Thanyawalai; Morscher, Gregory N.] Univ Akron, Dept Mech Engn, Akron, OH 44325 USA. [Smith, Craig E.] NASA, Glenn Res Ctr, Ohio Aerosp Inst, Ceram Branch, Cleveland, OH 44135 USA. [Ma, Zhijun] Xian Univ Technol, Sch Mat Sci & Engn, Xian, Peoples R China. [Xia, Zhenhai] Univ N Texas, Dept Chem, Dept Mat Sci & Engn, Denton, TX 76203 USA. RP Xia, ZH (reprint author), Univ N Texas, Dept Chem, Dept Mat Sci & Engn, Denton, TX 76203 USA. EM zhenhai.xia@unt.edu FU NASA Glenn Research Center ARMD Hypersonics program [NNX07AN56H]; NSF [CMMI-1212259, CMMI-1266295] FX We would like to thank the NASA Glenn Research Center ARMD Hypersonics program for the support of the graduate student research program under contract NNX07AN56H and the Glenn Research Center Ceramics branch for use of their research facilities. The project is also supported partially by NSF (CMMI-1212259 and CMMI-1266295). NR 26 TC 1 Z9 1 U1 2 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-7820 EI 1551-2916 J9 J AM CERAM SOC JI J. Am. Ceram. Soc. PD SEP PY 2014 VL 97 IS 9 BP 2936 EP 2942 DI 10.1111/jace.13019 PG 7 WC Materials Science, Ceramics SC Materials Science GA AP1JX UT WOS:000341826500037 ER PT J AU Chen, YC Christensen, MW Stephens, GL Seinfeld, JH AF Chen, Yi-Chun Christensen, Matthew W. Stephens, Graeme L. Seinfeld, John H. TI Satellite-based estimate of global aerosol-cloud radiative forcing by marine warm clouds SO NATURE GEOSCIENCE LA English DT Article ID GENERAL-CIRCULATION MODEL; OPTICAL DEPTH; STRATOCUMULUS; ALBEDO; REANALYSIS; ALGORITHM; COVER AB Changes in aerosol concentrations affect cloud albedo and Earth's radiative balance(1). Aerosol radiative forcing from pre-industrial time to the present due to the effect of atmospheric aerosol levels on the micro- and macrophysics of clouds bears the largest uncertainty among external influences on climate change(1). Of all cloud forms, low-level marine clouds exert the largest impact on the planet's albedo(2). For example, a 6% increase in the albedo of global marine stratiform clouds could offset the warming that would result from a doubling of atmospheric CO2 concentrations(3). Marine warm cloud properties are thought to depend on aerosol levels and large-scale dynamic or thermodynamic states(4-6). Here we present a comprehensive analysis of multiple measurements from the A-Train constellation of Earth-observing satellites, to quantify the radiative forcing exerted by aerosols interacting with marine clouds. Specifically, we analyse observations of co-located aerosols and clouds over the world's oceans for the period August 2006-April 2011, comprising over 7.3 million CloudSat single-layer marine warm cloud pixels. We find that thermodynamic conditions-that is, tropospheric stability and humidity in the free troposphere-and the state of precipitation act together to govern the cloud liquid water responses to the presence of aerosols and the strength of aerosol-cloud radiative forcing. C1 [Chen, Yi-Chun; Seinfeld, John H.] CALTECH, Pasadena, CA 91125 USA. [Chen, Yi-Chun; Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Christensen, Matthew W.] Colorado State Univ, Ft Collins, CO 80523 USA. RP Seinfeld, JH (reprint author), CALTECH, Pasadena, CA 91125 USA. EM seinfeld@caltech.edu RI Christensen, Matthew/C-5733-2013 FU Office of Naval Research grant [N00014-14-1-0097] FX This work was supported by Office of Naval Research grant N00014-14-1-0097. NR 29 TC 22 Z9 23 U1 6 U2 29 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD SEP PY 2014 VL 7 IS 9 BP 643 EP 646 DI 10.1038/NGEO2214 PG 4 WC Geosciences, Multidisciplinary SC Geology GA AO8WI UT WOS:000341635600011 ER PT J AU Burton, AS Grunsfeld, S Elsila, JE Glavin, DP Dworkin, JP AF Burton, Aaron S. Grunsfeld, Sarah Elsila, Jamie E. Glavin, Daniel P. Dworkin, Jason P. TI The effects of parent-body hydrothermal heating on amino acid abundances in CI-like chondrites SO POLAR SCIENCE LA English DT Article DE Meteorite; Amino acid; CI chondrite; Aqueous alteration; Thermal metamorphism ID CARBONACEOUS CHONDRITES; THERMAL METAMORPHISM; AQUEOUS ALTERATION; MASS SPECTROMETRY; METEORITES; STABILITY; MURCHISON; CM; DECARBOXYLATION; TEMPERATURES AB We determined the amino acid abundances and enantiomeric compositions of the Antarctic CI1 carbonaceous chondrites Yamato (Y)-86029 and Y-980115, as well as the Ivuna and Orgueil CI1 carbonaceous chondrites by liquid chromatography with fluorescence detection and time-of-flight mass spectrometry. Y-86029 and Y-980115 both show evidence of parent-body heating (500-600 degrees C) in addition to aqueous alteration, while Ivuna and Orgueil only show evidence for aqueous alteration. In contrast to Ivuna and Orgueil, which each contain similar to 70 nmol/g of amino acids in acid-hydrolyzed, water extracts, both heated Yamato CI meteorites contain only low levels of amino acids that were primarily L-enantiomers of proteinogenic amino acids, indicating that they are likely to be terrestrial in origin. Because indigenous amino acids have been found in meteorites that have experienced metamorphic temperatures of >1000 degrees C with only minimal aqueous alteration, heating alone is not sufficient to explain the lack of amino acids in Y-86029 and Y-980115. Rather, our data suggest that the combination of heating and aqueous alteration has a profound destructive effect on amino acids in meteorites. This finding has implications for the origins of amino acids and other molecules in the early evolution of our solar system. Published by Elsevier B.V. and NIPR. C1 [Burton, Aaron S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Burton, Aaron S.; Grunsfeld, Sarah; Elsila, Jamie E.; Glavin, Daniel P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Grunsfeld, Sarah] River Hill High Sch, Clarksville, MD 21029 USA. RP Burton, AS (reprint author), NASA, Lyndon B Johnson Space Ctr, KR,2101 NASA Pkwy, Houston, TX 77058 USA. EM aaron.s.burton@nasa.gov RI Burton, Aaron/H-2212-2011; Elsila, Jamie/C-9952-2012; Glavin, Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012 OI Burton, Aaron/0000-0002-7137-1605; Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997 FU National Aeronautics and Space Administration (NASA) Astrobiology Institute, Goddard Center for Astrobiology; NASA Cosmochemistry Program; Simons Foundation (SCOL) [302497]; NASA Postdoctoral Program at the Goddard Space Flight Center; NASA; Gifted and Talented Education Program of the Howard County Public School System FX We thank the National Institute of Polar Research of Japan for the Yamato meteorite samples, the Natural History Museum of the United Kingdom for the Ivuna sample, and the Musee National of Paris for the sample of Orgueil. J.E.E., D.P.G. and J.P.D. acknowledge funding support from the National Aeronautics and Space Administration (NASA) Astrobiology Institute, the Goddard Center for Astrobiology and the NASA Cosmochemistry Program. This work was also supported in part by a grant from the Simons Foundation (SCOL award 302497 to J.P.D.). A.S.B. acknowledges support from the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. S.G. acknowledges institutional support through the Gifted and Talented Education Program of the Howard County Public School System. NR 47 TC 10 Z9 10 U1 1 U2 18 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1873-9652 EI 1876-4428 J9 POLAR SCI JI Polar Sci. PD SEP PY 2014 VL 8 IS 3 BP 255 EP 263 DI 10.1016/j.polar.2014.05.002 PG 9 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA AP0YW UT WOS:000341793800005 ER PT J AU Numata, K Wu, S Riris, H AF Numata, Kenji Wu, Stewart Riris, Haris TI Fast-switching methane lidar transmitter based on a seeded optical parametric oscillator SO APPLIED PHYSICS B-LASERS AND OPTICS LA English DT Article ID DIFFERENTIAL ABSORPTION LIDAR; ATMOSPHERIC CARBON-DIOXIDE; CO2 COLUMN ABSORPTION; FREQUENCY STABILIZATION; AIRBORNE MEASUREMENTS; LASER; SENSITIVITY; PHASE; SPECTROSCOPY; MODULATION AB We report on our development effort for a trace-gas-sensing lidar transmitter to be used in future Earth-orbiting satellites. Our lidar transmitter is based on an optical parametric oscillator (OPO), whose output wavelength is switched at a rate of 5 kHz across the target line. The OPO cavity length and the seed laser wavelengths are stabilized to molecular and atomic references. We demonstrated the concept of the OPO-based lidar transmitter at 1,651 nm, achieving similar to 300-mu J output energy and < 300-MHz linewidth, which are anticipated to be required for a future methane lidar spaceborne mission. C1 [Numata, Kenji] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Numata, Kenji; Wu, Stewart; Riris, Haris] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Numata, K (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM kenji.numata@nasa.gov FU NASA Advanced Component Technology program FX This research was funded by the NASA Advanced Component Technology program. We would like to thank Dr. Stephan Kawa, Dr. Mark Stephen, Dr. Steven Li, Dr. Jeffrey Chen, Dr. Jim Abshire, and Dr. Michael Krainak for their support throughout the program. We would also like to thank the Earth Science Technology Office (ESTO), the Instrument Incubator Program, and the Goddard Space Flight Center IRAD program. NR 29 TC 7 Z9 7 U1 0 U2 14 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0946-2171 EI 1432-0649 J9 APPL PHYS B-LASERS O JI Appl. Phys. B-Lasers Opt. PD SEP PY 2014 VL 116 IS 4 BP 959 EP 966 DI 10.1007/s00340-014-5783-4 PG 8 WC Optics; Physics, Applied SC Optics; Physics GA AO5FQ UT WOS:000341369600022 ER PT J AU Cordiner, MA Remijan, AJ Boissier, J Milam, SN Mumma, MJ Charnley, SB Paganini, L Villanueva, G Bockelee-Morvan, D Kuan, YJ Chuang, YL Lis, DC Biver, N Crovisier, J Minniti, D Coulson, IM AF Cordiner, M. A. Remijan, A. J. Boissier, J. Milam, S. N. Mumma, M. J. Charnley, S. B. Paganini, L. Villanueva, G. Bockelee-Morvan, D. Kuan, Y-J. Chuang, Y-L. Lis, D. C. Biver, N. Crovisier, J. Minniti, D. Coulson, I. M. TI MAPPING THE RELEASE OF VOLATILES IN THE INNER COMAE OF COMETS C/2012 F6 (LEMMON) AND C/2012 S1 (ISON) USING THE ATACAMA LARGE MILLIMETER/SUBMILLIMETER ARRAY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE comets: individual (C/2012 S1 (ISON), C/2012 F6 (Lemmon)); techniques: interferometric ID O1 HALE-BOPP; C/1995 O1; MOLECULAR OBSERVATIONS; INFRARED WAVELENGTHS; ORGANIC-MOLECULES; EXTENDED SOURCES; FORMALDEHYDE; ORIGIN; POLYOXYMETHYLENE; DEGRADATION AB Results are presented from the first cometary observations using the Atacama Large Millimeter/Submillimeter Array (ALMA), including measurements of the spatially resolved distributions of HCN, HNC, H2CO, and dust within the comae of two comets: C/2012 F6 (Lemmon) and C/2012 S1 (ISON), observed at heliocentric distances of 1.5 AU and 0.54 AU, respectively. These observations (with angular resolution approximate to 0 ''.5), reveal an unprecedented level of detail in the distributions of these fundamental cometary molecules, and demonstrate the power of ALMA for quantitative measurements of the distributions of molecules and dust in the inner comae of typical bright comets. In both comets, HCN is found to originate from (or within a few hundred kilometers of) the nucleus, with a spatial distribution largely consistent with spherically symmetric, uniform outflow. By contrast, the HNC distributions are clumpy and asymmetrical, with peaks at cometocentric radii similar to 500-1000 km, consistent with release of HNC in collimated outflow(s). Compared to HCN, the H2CO distribution in comet Lemmon is very extended. The interferometric visibility amplitudes are consistent with coma production of H2CO and HNC from unidentified precursor material(s) in both comets. Adopting a Haser model, the H2CO parent scale length is found to be a few thousand kilometers in Lemmon and only a few hundred kilometers in ISON, consistent with the destruction of the precursor by photolysis or thermal degradation at a rate that scales in proportion to the solar radiation flux. C1 [Cordiner, M. A.; Milam, S. N.; Mumma, M. J.; Charnley, S. B.; Paganini, L.; Villanueva, G.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Cordiner, M. A.; Paganini, L.; Villanueva, G.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Remijan, A. J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Boissier, J.] IRAM, F-38406 St Martin Dheres, France. [Bockelee-Morvan, D.; Biver, N.; Crovisier, J.] Univ Paris Diderot, CNRS, LEISA, Observ Paris,UPMC, F-92195 Meudon, France. [Kuan, Y-J.; Chuang, Y-L.] Natl Taiwan Normal Univ, Taipei 116, Taiwan. [Kuan, Y-J.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Lis, D. C.] Univ Paris 06, Sorbonne Univ, CNRS, Observ Paris,UMR 8112,LERMA, F-75014 Paris, France. [Lis, D. C.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Minniti, D.] Pontificia Univ Catolica Chile, Santiago, Chile. [Minniti, D.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Coulson, I. M.] Joint Astron Ctr, Hilo, HI 96720 USA. RP Cordiner, MA (reprint author), NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM martin.cordiner@nasa.gov RI Milam, Stefanie/D-1092-2012 OI Milam, Stefanie/0000-0001-7694-4129 FU NASA Astrobiology Institute through the Goddard Center for Astrobiology; NASA's Planetary Atmospheres and Planetary Astronomy Programs; NASA through JPL/Caltech; Basal CATA [PFB-06]; ICM MAS; NSC [99-2112-M-003-003-MY3, 100-2119-M-003-001-MY3] FX This work was supported by the NASA Astrobiology Institute through the Goddard Center for Astrobiology, and NASA's Planetary Atmospheres and Planetary Astronomy Programs. It makes use of the following ALMA data: ADS/JAO. ALMA #2012.A.00020.S and #2012.A.00033.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. D. C. L. is supported by NASA through JPL/Caltech. D. M. is supported by Basal CATA PFB-06 and the ICM MAS. Y.J.K. is supported by NSC grants 99-2112-M-003-003-MY3 and 100-2119-M-003-001-MY3. NR 30 TC 19 Z9 19 U1 1 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2014 VL 792 IS 1 AR L2 DI 10.1088/2041-8205/792/1/L2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4KO UT WOS:000341306900002 ER PT J AU Coutens, A Jorgensen, JK Persson, MV van Dishoeck, EF Vastel, C Taquet, V AF Coutens, A. Jorgensen, J. K. Persson, M. V. van Dishoeck, E. F. Vastel, C. Taquet, V. TI HIGH D2O/HDO RATIO IN THE INNER REGIONS OF THE LOW-MASS PROTOSTAR NGC 1333 IRAS2A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: individual objects (NGC 1333 IRAS2A); ISM: molecules; stars: protostars ID WATER DEUTERIUM FRACTIONATION; SOLAR-TYPE PROTOSTARS; DEUTERATED WATER; HEAVY-WATER; INTERSTELLAR-MEDIUM; CHEMICAL HISTORY; STAR-FORMATION; WARM WATER; MOLECULES; DISKS AB Water plays a crucial role both in the interstellar medium and on Earth. To constrain its formation mechanisms and its evolution through the star formation process, the determination of the water deuterium fractionation ratios is particularly suitable. Previous studies derived HDO/H2O ratios in the warm inner regions of low-mass protostars. We here report a detection of the D2O 1(1,0)-1(0,1) transition toward the low-mass protostar NGC 1333 IRAS2A with the Plateau de Bure interferometer: this represents the first interferometric detection of D2O-and only the second solar-type protostar for which this isotopologue is detected. Using the observations of the HDO 5(4,2)-6(3,3) transition simultaneously detected and three other HDO lines previously observed, we show that the HDO line fluxes are well reproduced with a single excitation temperature of 218 +/- 21 K and a source size of similar to 0 ''.5. The D2O/HDO ratio is similar to(1.2 +/- 0.5) x 10(-2), while the use of previous (H2O)-O-18 observations give an HDO/H2O ratio of similar to(1.7 +/- 0.8) x 10(-3), i.e., a factor of seven lower than the D2O/HDO ratio. These results contradict the predictions of current grain surface chemical models and indicate that either the surface deuteration processes are poorly understood or that both sublimation of grain mantles and water formation at high temperatures (greater than or similar to 230 K) take place in the inner regions of this source. In the second scenario, the thermal desorption of the grain mantles would explain the high D2O/HDO ratio, while water formation at high temperature would explain significant extra production of H2O leading to a decrease of the HDO/H2O ratio. C1 [Coutens, A.; Jorgensen, J. K.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Coutens, A.; Jorgensen, J. K.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark. [Persson, M. V.; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Vastel, C.] Univ Toulouse, UPS OMP, IRAP, F-31062 Toulouse, France. [Vastel, C.] IRAP, CNRS, F-31028 Toulouse 4, France. [Taquet, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. RP Coutens, A (reprint author), Univ Copenhagen, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. EM acoutens@nbi.dk RI Coutens, Audrey/M-4533-2014 OI Coutens, Audrey/0000-0003-1805-3920 FU INSU/CNRS (France); MPG (Germany); IGN (Spain) FX Based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). NR 36 TC 10 Z9 10 U1 3 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2014 VL 792 IS 1 AR L5 DI 10.1088/2041-8205/792/1/L5 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4KO UT WOS:000341306900005 ER PT J AU Kelley, MSP Farnham, TL Bodewits, D Tricarico, P Farnocchia, D AF Kelley, Michael S. P. Farnham, Tony L. Bodewits, Dennis Tricarico, Pasquale Farnocchia, Davide TI A STUDY OF DUST AND GAS AT MARS FROM COMET C/2013 A1 (SIDING SPRING) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE celestial mechanics; comets: individual (C/2013 A1 (Siding Spring)); meteorites, meteors, meteoroids; methods: numerical ID NUCLEUS; ATMOSPHERE; EQUATIONS AB Although the nucleus of comet C/2013 A1 (Siding Spring) will safely pass Mars in 2014 October, the dust in the coma and tail will more closely approach the planet. Using a dynamical model of comet dust, we estimate the impact fluence. Based on our nominal model no impacts are expected at Mars. Relaxing our nominal model's parameters, the fluence is no greater than similar to 10(-7) grains m(-2) for grain radii larger than 10 mu m. Mars-orbiting spacecraft are unlikely to be impacted by large dust grains, but Mars may receive as many as similar to 10(7) grains, or similar to 100 kg of total dust. We also estimate the flux of impacting gas molecules commonly observed in comet comae. C1 [Kelley, Michael S. P.; Farnham, Tony L.; Bodewits, Dennis] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Tricarico, Pasquale] Planetary Sci Inst, Tucson, AZ 85719 USA. [Farnocchia, Davide] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kelley, MSP (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM msk@astro.umd.edu OI Kelley, Michael/0000-0002-6702-7676; Bodewits, Dennis/0000-0002-2668-7248 FU University of Maryland by the NASA JPL Mars Critical Data Products Program FX This research was supported by a contract to the University of Maryland by the NASA JPL Mars Critical Data Products Program. NR 25 TC 15 Z9 15 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2014 VL 792 IS 1 AR L16 DI 10.1088/2041-8205/792/1/L16 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4KO UT WOS:000341306900016 ER PT J AU Pereira, TMD De Pontieu, B Carlsson, M Hansteen, V Tarbell, TD Lemen, J Title, A Boerner, P Hurlburt, N Wulser, JP Martinez-Sykora, J Kleint, L Golub, L McKillop, S Reeves, KK Saar, S Testa, P Tian, H Jaeggli, S Kankelborg, C AF Pereira, T. M. D. De Pontieu, B. Carlsson, M. Hansteen, V. Tarbell, T. D. Lemen, J. Title, A. Boerner, P. Hurlburt, N. Wuelser, J. P. Martinez-Sykora, J. Kleint, L. Golub, L. McKillop, S. Reeves, K. K. Saar, S. Testa, P. Tian, H. Jaeggli, S. Kankelborg, C. TI AN INTERFACE REGION IMAGING SPECTROGRAPH FIRST VIEW ON SOLAR SPICULES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: atmosphere; Sun: chromosphere; Sun: transition region ID OPTICAL TELESCOPE; II SPICULES; K LINES; MG II; IRIS; DYNAMICS; HINODE; CHROMOSPHERE; MISSION; EVENTS AB Solar spicules have eluded modelers and observers for decades. Since the discovery of the more energetic type II, spicules have become a heated topic but their contribution to the energy balance of the low solar atmosphere remains unknown. Here we give a first glimpse of what quiet-Sun spicules look like when observed with NASA's recently launched Interface Region Imaging Spectrograph (IRIS). Using IRIS spectra and filtergrams that sample the chromosphere and transition region, we compare the properties and evolution of spicules as observed in a coordinated campaign with Hinode and the Atmospheric Imaging Assembly. Our IRIS observations allow us to follow the thermal evolution of type II spicules and finally confirm that the fading of Ca II H spicules appears to be caused by rapid heating to higher temperatures. The IRIS spicules do not fade but continue evolving, reaching higher and falling back down after 500-800 s. Ca II H type II spicules are thus the initial stages of violent and hotter events that mostly remain invisible in Ca II H filtergrams. These events have very different properties from type I spicules, which show lower velocities and no fading from chromospheric passbands. The IRIS spectra of spicules show the same signature as their proposed disk counterparts, reinforcing earlier work. Spectroheliograms from spectral rasters also confirm that quiet-Sun spicules originate in bushes from the magnetic network. Our results suggest that type II spicules are indeed the site of vigorous heating (to at least transition region temperatures) along extensive parts of the upward moving spicular plasma. C1 [Pereira, T. M. D.; De Pontieu, B.; Carlsson, M.; Hansteen, V.] Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway. [De Pontieu, B.; Tarbell, T. D.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Wuelser, J. P.; Martinez-Sykora, J.; Kleint, L.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Martinez-Sykora, J.; Kleint, L.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Kleint, L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Golub, L.; McKillop, S.; Reeves, K. K.; Saar, S.; Testa, P.; Tian, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jaeggli, S.; Kankelborg, C.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. RP Pereira, TMD (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway. EM tiago.pereira@astro.uio.no RI Reeves, Katharine/P-9163-2014 FU NSC (Norway); European Research Council [291058]; NASA [NNM07AA01C, NNG09FA40C] FX IRIS is a NASA Small Explorer mission developed and operated by LMSAL with mission operations executed at NASA ARC and major contributions to downlink communications funded by the NSC (Norway). Hinode is a Japanese mission developed by ISAS/JAXA, with the NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated in cooperation with ESA and NSC (Norway). This work was supported by the European Research Council grant No. 291058 and by NASA under contracts NNM07AA01C (Hinode), and NNG09FA40C (IRIS). NR 30 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 SEP 1 PY 2014 VL 792 IS 1 AR L15 DI 10.1088/2041-8205/792/1/L15 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4KO UT WOS:000341306900015 ER PT J AU Landerer, FW Gleckler, PJ Lee, T AF Landerer, Felix W. Gleckler, Peter J. Lee, Tong TI Evaluation of CMIP5 dynamic sea surface height multi-model simulations against satellite observations SO CLIMATE DYNAMICS LA English DT Article DE Sea surface height; CMIP5; GCM skill; Model evaluation; AR5 ID OCEAN CIRCULATION; CLIMATE MODELS; LEVEL CHANGE; VARIABILITY; ATTRIBUTION; PROJECTIONS; PRODUCTS; IMPACT; RISE; FLUX AB We evaluate the representation of dynamic sea surface height (SSH) fields of 33 global coupled models (GCMs) contributed to the fifth phase of the Coupled Model Intercomparison Project (CMIP5). We use observations from satellite altimetry and basic performance metrics to quantify the ability of the GCMs to replicate observed SSH of the time-mean, seasonal cycle, and inter-annual variability patterns. The time-mean SSH representation has markedly improved from CMIP3 to CMIP5, both in terms of overall reduction in root-mean square differences, and in terms of reduced GCM ensemble spread. Biases of the time-mean SSH field in the Indian and Pacific Ocean equatorial regions are consistent with biases in the zonal surface wind stress fields identified with independent measurements. In the Southern Ocean, the latitude of the maximum meridional gradient of the zonal mean SSH CMIP5 models is shifted equatorward, consistent with the GCMs' spatial biases in the maximum of the zonal mean westerly surface wind stress fields. However, while the Southern Ocean SSH gradients correlate well with the maximum Antarctic circumpolar current transports, there is no significant correlation with the maximum zonal mean wind stress amplitudes, consistent with recent findings that the eddy parameterisations in GCMs dominate over wind stress amplitudes in this region. There is considerable spread across the CMIP5 ensemble for the seasonal and interannual SSH variability patterns. Because of the short observational period, the interannual variability patterns depend on the time-period over which they are derived, while no such dependency is found for the time-mean patterns. The model performance metrics for SSH presented here provide insight into GCM shortcoming due to inadequate model physics or processes. While the diagnostics of CMIP5 GCM performance relative to observations reveal that some models are clearly better than others, model performance is sensitive to the spatio-temporal scales chosen. C1 [Landerer, Felix W.; Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Gleckler, Peter J.] Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA USA. RP Landerer, FW (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM felix.w.landerer@jpl.nasa.gov OI Landerer, Felix/0000-0003-2678-095X FU NASA FX We acknowledge the GCM modeling groups, the PCMDI, and the WCRP's Working Group on Coupled Modeling for their roles in making available the WCRP CMIP3 and CMIP5 multimodel data sets. Support of these data sets is provided by the Office of Science, US Department of Energy. FWL's and TL's work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 47 TC 9 Z9 9 U1 1 U2 20 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD SEP PY 2014 VL 43 IS 5-6 BP 1271 EP 1283 DI 10.1007/s00382-013-1939-x PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AO5FR UT WOS:000341369700008 ER PT J AU Boussaha, F Kawamura, J Stern, J Jung-Kubiak, C AF Boussaha, Faouzi Kawamura, Jonathan Stern, Jeffery Jung-Kubiak, Cecile TI 2.7 THz Balanced Waveguide HEB Mixer SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Heterodyne detection; hot electron bolometer; hybrid coupler; silicon micromachining; terahertz (THz) frequency; waveguide ID SIS MIXER AB We report on the development of a waveguide-based balanced superconducting mixer for operation near 2.7 THz. The mixer employs a pair of NbN hot-electron bolometers defined on 6 mu m-thick silicon substrate that follows a 90 degrees hybrid coupler. To produce the critical structures of the coupler and waveguide embedding circuit, we have utilized silicon micromachining techniques based on deep reactive ion etching. Operating near 4.2 K bath temperature, we have measured a minimum uncorrected DSB receiver noise temperature of less than 2000 K using Callen-Welton formula and local oscillator sideband noise rejection better than 13 +/- 3 dB at 2.74 THz. The concept is suitable for building arrays, readily scalable for higher frequencies up 5 THz, and could accommodate other mixer technologies, such as room-temperature Schottky diode mixers. C1 [Boussaha, Faouzi; Kawamura, Jonathan; Stern, Jeffery; Jung-Kubiak, Cecile] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Boussaha, Faouzi] Observ Paris, LERMA CNRS UMR 8112, F-75014 Paris, France. RP Boussaha, F (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Jonathan.h.kawamura@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology; Oak Ridge Associated Universities through the NASA Postdoctoral Program (NPP); National Aeronautics and Space Administration FX This work was supported in part by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration, and partly supported by the Oak Ridge Associated Universities through the NASA Postdoctoral Program (NPP). NR 24 TC 8 Z9 8 U1 4 U2 22 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD SEP PY 2014 VL 4 IS 5 BP 545 EP 551 DI 10.1109/TTHZ.2014.2342507 PG 7 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA AO7YQ UT WOS:000341569400004 ER PT J AU Leal-Sevillano, CA Reck, TJ Chattopadhyay, G Ruiz-Cruz, JA Montejo-Garai, JR Rebollar, JM AF Leal-Sevillano, Carlos A. Reck, Theodore J. Chattopadhyay, Goutam Ruiz-Cruz, Jorge A. Montejo-Garai, Jose R. Rebollar, Jesus M. TI Development of a Wideband Compact Orthomode Transducer for the 180-270 GHz Band SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Orthomode transducer; terahertz; waveguide; wideband AB In this paper, we report the development of a wideband compact orthomode transducer (OMT) for the 180-270 GHz band. The OMT design is based on the classical high performance Boifot waveguide junction and implemented in split-block using high precision CNC milling. The obtained results validate the high performance operation in a 40% fractional bandwidth and constitute a remarkable achievement at this high frequency band. C1 [Leal-Sevillano, Carlos A.; Montejo-Garai, Jose R.; Rebollar, Jesus M.] Univ Politecn Madrid, ETSI Telecomunicac, Dept Electromagnetismo & Teoria Circuitos, E-28040 Madrid, Spain. [Reck, Theodore J.; Chattopadhyay, Goutam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ruiz-Cruz, Jorge A.] Univ Autonoma Madrid, Escuela Politecn Super, E-28049 Madrid, Spain. RP Leal-Sevillano, CA (reprint author), Univ Politecn Madrid, ETSI Telecomunicac, Dept Electromagnetismo & Teoria Circuitos, E-28040 Madrid, Spain. EM caleal@etc.upm.es RI Ruiz-Cruz, Jorge/C-8159-2014 OI Ruiz-Cruz, Jorge/0000-0003-3909-8263 FU Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA; National Aeronautics and Space Administration; Spanish government program [TEC2010-17795]; CONSOLIDER [CSD2008-00068]; Universidad Politecnica de Madrid FX This work was supported by the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, under a contract with the National Aeronautics and Space Administration. This work was supported in part by the Spanish government program under TEC2010-17795, by CONSOLIDER under CSD2008-00068, and by the Universidad Politecnica de Madrid under a Ph.D. grant. NR 10 TC 4 Z9 4 U1 1 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD SEP PY 2014 VL 4 IS 5 BP 634 EP 636 DI 10.1109/TTHZ.2014.2336540 PG 3 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA AO7YQ UT WOS:000341569400017 ER PT J AU Hurwitz, FI Gallagher, M Olin, TC Shave, MK Ittes, MA Olafson, KN Fields, MG Rogers, RB Guo, HQ AF Hurwitz, Frances I. Gallagher, Meghan Olin, Tracy C. Shave, Molly K. Ittes, Marlyssa A. Olafson, Katy N. Fields, Meredith G. Rogers, Richard B. Guo, Haiquan TI Optimization of Alumina and Aluminosilicate Aerogel Structure for High-Temperature Performance SO INTERNATIONAL JOURNAL OF APPLIED GLASS SCIENCE LA English DT Article ID SOL-GEL PROCESS; MULLITE; PHASE; NMR; PRECURSORS; SYSTEM; AL-27; HYDROLYSIS; ALKOXIDES; XEROGELS AB Alumina and aluminosilicate aerogels offer potential for use at temperatures above 700 degrees C, where silica aerogels begin to sinter. Stability of alumina and aluminosilicate pore structures at high temperatures is governed by the starting aerogel structure, which, in turn is controlled by the synthesis route. Structure, morphology, and crystallization behavior are compared for aerogels synthesized from AlCl3 and propylene oxide with those synthesized from a variety of boehmite precursors. The aerogels possessing a crystalline boehmite structure in the as-synthesized condition retained mesoporous structures to temperatures of 1200 degrees C, while the AlCl3-derived aerogels, although exhibiting higher as-synthesized surface areas, crystallized and densified at 980-1005 degrees C. C1 [Hurwitz, Frances I.; Gallagher, Meghan; Olin, Tracy C.; Shave, Molly K.; Ittes, Marlyssa A.; Olafson, Katy N.; Fields, Meredith G.; Rogers, Richard B.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Guo, Haiquan] Ohio Aerosp Inst, Cleveland, OH 44135 USA. RP Hurwitz, FI (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM frances.hurwitz@nasa.gov FU NASA Aeronautics Research and Space Technology Mission Directorates; Radioisotope Power Systems Program; NASA USRP; NASA LERCIP FX The authors wish to acknowledge the late Anna R. Palczer of NASA Glenn Research Center for her many contributions to this work. We wish to thank Dr. Matthew P. Espe and Anna M. Reinsel of the University of Akron for the NMR characterization, Derek F. Johnson of NASA Glenn Research Center for thermal and elemental analysis, and Michael T. Cox of NASA Glenn Research Center for XRD. Thanks as well to Sasol N. A. for donation of the boehmite powders. We also wish to acknowledge funding support from the NASA Aeronautics Research and Space Technology Mission Directorates, the Radioisotope Power Systems Program, and the NASA USRP and LERCIP student internship programs. NR 36 TC 6 Z9 6 U1 7 U2 40 PU WILEY PERIODICALS, INC PI SAN FRANCISCO PA ONE MONTGOMERY ST, SUITE 1200, SAN FRANCISCO, CA 94104 USA SN 2041-1286 EI 2041-1294 J9 INT J APPL GLASS SCI JI Int. J. Appl. Glass Sci. PD SEP PY 2014 VL 5 IS 3 SI SI BP 276 EP 286 DI 10.1111/ijag.12070 PG 11 WC Materials Science, Ceramics SC Materials Science GA AO9GG UT WOS:000341663500008 ER PT J AU Kim, JH Ou, ML Park, JD Morris, KR Schwaller, MR Wolff, DB AF Kim, Ji-Hye Ou, Mi-Lim Park, Jun-Dong Morris, Kenneth R. Schwaller, Mathew R. Wolff, David B. TI Global Precipitation Measurement (GPM) Ground Validation (GV) Prototype in the Korean Peninsula SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID MEASURING MISSION TRMM; LATENT HEATING DISTRIBUTIONS; RAIN-GAUGE MEASUREMENTS; RADAR OBSERVATIONS; MICROWAVE IMAGER; SPACEBORNE RADAR; SATELLITE; CALIBRATION; ALGORITHMS; VERSION-6 AB Since 2009, the Korea Meteorological Administration (KMA) has participated in ground validation (GV) projects through international partnerships within the framework of the Global Precipitation Measurement (GPM) Mission. The goal of this work is to assess the reliability of ground-based measurements in the Korean Peninsula as a means for validating precipitation products retrieved from satellite microwave sensors, with an emphasis on East Asian precipitation. KMA has a well-developed operational weather service infrastructure composed of meteorological radars, a dense rain gauge network, and automated weather stations. Measurements from these systems, including data from four ground-based radars (GRs), were combined with satellite data from the Tropical Rainfall Measuring Mission (TRMM) precipitation radar (PR) and used as a proxy for GPM GV over the Korean Peninsula. A time series of mean reflectivity differences (GR-PR) for stratiform-only and above-brightband-only data showed that the time-averaged difference fell between -2.0 and +1.0 dBZ for the four GRs used in this study. Site-specific adjustments for these relative mean biases were applied to GR reflectivities, and detailed statistical comparisons of reflectivity and rain rate between PR and bias-adjusted GR were carried out. In rain-rate comparisons, surface rain from the TRMM Microwave Imager (TMI) and the rain gauges were added and the results varied according to rain type. Bias correction has had a positive effect on GR rain rate comparing with PR and gauge rain rates. This study confirmed advance preparation for GPM GV system was optimized on the Korean Peninsula using the official framework. C1 [Kim, Ji-Hye; Ou, Mi-Lim] Korea Meteorol Adm, Natl Inst Meteorol Res, Seogwipo Si 697845, Jeju Do, South Korea. [Kim, Ji-Hye] Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea. [Park, Jun-Dong] Korea Meteorol Adm, Natl Meteorol Satellite Ctr, Jincheon, South Korea. [Park, Jun-Dong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Morris, Kenneth R.; Schwaller, Mathew R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wolff, David B.] NASA, Wallops Flight Facil, Wallops Isl, VA USA. RP Ou, ML (reprint author), Korea Meteorol Adm, Natl Inst Meteorol Res, 33 Seohobuk Ro, Seogwipo Si 697845, Jeju Do, South Korea. EM milim@korea.kr RI Measurement, Global/C-4698-2015 FU Research for the Meteorological and Earthquake Observation Technology and Its Application of the National Institute of Meteorological Research, Korea Meteorological Administration (KMA), South Korea FX This study was supported by the Research for the Meteorological and Earthquake Observation Technology and Its Application of the National Institute of Meteorological Research, Korea Meteorological Administration (KMA), South Korea. The authors thank the NASA Goddard Space Flight Center (GSFC) for providing data processing software for the GPM Ground Validation System (GVS) and TRMM products. NR 44 TC 1 Z9 2 U1 0 U2 13 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD SEP PY 2014 VL 31 IS 9 BP 1902 EP 1921 DI 10.1175/JTECH-D-13-00193.1 PG 20 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AO4WM UT WOS:000341342100004 ER PT J AU Song, H Lin, WY Lin, YL Wolf, AB Donner, LJ Del Genio, AD Neggers, R Endo, S Liu, YG AF Song, Hua Lin, Wuyin Lin, Yanluan Wolf, Audrey B. Donner, Leo J. Del Genio, Anthony D. Neggers, Roel Endo, Satoshi Liu, Yangang TI Evaluation of Cloud Fraction Simulated by Seven SCMs against the ARM Observations at the SGP Site SO JOURNAL OF CLIMATE LA English DT Article ID SINGLE-COLUMN MODELS; RADIATION MEASUREMENT PROGRAM; GENERAL-CIRCULATION MODELS; SHALLOW CUMULUS CONVECTION; PHASE ARCTIC CLOUD; LARGE-SCALE MODELS; CLIMATE MODELS; SURFACE OBSERVATIONS; PARAMETERIZATION; SYSTEM AB This study evaluates the performances of seven single-column models (SCMs) by comparing simulated cloud fraction with observations at the Atmospheric Radiation Measurement Program (ARM) Southern Great Plains (SGP) site from January 1999 to December 2001. Compared with the 3-yr mean observational cloud fraction, the ECMWF SCM underestimates cloud fraction at all levels and the GISS SCM underestimates cloud fraction at levels below 200 hPa. The two GFDL SCMs underestimate lower-to-middle level cloud fraction but overestimate upper-level cloud fraction. The three Community Atmosphere Model (CAM) SCMs overestimate upper-level cloud fraction and produce lower-level cloud fraction similar to the observations but as a result of compensating overproduction of convective cloud fraction and underproduction of stratiform cloud fraction. Besides, the CAM3 and CAM5 SCMs both overestimate midlevel cloud fraction, whereas the CAM4 SCM underestimates. The frequency and partitioning analyses show a large discrepancy among the seven SCMs: Contributions of nonstratiform processes to cloud fraction production are mainly in upper-level cloudy events over the cloud cover range 10%-80% in SCMs with prognostic cloud fraction schemes and in lower-level cloudy events over the cloud cover range 15%-50% in SCMs with diagnostic cloud fraction schemes. Further analysis reveals different relationships between cloud fraction and relative humidity (RH) in the models and observations. The underestimation of lower-level cloud fraction in most SCMs is mainly due to the larger threshold RH used in models. The overestimation of upper-level cloud fraction in the three CAM SCMs and two GFDL SCMs is primarily due to the overestimation of RH and larger mean cloud fraction of cloudy events plus more occurrences of RH around 40%-80%, respectively. C1 [Song, Hua; Lin, Wuyin; Endo, Satoshi; Liu, Yangang] Brookhaven Natl Lab, Upton, NY 11973 USA. [Lin, Yanluan] Tsinghua Univ, Ctr Earth Syst Sci, Key Lab Earth Syst Modeling, Minist Educ, Beijing 100084, Peoples R China. [Wolf, Audrey B.] Columbia Univ, New York, NY USA. [Donner, Leo J.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Neggers, Roel] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. RP Song, H (reprint author), Brookhaven Natl Lab, Div Atmospher Sci, 75 Rutherford Dr,Bldg 815E, Upton, NY 11973 USA. EM hsong@bnl.gov RI lin, yanluan/A-6333-2015; Liu, Yangang/H-6154-2011 FU Office of Biological and Environmental Research of the U.S. Department of Energy as part of the Earth Systems Modeling (ESM) program via the FASTER project; Atmospheric System Research program; NASA Modeling and Analysis Program FX This work is supported by the Office of Biological and Environmental Research of the U.S. Department of Energy as part of the Earth Systems Modeling (ESM) program via the FASTER project (http://www.bnl.gov/faster) and Atmospheric System Research program. Del Genio is supported also by the NASA Modeling and Analysis Program. We thank Editor Dr. Robert Wood and three anonymous reviewers for their insightful and constructive comments. We also thank Dr. Stephen Schwartz for his interest and helpful suggestions. NR 61 TC 4 Z9 4 U1 1 U2 14 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD SEP 1 PY 2014 VL 27 IS 17 BP 6698 EP 6719 DI 10.1175/JCLI-D-13-00555.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AO4BS UT WOS:000341281800021 ER PT J AU Shindell, D AF Shindell, Drew TI Reply to 'Questions of bias in climate models' SO NATURE CLIMATE CHANGE LA English DT Letter C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Shindell, D (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM drew.shindell@duke.edu RI Shindell, Drew/D-4636-2012 NR 6 TC 2 Z9 2 U1 0 U2 13 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X EI 1758-6798 J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD SEP PY 2014 VL 4 IS 9 BP 742 EP 743 PG 3 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AO7YS UT WOS:000341569700005 ER PT J AU Badavi, FF Walker, SA Koos, LMS AF Badavi, Francis F. Walker, Steven A. Koos, Lindsey M. Santos TI Evaluation of the new radiation belt AE9/AP9/SPM model for a cislunar mission SO ACTA ASTRONAUTICA LA English DT Article DE Trapped radiation belts; Cislunar space; Lagrange point L2; Effective dose ID ADULT VOXEL PHANTOM; PROTECTION DOSIMETRY AB Space mission planners continue to experience challenges associated with human space flight. Concerned with the omnipresence of harmful ionizing radiation in space, at the mission design stage, mission planners must evaluate the amount of exposure the crew of a spacecraft is subjected to during the transit trajectory from low Earth orbit (LEO) to geosynchronous orbit (GEO) and beyond (free space). The Earth's geomagnetic field is located within the domain of LEO-GEO and, depending on latitude, extends out some 40,000-60,000 km. This field contains the Van Allen trapped electrons, protons, and low-energy plasmas, such as the nuclei of hydrogen, helium, oxygen, and to a lesser degree other atoms. In addition, there exist the geomagnetically attenuated energetic galactic cosmic rays (GCR). These particles are potentially harmful to improperly shielded crew members and onboard subsystems. Mitigation strategies to limit the exposure due to free space GCR and sporadic solar energetic particles (SEP) such as flare and coronal mass ejection (CME) must also be exercised beyond the trapped field. Presented in this work is the exposure analysis for a multi-vehicle mission planned for the epoch of February 2020 from LEO to the Earth-moon Lagrange-point two (L2), located approximately 63,000 km beyond the orbit of the Earth-moon binary system. Space operation at 12 provides a gravitationally stable orbit for a vehicle and partially eliminates the need for periodic thrust-vectoring to maintain orbital stability. In the cislunar (Earth-moon) space of L2, the mission trajectory and timeline in this work call for a cargo vehicle to rendezvous with a crew vehicle. This is followed by 15 days of space activities at 12 while the cargo and crew vehicles are docked after which the crew returns to Earth. The mission epoch of 2020 is specifically chosen as it is anticipated that the next solar minimum (i.e. end of cycle 24) in the Sun's approximate 11 years cycle will take place around this time. From a mission planning point of view, this date is ideal as the predictable GCR exposure will be at a maximum, while the sporadic SEP will be at a minimum. In addition, it is anticipated that by 2020 a vehicle capable of launching a crew of four will be operationally ready. During the LEO-GEO transit, the crew and cargo vehicles will encounter exposure from trapped particles and attenuated GCR, followed by free space exposure due to GCR and SEP during solar active times. Within the trapped field, a challenge arises from properly calculating the amount of exposure acquired. Within this field, in the absence of SEP (i.e. solar quiet times), the vehicles will have to transit through an inner proton belt, an inner and outer electron belts, and an attenuated GCR field. There exist a number of models to define the intensities of the trapped particles during the quiet and active SEP. Among the more established trapped models are the historic and popular electron/proton AE8/AP8 model dating back to the 1980s, the historic and less popular electron/proton CRRES model dating back to 1990s, and the recently released electron/proton/space plasma AE9/AP9/SPM model. The AE9/AP9/SPM model is a major improvement over the older AE8/AP8 and CRRES models. This model is derived from numerous measurements acquired over four solar cycles dating back to the 1970s, roughly representing 40 years of data collection. In contrast, the older AE8/AP8 and CRRES models were limited to only a few months of measurements taken during the prior solar minima and maxima. In this work, within the trapped field, along the design trajectory of the crew vehicle, the AE9/AP9/SPM model is evaluated against the older AE8/AP8 model during solar quiet times. The analysis is then extended to the GCR dominated en-route, cislunar L2 space and return trajectories in order to provide cumulative exposure estimates to the crew vehicle for the duration of the entire mission. (C) 2014 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Badavi, Francis F.; Walker, Steven A.; Koos, Lindsey M. Santos] Old Dominion Univ, Norfolk, VA 23529 USA. RP Badavi, FF (reprint author), NASA, Langley Res Ctr, MS 188E, Hampton, VA 23681 USA. EM francis.f.badavi@nasa.gov FU NASA Human Research Program (HRP) under the Human Exploration and Operations Mission Directorate; NASA [NNX12AN58A, NNX09AR20A] FX The authors wish to express their gratitude to Garry Qualls of LaRC for providing the CEV604 crew vehicle geometry; Jonathan Chrone of Analytical Mechanics Associates (AMA) Inc. for providing the epoch specific cislunar trajectory; W.R. Johnston of Space Vehicles Directorate, Air Force Research Laboratory, Kirtland AFB and T.P. O'Brien of Aerospace Corporation for assistance with the AE9/AP9/SPM trapped model. This work was supported by the NASA Human Research Program (HRP) under the Human Exploration and Operations Mission Directorate, and partially by the NASA Grants NNX12AN58A and NNX09AR20A. NR 27 TC 1 Z9 2 U1 1 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD SEP-OCT PY 2014 VL 102 BP 156 EP 168 DI 10.1016/j.actaastro.2014.06.008 PG 13 WC Engineering, Aerospace SC Engineering GA AN6HB UT WOS:000340694500014 ER PT J AU Kakoi, M Howell, KC Folta, D AF Kakoi, Masaki Howell, Kathleen C. Folta, David TI Access to Mars from Earth-Moon libration point orbits: Manifold and direct options SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 64th International Astronautical Congress (IAC) CY SEP 23-27, 2013 CL Beijing, PEOPLES R CHINA DE Multi-body dynamics; Circular restricted three-body problem; Invariant manifolds; Libration point orbits; System-to-system transfer; Mars ID DYNAMICAL-SYSTEMS THEORY; INVARIANT-MANIFOLDS; SUN-EARTH; TRANSFERS; DESIGN; TRAJECTORIES; MISSION; CAPTURE; ESCAPE AB This investigation is focused specifically on transfers from Earth-Moon L-1/L-2 libration point orbits to Mars. Initially, the analysis is based on the circular restricted three-body problem to utilize the framework of the invariant manifolds. Various departure scenarios are compared, including arcs that leverage manifolds associated with the Sun-Earth L-2 orbits as well as non-manifold trajectories. For the manifold options, ballistic transfers from Earth-Moon L-2 libration point orbits to Sun-Earth L-1/L-2 halo orbits are first computed. This autonomous procedure applies to both departure and arrival between the Earth-Moon and Sun-Earth systems. Departure times in the lunar cycle, amplitudes and types of libration point orbits, manifold selection, and the orientation/location of the surface of section all contribute to produce a variety of options. As the destination planet, the ephemeris position for Mars is employed throughout the analysis. The complete transfer is transitioned to the ephemeris model after the initial design phase. Results for multiple departure/arrival scenarios are compared. (C) 2014 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Kakoi, Masaki; Howell, Kathleen C.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. [Folta, David] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kakoi, M (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, 701 W Stadium Ave, W Lafayette, IN 47907 USA. EM kakoi@purdue.edu; howell@purdue.edu; david.c.folta@nasa.gov OI Howell, Kathleen/0000-0002-1298-5017 NR 42 TC 6 Z9 6 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD SEP-OCT PY 2014 VL 102 BP 269 EP 286 DI 10.1016/j.actaastro.2014.06.010 PG 18 WC Engineering, Aerospace SC Engineering GA AN6HB UT WOS:000340694500025 ER PT J AU Clegg, SM Wiens, R Misra, AK Sharma, SK Lambert, J Bender, S Newell, R Nowak-Lovato, K Smrekar, S Dyar, MD Maurice, S AF Clegg, Samuel M. Wiens, Roger Misra, Anupam K. Sharma, Shiv K. Lambert, James Bender, Steven Newell, Raymond Nowak-Lovato, Kristy Smrekar, Sue Dyar, M. Darby Maurice, Sylvestre TI Planetary Geochemical Investigations Using Raman and Laser-Induced Breakdown Spectroscopy SO APPLIED SPECTROSCOPY LA English DT Article DE Raman spectroscopy; Laser-induced breakdown spectroscopy; LIBS; Mars geology; Venus geology; Remote sensing ID CHEMCAM INSTRUMENT SUITE; BULK AQUEOUS-SOLUTIONS; IN-SITU; HIGH-PRESSURE; GALE CRATER; PIGMENT IDENTIFICATION; MARS; EXPLORATION; SURFACES; SCIENCE AB An integrated Raman spectroscopy and laser-induced breakdown spectroscopy (LIBS) instrument is a valuable geoanalytical tool for future planetary missions to Mars, Venus, and elsewhere. The Chem Cam instrument operating on the Mars Curiosity rover includes a remote LIBS instrument. An integrated Raman-LIBS spectrometer (RLS) based on the Chem Cam architecture could be used as a reconnaissance tool for other contact instruments as well as a primary science instrument capable of quantitative mineralogical and geochemical analyses. Replacing one of the Chem Cam spectrometers with a miniature transmission spectrometer enables a Raman spectroscopy mineralogical analysis to be performed, complementing the LIBS chemical analysis while retaining an overall architecture resembling Chem Cam. A prototype transmission spectrometer was used to record Raman spectra under both Martian and Venus conditions. Two different high-pressure and high-temperature cells were used to collect the Raman and LIBS spectra to simulate surface conditions on Venus. The resulting LIBS spectra were used to generate a limited partial least squares Venus calibration model for the major elements. These experiments demonstrate the utility and feasibility of a combined RLS instrument. C1 [Clegg, Samuel M.; Wiens, Roger; Bender, Steven; Newell, Raymond; Nowak-Lovato, Kristy] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Misra, Anupam K.; Sharma, Shiv K.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Lambert, James; Smrekar, Sue] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dyar, M. Darby] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. [Maurice, Sylvestre] Univ Toulouse, Inst Rech Astrophys & Planetol, Toulouse 04, France. RP Clegg, SM (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA. EM sclegg@lanl.gov OI Clegg, Sam/0000-0002-0338-0948 FU LANL Laboratory Directed Research and Development (LORD) program; NASA New Frontiers program; NASA Mars Science Laboratory program FX We gratefully acknowledge the LANL Laboratory Directed Research and Development (LORD) program, the NASA New Frontiers program, and the NASA Mars Science Laboratory program for funding various aspects of the study presented here. We also gratefully acknowledge David J. Cremers and Amy J. Bauer for the gracious invitation to present at the SCIX conference as well as the SCIX organizers for the opportunity to contribute to this special issue. NR 61 TC 14 Z9 14 U1 11 U2 66 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0003-7028 EI 1943-3530 J9 APPL SPECTROSC JI Appl. Spectrosc. PD SEP PY 2014 VL 68 IS 9 BP 925 EP 936 DI 10.1366/13-07386 PG 12 WC Instruments & Instrumentation; Spectroscopy SC Instruments & Instrumentation; Spectroscopy GA AN8PF UT WOS:000340865400003 PM 25226246 ER PT J AU Ade, PAR Aikin, RW Amiri, M Barkats, D Benton, SJ Bischoff, CA Bock, JJ Brevik, JA Buder, I Bullock, E Davis, G Day, PK Dowell, CD Duband, L Filippini, JP Fliescher, S Golwala, SR Halpern, M Hasselfield, M Hildebrandt, SR Hilton, GC Irwin, KD Karkare, KS Kaufman, JP Keating, BG Kernasovskiy, SA Kovac, JM Kuo, CL Leitch, EM Llombart, N Lueker, M Netterfield, CB Nguyen, HT O'Brient, R Ogburn, RW Orlando, A Pryke, C Reintsema, CD Richter, S Schwarz, R Sheehy, CD Staniszewski, ZK Story, KT Sudiwala, RV Teply, GP Tolan, JE Turner, AD Vieregg, AG Wilson, P Wong, CL Yoon, KW AF Ade, P. A. R. Aikin, R. W. Amiri, M. Barkats, D. Benton, S. J. Bischoff, C. A. Bock, J. J. Brevik, J. A. Buder, I. Bullock, E. Davis, G. Day, P. K. Dowell, C. D. Duband, L. Filippini, J. P. Fliescher, S. Golwala, S. R. Halpern, M. Hasselfield, M. Hildebrandt, S. R. Hilton, G. C. Irwin, K. D. Karkare, K. S. Kaufman, J. P. Keating, B. G. Kernasovskiy, S. A. Kovac, J. M. Kuo, C. L. Leitch, E. M. Llombart, N. Lueker, M. Netterfield, C. B. Nguyen, H. T. O'Brient, R. Ogburn, R. W. Orlando, A. Pryke, C. Reintsema, C. D. Richter, S. Schwarz, R. Sheehy, C. D. Staniszewski, Z. K. Story, K. T. Sudiwala, R. V. Teply, G. P. Tolan, J. E. Turner, A. D. Vieregg, A. G. Wilson, P. Wong, C. L. Yoon, K. W. CA Bicep2 Collaboration TI BICEP2. II. EXPERIMENT AND THREE-YEAR DATA SET SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; gravitational waves; inflation; instrumentation: polarimeters; telescopes ID TRANSITION-EDGE SENSORS; BACKGROUND POLARIZATION EXPERIMENTS; ANGULAR SCALE POLARIZATION; POWER SPECTRA; GRAVITY-WAVES; SOUTH-POLE; MICROWAVE; ANISOTROPY; RADIATION; PROBE AB We report on the design and performance of the BICEP2 instrument and on its three-year data set. BICEP2 was designed to measure the polarization of the cosmic microwave background (CMB) on angular scales of 1 degrees-5 degrees(l = 40-200), near the expected peak of the B-mode polarization signature of primordial gravitational waves from cosmic inflation. Measuring B-modes requires dramatic improvements in sensitivity combined with exquisite control of systematics. The BICEP2 telescope observed from the South Pole with a 26 cm aperture and cold, on-axis, refractive optics. BICEP2 also adopted a new detector design in which beam-defining slot antenna arrays couple to transition-edge sensor (TES) bolometers, all fabricated on a common substrate. The antenna-coupled TES detectors supported scalable fabrication and multiplexed readout that allowed BICEP2 to achieve a high detector count of 500 bolometers at 150 GHz, giving unprecedented sensitivity to B-modes at degree angular scales. After optimization of detector and readout parameters, BICEP2 achieved an instrument noise-equivalent temperature of 15.8 mu K root s. The full data set reached Stokes Q and U map depths of 87.2 nK in square-degree pixels (5'.2 mu K) over an effective area of 384 deg(2) within a 1000 deg(2) field. These are the deepest CMB polarization maps at degree angular scales to date. The power spectrum analysis presented in a companion paper has resulted in a significant detection of B-mode polarization at degree scales. C1 [Ade, P. A. R.; Sudiwala, R. V.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aikin, R. W.; Bock, J. J.; Brevik, J. A.; Filippini, J. P.; Golwala, S. R.; Hildebrandt, S. R.; Lueker, M.; Staniszewski, Z. K.; Teply, G. P.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Amiri, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Barkats, D.] ESO, Joint ALMA Observ, Santiago, Chile. [Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Bischoff, C. A.; Buder, I.; Karkare, K. S.; Kovac, J. M.; Richter, S.; Vieregg, A. G.; Wong, C. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bock, J. J.; Day, P. K.; Dowell, C. D.; Hildebrandt, S. R.; Llombart, N.; Nguyen, H. T.; O'Brient, R.; Turner, A. D.; Wilson, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bullock, E.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Duband, L.] Univ Grenoble Alpes, CEA INAC SBT, F-38000 Grenoble, France. [Fliescher, S.; Schwarz, R.; Sheehy, C. D.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Hilton, G. C.; Irwin, K. D.; Reintsema, C. D.] NIST, Boulder, CO 80305 USA. [Irwin, K. D.; Kernasovskiy, S. A.; Kuo, C. L.; Ogburn, R. W.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Irwin, K. D.; Ogburn, R. W.; Yoon, K. W.] Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Keating, B. G.; Orlando, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Leitch, E. M.; Sheehy, C. D.; Vieregg, A. G.] Univ Chicago, Chicago, IL 60637 USA. RP Ade, PAR (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. EM ogburn@stanford.edu OI Orlando, Angiola/0000-0001-8004-5054; Karkare, Kirit/0000-0002-5215-6993; Barkats, Denis/0000-0002-8971-1954; Bischoff, Colin/0000-0001-9185-6514 FU U.S. National Science Foundation [ANT-0742818, ANT-1044978, ANT-0742592, ANT-1110087]; NASA APRA and SAT programs [06-ARPA206-0040, 10-SAT10-0017]; Gordon and Betty Moore Foundation at Caltech; Canada Foundation for Innovation; W.M. Keck Foundation; FAS Science Division Research Computing Group at Harvard University; JPL Research and Technology Development Fund FX BICEP2 was supported by the U.S. National Science Foundation under grants ANT-0742818 and ANT-1044978 (Caltech/Harvard) and ANT-0742592 and ANT-1110087 (Chicago/Minnesota). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and grants 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The receiver development was supported in part by a grant from the W.M. Keck Foundation. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. Tireless administrative support was provided by Irene Coyle and Kathy Deniston. NR 71 TC 64 Z9 64 U1 2 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2014 VL 792 IS 1 AR 62 DI 10.1088/0004-637X/792/1/62 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100062 ER PT J AU Bradley, LD Zitrin, A Coe, D Bouwens, R Postman, M Balestra, I Grillo, C Monna, A Rosati, P Seitz, S Host, O Lemze, D Moustakas, J Moustakas, LA Shu, X Zheng, W Broadhurst, T Carrasco, M Jouvel, S Koekemoer, A Medezinski, E Meneghetti, M Nonino, M Smit, R Umetsu, K Bartelmann, M Benitez, N Donahue, M Ford, H Infante, L Jimenez-Teja, Y Kelson, D Lahav, O Maoz, D Melchior, P Merten, J Molino, A AF Bradley, L. D. Zitrin, A. Coe, D. Bouwens, R. Postman, M. Balestra, I. Grillo, C. Monna, A. Rosati, P. Seitz, S. Host, O. Lemze, D. Moustakas, J. Moustakas, L. A. Shu, X. Zheng, W. Broadhurst, T. Carrasco, M. Jouvel, S. Koekemoer, A. Medezinski, E. Meneghetti, M. Nonino, M. Smit, R. Umetsu, K. Bartelmann, M. Benitez, N. Donahue, M. Ford, H. Infante, L. Jimenez-Teja, Y. Kelson, D. Lahav, O. Maoz, D. Melchior, P. Merten, J. Molino, A. TI CLASH: A CENSUS OF MAGNIFIED STAR-FORMING GALAXIES AT z similar to 6-8 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; gravitational lensing: strong ID ULTRA-DEEP-FIELD; HIGH-REDSHIFT GALAXIES; LYMAN-BREAK GALAXIES; EXTRAGALACTIC LEGACY SURVEY; EARLY RELEASE SCIENCE; SPECTRAL ENERGY-DISTRIBUTIONS; CLUSTER RXC J2248.7-4431; STRONG-LENSING ANALYSIS; EMISSION-LINE GALAXIES; LUMINOSITY FUNCTION AB We utilize 16 band Hubble Space Telescope (HST) observations of 18 lensing clusters obtained as part of the Cluster Lensing And Supernova survey with Hubble (CLASH) Multi-Cycle Treasury program to search for z similar to 6-8 galaxies. We report the discovery of 204, 45, and 13 Lyman-break galaxy candidates at z similar to 6, z similar to 7, and z similar to 8, respectively, identified from purely photometric redshift selections. This large sample, representing nearly an order of magnitude increase in the number of magnified star-forming galaxies at z similar to 6-8 presented to date, is unique in that we have observations in four WFC3/UVIS UV, seven ACS/WFC optical, and all five WFC3/IR broadband filters, which enable very accurate photometric redshift selections. We construct detailed lensing models for 17 of the 18 clusters to estimate object magnifications and to identify two new multiply lensed z greater than or similar to 6 candidates. The median magnifications over the 17 clusters are 4, 4, and 5 for the z similar to 6, z similar to 7, and z similar to 8 samples, respectively, over an average area of 4.5 arcmin(2) per cluster. We compare our observed number counts with expectations based on convolving "blank" field UV luminosity functions through our cluster lens models and find rough agreement down to similar to 27 mag, where we begin to suffer significant incompleteness. In all three redshift bins, we find a higher number density at brighter observed magnitudes than the field predictions, empirically demonstrating for the first time the enhanced efficiency of lensing clusters over field surveys. Our number counts also are in general agreement with the lensed expectations from the cluster models, especially at z 6, where we have the best statistics. C1 [Bradley, L. D.; Coe, D.; Postman, M.; Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Zitrin, A.; Carrasco, M.; Bartelmann, M.] Inst Theoret Astrophys, Zentrum Astron, D-29120 Heidelberg, Germany. [Bouwens, R.; Smit, R.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Balestra, I.; Nonino, M.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Balestra, I.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Grillo, C.; Host, O.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Monna, A.; Seitz, S.] Univ Observ Munich, D-81679 Munich, Germany. [Monna, A.; Seitz, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Rosati, P.] European So Observ, D-85748 Garching, Germany. [Lemze, D.; Zheng, W.; Medezinski, E.; Ford, H.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Moustakas, J.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Moustakas, L. A.; Meneghetti, M.; Merten, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Shu, X.] Univ Sci & Technol China, Dept Astron, Hefei 230026, Anhui, Peoples R China. [Broadhurst, T.] Univ Basque Country, UPV EHU, Dept Theoret Phys & Hist Sci, E-48080 Bilbao, Spain. [Broadhurst, T.] Ikerbasque, Basque Fdn Sci, E-48011 Bilbao, Spain. [Carrasco, M.] Pontificia Univ Catolica Chile, Ctr Astroingn, Dept Astron & Astrofis, Santiago, Chile. [Jouvel, S.] CSIC, IEEC, Inst Ciencies Espai, E-08193 Barcelona, Spain. [Jouvel, S.; Lahav, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Meneghetti, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Meneghetti, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Benitez, N.; Jimenez-Teja, Y.; Molino, A.] CSIC, IAA, E-18008 Granada, Spain. [Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Kelson, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Maoz, D.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Melchior, P.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Melchior, P.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. RP Bradley, LD (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. RI Jimenez-Teja, Yolanda/D-5933-2011; Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015; Shu, Xinwen/D-7294-2017; OI Grillo, Claudio/0000-0002-5926-7143; Meneghetti, Massimo/0000-0003-1225-7084; Shu, Xinwen/0000-0002-7020-4290; Nonino, Mario/0000-0001-6342-9662; Balestra, Italo/0000-0001-9660-894X; Umetsu, Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360; Koekemoer, Anton/0000-0002-6610-2048; Benitez, Narciso/0000-0002-0403-7455 FU contract research "Internationale Spitzenforschung II/2-6" of the Baden Wurttemberg Stiftung; DNRF FX The CLASH Multi-Cycle Treasury Program (GO-12065) is based on observations made with the NASA/ESA Hubble Space Telescope. The Space Telescope Science Institute is operatedby the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. A.Z. is supported by contract research "Internationale Spitzenforschung II/2-6" of the Baden Wurttemberg Stiftung. The work of L.A.M., J.M., and M.M. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The Dark Cosmology Centre is funded by the DNRF. NR 104 TC 48 Z9 48 U1 2 U2 17 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2014 VL 792 IS 1 AR 76 DI 10.1088/0004-637X/792/1/76 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100076 ER PT J AU Burke, CJ McCullough, PR AF Burke, Christopher J. McCullough, P. R. TI TRANSIT AND RADIAL VELOCITY SURVEY EFFICIENCY COMPARISON FOR A HABITABLE ZONE EARTH SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; methods: statistical; planetary systems; surveys; techniques: photometric; techniques: radial velocities ID SUN-LIKE STAR; MAIN-SEQUENCE STARS; EXTRASOLAR PLANETS; ORBITAL ECCENTRICITY; FALSE POSITIVES; SPACE-TELESCOPE; BLEND SCENARIOS; MULTIPLE SYSTEM; LIGHT CURVES; LOW-MASS AB Transit and radial velocity searches are two techniques for identifying nearby extrasolar planets to Earth that transit bright stars. Identifying a robust sample of these exoplanets around bright stars for detailed atmospheric characterization is a major observational undertaking. In this study we describe a framework that answers the question of whether a transit or radial velocity survey is more efficient at finding transiting exoplanets given the same amount of observing time. Within the framework we show that a transit survey's window function can be approximated using the hypergeometric probability distribution. We estimate the observing time required for a transit survey to find a transiting Earth-sized exoplanet in the habitable zone (HZ) with an emphasis on late-type stars. We also estimate the radial velocity precision necessary to detect the equivalent HZ Earth-mass exoplanet that also transits when using an equal amount of observing time as the transit survey. We find that a radial velocity survey with sigma(rv) similar to 0.6 m s(-1) precision has comparable efficiency in terms of observing time to a transit survey with the requisite photometric precision sigma(phot) similar to 300 ppm to find a transiting Earth-sized exoplanet in the HZ of late M dwarfs. For super-Earths, a sigma(rv) similar to 2.0 m s(-1) precision radial velocity survey has comparable efficiency to a transit survey with sigma(phot) similar to 2300 ppm. C1 [Burke, Christopher J.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [McCullough, P. R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [McCullough, P. R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Burke, CJ (reprint author), NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. EM christopher.j.burke@nasa.gov NR 72 TC 4 Z9 4 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2014 VL 792 IS 1 AR 79 DI 10.1088/0004-637X/792/1/79 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100079 ER PT J AU Burke-Spolaor, S Bannister, KW AF Burke-Spolaor, Sarah Bannister, Keith W. TI THE GALACTIC POSITION DEPENDENCE OF FAST RADIO BURSTS AND THE DISCOVERY OF FRB011025 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: general; radio continuum: general ID MULTIBEAM PULSAR SURVEY; TRANSIENTS; LATITUDES; SEARCHES; ORIGIN AB We report the detection of a dispersed fast radio burst (FRB) in archival intermediate-latitude Parkes Radio Telescope data. The burst appears to be of the same physical origin as the four purported extragalactic FRBs reported by Thornton et al. This burst's arrival time precedes the Thornton et al. bursts by 10 years. We consider that this survey, and many other archival low-latitude (vertical bar gb vertical bar < 30 degrees) pulsar surveys, have been searched for FRBs but produced fewer detections than the comparatively brief Thornton et al. search. Such a rate dependence on Galactic position could provide critical supporting evidence for an extragalactic origin for FRBs. To test this, we form an analytic expression to account for Galactic position and survey setup in FRB rate predictions. Employing a sky temperature, scattering, and dispersion model of the Milky Way, we compute the expected number of FRBs if they are isotropically distributed on the sky with respect to the Galactic position (i.e., local), and if they are of extragalactic origin. We demonstrate that the relative detection rates reject a local origin with a confidence of 99.96% (similar to 3.6 sigma). The extragalactic predictions provide a better agreement; however, there are still strong discrepancies with the low-latitude detection rate at a confidence of 99.69% (similar to 2.9 sigma). However, for the extragalactic population, the differences in predicted versus detected population may be accounted for by a number of factors, which we discuss. C1 [Burke-Spolaor, Sarah] CALTECH, Pasadena, CA 91125 USA. [Burke-Spolaor, Sarah] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Bannister, Keith W.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. RP Burke-Spolaor, S (reprint author), CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA. EM sarahbspolaor@gmail.com OI Bannister, Keith/0000-0003-2149-0363 FU Commonwealth of Australia FX The Australia Telescope Compact Array Parkes Radio Telescope is part of the Australia Telescope National Facility, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. Processing for our archival search was performed on the Swinburne University Green Machine; we acknowledge the use of this supercomputer facility in this work. We thank B. Stappers, D. Thornton, J. Deneva, and A. Brazier for providing information about survey pointing directions which were used in this paper's analysis. We thank an anonymous referee for contributing valuable comments on this paper. Cosmological redshift calculations used the online calculator provided by Wright (2006). NR 31 TC 67 Z9 68 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2014 VL 792 IS 1 AR 19 DI 10.1088/0004-637X/792/1/19 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100019 ER PT J AU Emslie, AG Holman, GD Litvinenko, YE AF Emslie, A. Gordon Holman, Gordon D. Litvinenko, Yuri E. TI ON THE SOLUTION OF THE CONTINUITY EQUATION FOR PRECIPITATING ELECTRONS IN SOLAR FLARES SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: analytical; plasmas; Sun: atmosphere; Sun: flares; Sun: particle emission; Sun: X-rays, gamma rays ID X-RAY OBSERVATIONS; IMPULSIVE PHASE; BREMSSTRAHLUNG; SPECTRA; TARGET; BEAMS; COLLISIONS AB Electrons accelerated in solar flares are injected into the surrounding plasma, where they are subjected to the influence of collisional (Coulomb) energy losses. Their evolution is modeled by a partial differential equation describing continuity of electron number. In a recent paper, Dobranskis & Zharkova claim to have found an "updated exact analytical solution" to this continuity equation. Their solution contains an additional term that drives an exponential decrease in electron density with depth, leading them to assert that the well-known solution derived by Brown, Syrovatskii & Shmeleva, and many others is invalid. We show that the solution of Dobranskis & Zharkova results from a fundamental error in the application of the method of characteristics and is hence incorrect. Further, their comparison of the "new" analytical solution with numerical solutions of the Fokker-Planck equation fails to lend support to their result. We conclude that Dobranskis & Zharkova's solution of the universally accepted and well-established continuity equation is incorrect, and that their criticism of the correct solution is unfounded. We also demonstrate the formal equivalence of the approaches of Syrovatskii & Shmeleva and Brown, with particular reference to the evolution of the electron flux and number density (both differential in energy) in a collisional thick target. We strongly urge use of these long-established, correct solutions in future works. C1 [Emslie, A. Gordon] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA. [Holman, Gordon D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Litvinenko, Yuri E.] Univ Waikato, Dept Math, Hamilton, New Zealand. RP Emslie, AG (reprint author), Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA. EM emslieg@wku.edu; gordon.d.holman@nasa.gov FU NASA [NNX10AT78J]; NASA Heliophysics Guest Investigator and Living with a Star TRT Grants; RHESSI project FX Useful discussions with Professor Ian Craig are gratefully acknowledged. A.G.E. was supported by NASA Grant NNX10AT78J. G.D.H. was supported by NASA Heliophysics Guest Investigator and Living with a Star TR&T Grants and the RHESSI project. We thank the referee for suggesting the inclusion of the material in Section 2.2 and the editor for suggesting that two independently submitted papers with similar content be combined into the current work. NR 16 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2014 VL 792 IS 1 AR 5 DI 10.1088/0004-637X/792/1/5 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100005 ER PT J AU Hemphill, PB Rothschild, RE Markowitz, A Furst, F Pottschmidt, K Wilms, J AF Hemphill, Paul B. Rothschild, Richard E. Markowitz, Alex Fuerst, Felix Pottschmidt, Katja Wilms, Joern TI A CLUMPY STELLAR WIND AND LUMINOSITY-DEPENDENT CYCLOTRON LINE REVEALED BY THE FIRST SUZAKU OBSERVATION OF THE HIGH-MASS X-RAY BINARY 4U 1538-522 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (4U 1538-522); stars: magnetic field; stars: oscillations; X-rays: binaries; X-rays: stars ID OPTICAL SPECTROSCOPY; PULSAR 4U-1538-52; VELA X-1; SPECTRA; ASTROPHYSICS; ABSORPTION; EVOLUTION; DISCOVERY; BEPPOSAX; MODELS AB We present results from the first Suzaku observation of the high-mass X-ray binary 4U 1538-522. The broadband spectral coverage of Suzaku allows for a detailed spectral analysis, characterizing the cyclotron resonance scattering feature at 23.0 +/- 0.4 keV and the iron K alpha line at 6.426 +/- 0.008 keV, as well as placing limits on the strengths of the iron K beta line and the iron K edge. We track the evolution of the spectral parameters both in time and in luminosity, notably finding a significant positive correlation between cyclotron line energy and luminosity. A dip and spike in the light curve is shown to be associated with an order-of-magnitude increase in column density along the line of sight, as well as significant variation in the underlying continuum, implying the accretion of a overdense region of a clumpy stellar wind. We also present a phase-resolved analysis, with most spectral parameters of interest showing significant variation with phase. Notably, both the cyclotron line energy and the iron K alpha line intensity vary significantly with phase, with the iron line intensity significantly out of phase with the pulse profile. We discuss the implications of these findings in the context of recent work in the areas of accretion column physics and cyclotron resonance scattering feature formation. C1 [Hemphill, Paul B.; Rothschild, Richard E.; Markowitz, Alex] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Markowitz, Alex; Wilms, Joern] Dr Karl Remeis Sternwarte Erlangen Ctr Astroparti, D-96049 Bamberg, Germany. [Fuerst, Felix] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Pottschmidt, Katja] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Pottschmidt, Katja] CRESST, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hemphill, PB (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM pbhemphill@physics.ucsd.edu RI Wilms, Joern/C-8116-2013; XRAY, SUZAKU/A-1808-2009; OI Wilms, Joern/0000-0003-2065-5410; Hemphill, Paul/0000-0002-1676-6954 FU NASA [NNX13AE68G] FX This research has made use of data and software obtained from NASA's High Energy Astrophysics Science Archive Research Center (HEASARC), a service of the Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. P.B.H. was supported by NASA grant NNX13AE68G. NR 45 TC 7 Z9 7 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2014 VL 792 IS 1 AR 14 DI 10.1088/0004-637X/792/1/14 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100014 ER PT J AU Mainzer, A Bauer, J Cutri, RM Grav, T Masiero, J Beck, R Clarkson, P Conrow, T Dailey, J Eisenhardt, P Fabinsky, B Fajardo-Acosta, S Fowler, J Gelino, C Grillmair, C Heinrichsen, I Kendall, M Kirkpatrick, JD Liu, F Masci, F McCallon, H Nugent, CR Papin, M Rice, E Royer, D Ryan, T Sevilla, P Sonnett, S Stevenson, R Thompson, DB Wheelock, S Wiemer, D Wittman, M Wright, E Yan, L AF Mainzer, A. Bauer, J. Cutri, R. M. Grav, T. Masiero, J. Beck, R. Clarkson, P. Conrow, T. Dailey, J. Eisenhardt, P. Fabinsky, B. Fajardo-Acosta, S. Fowler, J. Gelino, C. Grillmair, C. Heinrichsen, I. Kendall, M. Kirkpatrick, J. Davy Liu, F. Masci, F. McCallon, H. Nugent, C. R. Papin, M. Rice, E. Royer, D. Ryan, T. Sevilla, P. Sonnett, S. Stevenson, R. Thompson, D. B. Wheelock, S. Wiemer, D. Wittman, M. Wright, E. Yan, L. TI INITIAL PERFORMANCE OF THE NEOWISE REACTIVATION MISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: general; infrared: general; minor planets, asteroids: general; space vehicles; surveys ID NEAR-EARTH OBJECTS; THERMAL-MODEL CALIBRATION; INFRARED-SURVEY-EXPLORER; MAIN BELT ASTEROIDS; WISE/NEOWISE OBSERVATIONS; SOLAR-SYSTEM; POPULATION; METEORITES; DUST; ALBEDO AB NASA's Wide-field Infrared Survey Explorer (WISE) spacecraft has been brought out of hibernation and has resumed surveying the sky at 3.4 and 4.6 mu m. The scientific objectives of the NEOWISE reactivation mission are to detect, track, and characterize near-Earth asteroids and comets. The search for minor planets resumed on 2013 December 23, and the first new near-Earth object (NEO) was discovered 6 days later. As an infrared survey, NEOWISE detects asteroids based on their thermal emission and is equally sensitive to high and low albedo objects; consequently, NEOWISE-discovered NEOs tend to be large and dark. Over the course of its three-year mission, NEOWISE will determine radiometrically derived diameters and albedos for similar to 2000 NEOs and tens of thousands of Main Belt asteroids. The 32 months of hibernation have had no significant effect on the mission's performance. Image quality, sensitivity, photometric and astrometric accuracy, completeness, and the rate of minor planet detections are all essentially unchanged from the prime mission's post-cryogenic phase. C1 [Mainzer, A.; Bauer, J.; Masiero, J.; Eisenhardt, P.; Fabinsky, B.; Heinrichsen, I.; Liu, F.; Nugent, C. R.; Rice, E.; Royer, D.; Sonnett, S.; Stevenson, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bauer, J.; Cutri, R. M.; Beck, R.; Conrow, T.; Dailey, J.; Fajardo-Acosta, S.; Fowler, J.; Gelino, C.; Grillmair, C.; Kirkpatrick, J. Davy; Masci, F.; McCallon, H.; Papin, M.; Wheelock, S.; Wittman, M.; Yan, L.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Grav, T.] Planetary Sci Inst, Tucson, AZ USA. [Clarkson, P.; Kendall, M.; Ryan, T.; Wiemer, D.] Ball Aerosp & Technol Ctr, Boulder, CO USA. [Sevilla, P.; Thompson, D. B.] Utah State Univ, Space Dynam Lab, Logan, UT 84322 USA. [Wright, E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM amainzer@jpl.nasa.gov OI Masiero, Joseph/0000-0003-2638-720X FU National Aeronautics and Space Administration FX This publication makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. We thank the paper's referee for helpful comments that greatly improved the manuscript. We gratefully acknowledge the services specific to NEOWISE contributed by the International Astronomical Union's Minor Planet Center, operated by the Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for Astronomical Telegrams, operated by Harvard University. We also thank the worldwide community of dedicated amateur and professional astronomers devoted to minor planet follow-up observations. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 61 TC 33 Z9 33 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 SEP 1 PY 2014 VL 792 IS 1 AR 30 DI 10.1088/0004-637X/792/1/30 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100030 ER PT J AU McIntosh, SW Wang, X Leamon, RJ Davey, AR Howe, R Krista, LD Malanushenko, AV Markel, RS Cirtain, JW Gurman, JB Pesnell, WD Thompson, MJ AF McIntosh, Scott W. Wang, Xin Leamon, Robert J. Davey, Alisdair R. Howe, Rachel Krista, Larisza D. Malanushenko, Anna V. Markel, Robert S. Cirtain, Jonathan W. Gurman, Joseph B. Pesnell, William D. Thompson, Michael J. TI DECIPHERING SOLAR MAGNETIC ACTIVITY. I. ON THE RELATIONSHIP BETWEEN THE SUNSPOT CYCLE AND THE EVOLUTION OF SMALL MAGNETIC FEATURES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: atmosphere; Sun: evolution; Sun: general; Sun: interior; Sun: rotation; sunspots ID DIFFERENTIAL ROTATION; MERIDIONAL CIRCULATION; DYNAMO SIMULATION; BRIGHT POINTS; CORONAL HOLE; SUN-SPOTS; FIELD; FLUX; FLOW; OSCILLATIONS AB Sunspots are a canonical marker of the Sun's internal magnetic field which flips polarity every similar to 22 yr. The principal variation of sunspots, an similar to 11 yr variation, modulates the amount of the magnetic field that pierces the solar surface and drives significant variations in our star's radiative, particulate, and eruptive output over that period. This paper presents observations from the Solar and Heliospheric Observatory and Solar Dynamics Observatory indicating that the 11 yr sunspot variation is intrinsically tied to the spatio-temporal overlap of the activity bands belonging to the 22 yr magnetic activity cycle. Using a systematic analysis of ubiquitous coronal brightpoints and the magnetic scale on which they appear to form, we show that the landmarks of sunspot cycle 23 can be explained by considering the evolution and interaction of the overlapping activity bands of the longer-scale variability. C1 [McIntosh, Scott W.; Wang, Xin; Markel, Robert S.; Thompson, Michael J.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Wang, Xin] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China. [Leamon, Robert J.; Malanushenko, Anna V.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Davey, Alisdair R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howe, Rachel] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Krista, Larisza D.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80205 USA. [Malanushenko, Anna V.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Cirtain, Jonathan W.] Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Gurman, Joseph B.; Pesnell, William D.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. RP McIntosh, SW (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA. EM mscott@ucar.edu RI Pesnell, William/D-1062-2012; OI Pesnell, William/0000-0002-8306-2500; McIntosh, Scott/0000-0002-7369-1776 FU NASA [NNX08AU30G, NNX08AL23G, NNM07AA01C-Hinode, NNG09FA40C-IRIS, NNG04EA00C]; National Science Foundation FX The data used in this paper are openly available from the SOHO, SDO, and the Virtual Solar Observatory (VSO; http://virtualsolar.org) data archives. S.W.M., R.J.L., A.R.D., and R.S.M. were partly funded by NASA grants (NNX08AU30G, NNX08AL23G, NNM07AA01C-Hinode, NNG09FA40C-IRIS). A.V.M. is supported by NASA grant NNG04EA00C (SDO/AIA). SOHO is a project of international collaboration between ESA and NASA. Sunspot data are from David Hathaway and the World Data Center SILSO, Royal Observatory of Belgium, Brussels. S.W.M. is grateful to Matthias Rempel, Yuhong Fan, Dick Altrock, SaraMartin, Roger Ulrich, Paul Charbonneau, Mark Miesch, and Eugene Parker for helpful discussions. NCAR is sponsored by the National Science Foundation. NR 53 TC 13 Z9 13 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 SEP 1 PY 2014 VL 792 IS 1 AR 12 DI 10.1088/0004-637X/792/1/12 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100012 ER PT J AU Misra, A Meadows, V Crisp, D AF Misra, Amit Meadows, Victoria Crisp, Dave TI THE EFFECTS OF REFRACTION ON TRANSIT TRANSMISSION SPECTROSCOPY: APPLICATION TO EARTH-LIKE EXOPLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; planets and satellites: atmospheres; radiative transfer ID GIANT PLANET TRANSITS; EXTRASOLAR PLANET; MU-M; SPACE-TELESCOPE; LUNAR ECLIPSE; WATER-VAPOR; ATMOSPHERE; ABSORPTION; MODEL; SPECTRUM AB We quantify the effects of refraction in transit transmission spectroscopy on spectral absorption features and on temporal variations that could be used to obtain altitude-dependent spectra for planets orbiting stars of different stellar types. We validate our model against altitude-dependent transmission spectra of the Earth from ATMOS and against lunar eclipse spectra from Palle et al. We perform detectability studies to show the potential effects of refraction on hypothetical observations of Earth analogs with the James Webb Space Telescope NIRSPEC. Due to refraction, there will be a maximum tangent pressure level that can be probed during transit for each given planet-star system. We show that because of refraction, for an Earth-analog planet orbiting in the habitable zone of a Sun-like star only the top 0.3 bars of the atmosphere can be probed, leading to a decrease in the signal-to-noise ratio (S/N) of absorption features by 60%, while for an Earth-analog planet orbiting in the habitable zone of an M5V star it is possible to probe almost the entire atmosphere with minimal decreases in S/N. We also show that refraction can result in temporal variations in the transit transmission spectrum which may provide a way to obtain altitude-dependent spectra of exoplanet atmospheres. Additionally, the variations prior to ingress and subsequent to egress provide away to probe pressures greater than the maximum tangent pressure that can be probed during transit. Therefore, probing the maximum range of atmospheric altitudes, and in particular the near-surface environment of an Earth-analog exoplanet, will require looking at out-of-transit refracted light in addition to the in-transit spectrum. C1 [Misra, Amit; Meadows, Victoria] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Misra, Amit; Meadows, Victoria; Crisp, Dave] NAI, Virtual Planetary Lab, Seattle, WA USA. [Misra, Amit; Meadows, Victoria] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA. [Crisp, Dave] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Misra, A (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM amit0@astro.washington.edu FU National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement solicitation [NNH05ZDA001C]; ARCS Seattle chapter; Astrobiology program at the University of Washington under an NSF IGERT award FX This work was performed by the NASA Astrobiology Institute's Virtual Planetary Laboratory, supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement solicitation NNH05ZDA001C. This work has also been supported by a generous fellowship from the ARCS Seattle chapter and funding from the Astrobiology program at the University of Washington under an NSF IGERT award. NR 50 TC 15 Z9 15 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2014 VL 792 IS 1 AR 61 DI 10.1088/0004-637X/792/1/61 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100061 ER PT J AU Pawellek, N Krivov, AV Marshall, JP Montesinos, B Abraham, P Moor, A Bryden, G Eiroa, C AF Pawellek, Nicole Krivov, Alexander V. Marshall, Jonathan P. Montesinos, Benjamin Abraham, Peter Moor, Attila Bryden, Geoffrey Eiroa, Carlos TI DISK RADII AND GRAIN SIZES IN HERSCHEL-RESOLVED DEBRIS DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; planetary systems; stars: individual (GJ 581, HD 9672, HD 10647, HD 10939, HD 13161, HD 14055, HD 17848, HD 20320, HD 21997, HD 23484, HD 27290, HD 48682, HD 50571, HD 71155, HD 71722, HD 95086, HD 95418, HD 102647, HD 104860, HD 109085, HD 110411, HD 125162, HD 139006, HD 142091, HD 161868, HD 170773, HD 172167, HD 182681, HD 188228, HD 195627, HD 197481, HD 207129, HD 216956, HD 218396) ID STARS NSTARS PROJECT; MAIN-SEQUENCE STARS; SOLAR-TYPE STAR; PLANET FORMATION; NEARBY STARS; KUIPER-BELT; COLLISIONAL EVOLUTION; DUST DISTRIBUTIONS; SMALL PARTICLES; BETA-PICTORIS AB The radii of debris disks and the sizes of their dust grains are important tracers of the planetesimal formation mechanisms and physical processes operating in these systems. Here we use a representative sample of 34 debris disks resolved in various Herschel Space Observatory (Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA) programs to constrain the disk radii and the size distribution of their dust. While we modeled disks with both warm and cold components, and identified warm inner disks around about two-thirds of the stars, we focus our analysis only on the cold outer disks, i.e., Kuiper-belt analogs. We derive the disk radii from the resolved images and find a large dispersion for host stars of any spectral class, but no significant trend with the stellar luminosity. This argues against ice lines as a dominant player in setting the debris disk sizes, since the ice line location varies with the luminosity of the central star. Fixing the disk radii to those inferred from the resolved images, we model the spectral energy distribution to determine the dust temperature and the grain size distribution for each target. While the dust temperature systematically increases toward earlier spectral types, the ratio of the dust temperature to the blackbody temperature at the disk radius decreases with the stellar luminosity. This is explained by a clear trend of typical sizes increasing toward more luminous stars. The typical grain sizes are compared to the radiation pressure blowout limit S-blow that is proportional to the stellar luminosity-to-mass ratio and thus also increases toward earlier spectral classes. The grain sizes in the disks of G- to A-stars are inferred to be several times S-blow at all stellar luminosities, in agreement with collisional models of debris disks. The sizes, measured in the units of S-blow, appear to decrease with the luminosity, which may be suggestive of the disk's stirring level increasing toward earlier-type stars. The dust opacity index beta ranges between zero and two, and the size distribution index q varies between three and five for all the disks in the sample. C1 [Pawellek, Nicole; Krivov, Alexander V.] Univ Jena, Inst Astrophys, D-07745 Jena, Germany. [Pawellek, Nicole; Krivov, Alexander V.] Univ Jena, Universitatssternwarte, D-07745 Jena, Germany. [Marshall, Jonathan P.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Marshall, Jonathan P.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Marshall, Jonathan P.] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, E-28049 Madrid, Spain. [Montesinos, Benjamin] CSIC, INTA, CAB, Ctr Astrobiol,Dept Astrofis, E-28691 Madrid, Spain. [Abraham, Peter; Moor, Attila] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, H-1525 Budapest, Hungary. [Bryden, Geoffrey] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pawellek, N (reprint author), Univ Jena, Inst Astrophys, Schillergasschen 2-3, D-07745 Jena, Germany. RI Montesinos, Benjamin/C-3493-2017; OI Montesinos, Benjamin/0000-0002-7982-2095; Marshall, Jonathan/0000-0001-6208-1801 FU DFG [Kr 2164/10-1]; Spanish [AYA 2011-26202]; Hungarian Scientific Research Fund [OTKA K101393]; Momentum grant of the MTA CSFK Lend "ulet Disk Research Group FX We thank Amy Bonsor, Grant Kennedy, Torsten Lohne, and Christian Vitense for stimulating discussions. N.P. is grateful to Steve Ertel for useful advice on various aspects of the SED fitting with the thermal annealing algorithm. Insightful and constructive comments of the anonymous referee greatly helped to improve the paper. N.P. and A.V.K. acknowledge support by the DFG through grant Kr 2164/10-1. J.P.M., B.M., C.E. are partly supported by Spanish grant AYA 2011-26202. This work was also partly supported by the grant OTKA K101393 of the Hungarian Scientific Research Fund, and the Momentum grant of the MTA CSFK Lendulet Disk Research Group. NR 107 TC 25 Z9 25 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 SEP 1 PY 2014 VL 792 IS 1 AR 65 DI 10.1088/0004-637X/792/1/65 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100065 ER PT J AU Pullen, AR Benson, AJ Moustakas, LA AF Pullen, Anthony R. Benson, Andrew J. Moustakas, Leonidas A. TI NONLINEAR EVOLUTION OF DARK MATTER SUBHALOS AND APPLICATIONS TO WARM DARK MATTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; dark matter; galaxies: formation; galaxies: halos ID MILKY-WAY SATELLITES; UNIVERSAL DENSITY PROFILE; GALAXY FORMATION; NUMERICAL SIMULATIONS; MASS SUBSTRUCTURE; DWARF GALAXIES; LOCAL GROUP; LAMBDA-CDM; TOO BIG; HALOES AB We describe the methodology to include nonlinear evolution, including tidal effects, in the computation of subhalo distribution properties in both cold (CDM) and warm (WDM) dark matter universes. Using semi-analytic modeling, we include effects from dynamical friction, tidal stripping, and tidal heating, allowing us to dynamically evolve the subhalo distribution. We calibrate our nonlinear evolution scheme to the CDM subhalo mass function in the Aquarius N-body simulation, producing a subhalo mass function within the range of simulations. We find tidal effects to be the dominant mechanism of nonlinear evolution in the subhalo population. Finally, we compute the subhalo mass function for m(chi) = 1.5 keV WDM including the effects of nonlinear evolution, and compare radial number densities and mass density profiles of subhalos in CDM and WDM models. We show that all three signatures differ between the two dark matter models, suggesting that probes of substructure may be able to differentiate between them. C1 [Pullen, Anthony R.; Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Benson, Andrew J.] Carnegie Observ, Pasadena, CA 91101 USA. RP Pullen, AR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM anthony.r.pullen@jpl.nasa.gov RI Pullen, Anthony/I-7007-2015; OI Pullen, Anthony/0000-0002-2091-8738; Moustakas, Leonidas/0000-0003-3030-2360 NR 77 TC 4 Z9 4 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 SEP 1 PY 2014 VL 792 IS 1 AR 24 DI 10.1088/0004-637X/792/1/24 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100024 ER PT J AU Ruel, J Bazin, G Bayliss, M Brodwin, M Foley, RJ Stalder, B Aird, KA Armstrong, R Ashby, MLN Bautz, M Benson, BA Bleem, LE Bocquet, S Carlstrom, JE Chang, CL Chapman, SC Cho, HM Clocchiatti, A Crawford, TM Crites, AT De Haan, T Desai, S Dobbs, MA Dudley, JP Forman, WR George, EM Gladders, MD Gonzalez, AH Halverson, NW Harrington, NL High, FW Holder, GP Holzapfel, WL Hrubes, JD Jones, C Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Liu, J Lueker, M Luong-Van, D Mantz, A Marrone, DP McDonald, M McMahon, JJ Mehl, J Meyer, SS Mocanu, L Mohr, JJ Montroy, TE Murray, SS Natoli, T Nurgaliev, D Padin, S Plagge, T Pryke, C Reichardt, CL Rest, A Ruhl, JE Saliwanchik, BR Saro, A Sayre, JT Schaffer, KK Shaw, L Shirokoff, E Song, J Suhada, R Spieler, HG Stanford, SA Staniszewski, Z Starsk, AA Story, K Stubbs, CW Van Engelen, A Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zahn, O Zenteno, A AF Ruel, J. Bazin, G. Bayliss, M. Brodwin, M. Foley, R. J. Stalder, B. Aird, K. A. Armstrong, R. Ashby, M. L. N. Bautz, M. Benson, B. A. Bleem, L. E. Bocquet, S. Carlstrom, J. E. Chang, C. L. Chapman, S. C. Cho, H. M. Clocchiatti, A. Crawford, T. M. Crites, A. T. De Haan, T. Desai, S. Dobbs, M. A. Dudley, J. P. Forman, W. R. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. Harrington, N. L. High, F. W. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Jones, C. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Liu, J. Lueker, M. Luong-Van, D. Mantz, A. Marrone, D. P. McDonald, M. McMahon, J. J. Mehl, J. Meyer, S. S. Mocanu, L. Mohr, J. J. Montroy, T. E. Murray, S. S. Natoli, T. Nurgaliev, D. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Rest, A. Ruhl, J. E. Saliwanchik, B. R. Saro, A. Sayre, J. T. Schaffer, K. K. Shaw, L. Shirokoff, E. Song, J. Suhada, R. Spieler, H. G. Stanford, S. A. Staniszewski, Z. Starsk, A. A. Story, K. Stubbs, C. W. Van Engelen, A. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zahn, O. Zenteno, A. TI OPTICAL SPECTROSCOPY AND VELOCITY DISPERSIONS OF GALAXY CLUSTERS FROM THE SPT-SZ SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; galaxies: clusters: general ID SOUTH-POLE TELESCOPE; BLANCO COSMOLOGY SURVEY; ZELDOVICH EFFECT SURVEY; 720 SQUARE DEGREES; GREATER-THAN 1; SAMPLE; MASS; ANISOTROPY; REDSHIFTS; CATALOG AB We present optical spectroscopy of galaxies in clusters detected through the Sunyaev-Zel'dovich (SZ) effect with the South Pole Telescope (SPT). We report our own measurements of 61 spectroscopic cluster redshifts, and 48 velocity dispersions each calculated with more than 15 member galaxies. This catalog also includes 19 dispersions of SPT-observed clusters previously reported in the literature. The majority of the clusters in this paper are SPT-discovered; of these, most have been previously reported in other SPT cluster catalogs, and five are reported here as SPT discoveries for the first time. By performing a resampling analysis of galaxy velocities, we find that unbiased velocity dispersions can be obtained from a relatively small number of member galaxies (less than or similar to 30), but with increased systematic scatter. We use this analysis to determine statistical confidence intervals that include the effect of membership selection. We fit scaling relations between the observed cluster velocity dispersions and mass estimates from SZ and X-ray observables. In both cases, the results are consistent with the scaling relation between velocity dispersion and mass expected from dark-matter simulations. We measure a similar to 30% log-normal scatter in dispersion at fixed mass, and a similar to 10% offset in the normalization of the dispersion-mass relation when compared to the expectation from simulations, which is within the expected level of systematic uncertainty. C1 [Ruel, J.; Bayliss, M.; Nurgaliev, D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bazin, G.; Bocquet, S.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Suhada, R.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Bazin, G.; Bocquet, S.; Desai, S.; Liu, J.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [Bayliss, M.; Foley, R. J.; Stalder, B.; Ashby, M. L. N.; Forman, W. R.; Jones, C.; Murray, S. S.; Starsk, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, R. J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Armstrong, R.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bautz, M.; McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Keisler, R.; Leitch, E. M.; Mantz, A.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Natoli, T.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago, Chile. [De Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; Van Engelen, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [George, E. M.; Harrington, N. L.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Lueker, M.; Shirokoff, E.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP Ruel, J (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM mbayliss@cfa.harvard.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; Stubbs, Christopher/C-2829-2012; OI Williamson, Ross/0000-0002-6945-2975; Stubbs, Christopher/0000-0003-0347-1724; Marrone, Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Forman, William/0000-0002-9478-1682; Stark, Antony/0000-0002-2718-9996 FU NASA; National Science Foundation [ANT-0638937]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NSF [AST-1009012, AST-1009649, MRI-0723073]; NASA [12800071, 12800088, 13800883, NAS 8-03060]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; Cluster of Excellence "Origin and Structure of the Universe," - Excellence Initiative of the Federal Government of Germany, EXC project [153]; Clay Fellowship; KICP Fellowship; Pennsylvania State University [2834-MIT-SAO-4018]; Alfred P. Sloan Research Fellowship; Smithsonian Institution; Brinson Foundation; PFB-06 CATA, Chile; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; Blanco 4 m at Cerro Tololo Interamerican Observatories [2005B-0043, 2009B-0400, 2010A-0441, 2010B-0598] FX Optical imaging data from the Blanco 4 m at Cerro Tololo Interamerican Observatories (programs 2005B-0043, 2009B-0400, 2010A-0441, 2010B-0598) are included in this work. Additional imaging data were obtained with the 6.5 m Magellan Telescopes and the Swope telescope, which are located at the Las Campanas Observatory in Chile. This work is based in part on observations made with the Spitzer Space Telescope (PIDs 60099, 70053), 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 South Pole Telescope program is supported by the National Science Foundation through grant ANT-0638937. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012. Galaxy cluster research at SAO is supported in part by NSF grants AST-1009649 and MRI-0723073. Support for X-ray analysis was provided by NASA through Chandra Award Nos. 12800071, 12800088, and 13800883 issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. X-ray research at the CfA is supported through NASA Contract NAS 8-03060. The Munich group was supported by The Cluster of Excellence "Origin and Structure of the Universe," funded by the Excellence Initiative of the Federal Government of Germany, EXC project number 153. R.J.F. is supported by a Clay Fellowship. B. A. B is supported by a KICP Fellowship, M. B. and M. M. acknowledge support from contract 2834-MIT-SAO-4018 from the Pennsylvania State University to the Massachusetts Institute of Technology. M. D. acknowledges support from an Alfred P. Sloan Research Fellowship, W. F. and C.J. acknowledge support from the Smithsonian Institution. B. S. acknowledges support from the Brinson Foundation. A. C. received support from PFB-06 CATA, Chile. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. NR 58 TC 30 Z9 30 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2014 VL 792 IS 1 AR 45 DI 10.1088/0004-637X/792/1/45 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100045 ER PT J AU Skemer, AJ Marley, MS Hinz, PM Morzinski, KM Skrutskie, MF Leisenring, JM Close, LM Saumon, D Bailey, VP Briguglio, R Defrere, D Esposito, S Follette, KB Hill, JM Males, JR Puglisi, A Rodigas, TJ Xompero, M AF Skemer, Andrew J. Marley, Mark S. Hinz, Philip M. Morzinski, Katie M. Skrutskie, Michael F. Leisenring, Jarron M. Close, Laird M. Saumon, Didier Bailey, Vanessa P. Briguglio, Runa Defrere, Denis Esposito, Simone Follette, Katherine B. Hill, John M. Males, Jared R. Puglisi, Alfio Rodigas, Timothy J. Xompero, Marco TI DIRECTLY IMAGED L-T TRANSITION EXOPLANETS IN THE MID-INFRARED SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; infrared: planetary systems; instrumentation: adaptive optics; planets and satellites: atmospheres; planets and satellites: gaseous planets; stars: individual (HR 8799 2M1207 b) ID PLANETARY-MASS COMPANION; NEAR-INFRARED SPECTROSCOPY; YOUNG BROWN DWARF; ORBITING HR 8799; EDGE-ON DISK; GIANT PLANETS; MU-M; EXTRASOLAR PLANET; FINDING CAMPAIGN; CARBON-MONOXIDE AB Gas-giant planets emit a large fraction of their light in the mid-infrared (greater than or similar to 3 mu m), where photometry and spectroscopy are critical to our understanding of the bulk properties of extrasolar planets. Of particular importance are the L- and M-band atmospheric windows (3-5 mu m), which are the longest wavelengths currently accessible to ground-based, high-contrast imagers. We present binocular LBT adaptive optics (AO) images of the HR 8799 planetary system in six narrow-band filters from 3 to 4 mu m, and a Magellan AO image of the 2M1207 planetary system in a broader 3.3 mu m band. These systems encompass the five known exoplanets with luminosities consistent with L -> T transition brown dwarfs. Our results show that the exoplanets are brighter and have shallower spectral slopes than equivalent temperature brown dwarfs in a wavelength range that contains the methane fundamental absorption feature (spanned by the narrow-band filters and encompassed by the broader 3.3 mu m filter). For 2M1207 b, we find that thick clouds and non-equilibrium chemistry caused by vertical mixing can explain the object's appearance. For the HR 8799 planets, we present new models that suggest the atmospheres must have patchy clouds, along with non-equilibrium chemistry. Together, the presence of a heterogeneous surface and vertical mixing presents a picture of dynamic planetary atmospheres in which both horizontal and vertical motions influence the chemical and condensate profiles. C1 [Skemer, Andrew J.; Hinz, Philip M.; Morzinski, Katie M.; Leisenring, Jarron M.; Close, Laird M.; Bailey, Vanessa P.; Defrere, Denis; Follette, Katherine B.; Males, Jared R.; Rodigas, Timothy J.] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA. [Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Leisenring, Jarron M.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Saumon, Didier] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Briguglio, Runa; Esposito, Simone; Puglisi, Alfio; Xompero, Marco] Osserv Astrofis Arcetri, Ist Nazl Astrofis, I-50125 Florence, Italy. [Hill, John M.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. [Rodigas, Timothy J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. RP Skemer, AJ (reprint author), Univ Arizona, Dept Astron, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. RI Marley, Mark/I-4704-2013; OI Esposito, Simone/0000-0002-3114-677X; Xompero, Marco/0000-0002-5565-084X; Marley, Mark/0000-0002-5251-2943; Skemer, Andrew/0000-0001-6098-3924; Morzinski, Katie/0000-0002-1384-0063; Bailey, Vanessa/0000-0002-5407-2806 FU NASA Origins of Solar Systems Program [NNX13AJ17G]; NSF Graduate Research Fellowship Program [DGE-1143953]; National Aeronautics and Space Administration, Exoplanet Exploration program; National Science Foundation [AST-0705296] FX The authors thank Travis Barman for his insightful comments and for supplying his 2M1207 b model. We also thank the anonymous referee for excellent suggestions. This work would not have been possible without the dedication of the LBTI staff, in particular Vidhya Vaitheeswaran, who programmed LBTI's rapid filter changing capabilities. A.S. was supported by the NASA Origins of Solar Systems Program, grant NNX13AJ17G. V.B. is supported by the NSF Graduate Research Fellowship Program (DGE-1143953). The Large Binocular Telescope Interferometer is funded by the National Aeronautics and Space Administration as part of its Exoplanet Exploration program. LMIRCam is funded by the National Science Foundation through grant NSF AST-0705296. NR 88 TC 34 Z9 34 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2014 VL 792 IS 1 AR 17 DI 10.1088/0004-637X/792/1/17 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100017 ER PT J AU Wik, DR Hornstrup, A Molendi, S Madejski, G Harrison, FA Zoglauer, A Grefenstette, BW Gastaldello, F Madsen, KK Westergaard, NJ Ferreira, DDM Kitaguchi, T Pedersen, K Boggs, SE Christensen, FE Craig, WW Hailey, CJ Stern, D Zhang, WW AF Wik, Daniel R. Hornstrup, A. Molendi, S. Madejski, G. Harrison, F. A. Zoglauer, A. Grefenstette, B. W. Gastaldello, F. Madsen, K. K. Westergaard, N. J. Ferreira, D. D. M. Kitaguchi, T. Pedersen, K. Boggs, S. E. Christensen, F. E. Craig, W. W. Hailey, C. J. Stern, D. Zhang, W. W. TI NuSTAR OBSERVATIONS OF THE BULLET CLUSTER: CONSTRAINTS ON INVERSE COMPTON EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (Bullet cluster); intergalactic medium; magnetic fields; radiation mechanisms: non-thermal; X-rays: galaxies: clusters ID X-RAY-SPECTRA; HOTTEST KNOWN CLUSTER; GALAXY CLUSTERS; COMA CLUSTER; MAGNETIC-FIELDS; 1E 0657-56; NONTHERMAL EMISSION; EXCESS EMISSION; XMM-NEWTON; CHANDRA AB The search for diffuse non-thermal inverse Compton (IC) emission from galaxy clusters at hard X-ray energies has been undertaken with many instruments, with most detections being either of low significance or controversial. Because all prior telescopes sensitive at E > 10 keV do not focus light and have degree-scale fields of view, their backgrounds are both high and difficult to characterize. The associated uncertainties result in lower sensitivity to IC emission and a greater chance of false detection. In this work, we present 266 ks NuSTAR observations of the Bullet cluster, which is detected in the energy range 3-30 keV. NuSTAR's unprecedented hard X-ray focusing capability largely eliminates confusion between diffuse IC and point sources; however, at the highest energies, the background still dominates and must be well understood. To this end, we have developed a complete background model constructed of physically inspired components constrained by extragalactic survey field observations, the specific parameters of which are derived locally from data in non-source regions of target observations. Applying the background model to the Bullet cluster data, we find that the spectrum is well-but not perfectly-described as an isothermal plasma with kT = 14.2 +/- 0.2 keV. To slightly improve the fit, a second temperature component is added, which appears to account for lower temperature emission from the cool core, pushing the primary component to kT similar to 15.3 keV. We see no convincing need to invoke an IC component to describe the spectrum of the Bullet cluster, and instead argue that it is dominated at all energies by emission from purely thermal gas. The conservatively derived 90% upper limit on the IC flux of 1.1 x 10(-12) erg s(-1) cm(-2) (50-100 keV), implying a lower limit on B greater than or similar to 0.2 mu G, is barely consistent with detected fluxes previously reported. In addition to discussing the possible origin of this discrepancy, we remark on the potential implications of this analysis for the prospects for detecting IC in galaxy clusters in the future. C1 [Wik, Daniel R.; Zhang, W. W.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wik, Daniel R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Hornstrup, A.; Westergaard, N. J.; Ferreira, D. D. M.; Pedersen, K.; Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Molendi, S.; Gastaldello, F.] INAF, IASF Milano, I-20133 Milan, Italy. [Madejski, G.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Harrison, F. A.; Grefenstette, B. W.; Madsen, K. K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Zoglauer, A.; Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Kitaguchi, T.] RIKEN, Nishina Ctr, Wako, Saitama 3510198, Japan. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wik, DR (reprint author), NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM daniel.r.wik@nasa.gov RI Boggs, Steven/E-4170-2015; Gastaldello, Fabio/N-4226-2015; Ferreira, Desiree/M-1666-2016; OI Boggs, Steven/0000-0001-9567-4224; Gastaldello, Fabio/0000-0002-9112-0184; Ferreira, Desiree/0000-0003-4003-3256; Molendi, Silvano/0000-0002-2483-278X NR 43 TC 51 Z9 51 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 SEP 1 PY 2014 VL 792 IS 1 AR 48 DI 10.1088/0004-637X/792/1/48 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100048 ER PT J AU Zhai, CX Shao, M Nemati, BJ Werne, T Zhou, HY Turyshev, SG Sandhu, J Hallinan, G Harding, LK AF Zhai, Chengxing Shao, Michael Nemati, Bijan Werne, Thomas Zhou, Hanying Turyshev, Slava G. Sandhu, Jagmit Hallinan, Gregg Harding, Leon K. TI DETECTION OF A FAINT FAST-MOVING NEAR-EARTH ASTEROID USING THE SYNTHETIC TRACKING TECHNIQUE SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; atmospheric effects; methods: data analysis; methods: observational; minor planets, asteroids: general ID PHOTOMETRY AB We report a detection of a faint near-Earth asteroid (NEA) using our synthetic tracking technique and the CHIMERA instrument on the Palomar 200 inch telescope. With an apparent magnitude of 23 (H = 29, assuming detection at 20 lunar distances), the asteroid was moving at 6 degrees.32 day(-1) and was detected at a signal-to-noise ratio (S/N) of 15 using 30 s of data taken at a 16.7 Hz frame rate. The detection was confirmed by a second observation 77 minutes later at the same S/N. Because of its high proper motion, the NEA moved 7 arcsec over the 30 s of observation. Synthetic tracking avoided image degradation due to trailing loss that affects conventional techniques relying on 30 s exposures; the trailing loss would have degraded the surface brightness of the NEA image on the CCD down to an approximate magnitude of 25 making the object undetectable. This detection was a result of our 12 hr blind search conducted on the Palomar 200 inch telescope over two nights, scanning twice over six (5 degrees.3 x 0 degrees.046) fields. Detecting only one asteroid is consistent with Harris's estimates for the distribution of the asteroid population, which was used to predict a detection of 1.2 NEAs in the H-magnitude range 28-31 for the two nights. The experimental design, data analysis methods, and algorithms are presented. We also demonstrate milliarcsecond-level astrometry using observations of two known bright asteroids on the same system with synthetic tracking. We conclude by discussing strategies for scheduling observations to detect and characterize small and fast-moving NEAs using the new technique. C1 [Zhai, Chengxing; Shao, Michael; Nemati, Bijan; Werne, Thomas; Zhou, Hanying; Turyshev, Slava G.; Sandhu, Jagmit] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hallinan, Gregg; Harding, Leon K.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. RP Zhai, CX (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM chengxing.zhai@jpl.nasa.gov NR 20 TC 8 Z9 8 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2014 VL 792 IS 1 AR 60 DI 10.1088/0004-637X/792/1/60 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100060 ER PT J AU Zwart, SR Launius, RD Coen, GK Morgan, JLL Charles, JB Smith, SM AF Zwart, Sara R. Launius, Ryan D. Coen, Geoffrey K. Morgan, Jennifer L. L. Charles, John B. Smith, Scott M. TI Body Mass Changes During Long-Duration Spaceflight SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE body mass; energy intake; spaceflight; weightlessness ID INTERNATIONAL-SPACE-STATION; ENERGY-EXPENDITURE; NUTRITIONAL-STATUS; FLIGHT; HUMANS; ASTRONAUTS; BONE AB Background: During early spaceflights, many crewmembers did not meet their caloric requirements and consequently lost body mass during flight, as assessed by a decrease in postflight body mass. Maintaining body mass during spaceflight is crucial for maintaining crew health and monitoring body mass is thus important to medical operations as well as being a key component of human research. Determining body mass becomes difficult in a microgravity environment. Methods: We report data from two mass measurement devices on the International Space Station (ISS): the Russian body mass measuring device (BMMD), which uses spring oscillation physics, and NASA's Space Linear Acceleration Mass Measurement Device (SLAMMD), which uses Newton's second law of motion (F = ma). Results: For 25 crewmembers whose body mass was measured on both devices, significant body mass loss occurred compared to preflight (gravimetric scale) and averaged -4.4% as assessed by BMMD and -2.8% as assessed by SLAMMD. After an initial loss in the first 30 d of flight, body mass remained constant through the rest of the mission, as determined using either device. The mean difference between the two devices was 1.1 kg when the closest SLAMMD and BMMD measurements were compared (6.9 +/- 6.2 d apart). Dietary intake during flight is approximately 80% of the World Health Organization estimated requirement and the decrease in body mass follows in-flight energy intake closely on average. Conclusion: Body mass monitoring is important for monitoring crew health during a mission and to help ensure that crewmembers consume adequate energy intake to mitigate the risks of spaceflight. C1 [Zwart, Sara R.; Launius, Ryan D.; Coen, Geoffrey K.; Morgan, Jennifer L. L.; Charles, John B.; Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA. EM scott.m.smith@nasa.gov FU NASA Human Research Program's Human Health and Countermeasure Element FX We thank the astronauts who participated in these studies for their time and effort, and the staff of the NASA Johnson Space Center Nutritional Biochemistry Laboratory for their efforts in all aspects of carrying out this project. We thank Jane Krauhs for editorial assistance. This study was funded by the NASA Human Research Program's Human Health and Countermeasure Element. NR 21 TC 6 Z9 6 U1 0 U2 6 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD SEP PY 2014 VL 85 IS 9 BP 897 EP 904 DI 10.3357/ASEM.3979.2014 PG 8 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AN7XD UT WOS:000340813400001 PM 25197887 ER PT J AU Somers, JT Gohmert, DM Brinkley, JW AF Somers, Jeffrey T. Gohmert, Dustin M. Brinkley, James W. TI Spacecraft Occupant Protection Requirements: A Review of the Recent Changes SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Review DE injury biomechanics; Hybrid III; multi-axial dynamic response criterion; Brinkley model; anthropomorphic test device; impact biomechanics ID CERVICAL-SPINE; HUMAN RESPONSE; STRUCTURAL-PROPERTIES; SPACEFLIGHT; IMPACTS; INJURY; CONCUSSION; FOOTBALL; MUSCLE; RISK AB NASA has recently updated spacecraft design requirements for protecting crewmembers during dynamic spaceflight phases. The details of the update are available in a NASA publication (NASA TM-2013-217380) and are summarized here. Previously, NASA's occupant protection requirements relied primarily on the multiaxial dynamic response criterion, which NASA refers to as the Brinkley Dynamic Response Criteria (BDRC). Although simple to implement, there are several important ground rules that must be met for the injury predictions to be applicable. These include proper restraint, flail controls, proper seating support, pressure suit considerations, head protection including consideration of helmet mass, and spaceflight deconditioning. Even if these ground rules are met, there are limitations to the model that must be addressed, including: model validation, sex differences, age effects, anthropometry effects, and differences between the physical fitness of military test subjects and future crewmembers. To address these limitations, new injury assessment reference values (IARV) have been prescribed for the 5th percentile female and 95th percentile male Hybrid III anthropomorphic test devices (ATD). These metrics are head-injury criterion, head-rotational acceleration, neck injury criterion, neck-axial-force limits, flail prevention, and lumbar-axial compression force. Using these new ATD IARVs, NASA can have increased confidence that vehicle designs mitigate the risk of injury during dynamic phases of flight. C1 NASA Johnson Space Ctr, Wyle Sci Technol & Engn Grp, Houston, TX USA. NASA Johnson Space Ctr, Crew & Thermal Syst Div, Houston, TX USA. RP Somers, JT (reprint author), 1290 Hercules Dr, Houston, TX 77058 USA. EM jeff.somers@nasa.gov RI Somers, Jeffrey/N-4168-2014 OI Somers, Jeffrey/0000-0003-3347-6614 FU NASA Human Research Program, Johnson Space Center (JSC) Health and Human Performance Directorate; JSC Engineering Directorate; [NAS9-02078] FX This work was funded by the NASA Human Research Program, Johnson Space Center (JSC) Health and Human Performance Directorate, and the JSC Engineering Directorate. Portions of the work were performed under the Bioastronautics Contract (NAS9-02078). In addition, the authors would like especially thank the NASA Engineering and Safety Center and outside experts for their thorough review of the proposed requirements. NR 73 TC 1 Z9 1 U1 1 U2 12 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD SEP PY 2014 VL 85 IS 9 BP 940 EP 948 DI 10.3357/ASEM.4004.2014 PG 9 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AN7XD UT WOS:000340813400007 PM 25197893 ER PT J AU Godinez, A Liston, DB Ayzenberg, R Toscano, WB Cowings, PA Stone, LS AF Godinez, Angelica Liston, Dorion B. Ayzenberg, Ruthie Toscano, William B. Cowings, Patricia A. Stone, Leland S. TI G-Loading and Vibration Effects on Heart and Respiration Rates SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE stress; launch; ascent; interaction; autonomic nervous system ID SUSTAINED ACCELERATION; MECHANICAL IMPEDANCE; BODY AB Background: Operational environments expose pilots and astronauts to sustained acceleration (G loading) and whole-body vibration, alone and in combination. Separately, the physiological effects of G loading and vibration have been well studied; both have effects similar to mild exercise. The few studies of combined G loading and vibration have not reported an interaction between these factors on physiological responses. Methods: We tested the effects of G loading (+1 and +3.8 G(x)) and vibration (0.5 g(x) at 8, 12, and 16 Hz), alone and in combination, on heart and respiration rate. Results: We observed an effect of G loading on heart rate (average increase of 23 bpm, SD: 12) and respiration rate (average increase of 5 breaths per minute, SD: 5), an effect of vibration on heart rate, and an interaction on heart rate. With vibration, we observed heart rate increases of 4 bpm (SD: 3) with no increase in respiration rate. In the +1 G(x) condition, the largest heart rate increase occurred during low-frequency (8 Hz) vibration, while at +3.8 G(x), the largest heart rate increase occurred during high-frequency (16 Hz) vibration, demonstrating interaction. Discussion: Consistent with previous reports, our G-loading and vibration effects are similar to mild exercise. In addition, we observed an interaction between G loading and vibration on heart rate, with maximum heart rates occurring at a higher vibration frequency at +3.8 G(x) compared to +1 G(x). The observed interaction demonstrates that G-loading and vibration effects are not independent and can only be properly assessed during combined exposure. C1 [Godinez, Angelica; Liston, Dorion B.] San Jose State Univ, San Jose, CA 95192 USA. [Ayzenberg, Ruthie] Santa Clara Univ, Santa Clara, CA 95053 USA. [Toscano, William B.; Cowings, Patricia A.; Stone, Leland S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Stone, LS (reprint author), NASA, Ames Res Ctr, Mail Stop 262-2,POB 1, Moffett Field, CA 94035 USA. EM leland.s.stone@nasa.gov FU National Space Biomedical Research Institute [SA002002] FX This work was supported by grant SA002002 from the National Space Biomedical Research Institute. NR 15 TC 2 Z9 2 U1 1 U2 3 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD SEP PY 2014 VL 85 IS 9 BP 949 EP 953 DI 10.3357/ASEM.4015.2014 PG 5 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AN7XD UT WOS:000340813400008 PM 25197894 ER PT J AU Gatti, E Villa, IM Achyuthan, H Gibbard, PL Oppenheimer, C AF Gatti, E. Villa, I. M. Achyuthan, H. Gibbard, P. L. Oppenheimer, C. TI Geochemical variability in distal and proximal glass from the Youngest Toba Tuff eruption SO BULLETIN OF VOLCANOLOGY LA English DT Article DE Youngest Toba Tuff; Chemical variability; Crystal fractionation; Post-depositional alteration; Oldest Toba Tuff ID SOUTH CHINA SEA; SUPER-ERUPTION; VOLCANIC ASH; 75 KA; INDIAN SUBCONTINENT; PENINSULAR INDIA; AR-40/AR-39 AGE; NORTH SUMATRA; TEPHRA; INDONESIA AB The Youngest Toba Tuff (YTT, erupted at ca. 74 ka) is a distinctive and widespread tephra marker across South and Southeast Asia. The climatic, human and environmental consequences of the YTT eruption are widely debated. Although a considerable body of geochemical data is available for this unit, there has not been a systematic study of the variability of the ash geochemistry. Intrinsic (magmatic) and extrinsic (post-depositional) chemical variations bring fundamental information regarding the petrogenesis of the magma, the distribution of the tephra and the interaction between the ash and the receiving environment. Considering the importance of the geochemistry of the YTT for stratigraphic correlations and eruptive models, it is central to the YTT debate to quantify and interpret such variations. Here, we collate all published geochemical data on the YTT glass, including analyses from 67 sites described in the literature and three new samples. Two principal sources of chemical variation are investigated: (i) compositional zonation of the magma reservoir and (ii) post-depositional alteration. Post-depositional leaching is responsible for up to ca. 11 % differences in Na2O/K2O and ca. 1 % differences in SiO2/Al2O3 ratios in YTT glass from marine sites. Continental tephras are 2 % higher in Na2O/K2O and 3 % higher in SiO2/Al2O3 with respect to the marine tephra. We interpret such post-depositional glass alteration as related to seawater-induced alkali migration in marine environments. Crystal fractionation and consequential magmatic differentiation, which produced order-of-magnitude variations in trace element concentrations reported in the literature, also produced major element differences in the YTT glass. FeO/Al2O3 ratios vary by about 50 %, which is analytically significant. These variations represent magmatic fractionation involving Fe-bearing phases. We also compared major element concentrations in YTT and Oldest Toba Tuff (OTT) ash samples, to identify potential compositional differences that could constrain the stratigraphic identity of the Morgaon ash (western India); no differences between the OTT and YTT samples were observed. C1 [Gatti, E.; Gibbard, P. L.; Oppenheimer, C.] Univ Cambridge, Dept Geog, Cambridge CB2 3EN, England. [Villa, I. M.] Univ Bern, Inst Geol, CH-3012 Bern, Switzerland. [Villa, I. M.] Univ Milano Bicocca, I-20126 Milan, Italy. [Achyuthan, H.] Anna Univ, Dept Geol, Chennai 600025, Tamil Nadu, India. RP Gatti, E (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM emma.gatti@jpl.nasa.gov RI Oppenheimer, Clive/G-9881-2013 OI Oppenheimer, Clive/0000-0003-4506-7260 FU Dudley Stamp Memorial Award (Royal Geographical Society); Cambridge-India Partnership; SMUTS Memorial Fund; Philip Lake Fund; Sidney Sussex College; William George Fearnsides Fund (Geological Society of London) FX This work was supported by the Dudley Stamp Memorial Award (Royal Geographical Society), the Cambridge-India Partnership, the SMUTS Memorial Fund, Philip Lake Fund, Sidney Sussex College and the William George Fearnsides Fund (Geological Society of London). We thank Rachna Raj, Alpa Shridar, L.S. Chamyal, N. Karmalkar and V. Kale for support provided during fieldwork. E. G. particularly thanks Steve Boreham, Chris Rolfe, Chiara Petrone and Jason Day for facilitating her work in the Geography Science Laboratories, Department of Geography and in the Department of Earth Sciences at the University of Cambridge. We also thank Sacha Jones for providing ash samples from Jwalapuram and Hermann Kudrass for providing information about the Bay of Bengal cores. We thank the editors and the anonymous reviewers of the original manuscript for their valuable comments. NR 70 TC 3 Z9 3 U1 7 U2 22 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0258-8900 EI 1432-0819 J9 B VOLCANOL JI Bull. Volcanol. PD SEP PY 2014 VL 76 IS 9 AR 859 DI 10.1007/s00445-014-0859-x PG 16 WC Geosciences, Multidisciplinary SC Geology GA AO5EM UT WOS:000341366100009 ER PT J AU Kitamura, K Liou, MS Chang, CH AF Kitamura, Keiichi Liou, Meng-Sing Chang, Chih-Hao TI Extension and Comparative Study of AUSM-Family Schemes for Compressible Multiphase Flow Simulations SO COMMUNICATIONS IN COMPUTATIONAL PHYSICS LA English DT Article DE Multiphase flow; two-fluid model; AUSM-family; stratified flow model ID HYPERSONIC HEATING COMPUTATIONS; GHOST FLUID METHOD; 2-PHASE FLOW; NUMERICAL-METHOD; EULER FLUXES; ACCURATE; INTERFACE; EQUATIONS; MODELS; SEQUEL AB Several recently developed AUSM-family numerical flux functions (SLAU, SLAU2, AUSM(+)-up2, and AUSMPW+) have been successfully extended to compute compressible multiphase flows, based on the stratified flow model concept, by following two previous works: one by M.-S. Liou, C.-H. Chang, L. Nguyen, and T. G. Theofanous [AIAA J. 46:2345-2356, 2008], in which AUSM(+)-up was used entirely, and the other by C.-H. Chang, and M.-S. Liou [J. Comput. Phys. 225:840-873, 2007], in which the exact Riemann solver was combined into AUSM(+)-up at the phase interface. Through an extensive survey by comparing flux functions, the following are found: (1) AUSM(+)-up with dissipation parameters of K-p and K-u equal to 0.5 or greater, AUSMPW+, SLAU2, AUSM(+)-up2, and SLAU can be used to solve benchmark problems, including a shock/water-droplet interaction; (2) SLAU shows oscillatory behaviors [though not as catastrophic as those of AUSM(+) (a special case of AUSM(+)-up with K-p - K-u - 0)] due to insufficient dissipation arising from its ideal-gas-based dissipation term; and (3) when combined with the exact Riemann solver, AUSM(+)-up (K-p = K-u = 1), SLAU2, and AUSMPW+ are applicable to more challenging problems with high pressure ratios. C1 [Kitamura, Keiichi; Liou, Meng-Sing] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Kitamura, Keiichi] JAXAs Engn Digital Innovat JEDI Ctr, JSPS, Chuo Ku, Sagamihara, Kanagawa, Japan. [Kitamura, Keiichi] Nagoya Univ, Chikusa Ku, Nagoya, Aichi 4648603, Japan. [Chang, Chih-Hao] Theofanous & Co Inc, Santa Barbara, CA 93109 USA. RP Kitamura, K (reprint author), Yokohama Natl Univ, Hodogaya Ku, Yokohama, Kanagawa 2408501, Japan. EM kitamura@ynu.ac.jp; meng-sing.liou@nasa.gov; chchang@theofanous.net RI KITAMURA, Keiichi/M-5488-2014 OI KITAMURA, Keiichi/0000-0001-7550-8990 NR 59 TC 2 Z9 2 U1 0 U2 9 PU GLOBAL SCIENCE PRESS PI WANCHAI PA ROOM 3208, CENTRAL PLAZA, 18 HARBOUR RD, WANCHAI, HONG KONG 00000, PEOPLES R CHINA SN 1815-2406 EI 1991-7120 J9 COMMUN COMPUT PHYS JI Commun. Comput. Phys. PD SEP PY 2014 VL 16 IS 3 BP 632 EP 674 DI 10.4208/cicp.020813.190214a PG 43 WC Physics, Mathematical SC Physics GA AN7NS UT WOS:000340787900004 ER PT J AU Hurford, TA Brunt, KM AF Hurford, T. A. Brunt, K. M. TI Antarctic analog for dilational bands on Europa SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Europa; tectonics; Earth analog; Antarctica ID ROSS ICE SHELF; ENCELADUS; MORPHOLOGY; MODEL; TECTONICS; FRACTURES; SURFACE; FLEXURE; RIDGES; TIDES AB Europa's surface shows signs of extension, which is revealed as lithospheric dilation expressed along ridges, dilational bands and ridged bands. Ridges, the most common tectonic feature on Europa, comprise a central crack flanked by two raised banks a few hundred meters high on each side. Together these three classes may represent a continuum of formation. In Tufts' Dilational Model ridge formation is dominated by daily tidal cycling of a crack, which can be superimposed with regional secular dilation. The two sources of dilation can combine to form the various band morphologies observed. New GPS data along a rift on the Ross Ice Shelf, Antarctica is a suitable Earth analog to test the framework of Tufts' Dilational Model. As predicted by Tufts' Dilational Model, tensile failures in the Ross Ice Shelf exhibit secular dilation, upon which a tidal signal can be seen. From this analog we conclude that Tufts' Dilational Model for Europan ridges and bands may be credible and that the secular dilation is most likely from a regional source and not tidally driven. Published by Elsevier B.V. C1 [Hurford, T. A.] NASA, Planetary Syst Lab, Goddard Spaceflight Ctr, Greenbelt, MD 20771 USA. [Brunt, K. M.] Univ Maryland, ESSIC, College Pk, MD 20740 USA. [Brunt, K. M.] NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hurford, TA (reprint author), NASA, Planetary Syst Lab, Goddard Spaceflight Ctr, Greenbelt, MD 20771 USA. EM Terry.A.Hurford@nasa.gov RI Hurford, Terry/F-2625-2012 FU NASA Headquarters FX We thank NASA Headquarters for funding through the Science Innovation Fund (Surface Deformation of Icy Moons: Insights from Earth Analogs and Modeling). We thank Douglas MacAyeal and the NSIDC for Nascent Iceberg GPS data. We thank Jeanne Sauber, Alyssa Rhoden, Wade Henning, Ryan Walker and Tom Neumann for insightful comments and discussions. NR 38 TC 0 Z9 0 U1 2 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD SEP 1 PY 2014 VL 401 BP 275 EP 283 DI 10.1016/j.epsl.2014.05.015 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AO3GV UT WOS:000341218600025 ER PT J AU Kuhn, CE Baker, JD Towell, RG Ream, RR AF Kuhn, Carey E. Baker, Jason D. Towell, Rodney G. Ream, Rolf R. TI Evidence of localized resource depletion following a natural colonization event by a large marine predator SO JOURNAL OF ANIMAL ECOLOGY LA English DT Article DE Callorhinus ursinus; dive behaviour; foraging behaviour; intraspecific competition; northern fur seal; satellite telemetry ID NORTHERN FUR SEALS; CALLORHINUS-URSINUS; PRIBILOF ISLANDS; COLONY SIZE; GEOGRAPHIC STRUCTURE; FORAGING ENERGETICS; DENSITY-DEPENDENCE; ASHMOLES HALO; ELEPHANT SEAL; POPULATION AB 1. For central place foragers, forming colonies can lead to extensive competition for prey around breeding areas and a zone of local prey depletion. As populations grow, this area of reduced prey can expand impacting foraging success and forcing animals to alter foraging behaviour. 2. Here, we examine a population of marine predators, the northern fur seal (Callorhinus ursinus), which colonized a recently formed volcanic island, and assess changes in foraging behaviour associated with increasing population density. Specifically, we measured pup production and adult foraging behaviour over a 15-year period, during which the population increased 4-fold. 3. Using measures of at-sea movements and dive behaviour, we found clear evidence that as the population expanded, animals were required to allot increasing effort to obtain resources. These changes in behaviour included longer duration foraging trips, farther distances travelled, a larger foraging range surrounding the island and deeper maximum dives. 4. Our results suggest that as the northern fur seal population increased, local prey resources were depleted as a result of increased intraspecific competition. In addition, the recent slowing of population growth indicates that this population may be approaching carrying capacity just 31 years after a natural colonization event. 5. Our study offers insight into the dynamics of population growth and impacts of increasing population density on a large marine predator. Such data could be vital for understanding future population fluctuations that occur in response to the dynamic environment, as natural and anthropogenic factors continue to modify marine habitats. C1 [Kuhn, Carey E.; Towell, Rodney G.; Ream, Rolf R.] NOAA, Natl Marine Mammal Lab, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98115 USA. [Baker, Jason D.] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96822 USA. RP Kuhn, CE (reprint author), NOAA, Natl Marine Mammal Lab, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 7600 Sand Point Way NE, Seattle, WA 98115 USA. EM Carey.Kuhn@noaa.gov FU University of Alaska Fairbanks; North Pacific Research Board FX This research was conducted under Marine Mammal Protection Act permit numbers 782-1455, 782-1694, 782-1708. A. Banks, K. Call, B. Fadely, T. Gelatt, J. L. Guerrero, J. Sterling, J. Thomason and M. Williams assisted with field research. J. Thomason, B. Walker and T. Zeppelin provided diet analysis, and D. Johnson assisted with statistical analysis and data processing. Funding and personnel were also contributed by the University of Alaska Fairbanks and the North Pacific Research Board. Additional logistic support was provided by R. Brewer, the US Fish and Wildlife Service (M/V Tiglax), and J. and A. MacDonald. The findings and conclusions in the study are those of the author(s) and do not necessarily represent the views of the National Marine Fisheries Service, NOAA. Reference to trade names does not imply endorsement by the National Marine Fisheries Service, NOAA. NR 58 TC 10 Z9 10 U1 3 U2 25 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8790 EI 1365-2656 J9 J ANIM ECOL JI J. Anim. Ecol. PD SEP PY 2014 VL 83 IS 5 BP 1169 EP 1177 DI 10.1111/1365-2656.12202 PG 9 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA AN8TP UT WOS:000340877700017 PM 24450364 ER PT J AU Frazier, BS Driggers, WB Adams, DH Jones, CM Loefer, JK AF Frazier, B. S. Driggers, W. B., III Adams, D. H. Jones, C. M. Loefer, J. K. TI Validated age, growth and maturity of the bonnethead Sphyrna tiburo in the western North Atlantic Ocean SO JOURNAL OF FISH BIOLOGY LA English DT Article DE longevity; elasmobranch; life history; oxytetracycline ID GULF-OF-MEXICO; RHIZOPRIONODON-TERRAENOVAE RICHARDSON; SHARPNOSE SHARK; LIFE-HISTORY; CARCHARHINUS-ACRONOTUS; CHONDRICHTHYAN FISHES; BLACKNOSE SHARK; 2 POPULATIONS; CONSISTENCY; PRECISION AB The age, growth and maturity of bonnetheads Sphyrna tiburo inhabiting the estuarine and coastal waters of the western North Atlantic Ocean (WNA) from Onslow Bay, North Carolina, south to West Palm Beach, Florida, were examined. Vertebrae were collected and aged from 329 females and 217 males ranging in size from 262 to 1043 mm and 245 to 825 mm fork length, L-F, respectively. Sex-specific von Bertalanffy growth curves were fitted to length-at-age data. Female von Bertalanffy parameters were L-infinity = 1036 mm L-F, k = 0.18, t(0) = -1.64 and L-0 = 272 mm L-F. Males reached a smaller theoretical asymptotic length and had a higher growth coefficient (L-infinity = 782 mm L-F, k = 0.29, t(0) = -1.43 and L-0 = 266 mm L-F). Maximum observed age was 17.9 years for females and 16.0 years for males. Annual deposition of growth increments was verified by marginal increment analysis and validated for age classes 2.5+ to 10.5+ years through recapture of 13 oxytetracycline-injected specimens at liberty in the wild for 1-4 years. Length (L-F50) and age (A(50)) at 50% maturity were 819 mm and 6.7 years for females, and 618 mm and 3.9 years for males. Both female and male S. tiburo in the WNA had a significantly higher maximum observed age, L-F50, A(50) and L-infinity, and a significantly lower k and estimated L-0 than evident in the Gulf of Mexico (GOM). These significant differences in life-history parameters, as well as evidence from tagging and genetic studies, suggest that S. tiburo in the WNA and GOM should be considered separate stocks. (C) 2014 The Fisheries Society of the British Isles C1 [Frazier, B. S.] South Carolina Dept Nat Resources, Charleston, SC 29412 USA. [Driggers, W. B., III; Jones, C. M.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA. [Adams, D. H.] Florida Fish & Wildlife Conservat Commiss, Fish & Wildlife Res Inst, Melbourne, FL 32901 USA. [Loefer, J. K.] Univ S Carolina, Dept Biol Sci, Columbia, SC 29208 USA. RP Frazier, BS (reprint author), South Carolina Dept Nat Resources, 217 Ft Johnson Rd, Charleston, SC 29412 USA. EM frazierb@dnr.sc.gov FU Cooperative Atlantic States Shark Pupping and Nursery Habitat Survey (COASTSPAN); U.S. Department of the Interior; U.S. Fish and Wildlife Service; Federal Aid for Sportfish Restoration Project [F-43]; State of Florida saltwater recreational fishing licence monies FX We are especially grateful to the many folks who helped make this study possible. C. Hendrix, J. Richardson, D. Shiffman, H. Davega, J. Tucker, A. Shaw and P. Webster helped with field work, specimen collection, workup and vertebrae prepping. We received advice, support and guidance from many colleagues including: E. Levesque, G. Ulrich, J. Gelsleichter, J. Carlson, E. Cortes, L. Natanson, J. Neer and C. McCandless. K. Ware and J. Henne of Bears Bluff National Fish Hatchery were critical to age validation work. This work was conducted as part of the Master's in Environmental Science programme at the College of Charleston, and we thank committee members, A. Strand and S. Arnott as well as directors T. Callahan and M. McConnell for their support. Funding for this study was provided by the Cooperative Atlantic States Shark Pupping and Nursery Habitat Survey (COASTSPAN) and, in part, by funding from the U.S. Department of the Interior, U.S. Fish and Wildlife Service, Federal Aid for Sportfish Restoration Project Number F-43 and by State of Florida saltwater recreational fishing licence monies. Collection of specimens was performed under SCDNR Scientific Permit #2212, and as such this study was granted an IACUC exemption. We appreciate the guidance of the editors and two anonymous reviewers who greatly improved the manuscript. This is contribution 719 of the South Carolina Marine Resources Center. NR 52 TC 4 Z9 4 U1 5 U2 30 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1112 EI 1095-8649 J9 J FISH BIOL JI J. Fish Biol. PD SEP PY 2014 VL 85 IS 3 BP 688 EP 712 DI 10.1111/jfb.12450 PG 25 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA AN8HR UT WOS:000340845500009 PM 25040650 ER PT J AU Gyekenyesi, A AF Gyekenyesi, Andrew TI Techniques for monitoring damage in ceramic matrix composites SO JOURNAL OF INTELLIGENT MATERIAL SYSTEMS AND STRUCTURES LA English DT Review DE Ceramic matrix composite; electrical resistance; cracking; nondestructive evaluation; damage; ultrasonics; acoustic emissions; thermography; impedance-based structural health monitoring; thermoelastic stress analysis ID ELECTRICAL-RESISTANCE; PULSED THERMOGRAPHY; SENSORS AB This article offers a review of various nondestructive evaluation and structural health monitoring techniques that have been successfully utilized for assessing the damage state of woven ceramic matrix composites consisting of silicon carbide fibers and silicon carbide matrices. The techniques include acousto-ultrasonics, modal acoustic emissions, electrical resistance, impedance-based structural health monitoring, pulsed thermography, as well as thermoelastic stress analysis. The damage, in the form of distributed matrix cracks and delaminations, was introduced using multiple tactics. These included load/unload/reload uniaxial tensile tests, creep tests, and ballistic impact. Although other nondestructive evaluation techniques have been applied to this material system, the select nondestructive evaluation tools described here are limited to approaches that are of current research interest within programs at the NASA Glenn Research Center. C1 NASA, Ohio Aerosp Inst, Glenn Res Ctr, Lewis Field, Cleveland, OH 44135 USA. RP Gyekenyesi, A (reprint author), NASA, Ohio Aerosp Inst, Glenn Res Ctr, Lewis Field, 21000 Brookpk Rd,Mail Stop 6-1, Cleveland, OH 44135 USA. EM Andrew.L.Gyekenyesi@nasa.gov FU NASA Glenn Research Center at Lewis Field; Vehicle Systems Safety Technologies Project (Aviation Safety Program) under NASA [NNC07BA13B] FX This study was supported by the NASA Glenn Research Center at Lewis Field and the Vehicle Systems Safety Technologies Project (Aviation Safety Program) under NASA Contract Number-NNC07BA13B. NR 31 TC 0 Z9 0 U1 3 U2 41 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1045-389X EI 1530-8138 J9 J INTEL MAT SYST STR JI J. Intell. Mater. Syst. Struct. PD SEP PY 2014 VL 25 IS 13 BP 1531 EP 1540 DI 10.1177/1045389X13510221 PG 10 WC Materials Science, Multidisciplinary SC Materials Science GA AN8BV UT WOS:000340827400001 ER PT J AU Taylor, PC AF Taylor, Patrick C. TI Variability of Regional TOA Flux Diurnal Cycle Composites at the Monthly Time Scale SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID OUTGOING LONGWAVE RADIATION; HYDROLOGIC-CYCLE; CLOUD COVER; BUDGET; STRATOCUMULUS; CONVECTION; TROPICS; MODEL; LAYER; CIRCULATION AB Diurnal variability is a fundamental component of Earth's climate system. Clouds, temperature, and precipitation exhibit robust responses to the daily cycle of solar insolation. Recent work indicates significant variability in the top-of-the-atmosphere (TOA) flux diurnal cycle in the tropics associated with monthly changes in the cloud diurnal cycle evolution. It has been proposed that the observed month-to-month variations in the TOA flux diurnal cycle are caused by anomalies in the atmospheric dynamic and thermodynamic state. This hypothesis is tested using a regression analysis to quantify the relationship between diurnal cycle shape and the atmospheric dynamic and thermodynamic state. TOA radiative fluxes are obtained from Clouds and the Earth's Radiant Energy System (CERES) Edition 3 data and the atmospheric dynamic and thermodynamic state is taken from the European Centre for Medium-Range Weather Forecasts (ECMWF) Interim Re-Analysis. Four regions representing traditional diurnal cycle regimes are used in this analysis: North Africa (land nonconvective), central South America (land convective), Peru marine stratocumulus (ocean nonconvective), and Indian Ocean (ocean convective). The results show a statistically significant diurnal cycle shape change and cloud response related to monthly atmospheric state anomalies. Using the single-variable regression relationships to predict monthly diurnal cycle variability shows improvements of 1%-18% over assuming a climatological diurnal cycle shape; the most significant gains are found in North Africa. The proposed hypothesis, therefore, contributes to diurnal cycle variability explaining at least 10%-20% of the total monthly-mean diurnal cycle variability. C1 [Taylor, Patrick C.] NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA. RP Taylor, PC (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd,Mail Stop 420, Hampton, VA 23681 USA. EM patrick.c.taylor@nasa.gov RI Taylor, Patrick/D-8696-2015 OI Taylor, Patrick/0000-0002-8098-8447 FU NASA Energy and Water Cycle Study program [NNH10ZDA001N] FX The author would like to thank the anonymous reviewers for their insightful comments, which significantly improved the clarity of this manuscript. This work is supported by the NASA Energy and Water Cycle Study program through Grant NNH10ZDA001N. The CERES data used in this study are stored at the Atmospheric Science Data Center at NASA Langley (https://eosweb.larc.nasa.gov). ERA-Interim data used in this study are stored at the ECMWF data server (http://data-portal.ecmwf.int/datald/interim_nmthl). NR 40 TC 3 Z9 3 U1 0 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 EI 1520-0469 J9 J ATMOS SCI JI J. Atmos. Sci. PD SEP PY 2014 VL 71 IS 9 BP 3484 EP 3498 DI 10.1175/JAS-D-13-0336.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AO3KC UT WOS:000341227100022 ER PT J AU Tompson, SR AF Tompson, Sara R. TI Predator: The Secret Origins of the Drone Revolution SO LIBRARY JOURNAL LA English DT Book Review C1 [Tompson, Sara R.] Jet Prop Lab Lib, Pasadena, CA 91109 USA. RP Tompson, SR (reprint author), Jet Prop Lab Lib, Pasadena, CA 91109 USA. NR 1 TC 0 Z9 0 U1 1 U2 6 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 1 PY 2014 VL 139 IS 14 BP 123 EP 124 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA AO1MJ UT WOS:000341075900203 ER PT J AU Tompson, SR AF Tompson, Sara R. TI The Large Hadron Collider: The Extraordinary Story of the Higgs Boson and Other Stuff That Will Blow Your Mind SO LIBRARY JOURNAL LA English DT Book Review C1 [Tompson, Sara R.] Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA 91109 USA. RP Tompson, SR (reprint author), Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA 91109 USA. NR 1 TC 0 Z9 0 U1 1 U2 4 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 1 PY 2014 VL 139 IS 14 BP 135 EP + PG 2 WC Information Science & Library Science SC Information Science & Library Science GA AO1MJ UT WOS:000341075900247 ER PT J AU Pfaller, JB Alfaro-Shigueto, J Balazs, GH Ishihara, T Kopitsky, K Mangel, JC Peckham, SH Bolten, AB Bjorndal, KA AF Pfaller, Joseph B. Alfaro-Shigueto, Joanna Balazs, George H. Ishihara, Takashi Kopitsky, Kerry Mangel, Jeffrey C. Peckham, S. Hoyt Bolten, Alan B. Bjorndal, Karen A. TI Hitchhikers reveal cryptic host behavior: new insights from the association between Planes major and sea turtles in the Pacific Ocean SO MARINE BIOLOGY LA English DT Article ID CENTRAL NORTH PACIFIC; FEEDING HABITAT USE; CARETTA-CARETTA; LEPIDOCHELYS-OLIVACEA; CHELONIA-MYDAS; LOGGERHEAD TURTLES; COLUMBUS CRABS; SATELLITE TELEMETRY; CARAPACE EPIBIONTS; DEPTH DISTRIBUTION AB Studies that incorporate information from habitat-specific ecological interactions (e.g., epibiotic associations) can reveal valuable insights into the cryptic habitat-use patterns and behavior of marine vertebrates. Sea turtles, like other large, highly mobile marine vertebrates, are inherently difficult to study, and such information can inform the implementation of conservation measures. The presence of epipelagic epibionts, such as the flotsam crab Planes major, on sea turtles strongly suggests that neritic turtles have recently occupied epipelagic habitats (upper 200 m in areas with > 200 m depth) and that epipelagic turtles spend time at or near the surface. We quantified the effects of turtle species, turtle size, and habitat (neritic or epipelagic) on the frequency of epibiosis (F (0)) by P. major on sea turtles in the Pacific Ocean. In neritic habitats, we found that loggerhead (F (0) = 27.6 %) and olive ridley turtles (F (0) = 26.2 %) host crabs frequently across a wide range of body sizes, and green turtles almost never host crabs (F (0) = 0.7 %). These results suggest that loggerheads and olive ridleys display variable/flexible epipelagic-neritic transitions, while green turtles tend to transition unidirectionally at small body sizes. In epipelagic habitats, we found that loggerheads host crabs (F (0) = 92.9 %) more frequently than olive ridleys (F (0) = 50 %) and green turtles (F (0) = 38.5 %). These results suggest that epipelagic loggerheads tend to spend more time at or near the surface than epipelagic olive ridleys and green turtles. Results of this study reveal new insights into habitat-use patterns and behavior of sea turtles and display how epibiont data can supplement data from more advanced technologies to gain a better understanding of the ecology of marine vertebrates during cryptic life stages. C1 [Pfaller, Joseph B.; Bolten, Alan B.; Bjorndal, Karen A.] Univ Florida, Archie Carr Ctr Sea Turtle Res, Dept Biol, Gainesville, FL 32611 USA. [Pfaller, Joseph B.] Caretta Res Project, Savannah, GA 31412 USA. [Alfaro-Shigueto, Joanna; Mangel, Jeffrey C.] ProDelphinus, Lima 630204 18, Peru. [Alfaro-Shigueto, Joanna; Mangel, Jeffrey C.] Univ Exeter, Ctr Ecol & Conservat, Penryn TR10 9EZ, Cornwall, England. [Balazs, George H.] NOAA, Marine Turtle Res Program, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA. [Ishihara, Takashi] Sea Turtle Assoc Japan, Osaka, Japan. [Ishihara, Takashi] Suma Aqualife Pk, Kobe, Hyogo, Japan. [Kopitsky, Kerry] Rising Tides Restorat, Dover, DE 19904 USA. [Peckham, S. Hoyt] Stanford Univ, Ctr Ocean Solut, Pacific Grove, CA 93950 USA. RP Pfaller, JB (reprint author), Univ Florida, Archie Carr Ctr Sea Turtle Res, Dept Biol, Gainesville, FL 32611 USA. EM jpfaller@ufl.edu OI Bjorndal, Karen/0000-0002-6286-1901 NR 62 TC 3 Z9 3 U1 3 U2 20 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD SEP PY 2014 VL 161 IS 9 BP 2167 EP 2178 DI 10.1007/s00227-014-2498-3 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AN8QT UT WOS:000340869600017 ER PT J AU Inoue, M Matheou, G Teixeira, J AF Inoue, M. Matheou, G. Teixeira, J. TI LES of a Spatially Developing Atmospheric Boundary Layer: Application of a Fringe Method for the Stratocumulus to Shallow Cumulus Cloud Transition SO MONTHLY WEATHER REVIEW LA English DT Article ID LARGE-EDDY SIMULATION; SEA-SURFACE TEMPERATURE; SUBGRID-STRESS MODEL; NUMERICAL-SIMULATION; FLOW AB An arrangement of a large-eddy simulation (LES) is described that facilitates a spatially developing thermally stratified atmospheric boundary layer (ABL). When the inflow and outflow boundary conditions are specified, the LES of stably stratified ABL turns out to be challenging because spurious reflections of waves at the boundary accumulate inside the domain. To tackle this problem, a fringe method with an auxiliary LES running concurrently is applied to enforce upstream/downstream boundary conditions. An artificial forcing term is applied within a fringe region located at the beginning of the main LES domain in order to ensure statistically stationary inflow boundary conditions. The auxiliary LES, which is horizontally homogeneous in a doubly periodic domain, is used to determine the inflow condition of the main LES domain. The present scheme is used to provide an Eulerian perspective of the stratocumulus to shallow cumulus cloud (Sc-Cu) transition, one of the key cloud regimes over the subtropical ocean. In this study, the transition is triggered by increasing the sea surface temperature (SST) and the LES runs until a statistically steady evolution of the Sc-Cu transition is achieved. The flow statistics are compared with those from a recycling-type method and it is found that the fringe method is more suitable for the current applications. C1 [Inoue, M.; Matheou, G.; Teixeira, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Inoue, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM michio.inoue@jpl.nasa.gov FU Office of Naval Research, Marine Meteorology Program [N00014111P20087, N0001411IP20069]; NASA MAP Program; NOAA/CPO MAPP Program FX The authors acknowledge the support provided by the Office of Naval Research, Marine Meteorology Program under Awards N00014111P20087 and N0001411IP20069, the NASA MAP Program, and the NOAA/CPO MAPP Program. Helpful discussions with K. Suselj and K. Suzuki (JPL) are also greatly acknowledged. 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 32 TC 3 Z9 3 U1 0 U2 7 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 EI 1520-0493 J9 MON WEATHER REV JI Mon. Weather Rev. PD SEP PY 2014 VL 142 IS 9 BP 3418 EP 3424 DI 10.1175/MWR-D-13-00400.1 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AO2QU UT WOS:000341171100021 ER PT J AU Smith, SM Castaneda-Sceppa, C O'Brien, KO Abrams, SA Gillman, P Brooks, NE Cloutier, GJ Heer, M Zwart, SR Wastney, ME AF Smith, S. M. Castaneda-Sceppa, C. O'Brien, K. O. Abrams, S. A. Gillman, P. Brooks, N. E. Cloutier, G. J. Heer, M. Zwart, S. R. Wastney, M. E. TI Calcium kinetics during bed rest with artificial gravity and exercise countermeasures SO OSTEOPOROSIS INTERNATIONAL LA English DT Article DE Biochemical markers of bone turnover; Exercise; Microgravity; Nutrition; Space flight ID INDUCED BONE LOSS; AMINO-ACID SUPPLEMENTATION; RESISTANCE EXERCISE; SPACE-FLIGHT; ENERGY DEFICIT; METABOLISM; SPACEFLIGHT; WEIGHTLESSNESS; RESORPTION; RECOVERY AB We assessed the potential for countermeasures to lessen the loss of bone calcium during bed rest. Subjects ingested less calcium during bed rest, and with artificial gravity, they also absorbed less calcium. With exercise, they excreted less calcium. To retain bone during bed rest, calcium intake needs to be maintained. This study aims to assess the potential for artificial gravity (AG) and exercise (EX) to mitigate loss of bone calcium during space flight. We performed two studies: (1) a 21-day bed rest (BR) study with subjects receiving 1 h/day AG (n = 8) or no AG (n = 7) and (2) a 28-day BR study with 1 h/day resistance EX (n = 10) or no EX (n = 3). In both studies, stable isotopes of Ca were administered orally and intravenously, at baseline and after 10 days of BR, and blood, urine, and feces were sampled for up to 14 days post dosing. Tracers were measured using thermal ionization mass spectrometry. Data were analyzed by compartmental modeling. Less Ca was absorbed during BR, resulting in lower Ca balance in BR+AG (-6.04 +/- 3.38 mmol/day, P = 0.023). However, Ca balance did not change with BR+EX, even though absorbed Ca decreased and urinary Ca excretion increased, because endogenous excretion decreased, and there was a trend for increased bone deposition (P = 0.06). Urinary N-telopeptide excretion increased in controls during BR, but not in the EX group. Markers of bone formation were not different between treatment groups for either study. Ca intake decreased during BR (by 5.4 mmol/day in the AG study and 2.8 mmol/day in the EX study), resulting in lower absorbed Ca. During BR (or space flight), Ca intake needs to be maintained or even increased with countermeasures such as exercise, to enable maintenance of bone Ca. C1 [Smith, S. M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Castaneda-Sceppa, C.; Cloutier, G. J.] Northeastern Univ, Boston, MA 02115 USA. [O'Brien, K. O.] Cornell Univ, Ithaca, NY USA. [Abrams, S. A.] ARS, Baylor Coll Med, USDA, Childrens Nutr Res Ctr, Houston, TX USA. [Gillman, P.] EASI, Houston, TX USA. [Brooks, N. E.] Univ Stirling, Stirling FK9 4LA, Scotland. [Heer, M.] Univ Bonn, Bonn, Germany. [Zwart, S. R.] Univ Space Res Assoc, Houston, TX USA. [Wastney, M. E.] Metab Modeling, W Lafayette, IN USA. RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Attn Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA. EM scott.m.smith@nasa.gov OI Abrams, Steven/0000-0003-4972-9233 FU NASA Flight Analogs Project of NASA's Human Research Program; National Center for Advancing Translational Sciences, National Institutes of Health [1UL1RR029876-01]; National Space Biomedical Research Institute (NSBRI) [NCC 9-58]; U.S. Department of Agriculture's Agricultural Research Service [58-1950-9-001]; National Institutes of Health GCRC [M01-RR-000054] FX We thank the subjects for their time and willingness to participate in these studies. We thank the staff of the UTMB Institute for Translational Sciences Clinical Research Center for their assistance with the AG study and the Tufts University GCRC for their support in conducting the exercise study. We thank the staff of the U.S. National Aeronautics and Space Administration (NASA) Johnson Space Center Nutritional Biochemistry Laboratory for their assistance in processing and analyzing the samples and in all aspects of carrying out this project. We thank Jane Krauhs for editorial assistance. The AG study was funded in part by the NASA Flight Analogs Project of NASA's Human Research Program and in part by grant 1UL1RR029876-01 from the National Center for Advancing Translational Sciences, National Institutes of Health. The exercise study was supported by the National Space Biomedical Research Institute (NSBRI) through NCC 9-58, by agreement 58-1950-9-001 from the U.S. Department of Agriculture's Agricultural Research Service, and by a grant M01-RR-000054 from the National Institutes of Health GCRC. NR 26 TC 2 Z9 2 U1 2 U2 7 PU SPRINGER LONDON LTD PI LONDON PA 236 GRAYS INN RD, 6TH FLOOR, LONDON WC1X 8HL, ENGLAND SN 0937-941X EI 1433-2965 J9 OSTEOPOROSIS INT JI Osteoporosis Int. PD SEP PY 2014 VL 25 IS 9 BP 2237 EP 2244 DI 10.1007/s00198-014-2754-x PG 8 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA AN6AK UT WOS:000340675200010 PM 24861908 ER PT J AU Cheung, KC Tachi, T Calisch, S Miura, K AF Cheung, Kenneth C. Tachi, Tomohiro Calisch, Sam Miura, Koryo TI Origami interleaved tube cellular materials SO SMART MATERIALS AND STRUCTURES LA English DT Article DE rigid origami; metametrial; cellular structure; dimensional scaling analysis AB A novel origami cellular material based on a deployable cellular origami structure is described. The structure is bi-directionally flat-foldable in two orthogonal (x and y) directions and is relatively stiff in the third orthogonal (z) direction. While such mechanical orthotropicity is well known in cellular materials with extruded two dimensional geometry, the interleaved tube geometry presented here consists of two orthogonal axes of interleaved tubes with high interfacial surface area and relative volume that changes with fold-state. In addition, the foldability still allows for fabrication by a flat lamination process, similar to methods used for conventional expanded two dimensional cellular materials. This article presents the geometric characteristics of the structure together with corresponding kinematic and mechanical modeling, explaining the orthotropic elastic behavior of the structure with classical dimensional scaling analysis. C1 [Cheung, Kenneth C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Tachi, Tomohiro] Univ Tokyo, Dept Gen Syst Studies, Meguro Ku, Tokyo 1538902, Japan. [Calisch, Sam] MIT, Ctr Bits & Atoms, Cambridge, MA 02139 USA. [Miura, Koryo] Univ Tokyo, Tokyo 1538902, Japan. RP Cheung, KC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM kenneth.c.cheung@nasa.gov; tachi@idea.c.u-tokyo.ac.jp; sam.calisch@cba.mit.edu; miurak@gakushikai.jp FU NASA Ames Research Center; University of Tokyo; MIT Center for Bits and Atoms; NASA STMD Center Innovation Fund; JST Presto Program FX The authors would like to acknowledge the support of the NASA Ames Research Center, the University of Tokyo, and the MIT Center for Bits and Atoms. The first author's contributions were supported by the NASA STMD Center Innovation Fund. The second author is supported by the JST Presto Program. NR 26 TC 14 Z9 14 U1 0 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0964-1726 EI 1361-665X J9 SMART MATER STRUCT JI Smart Mater. Struct. PD SEP PY 2014 VL 23 IS 9 AR 094012 DI 10.1088/0964-1726/23/9/094012 PG 10 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA AO1MX UT WOS:000341077700014 ER PT J AU Peng, TS Saxena, A Goebel, K Xiang, YB Liu, YM AF Peng, Tishun Saxena, Abhinav Goebel, Kai Xiang, Yibing Liu, Yongming TI Integrated experimental and numerical investigation for fatigue damage diagnosis in composite plates SO STRUCTURAL HEALTH MONITORING-AN INTERNATIONAL JOURNAL LA English DT Article DE Composite; Lamb wave; delamination; matrix cracking; finite element model ID LAMB WAVE-PROPAGATION; SIMULATION AB An integrated experimental and numerical investigation of fatigue damage diagnosis in composite plates is presented in this study. First, the fatigue testing setup for carbon-carbon composite coupons is described with corresponding health monitoring approach through Lamb wave-based diagnostic data collection. In order to study the effects of degradation evolution, a finite element model is used to simulate the effect on Lamb wave propagation due to fatigue-induced delamination and matrix cracking. Simulation results are compared with the experimental testing to first validate the model and then develop several features as potential damage indicators. A parametric study is conducted on the effects of varying degrees of delamination and matrix cracking on these features. Results from the model simulations are presented along with the data analysis and discussions on the capability and limitations of the approach. Finally, some conclusions are drawn and future work is proposed based on the results obtained so far. C1 [Peng, Tishun; Xiang, Yibing; Liu, Yongming] Arizona State Univ, Sch Engn Matter Transport & Energy, Tempe, AZ 85287 USA. [Saxena, Abhinav] NASA, SGT, Ames Res Ctr, Moffett Field, CA USA. [Goebel, Kai] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Liu, YM (reprint author), Arizona State Univ, Sch Engn Matter Transport & Energy, Tempe, AZ 85287 USA. EM yongming.liu@asu.edu FU National Aeronautical and Space Administration (NASA) through Global Engineering and Materials, Inc. (GEM) [NNX12CA86C] FX The research reported in this article was partially supported by the National Aeronautical and Space Administration (NASA) through Global Engineering and Materials, Inc. (GEM) under the project NNX12CA86C. NR 27 TC 1 Z9 1 U1 0 U2 6 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1475-9217 EI 1741-3168 J9 STRUCT HEALTH MONIT JI Struct. Health Monit. PD SEP PY 2014 VL 13 IS 5 BP 537 EP 547 DI 10.1177/1475921714532992 PG 11 WC Engineering, Multidisciplinary; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA AO2WP UT WOS:000341187700004 ER PT J AU Stebner, AP Bigelow, GS Yang, J Shukla, DP Saghaian, SM Rogers, R Garg, A Karaca, HE Chumlyakov, Y Bhattacharya, K Noebe, RD AF Stebner, Aaron P. Bigelow, Glen S. Yang, Jin Shukla, Dhwanil P. Saghaian, Sayed M. Rogers, Richard Garg, Anita Karaca, Haluk E. Chumlyakov, Yuriy Bhattacharya, Kaushik Noebe, Ronald D. TI Transformation strains and temperatures of a nickel-titanium-hafnium high temperature shape memory alloy SO ACTA MATERIALIA LA English DT Article DE Orientation; Texture; Precipitates; Grain boundaries; Transformation strain ID NI SINGLE-CRYSTALS; MARTENSITIC-TRANSFORMATION; YIELD SURFACE; TEXTURE; TENSION; PHASE; MICROSTRUCTURE; POLYCRYSTALS; COMPRESSION; BEHAVIOR AB A combined experimental and theoretical investigation of the transformation temperature and transformation strain behaviors of a promising new Ni50.3Ti29.7Hf20 high-temperature shape memory alloy was conducted. Actuation behavior of single crystals with loading orientations near [0 0 1](B2), [(1) over bar 1 0](B2), and [1 1 1](B2), as well as polycrystalline material in aged and unaged conditions was studied, together with the superelastic, polycrystalline torsion response. These results were compared to analytic calculations of the ideal transformation strains for tension, compression, and torsion loading of single crystals as a function of single crystal orientation, and polycrystalline material of common processing textures. H-phase precipitates on the order of 10-30 nm were shown to increase transformation temperatures and also to narrow thermal hysteresis, compared to unaged material. The mechanical effects of increased residual stresses and numbers of transformation nucleation sites caused by the precipitates provide a plausible explanation for the observed transformation temperature trends. Grain boundaries were shown to have similar effects on transformation temperatures. The work output and recoverable strain exhibited by the alloy were shown to approach maximums at stresses of 500-800 MPa, suggesting these to be optimal working loads with respect to single cycle performance. The potential for transformation strain in single crystals of this material was calculated to be superior to binary NiTi in tension, compression, and torsion loading modes. However, the large volume fraction of precipitate phase, in part, prevents the material from realizing its full single crystal transformation strain potential in return for outstanding functional stability by inhibiting plastic strain accumulation during transformation. Finally, calculations showed that of the studied polycrystalline textures, [0 0 1](B2) fiber texture results in superior torsion performance, while [0 1 1](B2) fiber texture results in superior tensile behavior, and both [0 1 1](B2) and random textures will result in the best possible compression performance. (C) 2014 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Stebner, Aaron P.; Yang, Jin; Shukla, Dhwanil P.; Bhattacharya, Kaushik] CALTECH, Pasadena, CA 91125 USA. [Bigelow, Glen S.; Rogers, Richard; Noebe, Ronald D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Saghaian, Sayed M.; Karaca, Haluk E.] Univ Kentucky, Lexington, KY 40506 USA. [Garg, Anita] Univ Toledo, Toledo, OH 43606 USA. [Chumlyakov, Yuriy] Tomsk State Univ, Siberian Phys Tech Inst, Tomsk 634050, Russia. RP Stebner, AP (reprint author), Colorado Sch Mines, 1610 Illinois St, Golden, CO 80401 USA. EM astebner@mines.edu RI Stebner, Aaron/A-7685-2015; Chumlyakov, Yuriy/R-6496-2016 FU NASA's Fundamental Aeronautics Program, Aeronautical Sciences Project; California Institute of Technology Summer Undergraduate Research Fellowship; Tsien fellowship at the California Institute of Technology FX This work was supported by NASA's Fundamental Aeronautics Program, Aeronautical Sciences Project. D.P.S. acknowledges the support of a California Institute of Technology Summer Undergraduate Research Fellowship. J.Y. acknowledges a Tsien fellowship that supported his undergraduate research at the California Institute of Technology. NR 50 TC 11 Z9 12 U1 9 U2 43 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 SEP 1 PY 2014 VL 76 BP 40 EP 53 DI 10.1016/j.actamat.2014.04.071 PG 14 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA AN1GJ UT WOS:000340330400004 ER PT J AU Nesbitt, JA AF Nesbitt, James A. TI Rate of Sublimation of Yb14MnSb11, a Thermoelectric Material for Space Power Applications SO JOURNAL OF ELECTRONIC MATERIALS LA English DT Article DE Zintl; Yb14MnSb11; sublimation; Yb2O3; oxidation ID PERFORMANCE; OXIDATION; YB14MN1-XALXSB11; YB14-XCAXMNSB11; TRANSITION; EFFICIENCY; CORROSION; ALLOYS AB The compound Yb14MnSb11 is a p-type thermoelectric material of interest for space power applications. However, average rates of sublimation previously measured at 1000A degrees C were unacceptably high. In at least one study, Yb2O3 was observed on the surface after testing. In this study, the rate of sublimation of Yb14MnSb11 was measured at 1000A degrees C by use of a vacuum thermogravimetric analyzer (TGA) which continuously measures weight loss as a result of sublimation. This experiment revealed that the rate of sublimation decreased with time, but also resulted in formation of Yb2O3 on the surface, even though the base pressure at the start of the test was 1.9 x 10(-4) Pa (1.4 x 10(-6) torr). Subsequently, the effect of the Yb2O3 on the rate of sublimation was evaluated by performing interrupted vacuum furnace tests in which the sample was weighed after exposure at 1000A degrees C for different times. During the weighing periods, the accumulated oxide scale was either completely removed or left to accumulate further on the surface. The interrupted furnace tests showed that formation of Yb2O3 on the surface was the likely cause of the reduction in the rate of sublimation of the Yb14MnSb11 when measured by use of the vacuum TGA, at least for the measured test duration. Therefore, uncoated material in the vacuum of space, where oxygen is absent, would be likely to sublime at a continuous rate in excess of 5 x 10(-3) g/cm(2)/h. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Nesbitt, JA (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM JNesbitt@nasa.gov FU Radioisotope Power Systems Office at the NASA Glenn Research Center under the Technology Advancement Project, Advanced Thermoelectric Couple (ATEC) Program FX Supply of the Yb14MnSb11 material by the Jet Propulsion Laboratory in Pasadena, CA,, USA, is gratefully acknowledged. This work was funded by the Radioisotope Power Systems Office at the NASA Glenn Research Center under the Technology Advancement Project, Advanced Thermoelectric Couple (ATEC) Program. NR 29 TC 3 Z9 3 U1 3 U2 20 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0361-5235 EI 1543-186X J9 J ELECTRON MATER JI J. Electron. Mater. PD SEP PY 2014 VL 43 IS 9 BP 3128 EP 3137 DI 10.1007/s11664-014-3261-8 PG 10 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA AN1SJ UT WOS:000340363600010 ER PT J AU Skonieczny, K Moreland, SJ Asnani, VM Creager, CM Inotsume, H Wettergreen, DS AF Skonieczny, Krzysztof Moreland, Scott J. Asnani, Vivake M. Creager, Colin M. Inotsume, Hiroaki Wettergreen, David S. TI Visualizing and Analyzing Machine-soil Interactions using Computer Vision SO JOURNAL OF FIELD ROBOTICS LA English DT Article ID BEHAVIOR; MOTION; SCALE; FIELD; FLOW AB This work presents an experimental method for visualizing and analyzing machine-soil interactions, namely the soil optical flow technique (SOFT). SOFT uses optical flow and clustering techniques to process images of soil interacting with a wheel or tool from photos taken through a glass wall of a soil bin. It produces results that are far richer than past approaches that utilized long-exposure photography. It achieves a performance comparable to particle image velocimetry or particle tracking velocimetry, but without the need for specialized measurement equipment or specially marked soil particles. The processing technique demonstrates robustness to different soil types. Ground-truth and cross-validation experiments exhibit subpixel accuracy in estimating soil motions. An example of an application of this technique for field robotics research is the detailed study of push-rolling for slope climbing and soft soil traverse. Push-rolling advances a vehicle by rolling a subset of its wheels while changing its wheelbase to keep the other wheels static and pushing against the ground. Experiments show that push-rolling achieves higher net traction than conventional rolling. Observing the two aspects of push-rolling (rolling and horizontal pushing) using SOFT shows that they result in entirely different forms of soil shearing ("grip failure" and "ground failure," respectively). SOFT also demonstrates how the direction of soil motion is more efficiently utilized for horizontal thrust by pushing than conventional rolling. Ongoing work utilizing SOFT has also demonstrated its potential use in studying excavation tool interactions, the effects of grousers on wheel efficiency, as well as a variety of other wheel-soil interactions. (C) 2014 Wiley Periodicals, Inc. C1 [Skonieczny, Krzysztof; Moreland, Scott J.] Carnegie Mellon Univ, Field Robot Ctr, Pittsburgh, PA 15213 USA. [Asnani, Vivake M.; Creager, Colin M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Inotsume, Hiroaki; Wettergreen, David S.] Carnegie Mellon Univ, Field Robot Ctr, Pittsburgh, PA 15213 USA. RP Skonieczny, K (reprint author), Carnegie Mellon Univ, Field Robot Ctr, 5000 Forbes Ave, Pittsburgh, PA 15213 USA. EM kskoniec@cmu.edu NR 28 TC 5 Z9 5 U1 1 U2 14 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1556-4959 EI 1556-4967 J9 J FIELD ROBOT JI J. Field Robot. PD SEP-OCT PY 2014 VL 31 IS 5 SI SI BP 753 EP 769 DI 10.1002/rob.21510 PG 17 WC Robotics SC Robotics GA AN2PF UT WOS:000340427100003 ER PT J AU Punge, HJ Bedka, KM Kunz, M Werner, A AF Punge, H. J. Bedka, K. M. Kunz, M. Werner, A. TI A new physically based stochastic event catalog for hail in Europe SO NATURAL HAZARDS LA English DT Article DE Hail; Climatology; Overshooting top; Europe ID DEEP CONVECTIVE CLOUDS; SATELLITE-OBSERVATIONS; SIZE DISTRIBUTIONS; SEVERE HAILSTORMS; KINETIC-ENERGY; CLIMATOLOGY; RADAR; DAMAGE; STORM; TOP AB Hailstorms represent one of the major sources of damage and insurance loss to residential, commercial, and agricultural assets in several parts of Central Europe. However, there is little knowledge of hail risk across Europe beyond local historical damage reports due to the relative rarity of severe hail events and the lack of uniform detection methods. Here we present a new stochastic catalog of hailstorms for Europe. It is based on satellite observations of overshooting cloud tops (OT) that indicate very strong convective updrafts and hail reports from the European Severe Weather Database (ESWD). Historic hail events are defined based on OT detections from satellite infrared brightness temperatures between 2004 and 2011 for the warm seasons (April-September). The satellite-based historical event properties are complemented by hailstone observations from ESWD to stochastically simulate more than 1 million individual events with an event footprint resolution of 10 km. The final hail event catalog presented in this paper is the first one with a spatial event distribution that is based on a single homogeneous observation source over Europe. Areas of high hail probability or hail risk are found over Central and Southern Europe, including mountainous regions such as the Alps or the Pyrenees. Another region of relatively high hail risk is present over central Eastern Europe. C1 [Punge, H. J.; Kunz, M.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76021 Karlsruhe, Germany. [Punge, H. J.] Willis Ltd, Willis Res Network, London, England. [Bedka, K. M.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA. [Werner, A.] Willis Re GmbH & Co KG, Munich, Germany. RP Punge, HJ (reprint author), Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76021 Karlsruhe, Germany. EM punge@kit.edu RI Kunz, Michael/B-1186-2013 FU Willis as part of Willis Research Network (WRN); Center for Disaster Management and Risk Reduction Technology (CEDIM) FX H.J.P. was funded as part of his Research Fellowship by Willis as part of Willis Research Network (WRN). The Center for Disaster Management and Risk Reduction Technology (CEDIM) supports the research on natural hazards at the Karlsruhe Institute of Technology (KIT) and the German Research Center for Geosciences (GFZ). The authors thank ESWD, European Severe Weather Database (eswd.eu) for providing hail report data. The authors also thank the GOES-R Algorithm Working Group for support in the development of the objective overshooting convective cloud top detection algorithm. The comments of two anonymous reviewers helped to improve this manuscript. NR 77 TC 11 Z9 11 U1 3 U2 15 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0921-030X EI 1573-0840 J9 NAT HAZARDS JI Nat. Hazards PD SEP PY 2014 VL 73 IS 3 BP 1625 EP 1645 DI 10.1007/s11069-014-1161-0 PG 21 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Water Resources SC Geology; Meteorology & Atmospheric Sciences; Water Resources GA AN3MQ UT WOS:000340492700026 ER PT J AU Brown, ME Grace, K Shively, G Johnson, KB Carroll, M AF Brown, Molly E. Grace, Kathryn Shively, Gerald Johnson, Kiersten B. Carroll, Mark TI Using satellite remote sensing and household survey data to assess human health and nutrition response to environmental change SO POPULATION AND ENVIRONMENT LA English DT Article DE DHS; NDVI; Environment; Health; Survey; Nutrition ID NET PRIMARY PRODUCTION; LAND DEGRADATION; FOOD SECURITY; MODIS DATA; CLIMATE; BIODIVERSITY; AVHRR; NDVI; AGRICULTURE; SEASONALITY AB Climate change and degradation of ecosystem services functioning may threaten the ability of current agricultural systems to keep up with demand for adequate and inexpensive food and for clean water, waste disposal and other broader ecosystem services. Human health is likely to be affected by changes occurring across multiple geographic and time scales. Impacts range from increasing transmissibility and the range of vectorborne diseases, such as malaria and yellow fever, to undermining nutrition through deleterious impacts on food production and concomitant increases in food prices. This paper uses case studies to describe methods that make use of satellite remote sensing and Demographic and Health Survey data to better understand individual-level human health and nutrition outcomes. By bringing these diverse datasets together, the connection between environmental change and human health outcomes can be described through new research and analysis. C1 [Brown, Molly E.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Grace, Kathryn] Univ Utah, Salt Lake City, UT 84112 USA. [Shively, Gerald] Purdue Univ, W Lafayette, IN 47907 USA. [Shively, Gerald] Norwegian Univ Life Sci, Dept Econ & Resource Management, N-1432 As, Norway. [Johnson, Kiersten B.] Westat Corp, Rockville, MD 20850 USA. [Carroll, Mark] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA. RP Brown, ME (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA. EM molly.e.brown@nasa.gov RI Brown, Molly/E-2724-2010 OI Brown, Molly/0000-0001-7384-3314 NR 67 TC 10 Z9 10 U1 2 U2 32 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0199-0039 EI 1573-7810 J9 POPUL ENVIRON JI Popul. Env. PD SEP PY 2014 VL 36 IS 1 BP 48 EP 72 DI 10.1007/s11111-013-0201-0 PG 25 WC Demography; Environmental Studies SC Demography; Environmental Sciences & Ecology GA AN4NZ UT WOS:000340566100003 ER PT J AU Maynard, DJ Trial, JG AF Maynard, Desmond J. Trial, Joan G. TI The use of hatchery technology for the conservation of Pacific and Atlantic salmon SO REVIEWS IN FISH BIOLOGY AND FISHERIES LA English DT Article DE Salmon; Oncorhynchus; Salmo salar; Conservation; Hatchery ID COLUMBIA-RIVER; BIOECONOMIC CONTRIBUTION; WILD POPULATIONS; COHO SALMON; FISHERIES; SALAR; ENHANCEMENT; WASHINGTON; ISSUES; BROODS AB Hatchery technology has been employed for the conservation of Pacific (Oncorhynchus spp.) and Atlantic salmon (Salmo salar) for over 140 years. The initial societal paradigm was that nature is inefficient and hatcheries could be used to conserve stocks that were over utilized or suffering habitat degradation. Although these early hatcheries failed to meet their conservation objectives, they succeeded in developing the spawning-to-swimup fry culture technology used today. In the 1930s the paradigm shifted to artificial and natural production being equally effective and led to the closure of Federal hatcheries in areas with intact freshwater habitat. Hatcheries were maintained to mitigate for habitat loss from hydropower development. With the development of cost effective smolt production technology by 1960, the paradigm returned to nature being inefficient and ushered in the massive conservation utilization production of Pacific salmon that continues to this day. The early 1990s saw another paradigm shift with nature's inefficiency recognized as being the foundation for evolution to maintain the fitness of salmon in their natural environment. This shift gave rise to a focus for hatchery technology to preserve stocks in their native habitats. Using hatcheries for preservation-conservation has become the norm for Atlantic salmon in the USA and Atlantic Canada and for Pacific salmon stocks listed under the Endangered Species Act in the USA or as species at risk in Canada. C1 [Maynard, Desmond J.] NOAA, Resource Utilizat & Technol Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Manchester, WA 98353 USA. [Trial, Joan G.] Maine Dept Marine Resources, Div Sea Run Fisheries & Habitat, Bangor, ME USA. RP Maynard, DJ (reprint author), NOAA, Resource Utilizat & Technol Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, POB 130, Manchester, WA 98353 USA. EM des.maynard@noaa.gov; joan.trial@maine.gov NR 80 TC 3 Z9 3 U1 6 U2 37 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3166 EI 1573-5184 J9 REV FISH BIOL FISHER JI Rev. Fish. Biol. Fish. PD SEP PY 2014 VL 24 IS 3 SI SI BP 803 EP 817 DI 10.1007/s11160-013-9341-7 PG 15 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA AN2ZS UT WOS:000340455200008 ER PT J AU Trail, M Tsimpidi, AP Liu, P Tsigaridis, K Rudokas, J Miller, P Nenes, A Hu, Y Russell, AG AF Trail, M. Tsimpidi, A. P. Liu, P. Tsigaridis, K. Rudokas, J. Miller, P. Nenes, A. Hu, Y. Russell, A. G. TI Sensitivity of air quality to potential future climate change and emissions in the United States and major cities SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Climate change; Air quality; Sensitivity; CMAQ; Downscaling; Projecting emissions ID US ANTHROPOGENIC AEROSOLS; MODEL; SCENARIOS; OZONE; GENERATION; MORTALITY; BURDEN; HEALTH AB Simulated present and future air quality is compared for the years 2006-2010 and 2048-2052 over the contiguous United States (CONUS) using the Community Multi-scale Air Quality (CMAQ) model. Regionally downscaled present and future climate results are developed using GISS and the Weather Research Forecasting (WRF) model. Present and future emissions are estimated using MARKAL 9R model. O-3 and PM2.5 sensitivities to precursor emissions for the years 2010 and 2050 are calculated using CMAQ-DDM (Direct Decoupled Method). We find major improvements in future U.S. air quality including generally decreased MDA8 (maximum daily 8-hr average O-3) mixing ratios and PM2.5 concentrations and reduced frequency of NAAQS O-3 standard exceedances in most major U.S. cities. The Eastern and Pacific U.S. experience the largest reductions in summertime seasonal average MDA8 (up to 12 ppb) with localized decreases in the 4th highest MDA8 of the year, decreasing by up to 25 ppb. Results from a Climate Penalty (CP) scenario isolate the impact of climate change on air quality and show that future climate change tends to increase O-3 mixing ratios in some regions of the U.S., with climate change causing increases of over 10 ppb in the annual 4th highest MDA8 in Los Angeles. Seasonal average PM2.5 decreases (2-4 mu g m(-3)) over the Eastern U.S. are accounted for by decreases in sulfate and nitrate concentrations resulting from reduced mobile and point source emissions of NOx and SOx. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Trail, M.; Tsimpidi, A. P.; Liu, P.; Hu, Y.; Russell, A. G.] Georgia Inst Technol, Sch Civil & Environm Engn, Atlanta, GA 30332 USA. [Liu, P.; Nenes, A.] Georgia Inst Technol, Sch Chem & Biomol Engn, Atlanta, GA 30332 USA. [Tsigaridis, K.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. [Tsigaridis, K.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Rudokas, J.; Miller, P.] Northeast States Coordinated Air Use Management, Boston, MA 02111 USA. [Nenes, A.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. RP Trail, M (reprint author), Georgia Inst Technol, Sch Civil & Environm Engn, Atlanta, GA 30332 USA. EM mcus2rail@gmail.com RI Hu, Yongtao/H-7543-2016 OI Hu, Yongtao/0000-0002-5161-0592 FU US EPA [EPA-G2008-STAR-J1]; NASA FX While this work was supported, in part, by grants from the US EPA (EPA-G2008-STAR-J1) and NASA, reference herein to any specific commercial products, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply their endorsement or recommendation. The views and opinions of authors expressed herein are those of the authors and do not necessarily state or reflect those of the United States Government. NR 41 TC 15 Z9 16 U1 6 U2 69 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD SEP PY 2014 VL 94 BP 552 EP 563 DI 10.1016/j.atmosenv.2014.05.079 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AN1AY UT WOS:000340316300060 ER PT J AU Duncan, BN Prados, AI Lamsal, LN Liu, Y Streets, DG Gupta, P Hilsenrath, E Kahn, RA Nielsen, JE Beyersdorf, AJ Burton, SP Fiore, AM Fishman, J Henze, DK Hostetler, CA Krotkov, NA Lee, P Lin, MY Pawson, S Pfister, G Pickering, KE Pierce, RB Yoshida, Y Ziemba, LD AF Duncan, Bryan N. Prados, Ana I. Lamsal, Lok N. Liu, Yang Streets, David G. Gupta, Pawan Hilsenrath, Ernest Kahn, Ralph A. Nielsen, J. Eric Beyersdorf, Andreas J. Burton, Sharon P. Fiore, Arlene M. Fishman, Jack Henze, Daven K. Hostetler, Chris A. Krotkov, Nickolay A. Lee, Pius Lin, Meiyun Pawson, Steven Pfister, Gabriele Pickering, Kenneth E. Pierce, R. Bradley Yoshida, Yasuko Ziemba, Luke D. TI Satellite data of atmospheric pollution for US air quality applications: Examples of applications, summary of data end-user resources, answers to FAQs, and common mistakes to avoid SO ATMOSPHERIC ENVIRONMENT LA English DT Review DE Satellite data; Air quality; End-user resources; Remote sensing ID AEROSOL OPTICAL DEPTH; OZONE MONITORING EXPERIMENT; RETRIEVAL ALGORITHM; TROPOSPHERIC OZONE; ECONOMIC RECESSION; ISOPRENE EMISSIONS; NITROGEN-OXIDES; UNITED-STATES; NOX EMISSIONS; MEXICO-CITY AB Satellite data of atmospheric pollutants are becoming more widely used in the decision-making and environmental management activities of public, private sector and non-profit organizations. They are employed for estimating emissions, tracking pollutant plumes, supporting air quality forecasting activities, providing evidence for "exceptional event" declarations, monitoring regional long-term trends, and evaluating air quality model output. However, many air quality managers are not taking full advantage of the data for these applications nor has the full potential of satellite data for air quality applications been realized. A key barrier is the inherent difficulties associated with accessing, processing, and properly interpreting observational data. A degree of technical skill is required on the part of the data end-user, which is often problematic for air quality agencies with limited resources. Therefore, we 1) review the primary uses of satellite data for air quality applications, 2) provide some background information on satellite capabilities for measuring pollutants, 3) discuss the-many resources available to the end-user for accessing, processing, and visualizing the data, and 4) provide answers to common questions in plain language. Published by Elsevier Ltd. C1 [Duncan, Bryan N.; Prados, Ana I.; Lamsal, Lok N.; Gupta, Pawan; Kahn, Ralph A.; Krotkov, Nickolay A.; Pawson, Steven; Pickering, Kenneth E.; Yoshida, Yasuko] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Prados, Ana I.; Hilsenrath, Ernest] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA. [Lamsal, Lok N.; Gupta, Pawan] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA. [Liu, Yang] Emory Univ, Rollins Sch Publ Hlth, Atlanta, GA 30322 USA. [Streets, David G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Hilsenrath, Ernest] Sigma Space Corp, Lanham, MD USA. [Nielsen, J. Eric; Yoshida, Yasuko] Sci Syst & Applicat Inc, Lanham, MD USA. [Beyersdorf, Andreas J.; Burton, Sharon P.; Hostetler, Chris A.; Ziemba, Luke D.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Fiore, Arlene M.] Columbia Univ, Dept Earth & Environm Sci, Palisades, NY USA. [Fiore, Arlene M.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Fishman, Jack] St Louis Univ, St Louis, MO 63103 USA. [Henze, Daven K.] Univ Colorado, Boulder, CO 80309 USA. [Lee, Pius] NOAA, College Pk, MD USA. [Lin, Meiyun] Princeton Univ, Princeton, NJ 08544 USA. [Lin, Meiyun] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Pfister, Gabriele] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Pierce, R. Bradley] NOAA, Madison, WI USA. RP Duncan, BN (reprint author), NASA, Goddard Space Flight Ctr, Code 614, Greenbelt, MD 20771 USA. EM Bryan.N.Duncan@nasa.gov RI Lin, Meiyun/D-6107-2013; Pierce, Robert Bradley/F-5609-2010; Krotkov, Nickolay/E-1541-2012; Lee, Pius/D-5201-2016; Pickering, Kenneth/E-6274-2012; Pawson, Steven/I-1865-2014; Duncan, Bryan/A-5962-2011 OI Lin, Meiyun/0000-0003-3852-3491; Pierce, Robert Bradley/0000-0002-2767-1643; Krotkov, Nickolay/0000-0001-6170-6750; Pawson, Steven/0000-0003-0200-717X; FU NASA Air Quality Applied Sciences Team (AQAST); Applied Remote SEnsing Training (ARSET) program, within NASA's Applied Sciences Program FX This work was funded by the NASA Air Quality Applied Sciences Team (AQAST) and the Applied Remote SEnsing Training (ARSET) program, within NASA's Applied Sciences Program. We thank Ginger Butcher, the NASA Aura Mission's education and public outreach lead, for her comments which greatly improved the readability of the article. NR 89 TC 29 Z9 29 U1 4 U2 71 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD SEP PY 2014 VL 94 BP 647 EP 662 DI 10.1016/j.atmosenv.2014.05.061 PG 16 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AN1AY UT WOS:000340316300069 ER PT J AU Stapleton, SE Pineda, EJ Gries, T Waas, AM AF Stapleton, Scott E. Pineda, Evan J. Gries, Thomas Waas, Anthony M. TI Adaptive shape functions and internal mesh adaptation for modeling progressive failure in adhesively bonded joints SO INTERNATIONAL JOURNAL OF SOLIDS AND STRUCTURES LA English DT Article DE Adhesion; Bonded; Crack; Finite element; Joining; Numerical methods; Adaptive shape functions; Adaptive mesh ID COMPOSITE JOINTS; FINITE-ELEMENT; LAP JOINTS; ELASTIC-FOUNDATION; STIFFNESS-MATRIX; ANALYSIS TOOLS; ORDER THEORY; BEAMS; CRITERION; STRENGTH AB Macroscopic finite elements are elements with an embedded analytical solution that can capture detailed local fields, enabling more efficient, mesh independent finite element analysis. The shape functions are determined based on the analytical model rather than prescribed. This method was applied to adhesively bonded joints to model joint behavior with one element through the thickness. This study demonstrates two methods of maintaining the fidelity of such elements during adhesive non-linearity and cracking without increasing the mesh needed for an accurate solution. The first method uses adaptive shape functions, where the shape functions are recalculated at each load step based on the softening of the adhesive. The second method is internal mesh adaption, where cracking of the adhesive within an element is captured by further discretizing the element internally to represent the partially cracked geometry. By keeping mesh adaptations within an element, a finer mesh can be used during the, analysis without affecting the global finite element model mesh. Examples are shown which highlight when each method is most effective in reducing the number of elements needed to capture adhesive nonlinearity and cracking. These methods are validated against analogous finite element models utilizing cohesive zone elements. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Stapleton, Scott E.; Gries, Thomas] Rhein Westfal TH Aachen, Inst Textile Technol, D-52074 Aachen, Germany. [Pineda, Evan J.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. [Waas, Anthony M.] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48105 USA. RP Stapleton, SE (reprint author), Rhein Westfal TH Aachen, Inst Textile Technol, D-52074 Aachen, Germany. EM sstaple@umich.edu FU Space Vehicle Technology Institute [NCC3-989]; NASA; U.S. Department of Defense; NASA John H. Glenn Research Center at Lewis Field through the NASA Graduate Student Researchers Project Fellowship FX Portions of this work were financially supported by the Space Vehicle Technology Institute under Grant No. NCC3-989, jointly funded by NASA and the U.S. Department of Defense. The bulk of the financial support was provided by NASA John H. Glenn Research Center at Lewis Field through the NASA Graduate Student Researchers Project Fellowship. NR 43 TC 2 Z9 2 U1 2 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0020-7683 EI 1879-2146 J9 INT J SOLIDS STRUCT JI Int. J. Solids Struct. PD SEP PY 2014 VL 51 IS 18 BP 3252 EP 3264 DI 10.1016/j.ijsolstr.2014.05.022 PG 13 WC Mechanics SC Mechanics GA AM8QC UT WOS:000340141100023 ER PT J AU Porst, JP Bandler, SR Adams, JS Balvin, MA Busch, SE Eckart, ME Kelley, RL Kilbourne, CA Lee, SJ Nagler, PC Porter, FS Sadleir, JE Seidel, GM Smith, SJ Stevenson, TR AF Porst, J. -P. Bandler, S. R. Adams, J. S. Balvin, M. A. Busch, S. E. Eckart, M. E. Kelley, R. L. Kilbourne, C. A. Lee, S. J. Nagler, P. C. Porter, F. S. Sadleir, J. E. Seidel, G. M. Smith, S. J. Stevenson, T. R. TI Characterization and Performance of Magnetic Calorimeters for Applications in X-ray Spectroscopy SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Magnetic calorimeter; Microcalorimeter; X-ray; Spectrometer; Multiplexing ID HIGH-RESOLUTION AB We have developed prototype arrays of metallic magnetic calorimeters for applications in X-ray astronomy. Each pixel consists of an all-gold X-ray absorber in good thermal contact to a gold-erbium paramagnetic thin film thermometer that is operated in the temperature range of 30-100 mK. The para-magnetic response is coupled to a SQUID amplifier. We have characterized pixels in an array and observed the expected temperature dependence of the magnetization and heat capacity. We have demonstrated a full width at half maximum energy resolution of 1.7 0.1 eV at 6 keV and have also read out these devices using time-division multiplexing. C1 [Porst, J. -P.; Bandler, S. R.; Adams, J. S.; Balvin, M. A.; Busch, S. E.; Eckart, M. E.; Kelley, R. L.; Kilbourne, C. A.; Lee, S. J.; Nagler, P. C.; Porter, F. S.; Sadleir, J. E.; Smith, S. J.; Stevenson, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Porst, J. -P.] CRESST, Columbia, MD 21044 USA. [Porst, J. -P.] USRA, Columbia, MD 21044 USA. [Bandler, S. R.] CRESST, College Pk, MD 20742 USA. [Bandler, S. R.] Univ Maryland, College Pk, MD 20742 USA. [Adams, J. S.; Eckart, M. E.; Smith, S. J.] CRESST, Baltimore, MD 21250 USA. [Adams, J. S.; Eckart, M. E.; Smith, S. J.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Busch, S. E.; Lee, S. J.] NASA, Postdoctoral Program, Oakridge, TN USA. [Nagler, P. C.; Seidel, G. M.] Brown Univ, Providence, RI 02912 USA. RP Porst, JP (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM jpporst@gmail.com; Simon.R.Bandler@nasa.gov RI Bandler, Simon/A-6258-2010; Smith, Stephen/B-1256-2008; Lee, Sang Jun/A-3892-2015; Porter, Frederick/D-3501-2012 OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675; Lee, Sang Jun/0000-0002-8199-3993; Porter, Frederick/0000-0002-6374-1119 FU NASA Office of Space Science ROSES program [NNX12AL50G] FX We would like to thank J. Beyer of the Physikalisch-Technische Bundesanstalt (PTB) in Berlin for providing the SQUIDs used in these measurements and for many useful and stimulating discussions. We gratefully acknowledge the financial support of NASA Office of Space Science ROSES program, contract NNX12AL50G. NR 10 TC 6 Z9 6 U1 0 U2 6 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 617 EP 623 DI 10.1007/s10909-013-1019-y PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400001 ER PT J AU Shirokoff, E Barry, PS Bradford, CM Chattopadhyay, G Day, P Doyle, S Hailey-Dunsheath, S Hollister, MI Kovacs, A Leduc, HG McKenney, CM Mauskopf, P Nguyen, HT O'Brient, R Padin, S Reck, TJ Swenson, LJ Tucker, CE Zmuidzinas, J AF Shirokoff, E. Barry, P. S. Bradford, C. M. Chattopadhyay, G. Day, P. Doyle, S. Hailey-Dunsheath, S. Hollister, M. I. Kovacs, A. Leduc, H. G. McKenney, C. M. Mauskopf, P. Nguyen, H. T. O'Brient, R. Padin, S. Reck, T. J. Swenson, L. J. Tucker, C. E. Zmuidzinas, J. TI Design and Performance of SuperSpec: An On-Chip, KID-Based, mm-Wavelength Spectrometer SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Kinetic inductance detectors; Resonators; Millimeter-wavelength; Spectroscopy ID ASTRONOMY AB SuperSpec is an ultra-compact spectrometer-on-a-chip for mm and submm wavelength astronomy. Its very small size, wide spectral bandwidth, and highly multiplexed detector readout will enable construction of powerful multi-object spectrometers for observations of galaxies at high redshift. SuperSpec is a filter bank with planar, lithographed, superconducting transmission line resonator filters and lumped-element kinetic inductance detectors made from Titanium Nitride. We have built an 81 detector prototype that operates in the 195-310 GHz band. The prototype has a wide-band metal feed horn with a transition to microstrip that feeds the filter bank. The prototype has demonstrated optical filter bank channels with a range of resolving powers from 300 to 700, measured fractional frequency noise of at Hz. C1 [Shirokoff, E.; Hailey-Dunsheath, S.; Hollister, M. I.; Kovacs, A.; McKenney, C. M.; O'Brient, R.; Padin, S.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA. [Barry, P. S.; Doyle, S.; Mauskopf, P.; Tucker, C. E.] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3AX, S Glam, Wales. [Bradford, C. M.; Chattopadhyay, G.; Day, P.; Leduc, H. G.; Nguyen, H. T.; O'Brient, R.; Reck, T. J.; Swenson, L. J.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Mauskopf, P.] Arizona State Univ, Tempe, AZ USA. RP Shirokoff, E (reprint author), CALTECH, Pasadena, CA 91125 USA. EM erik.shirokoff@caltech.edu RI Kovacs, Attila/C-1171-2010 OI Kovacs, Attila/0000-0001-8991-9088 FU NASA Astrophysics Research and Analysis (APRA) [399131.02.06.03.43]; W. M. Keck Institute; NASA; Science and Technology Facilities Council [ST/G002711/1, ST/J001449/1] FX This project is supported by NASA Astrophysics Research and Analysis (APRA) Grant No. 399131.02.06.03.43. ES, CMM, and LJS acknowledge support from the W. M. Keck Institute for Space Studies. MIH, LJS, and TR acknowledge support from the NASA Postdoctoral Program. PSB acknowledges the continuing support from the Science and Technology Facilities Council Ph.D. studentship programme and grant programmes ST/G002711/1 and ST/J001449/1. Device fabrication was performed the JPL Microdevices Laboratory. NR 14 TC 5 Z9 5 U1 1 U2 6 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 657 EP 662 DI 10.1007/s10909-014-1122-8 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400007 ER PT J AU Datta, R Hubmayr, J Munson, C Austermann, J Beall, J Becker, D Cho, HM Halverson, N Hilton, G Irwin, K Li, D McMahon, J Newburgh, L Nibarger, J Niemack, M Schmitt, B Smith, H Staggs, S Van Lanen, J Wollack, E AF Datta, R. Hubmayr, J. Munson, C. Austermann, J. Beall, J. Becker, D. Cho, H. M. Halverson, N. Hilton, G. Irwin, K. Li, D. McMahon, J. Newburgh, L. Nibarger, J. Niemack, M. Schmitt, B. Smith, H. Staggs, S. Van Lanen, J. Wollack, E. TI Horn Coupled Multichroic Polarimeters for the Atacama Cosmology Telescope Polarization Experiment SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Cosmic microwave background; Superconducting detectors; Feedhorn; TES; Polarimeter; Millimeter-wave; Silicon lenses; Antireflection coating AB Multichroic polarization sensitive detectors enable increased sensitivity and spectral coverage for observations of the cosmic microwave background. An array optimized for dual frequency detectors can provide 1.7 times gain in sensitivity compared to a single frequency array. We present the design and measurements of horn coupled multichroic polarimeters encompassing the 90 and 150 GHz frequency bands and discuss our plans to field an array of these detectors as part of the ACTPol project. C1 [Datta, R.; Munson, C.; McMahon, J.; Smith, H.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Hubmayr, J.; Beall, J.; Becker, D.; Cho, H. M.; Hilton, G.; Irwin, K.; Li, D.; Niemack, M.; Van Lanen, J.] NIST, Boulder, CO 80305 USA. [Austermann, J.; Halverson, N.] Univ Colorado, Dept Astrophys Sci, Boulder, CO 80309 USA. [Newburgh, L.; Staggs, S.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Nibarger, J.] NIST, Boulder Microfabricat Facil, Boulder, CO 80305 USA. [Niemack, M.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Schmitt, B.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Datta, R (reprint author), Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. EM dattar@umich.edu RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU NASA [NNX13AE56G]; NASA Space Technology Research Fellowship [NNX12AM32H]; U.S. National Science Foundation [AST-0965625, PHY-1214379] FX This work was supported by NASA through award NNX13AE56G and the NASA Space Technology Research Fellowship grant NNX12AM32H and by the U.S. National Science Foundation through awards AST-0965625 and PHY-1214379. NR 9 TC 14 Z9 14 U1 0 U2 7 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 670 EP 676 DI 10.1007/s10909-014-1134-4 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400009 ER PT J AU Grace, EA Beall, J Cho, HM Devlin, MJ Fox, A Hilton, G Hubmayr, J Irwin, K Klein, J Li, D Lungu, M Newburgh, LB Nibarger, J Niemack, MD McMahon, J Page, LA Pappas, C Schmitt, BL Staggs, ST Van Lanen, J Wollack, E AF Grace, E. A. Beall, J. Cho, H. M. Devlin, M. J. Fox, A. Hilton, G. Hubmayr, J. Irwin, K. Klein, J. Li, D. Lungu, M. Newburgh, L. B. Nibarger, J. Niemack, M. D. McMahon, J. Page, L. A. Pappas, C. Schmitt, B. L. Staggs, S. T. Van Lanen, J. Wollack, E. TI Characterization and Performance of a Kilo-TES Sub-Array for ACTPol SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Cosmic microwave background; Transition edge sensor; Bolometer; Polarimetry AB ACTPol is a polarization-sensitive receiver upgrade to the Atacama Cosmology Telescope (ACT) which will make millimeter wavelength measurements of the small-scale polarization anisotropies of the cosmic microwave background to investigate the properties of inflation, dark energy, dark matter, and neutrinos in the early Universe. ACTPol will employ three arrays of transition edge sensor (TES) bolometer detectors. The detectors, with a target transition temperature of 150 mK, will be operated at a bath temperature of 100 mK provided by a dilution refrigerator. One array operating at a central frequency of 150 GHz and consisting of 1024 TESes achieved first light at the ACT site in July 2013. We anticipate fielding the remainder of the focal plane, consisting of a second 150 GHz array and a multi-chroic array sensitive to 90 and 150 GHz, at the end of the 2013 observing season. In these proceedings, we present characterization of key detector parameters from measurements performed on the first array both in the lab and during initial field testing. We comment on the design goals, measurements, and uniformity of the detector transition temperatures, saturation powers, and thermal conductivities while detailing measurement methods and results for the detector optical efficiencies and time constants. C1 [Grace, E. A.; Page, L. A.; Pappas, C.; Staggs, S. T.] Princeton Univ, Dept Phys, Princeton, NJ 08540 USA. [Beall, J.; Cho, H. M.; Fox, A.; Hilton, G.; Hubmayr, J.; Irwin, K.; Li, D.; Nibarger, J.; Van Lanen, J.] NIST, Boulder, CO 80305 USA. [Devlin, M. J.; Klein, J.; Lungu, M.; Schmitt, B. L.] Univ Penn, Dept Phys, Philadelphia, PA 19104 USA. [Newburgh, L. B.] Univ Toronto, Dunlap Inst, Toronto, ON M5S 3H4, Canada. [Niemack, M. D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [McMahon, J.] Univ Michigan, Ann Arbor, MI 48109 USA. [Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Grace, EA (reprint author), Princeton Univ, Dept Phys, Princeton, NJ 08540 USA. EM egrace@princeton.edu RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU U.S. National Science Foundation [AST-0965625, PHY-0855887, PHY-1214379]; NIST Quantum Initiative; NASA Office of the Chief Technologists Space Technology Research Fellowship awards FX This work was supported by the U.S. National Science Foundation through awards AST-0965625, PHY-0855887 and PHY-1214379. The NIST authors would like to acknowledge the support of the NIST Quantum Initiative. The work of E.A. Grace and B. Schmitt were supported by NASA Office of the Chief Technologists Space Technology Research Fellowship awards. We would like to acknowledge the work of Bert Harrop in the bonding and assembly of the first array. NR 10 TC 2 Z9 2 U1 0 U2 5 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 705 EP 711 DI 10.1007/s10909-014-1125-5 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400014 ER PT J AU Barron, D Ade, P Anthony, A Arnold, K Boettger, D Borrill, J Chapman, S Chinone, Y Dobbs, M Edwards, J Errard, J Fabbian, G Flanigan, D Fuller, G Ghribi, A Grainger, W Halverson, N Hasegawa, M Hattori, K Hazumi, M Holzapfel, W Howard, J Hyland, P Jaehnig, G Jaffe, A Keating, B Kermish, Z Keskitalo, R Kisner, T Lee, AT Le Jeune, M Linder, E Lungu, M Matsuda, F Matsumura, T Meng, X Miller, NJ Morii, H Moyerman, S Myers, M Nishino, H Paar, H Peloton, J Quealy, E Rebeiz, G Reichardt, CL Richards, PL Ross, C Shimizu, A Shimmin, C Shimon, M Sholl, M Siritanasak, P Spieler, H Stebor, N Steinbach, B Stompor, R Suzuki, A Tomaru, T Tucker, C Yadav, A Zahn, O AF Barron, D. Ade, P. Anthony, A. Arnold, K. Boettger, D. Borrill, J. Chapman, S. Chinone, Y. Dobbs, M. Edwards, J. Errard, J. Fabbian, G. Flanigan, D. Fuller, G. Ghribi, A. Grainger, W. Halverson, N. Hasegawa, M. Hattori, K. Hazumi, M. Holzapfel, W. Howard, J. Hyland, P. Jaehnig, G. Jaffe, A. Keating, B. Kermish, Z. Keskitalo, R. Kisner, T. Lee, A. T. Le Jeune, M. Linder, E. Lungu, M. Matsuda, F. Matsumura, T. Meng, X. Miller, N. J. Morii, H. Moyerman, S. Myers, M. Nishino, H. Paar, H. Peloton, J. Quealy, E. Rebeiz, G. Reichardt, C. L. Richards, P. L. Ross, C. Shimizu, A. Shimmin, C. Shimon, M. Sholl, M. Siritanasak, P. Spieler, H. Stebor, N. Steinbach, B. Stompor, R. Suzuki, A. Tomaru, T. Tucker, C. Yadav, A. Zahn, O. TI The POLARBEAR Cosmic Microwave Background Polarization Experiment SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Cosmic microwave background; CMB polarization; Millimeter-wave AB The polarbear cosmic microwave background (CMB) polarization experiment has been observing since early 2012 from its 5,200 m site in the Atacama Desert in Northern Chile. polarbear's measurements will characterize the expected CMB polarization due to gravitational lensing by large scale structure, and search for the possible B-mode polarization signature of inflationary gravitational waves. polarbear's 250 mK focal plane detector array consists of 1,274 polarization-sensitive antenna-coupled bolometers, each with an associated lithographed band-defining filter and contacting dielectric lenslet, an architecture unique in current CMB experiments. The status of the polarbear instrument, its focal plane, and the analysis of its measurements are presented. C1 [Barron, D.; Arnold, K.; Boettger, D.; Edwards, J.; Fuller, G.; Keating, B.; Matsuda, F.; Meng, X.; Moyerman, S.; Paar, H.; Rebeiz, G.; Siritanasak, P.; Stebor, N.; Yadav, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Ade, P.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3AX, S Glam, Wales. [Anthony, A.; Halverson, N.; Jaehnig, G.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Borrill, J.; Errard, J.; Keskitalo, R.; Kisner, T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Borrill, J.; Richards, P. L.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Chapman, S.; Ross, C.] Dalhousie Univ, Dept Phys, Halifax, NS B3H 3J5, Canada. [Chinone, Y.; Hasegawa, M.; Hattori, K.; Hazumi, M.; Matsumura, T.; Morii, H.; Shimizu, A.; Tomaru, T.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki, Japan. [Dobbs, M.] McGill Univ, Dept Phys, Montreal, PQ, Canada. [Fabbian, G.; Le Jeune, M.; Peloton, J.; Stompor, R.] Univ Paris 07, Lab Astroparticule & Cosmol APC, Paris, France. [Flanigan, D.; Ghribi, A.; Holzapfel, W.; Howard, J.; Lee, A. T.; Lungu, M.; Myers, M.; Quealy, E.; Reichardt, C. L.; Richards, P. L.; Shimmin, C.; Steinbach, B.; Suzuki, A.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Grainger, W.] STFC, Rutherford Appleton Lab, Didcot, Oxon, England. [Hyland, P.] Austin Coll, Dept Phys, Sherman, TX 75090 USA. [Jaffe, A.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London, England. [Kermish, Z.] Princeton Univ, Princeton, NJ 08544 USA. [Linder, E.; Sholl, M.; Spieler, H.; Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Miller, N. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nishino, H.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba, Japan. [Shimon, M.] Tel Aviv Univ, IL-69978 Tel Aviv, Israel. [Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys BCCP, Berkeley, CA 94720 USA. RP Barron, D (reprint author), Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. EM dbarron@physics.ucsd.edu RI Holzapfel, William/I-4836-2015; OI Fabbian, Giulio/0000-0002-3255-4695; Reichardt, Christian/0000-0003-2226-9169 FU National Science Foundation [AST-0618398]; NASA [NNG06GJ08G]; Natural Sciences and Engineering Research Council; Canadian Institute for Advanced Research; MEXT KAKENHI [21111002]; Simons Foundation FX POLARBEAR is funded by the National Science Foundation under Grant AST-0618398. Antenna-coupled bolometer development at Berkeley is funded by NASA under Grant NNG06GJ08G. The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council and Canadian Institute for Advanced Research. The KEK authors are supported by MEXT KAKENHI Grant Number 21111002. The Chilean site is located in the Parque Astronomico Atacama in agreement with the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile. The Simons Array is funded by the Simons Foundation. NR 14 TC 0 Z9 0 U1 3 U2 5 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 726 EP 732 DI 10.1007/s10909-013-1065-5 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400017 ER PT J AU Johnson, BR Ade, PAR Araujo, D Bradford, KJ Chapman, D Day, PK Didier, J Doyle, S Eriksen, HK Flanigan, D Groppi, C Hillbrand, S Jones, G Limon, M Mauskopf, P McCarrick, H Miller, A Mroczkowski, T Reichborn-Kjennerud, B Smiley, B Sobrin, J Wehus, IK Zmuidzinas, J AF Johnson, B. R. Ade, P. A. R. Araujo, D. Bradford, K. J. Chapman, D. Day, P. K. Didier, J. Doyle, S. Eriksen, H. K. Flanigan, D. Groppi, C. Hillbrand, S. Jones, G. Limon, M. Mauskopf, P. McCarrick, H. Miller, A. Mroczkowski, T. Reichborn-Kjennerud, B. Smiley, B. Sobrin, J. Wehus, I. K. Zmuidzinas, J. TI The Detector System for the Stratospheric Kinetic Inductance Polarimeter (SKIP) SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE CMB; CIB; MKID; LEKID AB The stratospheric kinetic inductance polarimeter is a proposed balloon-borne experiment designed to study the cosmic microwave background, the cosmic infrared background and Galactic dust emission by observing 1,133 deg of sky in the Northern Hemisphere with launches from Kiruna, Sweden. The instrument contains 2,317 single-polarization, horn-coupled, aluminum lumped-element kinetic inductance detectors (Lekids). The Lekids will be maintained at 100 mK with an adiabatic demagnetization refrigerator. The polarimeter operates in two configurations, one sensitive to a spectral band centered on 150 GHz and the other sensitive to 260 and 350 GHz bands. The detector readout system is based on the ROACH-1 board, and the detectors will be biased below 300 MHz. The detector array is fed by an F/2.4 crossed-Dragone telescope with a 500 mm aperture yielding a 15 arcmin FWHM beam at 150 GHz. To minimize detector loading and maximize sensitivity, the entire optical system will be cooled to 1 K. Linearly polarized sky signals will be modulated with a metal-mesh half-wave plate that is mounted at the telescope aperture and rotated by a superconducting magnetic bearing. The observation program consists of at least two, 5-day flights beginning with the 150 GHz observations. C1 [Johnson, B. R.; Araujo, D.; Bradford, K. J.; Chapman, D.; Didier, J.; Flanigan, D.; Hillbrand, S.; Jones, G.; Limon, M.; McCarrick, H.; Miller, A.; Reichborn-Kjennerud, B.; Smiley, B.; Sobrin, J.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Groppi, C.; Mauskopf, P.] Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA. [Mroczkowski, T.; Zmuidzinas, J.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Ade, P. A. R.; Doyle, S.] Cardiff Univ, Sch Phys & Astron, Cardiff CF243YB, S Glam, Wales. [Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Jones, G.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Day, P. K.; Wehus, I. K.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Johnson, BR (reprint author), Columbia Univ, Dept Phys, 538 W 120th St, New York, NY 10027 USA. EM bjohnson@phys.columbia.edu OI Limon, Michele/0000-0002-5900-2698; Mroczkowski, Tony/0000-0003-3816-5372 NR 12 TC 2 Z9 2 U1 1 U2 9 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 741 EP 748 DI 10.1007/s10909-013-1014-3 PG 8 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400019 ER PT J AU Pappas, CG Beall, J Brevick, J Cho, HM Devlin, MJ Fox, A Grace, EA Hilton, GC Hubmayr, J Irwin, KD Klein, J Li, D Lungu, M Newburgh, LB Nibarger, JP Niemack, MD McMahon, JJ Page, LA Schmitt, BL Staggs, ST Van Lanen, J Wollack, EJ AF Pappas, C. G. Beall, J. Brevick, J. Cho, H. M. Devlin, M. J. Fox, A. Grace, E. A. Hilton, G. C. Hubmayr, J. Irwin, K. D. Klein, J. Li, D. Lungu, M. Newburgh, L. B. Nibarger, J. P. Niemack, M. D. McMahon, J. J. Page, L. A. Schmitt, B. L. Staggs, S. T. Van Lanen, J. Wollack, E. J. TI Optical Efficiency and R(T,I) Measurements of ACTPol TESes Using Time Domain Multiplexing Electronics SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Transition edge sensor (TES); Cosmic microwave background (CMB); Polarization; Atacama cosmology telescope; ACTPol ID TRANSITION-EDGE SENSORS AB We present new data on feedhorn-coupled transition-edge sensor devices fabricated for the second-generation receiver (ACTPol) for the Atacama cosmology telescope (ACT). First, we describe optical efficiency measurements of the latest ACTPol detector wafer, which has a average optical efficiency. Next, we discuss measurements of the TES resistance as a function of temperature and bias current () using the ACTPol time-domain multiplexing electronics. Qualitative agreement between data at low bias current and the two-fluid model prediction is shown. Using the two-fluid model and low bias current data, and at our operating bias current are calculated. C1 [Pappas, C. G.; Grace, E. A.; Page, L. A.; Staggs, S. T.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Niemack, M. D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Randall Lab 1440, Ann Arbor, MI 48109 USA. [Beall, J.; Brevick, J.; Cho, H. M.; Fox, A.; Hilton, G. C.; Hubmayr, J.; Irwin, K. D.; Li, D.; Nibarger, J. P.; Van Lanen, J.] NIST, Quantum Elect & Photon Div, Boulder, CO 80305 USA. [Devlin, M. J.; Klein, J.; Lungu, M.; Schmitt, B. L.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Newburgh, L. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Pappas, CG (reprint author), Princeton Univ, Dept Phys, Jadwin Hall, Princeton, NJ 08544 USA. EM cpappas@princeton.edu RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 NR 15 TC 1 Z9 1 U1 1 U2 5 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 749 EP 754 DI 10.1007/s10909-013-1066-4 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400020 ER PT J AU Catalano, A Ade, P Atik, Y Benoit, A Breele, E Bock, J Camus, P Charra, M Crill, BP Coron, N Coulais, A Desert, FX Fauvet, L Giraud-Heraud, Y Guillaudin, O Holmes, W Jones, WC Lamarre, JM Macias-Perez, J Martinez, M Miniussi, A Monfardini, A Pajot, F Patanchon, G Pelissier, A Piat, M Puget, JL Renault, C Rosset, C Santos, D Sauve, A Spencer, L Sudiwala, R AF Catalano, A. Ade, P. Atik, Y. Benoit, A. Breele, E. Bock, J. J. Camus, P. Charra, M. Crill, B. P. Coron, N. Coulais, A. Desert, F. -X. Fauvet, L. Giraud-Heraud, Y. Guillaudin, O. Holmes, W. Jones, W. C. Lamarre, J. -M. Macias-Perez, J. Martinez, M. Miniussi, A. Monfardini, A. Pajot, F. Patanchon, G. Pelissier, A. Piat, M. Puget, J. -L. Renault, C. Rosset, C. Santos, D. Sauve, A. Spencer, L. Sudiwala, R. TI Characterization and Physical Explanation of Energetic Particles on Planck HFI Instrument SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Planck satellite; High impedance bolometers; Cosmic rays AB The Planck High Frequency Instrument (HFI) has been surveying the sky continuously from the second Lagrangian point (L2) between August 2009 and January 2012. It operates with 52 high impedance bolometers cooled at 100 mK in a range of frequency between 100 GHz and 1 THz with unprecedented sensitivity, but strong coupling with cosmic radiation. At L2, the particle flux is about 5 and is dominated by protons incident on the spacecraft. Protons with an energy above 40 MeV can penetrate the focal plane unit box causing two different effects: glitches in the raw data from direct interaction of cosmic rays with detectors (producing a data loss of about 15 % at the end of the mission) and thermal drifts in the bolometer plate at 100 mK adding non-Gaussian noise at frequencies below 0.1 Hz. The HFI consortium has made strong efforts in order to correct for this effect on the time ordered data and final Planck maps. This work intends to give a view of the physical explanation of the glitches observed in the HFI instrument in-flight. To reach this goal, we performed several ground-based experiments using protons and particles to test the impact of particles on the HFI spare bolometers with a better control of the environmental conditions with respect to the in-flight data. We have shown that the dominant part of glitches observed in the data comes from the impact of cosmic rays in the silicon die frame supporting the micro-machined bolometric detectors propagating energy mainly by ballistic phonons and by thermal diffusion. The implications of these results for future satellite missions will be discussed. C1 [Catalano, A.; Guillaudin, O.; Macias-Perez, J.; Pelissier, A.; Renault, C.; Santos, D.] Univ Grenoble 1, Inst Natl Polytech Grenoble, Lab Phys Subatom & Cosmol, CNRS,IN2P3, F-38026 Grenoble, France. [Ade, P.; Spencer, L.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Atik, Y.; Charra, M.; Coron, N.; Martinez, M.; Miniussi, A.; Pajot, F.; Puget, J. -L.] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France. [Benoit, A.; Camus, P.; Monfardini, A.] Univ Grenoble 1, CNRS, Inst Neel, F-38026 Grenoble, France. [Breele, E.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.] Univ Paris 07, CNRS, UMR 7164, Paris, France. [Bock, J. J.] CALTECH, Pasadena, CA 91125 USA. [Bock, J. J.; Crill, B. P.; Holmes, W.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Coulais, A.; Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Desert, F. -X.] Univ Grenoble 1, IPAG, Grenoble CNRS INSU 1, UMR 5274, F-38041 Grenoble, France. [Fauvet, L.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands. [Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Sauve, A.] IRAP, CNRS, F-31028 Toulouse 4, France. RP Catalano, A (reprint author), Univ Grenoble 1, Inst Natl Polytech Grenoble, Lab Phys Subatom & Cosmol, CNRS,IN2P3, 53 Rue Martyrs, F-38026 Grenoble, France. EM catalano@lpsc.in2p3.fr RI Martinez, Maria/K-4827-2012 OI Martinez, Maria/0000-0002-9043-4691 NR 11 TC 4 Z9 4 U1 0 U2 7 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 773 EP 786 DI 10.1007/s10909-014-1116-6 PG 14 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400024 ER PT J AU Miniussi, A Puget, JL Holmes, W Patanchon, G Catalano, A Giraud-Heraud, Y Pajot, F Piat, M Vibert, L AF Miniussi, A. Puget, J. -L. Holmes, W. Patanchon, G. Catalano, A. Giraud-Heraud, Y. Pajot, F. Piat, M. Vibert, L. TI Study of Cosmic Ray Impact on Planck/HFI Low Temperature Detectors SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Cosmic ray; Particle; HFI; Planck; Bolometer AB Once that the focal plane of the HFI instrument of the Planck mission (launched in May 2009) has reached operational temperature, we have observed the thermal effect of cosmic ray interaction with the Planck satellite, located at Lagrangian point L2. When a particle hits a component of the bolometers (e.g.: thermometer, grid or wafer) composing the focal plane of HFI, a thermal spike (called glitch), due to deposited energy, is observed. Processing these data revealed another effect due to high energy cosmic ray particle showers: High Coincidence Events (HCE), composed of glitches occurring coincidentally in many detectors and with a temperature increase from nK to K after the shower. A flux of about 100 HCE per hour has been calculated. Two types of HCE have been detected: fast and slow. For the first type, the untouched bolometers reach the same temperature as the touched ones in a few seconds which can be explained by a storage of the deposited energy in the stainless steel focal plane. The second type of HCE is not fully understood yet. These effects might be explained by extra conduction from the helium released from cryogenic surfaces, creating a temporary thermal link between the different stages of the HFI. C1 [Miniussi, A.; Puget, J. -L.; Pajot, F.; Vibert, L.] Univ Paris 11, IAS, F-91405 Orsay, France. [Holmes, W.] CALTECH, JPL, Pasadena, CA 91125 USA. [Patanchon, G.; Giraud-Heraud, Y.; Piat, M.] APC, F-75205 Paris 13, France. [Catalano, A.] LPSC, F-38026 Grenoble, France. RP Miniussi, A (reprint author), Univ Paris 11, IAS, Bt 121, F-91405 Orsay, France. EM antoine.miniussi@ias.u-psud.fr NR 8 TC 1 Z9 1 U1 1 U2 4 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 815 EP 821 DI 10.1007/s10909-014-1104-x PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400029 ER PT J AU Staguhn, J Benford, D Dwek, E Hilton, G Fixsen, D Irwin, K Jhabvala, C Kovacs, A Leclercq, S Maher, S Miller, T Moseley, SH Sharp, E Wollack, E AF Staguhn, Johannes Benford, Dominic Dwek, Eli Hilton, Gene Fixsen, Dale Irwin, Kent Jhabvala, Christine Kovacs, Attila Leclercq, Samuel Maher, Stephen Miller, Tim Moseley, S. Harvey Sharp, Elmer Wollack, Edward TI Design and Expected Performance of GISMO-2, a Two Color Millimeter Camera for the IRAM 30 m Telescope SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article ID INFRARED ASTRONOMY; ARRAYS AB We present the main design features for the GISMO-2 bolometer camera, which we build for background-limited operation at the IRAM 30 m telescope on Pico Veleta, Spain. GISMO-2 will operate simultaneously in the 1 and 2 mm atmospherical windows. The 1 mm channel uses a TES-based backshort under grid (BUG) bolometer array, the 2 mm channel operates with a BUG array. The camera utilizes almost the entire full field of view provided by the telescope. The optical design of GISMO-2 was strongly influenced by our experience with the GISMO 2 mm bolometer camera, which is successfully operating at the 30 m telescope. GISMO is accessible to the astronomical community through the regular IRAM call for proposals. C1 [Staguhn, Johannes] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Staguhn, Johannes; Benford, Dominic; Dwek, Eli; Fixsen, Dale; Jhabvala, Christine; Maher, Stephen; Miller, Tim; Moseley, S. Harvey; Sharp, Elmer; Wollack, Edward] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Hilton, Gene; Irwin, Kent] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Kovacs, Attila] Univ Minnesota, Minneapolis, MN 55455 USA. [Kovacs, Attila] CALTECH, Pasadena, CA 91125 USA. [Leclercq, Samuel] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. RP Staguhn, J (reprint author), Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM johannes.staguhn@nasa.gov RI Kovacs, Attila/C-1171-2010; Wollack, Edward/D-4467-2012; Benford, Dominic/D-4760-2012 OI Kovacs, Attila/0000-0001-8991-9088; Wollack, Edward/0000-0002-7567-4451; Benford, Dominic/0000-0002-9884-4206 FU NSF ATI [1020981, 1106284] FX This work was supported through NSF ATI grants 1020981 and 1106284. NR 8 TC 2 Z9 2 U1 0 U2 1 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 829 EP 834 DI 10.1007/s10909-014-1086-8 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400031 ER PT J AU Hailey-Dunsheath, S Barry, PS Bradford, CM Chattopadhyay, G Day, P Doyle, S Hollister, M Kovacs, A LeDuc, HG Llombart, N Mauskopf, P McKenney, C Monroe, R Nguyen, HT O'Brient, R Padin, S Reck, T Shirokoff, E Swenson, L Tucker, CE Zmuidzinas, J AF Hailey-Dunsheath, S. Barry, P. S. Bradford, C. M. Chattopadhyay, G. Day, P. Doyle, S. Hollister, M. Kovacs, A. LeDuc, H. G. Llombart, N. Mauskopf, P. McKenney, C. Monroe, R. Nguyen, H. T. O'Brient, R. Padin, S. Reck, T. Shirokoff, E. Swenson, L. Tucker, C. E. Zmuidzinas, J. TI Optical Measurements of SuperSpec: A Millimeter-Wave On-Chip Spectrometer SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Kinetic inductance detector; Millimeter-wave; Spectroscopy AB SuperSpec is a novel on-chip spectrometer we are developing for (sub)millimeter wavelength astronomy. Our approach utilizes a filterbank of moderate resolution ( channels, coupled to lumped element kinetic inductance detectors (KIDs), all integrated onto a single silicon chip. The channels are half-wave resonators formed by lithographically depositing segments of superconducting transmission line, and the KIDs are titanium nitride resonators. Here we present optical measurements of a first generation prototype, operating in the 180-280 GHz frequency range. We have used a coherent source to measure the spectral profiles of 17 channels, which achieve linewidths corresponding to quality factors as high as consistent with the designed values plus additional dissipation characterized by We have also used a Fourier Transform Spectrometer to characterize the spectral purity of all 72 channels on the chip, and measure typical out of band responses dB below the peak response. C1 [Hailey-Dunsheath, S.; Hollister, M.; Kovacs, A.; McKenney, C.; O'Brient, R.; Padin, S.; Shirokoff, E.; Swenson, L.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA. [Barry, P. S.; Doyle, S.; Tucker, C. E.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Bradford, C. M.; Chattopadhyay, G.; Day, P.; LeDuc, H. G.; Monroe, R.; Nguyen, H. T.; Reck, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kovacs, A.] Univ Minnesota, Inst Astrophys, Minneapolis, MN 55455 USA. [Llombart, N.] Univ Complutense Madrid, Dept Opt, Madrid 28037, Spain. [Mauskopf, P.] Arizona State Univ, Tempe, AZ 85287 USA. RP Hailey-Dunsheath, S (reprint author), CALTECH, Mail Code 301-17,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM haileyds@caltech.edu RI Kovacs, Attila/C-1171-2010 OI Kovacs, Attila/0000-0001-8991-9088 FU NASA Astrophysics Research and Analysis (APRA) [399131.02.06.03.43]; W. M. Keck Institute for Space Studies; NASA Postdoctoral Program; Science and Technology Facilities Council [ST/G002711/1, ST/J001449/1] FX This project is supported by NASA Astrophysics Research and Analysis (APRA) Grant No. 399131.02.06.03.43. ES, CMM, and LJS acknowledge support from the W. M. Keck Institute for Space Studies. MIH, LJS, and TR acknowledge support from the NASA Postdoctoral Program. PSB acknowledges the continuing support from the Science and Technology Facilities Council Ph.D studentship programme and grant programmes ST/G002711/1 and ST/J001449/1. Device fabrication was performed the JPL Microdevices Laboratory. NR 7 TC 3 Z9 3 U1 0 U2 3 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 841 EP 847 DI 10.1007/s10909-013-1068-2 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400033 ER PT J AU Ferri, E Bagliani, D Biassotti, M Ceruti, G Corsini, D Faverzani, M Gatti, F Giachero, A Gotti, C Kilbourne, C Kling, A Kraft-Bermuth, S Maino, M Manfrinetti, P Nucciotti, A Pessina, G Pizzigoni, G Gomes, MR Schaeffer, D Sisti, M AF Ferri, E. Bagliani, D. Biassotti, M. Ceruti, G. Corsini, D. Faverzani, M. Gatti, F. Giachero, A. Gotti, C. Kilbourne, C. Kling, A. Kraft-Bermuth, S. Maino, M. Manfrinetti, P. Nucciotti, A. Pessina, G. Pizzigoni, G. Ribeiro Gomes, M. Schaeffer, D. Sisti, M. TI Preliminary Results of the MARE Experiment SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Thermal detectors; Neutrino mass; Single beta decay; Electron capture ID NEUTRINO MASS EXPERIMENT; MICROCALORIMETERS; SEARCH; MILAN AB The microcalorimeter array for a rhenium experiment (MARE) project aims at the direct and calorimetric measurement of the electron neutrino mass with sub-eV sensitivity. The design is based on large arrays of thermal detectors to study the beta decay of Re and the electron capture of Ho. One of the activities of the project, MARE 1 in Milan, has started in Milan using one array of 6 6 silicon implanted thermistors equipped with AgReO absorbers. The purposes of MARE 1 in Milan are to achieve a sensitivity on the neutrino mass of a few eV and to investigate the systematics of Re neutrino mass measurements, focusing on those caused by the beta environmental fine structure and the beta spectrum theoretical shape. In parallel, the MARE collaboration is performing an R&D work for producing absorbers embedded with radioactive metal Ho. We report here the status of MARE using Re as beta source and the preliminary results obtained with Ho-163. C1 [Ferri, E.; Ceruti, G.; Faverzani, M.; Giachero, A.; Gotti, C.; Maino, M.; Nucciotti, A.; Pessina, G.; Sisti, M.] Univ Milano Bicocca, Milan, Italy. [Ferri, E.; Ceruti, G.; Faverzani, M.; Giachero, A.; Gotti, C.; Maino, M.; Nucciotti, A.; Pessina, G.; Sisti, M.] Ist Nazl Fis Nucl, Sez Milan Bicocca, I-20133 Milan, Italy. [Bagliani, D.; Biassotti, M.; Corsini, D.; Gatti, F.; Manfrinetti, P.; Pizzigoni, G.] Univ Genoa, Genoa, Italy. [Bagliani, D.; Biassotti, M.; Corsini, D.; Gatti, F.; Manfrinetti, P.; Pizzigoni, G.] Ist Nazl Fis Nucl, Sez Genoa, I-16146 Genoa, Italy. [Kilbourne, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MA USA. [Kling, A.; Ribeiro Gomes, M.] Univ Lisbon, Ctr Nucl Phys, P-1699 Lisbon, Portugal. [Kling, A.] IST ID, Lisbon, Portugal. [Kraft-Bermuth, S.] Johannes Gutenberg Univ Mainz, Inst Phys, Mainz, Germany. [Schaeffer, D.] ABB AB, Corp Res, Vasteras, Sweden. RP Ferri, E (reprint author), Univ Milano Bicocca, Milan, Italy. EM elena.ferri@mib.infn.it RI Giachero, Andrea/I-1081-2013; Nucciotti, Angelo/I-8888-2012; Ferri, Elena/L-8531-2014; Kling, Andreas/C-1115-2012; Kraft-Bermuth, Saskia/G-4007-2012; Sisti, Monica/B-7550-2013; Faverzani, Marco/K-3865-2016; OI Giachero, Andrea/0000-0003-0493-695X; Nucciotti, Angelo/0000-0002-8458-1556; Ferri, Elena/0000-0003-1425-3669; Kling, Andreas/0000-0002-5597-502X; Kraft-Bermuth, Saskia/0000-0002-0864-7912; Sisti, Monica/0000-0003-2517-1909; Faverzani, Marco/0000-0001-8119-2953; Pessina, Gianluigi Ezio/0000-0003-3700-9757; Gotti, Claudio/0000-0003-2501-9608 FU Fondazione Cariplo through the project Development of Microresonator Detectors for Neutrino Physics [2010-2351]; Marie Curie Actions [FP7-PEOPLE-2007-2-2-ERG]; FCT-Portugal programs [PTDC-FIS-116719-2010] FX These activities are supported by Fondazione Cariplo through the project Development of Microresonator Detectors for Neutrino Physics (Grant 2010-2351). The MARE-Ho work was partially supported by the Marie Curie Actions (FP7-PEOPLE-2007-2-2-ERG) and FCT-Portugal programs (Project PTDC-FIS-116719-2010). NR 12 TC 7 Z9 7 U1 0 U2 12 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 885 EP 890 DI 10.1007/s10909-013-1026-z PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400038 ER PT J AU Cornell, B Moore, DC Golwala, SR Bumble, B Day, PK LeDuc, HG Zmuidzinas, J AF Cornell, B. Moore, D. C. Golwala, S. R. Bumble, B. Day, P. K. LeDuc, H. G. Zmuidzinas, J. TI Particle Detection Using MKID-Based Athermal-Phonon Mediated Detectors SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Kinetic inductance detectors; Phonon; Rare event search; MKID AB We are developing athermal-phonon mediated particle detectors that utilize microwave kinetic inductance detectors (MKIDs) as phonon sensors. MKIDs afford natural frequency domain multiplexing, which allows for massive substrates to be patterned with hundreds of sensors while keeping readout complexity to a minimum. Previously, our 2 cm 2 cm 1 mm proof-of-principle device utilized 20 MKIDs and, from the magnitude and timing of their response, we were able to reconstruct the position of a particle interaction to 1 mm. From this, we corrected for variations in detector response across the device and measured an energy resolution of keV at 30 keV. We have designed and fabricated a new 3-inch prototype device that utilizes 256 MKID sensors, and we present results from its initial testing. Applications include rare event searches, such as the direct detection of dark matter and neutrinoless double beta decay, as well as hard X-ray/soft -ray astrophysics. C1 [Cornell, B.; Moore, D. C.; Golwala, S. R.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA. [Bumble, B.; Day, P. K.; LeDuc, H. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cornell, B (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM cornell@caltech.edu FU Gordon and Betty Moore Foundation; NASA FX Our research was carried out primarily at the Jet Propulsion Laboratory (JPL) and the California Institute for Technology, under contract from NASA. JPL's Microdevices Laboratory fabricated the devices used in this work. We would like to acknowledge the generous support of the Gordon and Betty Moore Foundation. Our work benefited greatly from the expertise of, as well as software developed by, the CDMS/SuperCDMS collaboration for the development of phonon-mediated particle detectors. We would also like to thank NASA's Space Technology Research Fellowship program for its ongoing support. NR 10 TC 1 Z9 1 U1 1 U2 7 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 891 EP 897 DI 10.1007/s10909-013-1039-7 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400039 ER PT J AU Kraft-Bermuth, S Andrianov, V Bleile, A Echler, A Egelhof, P Grabitz, P Kilbourne, C Kiselev, O McCammon, D Scholz, P AF Kraft-Bermuth, S. Andrianov, V. Bleile, A. Echler, A. Egelhof, P. Grabitz, P. Kilbourne, C. Kiselev, O. McCammon, D. Scholz, P. TI Precise Determination of the Lyman-1 Transition Energy in Hydrogen-like Gold Ions with Microcalorimeters SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Microcalorimeters for X-rays; Precision test of QED; Highly-charged ions ID X-RAY SPECTROSCOPY; LOW-TEMPERATURE DETECTORS; HEAVY-IONS AB The precise determination of the transition energy of the Lyman-1 line in hydrogen-like heavy ions provides a sensitive test of quantum electrodynamics in very strong Coulomb fields. We report the determination of the Lyman-1 transition energy of gold ions (Au) with microcalorimeters at the experimental storage ring at GSI. X-rays produced by the interaction of 125 MeV/u Au ions with an internal argon gas-jet target were detected. The detector array consisted of 14 pixels with silicon thermistors and Sn absorbers, for which an energy resolution of 50 eV for an X-ray energy of 59.5 keV was obtained in the laboratory. The Lyman-1 transition energy was determined for each pixel in the laboratory frame, then transformed into the emitter frame and averaged. A Dy-159 source was used for energy calibration. The absolute positions of the detector pixels, which are needed for an accurate correction of the Doppler shift, were determined by topographic measurements and by scanning a collimated Am-241 source across the cryostat window. The energy of the Lyman-1 line in the emitter frame is eV, in good agreement with theoretical predictions. The systematic error is dominated by the uncertainty in the position of the cryostat relative to the interaction region of beam and target. C1 [Kraft-Bermuth, S.; Echler, A.; Scholz, P.] Univ Giessen, Inst Atom Phys, D-35390 Giessen, Germany. [Andrianov, V.; Bleile, A.; Echler, A.; Egelhof, P.; Grabitz, P.; Kiselev, O.] GSI Helmholtzzentrum, Darmstadt, Germany. [Andrianov, V.] Moscow MV Lomonosov State Univ, Inst Nucl Phys, Moscow, Russia. [Egelhof, P.; Grabitz, P.] Johannes Gutenberg Univ Mainz, D-55122 Mainz, Germany. [Kilbourne, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McCammon, D.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. RP Kraft-Bermuth, S (reprint author), Univ Giessen, Inst Atom Phys, D-35390 Giessen, Germany. EM saskia.kraft-bermuth@iamp.physik.uni-giessen.de RI Kraft-Bermuth, Saskia/G-4007-2012 OI Kraft-Bermuth, Saskia/0000-0002-0864-7912 FU Deutsche Forschungsgemeinschaft (DFG) FX We thank K. Eberhard and J. Runke from the Institute of Nuclear Chemistry of the Johannes Gutenberg Universitat Mainz for producing the Dy-159 source. We also thank our co-experimentators from the FOCAL group for good cooperation during the measurements. The ESR group of GSI provided us with stable experimental conditions. This work was supported by the Emmy Noether Young Researchers Program of the Deutsche Forschungsgemeinschaft (DFG). NR 12 TC 4 Z9 4 U1 0 U2 8 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 1002 EP 1008 DI 10.1007/s10909-013-1002-7 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400055 ER PT J AU Heine, SNT Figueroa-Feliciano, E Rutherford, JM Wikus, P Oakley, P Porter, FS McCammon, D AF Heine, S. N. T. Figueroa-Feliciano, E. Rutherford, J. M. Wikus, P. Oakley, P. Porter, F. S. McCammon, D. TI Vibration Isolation Design for the Micro-X Rocket Payload SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Vibration isolation; Transition-edge sensors; Sounding rockets; X-ray spectrometers ID MICROCALORIMETERS AB Micro-X is a NASA-funded, sounding rocket-borne X-ray imaging spectrometer that will allow high precision measurements of velocity structure, ionization state and elemental composition of extended astrophysical systems. One of the biggest challenges in payload design is to maintain the temperature of the detectors during launch. There are several vibration damping stages to prevent energy transmission from the rocket skin to the detector stage, which causes heating during launch. Each stage should be more rigid than the outer stages to achieve vibrational isolation. We describe a major design effort to tune the resonance frequencies of these vibration isolation stages to reduce heating problems prior to the projected launch in the summer of 2014. C1 [Heine, S. N. T.; Figueroa-Feliciano, E.; Rutherford, J. M.; Wikus, P.; Oakley, P.; Porter, F. S.; McCammon, D.] MIT, MIT Kavli Inst, Cambridge, MA 02139 USA. [Porter, F. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McCammon, D.] Univ Wisconsin, Madison, WI USA. RP Heine, SNT (reprint author), MIT, MIT Kavli Inst, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM saraht@mit.edu RI Porter, Frederick/D-3501-2012 OI Porter, Frederick/0000-0002-6374-1119 NR 5 TC 3 Z9 3 U1 0 U2 3 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2014 VL 176 IS 5-6 BP 1082 EP 1088 DI 10.1007/s10909-013-1032-1 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AM5DE UT WOS:000339875400066 ER PT J AU Doude, HR Schneider, JA Nunes, AC AF Doude, Haley R. Schneider, Judy A. Nunes, Arthur C., Jr. TI Influence of the Tool Shoulder Contact Conditions on the Material Flow During Friction Stir Welding SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND MATERIALS SCIENCE LA English DT Article ID TEMPERATURE DISTRIBUTION; MECHANICAL-PROPERTIES; ALUMINUM-ALLOYS; HEAT-TRANSFER; PROCESS MODEL; ONION RINGS; METAL FLOW; MICROSTRUCTURE; VISUALIZATION; GEOMETRY AB Friction stir welding (FSWing) is a solid-state joining process of special interest in joining alloys that are traditionally difficult to fusion weld. In order to optimize the process, various numeric modeling approaches have been pursued. Of importance to furthering modeling efforts is a better understanding of the contact conditions between the workpiece and the weld tool. Both theoretical and experimental studies indicate the contact conditions between the workpiece and weld tool are unknown, possibly varying during the FSW process. To provide insight into the contact conditions, this study characterizes the material flow in the FSW nugget by embedding a lead (Pb) wire that melted at the FSWing temperature of aluminum alloy 2195. The Pb trace provided evidence of changes in material flow characteristics which were attributed to changes in the contact conditions between the weld tool and workpiece, as driven by temperature, as the tool travels the length of a weld seam. C1 [Doude, Haley R.] Mississippi State Univ, Ctr Adv Vehicular Syst, Mississippi State, MS 39762 USA. [Schneider, Judy A.] Mississippi State Univ, Dept Mech Engn, Mississippi State, MS 39762 USA. [Nunes, Arthur C., Jr.] NASA, MSFC, Huntsville, AL USA. RP Doude, HR (reprint author), Mississippi State Univ, Ctr Adv Vehicular Syst, Mississippi State, MS 39762 USA. EM har15@msstate.edu FU NASA Faculty Fellowship Program; NASA GSRP Fellowship FX The authors [HRD, JAS] acknowledge the funding support provided by the NASA Faculty Fellowship Program and a NASA GSRP Fellowship [HRD]. NR 51 TC 6 Z9 6 U1 9 U2 43 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1073-5623 EI 1543-1940 J9 METALL MATER TRANS A JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci. PD SEP PY 2014 VL 45A IS 10 BP 4411 EP 4422 DI 10.1007/s11661-014-2384-0 PG 12 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA AM5HP UT WOS:000339888100026 ER PT J AU Jones, SF Blain, AW Stern, D Assef, RJ Bridge, CR Eisenhardt, P Petty, S Wu, JW Tsai, CW Cutri, R Wright, EL Yan, L AF Jones, Suzy F. Blain, Andrew W. Stern, Daniel Assef, Roberto J. Bridge, Carrie R. Eisenhardt, Peter Petty, Sara Wu, Jingwen Tsai, Chao-Wei Cutri, Roc Wright, Edward L. Yan, Lin TI Submillimetre observations of WISE-selected high-redshift, luminous, dusty galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: formation; galaxies: high-redshift; infrared: galaxies; submillimetre: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; DEGREE EXTRAGALACTIC SURVEY; SUPERMASSIVE BLACK-HOLES; OBSCURED STAR-FORMATION; MU-M OBSERVATIONS; DEEP-FIELD-SOUTH; NUMBER COUNTS; XMM-NEWTON AB We present SCUBA-2 (Submillimetre Common-User Bolometer Array) 850 mu m submillimetre (submm) observations of the fields of 10 dusty, luminous galaxies at z similar to 1.7-4.6, detected at 12 and/or 22 mu m by the Wide-field Infrared Survey Explorer (WISE) all-sky survey, but faint or undetected at 3.4 and 4.6 mu m; dubbed hot, dust-obscured galaxies (Hot DOGs). The six detected targets all have total infrared luminosities greater than 10(13) L-aS (TM), with one greater than 10(14) L-aS (TM). Their spectral energy distributions (SEDs) are very blue from mid-infrared to submm wavelengths and not well fitted by standard active galactic nuclei (AGN) SED templates, without adding extra dust extinction to fit the WISE 3.4 and 4.6 mu m data. The SCUBA-2 850 mu m observations confirm that the Hot DOGs have less cold and/or more warm dust emission than standard AGN templates, and limit an underlying extended spiral or ULIRG-type galaxy to contribute less than about 2 or 55 per cent of the typical total Hot DOG IR luminosity, respectively. The two most distant and luminous targets have similar observed submm to mid-infrared ratios to the rest, and thus appear to have even hotter SEDs. The number of serendipitous submm galaxies detected in the 1.5-arcmin-radius SCUBA-2 850 mu m maps indicates there is a significant overdensity of serendipitous sources around Hot DOGs. These submm observations confirm that the WISE-selected ultraluminous galaxies have very blue mid-infrared to submm SEDs, suggesting that they contain very powerful AGN, and are apparently located in unusual arcmin-scale overdensities of very luminous dusty galaxies. C1 [Jones, Suzy F.; Blain, Andrew W.] Univ Leicester, Xray & Observat Astron Grp XROA, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Stern, Daniel; Eisenhardt, Peter; Tsai, Chao-Wei] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Assef, Roberto J.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. [Bridge, Carrie R.] CALTECH, Pasadena, CA 91125 USA. [Petty, Sara] Virginia Polytech Inst & State Univ, Dept Phys, Blacksburg, VA 24061 USA. [Wu, Jingwen; Wright, Edward L.] Univ Calif Los Angeles, Div Phys & Astron, Los Angeles, CA 90095 USA. [Cutri, Roc; Yan, Lin] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. RP Jones, SF (reprint author), Univ Leicester, Xray & Observat Astron Grp XROA, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM sfj8@le.ac.uk FU University of Leicester Physics & Astronomy Department; Gemini-CONICYT [32120009]; National Aeronautics and Space Administration; Canada Foundation for Innovation; [M12AU010] FX SFJ gratefully acknowledges support from the University of Leicester Physics & Astronomy Department. RJA was supported by Gemini-CONICYT grant number 32120009. This publication makes use of data products from the WISE, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.; The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the Netherlands Organization for Scientific Research, and the National Research Council of Canada. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. The project ID under which the data were obtained was M12AU010. NR 85 TC 19 Z9 19 U1 0 U2 11 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 2014 VL 443 IS 1 BP 146 EP 157 DI 10.1093/mnras/stu1157 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5UR UT WOS:000339927000014 ER PT J AU Gorbikov, E Gal-Yam, A Ofek, EO Vreeswijk, PM Nugent, PE Chotard, N Kulkarni, SR Cao, Y De Cia, A Yaron, O Tal, D Arcavi, I Kasliwal, MM Cenko, SB Sullivan, M Chen, JC AF Gorbikov, Evgeny Gal-Yam, Avishay Ofek, Eran O. Vreeswijk, Paul M. Nugent, Peter E. Chotard, Nicolas Kulkarni, Shrinivas R. Cao, Yi De Cia, Annalisa Yaron, Ofer Tal, David Arcavi, Iair Kasliwal, Mansi M. Cenko, S. Bradley Sullivan, Mark Chen, Juncheng TI iPTF13beo: the double-peaked light curve of a Type Ibn supernova discovered shortly after explosion SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; supernovae: individual: iPTF13beo; stars: winds, outflows; stars: Wolf-Rayet ID RICH CIRCUMSTELLAR MEDIUM; SN 2009IP; SHOCK BREAKOUT; DUST FORMATION; CORE-COLLAPSE; MASSIVE STAR; 2006JC; EMISSION; OUTBURST; SPECTROSCOPY AB We present optical photometric and spectroscopic observations of the Type Ibn (SN 2006jc-like) supernova (SN) iPTF13beo. Detected by the intermediate Palomar Transient Factory similar to 3 h after the estimated first light, iPTF13beo is the youngest and the most distant (similar to 430 Mpc) Type Ibn event ever observed. The iPTF13beo light curve is consistent with light curves of other Type Ibn SNe and with light curves of fast Type Ic events, but with a slightly faster rise-time of two days. In addition, the iPTF13beo R-band light curve exhibits a double-peak structure separated by similar to 9 d, not observed before in any Type Ibn SN. A low-resolution spectrum taken during the iPTF13beo rising stage is featureless, while a late-time spectrum obtained during the declining stage exhibits narrow and intermediate-width He i and Si ii features with full width at half-maximum a parts per thousand 2000-5000 km s(-1) and is remarkably similar to the prototypical SN Ibn 2006jc spectrum. We suggest that our observations support a model of a massive star exploding in a dense He-rich circumstellar medium (CSM). A shock breakout in a CSM model requires an eruption releasing a total mass of similar to 0.1 MaS (TM) over a time-scale of couple of weeks prior to the SN explosion. C1 [Gorbikov, Evgeny; Gal-Yam, Avishay; Ofek, Eran O.; Vreeswijk, Paul M.; De Cia, Annalisa; Yaron, Ofer; Tal, David; Arcavi, Iair] Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Nugent, Peter E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Res Div, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Chotard, Nicolas] Univ Lyon, F-69622 Lyon, France. [Chotard, Nicolas] Univ Lyon 1, F-69622 Villeurbanne, France. [Chotard, Nicolas] CNRS, IN2P3, Inst Phys Nucl Lyon, F-75700 Paris, France. [Kulkarni, Shrinivas R.; Cao, Yi] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Kasliwal, Mansi M.] Carnegie Inst Sci, Pasadena, CA 91101 USA. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Sullivan, Mark] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Chen, Juncheng] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China. RP Gorbikov, E (reprint author), Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. EM mrmagnate@mail.ru OI Sullivan, Mark/0000-0001-9053-4820 FU W. M. Keck Foundation; Israeli Ministry of Science; I-CORE Programme of the Planning and Budgeting Committee; Israel Science Foundation [1829/12]; EU/FP7 via ERC grant [307260]; ISF grant; BSF grant; Minerva grant; GIF grant; ISF; Israeli Planning and Budgeting Committee; Kimmel award; Lyon Institute of Origins [ANR-10-LABX-66] FX This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We are grateful for excellent staff assistance at Palomar, Lick, and Keck Observatories. EOO is incumbent of the Arye Dissentshik career development chair and is grateful to support by a grant from the Israeli Ministry of Science and the I-CORE Programme of the Planning and Budgeting Committee and The Israel Science Foundation (grant no. 1829/12).; AG-Y acknowledges support by the EU/FP7 via ERC grant no. 307260, ISF, BSF, Minerva and GIF grants, the 'Quantum Universe' I-Core programme funded by the ISF and the Israeli Planning and Budgeting Committee, and the Kimmel award.; NC acknowledges support from the Lyon Institute of Origins under grant ANR-10-LABX-66. NR 45 TC 17 Z9 18 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 2014 VL 443 IS 1 BP 671 EP 677 DI 10.1093/mnras/stu1184 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5UR UT WOS:000339927000052 ER PT J AU Snyder, TJ Andrews, M Weislogel, M Moeck, P Stone-Sundberg, J Birkes, D Hoffert, MP Lindeman, A Morrill, J Fercak, O Friedman, S Gunderson, J Ha, A McCollister, J Chen, YK Geile, J Wollman, A Attari, B Botnen, N Vuppuluri, V Shim, J Kaminsky, W Adams, D Graft, J AF Snyder, Trevor J. Andrews, Mike Weislogel, Mark Moeck, Peter Stone-Sundberg, Jennifer Birkes, Derek Hoffert, Madeline Paige Lindeman, Adam Morrill, Jeff Fercak, Ondrej Friedman, Sasha Gunderson, Jeff Ha, Anh McCollister, Jack Chen, Yongkang Geile, John Wollman, Andrew Attari, Babak Botnen, Nathan Vuppuluri, Vasant Shim, Jennifer Kaminsky, Werner Adams, Dustin Graft, John TI 3D Systems' Technology Overview and New Applications in Manufacturing, Engineering, Science, and Education SO 3D PRINTING AND ADDITIVE MANUFACTURING LA English DT Article AB Since the inception of 3D printing, an evolutionary process has taken place in which specific user and customer needs have crossed paths with the capabilities of a growing number of machines to create value-added businesses. Even today, over 30 years later, the growth of 3D printing and its utilization for the good of society is often limited by the various users 'understanding of the technology for their specific needs. This article presents an overview of current 3D printing technologies and shows numerous examples from a multitude of fields from manufacturing to education. C1 [Snyder, Trevor J.; Andrews, Mike] 3D Syst, 26600 SW Pkwy, Wilsonville, OR 97070 USA. [Weislogel, Mark; Moeck, Peter; Stone-Sundberg, Jennifer; Birkes, Derek; Hoffert, Madeline Paige; Lindeman, Adam; Morrill, Jeff; Fercak, Ondrej; Friedman, Sasha; Gunderson, Jeff; Ha, Anh; McCollister, Jack; Chen, Yongkang; Geile, John; Wollman, Andrew; Attari, Babak; Botnen, Nathan; Vuppuluri, Vasant] Portland State Univ, Portland, OR 97207 USA. [Shim, Jennifer] Princeton Univ, Princeton, NJ 08544 USA. [Kaminsky, Werner] Univ Washington, Seattle, WA 98195 USA. [Adams, Dustin] Xerox Corp, Wilsonville, OR USA. [Graft, John] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Snyder, TJ (reprint author), 3D Syst, 26600 SW Pkwy, Wilsonville, OR 97070 USA. NR 13 TC 10 Z9 10 U1 5 U2 11 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 2329-7662 EI 2329-7670 J9 3D PRINT ADDIT MANUF JI 3D Print. Addit. Manuf. PD SEP PY 2014 VL 1 IS 3 BP 169 EP 176 DI 10.1089/3dp.2014.1502 PG 8 WC Engineering, Manufacturing; Materials Science, Multidisciplinary SC Engineering; Materials Science GA V43BV UT WOS:000209657800010 ER PT J AU Hossain, F Maswood, M Siddique-E-Akbor, AH Yigzaw, W Mazumder, LC Ahmed, T Hossain, M Shah-Newaz, SM Limaye, A Lee, H Pradhan, S Shrestha, B Bajracahrya, B Biancamaria, S Shum, CK Turk, FJ AF Hossain, Faisal Maswood, Mehedi Siddique-E-Akbor, A. H. Yigzaw, Wondmagegn Mazumder, Liton Chandra Ahmed, Tanvir Hossain, Monowar Shah-Newaz, S. M. Limaye, Ashutosh Lee, Hyongki Pradhan, Sudip Shrestha, Basanta Bajracahrya, Birendra Biancamaria, Sylvain Shum, C. K. Turk, F. J. TI A Promising Radar Altimetry Satellite System for Operational Flood Forecasting in Flood-Prone Bangladesh SO IEEE GEOSCIENCE AND REMOTE SENSING MAGAZINE LA English DT Article AB Building on a recent suite of work that has demonstrated theoretical feasibility and operational readiness of a satellite altimeter based flood forecasting system, we recently put a progressively designed altimeter based transboundary flood forecasting system to the ultimate test of real-time operational delivery in Bangladesh. The JASON-2 satellite altimeter, which was in orbit at the time of writing this manuscript, was used as the flagship altimeter mission. This paper summarizes the entire process of designing the system, customizing the workflow, and putting the system in place for complete ownership by the Bangladesh stakeholder agency for a 100 day operational skill test spanning the period of June 1 2013 through Sept. 9, 2013. Correlation for most of the flood warning stations ranged between 0.95 to 0.80 during the 1 day to 8 days lead time range. The RMSE of forecast typically ranged between 0.75m to 1.5m at locations where the danger level relative to the river bed was more than an order higher (i.e., > 20m). The RMSE of forecast at the 8 days lead time did not exceed 2m for upstream and mid-stream rivers inside Bangladesh. The RMSE of forecast at the 8 days lead time exceeded 2m at a few estuarine river locations affected by tidal effects, where danger level relative to river bed was smaller (i.e., < 20m). Such a satellite altimeter system, such as one based on the JASON-2 altimeter, is now poised to serve the entire inhabitants of the Ganges-Brahmaputra-Meghna river basins as well as 30 or more flood-prone downstream nations currently deprived of real-time flow data from upstream nations. C1 [Hossain, Faisal; Maswood, Mehedi] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA. [Siddique-E-Akbor, A. H.; Yigzaw, Wondmagegn] Tennessee Technol Univ, Cookeville, TN 38505 USA. [Mazumder, Liton Chandra; Ahmed, Tanvir; Hossain, Monowar; Shah-Newaz, S. M.] Inst Water Modeling, Dhaka, Bangladesh. [Limaye, Ashutosh] NASA Marshall Space Flight Ctr, Huntsville, AL USA. [Lee, Hyongki] Univ Houston, Dept Civil & Environm Engn, Houston, TX 77204 USA. [Pradhan, Sudip; Shrestha, Basanta; Bajracahrya, Birendra] Int Ctr Integrated Mt Dev ICIMOD, Kathmandu, Nepal. [Biancamaria, Sylvain] LEGOS, Toulouse, France. [Shum, C. K.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. [Turk, F. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Hossain, F (reprint author), Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA. FU NASA Physical Oceanography program [NN13AD97G]; NASA SERVIR program [NNX12AM85AG]; Institute of Water Modeling (IWM) in Bangladesh FX The first author acknowledges the gracious support provided by the US Department of State (Fulbright Program) for capacity building of Bangladesh flood forecasting infrastructure. Additional support from NASA Physical Oceanography program (NN13AD97G) and NASA SERVIR program (NNX12AM85AG) is also acknowledged. The authors are also grateful to the generous support received from the Institute of Water Modeling (IWM) in Bangladesh for access to quality controlled discharge and river level data as part of a 5-year MOU between TTU and IWM. NR 16 TC 3 Z9 3 U1 1 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2168-6831 J9 IEEE GEOSC REM SEN M JI IEEE Geosci. Remote Sens. Mag. PD SEP PY 2014 VL 2 IS 3 BP 27 EP 36 DI 10.1109/MGRS.2014.2345414 PG 10 WC Geochemistry & Geophysics; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Remote Sensing; Imaging Science & Photographic Technology GA V45PW UT WOS:000209829500004 ER PT J AU Ely, TA AF Ely, Todd A. TI Mean Element Propagations Using Numerical Averaging SO JOURNAL OF THE ASTRONAUTICAL SCIENCES LA English DT Article DE Averaging; Mean Elements; Orbits; Nonlinear Dynamics AB The long-term evolution characteristics and stability of an orbit are well characterized using a mean element propagation of the perturbed two body variational equations of motion. The averaging process eliminates short period terms leaving only secular and long period effects. In this study, a non-traditional approach is taken that averages the variational equations using adaptive numerical techniques and then numerically integrating the resulting equations of motion. Doing this avoids the Fourier series expansions and truncations required by the traditional analytic methods. The resultant numerical techniques can be easily adapted to propagations at most solar system bodies. C1 [Ely, Todd A.] CALTECH, Jet Prop Lab, Miss Design & Nav Sect, MS 301-121,4800 Oak Grove Dr, Pasadena, CA USA. RP Ely, TA (reprint author), CALTECH, Jet Prop Lab, Miss Design & Nav Sect, MS 301-121,4800 Oak Grove Dr, Pasadena, CA USA. EM Todd.A.Ely@jpl.nasa.gov FU National Aeronautics and Space Administration FX This work was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 37 TC 1 Z9 1 U1 1 U2 1 PU AMER ASTRONAUTICAL SOC PI SPRINGFIELD PA 6352 ROLLING MILL PLACE SUITE 102, SPRINGFIELD, VA 22152 USA SN 0021-9142 EI 2195-0571 J9 J ASTRONAUT SCI JI J. Astronaut. Sci. PD SEP PY 2014 VL 61 IS 3 BP 275 EP 304 DI 10.1007/s40295-014-0020-2 PG 30 WC Engineering, Aerospace SC Engineering GA V41VZ UT WOS:000209575000003 ER PT J AU Reuveni, Y Kedar, S Moore, A Webb, F AF Reuveni, Yuval Kedar, Sharon Moore, Angelyn Webb, Frank TI Analyzing slip events along the Cascadia margin using an improved subdaily GPS analysis strategy SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE Satellite geodesy; Transient deformation ID SUBDUCTION ZONE; EPISODIC TREMOR; SILENT SLIP; SLOW; EARTHQUAKE; INTERFACE; JAPAN; MODEL AB A GPS analysis strategy that reduces the noise level of GPS-based subdaily strain measurements and improves subdaily resolution of positions enables the use of baseline estimates in the study of slow slip events along the northern Cascadia margin. We first evaluate this strategy's performance through comparisons of strain estimates at co-located GPS stations and borehole strainmetres, and then examine the strain migration during the 2008 May episodic tremor and slip (ETS) event. The temporal evolution of the ETS event is extracted from the GPS baseline analysis of the bidirectional propagation of the 2008 May event. These results establish the strain estimates from subdaily GPS baseline measurements as a reliable technique that can be used for mapping regional strain variations during episodic slip in regions where no laser or borehole strainmetres exist and GPS stations are abundant. C1 [Reuveni, Yuval; Kedar, Sharon; Moore, Angelyn; Webb, Frank] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Reuveni, Y (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Inst Geophys & Planetary Phys, La Jolla, CA 92093 USA. EM yreuveni@ucsd.edu RI Reuveni, Yuval/J-8287-2015 FU National Aeronautics and Space Administration FX The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. (C) 2012 California Institute of Technology. Government sponsorship acknowledged. We would like to thank Dr Susan Owen from Jet Propulsion Laboratory, California Institute of Technology, for her suggestions and comments. We would also like to thank Dr Herb Dragert from the Pacific Geo-science Center, Geological Survey of Canada, for his assistance with GPS data. BSM data were obtained from the PBO archives at UNAVCO-ftp://bsm.unavco.org/pub/bsm/level2/. NR 31 TC 2 Z9 2 U1 0 U2 15 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0956-540X EI 1365-246X J9 GEOPHYS J INT JI Geophys. J. Int. PD SEP PY 2014 VL 198 IS 3 BP 1269 EP 1278 DI 10.1093/gji/ggu208 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AM6EN UT WOS:000339955900001 ER PT J AU Mousis, O Choukroun, M Lunine, JI Sotin, C AF Mousis, Olivier Choukroun, Mathieu Lunine, Jonathan I. Sotin, Christophe TI Equilibrium composition between liquid and clathrate reservoirs on Titan SO ICARUS LA English DT Article DE Titan; Titan, hydrology; Titan, surface; Titan, atmosphere ID VAPOR-PRESSURE; DISSOCIATION PRESSURES; CHEMICAL-COMPOSITION; NOBLE-GASES; STRUCTURE-I; METHANE; ETHANE; LAKES; ATMOSPHERE; NITROGEN AB Hundreds of lakes and a few seas of liquid hydrocarbons have been observed by the Cassini spacecraft to cover the polar regions of Titan. A significant fraction of these lakes or seas could possibly be interconnected with subsurface liquid reservoirs of alkanes. In this paper, we investigate the interplay that would happen between a reservoir of liquid hydrocarbons located in Titan's subsurface and a hypothetical clathrate reservoir that progressively forms if the liquid mixture diffuses throughout a preexisting porous icy layer. To do so, we use a statistical-thermodynamic model in order to compute the composition of the clathrate reservoir that forms as a result of the progressive entrapping of the liquid mixture. This study shows that clathrate formation strongly fractionates the molecules between the liquid and the solid phases. Depending on whether the structures I or II clathrate forms, the present model predicts that the liquid reservoirs would be mainly composed of either propane or ethane, respectively. The other molecules present in the liquid are trapped in clathrates. Any river or lake emanating from subsurface liquid reservoirs that significantly interacted with clathrate reservoirs should present such composition. On the other hand, lakes and rivers sourced by precipitation should contain higher fractions of methane and nitrogen, as well as minor traces of argon and carbon monoxide. (C) 2014 Elsevier Inc. All rights reserved. C1 [Mousis, Olivier] Univ Franche Comte, Inst UTINAM, UMR 6213, CNRS INSU, F-25030 Besancon, France. [Mousis, Olivier; Lunine, Jonathan I.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Choukroun, Mathieu; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mousis, O (reprint author), Univ Franche Comte, Inst UTINAM, UMR 6213, CNRS INSU, F-25030 Besancon, France. EM olivier.mousis@obs-besancon.fr RI Choukroun, Mathieu/F-3146-2017 OI Choukroun, Mathieu/0000-0001-7447-9139 FU CNES; NASA Outer Planets Research Program; Jet Propulsion Laboratory, California Institute of Technology, under NASA FX O.M. acknowledges support from CNES. M.C. and C.S. acknowledge support from the NASA Outer Planets Research Program. Part of this work has been conducted at the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. Government sponsorship acknowledged. NR 40 TC 5 Z9 5 U1 0 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 SEP 1 PY 2014 VL 239 BP 39 EP 45 DI 10.1016/j.icarus.2014.05.032 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM3WE UT WOS:000339782700005 ER PT J AU O'Brien, DP Walsh, KJ Morbidelli, A Raymond, SN Mandell, AM AF O'Brien, David P. Walsh, Kevin J. Morbidelli, Alessandro Raymond, Sean N. Mandell, Avi M. TI Water delivery and giant impacts in the 'Grand Tack' scenario SO ICARUS LA English DT Article DE Planetary formation; Planetary dynamics; Planets, migration ID TERRESTRIAL PLANET FORMATION; GASEOUS PROTOPLANETARY DISK; HIGH-RESOLUTION SIMULATIONS; EARTH-LIKE PLANETS; ASTEROID BELT; HEAVY BOMBARDMENT; PRIMORDIAL EXCITATION; SIDEROPHILE ELEMENTS; OLIGARCHIC GROWTH; FORMING IMPACT AB A new model for terrestrial planet formation (Hansen [2009]. Astrophys. J., 703, 1131-1140; Walsh, KJ., et al. [2011]. Nature, 2011, 206-209) has explored accretion in a truncated protoplanetary disk, and found that such a configuration is able to reproduce the distribution of mass among the planets in the Solar System, especially the Earth/Mars mass ratio, which earlier simulations have generally not been able to match. Walsh et al. (Walsh, KJ., et al. [2011]. Nature, 2011,206-209) tested a possible mechanism to truncate the disk a two-stage, inward-then-outward migration of Jupiter and Saturn, as found in numerous hydrodynamical simulations of giant planet formation. In addition to truncating the disk and producing a more realistic Earth/Mars mass ratio, the migration of the giant planets also populates the asteroid belt with two distinct populations of bodies the inner belt is filled by bodies originating inside of 3 AU, and the outer belt is filled with bodies originating from between and beyond the giant planets (which are hereafter referred to as 'primitive' bodies). One implication of the truncation mechanism proposed in Walsh et al. (Walsh, KJ., et al. [2011]. Nature, 2011, 206-209) is the scattering of primitive planetesimals onto planet-crossing orbits during the formation of the planets. We find here that the planets will accrete on order 1-2% of their total mass from these bodies. For an assumed value of 10% for the water mass fraction of the primitive planetesimals, this model delivers a total amount of water comparable to that estimated to be on the Earth today. The radial distribution of the planetary masses and the dynamical excitation of their orbits are a good match to the observed system. However, we find that a truncated disk leads to formation timescales more rapid than suggested by radiometric chronometers. In particular, the last giant impact is typically earlier than 20 Myr, and a substantial amount of mass is accreted after that event. This is at odds with the dating of the Moon-forming impact and the estimated amount of mass accreted by Earth following that event. However, 5 of the 27 planets larger than half an Earth mass formed in all simulations do experience large late impacts and subsequent accretion consistent with those constraints. (C) 2014 The Authors. Published by Elsevier Inc. This is an open access article under the CC BY license C1 [O'Brien, David P.] Planetmy Sci Inst, Tucson, AZ 85719 USA. [Walsh, Kevin J.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Morbidelli, Alessandro] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice 4, France. [Raymond, Sean N.] Univ Bordeaux, Observ Aquitain Sci Univers, F-33270 Floirac, France. [Raymond, Sean N.] CNRS, UMR 5804, Lab Astrophys Bordeaux, F-33270 Floirac, France. [Mandell, Avi M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP O'Brien, DP (reprint author), Planetmy Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA. EM obrien@psi.edu FU NASA's Planetary Geology and Geophysics research program [NNX09AE36G]; NASA Lunar Science Institute (Center for Lunar Origin and Evolution at the Southwest Research Institute in Boulder, Colorado); NASA [NNA09DB32A]; European Research Council (ERC) [290568] FX D.P. O'Brien was supported by Grant NNX09AE36G from NASA's Planetary Geology and Geophysics research program. K.J. Walsh was supported by the NASA Lunar Science Institute (Center for Lunar Origin and Evolution at the Southwest Research Institute in Boulder, Colorado), NASA Grant NNA09DB32A. D.P. O'Brien and A. Morbidelli acknowledge European Research Council (ERC) Advanced Grant "ACCRETE" for support (contract Number 290568). We thank the two reviewers for their helpful comments and suggestions. NR 79 TC 48 Z9 48 U1 2 U2 32 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD SEP 1 PY 2014 VL 239 BP 74 EP 84 DI 10.1016/j.icarus.2014.05.009 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM3WE UT WOS:000339782700007 ER PT J AU Rubincam, DP AF Rubincam, David Parry TI The thermal expansion of particles and their secular orbital evolution as they circle a planet SO ICARUS LA English DT Article DE Planetary rings; Celestial mechanics; Near-Earth objects; Mars, satellites; zodiacal light ID RADIATION PRESSURE; SOLAR-SYSTEM; RING; ASTEROIDS; TEMPERATURE; FORCES; BODIES; EARTH AB The thermal expansion and contraction of particles orbiting a planet can cause secular orbit evolution. This effect, called here the thermal expansion effect, depends on particles entering and exiting the shadow of the body they orbit. A particle cools off in the shadow and heats up again in the sunshine, suffering thermal contraction and expansion. The changing cross-section that the particle presents to solar radiation pressure, plus a time lag due to thermal inertia, lead to a net along-track force. The effect causes outward drift for rocky particles in circular orbits. For particles in the size range similar to 0.002-0.02 m orbiting the inner planets, particle orbits can outwardly evolve at the rate of similar to 0.1R(Plan) per million years for Mars to similar to 1R(Plan) per million years for Mercury for distances similar to 2R(Plan) from the body, where R-Plan is the planet's radius. Poynting-Robertson dominates thermal expansion beyond a few R-Plan for the inner planets. Hence there are distances from a planet where the effects balance, depending on particle size. Orbits evolving outward from the thermal expansion effect would stop there, as well as those inwardly evolving from Poynting-Robertson. Thus particles would accumulate in these places, assuming the absence of other forces. Mars appears to be the best candidate for the operation of the thermal expansion effect. Particles in the size range considered here and orbiting in the Phobos-Deimos region would tend to be collected by the moons, sweeping the particles up and perhaps helping keep the region free of dust. The thermal expansion effect is overwhelmed by Poynting-Robertson for rocky particles orbiting Jupiter and Saturn and thus is unimportant; these planets are not considered here. For particles orbiting small asteroids, the thermal expansion effect is much larger than the Poynting-Robertson effect, but both are overwhelmed by ordinary solar radiation pressure, which increases orbital eccentricities rapidly. Meteoroids in eccentric orbits about the Sun also suffer the thermal expansion effect, but with only similar to 0.0003e(2) AU change in semimajor axis over a million years for a 2 m meteoroid orbiting between Mercury and Earth. Published by Elsevier Inc. C1 NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Rubincam, DP (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Solar Syst Explorat Div, Code 698,Bldg 34,Room S280, Greenbelt, MD 20771 USA. EM David.P.Rubincam@nasa.gov FU AES; SALMON FX I thank Susan Fricke for excellent programming support, and David D. Rowlands for making the GEODYN runs. I thank Stuart Pilorz and Daniel Scheeres for valuable comments which greatly improved the paper. The support of the AES and SALMON proposals is gratefully acknowledged. NR 29 TC 0 Z9 0 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD SEP 1 PY 2014 VL 239 BP 96 EP 104 DI 10.1016/j.icarus.2014.05.025 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM3WE UT WOS:000339782700009 ER PT J AU Neish, CD Madden, J Carter, LM Hawke, BR Giguere, T Bray, VJ Osinski, GR Cahill, JTS AF Neish, C. D. Madden, J. Carter, L. M. Hawke, B. R. Giguere, T. Bray, V. J. Osinski, G. R. Cahill, J. T. S. TI Global distribution of lunar impact melt flows SO ICARUS LA English DT Article DE Impact processes; Cratering; Moon; Moon, surface ID OBLIQUE IMPACTS; MOON; CRATERS; RADAR; INSTRUMENT; EJECTA AB In this study, we analyzed the distribution and properties of 146 craters with impact melt deposits exterior to their rims. Many of these craters were only recently discovered due to their unusual radar properties in the near-global Mini-RF data set. We find that most craters with exterior deposits of impact melt are small <= 20 km, and that the smallest craters have the longest melt flows relative to their size. In addition, exterior deposits of impact melt are more common in the highlands than the mare. This may be the result of differing target properties in the highlands and mare, the difference in titanium content, or the greater variation of topography in the highlands. We find that 80% of complex craters and 60% of simple craters have melt directions that are coincident or nearly coincident with the lowest point in their rim, implying that pre-existing topography plays a dominant role in melt emplacement. This is likely due to movement during crater modification (complex craters) or breached crater rims (simple craters). We also find that impact melt flows have very high circular polarization ratios compared to other features on the Moon. This suggests that their surfaces are some of the roughest material on the Moon at the centimeter to decimeter scale, even though they appear smooth at the meter scale. (C) 2014 Elsevier Inc. All rights reserved. C1 [Neish, C. D.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Madden, J.] Franklin & Marshall Coll, Lancaster, PA 17603 USA. [Carter, L. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hawke, B. R.; Giguere, T.] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Giguere, T.] Intergraph Corp, Kapolei, HI 96707 USA. [Bray, V. J.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Osinski, G. R.] Univ Western Ontario, Dept Earth Sci, Ctr Planetary Sci & Explorat, London, ON N6A 3K7, Canada. [Osinski, G. R.] Univ Western Ontario, Dept Phys & Astron, Ctr Planetary Sci & Explorat, London, ON N6A 3K7, Canada. [Cahill, J. T. S.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Neish, CD (reprint author), Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. EM cneish@fit.edu RI Carter, Lynn/D-2937-2012; Cahill, Joshua/I-3656-2012; OI Cahill, Joshua/0000-0001-6874-5533; Madden, Jack/0000-0002-4701-7833 FU NASA Postdoctoral Program at the Goddard Space Flight Center FX We thank the LRO project for their effort in returning the data presented here. We also wish to thank Bruce Campbell and Lillian Ostrach for their careful reviews, and Natalie Glines for help in the early stages of this work. This work was supported in part 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 to C.N. NR 53 TC 14 Z9 14 U1 0 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD SEP 1 PY 2014 VL 239 BP 105 EP 117 DI 10.1016/j.icarus.2014.05.049 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM3WE UT WOS:000339782700010 ER PT J AU Lee, S Hofstadter, M Frerking, MA Gulkis, S von Allmen, P Crovisier, J Biver, N Bockelee-Morvan, D Kamp, L Choukroun, M Keihm, S Janssen, M AF Lee, Seungwon Hofstadter, Mark Frerking, Margaret A. Gulkis, Samuel von Allmen, Paul Crovisier, Jacques Biver, Nicolas Bockelee-Morvan, Dominique Kamp, Lucas Choukroun, Mathieu Keihm, Stephen Janssen, Michael TI Sub-millimeter observation of water vapor at 557 GHz in Comet C/2002 T7 (LINEAR) SO ICARUS LA English DT Article DE Comets, coma; Radio observations; Comets, composition ID RADIATIVE-TRANSFER; NUCLEI; NEAT; Q4; 67P/CHURYUMOV-GERASIMENKO; WAVELENGTHS; INSTRUMENT; SIMULATION; MILLIMETER; ROTATION AB We present sub-millimeter observations of the ground-state rotational transition (1(10)-1(01)) of water vapor from Comet C/2002 T7 (LINEAR) obtained with the MIRO instrument on the ESA Rosetta spacecraft (s/c) orbiter on April 30, 2004. At the time of the observations, the comet was at a distance of 0.63 AU from the Sun, 0.68 AU from the MIRO telescope, and about 7.5 days after its perihelion. The ground state rotation transition of ortho-water at 556.936 GHz was observed and integrated for similar to 8 h using a frequency switched radiometer to provide short and long term stability. The MIRO beam size is 7.5 arcmin in terms of full width half maximum, corresponding to a radius of 1.1 x 10(5) km at the comet location. The observed signal line area of the water line spectrum is 4.3 +/- 0.8 K km/s. Using a molecular excitation and radiation transfer model and assuming the spherically symmetric and constant radial expansion of gas in the coma, we estimate that the production rate of water is (1.0 +/- 0.2) x 10(30) molecules/s and the expansion velocity is 1.1 +/- 0.2 km/s at the time of the MIRO observation. The present estimation of the water outgassing rate of the comet is in good agreement with other observation-based estimations when the outgassing rates with respect to the time after perihelion are compared. The Doppler-corrected center velocity of the observed line was red-shifted by 0.67 +/- 0.13 km/s, of which only 0.18 km/s shift is explained by the model and attributed to a self-absorption effect. The potential sources of the additional red shift are discussed. Published by Elsevier Inc. C1 [Lee, Seungwon; Hofstadter, Mark; Frerking, Margaret A.; Gulkis, Samuel; von Allmen, Paul] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Crovisier, Jacques; Biver, Nicolas; Bockelee-Morvan, Dominique; Kamp, Lucas; Choukroun, Mathieu; Keihm, Stephen; Janssen, Michael] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. RP Lee, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM seungwon.lee@jpl.nasa.gov RI Choukroun, Mathieu/F-3146-2017 OI Choukroun, Mathieu/0000-0001-7447-9139 NR 41 TC 1 Z9 1 U1 1 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD SEP 1 PY 2014 VL 239 BP 141 EP 153 DI 10.1016/j.icarus.2014.05.004 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM3WE UT WOS:000339782700013 ER PT J AU Schroder, SE Grynko, Y Pommerol, A Keller, HU Thomas, N Roush, TL AF Schroeder, S. E. Grynko, Ye. Pommerol, A. Keller, H. U. Thomas, N. Roush, T. L. TI Laboratory observations and simulations of phase reddening SO ICARUS LA English DT Article DE Spectrophotometry; Regoliths; Mineralogy; Radiative transfer ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; DAWN FRAMING CAMERA; OPTICS APPROXIMATION; LIGHT-SCATTERING; LUNAR-SURFACE; SEMITRANSPARENT PARTICLES; PHOTOMETRIC PROPERTIES; WAVELENGTH DEPENDENCE; SPECTRAL REFLECTANCE; PARTICULATE SURFACES AB The visible reflectance spectrum of many Solar System bodies changes with changing viewing geometry for reasons not fully understood. It is often observed to redden (increasing spectral slope) with increasing solar phase angle, an effect known as phase reddening. Only once, in an observation of the martian surface by the Viking 1 lander, was reddening observed up to a certain phase angle with bluing beyond, making the reflectance ratio as a function of phase angle shaped like an arch. However, in laboratory experiments this arch-shape is frequently encountered. To investigate this, we measured the bidirectional reflectance of particulate samples of several common rock types in the 400-1000 nm wavelength range and performed ray-tracing simulations. We confirm the occurrence of the arch for surfaces that are forward scattering, i.e. are composed of semi-transparent particles and are smooth on the scale of the particles, and for which the reflectance increases from the lower to the higher wavelength in the reflectance ratio. The arch shape is reproduced by the simulations, which assume a smooth surface. However, surface roughness on the scale of the particles, such as the Hapke and van Horn (Hapke, B., van Horn, H. [1963]. J. Geophys. Res. 68, 4545-4570) fairy castles that can spontaneously form when sprinkling a fine powder, leads to monotonic reddening. A further consequence of this form of microscopic roughness (being indistinct without the use of a microscope) is a flattening of the disk function at visible wavelengths, i.e. Lommel-Seeliger-type scattering. The experiments further reveal monotonic reddening for reflectance ratios at near-IR wavelengths. The simulations fail to reproduce this particular reddening, and we suspect that it results from roughness on the surface of the particles. Given that the regolith of atmosphereless Solar System bodies is composed of small particles, our results indicate that the prevalence of monotonic reddening and Lommel Seeliger-type scattering for these bodies results from microscopic roughness, both in the form of structures built by the particles and roughness on the surface of the particles themselves. It follows from the singular Viking 1 observation that the surface in front of the Lander was composed of semi-transparent particles, and was smooth on the scale of the particle size. (C) 2014 Elsevier Inc. All rights reserved. C1 [Schroeder, S. E.] Deutsch Zentrum Luft & Raumfahrt DLR, D-12489 Berlin, Germany. [Grynko, Ye.] Univ Paderborn, D-33098 Paderborn, Germany. [Pommerol, A.; Thomas, N.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Keller, H. U.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys IGEP, D-38106 Braunschweig, Germany. [Roush, T. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Schroder, SE (reprint author), Deutsch Zentrum Luft & Raumfahrt DLR, D-12489 Berlin, Germany. EM stefanus.schroeder@dlr.de RI Schroder, Stefan/D-9709-2013 OI Schroder, Stefan/0000-0003-0323-8324 FU Swiss National Science Foundation FX We are grateful to Lyuba Moroz for her help in procuring the samples and Ines Buttner for her assistance in preparing the samples. Fred Goesmann kindly allowed the first author to use his scanning electron microscope. Comments by reviewers J.R. Johnson and Y. Shkuratov helped to improve the manuscript. S.E.S. thanks Stefano Mottola for fruitful discussions and reviewing the draft paper. Development of the PHIRE goniometer has been supported by the Swiss National Science Foundation. NR 64 TC 10 Z9 10 U1 1 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 EI 1090-2643 J9 ICARUS JI Icarus PD SEP 1 PY 2014 VL 239 BP 201 EP 216 DI 10.1016/j.icarus.2014.06.010 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM3WE UT WOS:000339782700018 ER PT J AU Farrell, WM Wahlund, JE Morooka, M Gurnett, DA Kurth, WS MacDowall, RJ AF Farrell, W. M. Wahlund, J-E Morooka, M. Gurnett, D. A. Kurth, W. S. MacDowall, R. J. TI An estimate of the dust pickup current at Enceladus SO ICARUS LA English DT Article DE Saturn; Enceladus; Satellites, general ID SOUTH-POLE; PLASMA; ATMOSPHERE; RADIO; PLUME AB We demonstrate that the acceleration of submicron dust originating at Enceladus by a reduced co-rotating E-field is capable of creating a dust pickup current perpendicular to the magnetic field with values ranging from 3 to 15 kA (depending upon the effective grain charge). Such a current represents a new contribution to the total pickup current in the region. As such, we suggest that dust pickup currents, along with ion and electron pickup currents, are all active within the plume. Published by Elsevier Inc. C1 [Farrell, W. M.; MacDowall, R. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wahlund, J-E; Morooka, M.] Swedish Inst Space Phys, Uppsala, Sweden. [Gurnett, D. A.; Kurth, W. S.] Univ Iowa, Iowa City, IA 52242 USA. RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM william.m.farrell@nasa.gov RI Farrell, William/I-4865-2013; OI Kurth, William/0000-0002-5471-6202 NR 28 TC 5 Z9 5 U1 1 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD SEP 1 PY 2014 VL 239 BP 217 EP 221 DI 10.1016/j.icarus.2014.05.034 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM3WE UT WOS:000339782700019 ER PT J AU Nathues, A Hoffmann, M Cloutis, EA Schafer, M Reddy, V Christensen, U Sierks, H Thangjam, GS Le Corre, L Mengel, K Vincent, JB Russell, CT Prettyman, T Schmedemann, N Kneissl, T Raymond, C Gutierrez-Marques, P Hall, I Buttner, I AF Nathues, Andreas Hoffmann, Martin Cloutis, Edward A. Schaefer, Michael Reddy, Vishnu Christensen, Ulrich Sierks, Holger Thangjam, Guneshwar Singh Le Corre, Lucille Mengel, Kurt Vincent, Jean-Baptist Russell, Christopher T. Prettyman, Tom Schmedemann, Nico Kneissl, Thomas Raymond, Carol Gutierrez-Marques, Pablo Hall, Ian Buettner, Irene TI Detection of serpentine in exogenic carbonaceous chondrite material on Vesta from Dawn FC data SO ICARUS LA English DT Article DE Asteroid Vesta; Asteroids, composition; Mineralogy; Spectroscopy ID SPECTRAL REFLECTANCE PROPERTIES; ASTEROID 4 VESTA; HED METEORITES; CM CHONDRITES; DARK MATERIAL; GRAIN-SIZE; MAIN-BELT; MINERALS; SPECTROSCOPY; HOWARDITES AB The Dawn mission's Framing Camera (FC) observed Asteroid (4) Vesta in 2011 and 2012 using seven color filters and one clear filter from different orbits. In the present paper we analyze recalibrated HAMO color cubes (spatial resolution similar to 60 m/pixel) with a focus on dark material (DM). We present a definition of highly concentrated DM based on spectral parameters, subsequently map the DM across the Vestan surface, geologically classify DM, study its spectral properties on global and local scales, and finally, compare the FC in-flight color data with laboratory spectra. We have discovered an absorption band centered at 0.72 mu m in localities of DM that show the lowest albedo values by using FC data as well as spectral information from Dawn's imaging spectrometer VIR. Such localities are contained within impact-exposed outcrops on inner crater walls and ejecta material. Comparisons between spectral FC in-flight data, and laboratory spectra of meteorites and mineral mixtures in the wavelength range 0.4-1.0 mu m, revealed that the absorption band can be attributed to the mineral serpentine, which is typically present in CM chondrites. Dark material in its purest form is rare on Vesta's surface and is distributed globally in a non-uniform manner. Our findings confirm the hypothesis of an exogenic origin of the DM by the infall of carbonaceous chondritic material, likely of CM type. It further confirms the hypothesis that most of the DM was deposited by the Veneneia impact. (C) 2014 Elsevier Inc. All rights reserved. C1 [Nathues, Andreas; Hoffmann, Martin; Schaefer, Michael; Reddy, Vishnu; Christensen, Ulrich; Sierks, Holger; Thangjam, Guneshwar Singh; Vincent, Jean-Baptist; Gutierrez-Marques, Pablo; Hall, Ian; Buettner, Irene] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Cloutis, Edward A.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada. [Reddy, Vishnu; Le Corre, Lucille; Prettyman, Tom] Planetary Sci Inst, Tucson, AZ 85719 USA. [Mengel, Kurt] Tech Univ Clausthal, D-38678 Clausthal Zellerfeld, Germany. [Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Raymond, Carol] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Schmedemann, Nico; Kneissl, Thomas] Free Univ Berlin, Berlin, Germany. RP Nathues, A (reprint author), Max Planck Inst Solar Syst Res, Justus von Liebig Weg 3, D-37077 Gottingen, Germany. EM nathues@mps.mpg.de OI Reddy, Vishnu/0000-0002-7743-3491; Prettyman, Thomas/0000-0003-0072-2831; Le Corre, Lucille/0000-0003-0349-7932 FU Max Planck Society; DLR; NASA/JPL FX The authors would like to thank the Dawn Flight Operations team for a successful Vesta phase. AN would like to thank MPS, DLR and IDA colleagues which worked hard to design, built and test the Framing Cameras. The camera system was developed and built under the leadership of the Max-Planck-Institute for Solar System Research. The Institute for Planetary Research of the German Space Agency DLR provided the Front End Electronics as well as the CCD. The Institute of Computer and Communication Network Engineering provided the main electronics of the cameras. The project is financially supported by the Max Planck Society, DLR, and NASA/JPL. NR 79 TC 15 Z9 15 U1 0 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD SEP 1 PY 2014 VL 239 BP 222 EP 237 DI 10.1016/j.icarus.2014.06.003 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM3WE UT WOS:000339782700020 ER PT J AU Kim, JR Schumann, G Neal, JC Lin, SY AF Kim, Jung-Rack Schumann, Guy Neal, Jeffrey C. Lin, Shih-Yuan TI Megaflood analysis through channel networks of the Athabasca Valles, Mars based on multi-resolution stereo DTMs and 2D hydrodynamic modeling SO PLANETARY AND SPACE SCIENCE LA English DT Article DE DTM; Hydraulic model; Mars; Stereo analysis; Water flow ID ORBITER LASER ALTIMETER; DIGITAL TERRAIN MODELS; CERBERUS FOSSAE; LAVA; GROUNDWATER; EMPLACEMENT; DEPOSITS; ELYSIUM; EQUATOR; SURFACE AB Stereo analysis of in-orbital imagery provides valuable topographic data for scientific research over planetary surfaces especially for the interpretation of potential fluvial activity. The focus of research into planetary fluvial activity has been shifting toward quantitative modeling with various spatial resolution DTMs from visual interpretation with ortho images. Thus in this study, we tested the application of hydraulic analysis with multi resolution Martian DTMs, which were constructed following the approaches of Kim and Muller (2009). Planet. Space Sci. 57 (14), 2095. Subsequently, a two-dimensional hydraulic model was introduced to conduct flow simulation using the extracted 1.2-150 m resolution DTMs. As a result, it was found that the simulated water flows coincided with what might be water eroded geomorphic features over target areas. Moreover, the information acquired from the modeling, such as water depth along the time line, flow direction and travel time, is proving of great value for the interpretation of surface characteristics. Results highlighted the importance of DTM quality for simulating fluvial channel hydraulics across planetary surfaces. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Kim, Jung-Rack] Univ Seoul, Dept Geoinformat, Seoul 130743, South Korea. [Schumann, Guy] CALTECH, NASA, Jet Prop Lab, Pasadena, CA USA. [Neal, Jeffrey C.] Univ Bristol, Sch Geog Sci, Bristol, Avon, England. [Lin, Shih-Yuan] Natl Chengchi Univ, Dept Land Econ, Taipei 11623, Taiwan. RP Kim, JR (reprint author), Univ Seoul, Dept Geoinformat, 163 Seoulsiripdaero, Seoul 130743, South Korea. EM kjrr001@gmail.com RI Schumann, Guy/F-9760-2011 FU National Research Foundation of Korea [2013078206]; National Aeronautics and Space Administration FX The authors would like to acknowledge the HRSC-CoI team, especially the former PI, Prof. Gerhard Neukum and the HiRISE team for providing the valuable data sets. The first author would like to thank National Research Foundation of Korea for supporting this study (Grant no. 2013078206). Guy Schumann's time at the Jet Propulsion Laboratory, California Institute of Technology was funded under a contract with the National Aeronautics and Space Administration. NR 50 TC 3 Z9 3 U1 0 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD SEP PY 2014 VL 99 BP 55 EP 69 DI 10.1016/j.pss.2014.04.010 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2SA UT WOS:000339699900007 ER PT J AU Szwarc, T Hubbard, S AF Szwarc, Timothy Hubbard, Scott TI Thermal mapping and trends of Mars analog materials in sample acquisition operations using experimentation and models SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Rotary-percussive; Coring; Drilling; Mars; Analog ID STRENGTH; ROCK AB The effects of atmosphere, ambient temperature, and geologic material were studied experimentally and using a computer model to predict the heating undergone by Mars rocks during rover sampling operations. Tests were performed on five well-characterized and/or Mars analog materials: Indiana limestone, Saddleback basalt, kaolinite, travertine, and water ice. Eighteen tests were conducted to 55 mm depth using a Mars Sample Return prototype coring drill, with each sample containing six thermal sensors. A thermal simulation was written to predict the complete thermal profile within each sample during coring and this model was shown to be capable of predicting temperature increases with an average error of about 7%. This model may be used to schedule power levels and periods of rest during actual sample acquisition processes to avoid damaging samples or freezing the bit into icy formations. Maximum rock temperature increase is found to be modeled by a power law incorporating rock and operational parameters. Energy transmission efficiency in coring is found to increase linearly with rock hardness and decrease by 31% at Mars pressure. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Szwarc, Timothy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hubbard, Scott] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA. RP Szwarc, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM timothy.j.szwarc@jpl.nasa.gov; scotthub@stanford.edu FU JPL Strategic University research Partnership (SURP) [1481914] FX This research was made possible by the financial support of the JPL Strategic University research Partnership (SURP) (1481914). The authors would like to thank Neil Murphy and Lori Shiraishi of JPL. Experimental work was conducted at Honeybee Robotics Spacecraft Mechanisms corporation in Pasadena, CA. In particular, the authors would like to thank Dr. Kris Zacny and Gale Paulsen for their time and resources. The authors would also like to thank Professor Brian Cantwell, Professor Richard Christensen, and Professor David Pollard of Stanford University for their input to the experimental test plan and analysis. NR 12 TC 0 Z9 0 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 SEP PY 2014 VL 99 BP 158 EP 166 DI 10.1016/j.pss.2014.06.002 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2SA UT WOS:000339699900016 ER PT J AU McGillivray, DA Cravey, RL Dudley, KL Vedeler, E Gupta, MC AF McGillivray, Duncan A. Cravey, Robin L. Dudley, Kenneth L. Vedeler, Erik Gupta, Mool C. TI POLARIZATION PROPERTIES OF A 2-D SPLIT RING RESONATOR AND ROD TYPE METAMATERIAL LENS SO MICROWAVE AND OPTICAL TECHNOLOGY LETTERS LA English DT Article DE metamaterials; split ring resonators; polarization; transmission; sensors; metamaterial lens ID NEGATIVE REFRACTION AB The polarization state of microwave (MW) radiation transmitted through a 2-D split ring resonator and rod metamaterial (MTM) lens is investigated. At a resonance frequency of 3.63 GHz, the 2-D lens modifies the polarization state of the incident radiation. For E-y incident polarization, the transmitted wave exhibits elliptical polarization as well as a tilt in the principal axis. The ellipticity is dependent on the incident polarization angle. A Ex polarized incident MW is unaffected. Transformation of polarization properties plays an important role for manipulation and control of MW radiation, impacting existing applications and providing opportunities for novel MTMs-based sensors and other applications. (C) 2014 Wiley Periodicals, Inc. C1 [McGillivray, Duncan A.; Gupta, Mool C.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. [Cravey, Robin L.; Dudley, Kenneth L.; Vedeler, Erik] NASA, Langley Res Ctr, Electromagnet & Sensors Branch, Hampton, VA 23681 USA. RP Gupta, MC (reprint author), Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. EM mgupta@virginia.edu NR 16 TC 0 Z9 0 U1 2 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0895-2477 EI 1098-2760 J9 MICROW OPT TECHN LET JI Microw. Opt. Technol. Lett. PD SEP PY 2014 VL 56 IS 9 BP 2146 EP 2150 DI 10.1002/mop.28547 PG 6 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA AL9DE UT WOS:000339439000047 ER PT J AU Madni, AM Sievers, M AF Madni, Azad M. Sievers, Michael TI System of Systems Integration: Key Considerations and Challenges SO SYSTEMS ENGINEERING LA English DT Article DE system of systems; system of systems integration; human-systems integration; interoperability; integration ontology ID FUTURE AB As systems are called on to participate on demand within system-of-systems (SoS), system-of-systems integration (SoSI) has become a key concern. This capability is especially important in defense and aerospace where systems are increasingly required to interoperate on demand to satisfy mission requirements. SoSI is also becoming increasingly important in healthcare and energy domains. SoSI involves interfacing and enabling the interactions of component systems to create the needed SoS capability to accomplish mission or business goals. SoSI, which is part of the overall SoS development life cycle, increases in complexity when there are legacy systems that need to be integrated, and when humans are tasked to perform in various capacities within the SoS. An added layer of complexity is introduced when the SoS has to exhibit certain quality attributes such as adaptability and resilience in the face of contingencies and disruptions in the operational environment. This paper addresses key considerations and challenges in SoSI. (C) 2013 Wiley Periodicals, Inc. C1 [Madni, Azad M.] Univ So Calif, Daniel J Epstein Dept Ind & Syst Engn, Viterbi Sch Engn, Los Angeles, CA 90089 USA. [Sievers, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Madni, AM (reprint author), Univ So Calif, Daniel J Epstein Dept Ind & Syst Engn, Viterbi Sch Engn, Los Angeles, CA 90089 USA. EM azad.madni@usc.edu NR 43 TC 6 Z9 6 U1 1 U2 25 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1098-1241 EI 1520-6858 J9 SYSTEMS ENG JI Syst. Eng. PD FAL PY 2014 VL 17 IS 3 BP 330 EP 347 DI 10.1002/sys.21272 PG 18 WC Engineering, Industrial; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA AL8HG UT WOS:000339378300006 ER PT J AU Weisbin, CR Lincoln, W Saatchi, S AF Weisbin, Charles R. Lincoln, William Saatchi, Sassan TI A Systems Engineering Approach to Estimating Uncertainty in Above-Ground Biomass (AGB) Derived from Remote-Sensing Data SO SYSTEMS ENGINEERING LA English DT Article DE above-ground biomass (AGB); uncertainty; correlation of uncertainties; remote sensing; carbon; carbon cycle; carbon monitoring; carbon measurement; forests; risk reduction ID RADAR BACKSCATTER; TROPICAL REGIONS; FOREST BIOMASS; CARBON STOCKS; SAR DATA; DEFORESTATION; INVENTORY; EMISSIONS; LIDAR; MAP AB We integrate systems of measurement and modeling to improve estimation of uncertainties in above-ground biomass (AGB) derived from remote sensing. The outcome provides a unified starting point for the climate-change carbon community to assess uncertainty and sensitivity data and methodologies, and ultimately supports decision-making about which missions and instruments to develop for a desired cost/benefit ratio. Initial results include fusion of remote-sensing techniques (e. g., radar and lidar), uncertainties associated with measurement and modeling, and the impact of potential uncertainty correlations across aggregated unit areas. Biomass uncertainty estimates are presented at the single-hectare level for the forestlands of California. Using a forest biomass map of California, we calculate changes in variance (e. g., 2 orders of magnitude) as a function of uncertainty correlation assumptions, with correlations extending to spatial scales up to 100 km. Using a variogram formalism to derive the correlation shape and magnitude, we show that the estimated variance for California above-ground biomass is between 1% and 2% (1 standard deviation) for our current best estimate of the correlation range at 5-10 km-i.e., we bound the standard deviation by a factor of 2. This contrasts with 0.025% (1 standard deviation) if one does not include the correlation term. (C) 2013 Wiley Periodicals, Inc. C1 [Weisbin, Charles R.; Lincoln, William; Saatchi, Sassan] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA. RP Weisbin, CR (reprint author), CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA. EM Charles.R.Weisbin@jpl.nasa.gov; William.Lincoln@jpl.nasa.gov; Saatchi@jpl.nasa.gov FU NASA under the Carbon Monitoring System study task within the NASA Earth Science Program FX NASA under the Carbon Monitoring System study task within the NASA Earth Science Program. NR 43 TC 1 Z9 1 U1 1 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1098-1241 EI 1520-6858 J9 SYSTEMS ENG JI Syst. Eng. PD FAL PY 2014 VL 17 IS 3 BP 361 EP 373 DI 10.1002/sys.21275 PG 13 WC Engineering, Industrial; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA AL8HG UT WOS:000339378300008 ER PT J AU Guhathakurta, M AF Guhathakurta, Madhulika TI Preface SO SOLAR PHYSICS LA English DT Editorial Material C1 NASA Headquarters, Washington, DC 20546 USA. RP Guhathakurta, M (reprint author), NASA Headquarters, Washington, DC 20546 USA. EM madhulika.guhathakurta@nasa.gov NR 17 TC 1 Z9 1 U1 0 U2 1 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 SEP PY 2014 VL 289 IS 9 BP 3231 EP 3232 DI 10.1007/s11207-014-0560-4 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL3AL UT WOS:000338997200001 ER PT J AU Liu, W Ofman, L AF Liu, Wei Ofman, Leon TI Advances in Observing Various Coronal EUV Waves in the SDO Era and Their Seismological Applications (Invited Review) SO SOLAR PHYSICS LA English DT Article DE Corona, structures; Coronal mass ejections, low coronal signatures; Coronal seismology; Flares, waves; Waves, magnetohydrodynamic; Waves, propagation ID EXTREME-ULTRAVIOLET WAVE; KELVIN-HELMHOLTZ INSTABILITY; QUASI-PERIODIC PULSATIONS; SOLAR ENERGETIC PARTICLES; MAGNETIC-FIELD STRENGTH; FAST MAGNETOSONIC WAVES; 2011 FEBRUARY 15; EMISSION MEASURE DIAGNOSTICS; IMAGING TELESCOPE WAVE; MICRO-SIGMOID ERUPTION AB Global extreme-ultraviolet (EUV) waves are spectacular traveling disturbances in the solar corona associated with energetic eruptions such as coronal mass ejections (CMEs) and flares. Over the past 15 years, observations from three generations of space-borne EUV telescopes have shaped our understanding of this phenomenon and at the same time led to controversy about its physical nature. Since its launch in 2010, the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) has observed more than 210 global EUV waves in exquisite detail, thanks to its high spatio-temporal resolution and full-disk, wide-temperature coverage. A combination of statistical analysis of this large sample, more than 30 detailed case studies, and data-driven MHD modeling, has been leading their physical interpretations to a convergence, favoring a bimodal composition of an outer, fast-mode magnetosonic wave component and an inner, non-wave CME component. Adding to this multifaceted picture, AIA has also discovered new EUV wave and wave-like phenomena associated with various eruptions, including quasi-periodic fast propagating (QFP) wave trains, magnetic Kelvin-Helmholtz instabilities (KHI) in the corona and associated nonlinear waves, and a variety of mini-EUV waves. Seismological applications using such waves are now being actively pursued, especially for the global corona. We review such advances in EUV wave research focusing on recent SDO/AIA observations, their seismological applications, related data-analysis techniques, and numerical and analytical models. C1 [Liu, Wei] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Liu, Wei] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Ofman, Leon] Catholic Univ Amer, Greenbelt, MD 20771 USA. [Ofman, Leon] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ofman, Leon] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. RP Liu, W (reprint author), Lockheed Martin Solar & Astrophys Lab, Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA. EM weiliu@lmsal.com; Leon.Ofman@nasa.gov OI Liu, Wei/0000-0001-8794-3420 FU NASA Living With a Star (LWS) Program [NNX11AO68G]; NASA [NNX12AB34G] FX This work is supported by the NASA Living With a Star (LWS) Program (grant NNX11AO68G). Additional support to LO was provided by NASA grant NNX12AB34G. Special thanks go to Barbara Thompson for inviting both authors to the 2013 LWS SDO Science Workshop that led to this topical issue and this review. We are grateful to the anonymous referee for constructive comments and suggestions that helped improve this article. WL thanks Nariaki Nitta, Cooper Downs, Barbara Thompson, Angelos Vourlidas, Peng-Fei Chen, Spiros Patsourakos, and Kyoung-Sun Lee for critical comments on the manuscript and/or fruitful discussions. We thank Suli Ma, Alexander Warmuth, Nariaki Nitta, Ding Yuan, Ute Mostl (now Ute Amerstorfer), Nat Gopalswamy, Jason Byrne, and David Pascoe for providing the original figures, and especially Cooper Downs, Liheng Yang, Ting Li, Eoin Carley, and Ryun-Young Kwon for customizing their figures to fit the layout of this article. Figures 1c and 1d, 2, 3, 4 (right), 5, 6a, 6c, and 6i, 8, 9, 11 (middle and right), 12a, 13, 14, 15a-15c, and 16 (left and middle) are reproduced by permission of the AAS. Figures 4 (left), 11 (left), 15 (right), and 16 (right) are reproduced with permission from Astronomy & Astrophysics, (C) ESO. NR 281 TC 63 Z9 64 U1 5 U2 15 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 SEP PY 2014 VL 289 IS 9 BP 3233 EP 3277 DI 10.1007/s11207-014-0528-4 PG 45 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL3AL UT WOS:000338997200002 ER PT J AU Young, PR Muglach, K AF Young, P. R. Muglach, K. TI Solar Dynamics Observatory and Hinode Observations of a Blowout Jet in a Coronal Hole SO SOLAR PHYSICS LA English DT Article DE Coronal holes; Jets; Magnetic fields, photosphere; Spectral line, intensity and diagnostics; Spectrum, ultraviolet; Velocity fields, photosphere ID X-RAY TELESCOPE; MAGNETIC-FIELD; IMAGING SPECTROMETER; ATOMIC DATABASE; EMISSION-LINES; QUIET SUN; SDO; MISSION; BOUNDARIES; CHIANTI AB A blowout jet occurred within the south coronal hole on 9 February 2011 at 09:00 UT and was observed by the Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory, and by the EUV Imaging Spectrometer (EIS) and X-Ray Telescope (XRT) onboard the Hinode spacecraft during coronal-hole monitoring performed as part of Hinode Operations Program No. 177. Images from AIA show expanding hot and cold loops from a small bright point with plasma ejected in a curtain up to 30 Mm wide. The initial intensity front of the jet had a projected velocity of 200 km s(-1), and the line-of-sight (LOS) velocities measured by EIS are between 100 and 250 km s(-1). The LOS velocities increased along the jet, implying that an acceleration mechanism operates within the body of the jet. The jet plasma had a density of 2.7x10(8) cm(-3) and a temperature of 1.4 MK. During the event a number of bright kernels were seen at the base of the bright point. The kernels have sizes of a parts per thousand aEuro parts per thousand 1000 km, are variable in brightness, and have lifetimes of 1 -aEuro parts per thousand 15 minutes. An XRT filter ratio yields temperatures of 1.5 -aEuro parts per thousand 3.0 MK for the kernels. The bright point existed for at least ten hours, but disappeared within two hours after the jet, which lasted for 30 minutes. HMI data reveal converging photospheric flows at the location of the bright point, and the mixed-polarity magnetic flux canceled over a period of four hours on either side of the jet. C1 [Young, P. R.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Muglach, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Muglach, K.] ARTEP Inc, Ellicott City, MD 21042 USA. RP Young, PR (reprint author), George Mason Univ, Coll Sci, 4400 Univ Dr, Fairfax, VA 22030 USA. EM pyoung9@gmu.edu; kmuglach@gmx.de OI Young, Peter/0000-0001-9034-2925 FU National Science Foundation [AGS-1159353] FX The authors acknowledge funding from National Science Foundation grant AGS-1159353. Valuable comments from the anonymous referee and E. Pariat are acknowledged. SDO is a mission for NASA's Living With a Star program. Data are provided courtesy of NASA/SDO and the AIA and HMI science teams. 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 co-operation with ESA and NSC (Norway). NR 31 TC 22 Z9 22 U1 0 U2 5 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 SEP PY 2014 VL 289 IS 9 BP 3313 EP 3329 DI 10.1007/s11207-014-0484-z PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL3AL UT WOS:000338997200005 ER PT J AU Karna, N Webber, SAH Pesnell, WD AF Karna, N. Webber, S. A. Hess Pesnell, W. D. TI Using Polar Coronal Hole Area Measurements to Determine the Solar Polar Magnetic Field Reversal in Solar Cycle 24 SO SOLAR PHYSICS LA English DT Article DE Coronal holes; Solar cycle; Magnetic reversal; Observation ID EXTREME-ULTRAVIOLET OBSERVATIONS AB An analysis of solar polar coronal hole (PCH) areas since the launch of the Solar Dynamics Observatory (SDO) shows how the polar regions have evolved during Solar Cycle 24. We present PCH areas from mid-2010 through 2013 using data from the Atmospheric Imager Assembly (AIA) and Helioseismic and Magnetic Imager (HMI) instruments onboard SDO. Our analysis shows that both the northern and southern PCH areas have decreased significantly in size since 2010. Linear fits to the areas derived from the magnetic-field properties indicate that, although the northern hemisphere went through polar-field reversal and reached solar-maximum conditions in mid-2012, the southern hemisphere had not reached solar-maximum conditions in the polar regions by the end of 2013. Our results show that solar-maximum conditions in each hemisphere, as measured by the area of the polar coronal holes and polar magnetic field, will be offset in time. C1 [Karna, N.; Webber, S. A. Hess; Pesnell, W. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Karna, N.; Webber, S. A. Hess] George Mason Univ, Fairfax, VA 22030 USA. RP Pesnell, WD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM nkarna@masonlive.gmu.edu; shessweb@masonlive.gmu.edu; william.d.pesnell@nasa.gov RI Pesnell, William/D-1062-2012; OI Pesnell, William/0000-0002-8306-2500; Hess Webber, Shea A/0000-0002-3631-6491 FU Schlumberger Foundation Faculty for the Future; Catholic University of America; NASA's Solar Dynamics Observatory FX N. Karna thanks the Schlumberger Foundation Faculty for the Future for supporting this research. S. A. Hess Webber thanks the Catholic University of America and NASA's Solar Dynamics Observatory for supporting this research. The AIA and HMI data are courtesy of NASA/SDO and the AIA and HMI Science Investigation Teams. The HMI radial synoptic maps are available at the Stanford website. The GMU AIA Synoptic Maps Dataset can be accessed at the George Mason University (GMU) Space Weather Lab. The EIT images are courtesy of the SOHO/EIT consortium. SOHO is a mission of international cooperation between ESA and NASA. The MDI images are provided by the Solar Oscillations Investigation (SOI) team at the Stanford-Lockheed Institute for Space Research. Daily sunspot areas dataset were obtained from NASA/Marshall Solar Physics. Daily values of International Sunspot Number, [RZ], were obtained from the National Geophysical Data Center in Boulder, CO, USA. NR 22 TC 12 Z9 12 U1 0 U2 4 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 SEP PY 2014 VL 289 IS 9 BP 3381 EP 3390 DI 10.1007/s11207-014-0541-7 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL3AL UT WOS:000338997200009 ER PT J AU Duvall, TL Hanasoge, SM Chakraborty, S AF Duvall, T. L., Jr. Hanasoge, S. M. Chakraborty, S. TI Additional Evidence Supporting a Model of Shallow, High-Speed Supergranulation SO SOLAR PHYSICS LA English DT Article DE Helioseismology, observations; Helioseismology, direct modeling; Interior, convective zone; Supergranulation; Velocity fields, interior ID TIME-DISTANCE HELIOSEISMOLOGY; SOLAR INTERIOR; TRAVEL-TIMES; FLOWS; INVERSIONS; ATMOSPHERE; KERNELS AB Recently, Duvall and Hanasoge (Solar Phys. 287, 71, 2013) found that large-distance separation [Delta] travel-time differences from a center to an annulus [delta t (oi)] implied a model of the average supergranular cell that has a peak upflow of 240 m s(-1) at a depth of 2.3 Mm and a corresponding peak outward horizontal flow of 700 m s(-1) at a depth of 1.6 Mm. In the present work, this effect is further studied by measuring and modeling center-to-quadrant travel-time differences [delta t (qu)], which roughly agree with this model. Simulations are analyzed that show that such a model flow would lead to the expected travel-time differences. As a check for possible systematic errors, the center-to-annulus travel-time differences [delta t (oi)] are found not to vary with heliocentric angle. A consistency check finds an increase of delta t (oi) with the temporal frequency [nu] by a factor of two, which is not predicted by the ray theory. C1 [Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Hanasoge, S. M.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Hanasoge, S. M.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Chakraborty, S.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. RP Duvall, TL (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. EM Thomas.L.Duvall@nasa.gov; hanasoge@tifr.res.in; deepc@stanford.edu FU NASA SDO FX The data used here are courtesy of NASA/SDO and the HMI Science Team. We thank the HMI team members for their hard work. This work is supported by NASA SDO. NR 27 TC 8 Z9 8 U1 0 U2 0 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 SEP PY 2014 VL 289 IS 9 BP 3421 EP 3433 DI 10.1007/s11207-014-0537-3 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL3AL UT WOS:000338997200012 ER PT J AU Nagashima, K Loptien, B Gizon, L Birch, AC Cameron, R Couvidat, S Danilovic, S Fleck, B Stein, R AF Nagashima, Kaori Loeptien, Bjoern Gizon, Laurent Birch, Aaron C. Cameron, Robert Couvidat, Sebastien Danilovic, Sanja Fleck, Bernhard Stein, Robert TI Interpreting the Helioseismic and Magnetic Imager (HMI) Multi-Height Velocity Measurements SO SOLAR PHYSICS LA English DT Article DE Velocity fields, photosphere; Oscillations, solar; Helioseismology, observations ID SCALE CONVECTION SIMULATIONS; DYNAMICS-OBSERVATORY SDO; SOLAR PHOTOSPHERE; GRAVITY-WAVES; OSCILLATION MODES; ENERGY FLUX; ATMOSPHERE; CHROMOSPHERE; SURFACE; MURAM AB The Solar Dynamics Observatory/Helioseismic and Magnetic Imager (SDO/HMI) filtergrams, taken at six wavelengths around the Fe i 6173.3 line, contain information about the line-of-sight velocity over a range of heights in the solar atmosphere. Multi-height velocity inferences from these observations can be exploited to study wave motions and energy transport in the atmosphere. Using realistic convection-simulation datasets provided by the STAGGER and MURaM codes, we generate synthetic filtergrams and explore several methods for estimating Dopplergrams. We investigate at which height each synthetic Dopplergram correlates most strongly with the vertical velocity in the model atmospheres. On the basis of the investigation, we propose two Dopplergrams other than the standard HMI-algorithm Dopplergram produced from HMI filtergrams: a line-center Dopplergram and an average-wing Dopplergram. These two Dopplergrams correlate most strongly with vertical velocities at the heights of 30 -aEuro parts per thousand 40 km above (line center) and 30 -aEuro parts per thousand 40 km below (average wing) the effective height of the HMI-algorithm Dopplergram. Therefore, we can obtain velocity information from two layers separated by about a half of a scale height in the atmosphere, at best. The phase shifts between these multi-height Dopplergrams from observational data as well as those from the simulated data are also consistent with the height-difference estimates in the frequency range above the photospheric acoustic-cutoff frequency. C1 [Nagashima, Kaori; Gizon, Laurent; Birch, Aaron C.; Cameron, Robert; Danilovic, Sanja] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Loeptien, Bjoern; Gizon, Laurent] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Couvidat, Sebastien] Stanford Univ, Stanford, CA 94305 USA. [Fleck, Bernhard] NASA, Goddard Space Flight Ctr, ESA Sci Operat Dept, Greenbelt, MD 20771 USA. [Stein, Robert] Michigan State Univ, E Lansing, MI 48824 USA. RP Nagashima, K (reprint author), Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany. EM nagashima@mps.mpg.de OI Nagashima, Kaori/0000-0002-6927-2392 FU IMPRS Solar System School; EU; DFG [SFB 963]; NASA [NNX12AH49G]; NSF [AGS1141921]; German Aerospace Center (DLR) FX BL acknowledges support from the IMPRS Solar System School. BL computed the line profiles from the STAGGER data cubes and the response functions using the SPINOR code. We thank Michiel van Noort, Thomas Straus, and Jesper Schou for helpful discussions and comments. KN and LG acknowledge support from EU FP7 Collaborative Project "Exploitation of Space Data for Innovative Helio- and Asteroseismology" (SPACEINN). LG acknowledges support from DFG SFB 963 "Astrophysical Flow Instabilities and Turbulence" (Project A1). The HMI data used are courtesy of NASA/SDO and the HMI science team. This work was carried out using the data from the SDO HMI/AIA Joint Science Operations Center Data Record Management System and Storage Unit Management System (JSOC DRMS/SUMS). The NSO/Kitt Peak FTS data used here were produced by NSF/NSO. RS acknowledges support by NASA grant NNX12AH49G and NSF grant AGS1141921. The STAGGER calculations were performed on the Pleiades cluster of the NASA Advanced Supercomputing Division at Ames Research Center. The German Data Center for SDO (GDC-SDO), funded by the German Aerospace Center (DLR), provided the IT infrastructure to process the data. NR 37 TC 4 Z9 4 U1 0 U2 4 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 SEP PY 2014 VL 289 IS 9 BP 3457 EP 3481 DI 10.1007/s11207-014-0543-5 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL3AL UT WOS:000338997200014 ER PT J AU Hoeksema, JT Liu, Y Hayashi, K Sun, XD Schou, J Couvidat, S Norton, A Bobra, M Centeno, R Leka, KD Barnes, G Turmon, M AF Hoeksema, J. Todd Liu, Yang Hayashi, Keiji Sun, Xudong Schou, Jesper Couvidat, Sebastien Norton, Aimee Bobra, Monica Centeno, Rebecca Leka, K. D. Barnes, Graham Turmon, Michael TI The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Overview and Performance SO SOLAR PHYSICS LA English DT Article DE Magnetic fields, photosphere; HMI: vector field; Solar active regions ID QUIET ACTIVE REGIONS; DYNAMICS-OBSERVATORY SDO; MAJOR SOLAR-FLARES; MAGNETOGRAMS; AMBIGUITY; MISSION; SAMPLE AB The Helioseismic and Magnetic Imager (HMI) began near-continuous full-disk solar measurements on 1 May 2010 from the Solar Dynamics Observatory (SDO). An automated processing pipeline keeps pace with observations to produce observable quantities, including the photospheric vector magnetic field, from sequences of filtergrams. The basic vector-field frame list cadence is 135 seconds, but to reduce noise the filtergrams are combined to derive data products every 720 seconds. The primary 720 s observables were released in mid-2010, including Stokes polarization parameters measured at six wavelengths, as well as intensity, Doppler velocity, and the line-of-sight magnetic field. More advanced products, including the full vector magnetic field, are now available. Automatically identified HMI Active Region Patches (HARPs) track the location and shape of magnetic regions throughout their lifetime. The vector field is computed using the Very Fast Inversion of the Stokes Vector (VFISV) code optimized for the HMI pipeline; the remaining 180(a similar to) azimuth ambiguity is resolved with the Minimum Energy (ME0) code. The Milne-Eddington inversion is performed on all full-disk HMI observations. The disambiguation, until recently run only on HARP regions, is now implemented for the full disk. Vector and scalar quantities in the patches are used to derive active region indices potentially useful for forecasting; the data maps and indices are collected in the SHARP data series, hmi.sharp_720s. Definitive SHARP processing is completed only after the region rotates off the visible disk; quick-look products are produced in near real time. Patches are provided in both CCD and heliographic coordinates. HMI provides continuous coverage of the vector field, but has modest spatial, spectral, and temporal resolution. Coupled with limitations of the analysis and interpretation techniques, effects of the orbital velocity, and instrument performance, the resulting measurements have a certain dynamic range and sensitivity and are subject to systematic errors and uncertainties that are characterized in this report. C1 [Hoeksema, J. Todd; Liu, Yang; Hayashi, Keiji; Sun, Xudong; Schou, Jesper; Couvidat, Sebastien; Norton, Aimee; Bobra, Monica] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Centeno, Rebecca] High Altitude Observ NCAR, Boulder, CO USA. [Leka, K. D.; Barnes, Graham] Northwest Res Associates Inc, Boulder, CO USA. [Turmon, Michael] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Schou, Jesper] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. RP Hoeksema, JT (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. EM todd@sun.stanford.edu RI Sun, Xudong/M-3245-2013 OI Sun, Xudong/0000-0003-4043-616X FU NASA [NAS5-02139, NNH09CF22C]; National Science Foundation; NASA/Goddard Space Flight Center [PO#NNG12PP28D/C#GS-23F-0197P]; EU FX We thank the numerous team members who have contributed to the success of the SDO mission and particularly to the HMI instrument. This work was supported by NASA Contract NAS5-02139 (HMI) to Stanford University. Some of the research described here was carried out by staff of the Jet Propulsion Laboratory, California Institute of Technology. HAO/NCAR is supported by the National Science Foundation. Efforts at NWRA were also supported through NASA Contract NNH09CF22C and by PO#NNG12PP28D/C#GS-23F-0197P from NASA/Goddard Space Flight Center. J. Schou acknowledges support from EU FP7 Collaborative Project Exploitation of Space Data for Innovative Helio- and Asteroseismology (SPACEINN). NR 50 TC 84 Z9 84 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD SEP PY 2014 VL 289 IS 9 BP 3483 EP 3530 DI 10.1007/s11207-014-0516-8 PG 48 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL3AL UT WOS:000338997200015 ER PT J AU Bobra, MG Sun, X Hoeksema, JT Turmon, M Liu, Y Hayashi, K Barnes, G Leka, KD AF Bobra, M. G. Sun, X. Hoeksema, J. T. Turmon, M. Liu, Y. Hayashi, K. Barnes, G. Leka, K. D. TI The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: SHARPs - Space-Weather HMI Active Region Patches SO SOLAR PHYSICS LA English DT Article DE Active regions, magnetic fields; Flares, relation to magnetic field; Instrumentation and data management ID MAJOR SOLAR-FLARES; NULL POINTS; ENERGY; FLUX; MAGNETOGRAMS; HELICITY; SHEAR; PRODUCTIVITY; EMERGENCE; EVOLUTION AB A new data product from the Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO) called Space-weather HMI Active Region Patches (SHARPs) is now available. SDO/HMI is the first space-based instrument to map the full-disk photospheric vector magnetic field with high cadence and continuity. The SHARP data series provide maps in patches that encompass automatically tracked magnetic concentrations for their entire lifetime; map quantities include the photospheric vector magnetic field and its uncertainty, along with Doppler velocity, continuum intensity, and line-of-sight magnetic field. Furthermore, keywords in the SHARP data series provide several parameters that concisely characterize the magnetic-field distribution and its deviation from a potential-field configuration. These indices may be useful for active-region event forecasting and for identifying regions of interest. The indices are calculated per patch and are available on a twelve-minute cadence. Quick-look data are available within approximately three hours of observation; definitive science products are produced approximately five weeks later. SHARP data are available at jsoc.stanford.edu and maps are available in either of two different coordinate systems. This article describes the SHARP data products and presents examples of SHARP data and parameters. C1 [Bobra, M. G.; Sun, X.; Hoeksema, J. T.; Liu, Y.; Hayashi, K.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Turmon, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Barnes, G.; Leka, K. D.] Northwest Res Associates Inc, Boulder, CO USA. RP Hoeksema, JT (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. EM jthoeksema@sun.stanford.edu RI Sun, Xudong/M-3245-2013 OI Sun, Xudong/0000-0003-4043-616X FU NASA [NAS5-02139, NNH09CF22C, NNH12CG10C]; NASA/Goddard Space Flight Center [NNG12PP28D/C# GS-23F-0197P] FX We thank the many team members who have contributed to the success of the SDO mission and particularly to the HMI instrument. This work was supported by NASA Contract NAS5-02139 (HMI) to Stanford University. Some of the research described here was carried out by staff of the Jet Propulsion Laboratory, California Institute of Technology. Efforts at NWRA were also supported through NASA Contracts NNH09CF22C and NNH12CG10C and by NNG12PP28D/C# GS-23F-0197P from NASA/Goddard Space Flight Center. The authors thank Huned Botee for development of the SHARP Data Viewer. NR 58 TC 54 Z9 54 U1 1 U2 5 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 SEP PY 2014 VL 289 IS 9 BP 3549 EP 3578 DI 10.1007/s11207-014-0529-3 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL3AL UT WOS:000338997200017 ER PT J AU Ault, JS Smith, SG Browder, JA Nuttle, W Franklin, EC Luo, J DiNardoe, GT Bohnsack, JA AF Ault, J. S. Smith, S. G. Browder, J. A. Nuttle, W. Franklin, E. C. Luo, J. DiNardoe, G. T. Bohnsack, J. A. TI Indicators for assessing the ecological dynamics and sustainability of southern Florida's coral reef and coastal fisheries SO ECOLOGICAL INDICATORS LA English DT Article DE Average size; Length-based assessment; Fishery exploitation; Community-level sustainability ID LENGTH-BASED ASSESSMENT; STOCK PRODUCTION MODEL; FISH STOCKS; REFERENCE POINTS; AVERAGE-LENGTH; MANAGEMENT; PERFORMANCE; SITUATIONS; MORTALITY; STEEPNESS AB Commercial and recreational fisheries target hundreds of fish and shellfish species across the seascape of southern Florida including inshore coastal bays, the flats of barrier islands, coral reefs and offshore pelagic waters. The ecological dynamics and economic sustainability of these valuable fishery resources are key conservation concerns. This study examined two ecological indicators of fishing impacts on exploited populations: (1) the more traditional metric catch per unit of fishing effort (CPUE); and (2) the non-traditional metric average length (L) in the exploited life stage of a population. We show that both indicators were closely related to stock productivity via fisheries population dynamics theory, and that either indicator could be used to estimate fishing mortality rates (F). Data requirements are much less stringent for estimating F from the L indicator than CPUE, making it more practical for data-poor situations common to tropical marine fisheries. Using indicator-based estimates of F within a population dynamic modeling framework enabled an evaluation of fishing impacts on sustainability at both the species and community levels, an important step toward ecosystem-based fisheries assessment and management. A comparison of these approaches applied to the assessment of southern Florida coral reef fisheries suggested that fishing has fundamentally altered the ecological structure of the fish community by depleting the biomass of higher-trophic level carnivores to the extent that the stocks are unsustainable. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Ault, J. S.; Smith, S. G.; Luo, J.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Browder, J. A.; Bohnsack, J. A.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Miami, FL 33149 USA. [Nuttle, W.] Ecohydrol Com, Ottawa, ON K1SB46, Canada. [Franklin, E. C.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Kaneohe, HI 96744 USA. [DiNardoe, G. T.] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. RP Ault, JS (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. EM jault@rsmas.miami.edu RI Ault, Jerald/A-5241-2008 OI Ault, Jerald/0000-0001-9657-8007 FU NOAA NOS CSCOR Program Award [NA08OAR4320889]; Bonefish and Tarpon Trust; Robertson Foundation; NOAA Pacific Islands Fisheries Science Center iREEF (Integrated Reef Ecosystem Evaluation Framework) [WE- 133F-12-SE-2099]; NOAA Pulley Ridge Grant [NA11NOS4780045]; Papahanumokuakea MNS Grant [RA133C12SE2107]; National Fish and Wildlife Foundation Grant [0302-12-031178]; NOAA Fisheries Coral Reef Conservation Program Grant [NA17RJ1226]; NOM MARFIN Grant [NA11NMF4330129]; National Science Foundation [EAR-1204752] FX We appreciate the technical assistance provided by M.S. Adams, D.R. Bryan, M.O. Nadon and N.R. Vaughan. This paper is a result of research under the Marine and Estuarine Goal Setting (MARES) for South Florida Project funded by NOAA NOS CSCOR Program Award No. NA08OAR4320889, Bonefish and Tarpon Trust, Robertson Foundation, NOAA Pacific Islands Fisheries Science Center iREEF (Integrated Reef Ecosystem Evaluation Framework) Contract No. WE- 133F-12-SE-2099, NOAA Pulley Ridge Grant No. NA11NOS4780045, Papahanumokuakea MNS Grant No. RA133C12SE2107, National Fish and Wildlife Foundation Grant No. 0302-12-031178, NOAA Fisheries Coral Reef Conservation Program Grant No. NA17RJ1226, and the NOM MARFIN Grant No. NA11NMF4330129. This material was also based upon work supported by the National Science Foundation under Grant No. EAR-1204752. This manuscript was greatly improved by the comments of two anonymous reviewers. NR 35 TC 9 Z9 9 U1 3 U2 58 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1470-160X EI 1872-7034 J9 ECOL INDIC JI Ecol. Indic. PD SEP PY 2014 VL 44 SI SI BP 164 EP 172 DI 10.1016/j.ecolind.2014.04.013 PG 9 WC Biodiversity Conservation; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AK7KX UT WOS:000338608300016 ER PT J AU Martin, W Cairns, B Bal, G AF Martin, William Cairns, Brian Bal, Guillaume TI Adjoint methods for adjusting three-dimensional atmosphere and surface properties to fit multi-angle/multi-pixel polarimetric measurements SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Adjoint methods; Three-dimensional vector radiative transfer; Linearization; Remote sensing; Parameter derivatives ID RADIATIVE-TRANSFER MODEL; DISCRETE ORDINATE METHOD; PERTURBATION-THEORY; SPHERICAL ATMOSPHERE; WEIGHTING FUNCTIONS; OPTICAL TOMOGRAPHY; FREQUENCY-DOMAIN; RETRIEVAL; VALIDATION; ALGORITHM AB This paper derives an efficient procedure for using the three-dimensional (3D) vector radiative transfer equation (VRTE) to adjust atmosphere and surface properties and improve their with multi-angle/multi-pixel radiometric and polarimetric measurements of scattered sunlight The proposed adjoint method uses the 3D VRTE to compute the measurement misfit function and the adjoint 3D VRTE to compute its gradient with respect to all unknown parameters. In the remote sensing problems of interest, the scalar-valued misfit function quantifies with data as a function of atmosphere and surface properties, and its gradient guides the search through this parameter space. Remote sensing of the atmosphere and surface in a three-dimensional region may require thousands of unknown parameters and millions of data points. Many approaches would require calls to the 3D VRTE solver in proportion to the number unknown parameters or measurements. To avoid this issue of scale, we focus on computing the gradient of the misfit function as an alternative to the Jacobian of the measurement operator. The resulting adjoint method provides a way to adjust 3D atmosphere and surface properties with only two calls to the 3D VRTE solver for each spectral channel, regardless of the number retrieval parameters, measurement view angles or pixels. This gives a procedure for adjusting atmosphere and surface parameters that will scale to the large problems of 3D remote sensing. For certain types of multi-angle/multi-pixel polarimetric measurements, this encourages the development of a new class of three-dimensional retrieval algorithms with more flexible parametrizations of spatial heterogeneity, less reliance on data screening procedures, and improved coverage in terms of the resolved physical processes in the Earth's atmosphere. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Martin, William; Bal, Guillaume] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. [Cairns, Brian] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Martin, W (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. EM wgm2111@columbia.edu OI Cairns, Brian/0000-0002-1980-1022 FU NASA Head-quarters under the NASA Earth and Space Science Fellowship Program [NNX-10AN85H]; US National Science Foundation to Columbia University; Aerosol Cloud Ecosystem (ACE) mission by NASA Head-quarters; ACE program scientists Hal Mating and Paula Bontempi; NASA/ESTO's AIST program [1497551]; NSF [DMS-1108608] FX William Martin acknowledges support from NASA Head-quarters under the NASA Earth and Space Science Fellowship Program, Grant NNX-10AN85H, and he was partially funded by an IGERT grant from the US National Science Foundation to Columbia University Also, he is grateful to Alexander Kokhanovsky for organizing a workshop on aerosol remote sensing from space (July 15-19, 2013; International Space Sciences Institute, Bern, CH) and to Thomas Trautmann, Anthony Davis, and the other participants for encouragement and fruitful discussions. Brian Cairns would like to acknowledge support of the work presented here under pre-formulation funding of the Aerosol Cloud Ecosystem (ACE) mission by NASA Head-quarters and the ACE program scientists Hal Mating and Paula Bontempi. Guillaume Bal acknowledges support, through JPL Subcontract no. 1497551, from NASA/ESTO's AIST program (3D-TRACE project), and from the NSF under Grant DMS-1108608. NR 45 TC 5 Z9 5 U1 0 U2 10 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 SEP PY 2014 VL 144 BP 68 EP 85 DI 10.1016/j.jqsrt.2014.03.030 PG 18 WC Optics; Spectroscopy SC Optics; Spectroscopy GA AJ9AS UT WOS:000337999800006 ER PT J AU Majurec, N Johnson, JT Tanelli, S Durden, SL AF Majurec, Ninoslav Johnson, Joel T. Tanelli, Simone Durden, Stephen L. TI Comparison of Model Predictions With Measurements of Ku- and Ka-Band Near-Nadir Normalized Radar Cross Sections of the Sea Surface From the Genesis and Rapid Intensification Processes Experiment SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Airborne radar; doppler radar; meteorological radar; radar cross-sections; radar remote sensing; sea surface ID TRMM PRECIPITATION RADAR; SLOPE; WAVES; BACKSCATTER; SCATTERING; ALTIMETER; ROUGHNESS; SIGNALS AB A comparison of model predictions with measurements of near-nadir normalized radar cross sections (NRCSs) of the sea surface at Ku- and Ka-bands is reported. Measurements of Airborne Precipitation Radar Second Generation (APR-2) from near nadir to 25 degrees incidence angle, along with simultaneous wind truth from dropsonde observations, are compared with predictions of the "cutoff-invariant" two-scale model of sea scattering with the overall goal of assessing the model for possible future use in the APR-2 calibration process. The performance of the model as a function of wind speed and incidence angle is therefore emphasized. The measured data set, acquired primarily during the 2010 "Genesis and Rapid Intensification Processes" (GRIP) experiment, includes wind speeds from approximately 5 to 45 m/s. Model comparisons are limited by uncertainties in the wind fields due to limited dropsonde coverage; the data set is separated into "more reliable" (containing wind speeds of 5-20 m/s) and "less reliable" (wind speeds of 5-45 m/s) wind truth categories accordingly. Because a model of the sea spectrum is required for cutoff-invariant model predictions, comparisons with measured data are performed for three differing sea spectrum descriptions. It is found that a bias of less than similar to 1 dB over the wind speed range 5-40 m/s and a standard deviation less than 1 dB over the wind speed range 10-40 m/s can be achieved when using the "unified" sea spectrum description of Elfouhaily et al. The model also provides error levels that are near uniform with respect to both incidence angle and wind speed. C1 [Majurec, Ninoslav] Ohio State Univ, Dept Elect Engn & Comp, ElectroSci Lab, Columbus, OH 43212 USA. [Johnson, Joel T.] Ohio State Univ, Dept Elect & Comp Engn, ElectroSci Lab, Columbus, OH 43212 USA. [Tanelli, Simone; Durden, Stephen L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Majurec, N (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. FU NASA Precipitation Measurement Missions Program; National Aeronautics and Space Administration FX This work was performed in support to NASA Precipitation Measurement Missions Program, and it was made possible by the data acquired during the Genesis and Rapid Intensification Processes (GRIP) project. A portion of this work (S. L. Durden and S. Tanelli) was carried out at the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA, under a contract with the National Aeronautics and Space Administration. NR 25 TC 7 Z9 7 U1 1 U2 16 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2014 VL 52 IS 9 BP 5320 EP 5332 DI 10.1109/TGRS.2013.2288105 PG 13 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AI8MU UT WOS:000337171900005 ER PT J AU Paillou, P Sufyar, S Freeman, A AF Paillou, Philippe Sufyar, Sarah Freeman, Anthony TI The Chott El Djerid, Tunisia: Observation and Discussion of a SAR Phase Signature Over Evaporitic Soils SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Chott; El Djerid; integral equation model (IEM); phase; playa; polarimetry; synthetic aperture radar (SAR); Tunisia ID WET SUBSURFACE STRUCTURES; POLARIMETRIC L-BAND; SOUTHERN TUNISIA; DIELECTRIC-PROPERTIES; PLAYA; BACKSCATTERING; AVHRR AB The presence of water in arid regions is correlated to large evaporitic deposits, with high concentration of salts. Polarimetric synthetic aperture radar (SAR) observations over such areas show high variations for both the amplitude and phase of the backscattered copolarized signal. This is due to a large dynamic range for both surface roughness and dielectric constant parameters, between the wet and dry seasons: crystallized salt is rough and presents a low dielectric constant, whereas saline water corresponds to smooth and conductive surfaces. We observed a complete seasonal cycle over the chott El Djerid playa, in southern Tunisia, using the 5.6-GHz C-band polarimetric SAR on-board RADARSAT-2. One SAR image acquisition was performed every 24 days, from February to September 2009. In addition to expected variations in the radar backscattered power, we observed significant changes in the phase difference between horizontally and vertically polarized channels. In order to explain such a phase effect, we first considered the arguments of the Fresnel reflectivity coefficient when approaching the Brewster angle, for materials presenting a high loss tangent. A more complete analytical modeling derived from the integral equation model approach confirmed this hypothesis. C1 [Paillou, Philippe; Sufyar, Sarah] Univ Bordeaux, UMR 5804, LAB, F-33270 Floirac, France. [Sufyar, Sarah] Lab Integrat Mat Syst IMS, F-33607 Pessac, France. [Freeman, Anthony] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Paillou, P (reprint author), Univ Bordeaux, UMR 5804, LAB, F-33270 Floirac, France. EM paillou@obs.u-bordeaux1.fr FU French Space Agency (CNES); Programme National de Teledetection Spatiale (INSU) FX This work was supported in part by the French Space Agency (CNES) and in part by the Programme National de Teledetection Spatiale (INSU). NR 26 TC 0 Z9 0 U1 1 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2014 VL 52 IS 9 BP 5798 EP 5806 DI 10.1109/TGRS.2013.2292822 PG 9 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AI8MU UT WOS:000337171900047 ER PT J AU Jimenez-Munoz, JC Sobrino, JA Mattar, C Hulley, G Gottsche, FM AF Jimenez-Munoz, Juan C. Sobrino, Jose A. Mattar, Cristian Hulley, Glynn Goettsche, Frank-M. TI Temperature and Emissivity Separation From MSG/SEVIRI Data SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE MODIS; SEVIRI; surface emissivity; surface temperature; TES ID LAND-SURFACE TEMPERATURE; ASTER TEMPERATURE; ALGORITHM; PRODUCTS; VALIDATION; RETRIEVAL; SEA AB In this paper, we analyze the feasibility of applying the temperature and emissivity separation (TES) algorithm to thermal-infrared data acquired with three bands of the Spinning Enhanced Visible and Infrared Imager (SEVIRI) onboard the Meteosat Second Generation platform (SEVTES). The performance of the SEVTES algorithm was tested using data simulated over different atmospheric conditions and surface emissivities, with errors around 1.5% for emissivity and 1.5 K for temperature when atmospheric correction is accurate enough. In contrast, errors on land-leaving radiances higher than 2% or uncertainties on total atmospheric water vapor amount higher than 5% lead to errors on emissivity higher than 2% and errors on land surface temperature higher than 3 K, especially when the atmospheric absorption is overestimated. SEVIRI data acquired in August 2011 were also used to validate SEVTES emissivities against in situ measurements collected in five different homogeneous areas over Africa. Values were also intercompared to Moderate Resolution Imaging Spectroradiometer (MODIS)-derived and Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER)-derived emissivities and to the LSA SAF emissivity product. Results show that SEVTES-derived emissivity values are consistent with MODIS-TES and ASTER-TES retrievals and that SEVTES also improves the retrievals included in LSA SAF and MOD11Cx v5 products. When compared to laboratory measurements, accuracies of around 1%-2% were obtained, although occasional inaccuracies (2%-3%) were also found in some cases at band 8.7 mu m. The results presented in this paper show the potential SEVTES has for improving the LSA SAF product over arid and semiarid areas. C1 [Jimenez-Munoz, Juan C.; Sobrino, Jose A.] Univ Valencia, Image Proc Lab, Global Change Unit, Valencia 46071, Spain. [Mattar, Cristian] Univ Santiago, Dept Environm Sci & Renewable Nat Resources, Lab Anal Biosphere, Santiago 11315, Chile. [Hulley, Glynn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Goettsche, Frank-M.] Karlsruhe Inst Technol, D-76344 Eggenstein Leopoldshafen, Germany. RP Jimenez-Munoz, JC (reprint author), Univ Valencia, Image Proc Lab, Global Change Unit, Valencia 46071, Spain. EM jcjm@uv.es; sobrino@uv.es; cristian.mattar@uv.es; glynn.hulley@jpl.nasa.gov; frank.goettsche@kit.edu RI Sobrino, Jose/M-1585-2014; Mattar, Cristian/P-6711-2014; Gottsche, Frank-Michael/A-7362-2013; Jimenez-Munoz, Juan Carlos/K-2903-2015 OI Sobrino, Jose/0000-0003-3787-9373; Gottsche, Frank-Michael/0000-0001-5836-5430; Jimenez-Munoz, Juan Carlos/0000-0001-7562-4895 FU European Union (CEOP-AEGIS) [212921]; Ministerio de Economia y Competitividad (EODIX) [AYA2008-0595-C04-01]; Ministerio de Economia y Competitividad (CEOS-Spain) [AYA2011-29334-C02-01]; Universitat de Valencia [UV-INV-PRECOMP13-115366] FX This work was supported by the European Union (CEOP-AEGIS, project FP7-ENV-2007-1 Proposal No. 212921), the Ministerio de Economia y Competitividad (EODIX, project AYA2008-0595-C04-01; CEOS-Spain, project AYA2011-29334-C02-01), and the Universitat de Valencia (UV-INV-PRECOMP13-115366). NR 37 TC 11 Z9 11 U1 0 U2 19 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2014 VL 52 IS 9 BP 5937 EP 5951 DI 10.1109/TGRS.2013.2293791 PG 15 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AI8MU UT WOS:000337171900058 ER PT J AU Ouellette, JD Johnson, JT Kim, S van Zyl, JJ Moghaddam, M Spencer, MW Tsang, L Entekhabi, D AF Ouellette, Jeffrey D. Johnson, Joel T. Kim, Seungbum van Zyl, Jakob J. Moghaddam, Mahta Spencer, Michael W. Tsang, Leung Entekhabi, Dara TI A Simulation Study of Compact Polarimetry for Radar Retrieval of Soil Moisture SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Compact polarimetry; data cube; retrieval algorithm; soil moisture; time series AB A compact polarimetric (CP) radar system requires fewer measurements than a fully polarimetric (FP) system, thus allowing added flexibility in radar system design. Previous studies have shown the potential of using compact polarimetry for radar remote sensing of soil moisture. This paper extends previous studies by considering a time series data cube retrieval algorithm and measurements in the presence of vegetation. Vegetation information is assumed to be provided by an ancillary data source in the retrieval process. The performance of an algorithm for reconstructing FP information from CP measurements of vegetated soil surfaces is also examined. The results of the study show that only a modest degradation in soil moisture retrieval performance occurs when compact-pol measurements are used in place of full-pol data. C1 [Ouellette, Jeffrey D.; Johnson, Joel T.] Ohio State Univ, Columbus, OH 43210 USA. [Kim, Seungbum; van Zyl, Jakob J.; Spencer, Michael W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Moghaddam, Mahta] Univ So Calif, Los Angeles, CA 90089 USA. [Tsang, Leung] Univ Washington, Seattle, WA 98195 USA. [Entekhabi, Dara] MIT, Cambridge, MA 02139 USA. RP Ouellette, JD (reprint author), Ohio State Univ, Columbus, OH 43210 USA. EM ouellette.18@osu.edu; johnson@ece.osu.edu NR 15 TC 3 Z9 4 U1 1 U2 18 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2014 VL 52 IS 9 BP 5966 EP 5973 DI 10.1109/TGRS.2013.2294133 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 AI8MU UT WOS:000337171900060 ER PT J AU Stephens, E Schumann, G Bates, P AF Stephens, Elisabeth Schumann, Guy Bates, Paul TI Problems with binary pattern measures for flood model evaluation SO HYDROLOGICAL PROCESSES LA English DT Article DE remote sensing; flood modelling; performance measures; calibration; evaluation ID FINITE-VOLUME MODEL; RASTER-BASED MODEL; INUNDATION MODELS; CALIBRATION; UNCERTAINTY; RESOLUTION; EXTENT AB As the calibration and evaluation of flood inundation models are a prerequisite for their successful application, there is a clear need to ensure that the performance measures that quantify how well models match the available observations are fit for purpose. This paper evaluates the binary pattern performance measures that are frequently used to compare flood inundation models with observations of flood extent. This evaluation considers whether these measures are able to calibrate and evaluate model predictions in a credible and consistent way, i.e. identifying the underlying model behaviour for a number of different purposes such as comparing models of floods of different magnitudes or on different catchments. Through theoretical examples, it is shown that the binary pattern measures are not consistent for floods of different sizes, such that for the same vertical error in water level, a model of a flood of large magnitude appears to perform better than a model of a smaller magnitude flood. Further, the commonly used Critical Success Index (usually referred to as F-< 2 >) is biased in favour of overprediction of the flood extent, and is also biased towards correctly predicting areas of the domain with smaller topographic gradients. Consequently, it is recommended that future studies consider carefully the implications of reporting conclusions using these performance measures. Additionally, future research should consider whether a more robust and consistent analysis could be achieved by using elevation comparison methods instead. Copyright (C) 2013 John Wiley & Sons, Ltd. C1 [Stephens, Elisabeth; Schumann, Guy; Bates, Paul] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England. [Stephens, Elisabeth] Univ Oxford, Dept Phys, Oxford OX1 3PU, England. [Schumann, Guy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Stephens, E (reprint author), Univ Bristol, Sch Geog Sci, Univ Rd, Bristol BS8 1SS, Avon, England. EM stephens@atm.ox.ac.uk RI Bates, Paul/C-8026-2012; Schumann, Guy/F-9760-2011; OI Bates, Paul/0000-0001-9192-9963; Stephens, Elisabeth/0000-0002-5439-7563 FU European Union 'KULTURISK' project [FP7-ENV-2010-265280]; joint Great Western Research and Environment Agency studentship FX This work is supported by the European Union 'KULTURISK' project via grant FP7-ENV-2010-265280, and Elisabeth Stephens' time was also funded by a joint Great Western Research and Environment Agency studentship. NR 26 TC 8 Z9 8 U1 2 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0885-6087 EI 1099-1085 J9 HYDROL PROCESS JI Hydrol. Process. PD AUG 30 PY 2014 VL 28 IS 18 BP 4928 EP 4937 DI 10.1002/hyp.9979 PG 10 WC Water Resources SC Water Resources GA AN8YV UT WOS:000340893000008 ER PT J AU Kim, K Rim, T Park, C Kim, D Meyyappan, M Lee, JS AF Kim, Kihyun Rim, Taiuk Park, Chanoh Kim, Donghoon Meyyappan, M. Lee, Jeong-Soo TI Suspended honeycomb nanowire ISFETs for improved stiction-free performance SO NANOTECHNOLOGY LA English DT Article DE ion-sensitive field effect transistor; gate-all-around (GAA); honeycomb structure; stiction; pH sensing; top-down; suspended nanowire ID FIELD-EFFECT TRANSISTOR; BIOSENSORS; DNA; NANOSENSORS; ADSORPTION; ELECTRODE; DEVICES; SENSORS; PH AB This paper reports high performance ion-sensitive field-effect transistors (ISFETs) with a suspended honeycomb nanowire (SHNW) structure. The SHNW can provide a longer, stiction-free channel than that which is possible with a suspended straight nanowire (SSNW) for the realization of gate-all-around biosensors. Devices with SHNWs, SSNWs and conventional nanowires on the substrate have been fabricated using a top-down approach in order to compare their electrical performances. The SHNW devices exhibit excellent electrical characteristics such as lower subthreshold swing, higher transconductance and higher linear drain current. In addition, the SHNW ISFETs show better pH sensitivity than other ISFETs. Based on the results, the SHNW device appears promising for enhancing the intrinsic performance and ensuring the reliable operation of biosensor applications. C1 [Kim, Kihyun; Kim, Donghoon; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Dept Elect Engn, Pohang, South Korea. [Rim, Taiuk; Meyyappan, M.] Pohang Univ Sci & Technol POSTECH, Dept Creat IT Engn, Pohang, South Korea. [Rim, Taiuk; Meyyappan, M.] Pohang Univ Sci & Technol POSTECH, Future IT Innovat Lab, Pohang, South Korea. [Park, Chanoh; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang, South Korea. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kim, K (reprint author), Pohang Univ Sci & Technol POSTECH, Dept Elect Engn, Pohang, South Korea. EM ljs6951@postech.ac.kr FU National Research Foundation (NRF) [2013R1A1A2007094]; center for advanced soft electronics under the global frontier research program of the Ministry of Education, Science, and Technology (MEST) [2011-0031638]; 'IT Consilience Creative Program' [NIPA-2014-H0201-14-1001] FX This work was in part supported by the National Research Foundation (NRF) (No. 2013R1A1A2007094), by a grant (Code No. 2011-0031638) from the center for advanced soft electronics under the global frontier research program of the Ministry of Education, Science, and Technology (MEST) and by the 'IT Consilience Creative Program' (NIPA-2014-H0201-14-1001) supervised by the National IT Industry Promotion Agency, Korea. NR 32 TC 6 Z9 6 U1 2 U2 20 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0957-4484 EI 1361-6528 J9 NANOTECHNOLOGY JI Nanotechnology PD AUG 29 PY 2014 VL 25 IS 34 AR 345501 DI 10.1088/0957-4484/25/34/345501 PG 7 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA AP1DR UT WOS:000341807100013 PM 25091979 ER PT J AU Gershman, DJ Slavin, JA Raines, JM Zurbuchen, TH Anderson, BJ Korth, H Baker, DN Solomon, SC AF Gershman, Daniel J. Slavin, James A. Raines, Jim M. Zurbuchen, Thomas H. Anderson, Brian J. Korth, Haje Baker, Daniel N. Solomon, Sean C. TI Ion kinetic properties in Mercury's pre-midnight plasma sheet SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE mercury; plasma sheet; planetary ion ID MESSENGER OBSERVATIONS; PLANETARY IONS; MAGNETOSPHERE; MAGNETOMETER; DYNAMICS; MODEL; MAGNETOPAUSE; ENVIRONMENT; INSTRUMENT AB With data from the Fast Imaging Plasma Spectrometer sensor on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging spacecraft, we demonstrate that the average distributions for both solar wind and planetary ions in Mercury's pre-midnight plasma sheet are well-described by hot Maxwell-Boltzmann distributions. Temperatures and densities of the H+-dominated plasma sheet, in the ranges similar to 1-10cm(-3) and similar to 5-30MK, respectively, maintain thermal pressures of similar to 1nPa. The dominant planetary ion, Na+, has number densities about 10% that of H+. Solar wind ions retain near-solar-wind abundances with respect to H+ and exhibit mass-proportional ion temperatures, indicative of a reconnection-dominated heating in the magnetosphere. Conversely, planetary ion species are accelerated to similar average energies greater by a factor of similar to 1.5 than that of H+. This energization is suggestive of acceleration in an electric potential, consistent with the presence of a strong centrifugal acceleration process in Mercury's magnetosphere. C1 [Gershman, Daniel J.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Gershman, Daniel J.; Slavin, James A.; Raines, Jim M.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Baker, Daniel N.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA. RP Gershman, DJ (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. EM djgersh@umich.edu RI Slavin, James/H-3170-2012 OI Slavin, James/0000-0002-9206-724X FU NASA Discovery Program [NAS5-97271, NASW-00002]; Goddard Space Flight Center by NASA Postdoctoral Program FX The MESSENGER project is supported by the NASA Discovery Program under contracts NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. DJG is supported at Goddard Space Flight Center by an appointment to the NASA Postdoctoral Program administered by Oak Ridge Associated Universities. Data used in this study are available from the Planetary Data System. NR 31 TC 14 Z9 14 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 28 PY 2014 VL 41 IS 16 BP 5740 EP 5747 DI 10.1002/2014GL060468 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AQ4HT UT WOS:000342755400007 ER PT J AU Besserer, J Nimmo, F Wieczorek, MA Weber, RC Kiefer, WS McGovern, PJ Andrews-Hanna, JC Smith, DE Zuber, MT AF Besserer, Jonathan Nimmo, Francis Wieczorek, Mark A. Weber, Renee C. Kiefer, Walter S. McGovern, Patrick J. Andrews-Hanna, Jeffrey C. Smith, David E. Zuber, Maria T. TI GRAIL gravity constraints on the vertical and lateral density structure of the lunar crust SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Moon; Lunar crust; Density; Porosity; Admittance; Gravity ID SPECTRAL ESTIMATION; INTERNAL STRUCTURE; BASIN IMPACT; HEAT-FLOW; MOON; MISSION; SPHERE; INTERIOR; MEGAREGOLITH; ORBITER AB We analyzed data from the Gravity Recovery and Interior Laboratory (GRAIL) mission using a localized admittance approach to map out spatial variations in the vertical density structure of the lunar crust. Mare regions are characterized by a distinct decrease in density with depth, while the farside is characterized by an increase in density with depth at an average gradient of approximate to 35kgm(-3)km(-1) and typical surface porosities of at least 20%. The Apollo 12 and 14 landing site region has a similar density structure to the farside, permitting a comparison with seismic velocity profiles. The interior of the South Pole-Aitken (SP-A) impact basin appears distinct with a near-surface low-density (porous) layer 2-3 times thinner than the rest of the farside. This result suggests that redistribution of material during the large SP-A impact likely played a major role in sculpting the lunar crust. C1 [Besserer, Jonathan; Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Wieczorek, Mark A.] Univ Paris Diderot, Inst Phys Globe Paris, Sorbonne Paris Cite, Paris, France. [Weber, Renee C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Kiefer, Walter S.; McGovern, Patrick J.] Lunar & Planetary Inst, Ctr Lunar Sci & Explorat, Houston, TX 77058 USA. [Andrews-Hanna, Jeffrey C.] Colorado Sch Mines, Dept Geophys, Golden, CO 80401 USA. [Andrews-Hanna, Jeffrey C.] Colorado Sch Mines, Ctr Space Resources, Golden, CO 80401 USA. [Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. RP Besserer, J (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. EM jbessere@ucsc.edu RI Wieczorek, Mark/G-6427-2010; OI Wieczorek, Mark/0000-0001-7007-4222; McGovern, Patrick/0000-0001-9647-3096; Kiefer, Walter/0000-0001-6741-5460 FU NASA; NASA GRAIL Guest Scientist Program [NNX12AL08G] FX The GRAIL mission is supported by NASA's Discovery Program and is performed under contract to the Massachusetts Institute of Technology and the Jet Propulsion Laboratory, California Institute of Technology. We are grateful to the Editor, A. J. Dombard, and two anonymous reviewers for their great help in improving the initial version of the manuscript. J. B. and F.N. thank the NASA GRAIL Guest Scientist Program (grant NNX12AL08G), S. G. Mogilevskaya, B. Noyelles, S. Kamata, and T. Lay for fruitful discussions, and also J. M. Soderblom for comments on an earlier version of the manuscript. Data used to generate the results of this paper are available at http://pds-geosciences.wustl.edu and www.Ipgp.Fr/%7Ewieczor (see also Table S1). NR 50 TC 18 Z9 18 U1 1 U2 23 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 28 PY 2014 VL 41 IS 16 BP 5771 EP 5777 DI 10.1002/2014GL060240 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AQ4HT UT WOS:000342755400011 ER PT J AU Kliore, AJ Nagy, A Asmar, S Anabtawi, A Barbinis, E Fleischman, D Kahan, D Klose, J AF Kliore, Arvydas J. Nagy, Andrew Asmar, Sami Anabtawi, Aseel Barbinis, Elias Fleischman, Don Kahan, Danny Klose, John TI The ionosphere of Saturn as observed by the Cassini Radio Science System SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Saturn; ionosphere; Cassini; Radio Science ID ELECTRON-DENSITY; MODEL; OCCULTATION; ATMOSPHERE AB Fifty-nine ionsopheric radio occultation observations of the vertical electron density profile in the Saturn ionosphere have been made since the Cassini spacecraft was inserted in orbit around Saturn in 2004. Significant orbit to orbit variations were observed, but the general trend noted in earlier orbits, namely, increasing electron densities with increasing latitude was reconfirmed and bolstered with this extended data base. This trend is likely to be due to some combination of increasing ionization rates and decreasing water influx with latitude. C1 [Kliore, Arvydas J.; Asmar, Sami; Anabtawi, Aseel; Barbinis, Elias; Fleischman, Don; Kahan, Danny; Klose, John] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Nagy, Andrew] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Kliore, AJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM kliore@juno.com FU NASA; Cassini project FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, and the Department of Atmospheric, Oceanic, and Space Sciences, University of Michigan, under contracts from NASA. The authors thank the Cassini project for supporting the work presented in this paper. We also want to thank G. Bjoraker for providing us with yet unpublished information on water column contents derived from the Cassini CIRS observations. NR 13 TC 2 Z9 2 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 28 PY 2014 VL 41 IS 16 BP 5778 EP 5782 DI 10.1002/2014GL060512 PG 5 WC Geosciences, Multidisciplinary SC Geology GA AQ4HT UT WOS:000342755400012 ER PT J AU Han, SC Sauber, J Pollitz, F AF Han, Shin-Chan Sauber, Jeanne Pollitz, Fred TI Broadscale postseismic gravity change following the 2011 Tohoku-Oki earthquake and implication for deformation by viscoelastic relaxation and afterslip SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE postseismic gravity; viscoelastic relaxation; afterslip; GRACE; GPS ID SUMATRA-ANDAMAN EARTHQUAKE; LAYERED SPHERICAL EARTH; CRUSTAL DEFORMATION; SURFACE-WAVES; GRACE; SLIP; INVERSION; MODEL; ZONES AB The analysis of GRACE gravity data revealed postseismic gravity increase by 6 Gal over a 500 km scale within a couple of years after the 2011 Tohoku-Oki earthquake, which is nearly 40-50% of the coseismic gravity change. It originates mostly from changes in the isotropic component corresponding to the M-rr moment tensor element. The exponential decay with rapid change in a year and gradual change afterward is a characteristic temporal pattern. Both viscoelastic relaxation and afterslip models produce reasonable agreement with the GRACE free-air gravity observation, while their Bouguer gravity patterns and seafloor vertical deformations are distinctly different. The postseismic gravity variation is best modeled by the biviscous relaxation with a transient and steady state viscosity of 10(18) and 10(19)Pas, respectively, for the asthenosphere. Our calculated higher-resolution viscoelastic relaxation model, underlying the partially ruptured elastic lithosphere, yields the localized postseismic subsidence above the hypocenter reported from the GPS-acoustic seafloor surveying. C1 [Han, Shin-Chan; Sauber, Jeanne] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Pollitz, Fred] US Geol Survey, Menlo Pk, CA 94025 USA. RP Han, SC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. EM shin-chan.han@nasa.gov FU NASA's GRACE project; Earth Surface and Interior program FX This work was supported by NASA's GRACE project and Earth Surface and Interior program. We thank Riccardo Riva for sharing computer codes for the normal mode analysis, Roland Burgmann and Yan Hu for sharing their postseismic modeling and analysis, Faqi Diao for providing the finite fault models of afterslip, and an anonymous reviewer and M. Kogan for their constructive comments. The GRACE data for this paper are available at http://podaac.jpl.nasa.gov/GRACE. NR 39 TC 11 Z9 11 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 28 PY 2014 VL 41 IS 16 BP 5797 EP 5805 DI 10.1002/2014GL060905 PG 9 WC Geosciences, Multidisciplinary SC Geology GA AQ4HT UT WOS:000342755400015 ER PT J AU Castle, SL Thomas, BF Reager, JT Rodell, M Swenson, SC Famiglietti, JS AF Castle, Stephanie L. Thomas, Brian F. Reager, John T. Rodell, Matthew Swenson, Sean C. Famiglietti, James S. TI Groundwater depletion during drought threatens future water security of the Colorado River Basin SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Colorado River Basin; drought; GRACE; groundwater; water management; groundwater depletion ID UNITED-STATES; MODEL; HYDROLOGY; SYSTEM; GRACE AB Streamflow of the Colorado River Basin is the most overallocated in the world. Recent assessment indicates that demand for this renewable resource will soon outstrip supply, suggesting that limited groundwater reserves will play an increasingly important role in meeting future water needs. Here we analyze 9years (December 2004 to November 2013) of observations from the NASA Gravity Recovery and Climate Experiment mission and find that during this period of sustained drought, groundwater accounted for 50.1km(3) of the total 64.8km(3) of freshwater loss. The rapid rate of depletion of groundwater storage (-5.60.4km(3)yr(-1)) far exceeded the rate of depletion of Lake Powell and Lake Mead. Results indicate that groundwater may comprise a far greater fraction of Basin water use than previously recognized, in particular during drought, and that its disappearance may threaten the long-term ability to meet future allocations to the seven Basin states. C1 [Castle, Stephanie L.; Thomas, Brian F.; Reager, John T.; Famiglietti, James S.] Univ Calif Irvine, UC Ctr Hydrol Modeling, Irvine, CA 92697 USA. [Castle, Stephanie L.; Thomas, Brian F.; Reager, John T.; Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Thomas, Brian F.; Reager, John T.; Famiglietti, James S.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA USA. [Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Swenson, Sean C.] Natl Ctr Atmospher Res, Climate & Global Dynam Div, Boulder, CO 80307 USA. RP Famiglietti, JS (reprint author), Univ Calif Irvine, UC Ctr Hydrol Modeling, Irvine, CA 92697 USA. EM jfamigli@uci.edu RI Rodell, Matthew/E-4946-2012 OI Rodell, Matthew/0000-0003-0106-7437 FU NASA GRACE Science Team; University of California Office of the President, Multicampus Research Programs and Initiatives; NASA FX This research was funded by grants from the NASA GRACE Science Team and from the University of California Office of the President, Multicampus Research Programs and Initiatives. Jason Christensen of the U. S. Bureau of Reclamation provided the reservoir capacities and dam releases. We thank Q. Tang of the University of Washington for the use of the MODIS ET data and Min-Hui Lo of the National Taiwan University for the assistance with the GRACE validation. Access to all data sets used in this study is available through the links provided in the main text. Authors J.T. Reager and J.S. Famiglietti conducted some of this research at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 42 TC 59 Z9 60 U1 11 U2 65 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 28 PY 2014 VL 41 IS 16 BP 5904 EP 5911 DI 10.1002/2014GL061055 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AQ4HT UT WOS:000342755400029 ER PT J AU Bouman, J Fuchs, M Ivins, E van der Wal, W Schrama, E Visser, P Horwath, M AF Bouman, J. Fuchs, M. Ivins, E. van der Wal, W. Schrama, E. Visser, P. Horwath, M. TI Antarctic outlet glacier mass change resolved at basin scale from satellite gravity gradiometry SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE basin-scale ice mass change; Amundsen Sea Sector; Antarctica; satellite gravimetry ID ICE-SHEET; GRACE; FIELD; GOCE; GREENLAND; BALANCE; IMPACT; SHELF AB The orbit and instrumental measurement of the Gravity Field and Steady State Ocean Circulation Explorer (GOCE) satellite mission offer the highest ever resolution capabilities for mapping Earth's gravity field from space. However, past analysis predicted that GOCE would not detect changes in ice sheet mass. Here we demonstrate that GOCE gravity gradiometry observations can be combined with Gravity Recovery and Climate Experiment (GRACE) gravity data to estimate mass changes in the Amundsen Sea Sector. This refined resolution allows land ice changes within the Pine Island Glacier (PIG), Thwaites Glacier, and Getz Ice Shelf drainage systems to be measured at respectively -677, -6312, and -559 Gt/yr over the GOCE observing period of November 2009 to June 2012. This is the most accurate pure satellite gravimetry measurement to date of current mass loss from PIG, known as the weak underbelly of West Antarctica because of its retrograde bed slope and high potential for raising future sea level. C1 [Bouman, J.; Fuchs, M.] Deutsches Geodat Forschungsinst, Munich, Germany. [Ivins, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [van der Wal, W.; Schrama, E.; Visser, P.] Delft Univ Technol, Fac Aerosp Engn, Delft, Netherlands. [Horwath, M.] Tech Univ Munich, Inst Astron & Phys Geodasie, D-80290 Munich, Germany. RP Bouman, J (reprint author), Deutsches Geodat Forschungsinst, Munich, Germany. EM bouman@dgfi.badw.de RI Bouman, Johannes/C-3521-2015 FU European Space Agency as part of the Support to Science Element (STSE) FX This work was partially done in the context of the GOCE + Time-Variations study, which was supported by the European Space Agency as part of the Support to Science Element (STSE). All GOCE and GRACE products are freely available (e.g., http://podaac.jpl.nasa.gov/GRACE, http://icgem.gfz-potsdam.de, or http://earth.esa.int/goce). We thank Byron Tapley and Srinivas Bettadpur for providing the extended GRACE CSR RL05 solutions. NR 34 TC 7 Z9 8 U1 2 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 28 PY 2014 VL 41 IS 16 BP 5919 EP 5926 DI 10.1002/2014GL060637 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AQ4HT UT WOS:000342755400031 ER PT J AU Field, RD Kim, D LeGrande, AN Worden, J Kelley, M Schmidt, GA AF Field, Robert D. Kim, Daehyun LeGrande, Allegra N. Worden, John Kelley, Maxwell Schmidt, Gavin A. TI Evaluating climate model performance in the tropics with retrievals of water isotopic composition from Aura TES SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE climate models; convection; water isotopes; satellite retrievals; parameterizations; tropics ID GENERAL-CIRCULATION MODEL; BOUNDARY-LAYER; CONVECTION SCHEME; SENSITIVITY; HDO; PARAMETERIZATIONS; CONFIGURATION; SIMULATIONS; VARIABILITY; PROFILES AB We evaluate the NASA Goddard Institute for Space Studies ModelE2 general circulation model over the tropics against water isotope (HDO/H2O) retrievals from the Aura Tropospheric Emission Spectrometer. Observed isotopic distributions are distinct from other observable quantities and can therefore act as an independent constraint. We perform a small ensemble of simulations with physics perturbations to the cumulus and planetary boundary layer schemes. We examine the degree to which model-data agreement could be used to constrain a select group of internal processes in the model, namely, condensate evaporation, entrainment strength, and updraft mass flux. All are difficult to parameterize but exert strong influence over model performance. We find that the water isotope composition is more sensitive to physics changes than precipitation, temperature, or relative humidity in the lower and upper tropical tropospheres. Among the processes considered, this is most closely, and fairly exclusively, related to midtropospheric entrainment strength. Our study indicates that water isotope observations could provide useful constraints on model parameterizations. C1 [Field, Robert D.; LeGrande, Allegra N.; Kelley, Maxwell; Schmidt, Gavin A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Field, Robert D.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [Kim, Daehyun] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Worden, John] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Kelley, Maxwell] Trinnovim LLC, New York, NY USA. RP Field, RD (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM rf2426@columbia.edu RI Schmidt, Gavin/D-4427-2012 OI Schmidt, Gavin/0000-0002-2258-0486 FU NASA Postdoctoral Program; NASA [NNX13AK46G, NNX13AM18G]; Korea Meteorological Administration Research and Development Program [CATER 2013-3142]; National Aeronautics and Space Administration FX R.F. was supported by the NASA Postdoctoral Program and NASA grant NNX13AK46G and D. K. by NASA grant NNX13AM18G and the Korea Meteorological Administration Research and Development Program under grant CATER 2013-3142. 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. Resources supporting this work were provided by the NASA High-End Computing Program through the NASA Center for Climate Simulation at the Goddard Space Flight Center. All data used in the paper can be obtained from the authors. The authors thank three anonymous reviewers for their constructive comments. NR 45 TC 9 Z9 9 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 28 PY 2014 VL 41 IS 16 BP 6030 EP 6036 DI 10.1002/2014GL060572 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AQ4HT UT WOS:000342755400045 ER PT J AU Fortenberry, RC Huang, XC Crawford, TD Lee, TJ AF Fortenberry, Ryan C. Huang, Xinchuan Crawford, T. Daniel Lee, Timothy J. TI Quartic Force Field Rovibrational Analysis of Protonated Acetylene, C2H3+, and Its Isotopologues SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID FUNDAMENTAL VIBRATIONAL FREQUENCIES; SPECTROSCOPIC CONSTANTS; INFRARED-SPECTROSCOPY; WAVE-FUNCTIONS; LINEAR C3H3+; BASIS-SETS; ENERGIES; CYCLOPROPENYLIDENE; MOLECULES; HYDROGEN AB Protonated acetylene, C2H3+, is among the simplest carbocations. Comprehensive experimental or highly accurate computational spectroscopic data is lacking for this system due to its inherent complexities. Utilizing state-of-the-art quartic force fields (QFFs), the spectroscopic constants and fundamental vibrational frequencies are provided in this work for the nonclassical, bridged, cyclic global minimum. The rotational constants match experiment to better than 0.1%, and the computed nu(2) antisymmetric HCCH stretch is less than 3.0 cm(-1) different from experiment. Hence, the rovibrational spectroscopic data provided herein for c-C2H3+ and its deuterated isotopologues enrich the chemical understanding of this system. Unfortunately, the same rovibrational spectroscopic data is not as trustworthy for the classical, linear form of protonated acetylene due to the shallow well in which it resides on the potential energy surface. However, spectroscopic data are provided for this isomer in the Supporting Information to enhance future studies. C1 [Fortenberry, Ryan C.] Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA. [Fortenberry, Ryan C.; Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. [Crawford, T. Daniel] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA. [Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Fortenberry, RC (reprint author), Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA. EM rfortenberry@georgiasouthern.edu; Timothy.J.Lee@nasa.gov RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013; Crawford, Thomas/A-9271-2017 OI Crawford, Thomas/0000-0002-7961-7016 FU Georgia Southern University; NASA; National Science Foundation (NSF) [CHE-1058420]; NSF Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) Award [CHE-0741927]; NASA [12-APRA12-0107]; NASA/SETI Institute [NNX12AG96A]; NASA's Laboratory Astrophysics "Carbon in the Galaxy" Consortium Grant [NNH10ZDA001N] FX Georgia Southern University provided start-up funds, and the NASA Postdoctoral Program administered by Oak Ridge Associated Universities through a contract with NASA financially supported the work performed by R.C.F. T.D.C. was supported by National Science Foundation (NSF) Award CHE-1058420 and by NSF Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) Award CHE-0741927, which provided the employed computer hardware. T.J.L., R.C.F., and X.H. gratefully acknowledge funding from NASA Grant 12-APRA12-0107. X.H. was funded by NASA/SETI Institute Cooperative Agreement NNX12AG96A. Support from NASA's Laboratory Astrophysics "Carbon in the Galaxy" Consortium Grant (NNH10ZDA001N) is acknowledged by T.J.L., R.C.F., and X.H. The figures were created using the CheMVP program developed at the University of Georgia's Center for Computational Quantum Chemistry. NR 47 TC 22 Z9 22 U1 1 U2 10 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD AUG 28 PY 2014 VL 118 IS 34 BP 7034 EP 7043 DI 10.1021/jp506441g PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA AO2BR UT WOS:000341121000035 PM 25076406 ER PT J AU Li, JLF Forbes, RM Waliser, DE Stephens, G Lee, S AF Li, J. -L. F. Forbes, R. M. Waliser, D. E. Stephens, G. Lee, Seungwon TI Characterizing the radiative impacts of precipitating snow in the ECMWF Integrated Forecast System global model SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LARGE-SCALE MODELS; PARTICLE-SIZE DISTRIBUTIONS; CLIMATE MODELS; ACCURATE PARAMETERIZATION; MACROSCOPIC BEHAVIOR; ATMOSPHERE RADIATION; CLOUD-MICROPHYSICS; CUMULUS ENSEMBLES; CIRRUS CLOUDS; SENSITIVITY AB Global weather and climate models often exclude the effects of precipitating hydrometeors and convective core mass on radiative fluxes. In particular, many models split the ice phase into separate "cloud ice" and "snow" categories representing the smaller and larger ice particles, respectively; a separation that is generally not well defined in observations. A version of the European Centre for Medium-Range Weather Forecasts (ECMWF) global numerical weather prediction model which includes the radiative effects of cloud liquid, cloud ice, and precipitating snow is used to investigate the impact of including and excluding the radiative effects of the precipitating snow category. The results show that exclusion of precipitating snow in the radiation calculations leads to differences in the shortwave and longwave radiative fluxes of 5-15 Wm(-2) in strongly precipitating and convective areas. These differences are of the same order of magnitude as the systematic errors in the model compared to satellite observations. Corresponding biases in the radiative heating profiles are on the order of 0.15 K d(-1). The results imply that precipitating snow should be included in the radiative calculations in all weather and climate models in the context of improving model fidelity and reducing compensating errors. C1 [Li, J. -L. F.; Waliser, D. E.; Stephens, G.; Lee, Seungwon] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Forbes, R. M.] ECMWF, Reading, Berks, England. RP Li, JLF (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Juilin.F.Li@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology [NNH12ZDA001N ROSES 2012]; ATMOS COMP [NNH12ZDA001N-CCST] FX We thank Justin Stachnik and Terry Kubar at JPL for useful comments. The contributions by D. E. W., S. L., and J.L.L. to this study were carried out on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under contracts of NNH12ZDA001N ROSES 2012, Earth Science Program, the Modeling, Analysis, and Prediction (MAP) and ATMOS COMP 2013 (NNH12ZDA001N-CCST) with the National Aeronautics and Space Administration (NASA). The observations from the CloudSat radar (http://www.cloudsat.cira.colostate.edu/) and CERES Energy Balanced and Filled (CERES-EBAF) and corresponding surface flux radiation products constrained by TOA CERES-EBAF adjustments can be found at http://ceres.larc.nasa.gov/cmip5_data.php. NR 39 TC 5 Z9 5 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 27 PY 2014 VL 119 IS 16 BP 9626 EP 9637 DI 10.1002/2014JD021450 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AP3RF UT WOS:000341994000002 ER PT J AU Frith, SM Kramarova, NA Stolarski, RS McPeters, RD Bhartia, PK Labow, GJ AF Frith, S. M. Kramarova, N. A. Stolarski, R. S. McPeters, R. D. Bhartia, P. K. Labow, G. J. TI Recent changes in total column ozone based on the SBUV Version 8.6 Merged Ozone Data Set SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID QUASI-BIENNIAL OSCILLATION; ABSORPTION CROSS-SECTIONS; STRATOSPHERIC CHLORINE; UV SPECTROSCOPY; TEMPERATURE; TRENDS; CALIBRATION; INSTRUMENT; ALGORITHM; RECORD AB The Solar Backscatter Ultraviolet (SBUV) Merged Ozone Data Set (MOD) provides the longest available satellite-based time series of profile and total ozone from a single instrument type. The data span a 44 year period from 1970 to 2013 (except a 5 year gap in the 1970s). Data from nine independent SBUV-type instruments are included in the record, one of which is still operating. Although modifications in instrument design were made in the evolution from the Nimbus-4 Backscattered Ultraviolet instrument to the modern SBUV(/2) model, the basic principles of the measurement technique and retrieval algorithm remain the same, lending consistency to this record compared to those based on measurements using different instrument types. Nevertheless, each instrument has specific characteristics, and known anomalies must be incorporated in the MOD uncertainty estimates. In this study we describe the latest version of the MOD data set based on SBUV data processed using the Version 8.6 algorithm. We assess the measurement consistency across instruments and use this information to assign a drift uncertainty to the MOD. We then fit a multiple regression model to the MOD time series alternately using Equivalent Effective Stratospheric Chlorine (EESC) or linear trend fits over varying time series segments to analyze trends. Regression results indicate a statistically significant positive trend in total ozone outside the tropics based on the EESC proxy fit to the full record, but a linear trend fit to the last 13 years of data does not yield a statistically significant ozone increase. C1 [Frith, S. M.; Kramarova, N. A.; Labow, G. J.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Stolarski, R. S.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [McPeters, R. D.; Bhartia, P. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Frith, SM (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM stacey.m.frith@nasa.gov RI Stolarski, Richard/B-8499-2013; McPeters, Richard/G-4955-2013; Kramarova, Natalya/D-2270-2014 OI Stolarski, Richard/0000-0001-8722-4012; McPeters, Richard/0000-0002-8926-8462; Kramarova, Natalya/0000-0002-6083-8548 FU NASA [NNG12HP08C] FX The authors would like to acknowledge the SBUV instrument team members for their work producing the Version 8.6 SBUV data. SBUV Version 8.6 Level 2 and Level 3 data can be accessed from the "Instruments" tab on the MOD website at http://acdb-ext.gsfc.nasa.gov/Data_services/merged/index.html. Ground-based data are publicly available through the World Ozone and UV Data Center (WOUDC). The GTO merged ozone record used in this work was created within the framework of the ESA Climate Change Initiative program and is available from the ozone CCI website (http://www.esa-ozone-cci.org/). Data sources for proxies used in the regression analysis are provided in the text (Section 2.3). We also thank the three anonymous reviews for their comments and constructive improvements to this manuscript. S. M. Frith is supported under NASA Contract NNG12HP08C. NR 47 TC 18 Z9 22 U1 1 U2 19 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 27 PY 2014 VL 119 IS 16 BP 9735 EP 9751 DI 10.1002/2014JD021889 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AP3RF UT WOS:000341994000010 ER PT J AU Russell, PB Kacenelenbogen, M Livingston, JM Hasekamp, OP Burton, SP Schuster, GL Johnson, MS Knobelspiesse, KD Redemann, J Ramachandran, S Holben, B AF Russell, Philip B. Kacenelenbogen, Meloe Livingston, John M. Hasekamp, Otto P. Burton, Sharon P. Schuster, Gregory L. Johnson, Matthew S. Knobelspiesse, Kirk D. Redemann, Jens Ramachandran, S. Holben, Brent TI A multiparameter aerosol classification method and its application to retrievals from spaceborne polarimetry SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OPTICAL-PROPERTIES; CARBONACEOUS AEROSOLS; ABSORPTION PROPERTIES; LIDAR MEASUREMENTS; CENTRAL MEXICO; AERONET; INSTRUMENT; POLARIZATION; CLIMATOLOGY; INTENSITY AB Classifying observed aerosols into types (e. g., urban-industrial, biomass burning, mineral dust, maritime) helps to understand aerosol sources, transformations, effects, and feedback mechanisms; to improve accuracy of satellite retrievals; and to quantify aerosol radiative impacts on climate. The number of aerosol parameters retrieved from spaceborne sensors has been growing, from the initial aerosol optical depth (AOD) at one or a few wavelengths to a list that now includes AOD, complex refractive index, single scattering albedo (SSA), and depolarization of backscatter, each at several wavelengths, plus several particle size and shape parameters. Making optimal use of these varied data products requires objective, multidimensional analysis methods. We describe such a method, which makes explicit use of uncertainties in input parameters. It treats an N-parameter retrieved data point and its N-dimensional uncertainty as an extended data point, E. It then uses a modified Mahalanobis distance, D-EC, to assign an observation to the class (cluster) C that has minimum DEC from the point. We use parameters retrieved from the Aerosol Robotic Network (AERONET) to define seven prespecified clusters (pure dust, polluted dust, urban-industrial/developed economy, urban-industrial/developing economy, dark biomass smoke, light biomass smoke, and pure marine), and we demonstrate application of the method to a 5 year record of retrievals from the spaceborne Polarization and Directionality of the Earth's Reflectances 3 (POLDER 3) polarimeter over the island of Crete, Greece. Results show changes of aerosol type at this location in the eastern Mediterranean Sea, which is influenced by a wide variety of aerosol sources. C1 [Russell, Philip B.; Johnson, Matthew S.; Knobelspiesse, Kirk D.; Redemann, Jens] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kacenelenbogen, Meloe] Bay Area Environm Res Inst, Sonoma, CA USA. [Livingston, John M.] SRI Int, Menlo Pk, CA 94025 USA. [Hasekamp, Otto P.] SRON Netherlands Inst Space Res, Utrecht, Netherlands. [Burton, Sharon P.; Schuster, Gregory L.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Ramachandran, S.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. [Holben, Brent] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Russell, PB (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Philip.B.Russell@nasa.gov RI Knobelspiesse, Kirk/S-5902-2016 OI Knobelspiesse, Kirk/0000-0001-5986-1751 FU NASA Atmospheric Composition Modeling and Analysis Program (ACMAP); NASA Glory Science Team funding FX This research was supported by the NASA Atmospheric Composition Modeling and Analysis Program (ACMAP) and by NASA Glory Science Team funding. We appreciate the efforts of the AERONET principal investigators for obtaining, processing, documenting, and disseminating their respective data sets. The GEOS-5 data used in this study/project have been provided by the Global Modeling and Assimilation Office (GMAO) at NASA Goddard Space Flight Center. We appreciate the comments of three anonymous reviewers that have helped us to improve the paper. AERONET data used in this paper were obtained from http://aeronet.gsfc.nasa.gov/new_web/data.html. Relative humidity profiles were obtained from http://www-calipso.larc.nasa.gov/resources/calipso_users_guide/data_-sum maries/profile_data.php#relative_-humidity. POLDER data are available from Otto Hasekamp, SRON Netherlands Institute for Space Research, Utrecht, Netherlands, O.P. Hasekamp@sron.nl. NR 68 TC 17 Z9 17 U1 1 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 27 PY 2014 VL 119 IS 16 BP 9838 EP 9863 DI 10.1002/2013JD021411 PG 26 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AP3RF UT WOS:000341994000016 ER PT J AU Bi, JR Huang, JP Hu, ZY Holben, BN Guo, ZQ AF Bi, Jianrong Huang, Jianping Hu, Zhiyuan Holben, B. N. Guo, Zhiqiang TI Investigating the aerosol optical and radiative characteristics of heavy haze episodes in Beijing during January of 2013 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SKY RADIANCE MEASUREMENTS; AIR-POLLUTION; CHEMICAL-PROPERTIES; SOLAR IRRADIANCE; DUST AEROSOLS; CHINA; PM2.5; AERONET; CLIMATE; URBAN AB Several heavy atmospheric haze pollution episodes occurred over eastern and northern China during January of 2013. The pollution covered more than 100 km(2) and caused serious impacts on environmental quality, human health, and transportation. In this study, we characterize aerosol microphysical, optical, and radiative characteristics using a combination of ground-based Sun/sky radiometer retrievals and a radiative transfer model. Our results show that during about half of the total number of days, daily PM2.5 and PM10 concentrations are larger than 100 mu g/m(3), with maxima of 462 and 433 mu g/m(3), respectively, during the haze events. Fine-mode (PM2.5) particles dominated the aerosol size during the episodes. The volume size distribution and median radius of fine-mode particles generally increase as aerosol optical depth at 440 nm (AOD(440)) increases. The median effective radius of fine-mode particles increases from 0.15 mu m at low AOD value (AOD(440)similar to 0.3) to a radius of 0.25-0.30 mu m at high AOD value (AOD(440) >= 1.0). The daily mean single-scattering albedo (SSA), imaginary part of refractive index (RI), and asymmetry factor display pronounced spectral behaviors. The overall mean SSA(440) and SSA(675) are 0.892 and 0.905, respectively. The corresponding RI440 and RI675 are 0.016 and 0.011, respectively. This indicates that a significant amount of absorption occurred under the haze event in Beijing during January 2013. Approximately half of the incident solar radiation energy went into heating the atmosphere as a result of strong aerosol loading and absorption. The daily averaged heating rate in the haze particle layer (0-3.2 km) varies from 0.12 to 0.81 K/day in Beijing, which might exert profound impact on the atmospheric thermodynamic and dynamical structures and cloud development, which should be further studied. C1 [Bi, Jianrong; Huang, Jianping; Hu, Zhiyuan] Lanzhou Univ, Minist Educ, Key Lab Semiarid Climate Change, Lanzhou 730000, Peoples R China. [Bi, Jianrong; Huang, Jianping; Hu, Zhiyuan] Lanzhou Univ, Coll Atmospher Sci, Lanzhou 730000, Peoples R China. [Holben, B. N.] NASA, Biospher Sci Branch, GSFC, Greenbelt, MD USA. [Guo, Zhiqiang] Baoding City Bur Meteorol, Baoding, Peoples R China. RP Huang, JP (reprint author), Lanzhou Univ, Minist Educ, Key Lab Semiarid Climate Change, Lanzhou 730000, Peoples R China. EM hjp@lzu.edu.cn RI Xiongfei, Zhao/G-7690-2015 FU Lanzhou University through 985 Program; National Basic Research Program of China [2012CB955302, 2013CB955802]; National Science Foundation of China [41305025, 41175134]; Fundamental Research Funds for the Central Universities [lzujbky-2013-207, lzujbky-2013-ct05]; Developmental Program of Changjiang Scholarship and Research Team [IRT1018] FX SACOL was sponsored by Lanzhou University through 985 Program. This work was jointly supported by the National Basic Research Program of China (2012CB955302 and 2013CB955802), and National Science Foundation of China under grant 41305025 and 41175134. The Fundamental Research Funds for the Central Universities lzujbky-2013-207 and lzujbky-2013-ct05, and the Developmental Program of Changjiang Scholarship and Research Team (IRT1018). We thank the GSFC/NASA AERONET group for processing the AERONET data (http://aeronet.gsfc.nasa.gov). The authors would like to express special thanks to the principal investigators at Beijing-CAMS site (Huizheng Che, Chinese Academy of Meteorological Sciences, China Meteorological Administration), Beijing site (Hongbin Chen, Institute of Atmospheric Physics, Chinese Academy of Sciences), and Beijing_RADI site (Zhengqiang Li, Institute of Remote Sensing and Digital Earth of Chinese Academy of Sciences) together with their staff for establishing and maintaining the instruments. We are grateful to the Chinese Environmental Protection Bureau and the U. S. Embassy to provide the daily mean data of PM2.5 and PM10 concentrations in Beijing. We appreciate the MODIS and TOMS teams for supplying the satellite data. We would also like to thank all anonymous reviewers for their constructive and insightful comments. NR 60 TC 17 Z9 19 U1 3 U2 77 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 27 PY 2014 VL 119 IS 16 BP 9884 EP 9900 DI 10.1002/2014JD021757 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AP3RF UT WOS:000341994000018 ER PT J AU Lee, SS Feingold, G McComiskey, A Yamaguchi, T Koren, I Martins, JV Yu, HB AF Lee, Seoung Soo Feingold, Graham McComiskey, Allison Yamaguchi, Takanobu Koren, Ilan Martins, J. Vanderlei Yu, Hongbin TI Effect of gradients in biomass burning aerosol on shallow cumulus convective circulations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID BLACK CARBON AEROSOLS; BOUNDARY-LAYER; WRF MODEL; PART I; CLOUDS; SIMULATIONS; CLIMATE; AMAZON; SMOKE; SENSITIVITY AB This study examines the effect of spatial gradients in biomass burning (BB) aerosol on mesoscale circulations and clouds in the Amazon through high-resolution numerical modeling over areas of 30 km to 60 km. Inhomogeneous horizontal distribution of BB aerosol results in differential surface heat fluxes and radiative heating of the air, which generates circulation patterns that strongly influence cloud formation. The influence on air circulation and cumulus cloud formation depends on the BB aerosol loading, its vertical location, and the width of the plume. Plumes that reside at higher altitudes (similar to 1.5 km altitude) produce monotonic responses to aerosol loading whereas the response to plumes close to the surface changes nonmonotonically with plume width and aerosol loading. Sensitivity tests highlight the importance of interactive calculations of surface latent and heat fluxes with a coupled land surface model. In the case of the plume residing at higher altitude, failure to use interactive fluxes results in a reversal of the circulation whereas for the plume residing nearer the surface, the interactive surface model weakens the circulation. The influence of the BB aerosol on heating patterns, circulations, surface fluxes, and resultant cloud amount prevails over the BB aerosol-cloud microphysical influences. C1 [Lee, Seoung Soo; Feingold, Graham; McComiskey, Allison; Yamaguchi, Takanobu] NOAA, Chem Sci Div, Earth Syst Res Lab, Boulder, CO 80305 USA. [Lee, Seoung Soo; McComiskey, Allison; Yamaguchi, Takanobu] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Koren, Ilan] Weizmann Inst Sci, Dept Earth & Planetary Sci, IL-76100 Rehovot, Israel. [Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA. [Yu, Hongbin] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Yu, Hongbin] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA. RP Lee, SS (reprint author), NOAA, Chem Sci Div, Earth Syst Res Lab, Boulder, CO 80305 USA. EM cumulss@gmail.com RI Manager, CSD Publications/B-2789-2015; Feingold, Graham/B-6152-2009; Koren, Ilan/K-1417-2012; Yamaguchi, Takanobu/H-9169-2013; Yu, Hongbin/C-6485-2008 OI Koren, Ilan/0000-0001-6759-6265; Yamaguchi, Takanobu/0000-0001-8059-0757; Yu, Hongbin/0000-0003-4706-1575 FU NASA's IDS program; NOAA's Climate Goal Program FX The authors thank NASA's IDS program administered by Hal Maring and NOAA's Climate Goal Program for supporting this work. NOAA's HPCC is acknowledged for computing support. Data used in this study can be obtained by contacting Seoung Soo Lee (Seoung.Soo.Lee@noaa.gov). NR 44 TC 6 Z9 6 U1 3 U2 28 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 27 PY 2014 VL 119 IS 16 BP 9948 EP 9964 DI 10.1002/2014JD021819 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AP3RF UT WOS:000341994000022 ER PT J AU Cooper, M Martin, RV Wespes, C Coheur, PF Clerbaux, C Murray, LT AF Cooper, Matthew Martin, Randall V. Wespes, Catherine Coheur, Pierre-Francois Clerbaux, Cathy Murray, Lee T. TI Tropospheric nitric acid columns from the IASI satellite instrument interpreted with a chemical transport model: Implications for parameterizations of nitric oxide production by lightning SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID PACIFIC EXPLORATORY MISSION; ATMOSPHERIC-CHEMISTRY; OZONE PRODUCTION; NITROGEN-OXIDES; AIRBORNE MEASUREMENTS; TROPICAL PACIFIC; NOX PRODUCTION; GEOS-CHEM; DISTRIBUTIONS; EMISSIONS AB This paper interprets tropical tropospheric nitric acid columns from the Infrared Atmospheric Sounding Interferometer (IASI) satellite instrument with a global chemical transport model (GEOS-Chem). GEOS-Chemand IASI columns generally agree over the tropical ocean to within 10%. However, the GEOS-Chem simulation underestimates IASI nitric acid over Southeast Asia by a factor of 2. The regional nitric acid bias is confirmed by comparing the GEOS-Chem simulation with additional satellite (High Resolution Dynamics Limb Sounder, Atmospheric Chemistry Experiment Fourier Transform Spectrometer) and aircraft (Pacific Exploratory Mission (PEM)-Tropics A and PEM-West B) observations of the middle and upper troposphere. This bias appears to be driven by the lightning NOx parameterization, both in terms of the magnitude of the NOx source and the ozone production efficiency of concentrated lightning NOx plumes. We tested a subgrid lightning plume parameterization and found that an ozone production efficiency of 15 mol/mol in lightning plumes over Southeast Asia in conjunction with an additional 0.5 Tg N would reduce the regional nitric acid bias from 92% to 6% without perturbing the rest of the tropics. Other sensitivity studies such as modified NOx yield per flash, increased altitude of lightning NOx emissions, decreased convective mass flux, or increased scavenging of nitric acid required unrealistic changes to reduce the bias. C1 [Cooper, Matthew; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wespes, Catherine; Coheur, Pierre-Francois; Clerbaux, Cathy] Univ Libre Bruxelles, Brussels, Belgium. [Clerbaux, Cathy] Univ Paris 06, Sorbonne Univ, Paris, France. [Clerbaux, Cathy] Univ Versailles St Quentin, Paris, France. [Clerbaux, Cathy] LATMOS IPSL, CNRS INSU, Paris, France. [Murray, Lee T.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Murray, Lee T.] Columbia Univ, Lamont Doherty Earth Observ, New York, NY USA. RP Cooper, M (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. EM cooperm2@dal.ca RI Chem, GEOS/C-5595-2014; Murray, Lee/F-2296-2014; Martin, Randall/C-1205-2014; clerbaux, cathy/I-5478-2013 OI Murray, Lee/0000-0002-3447-3952; Martin, Randall/0000-0003-2632-8402; FU Natural Sciences and Engineering Research Council of Canada; Belgian State Federal Office for Scientific, Technical and Cultural Affairs; European Space Agency (ESA Prodex IASI.Flow); EUMETSAT (O3MSAF) FX IASI HNO3 data are available on request by contacting P.-F Coheur. IASI CO data were provided by LATMOS/CNRS and ULB and are available online at the Ether database at http://www.pole-ether.fr/. HIRDLS data products are available online at NASA's Goddard Earth Sciences Data and Information Services Center. ACE-FTS data are available on request by contacting the ACE Science Team at info@scisat.ca. Aircraft data from PEM West and PEM-Tropics campaigns are made available online at NASA's Global Tropospheric Experiment webpage at http://www-gte.larc.nasa.gov/gte_fld.htm. SHADOZ ozonesonde measurements are available online at http://croc.gsfc.nasa.gov/shadoz/. Information on accessing GEOS-Chem code can be found online at geos-chem.org. This work was supported by the Natural Sciences and Engineering Research Council of Canada. P.-F. Coheur and C. Wespes are, respectively, Senior Research Associate and Postdoctoral Researcher with F.R.S.-FNRS. The research in Belgium was also funded by the Belgian State Federal Office for Scientific, Technical and Cultural Affairs and the European Space Agency (ESA Prodex IASI.Flow), as well as by EUMETSAT (O3MSAF). NR 62 TC 5 Z9 5 U1 0 U2 27 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 27 PY 2014 VL 119 IS 16 BP 10068 EP 10079 DI 10.1002/2014JD021907 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AP3RF UT WOS:000341994000030 ER PT J AU Moriarty, JA Haskins, JB AF Moriarty, John A. Haskins, Justin B. TI Efficient wide-range calculation of free energies in solids and liquids using reversible-scaling molecular dynamics SO PHYSICAL REVIEW B LA English DT Article ID STRUCTURAL PHASE-STABILITY; EQUATION-OF-STATE; TRANSITION-METALS; INTERATOMIC POTENTIALS; HIGH-PRESSURE; ATOMISTIC SIMULATION; TANTALUM; MAGNESIUM; THERMODYNAMICS; ALUMINUM AB We elaborate a novel and efficient method to obtain multiphase Helmholtz free energies from molecular dynamics (MD) simulations over wide ranges of volume and temperature in materials that can be described by temperature-independent ion forces, with both higher accuracy and order-of-magnitude cost savings compared to direct thermodynamic-integration techniques. Our method leverages and significantly extends the technique of reversible-scaling molecular dynamics (RSMD) proposed by de Koning et al. [Phys. Rev. Lett. 83, 3973 (1999)], which allows a free-energy difference in a given phase at constant volume to be calculated as a function of temperature from a single MD simulation. In mechanically stable solid phases, our approach carefully combines quasiharmonic lattice dynamics at low temperatures with an accurate and fully isolated RSMD simulation of the anharmonic vibrational free energy at high temperatures to produce a seamless free energy from zero temperature to above melt along constant-volume isochores. In the liquid, we combine a unique calculation of the free energy along a high-temperature reference isotherm with isochoric RSMD simulations from that temperature to below melt. In metastable solid phases that are mechanically unstable at low temperature, we use two-phase MD melt simulations together with the liquid free energy to obtain the solid free energy along the solidus melt line and then perform isochoric RSMD simulations to temperatures above and below that point. While our free-energy method is general, we have specifically adapted it here to the case of metals in which the ion forces are well described by model generalized pseudopotential theory (MGPT) multi-ion interatomic potentials, and additive electron-thermal free-energy contributions can be included. Then using refined Ta6.8x MGPT potentials, we have converged total free energies and their components to very high and unprecedented sub-milli-Rydberg (mRy) numerical accuracy in the stable-bcc, liquid, and metastable-fcc phases of tantalum for volumes ranging from up to 26% expansion to nearly twofold compression and for temperatures to 25 000 K. In turn, we have successfully used the free energies so obtained to calculate physically accurate thermodynamic properties and gain new insight into their behavior, including sensitive thermodynamic derivatives, bcc and fcc melt curves, and a multiphase equation of state for tantalum (Ta) over the same temperature range and for pressures as high as 600 GPa. We show that the anharmonic free-energy component in the bcc solid, although only 1-5 mRy in magnitude for Ta, can have a significant (15%-20%) effect on thermal expansivity, the Gruneisen parameter, and melt temperatures. We further show that the electron-thermal free-energy component can similarly impact the specific heat and thermal expansivity in both the solid and the liquid, while only minimally affecting (to <= 3%) the bcc and fcc melt curves. C1 [Moriarty, John A.] Lawrence Livermore Natl Lab, Condensed Matter & Mat Div, Livermore, CA 94551 USA. [Haskins, Justin B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Moriarty, JA (reprint author), Lawrence Livermore Natl Lab, Condensed Matter & Mat Div, Livermore, CA 94551 USA. FU U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; DOE SciDAC [DE-FC02-06ER25788] FX This work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract No. DE-AC52-07NA27344. J.B.H. acknowledges support as a summer student at LLNL in 2011 from DOE SciDAC Grant No. DE-FC02-06ER25788, during which time some of this work was begun. NR 59 TC 2 Z9 2 U1 2 U2 23 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 EI 1550-235X J9 PHYS REV B JI Phys. Rev. B PD AUG 22 PY 2014 VL 90 IS 5 AR 054113 DI 10.1103/PhysRevB.90.054113 PG 19 WC Physics, Condensed Matter SC Physics GA AO3NI UT WOS:000341237600002 ER PT J AU Stecker, FW Scully, ST AF Stecker, Floyd W. Scully, Sean T. TI Propagation of superluminal PeV IceCube neutrinos: A high energy spectral cutoff or new constraints on Lorentz invariance violation SO PHYSICAL REVIEW D LA English DT Article ID GAMMA-RAYS; RADIATION; GALAXIES AB The IceCube observation of cosmic neutrinos with E-nu > 60 TeV, most of which are likely of extragalactic origin, allows one to severely constrain Lorentz invariance violation (LIV) in the neutrino sector, allowing for the possible existence of superluminal neutrinos. The subsequent neutrino energy loss by vacuum e(+)e(-) pair emission (VPE) is strongly dependent on the strength of LIV. In this paper we explore the physics and cosmology of superluminal neutrino propagation. We consider a conservative scenario for the redshift distribution of neutrino sources. Then by propagating a generic neutrino spectrum, using Monte Carlo techniques to take account of energy losses from both VPE and redshifting, we obtain the best present constraints on LIV parameters involving neutrinos. We find that delta(nu e) = delta(nu) - delta(e) <= 5.2 x 10(-21). Taking delta(e) <= 5 x 10(-21), we then obtain an upper limit on the superluminal velocity fraction for neutrinos alone of 1.0 x 10(-21). Interestingly, by taking delta(nu e) = 5.2 x 10(-21), we obtain a cutoff in the predicted neutrino spectrum above 2 PeV that is consistent with the lack of observed neutrinos at those energies, and particularly at the Glashow resonance energy of 6.3 PeV. Thus, such a cutoff could be the result of neutrinos being slightly superluminal, with delta(nu) being (0.5 to 1.0) x 10(-20). C1 [Stecker, Floyd W.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Scully, Sean T.] James Madison Univ, Dept Phys, Harrisonburg, VA 22807 USA. RP Stecker, FW (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. EM Floyd.W.Stecker@nasa.gov NR 39 TC 14 Z9 14 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD AUG 22 PY 2014 VL 90 IS 4 AR 043012 DI 10.1103/PhysRevD.90.043012 PG 5 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AO3OZ UT WOS:000341243600002 ER PT J AU Aasi, J Abbott, BP Abbott, R Abbott, T Abernathy, MR Accadia, T Acernese, F Ackley, K Adams, C Adams, T Addesso, P Adhikari, RX Affeldt, C Agathos, M Aggarwal, N Aguiar, OD Ain, A Ajith, P Alemic, A Allen, B Allocca, A Amariutei, D Andersen, M Anderson, R Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, C Areeda, J Aston, SM Astone, P Aufmuth, P Aulbert, C Austin, L Aylott, BE Babak, S Baker, PT Ballardin, G Ballmer, SW Barayoga, JC Barbet, M Barish, BC Barker, D Barone, F Barr, B Barsotti, L Barsuglia, M Barton, MA Bartos, I Bassiri, R Basti, A Batch, JC Bauchrowitz, J Bauer, TS Behnke, B Bejger, M Beker, MG Belczynski, C Bell, AS Bell, C Bergmann, G Bersanetti, D Bertolini, A Betzwieser, J Beyersdorf, PT Bilenko, IA Billingsley, G Birch, J Biscans, S Bitossi, M Bizouard, MA Black, E Blackburn, JK Blackburn, L Blair, D Bloemen, S Blom, M Bock, O Bodiya, TP Boer, M Bogaert, G Bogan, C Bond, C Bondu, F Bonelli, L Bonnand, R Bork, R Born, M Borkowski, K Boschi, V Bose, S Bosi, L Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brau, JE Briant, T Bridges, DO Brillet, A Brinkmann, M Brisson, V Brooks, AF Brown, DA Brown, DD Bruckner, F Buchman, S Bulik, T Bulten, HJ Buonanno, A Burman, R Buskulic, D Buy, C Cadonati, L Cagnoli, G Bustillo, JC Calloni, E Camp, JB Campsie, P Cannon, KC Canuel, B Cao, J Capano, CD Carbognani, F Carbone, L Caride, S Castiglia, A Caudill, S Cavalier, F Cavalieri, R Celerier, C Cella, G Cepeda, C Cesarini, E Chakraborty, R Chalermsongsak, T Chamberlin, SJ Chao, S Charlton, P Mottin, EC Chen, X Chen, Y Chincarini, A Chiummo, A Cho, HS Chow, J Christensen, N Chu, Q Chua, SSY Chung, S Ciani, G Clara, F Clark, JA Cleva, F Coccia, E Cohadon, PF Colla, A Collette, C Colombini, M Cominsky, L Conte, A Cook, D Corbitt, TR Cordier, M Cornish, N Corpuz, A Corsi, A Costa, CA Coughlin, MW Coughlin, S Coulon, JP Countryman, S Couvares, P Coward, DM Cowart, M Coyne, DC Coyne, R Craig, K Creighton, JDE Crowder, SG Cumming, A Cunningham, L Cuoco, E Dahl, K Dal Canton, T Damjanic, M Danilishin, SL D'Antonio, S Danzmann, K Dattilo, V Daveloza, H Davier, M Davies, GS Daw, EJ Day, R Dayanga, T Debreczeni, G Degallaix, J Deleglise, S Del Pozzo, W Denker, T Dent, T Dereli, H Dergachev, V De Rosa, R DeRosa, RT DeSalvo, R Dhurandhar, S Diaz, M Di Fiore, L Di Lieto, A Di Palma, I Di Virgilio, A Donath, A Donovan, F Dooley, KL Doravari, S Dorosh, O Dossa, S Douglas, R Downes, TP Drago, M Drever, RWP Driggers, JC Du, Z Dwyer, S Eberle, T Edo, T Edwards, M Effler, A Eggenstein, H Ehrens, P Eichholz, J Eikenberry, SS Endroczi, G Essick, R Etzel, T Evans, M Evans, T Factourovich, M Fafone, V Fairhurst, S Fang, Q Farinon, S Farr, B Farr, WM Favata, M Fehrmann, H Fejer, MM Feldbaum, D Feroz, F Ferrante, I Ferrini, F Fidecaro, F Finn, LS Fiori, I Fisher, RP Flaminio, R Fournier, JD Franco, S Frasca, S Frasconi, F Frede, M Frei, Z Freise, A Frey, R Fricke, TT Fritschel, P Frolov, VV Fulda, P Fyffe, M Gair, J Gammaitoni, L Gaonkar, S Garufi, F Gehrels, N Gemme, G Genin, E Gennai, A Ghosh, S Giaime, JA Giardina, KD Giazotto, A Gill, C Gleason, J Goetz, E Goetz, R Gondan, L Gonzalez, G Gordon, N Gorodetsky, ML Gossan, S Gossler, S Gouaty, R Graf, C Graff, PB Granata, M Grant, A Gras, S Gray, C Greenhalgh, RJS Gretarsson, AM Groot, P Grote, H Grover, K Grunewald, S Guidi, GM Guido, C Gushwa, K Gustafson, EK Gustafson, R Hammer, D Hammond, G Hanke, M Hanks, J Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Hart, M Hartman, MT Haster, CJ Haughian, K Heidmann, A Heintze, M Heitmann, H Hello, P Hemming, G Hendry, M Heng, IS Heptonstall, AW Heurs, M Hewitson, M Hild, S Hoak, D Hodge, KA Holt, K Hooper, S Hopkins, P Hosken, DJ Hough, J Howell, EJ Hu, Y Huerta, E Hughey, B Husa, S Huttner, SH Huynh, M Dinh, TH Ingram, DR Inta, R Isogai, T Ivanov, A Iyer, BR Izumi, K Jacobson, M James, E Jang, H Jaranowski, P Ji, Y Forteza, FJ Johnson, WW Jones, DI Jones, R Jonker, RJG Ju, L Haris, K Kalmus, P Kalogera, V Kandhasamy, S Kang, G Kanner, JB Karlen, J Kasprzack, M Katsavounidis, E Katzman, W Kaufer, H Kawabe, K Kawazoe, F Kefelian, F Keiser, GM Keitel, D Kelley, DB Kells, W Khalaidovski, A Khalili, FY Khazanov, EA Kim, C Kim, K Kim, N Kim, NG Kim, YM King, EJ King, PJ Kinzel, DL Kissel, JS Klimenko, S Kline, J Koehlenbeck, S Kokeyama, K Kondrashov, V Koranda, S Korth, WZ Kowalska, I Kozak, DB Kremin, A Kringel, V Krishnan, B Krolak, A Kuehn, G Kumar, A Kumar, P Kumar, R Kuo, L Kutynia, A Kwee, P Landry, M Lantz, B Larson, S Lasky, PD Lawrie, C Lazzarini, A Lazzaro, C Leaci, P Leavey, S Lebigot, EO Lee, CH Lee, HK Lee, HM Lee, J Leonardi, M Leong, JR Le Roux, A Leroy, N Letendre, N Levin, Y Levine, B Lewis, J Li, TGF Libbrecht, K Libson, A Lin, AC Littenberg, TB Litvine, V Lockerbie, NA Lockett, V Lodhia, D Loew, K Logue, J Lombardi, AL Lorenzini, M Loriette, V Lormand, M Losurdo, G Lough, J Lubinski, MJ Luck, H Luijten, E Lundgren, AP Lynch, R Ma, Y Macarthur, J Macdonald, EP MacDonald, T Machenschalk, B Maclnnis, M Macleod, DM Sandoval, FM Mageswaran, M Maglione, C Mailand, K Majorana, E Maksimovic, I Malvezzi, V Man, N Manca, GM Mandel, I Mandic, V Mangano, V Mangini, N Mantovani, M Marchesoni, F Marion, F Marka, S Marka, Z Markosyan, A Maros, E Marque, J Martelli, F Martin, IW Martin, RM Martinelli, L Martynov, D Marx, JN Mason, K Masserot, A Massinger, TJ Matichard, F Matone, L Matzner, RA Mavalvala, N Mazumder, N Mazzolo, G McCarthy, R McClelland, DE McGuire, SC McIntyre, G McIver, J Mclin, K Meacher, D Meadors, GD Mehmet, M Meidam, J Meinders, M Melatos, A Mendell, G Mercer, RA Meshkov, S Messenger, C Meyers, P Miao, H Michel, C Mikhailov, EE Milano, L Milde, S Miller, J Minenkov, Y Mingarelli, CMF Mishra, C Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Moe, B Moesta, P Mohan, M Mohapatra, SRP Moraru, D Moreno, G Morgado, N Morriss, SR Mossavi, K Mours, B Lowry, CMM Mueller, CL Mueller, G Mukherjee, S Mullavey, A Munch, J Murphy, D Murray, PG Mytidis, A Nagy, MF Kumar, DN Nardecchia, I Naticchioni, L Nayak, RK Necula, V Nelemans, G Neri, I Neri, M Newton, G Nguyen, T Nitz, A Nocera, F Nolting, D Normandin, MEN Nuttall, LK Ochsner, E O'Dell, J Oelker, E Oh, JJ Oh, SH Ohme, F Oppermann, P O'Reilly, B O'Shaughnessy, R Osthelder, C Ottaway, DJ Ottens, RS Overmier, H Owen, BJ Padilla, C Pai, A Palashov, O Palomba, C Pan, H Pan, Y Pankow, C Paoletti, F Paoletti, R Papa, MA Paris, H Pasqualetti, A Passaquieti, R Passuello, D Pedraza, M Penn, S Perreca, A Phelps, M Pichot, M Pickenpack, M Piergiovanni, F Pierro, V Pietka, M Pinard, L Pinto, IM Pitkin, M Poeld, J Poggiani, R Poteomkin, A Powell, J Prasad, J Premachandra, S Prestegard, T Price, LR Prijatelj, M Privitera, S Prodi, GA Prokhorov, L Puncken, O Punturo, M Puppo, P Qin, J Quetschke, V Quintero, E Quiroga, G James, RQ Raab, FJ Rabeling, DS Racz, I Radkins, H Raffai, P Raja, S Rajalakshmi, G Rakhmanov, M Ramet, C Ramirez, K Rapagnani, P Raymond, V Re, V Read, J Reed, CM Regimbau, T Reid, S Reitze, DH Rhoades, E Ricci, F Riles, K Robertson, NA Robinet, F Rocchi, A Rodruck, M Rolland, L Rollins, JG Romano, R Romanov, G Romie, JH Rosinska, D Rowan, S Rudiger, A Ruggi, P Ryan, K Salemi, F Sammut, L Sandberg, V Sanders, JR Sannibale, V Prieto, IS Saracco, E Sassolas, B Sathyaprakash, BS Saulson, PR Savage, R Scheuer, J Schilling, R Schnabel, R Schofield, RMS Schreiber, E Schuette, D Schutz, BF Scott, J Scott, SM Sellers, D Sengupta, AS Sentenac, D Sequino, V Sergeev, A Shaddock, D Shah, S Shahriar, MS Shaltev, M Shapiro, B Shawhan, P Shoemaker, DH Sidery, TL Siellez, K Siemens, X Sigg, D Simakov, D Singer, A Singer, L Singh, R Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, M Smith, RJE Lefebvre, NDS Son, EJ Sorazu, B Souradeep, T Sperandio, L Staley, A Stebbins, J Steinlechner, J Steinlechner, S Stephens, BC Steplewski, S Stevenson, S Stone, R Stops, D Strain, KA Straniero, N Strigin, S Sturani, R Stuver, AL Summerscales, TZ Susmithan, S Sutton, PJ Swinkels, B Tacca, M Talukder, D Tanner, DB Tarabrin, SP Taylor, R ter Braack, APM Thirugnanasambandam, MP Thomas, M Thomas, P Thorne, KA Thorne, KS Thrane, E Tiwari, V Tokmakov, KV Tomlinson, C Toncelli, A Tonelli, M Torre, O Torres, CV Torrie, CI Travasso, F Traylor, G Tse, M Ugolini, D Unnikrishnan, CS Urban, AL Urbanek, K Vahlbruch, H Vajente, G Valdes, G Vallisneri, M vanden Brand, JFJ VanDen Broeck, C vander Putten, S vander Sluys, MV van Heijningen, J van Veggel, AA Vass, S Vasuth, M Vaulin, R Vecchio, A Vedovato, G Veitch, J Veitch, PJ Venkateswara, K Verkindt, D Verma, SS Vetrano, F Vicere, A Finley, RV Vinet, JY Vitale, S Vo, T Vocca, H Vorvick, C Vousden, WD Vyachanin, SP Wade, A Wade, L Wade, M Walker, M Wallace, L Wang, M Wang, X Ward, RL Was, M Weaver, B Wei, LW Weinert, M Weinstein, AJ Weiss, R Welborn, T Wen, L Wessels, P West, M Westphal, T Wette, K Whelan, JT White, DJ Whiting, BF Wiesner, K Wilkinson, C Williams, K Williams, L Williams, R Williams, T Williamson, AR Willis, JL Willke, B Wimmer, M Winker, W Wipf, CC Wiseman, AG Wittel, H Woan, G Worden, J Yablon, J Yakushin, I Yamamoto, H Yancey, CC Yang, H Yang, Z Yoshida, S Yvert, M Zadrozny, A Zanolin, M Zendri, JP Zhang, F Zhang, L Zhao, C Zhu, XJ Zucker, ME Zuraw, S Zweizig, J AF Aasi, J. Abbott, B. P. Abbott, R. Abbott, T. Abernathy, M. R. Accadia, T. Acernese, F. Ackley, K. Adams, C. Adams, T. Addesso, P. Adhikari, R. X. Affeldt, C. Agathos, M. Aggarwal, N. Aguiar, O. D. Ain, A. Ajith, P. Alemic, A. Allen, B. Allocca, A. Amariutei, D. Andersen, M. Anderson, R. Anderson, S. B. Anderson, W. G. Arai, K. Araya, M. C. Arceneaux, C. Areeda, J. Aston, S. M. Astone, P. Aufmuth, P. Aulbert, C. Austin, L. Aylott, B. E. Babak, S. Baker, P. T. Ballardin, G. Ballmer, S. W. Barayoga, J. C. Barbet, M. Barish, B. C. Barker, D. Barone, F. Barr, B. Barsotti, L. Barsuglia, M. Barton, M. A. Bartos, I. Bassiri, R. Basti, A. Batch, J. C. Bauchrowitz, J. Bauer, Th S. Behnke, B. Bejger, M. Beker, M. G. Belczynski, C. Bell, A. S. Bell, C. Bergmann, G. Bersanetti, D. Bertolini, A. Betzwieser, J. Beyersdorf, P. T. Bilenko, I. A. Billingsley, G. Birch, J. Biscans, S. Bitossi, M. Bizouard, M. A. Black, E. Blackburn, J. K. Blackburn, L. Blair, D. Bloemen, S. Blom, M. Bock, O. Bodiya, T. P. 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TI Implementation of an F-statistic all-sky search for continuous gravitational waves in Virgo VSR1 data SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article DE gravitational waves; gravitational radiation detectors; pulsars; data analysis: algorithms and implementation ID RADIATION AB We present an implementation of the F-statistic to carry out the first search in data from the Virgo laser interferometric gravitational wave detector for periodic gravitational waves from a priori unknown, isolated rotating neutron stars. We searched a frequency f(0) range from 100 Hz to 1 kHz and the frequency dependent spindown f(1) range from -1.6(f(0)/100 Hz) x 10(-9) Hz s(-1) to zero. A large part of this frequency-spindown space was unexplored by any of the all-sky searches published so far. Our method consisted of a coherent search over two-day periods using the F-statistic, followed by a search for coincidences among the candidates from the two-day segments. We have introduced a number of novel techniques and algorithms that allow the use of the fast Fourier transform (FFT) algorithm in the coherent part of the search resulting in a fifty-fold speed-up in computation of the F-statistic with respect to the algorithm used in the other pipelines. No significant gravitational wave signal was found. The sensitivity of the search was estimated by injecting signals into the data. In the most sensitive parts of the detector band more than 90% of signals would have been detected with dimensionless gravitational-wave amplitude greater than 5 x 10(-24). C1 [Aasi, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Anderson, R.; Anderson, S. B.; Arai, K.; Araya, M. C.; Austin, L.; Barayoga, J. C.; Barish, B. C.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chakraborty, R.; Chalermsongsak, T.; Coyne, D. C.; Dergachev, V.; Drever, R. W. P.; Driggers, J. 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RI Aggarwal, Nancy/M-7203-2015; Shaddock, Daniel/A-7534-2011; Vicere, Andrea/J-1742-2012; Rocchi, Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Gehring, Tobias/A-8596-2016; Strain, Kenneth/D-5236-2011; Howell, Eric/H-5072-2014; Heidmann, Antoine/G-4295-2016; Nelemans, Gijs/D-3177-2012; Marchesoni, Fabio/A-1920-2008; Zhu, Xingjiang/E-1501-2016; M, Manjunath/N-4000-2014; Vecchio, Alberto/F-8310-2015; Strigin, Sergey/I-8337-2012; Leonardi, Matteo/G-9694-2015; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Bell, Angus/E-7312-2011; Ottaway, David/J-5908-2015; Garufi, Fabio/K-3263-2015; Deleglise, Samuel/B-1599-2015; Neri, Igor/F-1482-2010; Steinlechner, Sebastian/D-5781-2013; Khalili, Farit/D-8113-2012; Gorodetsky, Michael/C-5938-2008; McClelland, David/E-6765-2010; Hild, Stefan/A-3864-2010; Gammaitoni, Luca/B-5375-2009; Gemme, Gianluca/C-7233-2008; Iyer, Bala R./E-2894-2012; prodi, giovanni/B-4398-2010; 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Marchesoni, Fabio/0000-0001-9240-6793; Zhu, Xingjiang/0000-0001-7049-6468; M, Manjunath/0000-0001-8710-0730; Vecchio, Alberto/0000-0002-6254-1617; Sigg, Daniel/0000-0003-4606-6526; Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603; Bell, Angus/0000-0003-1523-0821; Garufi, Fabio/0000-0003-1391-6168; Deleglise, Samuel/0000-0002-8680-5170; Neri, Igor/0000-0002-9047-9822; Steinlechner, Sebastian/0000-0003-4710-8548; Gorodetsky, Michael/0000-0002-5159-2742; McClelland, David/0000-0001-6210-5842; Gammaitoni, Luca/0000-0002-4972-7062; Gemme, Gianluca/0000-0002-1127-7406; Iyer, Bala R./0000-0002-4141-5179; prodi, giovanni/0000-0001-5256-915X; Danilishin, Stefan/0000-0001-7758-7493; Lee, Chang-Hwan/0000-0003-3221-1171; Frasconi, Franco/0000-0003-4204-6587; Groot, Paul/0000-0002-4488-726X; Lazzaro, Claudia/0000-0001-5993-3372; Ferrante, Isidoro/0000-0002-0083-7228; Losurdo, Giovanni/0000-0003-0452-746X; Travasso, Flavio/0000-0002-4653-6156; Punturo, Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Ward, Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; Vedovato, Gabriele/0000-0001-7226-1320; Fairhurst, Stephen/0000-0001-8480-1961; Matichard, Fabrice/0000-0001-8982-8418; Husa, Sascha/0000-0002-0445-1971; Vocca, Helios/0000-0002-1200-3917; Farr, Ben/0000-0002-2916-9200; Collette, Christophe/0000-0002-4430-3703; Coccia, Eugenio/0000-0002-6669-5787; Vetrano, Flavio/0000-0002-7523-4296; Addesso, Paolo/0000-0003-0895-184X; Naticchioni, Luca/0000-0003-2918-0730; calloni, enrico/0000-0003-4819-3297; Bondu, Francois/0000-0001-6487-5197; Zweizig, John/0000-0002-1521-3397; Del Pozzo, Walter/0000-0003-3978-2030; O'Shaughnessy, Richard/0000-0001-5832-8517; Granata, Massimo/0000-0003-3275-1186; Kanner, Jonah/0000-0001-8115-0577; Freise, Andreas/0000-0001-6586-9901; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Ricci, Fulvio/0000-0001-5475-4447; Boschi, Valerio/0000-0001-8665-2293; Pinto, Innocenzo M./0000-0002-2679-4457; Guidi, Gianluca/0000-0002-3061-9870; Pierro, Vincenzo/0000-0002-6020-5521; Scott, Jamie/0000-0001-6701-6515; Sorazu, Borja/0000-0002-6178-3198 FU United States National Science Foundation; Science and Technology Facilities Council of the United Kingdom; Max-Planck-Society; State of Niedersachsen/Germany; Australian Research Council; International Science Linkages program of the Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Foundation for Fundamental Research; Netherlands Organisation; Polish Ministry of Science and Higher Education; FOCUS Programme of Foundation for Polish Science; PL-Grid Infrastructure; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P Sloan Foundation FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the PL-Grid Infrastructure, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P Sloan Foundation. This document has been assigned LIGO Laboratory document number LIGO-P1300133. NR 23 TC 11 Z9 11 U1 4 U2 47 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD AUG 21 PY 2014 VL 31 IS 16 AR 165014 DI 10.1088/0264-9381/31/16/165014 PG 27 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AO5XX UT WOS:000341421600014 ER PT J AU Steffen, W Teodoro, M Madura, TI Groh, JH Gull, TR Mehner, A Corcoran, MF Damineli, A Hamaguchi, K AF Steffen, W. Teodoro, M. Madura, T. I. Groh, J. H. Gull, T. R. Mehner, A. Corcoran, M. F. Damineli, A. Hamaguchi, K. TI The three-dimensional structure of the Eta Carinae Homunculus SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; circumstellar matter; stars: individual: Eta Carinae; stars: mass-loss; stars: winds; outflows ID HUBBLE-SPACE-TELESCOPE; LUMINOUS BLUE VARIABLES; PLANETARY-NEBULAE; COLLIDING WINDS; STELLAR WINDS; MASS-LOSS; INFRARED MORPHOLOGY; PERIASTRON PASSAGE; EDDINGTON LIMIT; LIGHT-CURVE AB We investigate, using the modelling code shape, the three-dimensional structure of the bipolar Homunculus nebula surrounding Eta Carinae as mapped by new ESO Very Large Telescope/X-Shooter observations of the H-2 lambda = 2.121 25 mu m emission line. Our results reveal for the first time important deviations from the axisymmetric bipolar morphology: (1) circumpolar trenches in each lobe positioned point symmetrically from the centre and (2) off-planar protrusions in the equatorial region from each lobe at longitudinal (similar to 55A degrees) and latitudinal (10A degrees-20A degrees) distances from the projected apastron direction of the binary orbit. The angular distance between the protrusions (similar to 110A degrees) is similar to the angular extent of each polar trench (similar to 130A degrees) and nearly equal to the opening angle of the wind-wind collision cavity (similar to 110A degrees). As in previous studies, we confirm a hole near the centre of each polar lobe and no detectable near-IR H-2 emission from the thin optical skirt seen prominently in visible imagery. We conclude that the interaction between the outflows and/or radiation from the central binary stars and their orientation in space has had, and possibly still has, a strong influence on the Homunculus. This implies that prevailing theoretical models of the Homunculus are incomplete as most assume a single-star origin that produces an axisymmetric nebula. We discuss how the newly found features might be related to the Homunculus ejection, the central binary, and the interacting stellar winds. C1 [Steffen, W.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. [Teodoro, M.; Madura, T. I.; Gull, T. R.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Groh, J. H.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [Mehner, A.] ESO, Vitacura, Santiago De Chi, Chile. [Corcoran, M. F.; Hamaguchi, K.] NASA, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Corcoran, M. F.; Hamaguchi, K.] NASA, Xray Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21046 USA. [Damineli, A.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508900 Sao Paulo, Brazil. [Hamaguchi, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. RP Steffen, W (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 106, Ensenada 22800, Baja California, Mexico. EM wsteffen@astro.unam.mx RI Damineli, Augusto/P-8829-2016 OI Damineli, Augusto/0000-0002-7978-2994 FU UNAM-PAPIIT [IN101014]; CNPq/MCT-Brazil [201978/2012-1]; NASA Postdoctoral Program at the Goddard Space Flight Center; Swiss National Science Foundation; FAPESP FX WS acknowledges financial support through grant UNAM-PAPIIT IN101014. MT is supported by CNPq/MCT-Brazil through grant 201978/2012-1. TIM is supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. JHG is supported by an Ambizione fellowship of the Swiss National Science Foundation. AD acknowledges FAPESP for continuous financial support. The authors thank D. Clark for useful discussions. NR 96 TC 9 Z9 9 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 21 PY 2014 VL 442 IS 4 BP 3316 EP 3328 DI 10.1093/mnras/stu1088 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5TZ UT WOS:000339924900042 ER PT J AU Buckley, MR Zavala, J Cyr-Racine, FY Sigurdson, K Vogelsberger, M AF Buckley, Matthew R. Zavala, Jesus Cyr-Racine, Francis-Yan Sigurdson, Kris Vogelsberger, Mark TI Scattering, damping, and acoustic oscillations: Simulating the structure of dark matter halos with relativistic force carriers SO PHYSICAL REVIEW D LA English DT Article ID DWARF SPHEROIDAL GALAXIES; LARGE-SCALE STRUCTURE; LYMAN-ALPHA FOREST; POWER SPECTRUM; LAMBDA-CDM; MILLICHARGED PARTICLES; BARYONS MATTER; MASS FUNCTION; MIRROR WORLD; SUBSTRUCTURE AB We demonstrate that self-interacting dark matter models with interactions mediated by light particles can have significant deviations in the matter power spectrum and detailed structure of galactic halos when compared to a standard cold dark matter scenario. While these deviations can take the form of suppression of small-scale structure that are in some ways similar to that of warm dark matter, the self-interacting models have a much wider range of possible phenomenology. A long-range force in the dark matter can introduce multiple scales to the initial power spectrum, in the form of dark acoustic oscillations and an exponential cutoff in the power spectrum. Using simulations we show that the impact of these scales can remain observationally relevant up to the present day. Furthermore, the self-interaction can continue to modify the small-scale structure of the dark matter halos, reducing their central densities and creating a dark matter core. The resulting phenomenology is unique to these type of models. C1 [Buckley, Matthew R.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Zavala, Jesus] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Cyr-Racine, Francis-Yan] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [Cyr-Racine, Francis-Yan] CALTECH, Pasadena, CA 91125 USA. [Sigurdson, Kris] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Vogelsberger, Mark] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Buckley, MR (reprint author), Rutgers State Univ, Dept Phys & Astron, POB 849, Piscataway, NJ 08854 USA. OI Buckley, Matthew/0000-0003-1109-3460; Cyr-Racine, Francis-Yan/0000-0002-7939-2988 FU National Science Foundation [1066293]; W. M. Keck Foundation; National Aeronautics and Space Administration; National Science and Engineering Research Council (NSERC) of Canada Discovery Grant; DNRF; EU under a Marie Curie International Incoming Fellowship [PIIF-GA-2013-627723] FX M. R. B. would like to thank Alyson Brooks for useful discussion and comments. M. R. B. and J. Z. thank the Aspen Center for Physics, where the initial conversations that led to their interest in this project were held. The Aspen Center for Physics is supported by the National Science Foundation under Grant No. 1066293. The work of F. Y. C. R. was performed in part at the California Institute of Technology for the Keck Institute for Space Studies, which is funded by the W. M. Keck Foundation. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The research of K. S. is supported in part by a National Science and Engineering Research Council (NSERC) of Canada Discovery Grant. The Dark Cosmology Centre is funded by the DNRF. J. Z. is supported by the EU under a Marie Curie International Incoming Fellowship, Contract No. PIIF-GA-2013-627723. The simulations in this paper were carried out on the Gardar supercomputer supported by the Nordic High Performance Computing (NHPC). NR 158 TC 36 Z9 36 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD AUG 20 PY 2014 VL 90 IS 4 AR 043524 DI 10.1103/PhysRevD.90.043524 PG 21 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AT2SH UT WOS:000344785100005 ER PT J AU Latvakoski, H Mlynczak, MG Cageao, RP Johnson, DG Kratz, DP AF Latvakoski, Harri Mlynczak, Martin G. Cageao, Richard P. Johnson, David G. Kratz, David P. TI Far-infrared spectroscopy of the troposphere: calibration with a cold background SO APPLIED OPTICS LA English DT Article ID PERFORMANCE; INSTRUMENT AB The far-infrared spectroscopy of the troposphere (FIRST) instrument is a Fourier-transform spectrometer developed to measure the Earth's thermal emission spectrum with a particular emphasis on the far-infrared. FIRST has observed the atmosphere from both the ground looking up and from a high-altitude balloon looking down. A recent absolute laboratory calibration of FIRST under ground-like operating conditions showed accuracy to better than 0.3 K at near-ambient temperatures (270-325 K) but reduced accuracy at lower temperatures. This paper presents calibration results for balloon-flight conditions using a cold blackbody to simulate the space view used for on-board calibration. An unusual detector nonlinearity was discovered and corrected, and stray light was measured and removed. Over most of the range of Earth scene temperatures (205-300 K), the accuracy of FIRST is 0.35-0.15 K (one sigma). (C) 2014 Optical Society of America C1 [Latvakoski, Harri] Space Dynam Lab, North Logan, UT 84341 USA. [Mlynczak, Martin G.; Kratz, David P.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Cageao, Richard P.; Johnson, David G.] NASA, Langley Res Ctr, Engn Directorate, Hampton, VA 23681 USA. RP Mlynczak, MG (reprint author), NASA, Langley Res Ctr, Sci Directorate, Mail Stop 420, Hampton, VA 23681 USA. EM m.g.mlynczak@nasa.gov RI Johnson, David/F-2376-2015; Richards, Amber/K-8203-2015 OI Johnson, David/0000-0003-4399-5653; NR 13 TC 1 Z9 1 U1 0 U2 5 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD AUG 20 PY 2014 VL 53 IS 24 BP 5425 EP 5433 DI 10.1364/AO.53.005425 PG 9 WC Optics SC Optics GA AN8BE UT WOS:000340825000026 PM 25321115 ER PT J AU Arevalo, P Bauer, FE Puccetti, S Walton, DJ Koss, M Boggs, SE Brandt, WN Brightman, M Christensen, FE Comastri, A Craig, WW Fuerst, F Gandhi, P Grefenstette, BW Hailey, CJ Harrison, FA Luo, B Madejski, G Madsen, KK Marinucci, A Matt, G Saez, C Stern, D Stuhlinger, M Treister, E Urry, CM Zhang, WW AF Arevalo, P. Bauer, F. E. Puccetti, S. Walton, D. J. Koss, M. Boggs, S. E. Brandt, W. N. Brightman, M. Christensen, F. E. Comastri, A. Craig, W. W. Fuerst, F. Gandhi, P. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Luo, B. Madejski, G. Madsen, K. K. Marinucci, A. Matt, G. Saez, C. Stern, D. Stuhlinger, M. Treister, E. Urry, C. M. Zhang, W. W. TI THE 2-79 keV X-RAY SPECTRUM OF THE CIRCINUS GALAXY WITH NuSTAR, XMM-Newton, AND CHANDRA: A FULLY COMPTON-THICK ACTIVE GALACTIC NUCLEUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Circinus); galaxies: Seyfert; X-rays: galaxies ID STAR-FORMATION RATE; SEYFERT-GALAXIES; NEARBY SEYFERT; RATE INDICATOR; LINE REGION; BEPPOSAX; VIEW; SPECTROSCOPY; ACCRETION; AGN AB The Circinus galaxy is one of the closest obscured active galactic nuclei (AGNs), making it an ideal target for detailed study. Combining archival Chandra and XMM-Newton data with new NuSTAR observations, we model the 2-79 keV spectrum to constrain the primary AGN continuum and to derive physical parameters for the obscuring material. Chandra's high angular resolution allows a separation of nuclear and off-nuclear galactic emission. In the off-nuclear diffuse emission, we find signatures of strong cold reflection, including high equivalent-width neutral Fe lines. This Compton-scattered off-nuclear emission amounts to 18% of the nuclear flux in the Fe line region, but becomes comparable to the nuclear emission above 30 keV. The new analysis no longer supports a prominent transmitted AGN component in the observed band. We find that the nuclear spectrum is consistent with Compton scattering by an optically thick torus, where the intrinsic spectrum is a power law of photon index Gamma = 2.2-2.4, the torus has an equatorial column density of N-H = (6-10) x 10(24) cm(-2), and the intrinsic AGN 2-10 keV luminosity is (2.3-5.1) x10(42) erg s(-1). These values place Circinus along the same relations as unobscured AGNs in accretion rate versus Gamma and L-X versus L-IR phase space. NuSTAR's high sensitivity and low background allow us to study the short timescale variability of Circinus at X-ray energies above 10 keV for the first time. The lack of detected variability favors a Compton-thick absorber, in line with the spectral fitting results. C1 [Arevalo, P.; Bauer, F. E.; Saez, C.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile. [Bauer, F. E.] Millennium Inst Astrophys, Boulder, CO 80301 USA. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Puccetti, S.] ASDC, ASI, I-00133 Rome, Italy. [Puccetti, S.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. [Walton, D. J.; Fuerst, F.; Grefenstette, B. W.; Harrison, F. A.; Madsen, K. K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Koss, M.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brightman, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Christensen, F. E.] Danish Tech Univ, Lyngby, Denmark. [Comastri, A.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hailey, C. J.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Madejski, G.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Marinucci, A.; Matt, G.] Univ Roma Tre, Dipartimento Matemat Fis, I-00146 Rome, Italy. [Saez, C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Stuhlinger, M.] ESAC, E-28691 Madrid, Spain. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Urry, C. M.] Yale Univ, Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Arevalo, P (reprint author), Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. RI Boggs, Steven/E-4170-2015; Koss, Michael/B-1585-2015; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; OI Boggs, Steven/0000-0001-9567-4224; Koss, Michael/0000-0002-7998-9581; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Puccetti, Simonetta/0000-0002-2734-7835; Urry, Meg/0000-0002-0745-9792 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; Basal-CATA [PFB-06/2007]; CONICYT-Chile FONDECYT [1140304, 1141218, 1120061, Anillo ACT1101]; ASI-INAF grant [I/037/12/0]; Caltech NuSTAR subcontract [44A-1092750]; NASA ADP grant [NNX10AC99G]; Swiss National Science Foundation [PP00P2_138979/1]; STFC [ST/J003697/1] FX We thank the anonymous referee for a thorough review and many useful suggestions that improved this paper. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We acknowledge financial support from Basal-CATA PFB-06/2007 (FEB), CONICYT-Chile FONDECYT 1140304 (PA), 1141218 (FEB), 1120061 (ET), and Anillo ACT1101 (PA, FEB, ET). A. C., A. M., and G. M. acknowledge the ASI-INAF grant I/037/12/0. W.N.B. and B. L. acknowledge support from Caltech NuSTAR subcontract 44A-1092750 and NASA ADP grant NNX10AC99G. M. K. gratefully acknowledges support from Swiss National Science Foundation Grant PP00P2_138979/1. P. G. thanks STFC for support (grant reference ST/J003697/1). NR 67 TC 38 Z9 38 U1 2 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2014 VL 791 IS 2 AR 81 DI 10.1088/0004-637X/791/2/81 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400008 ER PT J AU Bodenheimer, P Lissauer, JJ AF Bodenheimer, Peter Lissauer, Jack J. TI ACCRETION AND EVOLUTION OF similar to 2.5 M-circle plus PLANETS WITH VOLUMINOUS H/He ENVELOPES SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: formation; planets and satellites: individual (Kepler-11 f); planets and satellites: physical evolution ID IN-SITU FORMATION; GIANT PLANETS; SUPER-EARTHS; PROTOPLANETARY ATMOSPHERES; THERMAL EVOLUTION; KEPLER PLANETS; LOW-MASS; MODELS; PLANETESIMALS; OPACITIES AB Formation of planets in the Neptune size range with low-mass, but voluminous, H-2/He gaseous envelopes is modeled by detailed numerical simulations according to the core-nucleated accretion scenario. Formation locations ranging from 0.5 to 4 AU from a star of 1 M-circle dot are considered. The final planets have heavy-element cores of 2.2-2.5 M-circle plus and envelopes in the range 0.037-0.16 M-circle plus. After the formation process, which lasts 2 Myr or less, the planets evolve at constant mass up to an age of several Gyr. For assumed equilibrium temperatures of 250, 500, and 1000 K, their calculated final radii are compared with those observed by the Kepler spacecraft. For the particular case of Kepler-11 f, we address the question whether it could have formed in situ or whether migration from a formation location farther out in the disk is required. C1 [Bodenheimer, Peter] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Lissauer, Jack J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP Bodenheimer, P (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. EM peter@ucolick.org; Jack.J.Lissauer@nasa.gov OI Bodenheimer, Peter/0000-0001-6093-3097 FU NASA Origins of Solar Systems Program grant [NNX11AK54G]; NSF [AST0908807] FX Primary funding for this project was provided by the NASA Origins of Solar Systems Program grant NNX11AK54G (P.B. and J.L.). P.B. acknowledges additional support from NSF grant AST0908807. NR 40 TC 18 Z9 18 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2014 VL 791 IS 2 AR 103 DI 10.1088/0004-637X/791/2/103 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400030 ER PT J AU Bostrom, A Reynolds, CS Tombesi, F AF Bostrom, Allison Reynolds, Christopher S. Tombesi, Francesco TI AN XMM-NEWTON VIEW OF THE RADIO GALAXY 3C 411 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: active; galaxies: jets; galaxies: individual (3C411); X-rays: galaxies ID ULTRA-FAST OUTFLOWS; SHELL ABSORPTION-LINES; ACTIVE GALACTIC NUCLEI; BL LACERTAE OBJECTS; X-RAY; BLACK-HOLE; SEYFERT-GALAXIES; QUIET AGNS; SPECTRA; BLAZARS AB We present the first high signal-to-noise XMM-Newton observations of the broad-line radio galaxy 3C 411. After fitting various spectral models, an absorbed double power-law (PL) continuum and a blurred relativistic disk reflection model (kdblur) are found to be equally plausible descriptions of the data. While the softer PL component (Gamma = 2.11) of the double PL model is entirely consistent with that found in Seyfert galaxies (and hence likely originates from a disk corona), the additional PL component is very hard (Gamma = 1.05); amongst the active galactic nucleus zoo, only flat-spectrum radio quasars (FSRQ) have such hard spectra. Together with the flat radio-spectrum displayed by this source, we suggest that it should instead be classified as an FSRQ. This leads to potential discrepancies regarding the jet inclination angle, with the radio morphology suggesting a large jet inclination but the FSRQ classification suggesting small inclinations. The kdblur model predicts an inner disk radius of at most 20 r(g) and relativistic reflection. C1 [Bostrom, Allison; Reynolds, Christopher S.; Tombesi, Francesco] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Reynolds, Christopher S.] Joint Space Sci Inst JSI, College Pk, MD 20742 USA. [Reynolds, Christopher S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bostrom, A (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. FU NASA [NNX12AE13G] FX We thank David Ballantyne for interesting and fruitful discussions. C. S. R. thanks NASA for support under the ADAP program (grant NNX12AE13G). NR 42 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2014 VL 791 IS 2 AR 119 DI 10.1088/0004-637X/791/2/119 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400046 ER PT J AU Dawson, RI Johnson, JA Fabrycky, DC Foreman-Mackey, D Murray-Clay, RA Buchhave, LA Cargile, PA Clubb, KI Fulton, BJ Hebb, L Howard, AW Huber, D Shporer, A Valenti, JA AF Dawson, Rebekah I. Johnson, John Asher Fabrycky, Daniel C. Foreman-Mackey, Daniel Murray-Clay, Ruth A. Buchhave, Lars A. Cargile, Phillip A. Clubb, Kelsey I. Fulton, Benjamin J. Hebb, Leslie Howard, Andrew W. Huber, Daniel Shporer, Avi Valenti, Jeff A. TI LARGE ECCENTRICITY, LOW MUTUAL INCLINATION: THE THREE-DIMENSIONAL ARCHITECTURE OF A HIERARCHICAL SYSTEM OF GIANT PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems ID TRANSIT TIMING VARIATIONS; CANDIDATE HOST STARS; CLOSE-IN PLANETS; HOT JUPITERS; LIGHT CURVES; DYNAMICAL INSTABILITIES; ORBITAL EVOLUTION; ERROR-CORRECTION; V-ANDROMEDAE; STELLAR SPIN AB We establish the three-dimensional architecture of the Kepler-419 (previously KOI-1474) system to be eccentric yet with a low mutual inclination. Kepler-419b is a warm Jupiter at semi-major axis a = 0.370(-0.006)(+0.007) AU with a large eccentricity (e = 0.85(-0.07)(+0.08)) measured via the "photoeccentric effect." It exhibits transit timing variations (TTVs) induced by the non-transiting Kepler-419c, which we uniquely constrain to be a moderately eccentric (e = 0.184 +/- 0.002), hierarchically separated (a = 1.68 +/- 0.03 AU) giant planet (7.3 +/- 0.4 M-Jup). We combine 16 quarters of Kepler photometry, radial-velocity (RV) measurements from the HIgh Resolution Echelle Spectrometer on Keck, and improved stellar parameters that we derive from spectroscopy and asteroseismology. From the RVs, we measure the mass of the inner planet to be 2.5 +/- 0.3 M-Jup and confirm its photometrically measured eccentricity, refining the value to e = 0.83 +/- 0.01. The RV acceleration is consistent with the properties of the outer planet derived from TTVs. We find that despite their sizable eccentricities, the planets are coplanar to within 9(-6)(+8) degrees, and therefore the inner planet's large eccentricity and close-in orbit are unlikely to be the result of Kozai migration. Moreover, even over many secular cycles, the inner planet's periapse is most likely never small enough for tidal circularization. Finally, we present and measure a transit time and impact parameter from four simultaneous ground-based light curves from 1 m class telescopes, demonstrating the feasibility of ground-based follow-up of Kepler giant planets exhibiting large TTVs. C1 [Dawson, Rebekah I.; Clubb, Kelsey I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Johnson, John Asher; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60664 USA. [Foreman-Mackey, Daniel] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Cargile, Phillip A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Fulton, Benjamin J.; Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Hebb, Leslie] Hobart & William Smith Coll, Dept Phys, Geneva, NY 14456 USA. [Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA. [Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Valenti, Jeff A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Dawson, RI (reprint author), Univ Calif Berkeley, Dept Astron, Hearst Field Annex B-20, Berkeley, CA 94720 USA. EM rdawson@berkeley.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Buchhave, Lars A./0000-0003-1605-5666; Fabrycky, Daniel/0000-0003-3750-0183 FU Alfred P. Sloan and David and Lucile Packard foundations; NASA [NNX12AI50G, NNX14AB92G]; National Science Foundation [IIS-1124794]; NASA Postdoctoral Program at Ames Research Center; NASA Science Mission directorate; Association of Universities for Research in Astronomy, Inc., under NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; W. M. Keck Foundation FX We are grateful to the referee for a helpful report. We thank David Hogg, Gongjie Li, Katherine Deck, Joshua Carter, Guillaume Hebrard, Boas Katz, Yoram Lithwick, Smadar Naoz, Eugene Chiang, Scott Tremaine, Ellen Price, Leslie Rogers, Eric Ford, Cristobal Petrovich, and Doug Lin for helpful discussions. R. I. D. gratefully acknowledges the Miller Institute for Basic Research in Science, University of California Berkeley. J. A. J. is grateful for the generous grant support provided by the Alfred P. Sloan and David and Lucile Packard foundations. D. F. M. is supported by NASA under grant NNX12AI50G and the National Science Foundation under grant IIS-1124794. D. H. acknowledges support by an appointment to the NASA Postdoctoral Program at Ames Research Center administered by Oak Ridge Associated Universities, and NASA Grant NNX14AB92G issued through the Kepler Participating Scientist Program. This work benefited from the Summer Program on Modern Statistical and Computational Methods for Analysis of Kepler Data, held at SAMSI, Research Triangle Park, NC in 2013 June.; This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. We are grateful to the Kepler Team for their extensive efforts in producing such high-quality data. Some of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts.; We are very grateful to Geoff Marcy and Howard Isaacson for contributing to the radial-velocity observations of Kepler-419. J. A. J. is grateful for Keck/HIRES time allocated through the Caltech Time Allocation Committee for some of the spectra used herein. The spectroscopic and radial-velocity measurements presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We gratefully acknowledge the efforts and dedication of the Keck Observatory staff, especially Scott Dahm, Greg Doppman, Hien Tran, and Grant Hill for support of HIRES and GregWirth for support of remote observing. We extend special thanks to those of Hawai'ian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. NR 87 TC 21 Z9 21 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 AUG 20 PY 2014 VL 791 IS 2 AR 89 DI 10.1088/0004-637X/791/2/89 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400016 ER PT J AU Koenig, XP Leisawitz, DT AF Koenig, X. P. Leisawitz, D. T. TI A CLASSIFICATION SCHEME FOR YOUNG STELLAR OBJECTS USING THE WIDE-FIELD INFRARED SURVEY EXPLORER AllWISE CATALOG: REVEALING LOW-DENSITY STAR FORMATION IN THE OUTER GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; H II regions; infrared: stars; stars: formation; stars: pre-main sequence ID MAIN-SEQUENCE STARS; INTERSTELLAR-MEDIUM; SOLAR NEIGHBORHOOD; PLANETARY-NEBULAE; MOLECULAR CLOUDS; GALACTIC-CENTER; SPITZER SURVEY; WISE MISSION; OH/IR STARS; MU-M AB We present an assessment of the performance of WISE and the AllWISE data release for a section of the Galactic Plane. We lay out an approach to increasing the reliability of point-source photometry extracted from the AllWISE catalog in Galactic Plane regions using parameters provided in the catalog. We use the resulting catalog to construct a new, revised young star detection and classification scheme combining WISE and 2MASS near- and mid-infrared colors and magnitudes and test it in a section of the outer Milky Way. The clustering properties of the candidate Class I and II stars using a nearest neighbor density calculation and the two-point correlation function suggest that the majority of stars do form in massive star-forming regions, and any isolated mode of star formation is at most a small fraction of the total star forming output of the Galaxy. We also show that the isolated component may be very small and could represent the tail end of a single mechanism of star formation in line with models of molecular cloud collapse with supersonic turbulence and not a separate mode all to itself. C1 [Koenig, X. P.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Leisawitz, D. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Koenig, XP (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA. OI Koenig, Xavier/0000-0002-9478-4170 FU NASA ADAP grant [NNX13AF07G]; National Aeronautics and Space Administration (NASA); NASA; National Science Foundation FX We thank the anonymous referee whose comments and suggestions improved the paper. Author Koenig gratefully acknowledges support from NASA ADAP grant No. NNX13AF07G. This work is based on data obtained from (1) the Wide-Field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech), funded by the National Aeronautics and Space Administration (NASA); (2) the Two Micron All Sky Survey, a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center (IPAC)/Caltech, funded by NASA and the National Science Foundation; and (3) the NASA/IPAC Infrared Science Archive, which is operated by JPL, Caltech, under a contract with NASA. This research has made use of NASA's Astrophysics Data System. NR 61 TC 18 Z9 18 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2014 VL 791 IS 2 AR 131 DI 10.1088/0004-637X/791/2/131 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400058 ER PT J AU Masiero, JR Grav, T Mainzer, AK Nugent, CR Bauer, JM Stevenson, R Sonnett, S AF Masiero, Joseph R. Grav, T. Mainzer, A. K. Nugent, C. R. Bauer, J. M. Stevenson, R. Sonnett, S. TI MAIN-BELT ASTEROIDS WITH WISE/NEOWISE: NEAR-INFRARED ALBEDOS SO ASTROPHYSICAL JOURNAL LA English DT Article DE minor planets, asteroids: general ID SURVEY-EXPLORER; THERMAL-MODEL; SOLAR-SYSTEM; NEOWISE; IDENTIFICATION; METEORITES; FAMILIES; ORGANICS; MISSION; SURFACE AB We present revised near-infrared albedo fits of 2835 main-belt asteroids observed by WISE/NEOWISE over the course of its fully cryogenic survey in 2010. These fits are derived from reflected-light near-infrared images taken simultaneously with thermal emission measurements, allowing for more accurate measurements of the near-infrared albedos than is possible for visible albedo measurements. Because our sample requires reflected light measurements, it undersamples small, low-albedo asteroids, as well as those with blue spectral slopes across the wavelengths investigated. We find that the main belt separates into three distinct groups of 6%, 16%, and 40% reflectance at 3.4 mu m. Conversely, the 4.6 mu m albedo distribution spans the full range of possible values with no clear grouping. Asteroid families show a narrow distribution of 3.4 m albedos within each family that map to one of the three observed groupings, with the (221) Eos family being the sole family associated with the 16% reflectance 3.4 m albedo group. We show that near-infrared albedos derived from simultaneous thermal emission and reflected light measurements are important indicators of asteroid taxonomy and can identify interesting targets for spectroscopic follow-up. C1 [Masiero, Joseph R.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R.; Sonnett, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Grav, T.] Planetary Sci Inst, Tucson, AZ USA. [Bauer, J. M.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Masiero, JR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-601, Pasadena, CA 91109 USA. EM Joseph.Masiero@jpl.nasa.gov; tgrav@psi.edu; amainzer@jpl.nasa.gov; cnugent@jpl.nasa.gov; James.Bauer@jpl.nasa.gov; Rachel.A.Stevenson@jpl.nasa.gov; sarah.sonnett@jpl.nasa.gov OI Masiero, Joseph/0000-0003-2638-720X FU NASA Planetary Geology and Geophysics grant; National Aeronautics and Space Administration; Planetary Science Division of the National Aeronautics and Space Administration FX J.M. was partially supported by a NASA Planetary Geology and Geophysics grant. C.N., R. S., and S. S. were supported by an appointment to the NASA Postdoctoral Program at JPL, administered by Oak Ridge Associated Universities through a contract with NASA. We thank the referee for helpful comments that greatly improved this manuscript. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 39 TC 16 Z9 16 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 AUG 20 PY 2014 VL 791 IS 2 AR 121 DI 10.1088/0004-637X/791/2/121 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400048 ER PT J AU Paganini, L Mumma, MJ Villanueva, GL Keane, JV Blake, GA Bonev, BP DiSanti, MA Gibb, EL Meech, KJ AF Paganini, L. Mumma, M. J. Villanueva, G. L. Keane, J. V. Blake, G. A. Bonev, B. P. DiSanti, M. A. Gibb, E. L. Meech, K. J. TI C/2013 R1 (LOVEJOY) AT IR WAVELENGTHS AND THE VARIABILITY OF CO ABUNDANCES AMONG OORT CLOUD COMETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; comets: general; comets: individual (C/2013 R1 (Lovejoy)); infrared: planetary systems; molecular processes; Oort Cloud ID O1 HALE-BOPP; HUBBLE-SPACE-TELESCOPE; C/1996 B2 HYAKUTAKE; CARBON-MONOXIDE; CHEMICAL-COMPOSITION; INFRARED WAVELENGTHS; ORGANIC COMPOSITION; PARENT VOLATILES; Q2 MACHHOLZ; P1 GARRADD AB We report production rates, rotational temperatures, and related parameters for gases in C/2013 R1 (Lovejoy) using the Near InfraRed SPECtrometer at the Keck Observatory, on six UT dates spanning heliocentric distances (Rh) that decreased from 1.35 AU to 1.16 AU (pre-perihelion). We quantified nine gaseous species (H2O, OH*, CO, CH4, HCN, C2H6, CH3OH, NH3, and NH2) and obtained upper limits for two others (C2H2 and H2CO). Compared with organics-normal comets, our results reveal highly enriched CO, (at most) slightly enriched CH3OH, C2H6, and HCN, and CH4 consistent with " normal", yet depleted, NH3, C2H2, and H2CO. Rotational temperatures increased from similar to 50 K to similar to 70 K with decreasing Rh, following a power law in Rh of -2.0 +/- 0.2, while the water production rate increased from 1.0 to 3.9x1028 molecules s(-1), following a power law in Rh of-4.7 +/- 0.9. The ortho-para ratio for H2O was 3.01 +/- 0.49, corresponding to spin temperatures (Tspin) similar to 29 K (at the 1s level). The observed spatial profiles for these emissions showed complex structures, possibly tied to nucleus rotation, although the cadence of our observations limits any definitive conclusions. The retrieved CO abundance in Lovejoy is more than twice the median value for comets in our IR survey, suggesting this comet is enriched in CO. We discuss the enriched value for CO in comet C/2013 R1 in terms of the variability of CO among Oort Cloud comets. C1 [Paganini, L.; Mumma, M. J.; Villanueva, G. L.; Bonev, B. P.; DiSanti, M. A.] NASA GSFC, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Paganini, L.; Villanueva, G. L.; Bonev, B. P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Keane, J. V.; Meech, K. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Keane, J. V.; Meech, K. J.] NASA Astrobiol Inst, Mountain View, CA USA. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Gibb, E. L.] Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA. RP Paganini, L (reprint author), NASA GSFC, Goddard Ctr Astrobiol, MS 690, Greenbelt, MD 20771 USA. EM lucas.paganini@nasa.gov FU NASA's PAST Program; NAI through its member Teams at GSFC; UH [NNA09DA77A]; NSF [1211362] FX We gratefully acknowledge support by NASA's PAST Program (L. P., M.J.M, M. A. D., G. L. V.) and NAI through its member Teams at GSFC (M.J.M., M. A. D., B. P. B., G. A. B.) and at UH (J.V.K., K.J.M.; No. NNA09DA77A), and NSF (B. P. B., E. L. G.; Award 1211362). The data of October 24 and 25 were collected during part of the NASA Keck time awarded for observations of comet ISON, and are publicly available through the Keck Observatory Archive. We thank the anonymous referee for useful insights on this paper. The authors 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 67 TC 8 Z9 8 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 AUG 20 PY 2014 VL 791 IS 2 AR 122 DI 10.1088/0004-637X/791/2/122 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400049 ER PT J AU Tendulkar, SP Yang, CW An, HJ Kaspi, VM Archibald, AM Bassa, C Bellm, E Bogdanov, S Harrison, FA Hessels, JWT Janssen, GH Lyne, AG Patruno, A Stappers, B Stern, D Tomsick, JA Boggs, SE Chakrabarty, D Christensen, FE Craig, WW Hailey, CA Zhang, W AF Tendulkar, Shriharsh P. Yang, Chengwei An, Hongjun Kaspi, Victoria M. Archibald, Anne M. Bassa, Cees Bellm, Eric Bogdanov, Slavko Harrison, Fiona A. Hessels, Jason W. T. Janssen, Gemma H. Lyne, Andrew G. Patruno, Alessandro Stappers, Benjamin Stern, Daniel Tomsick, John A. Boggs, Steven E. Chakrabarty, Deepto Christensen, Finn E. Craig, William W. Hailey, Charles A. Zhang, William TI NuSTAR OBSERVATIONS OF THE STATE TRANSITION OF MILLISECOND PULSAR BINARY PSR J1023+0038 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: general; pulsars: individual (PSR J1023+0038); stars: neutron; X-rays: stars ID X-RAY BINARY; QUASI-PERIODIC OSCILLATIONS; 1ST J102347.6+003841; ACCRETION POWER; XSS J12270-4859; RADIO PULSARS; SPIN-DOWN; SYSTEM; EMISSION; ROTATION AB We report NuSTAR observations of the millisecond pulsar-low-mass X-ray binary (LMXB) transition system PSR J1023+0038 from 2013 June and October, before and after the formation of an accretion disk around the neutron star. Between June 10 and 12, a few days to two weeks before the radio disappearance of the pulsar, the 3-79 keV X-ray spectrum was well fit by a simple power law with a photon index of Gamma = 1.17(-0.07)(+0.08) (at 90% confidence) with a 3-79 keV luminosity of 7.4 +/- 0.4 x 10(32) erg s(-1). Significant orbital modulation was observed with a modulation fraction of 36% +/- 10%. During the October 19-21 observation, the spectrum is described by a softer power law (Gamma = 1.66(-0.05)(+0.06)) with an average luminosity of 5.8 +/- 0.2x10(33) erg s(-1) and a peak luminosity of approximate to 1.2x10(34) erg s(-1) observed during a flare. No significant orbital modulation was detected. The spectral observations are consistent with previous and current multiwavelength observations and show the hard X-ray power law extending to 79 keV without a spectral break. Sharp-edged, flat-bottomed dips are observed with widths between 30 and 1000 s and ingress and egress timescales of 30-60 s. No change in hardness ratio was observed during the dips. Consecutive dip separations are log-normal in distribution with a typical separation of approximately 400 s. These dips are distinct from dipping activity observed in LMXBs. We compare and contrast these dips to observations of dips and state changes in the similar transition systems PSR J1824-2452I and XSS J1227.0-4859 and discuss possible interpretations based on the transitions in the inner disk. C1 [Tendulkar, Shriharsh P.; Bellm, Eric; Harrison, Fiona A.] CALTECH, Pasadena, CA 91125 USA. [Yang, Chengwei; An, Hongjun; Kaspi, Victoria M.] McGill Univ, Dept Phys, Montreal II3A 2T8, PQ, Canada. [Yang, Chengwei] Chinese Acad Sci, Natl Space Sci Ctr, Beijing 100190, Peoples R China. [Archibald, Anne M.; Bassa, Cees; Hessels, Jason W. T.; Janssen, Gemma H.; Patruno, Alessandro] ASTRON, Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands. [Bogdanov, Slavko; Hailey, Charles A.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hessels, Jason W. T.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Lyne, Andrew G.; Stappers, Benjamin] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Patruno, Alessandro] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tomsick, John A.; Boggs, Steven E.; Craig, William W.] Univ Calif, Space Sci Lab, Berkeley, CA 94720 USA. [Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Christensen, Finn E.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Zhang, William] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Tendulkar, SP (reprint author), CALTECH, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. EM spt@astro.caltech.edu RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Bellm, Eric/0000-0001-8018-5348; An, Hongjun/0000-0002-6389-9012; Archibald, Anne/0000-0003-0638-3340 FU NASA [NNG08FD60C]; NuSTAR mission; California Institute of Technology; National Aeronautics and Space Administration; NSERC Discovery Grant; Centre de Recherche en Astrophysique du Quebec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Study; Canada Research Chairs Program; Lorne Trottier Chair in Astrophysics and Cosmology; ERC starting grant DRAGNET; Netherlands Organization for Scientic Research (NWO) Vidi fellowship FX We thank the anonymous referee for detailed suggestions and comments. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). VMKreceives support from an NSERC Discovery Grant and Accelerator Supplement, from the Centre de Recherche en Astrophysique du Quebec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Study, the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. J. W. T. H. acknowledges funding for this work from ERC starting grant DRAGNET. A. P. acknowledges support from the Netherlands Organization for Scientic Research (NWO) Vidi fellowship. NR 52 TC 20 Z9 20 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2014 VL 791 IS 2 AR 77 DI 10.1088/0004-637X/791/2/77 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400004 ER PT J AU Wang, J Fischer, DA Xie, JW Ciardi, DR AF Wang, Ji Fischer, Debra A. Xie, Ji-Wei Ciardi, David R. TI INFLUENCE OF STELLAR MULTIPLICITY ON PLANET FORMATION. II. PLANETS ARE LESS COMMON IN MULTIPLE-STAR SYSTEMS WITH SEPARATIONS SMALLER THAN 1500 AU SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: observational; methods: statistical; planetary systems; planets and satellites: fundamental parameters; techniques: high angular resolution; techniques: photometric ID EXOPLANET HOST STARS; TRANSITING CIRCUMBINARY PLANET; RADIAL-VELOCITY SEARCH; SOLAR-TYPE STARS; ADAPTIVE OPTICS; BINARY-SYSTEMS; EXTRASOLAR PLANETS; HABITABLE ZONES; INFRARED CAMERA; KEPLER OBJECTS AB Almost half of the stellar systems in the solar neighborhood are made up of multiple stars. In multiple-star systems, planet formation is under the dynamical influence of stellar companions, and the planet occurrence rate is expected to be different from that of single stars. There have been numerous studies on the planet occurrence rate of single star systems. However, to fully understand planet formation, the planet occurrence rate in multiple-star systems needs to be addressed. In this work, we infer the planet occurrence rate in multiple-star systems by measuring the stellar multiplicity rate for planet host stars. For a subsample of 56 Kepler planet host stars, we use adaptive optics (AO) imaging and the radial velocity (RV) technique to search for stellar companions. The combination of these two techniques results in high search completeness for stellar companions. We detect 59 visual stellar companions to 25 planet host stars with AO data. Three stellar companions are within 2 '' and 27 within 6 ''. We also detect two possible stellar companions (KOI 5 and KOI 69) showing long-term RV acceleration. After correcting for a bias against planet detection in multiple-star systems due to flux contamination, we find that planet formation is suppressed in multiple-star systems with separations smaller than 1500 AU. Specifically, we find that compared to single star systems, planets in multiple-star systems occur 4.5 +/- 3.2, 2.6 +/- 1.0, and 1.7 +/- 0.5 times less frequently when a stellar companion is present at a distance of 10, 100, and 1000 AU, respectively. This conclusion applies only to circumstellar planets; the planet occurrence rate for circumbinary planets requires further investigation. C1 [Wang, Ji; Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Xie, Ji-Wei] Nanjing Univ, Minist Educ, Dept Astron, Nanjing 210093, Jiangsu, Peoples R China. [Xie, Ji-Wei] Nanjing Univ, Minist Educ, Key Lab Modern Astron & Astrophys, Nanjing 210093, Jiangsu, Peoples R China. [Ciardi, David R.] NASA, Exoplanet Sci Inst, CALTECH, Pasadena, CA 91125 USA. RP Wang, J (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA. EM ji.wang@yale.edu OI Ciardi, David/0000-0002-5741-3047; Wang, Ji/0000-0002-4361-8885 FU Foundation for the Author of National Excellent Doctoral Dissertation (FANEDD) of PR China FX The authors thank Howard Isaacson and Matt Giguere for helpful comments and proofreading the paper. The research is made possible by the data from the Kepler Community Followup Observing Program (CFOP). The authors acknowledge all the CFOP users who uploaded the AO and RV data used in the paper. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Ji-wei Xie is supported by a Foundation for the Author of National Excellent Doctoral Dissertation (FANEDD) of PR China. NR 81 TC 40 Z9 40 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 AUG 20 PY 2014 VL 791 IS 2 AR 111 DI 10.1088/0004-637X/791/2/111 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400038 ER PT J AU Andreev-Andrievskiy, A Popova, A Boyle, R Alberts, J Shenkman, B Vinogradova, O Dolgov, O Anokhin, K Tsvirkun, D Soldatov, P Nemirovskaya, T Ilyin, E Sychev, V AF Andreev-Andrievskiy, Alexander Popova, Anfisa Boyle, Richard Alberts, Jeffrey Shenkman, Boris Vinogradova, Olga Dolgov, Oleg Anokhin, Konstantin Tsvirkun, Darya Soldatov, Pavel Nemirovskaya, Tatyana Ilyin, Eugeniy Sychev, Vladimir TI Mice in Bion-M 1 Space Mission: Training and Selection SO PLOS ONE LA English DT Article ID ENVIRONMENTAL ENRICHMENT; LABORATORY MICE; INBRED MICE; HEART-RATE; STRESS; SPACEFLIGHT; MOUSE; SUSCEPTIBILITY; RESPONSES; STRENGTH AB After a 16-year hiatus, Russia has resumed its program of biomedical research in space, with the successful 30-day flight of the Bion-M 1 biosatellite (April 19-May 19, 2013). The principal species for biomedical research in this project was the mouse. This paper presents an overview of the scientific goals, the experimental design and the mouse training/selection program. The aim of mice experiments in the Bion-M 1 project was to elucidate cellular and molecular mechanisms, underlying the adaptation of key physiological systems to long-term exposure in microgravity. The studies with mice combined in vivo measurements, both in flight and post-flight (including continuous blood pressure measurement), with extensive in vitro studies carried out shortly after return of the mice and in the end of recovery study. Male C57/BL6 mice group housed in space habitats were flown aboard the Bion-M 1 biosatellite, or remained on ground in the control experiment that replicated environmental and housing conditions in the spacecraft. Vivarium control groups were used to account for housing effects and possible seasonal differences. Mice training included the co-adaptation in housing groups and mice adaptation to paste food diet. The measures taken to co-adapt aggressive male mice in housing groups and the peculiarities of "space'' paste food are described. The training program for mice designated for in vivo studies was broader and included behavioral/functional test battery and continuous behavioral measurements in the home-cage. The results of the preliminary tests were used for the selection of homogenous groups. After the flight, mice were in good condition for biomedical studies and displayed signs of pronounced disadaptation to Earth's gravity. The outcomes of the training program for the mice welfare are discussed. We conclude that our training program was effective and that male mice can be successfully employed in space biomedical research. C1 [Andreev-Andrievskiy, Alexander; Popova, Anfisa; Shenkman, Boris; Vinogradova, Olga; Tsvirkun, Darya; Soldatov, Pavel; Nemirovskaya, Tatyana; Ilyin, Eugeniy; Sychev, Vladimir] Russian Acad Sci, Inst Biomed Problems, Moscow, Russia. [Andreev-Andrievskiy, Alexander; Popova, Anfisa] Moscow MV Lomonosov State Univ, Fac Biol, Moscow, Russia. [Boyle, Richard] NASA, Ames Res Ctr, Biovisualizat Imaging & Simulat Technol Ctr BioVI, Moffett Field, CA 94035 USA. [Alberts, Jeffrey] Indiana Univ, Dept Psychol & Brain Sci, Bloomington, IN USA. [Dolgov, Oleg; Anokhin, Konstantin] Russian Acad Med Sci, Anokhin Inst Normal Physiol, Moscow, Russia. [Anokhin, Konstantin] Kurchatov Inst, Kurchatov NBIC Ctr, Natl Res Ctr, Moscow, Russia. RP Andreev-Andrievskiy, A (reprint author), Russian Acad Sci, Inst Biomed Problems, Moscow, Russia. EM aandrievsky@gmail.com RI Andreev-Andrievskiy, Alexander/B-7336-2013 OI Andreev-Andrievskiy, Alexander/0000-0002-1173-8153 FU Russian Federal Space Agency; Russian Academy of Sciences; Division of Physiology and Fundamental Medicine of Russian Academy of Sciences; RFBR [12-04-01665-a] FX The project was supported by the Russian Federal Space Agency and the Russian Academy of Sciences. These funders took part in study design and data collection, but had no role in data analysis or decision to publish. The study was also supported by the Division of Physiology and Fundamental Medicine of Russian Academy of Sciences ("Integrative physiology" program) and RFBR grant 12-04-01665-a. These funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 36 TC 10 Z9 10 U1 1 U2 12 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD AUG 18 PY 2014 VL 9 IS 8 AR e104830 DI 10.1371/journal.pone.0104830 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AO4JF UT WOS:000341302700043 PM 25133741 ER PT J AU Cable, ML Vu, TH Hodyss, R Choukroun, M Malaska, MJ Beauchamp, P AF Cable, Morgan L. Vu, Tuan H. Hodyss, Robert Choukroun, Mathieu Malaska, Michael J. Beauchamp, Patricia TI Experimental determination of the kinetics of formation of the benzene-ethane co-crystal and implications for Titan SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE ethane; benzene; cocrystal; evaporite; hydrocarbon; Titan ID CHEMICAL-COMPOSITION; ATMOSPHERE; SPECTRA; DRIZZLE; LAKES AB Benzene is found on Titan and is a likely constituent of the putative evaporite deposits formed around the hydrocarbon lakes. We have recently demonstrated the formation of a benzene-ethane co-crystal under Titan-like surface conditions. Here we investigate the kinetics of formation of this new structure as a function of temperature. We show that the formation process would reach completion under Titan surface conditions in similar to 18 h and that benzene precipitates from liquid ethane as the co-crystal. This suggests that benzene-rich evaporite basins around ethane/methane lakes and seas may not contain pure crystalline benzene, but instead benzene-ethane co-crystals. This co-crystalline form of benzene with ethane represents a new class of materials for Titan's surface, analogous to hydrated minerals on Earth. This new structure may also influence evaporite characteristics such as particle size, dissolution rate, and infrared spectral properties. C1 [Cable, Morgan L.; Vu, Tuan H.; Hodyss, Robert; Choukroun, Mathieu; Malaska, Michael J.; Beauchamp, Patricia] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Hodyss, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Robert.P.Hodyss@jpl.nasa.gov RI Choukroun, Mathieu/F-3146-2017; Vu, Tuan/F-5223-2017; OI Choukroun, Mathieu/0000-0001-7447-9139; Vu, Tuan/0000-0001-6839-9765; Malaska, Michael/0000-0003-0064-5258 FU NASA Astrobiology Institute, Titan as a Prebiotic Chemical System; NASA Outer Planets Research (OPR) Program; NASA's Outer Planets Research Program; NASA Postdoctoral Program; NASA FX We thank Ralph Lorenz and Jason Barnes for helpful comments. M. L. C., M. C., P. B., and R. H. were funded by the NASA Astrobiology Institute, Titan as a Prebiotic Chemical System. TV was funded through the NASA Outer Planets Research (OPR) Program. M. M. was funded through NASA's Outer Planets Research Program and the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Data reported in this work may be accessed by contacting the corresponding author. Government sponsorship is gratefully acknowledged. NR 27 TC 2 Z9 2 U1 2 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 16 PY 2014 VL 41 IS 15 BP 5396 EP 5401 DI 10.1002/2014GL060531 PG 6 WC Geosciences, Multidisciplinary SC Geology GA AP0BI UT WOS:000341725200011 ER PT J AU Dutrieux, P Stewart, C Jenkins, A Nicholls, KW Corr, HFJ Rignot, E Steffen, K AF Dutrieux, Pierre Stewart, Craig Jenkins, Adrian Nicholls, Keith W. Corr, Hugh F. J. Rignot, Eric Steffen, Konrad TI Basal terraces on melting ice shelves SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE cryosphere; ice shelf-ocean interactions; ocean; ice ID PINE ISLAND GLACIER; PHASE-SENSITIVE RADAR; WEST ANTARCTICA; BENEATH; SHEET; RETREAT; CIRCULATION; CHANNELS; MODEL; WATER AB Ocean waters melt the margins of Antarctic and Greenland glaciers, and individual glaciers' responses and the integrity of their ice shelves are expected to depend on the spatial distribution of melt. The bases of the ice shelves associated with Pine Island Glacier (West Antarctica) and Petermann Glacier (Greenland) have similar geometries, including kilometer-wide, hundreds-of-meter high channels oriented along and across the direction of ice flow. The channels are enhanced by, and constrain, oceanic melt. New meter-scale observations of basal topography reveal peculiar glaciated landscapes. Channel flanks are not smooth, but are instead stepped, with hundreds-of-meters-wide flat terraces separated by 5-50m high walls. Melting is shown to be modulated by the geometry: constant across each terrace, changing from one terrace to the next, and greatly enhanced on the similar to 45 degrees inclined walls. Melting is therefore fundamentally heterogeneous and likely associated with stratification in the ice-ocean boundary layer, challenging current models of ice shelf-ocean interactions. C1 [Dutrieux, Pierre; Jenkins, Adrian; Nicholls, Keith W.; Corr, Hugh F. J.] British Antarctic Survey, NERC, Cambridge, England. [Stewart, Craig] Univ Cambridge, Scott Polar Res Inst, Cambridge CB2 1ER, England. [Rignot, Eric] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Rignot, Eric] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Steffen, Konrad] Swiss Fed Res Inst WLS, Birmensdorf, Switzerland. [Steffen, Konrad] Swiss Fed Inst Technol, Inst Atmosphere & Climate, Zurich, Switzerland. RP Dutrieux, P (reprint author), British Antarctic Survey, NERC, Cambridge, England. EM pierre.dutrieux@bas.ac.uk RI Steffen, Konrad/C-6027-2013; Rignot, Eric/A-4560-2014; Dutrieux, Pierre/B-7568-2012 OI Steffen, Konrad/0000-0001-8658-1026; Rignot, Eric/0000-0002-3366-0481; Dutrieux, Pierre/0000-0002-8066-934X FU NERC [NE/G001367/1, NE/J005770/1]; NSF [NAG5-12075]; NASA grant, Cryopshere Science Program FX P.D. was supported by the NERC grants NE/G001367/1 and NE/J005770/1. Stanley S. Jacobs and NSF are acknowledged for providing shipboard support during the Autosub observations. Stephen D. McPhail, James R. Perrett, Andrew T. Webb, and David White are acknowledged for configuring and preparing the Autosub missions. Field work on Petermann glacier was supported by the NSF grant NAG5-12075 and a NASA grant from the Cryopshere Science Program. The data used to produce the results of this paper are freely available upon request to the authors. NR 39 TC 11 Z9 11 U1 1 U2 26 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 16 PY 2014 VL 41 IS 15 BP 5506 EP 5513 DI 10.1002/2014GL060618 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AP0BI UT WOS:000341725200025 ER PT J AU Carlson, AE Winsor, K Ullman, DJ Brook, EJ Rood, DH Axford, Y LeGrande, AN Anslow, FS Sinclair, G AF Carlson, Anders E. Winsor, Kelsey Ullman, David J. Brook, Edward J. Rood, Dylan H. Axford, Yarrow LeGrande, Allegra N. Anslow, Faron S. Sinclair, Gaylen TI Earliest Holocene south Greenland ice sheet retreat within its late Holocene extent SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Greenland ice sheet; cosmogenic dating; early Holocene climate ID PRODUCTION-RATE CALIBRATION; SEA-LEVEL CHANGES; WEST GREENLAND; LAKE-SEDIMENTS; JAKOBSHAVN-ISFJORD; CLIMATE VARIATIONS; HISTORY; BE-10; TEMPERATURE; MAXIMUM AB Early Holocene summer warmth drove dramatic Greenland ice sheet (GIS) retreat. Subsequent insolation-driven cooling caused GIS margin readvance to late Holocene maxima, from which ice margins are now retreating. We use Be-10 surface exposure ages from four locations between 69.4 degrees N and 61.2 degrees N to date when in the early Holocene south to west GIS margins retreated to within these late Holocene maximum extents. We find that this occurred at 11.10.2 ka to 10.60.5 ka in south Greenland, significantly earlier than previous estimates, and 6.80.1 ka to 7.90.1 ka in southwest to west Greenland, consistent with existing Be-10 ages. At least in south Greenland, these Be-10 ages likely provide a minimum constraint for when on a multicentury timescale summer temperatures after the last deglaciation warmed above late Holocene temperatures in the early Holocene. Current south Greenland ice margin retreat suggests that south Greenland may have now warmed to or above earliest Holocene summer temperatures. C1 [Carlson, Anders E.; Ullman, David J.; Brook, Edward J.; Sinclair, Gaylen] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Winsor, Kelsey] Univ Wisconsin, Dept Geosci, Madison, WI USA. [Rood, Dylan H.] Univ Glasgow, Scottish Univ Environm Res Ctr, Glasgow, Lanark, Scotland. [Rood, Dylan H.] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA. [Axford, Yarrow] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL USA. [LeGrande, Allegra N.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [LeGrande, Allegra N.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Anslow, Faron S.] Univ Victoria, Pacific Climate Impacts Consortium, Victoria, BC, Canada. RP Carlson, AE (reprint author), Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA. EM acarlson@coas.oregonstate.edu RI Axford, Yarrow/N-4151-2014 OI Axford, Yarrow/0000-0002-8033-358X FU National Geographic Society [8687-09] FX We thank D. Murray, J. Harvey, B. Goehring, and S. Marcott for lab assistance, S. Marcott for discussion of the Northern Hemisphere temperature stack, N. Larsen for sharing data, and the National Geographic Society (award 8687-09 to A.E. Carlson). Comments by two anonymous reviewers significantly improved this manuscript. Data are available in Tables S1 and S2. NR 55 TC 12 Z9 12 U1 5 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 16 PY 2014 VL 41 IS 15 BP 5514 EP 5521 DI 10.1002/2014GL060800 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AP0BI UT WOS:000341725200026 ER PT J AU Allan, RP Liu, CL Loeb, NG Palmer, MD Roberts, M Smith, D Vidale, PL AF Allan, Richard P. Liu, Chunlei Loeb, Norman G. Palmer, Matthew D. Roberts, Malcolm Smith, Doug Vidale, Pier-Luigi TI Changes in global net radiative imbalance 1985-2012 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE radiative flux; climate variability; satellite data; climate model; energy balance; temperature ID CLIMATE-CHANGE; DECADAL VARIABILITY; WARMING HIATUS; ENERGY BUDGET; WATER-VAPOR; MODEL; TEMPERATURE; SYSTEM; CMIP5; EARTH AB Combining satellite data, atmospheric reanalyses, and climate model simulations, variability in the net downward radiative flux imbalance at the top of Earth's atmosphere (N) is reconstructed and linked to recent climate change. Over the 1985-1999 period mean N (0.34 0.67Wm(-2)) is lower than for the 2000-2012 period (0.62 0.43Wm(-2), uncertainties at 90% confidence level) despite the slower rate of surface temperature rise since 2000. While the precise magnitude of N remains uncertain, the reconstruction captures interannual variability which is dominated by the eruption of Mount Pinatubo in 1991 and the El Nino Southern Oscillation. Monthly deseasonalized interannual variability in N generated by an ensemble of nine climate model simulations using prescribed sea surface temperature and radiative forcings and from the satellite-based reconstruction is significantly correlated (r approximate to 0.6) over the 1985-2012 period. C1 [Allan, Richard P.; Liu, Chunlei; Vidale, Pier-Luigi] Univ Reading, Dept Meteorol, Reading, Berks, England. [Loeb, Norman G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Palmer, Matthew D.; Roberts, Malcolm; Smith, Doug] Met Off, Exeter, Devon, England. RP Allan, RP (reprint author), Univ Reading, Dept Meteorol, Reading, Berks, England. EM r.p.allan@reading.ac.uk RI Allan, Richard/B-5782-2008; OI Allan, Richard/0000-0003-0264-9447; Vidale, Pier Luigi/0000-0002-1800-8460 FU Natural Environment Research Council (NERC) DEEP-C [NE/K005480/1]; National Centre for Atmospheric Science; National Centre for Earth Observation FX This work was supported by the Natural Environment Research Council (NERC) DEEP-C grant NE/K005480/1, the National Centre for Atmospheric Science, and the National Centre for Earth Observation. We acknowledge the World Climate Research Programme's Working Group on Coupled Modelling, which is responsible for CMIP, and we thank the climate modeling groups (models listed in Table 1) for producing and making available their model outputs; for CMIP, the U.S. Department of Energy's PCMDI provided coordinating support and led development of software infrastructure in partnership with the Global Organization for Earth System Science Portals. The UPSCALE simulations were performed under a grant of supercomputing time from PRACE using the HLRS HERMIT Cray XE6. Data generated by this work are available at http://www.met.reading.ac.uk/similar to sgs02rpa/research/DEEP-C/GRL/. We thank Kevin Trenberth and Kyle Armour for taking the time to review our work, which helped to improve the manuscript. NR 57 TC 35 Z9 35 U1 2 U2 43 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 16 PY 2014 VL 41 IS 15 BP 5588 EP 5597 DI 10.1002/2014GL060962 PG 10 WC Geosciences, Multidisciplinary SC Geology GA AP0BI UT WOS:000341725200035 ER PT J AU Xi, BK Dong, XQ Minnis, P Sun-Mack, S AF Xi, Baike Dong, Xiquan Minnis, Patrick Sun-Mack, Sunny TI Comparison of marine boundary layer cloud properties from CERES-MODIS Edition 4 and DOE ARM AMF measurements at the Azores SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GROUND-BASED MEASUREMENTS; ENERGY SYSTEM CERES; LIQUID WATER PATH; STRATOCUMULUS CLOUD; SATELLITE-OBSERVATIONS; CLIMATE; RETRIEVALS; TERRA; AQUA; FRACTION AB Marine boundary layer (MBL) cloud properties derived from the NASA Clouds and the Earth's Radiant Energy System (CERES) project using Terra and Aqua Moderate Resolution Imaging Spectroradiometer (MODIS) data are compared with observations taken at the Department of Energy Atmospheric Radiation Measurement (ARM) Mobile Facility at the Azores (AMF-Azores) site from June 2009 through December 2010. Cloud properties derived from ARM ground-based observations were averaged over a 1 h interval centered at the satellite overpass time, while the CERES-MODIS (CM) results were averaged within a 30 km x 30 km grid box centered over the Azores site. A total of 63 daytime and 92 nighttime single-layered overcast MBL cloud cases were selected from 19 months of ARM radar-lidar and satellite observations. The CM cloud top/base heights (H-top/H-base) were determined from cloud top/base temperatures (T-top/T-base) using a regional boundary layer lapse rate method. For daytime comparisons, the CM-derived H-top (H-base), on average, is 0.063 km (0.068 km) higher (lower) than its ARM radar-lidar-observed counterpart, and the CM-derived T-top and T-base are 0.9 K less and 2.5 K greater than the surface values with high correlations (R-2 = 0.82 and 0.84, respectively). In general, the cloud top comparisons agree better than the cloud base comparisons, because the CM cloud base temperatures and heights are secondary products determined from cloud top temperatures and heights. No significant day-night difference was found in the analyses. The comparisons of MBL cloud microphysical properties reveal that when averaged over a 30 km x 30 km area, the CM-retrieved cloud droplet effective radius (r(e)) at 3.7 mu m is 1.3 mu m larger than that from the ARM retrievals (12.8 mu m), while the CM-retrieved cloud liquid water path (LWP) is 13.5 gm(-2) less than its ARM counterpart (114.2 gm(-2)) due to its small optical depth (9.6 versus 13.7). The differences are reduced by 50% when the CM averages are computed only using the MODIS pixel nearest the AMF site. Using the effective radius retrieved using 2.1 mu m channel to calculate LWP can reduce the difference between the CM and ARM microwave radiometer retrievals from -13.7 to 2.1 gm(-2). The 10% differences between the ARM and CERES-MODIS LWP and r(e) retrievals are within the uncertainties of the ARM LWP (similar to 20 gm(-2)) and r(e) (similar to 10%) retrievals; however, the 30% difference in optical depth is significant. Possible reasons contributing to this discrepancy are increased sensitivities in optical depth from both surface retrievals when tau similar to 10 and topography. The tau differences vary with wind direction and are consistent with the island orography. Much better agreement in tau is obtained when using only those data taken when the wind is from the northeast, where topographical effects on the sampled clouds are minimal. C1 [Xi, Baike; Dong, Xiquan] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58201 USA. [Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Sun-Mack, Sunny] SSAI, Hampton, VA USA. RP Xi, BK (reprint author), Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58201 USA. EM baike@aero.und.edu RI Minnis, Patrick/G-1902-2010; OI Minnis, Patrick/0000-0002-4733-6148; Dong, Xiquan/0000-0002-3359-6117 FU U.S. Department of Energy (DOE) Office of Energy Research, Office of Health and Environmental Research, Environmental Sciences Division; NASA CERES project [NNX10AI05G]; DOE ASR project at University of North Dakota [DE-SC008468]; DOE ASR project at NASA Langley Research Center [DE-SC0000991] FX The ground-based measurements were obtained from the Atmospheric Radiation Measurement (ARM) Program sponsored by the U.S. Department of Energy (DOE) Office of Energy Research, Office of Health and Environmental Research, Environmental Sciences Division. The data can be downloaded from http://www.archive.arm.gov/. The satellite data were obtained from the NASA CERES cloud working group at the NASA Langley Research Center. This research was supported by the NASA CERES project under grant NNX10AI05G and DOE ASR project under grant DE-SC008468 at University of North Dakota and DE-SC0000991 at the NASA Langley Research Center. Dates and times corresponding to the sample numbers used in several figures are available from the lead author on request. NR 58 TC 9 Z9 9 U1 2 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 16 PY 2014 VL 119 IS 15 BP 9509 EP 9529 DI 10.1002/2014JD021813 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AO2ZK UT WOS:000341197400020 ER PT J AU Warner, TA Lang, TJ Lyons, WA AF Warner, Tom A. Lang, Timothy J. Lyons, Walter A. TI Synoptic scale outbreak of self-initiated upward lightning (SIUL) from tall structures during the central U. S. blizzard of 1-2 February 2011 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LAKE-EFFECT THUNDERSTORMS; WINTER THUNDERSTORMS; UNITED-STATES; DISCHARGES; SPRITES; EVENTS; STROKES; RADAR; COAST AB A major central U. S. winter cyclone on 1-2 February 2011 produced a band of high winds, up to 75 cm of snow, and numerous reports of thundersnow from Oklahoma into Ontario over a 26 h period. The National Lightning Detection Network (NLDN) recorded 282 flashes comprised of 1153 events which were >96% negative polarity. Hopes of imaging winter sprites associated with energetic positive cloud-to-ground events that sometimes accompany such winter storms did not materialize. However, the lack of lightning over the Great Lakes waters, plus media reports of numerous thundersnow events in downtown Chicago, prompted a detailed analysis of the NLDN data. This revealed that >93% of all lightning in the snow band was likely or possibly associated with self-initiated upward lightning (SIUL) events from a variety of tall, and some not so tall, structures. In addition to 43 events from two Chicago skyscrapers, many shorter structures were involved, including wind turbines (13.1% of the total) and transmission line towers (6.7%). Wind speeds for all events exceeded the 8 m s(-1) minimum threshold associated with SIULs in Japanese winter lightning storms. Radar reflectivities at the event locations had a mean of 28 dBZ and were almost always <35 dBZ. While conventional radar displays suggested stratiform precipitation in the thundersnow region, detailed analysis of 3-D-gridded NMQ (National Mosaic and Multi-Sensor Quantitative Precipitation Estimation) radar reflectivity data confirmed elevated embedded cellular convection spanning the -10 degrees C region associated with isentropic lifting above a frontal surface, evidence of noninductive charge generation sufficient to allow upward leader initiation from tall objects. C1 [Warner, Tom A.] ZTResearch, Rapid City, SD 57702 USA. [Lang, Timothy J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Lyons, Walter A.] FMA Res Inc, Ft Collins, CO USA. RP Lyons, WA (reprint author), ZTResearch, Rapid City, SD 57702 USA. EM walyons@frii.com OI Lang, Timothy/0000-0003-1576-572X; Warner, Tom/0000-0001-8589-3351 FU Defense Advanced Research Projects Agency under the NIMBUS program; National Science Foundation [AGS-1010657]; NSF [AGS-1048103] FX Vaisala, Inc. graciously supplied the NLDN stroke-level data analyzed in this study. The NLDN also enables the CMCN by providing geolocation of high-iCMC strokes via a real-time, stroke-level data feed. The ongoing efforts of Steven Cummer at Duke University to maintain and operate the CMCN are vital to this and many related studies. The NMQ radar reflectivity mosaics were provided by NOAA's National Severe Storms Laboratory. The authors especially wish to thank Robert Rauber for his valuable insights into the nature of embedded convection within the comma cloud of winter cyclones. This research was partially supported by awards from the Defense Advanced Research Projects Agency under the NIMBUS program (to Duke University and NASA Marshall Space Flight Center) and a National Science Foundation grant AGS-1010657 to Colorado State University, and especially for the assistance of Steven Cummer and Steven Rutledge. This research was also partially funded by NSF grant AGS-1048103 to South Dakota School of Mines and Technology. We would like to acknowledge and thank Alana Ballweber and Ryan Lueck from the South Dakota School of Mines and Technology for providing data and analysis from the 4 October 2013 Rapid City, SD, blizzard events. The views, opinions, and findings in this report are those of the authors and should not be construed as an official NASA or U.S. Government position, policy, or decision. Data availability: Figure 1 was derived from http://www.crh.noaa.gov/arx/?n=feb0211. NLDN data are available for purchase from Vaisala, Inc., via http://www.vaisala.com/en/products/thunderstormandlightningdetectionsyst ems/Pages/NLDN.aspx. The tower database is available from http://wireless.fcc.gov/antenna/index.htm?&job=home. Google Earth, used for the identification of additional towers, is available from http://www.google.com/earth/. Microsoft Office (used in the management of the NLDN and tower databases as well as the composition of this article) is available from http://office.microsoft.com. Satellite and related weather imagery were obtained from http://www.mmm.ucar.edu/imagearchive. National Charge Moment Change data for this case are available upon request from Duke University (cummer@ee.duke.edu). NMQ reflectivity mosaics may be obtained by contacting NSSL (http://www.nssl.noaa.gov). Single NEXRAD radar data were obtained from the National Climate Data Center (http://www.ncdc.noaa.gov/). RUC data were pulled from http://nomads.ncdc.noaa.gov/data/rucanl/201102/. The Interactive Data Language (IDL) scripts used to analyze the data NR 70 TC 4 Z9 6 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 AUG 16 PY 2014 VL 119 IS 15 BP 9530 EP 9548 DI 10.1002/2014JD021691 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AO2ZK UT WOS:000341197400021 ER PT J AU Perez-Ramirez, D Whiteman, DN Smirnov, A Lyamani, H Holben, BN Pinker, R Andrade, M Alados-Arboledas, L AF Perez-Ramirez, Daniel Whiteman, David N. Smirnov, Alexander Lyamani, Hassan Holben, Brent N. Pinker, Rachel Andrade, Marcos Alados-Arboledas, Lucas TI Evaluation of AERONET precipitable water vapor versus microwave radiometry, GPS, and radiosondes at ARM sites SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GLOBAL POSITIONING SYSTEM; MOLECULAR SPECTROSCOPIC DATABASE; RADIATION MEASUREMENT SITE; SPECTRAL-LINE DATABASE; ATMOSPHERIC RADIATION; LOGNORMAL-DISTRIBUTION; OPTICAL-PROPERTIES; VAISALA RS92; RAMAN LIDAR; DRY BIAS AB In this paper we present comparisons of Aerosol Robotic Network (AERONET) precipitable water vapor (W) retrievals from Sun photometers versus radiosonde observations and other ground-based retrieval techniques such as microwave radiometry (MWR) and GPS. The comparisons make use of the extensive measurements made within the U.S. Department of Energy Atmospheric Radiation Measurement Program (ARM), mainly at their permanent sites located at the Southern Great Plains (Oklahoma, U.S.), Nauru Islands, and Barrow (Alaska, U.S.). These places experience different types of weather which allows the comparison of W under different conditions. Radiosonde and microwave radiometry data were provided by the ARM program while the GPS data were obtained from the SOUMINET network. In general, W obtained by AERONET is lower than those obtained by MWR and GPS by similar to 6.0-9.0% and similar to 6.0-8.0%, respectively. The AERONET values are also lower by approximately 5% than those obtained from the numerous balloon-borne radiosondes launched at the Southern Great Plains. These results point toward a consistent dry bias in the retrievals of W by AERONET of approximately 5-6% and a total estimated uncertainty of 12-15%. Differences with respect to MWR retrievals are a function of solar zenith angle pointing toward a possible bias in the MWR retrievals. Finally, the ability of AERONET precipitable water vapor retrievals to provide long-term records of W in diverse climate regimes is demonstrated. C1 [Perez-Ramirez, Daniel; Whiteman, David N.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA. [Perez-Ramirez, Daniel; Lyamani, Hassan; Alados-Arboledas, Lucas] Univ Granada, Dept Fis Aplicada, Granada, Spain. [Perez-Ramirez, Daniel] Univ Space Res Assoc, Columbia, MD USA. [Smirnov, Alexander; Holben, Brent N.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Smirnov, Alexander] Sigma Space Corp, Lanham, MD USA. [Lyamani, Hassan; Alados-Arboledas, Lucas] Andalusian Inst Earth Syst Res IISTA, Granada, Spain. [Pinker, Rachel] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Andrade, Marcos] Univ Mayor de San Andres, Lab Atmospher Phys, La Paz, Bolivia. RP Perez-Ramirez, D (reprint author), NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA. EM daniel.perezramirez@nasa.gov RI Alados-Arboledas, Lucas/P-5630-2014; Pinker, Rachel/F-6565-2010; Perez-Ramirez, Daniel/Q-1129-2016; Smirnov, Alexander/C-2121-2009; OI Alados-Arboledas, Lucas/0000-0003-3576-7167; Perez-Ramirez, Daniel/0000-0002-7679-6135; Smirnov, Alexander/0000-0002-8208-1304; Lyamani, Hassan/0000-0002-6386-1102 FU NASA/Goddard Space Flight Center; Spanish Ministry of Science and Technology [CGL2010-18782, CSD2007-00067]; Andalusian Regional Government [P10-RNM-6299, P08-RNM-3568]; EU through ACTRIS project [EU INFRA-2010-1.1.16-262254]; Postdoctoral Program of the University of Granada FX The data of AERONET Sun photometry used here are available at http://aeronet.gsfc.nasa.gov/. Radiosondes and microwave radiometers data are available in ARM data archive at http://www.archive.arm.gov/armlogin/login.jsp. Finally, GPS data used are available through SOUMINET webpage at http://www.suominet.ucar.edu/data/index.html. We thank ARM program for providing microwave radiometry and radiosonde data. We also are thankful to SOUMINET network for providing GPS data. This work was supported by NASA/Goddard Space Flight Center, by the Spanish Ministry of Science and Technology through projects CGL2010-18782 and CSD2007-00067, by the Andalusian Regional Government through projects P10-RNM-6299 and P08-RNM-3568, by EU through ACTRIS project (EU INFRA-2010-1.1.16-262254), and by the Postdoctoral Program of the University of Granada. NR 72 TC 17 Z9 17 U1 0 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 16 PY 2014 VL 119 IS 15 BP 9596 EP 9613 DI 10.1002/2014JD021730 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AO2ZK UT WOS:000341197400025 ER PT J AU Baek, KH Kim, JH Park, RJ Chance, K Kurosu, TP AF Baek, K. H. Kim, Jae H. Park, Rokjin J. Chance, Kelly Kurosu, Thomas P. TI Validation of OMI HCHO data and its analysis over Asia SO SCIENCE OF THE TOTAL ENVIRONMENT LA English DT Article DE OMI HCHO; EOF; SVD; Megacity pollution; Biomass burning ID ISOPRENE EMISSIONS; SATELLITE-OBSERVATIONS; COLUMN OBSERVATIONS; NORTH-AMERICA; FORMALDEHYDE; VARIABILITY; SPACE; AIR; OZONE; CHEMISTRY AB OMI HCHO is validated over the continental US (CONUS), and used to analyze regional sources in Northeast Asia (NA) and Southeast Asia (SA). OMI HCHO Version 2.0 data show unrealistic trends, which prompted the production of a corrected OMI HCHO data set. EOF and SVD are utilized to compare the spatial and temporal variability between OMI HCHO against GOME and SCIAMACHY, and against GEOS-Chem. CONUS HCHO chemistry is well studied; its concentrations are greatest in the southeastern US with annual cycle maximums corresponding to the summer vegetation. The corrected OMI HCHO agrees with this understanding as well as with the other sensors measurements and has no unrealistic trends. In NA the annual cycle is super-posed by extremely large concentrations in polluted mega-cities. The other sensors generally agree with NA's OMI HCHO regional distribution, but megacity signal is not seen in GEOS-Chem. Our study supports the findings proposed by others that the emission inventory used in GEOS-Chem significantly underestimates anthropogenic influence on HCHO emission over megacities. The persistent mega-city signal is also present in SA. In SA the spatial and temporal patterns of OMI HCHO show a maximum in the dry season. The patterns are in remarkably good agreement with fire counts, which illustrates that the variability of HCHO over SA is strongly influenced by biomass burning. The corrected OMI HCHO data has realistic trends, conforms to well-known sources over CONUS, and has shown a stationary large concentration over polluted Asian mega-cities, and a widespread biomass burning in SA. (C) 2014 Elsevier B.V. All rights reserved. C1 [Baek, K. H.; Kim, Jae H.] Pusan Natl Univ, Dept Atmospher Sci, Pusan, South Korea. [Park, Rokjin J.] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea. [Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Kurosu, Thomas P.] CA Inst Technol, Jet Prop Lab, Pasadena, CA USA. RP Kim, JH (reprint author), Pusan Natl Univ, Dept Atoms Sci, Room 525-1, Pusan, South Korea. EM jaekim@pusan.ac.kr RI Chem, GEOS/C-5595-2014; Park, Rokjin/I-5055-2012; OI Park, Rokjin/0000-0001-8922-0234; Chance, Kelly/0000-0002-7339-7577 FU National Research Foundation of Korea (NRF) - Ministry of Education, Science and Technology [2012R1A1A2040757] FX This research was supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science and Technology (2012R1A1A2040757). NR 44 TC 0 Z9 0 U1 2 U2 19 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0048-9697 EI 1879-1026 J9 SCI TOTAL ENVIRON JI Sci. Total Environ. PD AUG 15 PY 2014 VL 490 BP 93 EP 105 DI 10.1016/j.scitotenv.2014.04.108 PG 13 WC Environmental Sciences SC Environmental Sciences & Ecology GA AY0NT UT WOS:000347293800011 PM 24840284 ER PT J AU Dietrich, JP Van Gaest, AL Strickland, SA Hutchinson, GP Krupkin, AB Arkoosh, MR AF Dietrich, Joseph P. Van Gaest, Ahna L. Strickland, Stacy A. Hutchinson, Greg P. Krupkin, Alex B. Arkoosh, Mary R. TI Toxicity of PHOS-CHEK LC-95A and 259F fire retardants to ocean- and stream-type Chinook salmon and their potential to recover before seawater entry SO SCIENCE OF THE TOTAL ENVIRONMENT LA English DT Article DE Salmon; Wildfire; Toxicity; PHOS-CHEK; Smoltification; Fire retardant ID TROUT ONCORHYNCHUS-MYKISS; EARLY-LIFE STAGES; RAINBOW-TROUT; SMOLT TRANSFORMATION; CHEMICALS; AMMONIA; PARR; EXPOSURE; SMOLTIFICATION; TSHAWYTSCHA AB Long-termfire retardants are used to prevent the spread ofwildland fire, but have inadvertently entered aquatic habitats and resulted in fish kills. Weexamined the toxicity of two fire retardant products; PHOS-CHEK 259F and LC-95A, on Chinook salmon with two different life histories, ocean-type and stream-type, at different stages of their development. Ocean-type Chinook outmigrate to the ocean as subyearlings; while, stream-type salmon overwinter in freshwater and outmigrate as yearlings. Ocean-type and stream-type salmon were exposed to the fire retardants prior to their parr to smolt transition (presmolts) as subyearlings (stream-type and oceantype) and yearlings (stream-type only), as well as during their transition (smolts). The salmon were exposed to eight concentrations of each retardant and a control for 96 h to determine acute toxicity. Lethal concentration curves were modeled by logistic regression for each life history and life stage exposed to the two fire retardants. Among all life histories and life stages tested, PHOS-CHEK 259F was most toxic to stream-type salmon at smolt stage and PHOS-CHEK LC-95A was most toxic to ocean-type salmon at smolt stage. To determine the delayed effects of product exposures on fish health as well as for the potential of recovery, 24-hour seawater challenges were performed immediately after fire retardant exposure, as well as after a recovery period. Previous PHOSCHEK exposure reduced survival during seawater challenge among salmon from both life histories undergoing the parr-smolt transition and was more pronounced after PHOS-CHEK LC-95A exposure. However, this delayed effect was not observed 34 or more days after either PHOS-CHEK exposure. We conclude that accidental PHOSCHEK LC-95A or 259F drops during salmon outmigration would have adverse impacts that extend beyond the acute mortality that occurs within the immediate drop and dilution areas. Published by Elsevier B.V. C1 [Dietrich, Joseph P.; Van Gaest, Ahna L.; Strickland, Stacy A.; Hutchinson, Greg P.; Krupkin, Alex B.; Arkoosh, Mary R.] NOAA, Environm & Fisheries Sci Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Dietrich, JP (reprint author), 2032 SE OSU Dr, Newport, OR 97365 USA. EM joseph.dietrich@noaa.gov; vangaest@gmail.com; sas70@me.com; hutching@onid.orst.edu; krupkinalex@gmail.com; mary.arkoosh@noaa.gov FU U.S. Department of Agriculture-Forest Service Wildland Fire Chemical Systems Program [10-IA-11130206-046] FX We are sincerely grateful for the technical efforts of Deborah Boylen and the animal care assistance provided by Kalle Applegate, Lauren Arkoosh, Stacie Farwell, Athena Jackson, and Alice McKinstry. We also appreciate the insights provided by Edward E. Little, U.S. Geological Survey-CERC, Columbia, Missouri. The present study was financially supported by the U.S. Department of Agriculture (# 10-IA-11130206-046)-Forest Service Wildland Fire Chemical Systems Program. NR 37 TC 1 Z9 1 U1 5 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0048-9697 EI 1879-1026 J9 SCI TOTAL ENVIRON JI Sci. Total Environ. PD AUG 15 PY 2014 VL 490 BP 610 EP 621 DI 10.1016/j.scitotenv.2014.05.038 PG 12 WC Environmental Sciences SC Environmental Sciences & Ecology GA AY0NT UT WOS:000347293800065 PM 24880550 ER PT J AU Robertson, FR Bosilovich, MG Roberts, JB Reichle, RH Adler, R Ricciardulli, L Berg, W Huffman, GJ AF Robertson, F. R. Bosilovich, M. G. Roberts, J. B. Reichle, R. H. Adler, R. Ricciardulli, L. Berg, W. Huffman, G. J. TI Consistency of Estimated Global Water Cycle Variations over the Satellite Era SO JOURNAL OF CLIMATE LA English DT Article ID PACIFIC DECADAL VARIABILITY; CLIMATOLOGY PROJECT GPCP; DATA ASSIMILATION SYSTEM; SEA-SURFACE TEMPERATURE; LAND-SURFACE; PRECIPITATION PATTERNS; ATMOSPHERIC MOISTURE; HYDROLOGICAL CYCLE; HEAT FLUXES; WIND-SPEED AB Motivated by the question of whether recent interannual to decadal climate variability and a possible "climate shift" may have affected the global water balance, we examine precipitation minus evaporation (P - E) variability integrated over the global oceans and global land for the period 1979-2010 from three points of view-remotely sensed retrievals and syntheses over the oceans, reanalysis vertically integrated moisture flux convergence (VMFC) over land, and land surface models (LSMs) forced with observations-based precipitation, radiation, and near-surface meteorology. Over land, reanalysis VMFC and P - evapotranspiration (ET) from observationally forced LSMs agree on interannual variations (e.g., El Nino/La Nina events); however, reanalyses exhibit upward VMFC trends 3-4 times larger than P - ET trends of the LSMs. Experiments with other reanalyses using reduced observations show that upward VMFC trends in the full reanalyses are due largely to observing system changes interacting with assimilation model physics. The much smaller P - ET trend in the LSMs appears due to changes in frequency and amplitude of warm events after the 1997/98 El Nino, a result consistent with coolness in the eastern tropical Pacific sea surface temperature (SST) after that date. When integrated over the global oceans, E and especially P variations show consistent signals of El Nino/La Nina events. However, at scales longer than interannual there is considerable uncertainty especially in E. This results from differences among datasets in near-surface atmospheric specific humidity and wind speed used in bulk aerodynamic retrievals. The P variations, all relying substantially on passive microwave retrievals over ocean, also have uncertainties in decadal variability, but to a smaller degree. C1 [Robertson, F. R.; Roberts, J. B.] NASA, Earth Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Bosilovich, M. G.; Reichle, R. H.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Adler, R.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Ricciardulli, L.] Remote Sensing Syst, Santa Rosa, CA USA. [Berg, W.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Huffman, G. J.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA. RP Robertson, FR (reprint author), NASA, Earth Sci Off, Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM pete.robertson@nasa.gov RI Reichle, Rolf/E-1419-2012; Huffman, George/F-4494-2014; Bosilovich, Michael/F-8175-2012 OI Huffman, George/0000-0003-3858-8308; FU NASA Energy and Water Cycle Study (NEWS) FX The NASA Energy and Water Cycle Study (NEWS), Dr. Jared Entin, program manager, provided funding for this work. NEWS has been instrumental in encouraging cross-collaborative interactions both internal and external to the investigator team. The authors gratefully acknowledge discussions with numerous individuals, both data providers and users, whose suggestions and clarifications have added substantially to the paper. These include Chung-Lin Shie and Matt Rodell, NASA Goddard Space Flight Center; Lisan Yu and Carol Anne Clayson, Woods Hole Oceanographic Institution; Carl Mears and Kyle Hilburn of Remote Sensing Systems, Inc.; and Martin Jung and Markus Reichstein, Max Plank Institute for Biogeochemistry. The comments of three anonymous reviewers added significantly to this manuscript. NR 90 TC 8 Z9 8 U1 0 U2 20 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD AUG 15 PY 2014 VL 27 IS 16 BP 6135 EP 6154 DI 10.1175/JCLI-D-13-00384.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN0YV UT WOS:000340310800003 ER PT J AU Westphal, AJ Stroud, RM Bechtel, HA Brenker, FE Butterworth, AL Flynn, GJ Frank, DR Gainsforth, Z Hillier, JK Postberg, F Simionovici, AS Sterken, VJ Nittler, LR Allen, C Anderson, D Ansari, A Bajt, S Bastien, RK Bassim, N Bridges, J Brownlee, DE Burchell, M Burghammer, M Changela, H Cloetens, P Davis, AM Doll, R Floss, C Gruen, E Heck, PR Hoppe, P Hudson, B Huth, J Kearsley, A King, AJ Lai, B Leitner, J Lemelle, L Leonard, A Leroux, H Lettieri, R Marchant, W Ogliore, R Ong, WJ Price, MC Sandford, SA Tresseras, JAS Schmitz, S Schoonjans, T Schreiber, K Silversmit, G Sole, VA Srama, R Stadermann, F Stephan, T Stodolna, J Sutton, S Trieloff, M Tsou, P Tyliszczak, T Vekemans, B Vincze, L Von Korff, J Wordsworth, N Zevin, D Zolensky, ME AF Westphal, Andrew J. Stroud, Rhonda M. Bechtel, Hans A. Brenker, Frank E. Butterworth, Anna L. Flynn, George J. Frank, David R. Gainsforth, Zack Hillier, Jon K. Postberg, Frank Simionovici, Alexandre S. Sterken, Veerle J. Nittler, Larry R. Allen, Carlton Anderson, David Ansari, Asna Bajt, Sasa Bastien, Ron K. Bassim, Nabil Bridges, John Brownlee, Donald E. Burchell, Mark Burghammer, Manfred Changela, Hitesh Cloetens, Peter Davis, Andrew M. Doll, Ryan Floss, Christine Gruen, Eberhard Heck, Philipp R. Hoppe, Peter Hudson, Bruce Huth, Joachim Kearsley, Anton King, Ashley J. Lai, Barry Leitner, Jan Lemelle, Laurence Leonard, Ariel Leroux, Hugues Lettieri, Robert Marchant, William Ogliore, Ryan Ong, Wei Jia Price, Mark C. Sandford, Scott A. Tresseras, Juan-Angel Sans Schmitz, Sylvia Schoonjans, Tom Schreiber, Kate Silversmit, Geert Sole, Vicente A. Srama, Ralf Stadermann, Frank Stephan, Thomas Stodolna, Julien Sutton, Stephen Trieloff, Mario Tsou, Peter Tyliszczak, Tolek Vekemans, Bart Vincze, Laszlo Von Korff, Joshua Wordsworth, Naomi Zevin, Daniel Zolensky, Michael E. CA 30714 Stardust Home Dusters TI Evidence for interstellar origin of seven dust particles collected by the Stardust spacecraft SO SCIENCE LA English DT Article ID COMET 81P/WILD 2; SOLAR-SYSTEM; INTERPLANETARY DUST; SIZE DISTRIBUTION; GRAINS; IMPACTS; AEROGEL; EVENTS; WILD-2; RETURN AB Seven particles captured by the Stardust Interstellar Dust Collector and returned to Earth for laboratory analysis have features consistent with an origin in the contemporary interstellar dust stream. More than 50 spacecraft debris particles were also identified. The interstellar dust candidates are readily distinguished from debris impacts on the basis of elemental composition and/or impact trajectory. The seven candidate interstellar particles are diverse in elemental composition, crystal structure, and size. The presence of crystalline grains and multiple iron-bearing phases, including sulfide, in some particles indicates that individual interstellar particles diverge from any one representative model of interstellar dust inferred from astronomical observations and theory. C1 [Westphal, Andrew J.; Butterworth, Anna L.; Gainsforth, Zack; Anderson, David; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stroud, Rhonda M.; Bassim, Nabil] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA. [Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA. [Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Geosci Inst, D-60054 Frankfurt, Germany. [Flynn, George J.] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA. [Frank, David R.; Bastien, Ron K.] NASA Johnson Space Ctr JSC, Jacobs Technol ESCG, Houston, TX USA. [Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, D-69115 Heidelberg, Germany. [Simionovici, Alexandre S.] Observ Sci Univers Grenoble, Inst Sci Terre, Grenoble, France. [Sterken, Veerle J.] Univ Stuttgart, Inst Raumfahrtsyst IRS, D-70174 Stuttgart, Germany. [Sterken, Veerle J.] TU Braunschweig, IGEP, Braunschweig, Germany. [Sterken, Veerle J.; Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Sterken, Veerle J.; Heck, Philipp R.] Int Space Sci Inst, Bern, Switzerland. [Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA. [Allen, Carlton; Zolensky, Michael E.] NASA JSC, Houston, TX USA. [Ansari, Asna] Field Museum Nat Hist, Chicago, IL 60605 USA. [Bajt, Sasa] DESY, Hamburg, Germany. [Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England. [Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury, Kent, England. [Burghammer, Manfred; Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium. [Changela, Hitesh] Univ New Mexico, Albuquerque, NM 87131 USA. [Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] ESRF, Grenoble, France. [Davis, Andrew M.; King, Ashley J.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA. [Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Jia; Schreiber, Kate; Stadermann, Frank] Washington Univ, St Louis, MO USA. [Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany. [Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England. [Lai, Barry; Sutton, Stephen] Argonne Natl Lab, Adv Photon Source, Lemont, IL USA. [Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France. [Leroux, Hugues] Univ Lille 1, F-59655 Villeneuve Dascq, France. [Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Srama, Ralf] Univ Stuttgart, IRS, D-70174 Stuttgart, Germany. [Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Wordsworth, Naomi] Wexbury, Stoke Poges, Bucks, England. RP Westphal, AJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM westphal@ssl.berkeley.edu RI Sans Tresserras, Juan Angel/J-9362-2014; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015; Bajt, Sasa/G-2228-2010; Stroud, Rhonda/C-5503-2008; OI Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner, Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X; Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943 FU NASA [NNX09AC36G, NNX09AC63G, NNH11AQ61I, NNX11AC21G, NNX11AE15G]; Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy (DOE) [DE-AC02-05CH11231]; U.S. DOE, Office of Science, Office of Basic Energy Sciences [DE-AC02-98CH10886]; U.S. DOE [DE-AC02-06CH11357]; Klaus Tschira foundation; Tawani Foundation; Science and Technology Facilities Council (UK); German Science Foundation (DFG) [SPP1385]; Funds for Scientific Research (FWO), Flanders, Belgium [G.0395.11, G.0257.12N, G.0C12.13] FX We are deeply grateful to the Stardust@home dusters (list at http://stardustathome.ssl.berkeley.edu/sciencedusters), whose tremendous efforts were critically important to the success of this project. The ISPE consortium gratefully acknowledges the NASA Discovery Program for Stardust, the fourth NASA Discovery mission. NASA grants supported the following authors: NNX09AC36G-A.J.W., A. L. B., Z.G., R. L., D.Z., W. M., and J.V.K.; NNX09AC63G-C.F., R. D., A. L., W.J.O., K. S., and F.J.S.; NNH11AQ61I-R.M.S., H. C. G., and N.D.B.; NNX11AC21G-A.M.D., A.J.K., and T. S.; NNX11AE15G-G.J.F. The Advanced Light Source and the National Center for Electron Microscopy are supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy (DOE) under contract no. DE-AC02-05CH11231. Use of the National Synchrotron Light Source, Brookhaven National Laboratory, was supported by the U.S. DOE, Office of Science, Office of Basic Energy Sciences, under contract no. DE-AC02-98CH10886. Use of the Advanced Photon Source, an Office of Science User Facility operated for the U. S. DOE Office of Science by Argonne National Laboratory, was supported by the U.S. DOE under contract no. DE-AC02-06CH11357. M. T. and F. P. acknowledge support by Klaus Tschira foundation. A. A. and P. R. H. were supported by the Tawani Foundation. M.J.B. and M. C. P. are supported by Science and Technology Facilities Council (UK). F. E. B., J.K.H., P. H., J.L., F. P., S. S., R. S., and M. T. were supported by funding of the German Science Foundation (DFG) within SPP1385: the first ten million years of the solar system-a planetary materials approach. The ESRF ID13 measurements were performed in the framework of ESRF LTP EC337, with financial support by the Funds for Scientific Research (FWO), Flanders, Belgium (contract nr. G.0395.11, G.0257.12N and Big Science program G.0C12.13). G. Silversmit was postdoctoral fellow of the FWO during the ISPE investigations. Data presented in this paper are described in the supplementary materials and in references (9-20). NR 43 TC 39 Z9 39 U1 5 U2 67 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD AUG 15 PY 2014 VL 345 IS 6198 BP 786 EP 791 DI 10.1126/science.1252496 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AN4XM UT WOS:000340593100038 PM 25124433 ER PT J AU Mpagazehe, JN Street, KW Delgado, IR Higgs, CF AF Mpagazehe, Jeremiah N. Street, Kenneth W., Jr. Delgado, Irebert R. Higgs, C. Fred, III TI An experimental study of lunar dust erosive wear potential using the JSC-1AF lunar dust simulant SO WEAR LA English DT Article DE Erosive wear; Lunar dust; Optical performance; Particle advection ID SHAPE AB The exhaust plumes from spacecraft landing on Earth's moon advect lunar dust particles which have been shown to erode, or "sandblast", nearby objects. Evidence of this phenomenon was provided by NASA's Apollo 12 mission during which exhaust ejecta, generated by the Apollo Lunar Module landing, erosively wore components of the Surveyor III lunar probe located 155 m from the Apollo 12 landing site. Recently, interest in new lunar missions has been expressed by a number of different groups including countries and private companies. With the potential for a large number of new lunar landings in relatively close proximity to each other and existing lunar hardware, efforts must be taken to understand the damage that lunar dust particle erosion can cause to material surfaces. In this work, a study was conducted with the JSC-1AF lunar dust simulant to understand the erosive potential of lunar dust. Metallic and acrylic test specimens were exposed to erosive wear and the changes in mass, surface topography, transmittance, and reflectance are reported. It was observed that exposure to erosive wear from JSC-1AF, even at moderate velocities (approximately 105 m/s), resulted in a significant decrease in direct transmittance and total reflectance greater than 70% in some cases. The results in this study suggest that optical components, such as lenses and mirrors are highly susceptible to damage during lunar landings due to lunar dust particle impingement. (C) 2014 Elsevier B.V. All rights reserved. C1 [Mpagazehe, Jeremiah N.; Higgs, C. Fred, III] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA. [Street, Kenneth W., Jr.; Delgado, Irebert R.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Higgs, CF (reprint author), Carnegie Mellon Univ, 5000 Forbes Ave, Pittsburgh, PA 15213 USA. EM higgs@andrew.cmu.edu FU NASA Graduate Student Researchers (GSRP) Grant [NNX09AK96H]; Alfred P. Sloan Foundation FX The research in this work was supported by the NASA Graduate Student Researchers (GSRP) Grant (NNX09AK96H). Additional funding for this work was supplied by the Alfred P. Sloan Foundation. The authors are very grateful to Jim Gaier (NASA Glenn Research Center) for his consultation during the preparation of this manuscript. We also sincerely thank Philip Metzger (NASA Kennedy Space Center) for helpful and insightful discussions regarding this research. The authors would also like to gratefully acknowledge, Richard Mondry Jr. (Gilcrest Electric and Supply Co.) for his help constructing the experimental rig on which the tests were performed. We are sincerely grateful to Michelle Mrdenovich (Sierra Lobo Inc.), Laura Evans (NASA Glenn Research Center), and Joy Buehler (Vantage Partners, LLC) for their substantial assistance with SEM imaging, EDX analysis, and sample preparation. NR 24 TC 1 Z9 1 U1 3 U2 7 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0043-1648 J9 WEAR JI Wear PD AUG 15 PY 2014 VL 316 IS 1-2 BP 79 EP 91 DI 10.1016/j.wear.2014.04.018 PG 13 WC Engineering, Mechanical; Materials Science, Multidisciplinary SC Engineering; Materials Science GA AK7JX UT WOS:000338605700009 ER PT J AU Dynys, FW Sayir, A Mackey, J Sehirlioglu, A AF Dynys, F. W. Sayir, A. Mackey, J. Sehirlioglu, A. TI Thermoelectric properties of WSi2-SixGe1-x composites SO JOURNAL OF ALLOYS AND COMPOUNDS LA English DT Article DE Thermoelectric materials; Microstructure; Crystal growth; Composite materials; Electrical transport ID GE-SI ALLOYS; THERMAL CONDUCTIVITY; DIRECTIONAL SOLIDIFICATION; HIGH TEMPERATURES; SOLID-SOLUTIONS; FLASH METHOD; SILICIDE; DIFFUSIVITY; NUCLEATION; GROWTH AB Thermoelectric properties of the W/Si/Ge alloy system have been investigated with varying concentration levels of germanium and tungsten. The alloys were fabricated by directional solidification with the Bridgman method using boron nitride and fused silica crucibles. The effect of crucible contamination was investigated and found to result in doping the system to suitable levels for thermoelectric applications. The system has been demonstrated as a suitable high temperature p-type thermoelectric material exhibiting high power factors, >3000 mu W/m K-2. Seebeck coefficients of the system are on the order of +300 mu V/K and electrical conductivities of 2.8 x 10(4) S/m at the optimum operating temperature. The best composition, 0.9 at% W/9.3 at% Ge, achieved a figure of merit comparable to RTG values over the temperature range of interest. The results suggest that W addition can reduce the use of expensive Ge component of the alloy. Reported are the details of processing conditions, microstructure development, and temperature dependent thermoelectric properties. The material system was stable at the temperatures required for NASA's radioisotope thermoelectric generators. (C) 2014 Elsevier B.V. All rights reserved. C1 [Dynys, F. W.; Sayir, A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Mackey, J.] Univ Akron, Dept Mech Engn, Akron, OH 44325 USA. [Sehirlioglu, A.] Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA. RP Mackey, J (reprint author), Univ Akron, Dept Mech Engn, Akron, OH 44325 USA. EM jam151@zips.uakron.edu OI Mackey, Jonathan/0000-0003-1053-7007 FU NASA [NNX08AB43A]; AFOSR [FA9550-09-1-0312] FX The work was funded through NASA cooperative agreement NNX08AB43A. Alp Sehirlioglu acknowledges AFOSR FA9550-09-1-0312. The authors would like to thank Thomas Sabo and Raymond Babuder for their assistance with the experimental portion of the work. NR 38 TC 8 Z9 8 U1 1 U2 60 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-8388 EI 1873-4669 J9 J ALLOY COMPD JI J. Alloy. Compd. PD AUG 15 PY 2014 VL 604 BP 196 EP 203 DI 10.1016/j.jallcom.2014.03.133 PG 8 WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering GA AG6CH UT WOS:000335505600029 ER PT J AU Gandhiraman, RP Nordlund, D Javier, C Koehne, JE Chen, B Meyyappan, M AF Gandhiraman, Ram P. Nordlund, Dennis Javier, Cristina Koehne, Jessica E. Chen, Bin Meyyappan, M. TI X-ray Absorption Study of Graphene Oxide and Transition Metal Oxide Nanocomposites SO JOURNAL OF PHYSICAL CHEMISTRY C LA English DT Article ID INNER-SHELL EXCITATION; FINE-STRUCTURE SPECTRA; LITHIUM ION BATTERIES; ELECTROPHORETIC DEPOSITION; ELECTROCHEMICAL CAPACITORS; SUPERCAPACITOR ELECTRODES; THIN-FILM; SPECTROSCOPY; ENERGY; PERFORMANCE AB The surface properties of the electrode materials play a crucial role in determining the performance and efficiency of energy storage devices. Graphene oxide and nanostructures of 3d transition metal oxides were synthesized for construction of electrodes in supercapacitors, and the electronic structure and oxidation states were probed using near-edge X-ray absorption fine structure. Understanding the chemistry of graphene oxide would provide valuable insight into its reactivity and properties as the graphene oxide transformation to reduced-graphene oxide is a key step in the synthesis of the electrode materials. Polarized behavior of the synchrotron X-rays and the angular dependency of the near-edge X-ray absorption fine structures (NEXAFS) have been utilized to study the orientation of the sigma and pi bonds of the graphene oxide and graphene oxide-metal oxide nanocomposites. The core-level transitions of individual metal oxides and that of the graphene oxide nanocomposite showed that the interaction of graphene oxide with the metal oxide nanostructures has not altered the electronic structure of either of them. As the restoration of the pi network is important for good electrical conductivity, the C K edge NEXAFS spectra of reduced graphene oxide nanocomposites confirms the same through increased intensity of the sp(2)-derived unoccupied states pi* band. A pronounced angular dependency of the reduced sample and the formation of excitonic peaks confirmed the formation of extended conjugated network. C1 [Gandhiraman, Ram P.; Javier, Cristina; Koehne, Jessica E.; Chen, Bin; Meyyappan, M.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. [Nordlund, Dennis] Stanford Linear Accelerator Ctr, Stanford Synchrotron Radiat Lightsource, Menlo Pk, CA 94025 USA. RP Gandhiraman, RP (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA. EM ramprasad.gandhiraman@nasa.gov RI Gandhiraman, Ram Prasad/B-7004-2013; Nordlund, Dennis/A-8902-2008 OI Gandhiraman, Ram Prasad/0000-0001-8957-7938; Nordlund, Dennis/0000-0001-9524-6908 FU U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-76SF00515]; DOE Office of Biological and Environmental Research; National Institutes of Health, National Institute of General Medical Sciences [P41GM103393] FX R.P.G. is with Universities Space Research Association subcontracted to NASA Ames Research Center under NASA cooperative agreement. The beam time for synchrotron measurements was awarded to the authors through the peer-reviewed SLAC research proposal No. 2163. Use of the Stanford Synchrotron Radiation Lightsource, SLAC National Accelerator Laboratory, is supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences under Contract No. DE-AC02-76SF00515. The SSRL Structural Molecular Biology Program is supported by the DOE Office of Biological and Environmental Research and by the National Institutes of Health, National Institute of General Medical Sciences (including P41GM103393). The contents of this publication are solely the responsibility of the authors and do not necessarily represent the official views of NIGMS or NIH. NR 58 TC 7 Z9 7 U1 6 U2 56 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1932-7447 J9 J PHYS CHEM C JI J. Phys. Chem. C PD AUG 14 PY 2014 VL 118 IS 32 BP 18706 EP 18712 DI 10.1021/jp503941t PG 7 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA AN2VQ UT WOS:000340444500051 PM 25152800 ER PT J AU Galeazzi, M Chiao, M Collier, MR Cravens, T Koutroumpa, D Kuntz, KD Lallement, R Lepri, ST McCammon, D Morgan, K Porter, FS Robertson, IP Snowden, SL Thomas, NE Uprety, Y Ursino, E Walsh, BM AF Galeazzi, M. Chiao, M. Collier, M. R. Cravens, T. Koutroumpa, D. Kuntz, K. D. Lallement, R. Lepri, S. T. McCammon, D. Morgan, K. Porter, F. S. Robertson, I. P. Snowden, S. L. Thomas, N. E. Uprety, Y. Ursino, E. Walsh, B. M. TI The origin of the local 1/4-keV X-ray flux in both charge exchange and a hot bubble SO NATURE LA English DT Article ID SOLAR-WIND; BACKGROUND FLUX; EMISSION; GAS; INFERENCES; MODEL AB The solar neighbourhood is the closest and most easily studied sample of the Galactic interstellar medium, an understanding of which is essential for models of star formation and galaxy evolution. Observations of an unexpectedly intense diffuse flux of easily absorbed 1/4-kiloelectronvolt X-rays(1,2), coupled with the discovery that interstellar space within about a hundred parsecs of the Sun is almost completely devoid of cool absorbing gas(3), led to a picture of a 'local cavity' filled with X-ray-emitting hot gas, dubbed the local hot bubble(4-6). This model was recently challenged by suggestions that the emission could instead be readily produced within the Solar System by heavy solar-wind ions exchanging electrons with neutral H and He in interplanetary space(7-11), potentially removing the major piece of evidence for the local existence of million-degree gas within the Galactic disk(12-15). Here we report observations showing that the total solar-wind charge-exchange contribution is approximately 40 per cent of the 1/4-keV flux in the Galactic plane. The fact that the measured flux is not dominated by charge exchange supports the notion of a million-degree hot bubble extending about a hundred parsecs from the Sun. C1 [Galeazzi, M.; Uprety, Y.; Ursino, E.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. [Chiao, M.; Collier, M. R.; Porter, F. S.; Snowden, S. L.; Thomas, N. E.; Walsh, B. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cravens, T.; Robertson, I. P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Koutroumpa, D.] Univ Paris 06, Sorbonne Univ, Univ Versailles St Quentin, CNRS,INSU,LATMOS IPSL, F-78280 Guyancourt, France. [Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Lallement, R.] Univ Paris Diderot, GEPI Observ Paris, CNRS, UMR 8111, F-92190 Meudon, France. [Lepri, S. T.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [McCammon, D.; Morgan, K.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. RP Galeazzi, M (reprint author), Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. EM galeazzi@physics.miami.edu RI Uprety, Youaraj/C-8104-2015; Porter, Frederick/D-3501-2012; Walsh, Brian/C-4899-2016; Morgan, Kelsey/J-5053-2016; Collier, Michael/I-4864-2013 OI Uprety, Youaraj/0000-0001-9101-2063; Porter, Frederick/0000-0002-6374-1119; Walsh, Brian/0000-0001-7426-5413; Morgan, Kelsey/0000-0002-6597-1030; Collier, Michael/0000-0001-9658-6605 FU NASA [NNX11AF04G, NNX09AF09G]; French space agency CNES; National Program 'Physique Chimie du Milieu Interstellaire' of the Institut National des Sciences de l'Univers (INSU) FX We thank the personnel at NASA's Wallops Flight Facility and the White Sands Military Range for their support of payload development, integration and launch, and the technical personnel at the University of Miami, NASA's Goddard Space Flight Center and the University of Michigan for their support of the instrument's development. This work was supported by NASA award numbers NNX11AF04G and NNX09AF09G. D.K. and R.L. acknowledge financial support for their activity through the programme 'Soleil Heliosphere Magnetosphere' of the French space agency CNES, and the National Program 'Physique Chimie du Milieu Interstellaire' of the Institut National des Sciences de l'Univers (INSU). M.C. and N.E.T. are employed through the Center for Research and Exploration in Space Science and Technology (CRESST) and the University of Maryland, Baltimore County, Baltimore, Maryland, USA. NR 24 TC 21 Z9 21 U1 0 U2 10 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD AUG 14 PY 2014 VL 512 IS 7513 BP 171 EP + DI 10.1038/nature13525 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM9KO UT WOS:000340200700026 PM 25079321 ER PT J AU Thompson, MS Christoffersen, R Zega, TJ Keller, LP AF Thompson, Michelle S. Christoffersen, Roy Zega, Thomas J. Keller, Lindsay P. TI Microchemical and structural evidence for space weathering in soils from asteroid Itokawa SO EARTH PLANETS AND SPACE LA English DT Article DE Hayabusa; Itokawa; Space weathering; Irradiation; Micrometeorite impact; Airless body; Transmission electron microscopy; Sample return analysis ID BEAM-INDUCED AMORPHIZATION; LUNAR REGOLITH; DUST PARTICLES; VAPOR DEPOSITS; IRRADIATION; MGO-AL2O3-SIO2; CHONDRITES; INSIGHTS; SURFACE; SAMPLES AB Here we report microchemical and microstructural features indicative of space weathering in a particle returned from the surface of asteroid Itokawa by the Hayabusa mission. Space weathering features include partially and completely amorphous rims, chemically and structurally heterogeneous multilayer rims, amorphous surface islands, vesiculated rim textures, and nanophase iron particles. Solar-wind irradiation is likely responsible for the amorphization as well as the associated vesiculation of grain rims. The multilayer rims contain a nanocrystalline outer layer that is underlain by an amorphous inner layer, and both have compositions that are distinct from the underlying, crystalline orthopyroxene grain. The multilayer rim features could be derived from either radiation-induced sputter deposition or vapor deposition from micrometeorite impact events. The amorphous islands on grain surfaces have a distinctive morphology and composition suggesting that they represent surface deposits of melt derived from micrometeorite impact events. These observations indicate that both irradiation damage and micrometeorite impacts play a role in surface modification and space weathering on asteroid Itokawa. C1 [Thompson, Michelle S.; Zega, Thomas J.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Christoffersen, Roy] NASA, Lyndon B Johnson Space Ctr, Mail Code KR, Houston, TX 77058 USA. [Keller, Lindsay P.] NASA, JSC Mail Code KR, Houston, TX 77058 USA. RP Thompson, MS (reprint author), Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA. EM mst@lpl.arizona.edu FU NASA Laboratory Analysis of Returned Samples (LARS) program; Natural Sciences and Engineering Research Council of Canada (NSERC); NASA FX We thank JAXA for the allocation of Hayabusa samples for this study. We gratefully acknowledge the use of facilities within the Leroy Eyring Center for Solid State Science at Arizona State University. We acknowledge the use of facilities and assistance from Huikai Cheng at FEI. The TEM work at the Johnson Space Center was supported in part by a grant to LPK from the NASA Laboratory Analysis of Returned Samples (LARS) program. Funding for MS Thompson is provided by the Natural Sciences and Engineering Research Council of Canada (NSERC). This research was supported in part by NASA. Three anonymous reviewers are acknowledged for their constructive comments. NR 31 TC 11 Z9 11 U1 2 U2 8 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1880-5981 J9 EARTH PLANETS SPACE JI Earth Planets Space PD AUG 13 PY 2014 VL 66 AR 89 DI 10.1186/1880-5981-66-89 PG 10 WC Geosciences, Multidisciplinary SC Geology GA AQ9UW UT WOS:000343203500001 ER PT J AU Klebanoff, LE Breit, J Roe, GS Damberger, T Erbel, T Wingert, S Coleman, B Radley, CJ Oros, JM Schuttinger, P Woolley, R Ghotb, H Prey, S Velinsky, S White, W Saunders, R Saunders, C Drake, R Rea, G Fliess, D Hooson, R Elrick, WT Hamilton, J Skradski, T Brown, G Chao, B Zelinsky, M Sorkin, A McGlaughlin, R Moreland, G Hanley, RC Koonce, M Johnson, TA AF Klebanoff, L. E. Breit, Js. Roe, G. S. Damberger, T. Erbel, T. Wingert, S. Coleman, B. Radley, C. J. Oros, J. M. Schuttinger, P. Woolley, R. Ghotb, H. Prey, S. Velinsky, S. White, W. Saunders, R. Saunders, C. Drake, R. Rea, G. Fliess, D. Hooson, R. Elrick, W. T. Hamilton, J. Skradski, T. Brown, G. Chao, B. Zelinsky, M. Sorkin, A. McGlaughlin, R. Moreland, G. Hanley, R. C. Koonce, M. Johnson, T. A. TI Fuel cell mobile lighting: A fuel cell market transformation project SO INTERNATIONAL JOURNAL OF HYDROGEN ENERGY LA English DT Article DE Fuel cell; Market transformation; Mobile lighting; Construction equipment; Ground support equipment AB We report the results of a project aimed to introduce proton exchange membrane (PEM) hydrogen fuel cell technology into aviation ground support equipment (GSE) and rental construction equipment. The purpose of the project was to design, build, field-test and then commercialize fuel cell equipment that is superior to its diesel counterpart. The commercializing of this hydrogen-based technology will help to start the process of displacing diesel fuel use in aviation GSE and in mobile construction equipment. We describe a hydrogen fuel cell mobile lighting tower (H2LT) that combines hydrogen stored as a high pressure gas, PEM fuel cell technology, and advanced lighting into a single unit with uses in aviation and construction. We assembled a project team of 15 institutional partners combining new technology expertise (hydrogen, fuel cells), equipment mass manufacturing capability (mobile light towers, lighting) and influential end-users to field test the H2LT in real-world use in diverse environments. Seed funding provided by Boeing enabled additional funding from the U.S. Department of Energy (DOE) and a preponderance of in-kind contributions from the industrial partners. Prototype units were constructed and field tested in the entertainment industry, at the San Francisco International Airport, at the NASA Kennedy Space Center, with the California Department of Transportation (Caltrans), and with the Connecticut Department of Transportation. The goals of these approximately year-long field tests were to assess operation of the H2LT technology in a wide variety of potentially corrosive environments (cold, wet, hot, humid, salty air) performing a wide variety of tasks, to reduce diesel emissions at these locations, and to help promote hydrogen PEM technology in new influential markets. The H2LT proved to be exceptionally durable in these diverse environments, demonstrating the compatibility of PEM fuel cells and high-pressure hydrogen storage with the construction equipment application. Results from the field tests are discussed, including system performance (efficiency, duration, durability) and the efficacy of refueling the system by different methods (H-2 stations, mobile refueling). The H2LT system is compared directly to a comparable diesel-fueled light tower with regard to size, performance and emissions savings. Overall, end users were pleased with the performance of the H2LT, noting the lack of emissions and exceptionally low noise level. Recommendations for improvement were also collected and will be discussed. Two types of lighting used on the H2LT (plasma, LED) were characterized by U.C. Davis in collaboration with Caltrans. LED lighting was found to be the most energy efficient and robust lighting technology for the highly mobile H2LT application. The technical "lessons-learned" are reviewed, along with the plans for commercialization of the H2LT technology by Multiquip Inc. Finally, the benefits to the industrial participants of the project organization are described. Copyright (C) 2014, Hydrogen Energy Publications, LLC. Published by Elsevier Ltd. All rights reserved. C1 [Klebanoff, L. E.; Johnson, T. A.] Sandia Natl Labs, Livermore, CA 94551 USA. [Breit, Js.; Roe, G. S.] Boeing Commercial Airplanes, Syst Concept Ctr, Everett, WA 98203 USA. [Damberger, T.] Golden State Energy, Carson City, NV 89703 USA. [Erbel, T.; Wingert, S.; Coleman, B.] Multiquip Inc, Carson, CA 90746 USA. [Radley, C. J.; Oros, J. M.; Schuttinger, P.] Altergy Syst, Folsom, CA 95630 USA. [Woolley, R.; Ghotb, H.; Prey, S.] Caltrans Div Res, Innovat & Syst Informat Technol Applicat Off, Irvine, CA 92612 USA. [Velinsky, S.; White, W.] Univ Calif Davis, Dept Mech & Aerosp Engn, Davis, CA 95616 USA. [Saunders, R.; Saunders, C.] Saunders Elect Inc, Arleta, CA 91331 USA. [Drake, R.; Rea, G.] Stray Light Opt Technol Inc, Scottsburg, IN 47170 USA. [Fliess, D.; Hooson, R.] San Francisco Int Airport, City & Cty San Francisco, San Francisco, CA 94128 USA. [Elrick, W. T.; Hamilton, J.] Calif Fuel Cell Partnership, West Sacramento, CA 95691 USA. [Skradski, T.] Lumenworks, Oakland, CA 94610 USA. [Brown, G.] Luxirn Corp, Santa Clara, CA 95054 USA. [Chao, B.; Zelinsky, M.] Ovon Hydrogen Syst, Rochester Hills, MI 48309 USA. [Sorkin, A.; McGlaughlin, R.] NASA, TEERM Principal Ctr, Kennedy Space Ctr, FL 32899 USA. [Moreland, G.] SRA Int, Latham, NY USA. [Hanley, R. C.] Connecticut Dept Transportat, Newington, CT 06131 USA. [Koonce, M.] IGX Grp Inc, San Francisco, CA 94102 USA. RP Klebanoff, LE (reprint author), Sandia Natl Labs, POB 969,MS 9161,7011 East Ave, Livermore, CA 94551 USA. EM lekleba@sandia.gov FU Boeing Company [SC02/1651.14.00]; Fuel Cell Market Transformation Program at the U.S. DOE Fuel Cell Technologies Office; DOE; Division of Research and Innovation at Caltrans (under the direction of Larry Orcutt); U.C. Davis AHMCT; NASA KSC; U.S. Department of Energy's National Nuclear Security Administration [DE-AC04-94AL85000] FX Partial funding from the Boeing Company is gratefully acknowledged via the Boeing/Sandia CRADA SC02/1651.14.00. Funding from the Fuel Cell Market Transformation Program (led by Pete Devlin) at the U.S. DOE Fuel Cell Technologies Office was critical, making the broader and stronger development project possible, and specifically allowing the construction and field testing of five additional H2LT units. In addition to funding, we appreciate the encouragement of Pete and his colleagues Nancy Garland and John Christensen in the Market Transformation program. Special thanks to Sunita Satyapal at DOE for supporting this work. The authors thank Tien Nguyen of DOE for providing an analysis of GHG emissions for the H2LT technology, with the hydrogen derived from either steam reforming of natural gas, or wind-based electrolysis of water.; The project would not have been successful without the participation of Caltrans. We thank Randy Iwasaki, former director of Caltrans, for providing wonderful encouragement and support of the work in its early phases, and offering resources of the Division of Research and Innovation at Caltrans (under the direction of Larry Orcutt) to be applied in support of the project. Larry Orcutt directed Nancy Chinlund of Caltrans to become involved. Nancy was very proactive in launching the project from a Caltrans perspective, which led directly to Randy Woolley's involvement in the project. The Caltrans partners aggressively challenged the project to build a prototype in a few months' time to be shown at the 2009 AASHTO meeting.; Caltrans provided considerable in-kind support through the donation of its own technical expertise and through its support of the U.C. Davis AHMCT for characterizing the lighting options for the H2LT as well as supervising the Caltrans District 3 field test. We acknowledge the contributions of Gonzalo Gomez of Caltrans for discussions of lighting technology options for the H2LT. Ben Creed, Lauren Miller, Sean Donohoe and Matt Jones at U.C. Davis provided many hours of night work characterizing the illumination provided by the candidate plasma, LED and MH lighting options. In a related activity, Ty Larson of Boeing performed checks that the glass covering the plasma lights was sufficiently absorbing UV radiation, which was very helpful.; The staff at Saunders Electric, including Ron Brewer, Frank Soggiu and Pat Hess were instrumental in the 3-year field tests of the Alpha and Beta H2LT units used for the Los Angeles entertainment award shows and elsewhere in the entertainment industry.; The field test of the unit at the NASA KSC was an excellent example of cooperation between government agencies. We thank Chuck Griffin for providing local supervision of the project from the NASA KSC end, along with a lot of help from Melissa Clevenger of the propellants group and Ray Davis from operations. The KSC staff were extremely professional and helpful. We thank Pattie Lewis Burford (ITB Inc.) and Jerry Curran (EASI) for providing corrosion inspection of the Beta unit that was field tested at the NASA KSC for a year, and Randy Morris for extensive coordination.; Sandia National Laboratories is a multi-program laboratory managed and operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Corporation, for the U.S. Department of Energy's National Nuclear Security Administration under contract DE-AC04-94AL85000. NR 9 TC 3 Z9 3 U1 0 U2 23 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0360-3199 EI 1879-3487 J9 INT J HYDROGEN ENERG JI Int. J. Hydrog. Energy PD AUG 13 PY 2014 VL 39 IS 24 BP 12948 EP 12972 DI 10.1016/j.ijhydene.2014.05.180 PG 25 WC Chemistry, Physical; Electrochemistry; Energy & Fuels SC Chemistry; Electrochemistry; Energy & Fuels GA AN6FI UT WOS:000340689900058 ER PT J AU Tucker, PG DeBonis, JR AF Tucker, P. G. DeBonis, J. R. TI Aerodynamics, computers and the environment SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Editorial Material DE large eddy simulation; aerodynamics; turbulence C1 [Tucker, P. G.] Univ Cambridge, Dept Engn, Cambridge CB2 1PZ, England. [DeBonis, J. R.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Tucker, PG (reprint author), Univ Cambridge, Dept Engn, Cambridge CB2 1PZ, England. EM pgt23@cam.ac.uk NR 16 TC 3 Z9 3 U1 1 U2 12 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-503X EI 1471-2962 J9 PHILOS T R SOC A JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci. PD AUG 13 PY 2014 VL 372 IS 2022 SI SI AR 20130331 DI 10.1098/rsta.2013.0331 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AL0VJ UT WOS:000338844700013 PM 25024420 ER PT J AU Vitale, S Congedo, G Dolesi, R Ferroni, V Hueller, M Vetrugno, D Weber, WJ Audley, H Danzmann, K Diepholz, I Hewitson, M Korsakova, N Ferraioli, L Gibert, F Karnesis, N Nofrarias, M Inchauspe, H Plagnol, E Jennrich, O McNamara, PW Armano, M Thorpe, JI Wass, P AF Vitale, Stefano Congedo, Giuseppe Dolesi, Rita Ferroni, Valerio Hueller, Mauro Vetrugno, Daniele Weber, William Joseph Audley, Heather Danzmann, Karsten Diepholz, Ingo Hewitson, Martin Korsakova, Natalia Ferraioli, Luigi Gibert, Ferran Karnesis, Nikolaos Nofrarias, Miquel Inchauspe, Henri Plagnol, Eric Jennrich, Oliver McNamara, Paul W. Armano, Michele Thorpe, James Ira Wass, Peter TI Data series subtraction with unknown and unmodeled background noise SO PHYSICAL REVIEW D LA English DT Article AB LISA Pathfinder (LPF), the precursor mission to a gravitational wave observatory of the European Space Agency, will measure the degree to which two test masses can be put into free fall, aiming to demonstrate a suppression of disturbance forces corresponding to a residual relative acceleration with a power spectral density (PSD) below (30 fm/s(2)/root Hz)(2) around 1 mHz. In LPF data analysis, the disturbance forces are obtained as the difference between the acceleration data and a linear combination of other measured data series. In many circumstances, the coefficients for this linear combination are obtained by fitting these data series to the acceleration, and the disturbance forces appear then as the data series of the residuals of the fit. Thus the background noise or, more precisely, its PSD, whose knowledge is needed to build up the likelihood function in ordinary maximum likelihood fitting, is here unknown, and its estimate constitutes instead one of the goals of the fit. In this paper we present a fitting method that does not require the knowledge of the PSD of the background noise. The method is based on the analytical marginalization of the posterior parameter probability density with respect to the background noise PSD, and returns an estimate both for the fitting parameters and for the PSD. We show that both these estimates are unbiased, and that, when using averaged Welch's periodograms for the residuals, the estimate of the PSD is consistent, as its error tends to zero with the inverse square root of the number of averaged periodograms. Additionally, we find that the method is equivalent to some implementations of iteratively reweighted least-squares fitting. We have tested the method both on simulated data of known PSD and on data from several experiments performed with the LISA Pathfinder end-to-end mission simulator. C1 [Vitale, Stefano; Congedo, Giuseppe; Dolesi, Rita; Ferroni, Valerio; Hueller, Mauro; Vetrugno, Daniele; Weber, William Joseph] Univ Trento, Dept Phys, I-38123 Povo, Trento, Italy. [Vitale, Stefano; Congedo, Giuseppe; Dolesi, Rita; Ferroni, Valerio; Hueller, Mauro; Vetrugno, Daniele; Weber, William Joseph] Ist Nazl Fis Nucl, Trento Inst Fundamental Phys & Applicat, I-38123 Povo, Trento, Italy. [Audley, Heather; Danzmann, Karsten; Diepholz, Ingo; Hewitson, Martin; Korsakova, Natalia] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Audley, Heather; Danzmann, Karsten; Diepholz, Ingo; Hewitson, Martin; Korsakova, Natalia] Leibniz Univ Hannover, D-30167 Hannover, Germany. [Ferraioli, Luigi] ETH, Inst Geophys, CH-8092 Zurich, Switzerland. [Gibert, Ferran; Karnesis, Nikolaos; Nofrarias, Miquel] CSIC IEEC, Fac Ciencies, Inst Ciencies Espai, Bellaterra 08193, Spain. [Inchauspe, Henri; Plagnol, Eric] Univ Paris Diderot, APC, CNRS IN2P3, CEA Ifru,Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France. [Jennrich, Oliver; McNamara, Paul W.] European Space Agcy, European Space Technol Ctr, NL-2200 AG Noordwijk, Netherlands. [Armano, Michele] European Space Agcy, European Space Astron Ctr, Madrid 28692, Spain. [Thorpe, James Ira] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA. [Wass, Peter] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, High Energy Phys Grp, London SW7 2AZ, England. RP Vitale, S (reprint author), Univ Trento, Dept Phys, I-38123 Povo, Trento, Italy. EM stefano.vitale@unitn.it RI Weber, William/H-4351-2012; Vitale, Stefano/C-2312-2012; Nofrarias, Miquel/N-6249-2015; Wass, Peter/C-5767-2017 OI Weber, William/0000-0003-1536-2410; Vitale, Stefano/0000-0002-2427-8918; Nofrarias, Miquel/0000-0003-1518-2196; Wass, Peter/0000-0002-2945-399X FU Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare; Deutsches Zentrum fur Luft- und Raumfahrt e.V.; Swiss Space Office; State Secretariat for Education, Research and Innovation; United Kingdom Space Agency; Plan Nacional del Espacio of the Spanish Ministry of Science and Innovation; Centre Nationale d'Etudes Spatiales FX This work has been supported in part under contracts from Agenzia Spaziale Italiana, Istituto Nazionale di Fisica Nucleare, Deutsches Zentrum fur Luft- und Raumfahrt e.V., Swiss Space Office, State Secretariat for Education, Research and Innovation, United Kingdom Space Agency, Plan Nacional del Espacio of the Spanish Ministry of Science and Innovation, and Centre Nationale d'Etudes Spatiales. NR 18 TC 8 Z9 8 U1 1 U2 13 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD AUG 11 PY 2014 VL 90 IS 4 AR 042003 DI 10.1103/PhysRevD.90.042003 PG 15 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AO3SG UT WOS:000341255200001 ER PT J AU Pierens, A Raymond, SN AF Pierens, A. Raymond, S. N. TI Disruption of co-orbital (1:1) planetary resonances during gas-driven orbital migration SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; hydrodynamics; methods: numerical; planets and satellites: formation; planet-disc interactions ID MEAN-MOTION RESONANCES; TRANSITING EXTRASOLAR PLANETS; OUTWARD MIGRATION; PROTOSTELLAR DISC; TROJAN PLANETS; SUPER-EARTHS; SYSTEMS; PROTOPLANETS; NEBULA; MASS AB Planets close to their stars are thought to form farther out and migrate inwards due to angular momentum exchange with gaseous protoplanetary discs. This process can produce systems of planets in co-orbital (Trojan or 1:1) resonance, in which two planets share the same orbit, usually separated by 60 deg. Co-orbital systems are detectable among the planetary systems found by the Kepler mission either directly or by transit timing variations. However, no co-orbital systems have been found within the thousands of Kepler planets and candidates. Here, we study the orbital evolution of co-orbital planets embedded in a protoplanetary disc using a grid-based hydrodynamics code. We show that pairs of similar-mass planets in co-orbital resonance are disrupted during large-scale orbital migration. Destabilization occurs when one or both planets are near the critical mass needed to open a gap in the gaseous disc. A confined gap is opened that spans the 60 deg azimuthal separation between planets. This alters the torques imparted by the disc on each planet - pushing the leading planet outwards and the trailing planet inwards - and disrupts the resonance. The mechanism applies to systems in which the two planets' masses differ by a factor of 2 or less. In a simple flared disc model, the critical mass for gap opening varies from a few Earth masses at the inner edge of the disc to 1 Saturn mass at 5 au. A pair of co-orbital planets with masses in this range that migrates will enter a region where the planets are at the gap-opening limit. At that point, the resonance is disrupted. We therefore predict an absence of planets on co-orbital configurations with masses in the super-Earth to Saturn mass range with similar masses. C1 [Pierens, A.; Raymond, S. N.] Univ Bordeaux, Observ Aquitain Sci Univers, F-33271 Floirac, France. [Pierens, A.; Raymond, S. N.] CNRS, Lab Astrophys Bordeaux, F-33271 Floirac, France. [Raymond, S. N.] NASA, Astrobiol Inst, Virtual Planetary Lab, Washington, DC USA. RP Pierens, A (reprint author), Univ Bordeaux, Observ Aquitain Sci Univers, F-BP89, F-33271 Floirac, France. EM arnaud.pierens@obs.u-bordeaux1.fr FU Agence Nationale pour la Recherche [ANR-13-BS05-0003]; NASA [NNA13AA93A] FX Computer time for this study was provided by the computing facilities MCIA (Mesocentre de Calcul Intensif Aquitain) of the Universite de Bordeaux and by HPC resources of Cines under the allocation c2013046957 made by GENCI (Grand Equipement National de Calcul Intensif). We thank the Agence Nationale pour la Recherche under grant ANR-13-BS05-0003 (MOJO). SNR's contribution was performed as part of the NASA Astrobiology Institute's Virtual Planetary Laboratory Lead Team, supported by the NASA under Cooperative Agreement no. NNA13AA93A. NR 51 TC 3 Z9 3 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 11 PY 2014 VL 442 IS 3 BP 2296 EP 2303 DI 10.1093/mnras/stu1008 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5TU UT WOS:000339924300030 ER PT J AU Pretorius, ML Mukai, K AF Pretorius, Magaretha L. Mukai, Koji TI Constraints on the space density of intermediate polars from the Swift-BAT survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: observational; methods: statistical; novae; cataclysmic variables; X-rays: binaries ID MAGNETIC CATACLYSMIC VARIABLES; ALPHA-SELECTED SAMPLE; PALOMAR-GREEN SAMPLE; X-RAY BINARIES; TV-COLUMBAE; SYSTEM PARAMETERS; ACCRETION RATE; HST PARALLAX; PQ-GEMINORUM; DONOR STARS AB We construct a complete, hard X-ray flux-limited sample of intermediate polars (IPs) from the Swift-BAT 70-month survey, by imposing selection cuts in flux and Galactic latitude (F-X > 2.5 x 10(- 11) erg cm(- 2) s(- 1) at 14-195 keV, and |b| > 5A degrees). We then use it to estimate the space density (rho) of IPs. Assuming that this sample of 15 long-period systems is representative of the intrinsic IP population, the space density of long-period IPs is 1-(+1)(0.5) x 10(-7) pc(-3). The Swift-BAT data also allow us to place upper limits on the size of a hypothetical population of faint IPs that is not included in the flux-limited sample. While most IPs detected by Swift-BAT have 14-195 keV luminosities of similar to 10(33) erg s(-1), there is evidence of a fainter population at L-X similar to 10(31) erg s(- 1). We find that a population of IPs with this luminosity may have a space density as large as 5 x 10(-6) pc(-3). Furthermore, these low-luminosity IPs, despite appearing rare in observed samples, are probably at least as intrinsically common as the brighter systems that are better represented in the known IP sample. C1 [Pretorius, Magaretha L.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Mukai, Koji] CRESST, Greenbelt, MD 20771 USA. [Mukai, Koji] NASA, Xray Astrophys Lab, GSFC, Greenbelt, MD 20771 USA. [Mukai, Koji] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. RP Pretorius, ML (reprint author), Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. EM retha.pretorius@astro.ox.ac.uk FU Marie Curie International Incoming Fellowship [PIIF-GA-2012-328716] FX MLP is funded by a Marie Curie International Incoming Fellowship within the 7th European Community Framework Programme (grant no. PIIF-GA-2012-328716). NR 64 TC 13 Z9 13 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 11 PY 2014 VL 442 IS 3 BP 2580 EP 2585 DI 10.1093/mnras/stu990 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5TU UT WOS:000339924300052 ER PT J AU Walker, ES Mazzali, PA Pian, E Hurley, K Arcavi, I Cenko, SB Gal-Yam, A Horesh, A Kasliwal, M Poznanski, D Silverman, JM Sullivan, M Bloom, JS Filippenko, AV Kulkarni, SR Nugent, PE Ofek, E Barthelmy, S Boynton, W Goldsten, J Golenetskii, S Ohno, M Tashiro, MS Yamaoka, K Zhang, XL AF Walker, E. S. Mazzali, P. A. Pian, E. Hurley, K. Arcavi, I. Cenko, S. B. Gal-Yam, A. Horesh, A. Kasliwal, M. Poznanski, D. Silverman, J. M. Sullivan, M. Bloom, J. S. Filippenko, A. V. Kulkarni, S. R. Nugent, P. E. Ofek, E. Barthelmy, S. Boynton, W. Goldsten, J. Golenetskii, S. Ohno, M. Tashiro, M. S. Yamaoka, K. Zhang, X. L. TI Optical follow-up observations of PTF10qts, a luminous broad-lined Type Ic supernova found by the Palomar Transient Factory SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; supernovae: individual: PTF10qts ID GAMMA-RAY BURST; CORE-COLLAPSE SUPERNOVAE; LIGHT-CURVE; SN 1998BW; LOW-METALLICITY; DWARF GALAXIES; GRB 100316D; HYPERNOVA; GRB-031203; PHOTOMETRY AB We present optical photometry and spectroscopy of the broad-lined Type Ic supernova (SN Ic-BL) PTF10qts, which was discovered as part of the Palomar Transient Factory. The SN was located in a dwarf galaxy of magnitude r = 21.1 at a redshift z = 0.0907. We find that the R-band light curve is a poor proxy for bolometric data and use photometric and spectroscopic data to construct and constrain the bolometric light curve. The derived bolometric magnitude at maximum light is M-bol = -18.51 +/- 0.2 mag, comparable to that of SN 1998bw (M-bol = -18.7 mag) which was associated with a gamma-ray burst (GRB). PTF10qts is one of the most luminous SNe Ic-BL observed without an accompanying GRB. We estimate the physical parameters of the explosion using data from our programme of follow-up observations, finding that it produced a larger mass of radioactive nickel compared to other SNe Ic-BL with similar inferred ejecta masses and kinetic energies. The progenitor of the event was likely an similar to 20 M-aS (TM) star. C1 [Walker, E. S.; Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Walker, E. S.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Mazzali, P. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Mazzali, P. A.] INAF Padova Astron Observ, I-35122 Padua, Italy. [Mazzali, P. A.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Pian, E.] INAF IASF, I-40129 Bologna, Italy. [Pian, E.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Arcavi, I.; Gal-Yam, A.; Ofek, E.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Cenko, S. B.; Barthelmy, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cenko, S. B.; Bloom, J. S.; Filippenko, A. V.; Nugent, P. E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Horesh, A.; Kulkarni, S. R.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Kasliwal, M.] Carnegie Princeton Fellow, Pasadena, CA 91101 USA. [Poznanski, D.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Silverman, J. M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Sullivan, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Nugent, P. E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Boynton, W.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Goldsten, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Golenetskii, S.] Russian Acad Sci, Ioffe Physicotech Inst, St Petersburg 194021, Russia. [Ohno, M.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Tashiro, M. S.] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan. [Yamaoka, K.] Aoyama Gakuin Univ, Dept Phys & Math, Sagamihara, Kanagawa 2298558, Japan. [Zhang, X. L.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Walker, ES (reprint author), Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy. EM emma.walker@yale.edu RI Golenetskii, Sergey/B-3818-2015; Horesh, Assaf/O-9873-2016; OI Horesh, Assaf/0000-0002-5936-1156; Sullivan, Mark/0000-0001-9053-4820; Pian, Elena/0000-0001-8646-4858 FU ASI [I/016/07/0 (COFIS), I/088/06/0]; PRIN INAF; Minerva grant; ISF; BSF; GIF; EU [307260]; Gary and Cynthia Bengier; Christopher R. Redlich Fund; Richard and Rhoda Goldman Fund; TABASGO Foundation; NSF [AST-1211916, AST-1302771]; Israeli Ministry of Science; I-CORE programme of the Planning and Budgeting Committee; Israel Science Foundation [1829/12]; W.M. Keck Foundation; NASA [NNX10AI23G (Swift), NNX09AV61G (Suzaku), NNX09AU03G (Fermi), NNX09AR28G (INTEGRAL)] FX We acknowledge financial contributions from contract ASI I/016/07/0 (COFIS), ASI I/088/06/0, and PRIN INAF 2009 and 2011. PTF is a collaboration of Caltech, LCOGT, the Weizmann Institute, LBNL, Oxford, Columbia, IPAC, and UC Berkeley. Collaborative work between AG and PAM is supported by a Minerva grant. The Weizmann PTF membership is supported by the ISF via grants to AG. Joint work of AG and SRK is supported by a BSF grant. AG also acknowledges support by grants from the GIF, EU/FP7 via ERC grant 307260, 'The Quantum Universe', I-CORE programme by the Israeli Committee for planning and budgeting, the Kimmel award, and the Lord Sieff of Brimpton Fund. AVF's group at UC Berkeley has received generous financial assistance from Gary and Cynthia Bengier, the Christopher R. Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and NSF grant AST-1211916. JMS is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. EOO is incumbent of the Arye Dissentshik career development chair and is grateful to support by a grant from the Israeli Ministry of Science and the I-CORE programme of the Planning and Budgeting Committee and the Israel Science Foundation (grant No 1829/12).; We thank the very helpful staffs of the various observatories (Palomar, Lick, KNPO, TNG, Keck) at which data were obtained. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; it was made possible by the generous financial support of the W.M. Keck Foundation. M.T. Kandrashoff and J. Rex assisted with the Lick observations. We are grateful to the following contributors to the IPN for support and sharing their data: I. G. Mitrofanov, D. Golovin, M. L. Litvak, A. B. Sanin, C. Fellows, K. Harshman, and R. Starr (for the Odyssey team), R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and D. Svinkin (for the Konus-Wind team), A. von Kienlin and A. Rau (for the INTEGRAL team), T. Takahashi, M. Ohno, Y. Hanabata, Y. Fukazawa, M. Tashiro, Y. Terada, T. Murakami, and K. Makishima (for the Suzaku team), T. Cline, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer (for the Swift team), and V. Connaughton, M. S. Briggs, and C. Meegan (for the Fermi GBM team). KH acknowledges NASA support for the IPN under the following grants: NNX10AI23G (Swift), NNX09AV61G (Suzaku), NNX09AU03G (Fermi), and NNX09AR28G (INTEGRAL). NR 83 TC 7 Z9 7 U1 1 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 11 PY 2014 VL 442 IS 3 BP 2768 EP 2779 DI 10.1093/mnras/stu1017 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5TU UT WOS:000339924300067 ER PT J AU Cudjoe, E Nguyen, BN Meador, MAB Sandberg, A Rowan, SJ AF Cudjoe, Elvis Nguyen, Baochau N. Meador, Mary Ann B. Sandberg, Anna Rowan, Stuart J. TI Polyimide cellulose nanocrystal composite aerogels SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Cudjoe, Elvis; Rowan, Stuart J.] Case Western Reserve Univ, Cleveland, OH 44106 USA. [Meador, Mary Ann B.; Sandberg, Anna] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Nguyen, Baochau N.] NASA Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA. EM exc229@case.edu NR 0 TC 0 Z9 0 U1 3 U2 8 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 295-PMSE PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167404660 ER PT J AU Haskins, J Bennett, WR Hernandez-Lugo, DM Wu, J Borodin, O Monk, JD Bauschlicher, CW Lawson, J AF Haskins, Justin Bennett, William R. Hernandez-Lugo, Dione M. Wu, James Borodin, Oleg Monk, Joshua D. Bauschlicher, Charles W. Lawson, John TI Investigation of structure and transport in Li-doped ionic liquid electrolytes: [pyr14][TFSI], [pyr13][FSI], and [EMIM][BF4] SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Haskins, Justin; Monk, Joshua D.; Bauschlicher, Charles W.; Lawson, John] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bennett, William R.; Hernandez-Lugo, Dione M.; Wu, James] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Borodin, Oleg] US Army Res Lab, Adelphi, MD 20783 USA. EM justin.b.haskins@nasa.gov RI Borodin, Oleg/B-6855-2012 OI Borodin, Oleg/0000-0002-9428-5291 NR 0 TC 0 Z9 0 U1 1 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 629-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167404333 ER PT J AU Huang, XC Schwenke, DW Lee, TJ Tashkun, SA Gamache, RR Freedman, RS AF Huang, Xinchuan Schwenke, David W. Lee, Timothy J. Tashkun, Sergey A. Gamache, Robert R. Freedman, Richard S. TI Accurate infrared line lists computed for CO2 and SO2 isotopologues SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Huang, Xinchuan; Freedman, Richard S.] SETI Inst, Mountain View, CA 94043 USA. [Schwenke, David W.] NASA, Ames Res Ctr, NAS Facil, Moffett Field, CA 94035 USA. [Lee, Timothy J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Tashkun, Sergey A.] VE Zuev Inst Atmospher Opt, Tomsk 634021, Russia. [Gamache, Robert R.] Univ Massachusetts, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. EM xinchuan@gmail.com RI HUANG, XINCHUAN/A-3266-2013; Tashkun, Sergey/E-8682-2014 NR 0 TC 0 Z9 0 U1 0 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 256-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167403854 ER PT J AU Huang, XC Lee, TJ AF Huang, Xinchuan Lee, Timothy J. TI History of a theoretical spectroscopy package SPECTRO and its recent applications in astrophysical studies SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. [Huang, Xinchuan] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lee, Timothy J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. EM xinchuan@gmail.com RI HUANG, XINCHUAN/A-3266-2013 NR 0 TC 0 Z9 0 U1 0 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 472-COMP PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8JN UT WOS:000349165104675 ER PT J AU Hudson, R AF Hudson, Reggie TI Rise, fall, and fine print of Erlenmeyer's rule SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Hudson, Reggie] NASA Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD USA. EM reggie.hudson@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 5-HIST PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167400392 ER PT J AU Hudson, RL Gerakines, PA AF Hudson, Reggie L. Gerakines, Perry A. TI Radiolytic destruction of amino acids from Mars to the interstellar medium SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Hudson, Reggie L.; Gerakines, Perry A.] NASA, Goddard Space Flight Ctr, Astrochem Lab Code 691, Greenbelt, MD 20771 USA. EM reggie.hudson@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 219-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167403821 ER PT J AU Hui, AO Grieman, FJ Okumura, M Sander, SP AF Hui, Aileen O. Grieman, Frederick J. Okumura, Mitchio Sander, Stanley P. TI Laboratory experiments of HO2 reactions with peroxy radicals using infrared kinetic spectroscopy (IRKS) SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Hui, Aileen O.; Okumura, Mitchio] CALTECH, Dept Chem & Chem Engn, Pasadena, CA 91125 USA. [Grieman, Frederick J.] Pomona Coll, Dept Chem, Claremont, CA 91711 USA. [Hui, Aileen O.; Sander, Stanley P.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. EM aileenh@caltech.edu NR 4 TC 0 Z9 0 U1 2 U2 5 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 95-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167403700 ER PT J AU Liu, YD Zhang, JS Wang, LM Troy, T Ahmed, M AF Liu, Yingdi Zhang, Jingsong Wang, Liming Troy, Tyler Ahmed, Musahid TI Direct characterization of Criegee intermediate in ozonolysis reaction of alkene SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Liu, Yingdi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, Jingsong] Univ Calif Riverside, Riverside, CA 92521 USA. [Wang, Liming] S China Univ Technol, Sch Chem & Chem Engn, Guangzhou 510640, Guangdong, Peoples R China. [Troy, Tyler; Ahmed, Musahid] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Chem Sci, Berkeley, CA 94720 USA. EM yingdi@caltech.edu; jingsong.zhang@ucr.edu NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 41-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167403647 ER PT J AU Liu, YD Sander, SP AF Liu, Yingdi Sander, Stanley P. TI Pressure and temperature dependences of rate coefficients for the reaction OH + NO2 + M -> products SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Liu, Yingdi; Sander, Stanley P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM YINGDI@CALTECH.EDU NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 420-ENVR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8JN UT WOS:000349165105839 ER PT J AU Mathies, R Willis, P Lillis, R Amundson, R Beegle, K Butterworth, A Curtis, D Ehrenfreund, P Grunthaner, FA Hazen, R Kaiser, RI Kim, J Ludham, M Mora, M Scherer, J Stockton, A Turin, P Welten, K Williford, K AF Mathies, Richard Willis, Peter Lillis, Robert Amundson, Ronald Beegle, Kuther Butterworth, Anna Curtis, David Ehrenfreund, Pascale Grunthaner, Frank A. Hazen, Robert Kaiser, Ralf I. Kim, Jungkyu Ludham, Michael Mora, Maria Scherer, James Stockton, Amanda Turin, Paul Welten, Kees Williford, Kenneth TI Mars organic analyzer: Methods and instrumentation for detecting trace organic molecules in our solar system SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Mathies, Richard; Grunthaner, Frank A.; Scherer, James] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. [Willis, Peter; Beegle, Kuther; Mora, Maria; Stockton, Amanda; Williford, Kenneth] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lillis, Robert; Butterworth, Anna; Curtis, David; Ludham, Michael; Turin, Paul; Welten, Kees] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Amundson, Ronald] Univ Calif Berkeley, Dept Environm Sci, Berkeley, CA 94720 USA. [Ehrenfreund, Pascale] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA. [Hazen, Robert] Geophys Lab, Washington, DC 20052 USA. [Kaiser, Ralf I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. [Kim, Jungkyu] Texas Tech Univ, Dept Mech Engn, Lubbock, TX 79409 USA. EM ramathies@berkeley.edu RI Willis, Peter/I-6621-2012; Lillis, Robert/A-3281-2008 OI Lillis, Robert/0000-0003-0578-517X NR 0 TC 0 Z9 0 U1 2 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 104-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167403709 ER PT J AU Meador, MAB Guo, HQ Nguyen, B Williams, JC Vivod, SL AF Meador, Mary Ann B. Guo, Haiquan Baochau Nguyen Williams, Jarrod C. Vivod, Stephanie L. TI Recent advances in design of polymer aerogels for aerospace applications SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Meador, Mary Ann B.; Guo, Haiquan; Baochau Nguyen; Williams, Jarrod C.; Vivod, Stephanie L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM maryann.meador@nasa.gov NR 0 TC 0 Z9 0 U1 4 U2 8 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 617-PMSE PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167405103 ER PT J AU Meador, MA AF Meador, Michael A. TI Opportunities and challenges in nanomanufacturing for aerospace applications SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Meador, Michael A.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA. EM Michael.A.Meador@nasa.gov NR 0 TC 0 Z9 0 U1 1 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 32-POLY PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167405168 ER PT J AU Mertens, LA Okumura, M Sander, SP AF Mertens, Laura A. Okumura, Mitchio Sander, Stanley P. TI Temperature dependent branching ratios of HONO2 and HOONO from HOx and NOx cross reactions found using pulsed cavity-ringdown spectroscopy SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Mertens, Laura A.; Okumura, Mitchio] CALTECH, Pasadena, CA 91125 USA. [Sander, Stanley P.] NASA, Jet Prop Lab, Pasadena, CA 91125 USA. EM lmertens@caltech.edu NR 0 TC 0 Z9 0 U1 2 U2 5 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 468-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167404186 ER PT J AU Monk, J Lawson, JW Haskins, J Bauschlicher, C AF Monk, Joshua Lawson, John W. Haskins, Justin Bauschlicher, Charles TI Thermal and mechanical properties of cross-linked phenolic resins for thermal protection materials for space vehicles SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Monk, Joshua; Lawson, John W.; Haskins, Justin] NASA, Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA. [Bauschlicher, Charles] NASA, Ames Res Ctr, Entry Syst & Technol Div, Moffett Field, CA 94035 USA. EM joshua.d.monk@nasa.gov NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 477-COMP PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8JN UT WOS:000349165104680 ER PT J AU Parker, DSN Yang, T Kaiser, RI Troy, T Ahmed, M Lee, TJ AF Parker, Dorian S. N. Yang, Tao Kaiser, Ralf I. Troy, Tyler Ahmed, Musa Lee, Timothy J. TI On the formation of quinoline and the role of gas phase reactions in the synthesis of prebiotic molecules SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Parker, Dorian S. N.; Yang, Tao; Kaiser, Ralf I.] Univ Hawaii, Honolulu, HI 96816 USA. [Troy, Tyler; Ahmed, Musa] Adv Light Source LBNL, Berkeley, CA 94720 USA. [Lee, Timothy J.] NASA, Ames Res Ctr, Mountain View, CA USA. EM dparker3@hawaii.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 107-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167403712 ER PT J AU Pickering, K AF Pickering, Karen TI Water: A critical material enabling space exploration SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Pickering, Karen] NASA, Johnson Space Ctr, Dept Crew, Houston, TX 77058 USA. [Pickering, Karen] NASA, Johnson Space Ctr, Thermal Syst Div, Houston, TX 77058 USA. EM karen.d.pickering@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 155-ANYL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8JN UT WOS:000349165101604 ER PT J AU Rothschild, LJ Fujishima, K Paulino-LIma, I AF Rothschild, Lynn J. Fujishima, Kosuke Paulino-LIma, Ivan TI Synthetic biology and the search for extraterrestrial life SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Rothschild, Lynn J.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA. [Fujishima, Kosuke] Univ Calif Santa Cruz, Univ Affiliated Res Ctr, NASA Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA. [Paulino-LIma, Ivan] NASA, Ames Res Ctr, NPP, Div Earth Sci, Moffett Field, CA 94035 USA. EM Lynn.J.Rothschild@nasa.gov NR 0 TC 0 Z9 0 U1 1 U2 9 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 50-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167403656 ER PT J AU Schwenke, DW AF Schwenke, David W. TI Handy's harbinger SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Schwenke, David W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM david.w.schwenke@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 474-COMP PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8JN UT WOS:000349165104677 ER PT J AU Scott, VJ Manohara, H Toda, R Murthy, R Del Castillo, L AF Scott, Valerie J. Manohara, Harish Toda, Risaku Murthy, Rakesh Del Castillo, Linda TI Robust CNT field emitters: Growth and in situ welding on metal surfaces SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Scott, Valerie J.; Manohara, Harish; Toda, Risaku; Murthy, Rakesh; Del Castillo, Linda] CALTECH, Jet Prop Lab, Pasadena, CA 91108 USA. EM valerie.j.scott@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 98-IEC PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167400514 ER PT J AU Scott, VJ Amashukeli, X AF Scott, Valerie J. Amashukeli, Xenia TI RF-powered microreactor for efficient extraction and hydrolysis SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Scott, Valerie J.; Amashukeli, Xenia] CALTECH, Jet Prop Lab, Pasadena, CA USA. EM valerie.j.scott@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 11-ANYL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8JN UT WOS:000349165101469 ER PT J AU Simpson, WR Peterson, PK Nghiem, SV AF Simpson, William R. Peterson, Peter K. Nghiem, Son V. TI Vertical and horizontal gradients in bromine monoxide assist in understanding arctic halogen activation mechanisms SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Simpson, William R.; Peterson, Peter K.] Univ Alaska Fairbanks, Dept Chem & Biochem, Fairbanks, AK 99775 USA. [Simpson, William R.; Peterson, Peter K.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Nghiem, Son V.] CALTECH, Radar Sci & Engn Sect, Jet Prop Lab, Pasadena, CA 91109 USA. EM wrsimpson@alaska.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 92-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167403697 ER PT J AU Smith, KE Callahan, MP Gerakines, PA Dworkin, JP House, CH AF Smith, Karen E. Callahan, Michael P. Gerakines, Perry A. Dworkin, Jason P. House, Christopher H. TI Investigation of pyridine carboxylic acids in CM2 carbonaceous chondrites: Potential precursor molecules for ancient coenzymes SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Smith, Karen E.; House, Christopher H.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Smith, Karen E.; House, Christopher H.] Penn State Univ, Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA. [Smith, Karen E.] Oak Ridge Associated Univ, NASA Goddard Space Flight Ctr, Oak Ridge, TN 37831 USA. [Callahan, Michael P.; Gerakines, Perry A.; Dworkin, Jason P.] NASA Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. EM karen.e.smith@nasa.gov RI Dworkin, Jason/C-9417-2012 OI Dworkin, Jason/0000-0002-3961-8997 NR 0 TC 0 Z9 0 U1 1 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 120-ANYL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8JN UT WOS:000349165101571 ER PT J AU Templeton, PD Wagschal, K Paavola, CD Lee, CC AF Templeton, Paul D. Wagschal, Kurt Paavola, Chad D. Lee, Charles C. TI Lignocellulose hydrolysis by multienzyme complexes SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Templeton, Paul D.; Wagschal, Kurt; Lee, Charles C.] USDA ARS, Albany, CA 94710 USA. [Paavola, Chad D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM paul.templeton@ars.usda.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 68-BIOL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8JN UT WOS:000349165101875 ER PT J AU Vaidehi, N Jain, A Larsen, AB Wagner, JE Kandel, S Salomon-Ferrer, R AF Vaidehi, Nagarajan Jain, Abhinandan Larsen, Adrien B. Wagner, Jeffrey E. Kandel, Saugat Salomon-Ferrer, Romelia TI GNEIMO: An accurate internal coordinate molecular dynamics simulation method for studying biomolecular dynamics SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Vaidehi, Nagarajan; Larsen, Adrien B.; Wagner, Jeffrey E.; Kandel, Saugat; Salomon-Ferrer, Romelia] City Hope Natl Med Ctr, Beckman Res Inst, Dept Immunol, Duarte, CA 91010 USA. [Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM nvaidehi@coh.org NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 70-COMP PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8JN UT WOS:000349165104312 ER PT J AU Wang, LM Liu, YD Campos-Pineda, M Priest, C Zhang, JS AF Wang, Liming Liu, Yingdi Campos-Pineda, Mixtli Priest, Chad Zhang, Jingsong TI Studying ozonolysis reactions of 2-butenes using cavity ring-down spectroscopy SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Wang, Liming] S China Univ Technol, Sch Chem & Chem Engn, Guangzhou 510640, Guangdong, Peoples R China. [Liu, Yingdi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Campos-Pineda, Mixtli; Priest, Chad; Zhang, Jingsong] Univ Calif Riverside, Riverside, CA 92521 USA. EM yingdi@caltech.edu; jingsong.zhang@ucr.edu NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 576-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167404282 ER PT J AU Williams, JC Meador, MAB AF Williams, Jarrod C. Meador, Mary Ann B. TI Synthesis and properties of porous polyamide aerogels with flexible aliphatic segments SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Williams, Jarrod C.; Meador, Mary Ann B.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM jcwilli1@kent.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 623-PMSE PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8KC UT WOS:000349167405109 ER PT J AU Gatebe, C Kuznetsov, A Melnikova, I AF Gatebe, C. Kuznetsov, A. Melnikova, I. TI Cloud optical parameters from airborne observation of diffuse solar radiation accomplished in USA and USSR in different geographical regions SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID SPECTRAL MEASUREMENTS; ATMOSPHERE; OZONE; VARIABILITY; ECOSYSTEMS; ABSORPTION AB Cloud optical parameters (optical thickness, single scattering albedo, and ground albedo) are obtained from airborne experiments with NASA's Cloud Absorption Radiometer and analysed taking into account observational and processing uncertainties. The analytical approach of the inverse asymptotic formulas of the transfer theory, which uses observed values of solar diffuse radiance, is applied. The method is free from a priori restrictions and links put to desired parameters. The algorithms and first results of processing have been presented earlier. The first results, being the solution of the inverse problem, showed strong fluctuations in values, which required the regularization of the solution. The dependence of uncertainties of the result on viewing direction was revealed. Hence, here attention is focused on uncertainties of observation, angle function calculation, and processing approach, which is taken into account for result averaging, and the regularization procedure is described. Calculating the uncertainties of the processing approach is accomplished analytically using formulas for the retrieval of the optical parameters. The values of the desired parameters obtained in eight observational spectral channels above, below, and within the cloud - at 16 levels are presented. The final results are compared to the optical parameters of extended cloud layers obtained earlier using a similar method of inverse asymptotic formulas from spectral data of Russian aircraft solar irradiance measurements in different regions, made in the 1970s/1980s at Leningrad (now Saint Petersburg) University in the USSR. C1 [Gatebe, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kuznetsov, A.; Melnikova, I.] Russian State Hydrometeorol Univ, Atmospher Phys Dept, St Petersburg, Russia. RP Melnikova, I (reprint author), Russian State Hydrometeorol Univ, Atmospher Phys Dept, St Petersburg, Russia. EM irina.melnikova@pobox.spbu.ru RI Gatebe, Charles/G-7094-2011 OI Gatebe, Charles/0000-0001-9261-2239 NR 37 TC 3 Z9 4 U1 2 U2 4 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 EI 1366-5901 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD AUG 10 PY 2014 VL 35 IS 15 SI SI BP 5812 EP 5829 DI 10.1080/01431161.2014.945000 PG 18 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA AO8WU UT WOS:000341637000016 ER PT J AU Snowden, SL Chiao, M Collier, MR Porter, FS Thomas, NE Cravens, T Robertson, IP Galeazzi, M Uprety, Y Ursino, E Koutroumpa, D Kuntz, KD Lallement, R Puspitarini, L Lepri, ST McCammon, D Morgan, K Walsh, BM AF Snowden, S. L. Chiao, M. Collier, M. R. Porter, F. S. Thomas, N. E. Cravens, T. Robertson, I. P. Galeazzi, M. Uprety, Y. Ursino, E. Koutroumpa, D. Kuntz, K. D. Lallement, R. Puspitarini, L. Lepri, S. T. McCammon, D. Morgan, K. Walsh, B. M. TI PRESSURE EQUILIBRIUM BETWEEN THE LOCAL INTERSTELLAR CLOUDS AND THE LOCAL HOT BUBBLE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: bubbles; ISM: clouds; magnetic fields; solar neighborhood; X-rays: diffuse background; X-rays: ISM ID X-RAY-EMISSION; EXTREME-ULTRAVIOLET EMISSION; MAPS; GAS; SOLAR; ISM; ABUNDANCES; IONS; LINE; SUN AB Three recent results related to the heliosphere and the local interstellar medium (ISM) have provided an improved insight into the distribution and conditions of material in the solar neighborhood. These are the measurement of the magnetic field outside of the heliosphere by Voyager 1, the improved mapping of the three-dimensional structure of neutral material surrounding the Local Cavity using extensive ISM absorption line and reddening data, and a sounding rocket flight which observed the heliospheric helium focusing cone in X-rays and provided a robust estimate of the contribution of solar wind charge exchange emission to the ROSAT All-Sky Survey 1/4 keV band data. Combining these disparate results, we show that the thermal pressure of the plasma in the Local Hot Bubble (LHB) is P/k = 10,700 cm(-3) K. If the LHB is relatively free of a global magnetic field, it can easily be in pressure (thermal plus magnetic field) equilibrium with the local interstellar clouds, eliminating a long-standing discrepancy in models of the local ISM. C1 [Snowden, S. L.; Chiao, M.; Collier, M. R.; Porter, F. S.; Thomas, N. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cravens, T.; Robertson, I. P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Galeazzi, M.; Uprety, Y.; Ursino, E.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [Koutroumpa, D.] Univ Paris 06, Sorbonne Univ, Univ Versailles St Quentin, CNRS INSU,LATMOS IPSL, F-78280 Guyancourt, France. [Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Lallement, R.; Puspitarini, L.] Univ Paris Diderot, CNRS UMR8111, Observ Paris, GEPI, F-92190 Meudon, France. [Lepri, S. T.] Univ Michigan, Ann Arbor, MI 48109 USA. [McCammon, D.; Morgan, K.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Walsh, B. M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Snowden, SL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM steven.l.snowden@nasa.gov RI Porter, Frederick/D-3501-2012; Morgan, Kelsey/J-5053-2016; Collier, Michael/I-4864-2013 OI Porter, Frederick/0000-0002-6374-1119; Morgan, Kelsey/0000-0002-6597-1030; Collier, Michael/0000-0001-9658-6605 FU NASA's award [NNX11AF04G] FX We are grateful to Ed Jenkins for interesting and helpful insights into these results. This work has been supported in part by NASA's award #NNX11AF04G. NR 33 TC 7 Z9 7 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 10 PY 2014 VL 791 IS 1 AR L14 DI 10.1088/2041-8205/791/1/L14 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4JB UT WOS:000341302200015 ER PT J AU Walsh, C Juhasz, A Pinilla, P Harsono, D Mathews, GS Dent, WRF Hogerheijde, MR Birnstiel, T Meeus, G Nomura, H Aikawa, Y Millar, TJ Sandell, G AF Walsh, Catherine Juhasz, Attila Pinilla, Paola Harsono, Daniel Mathews, Geoffrey S. Dent, William R. F. Hogerheijde, Michiel R. Birnstiel, T. Meeus, Gwendolyn Nomura, Hideko Aikawa, Yuri Millar, T. J. Sandell, Goeran TI ALMA HINTS AT THE PRESENCE OF TWO COMPANIONS IN THE DISK AROUND HD 100546 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE protoplanetary disks; stars: formation; stars: individual (HD 100546); stars: pre-main sequence; submillimeter: planetary systems ID HERBIG AE/BE STARS; NEAR-INFRARED SPECTROSCOPY; CO EMISSION-LINES; PROTOPLANETARY DISKS; DIGIT SURVEY; TW-HYDRAE; WARM GAS; DUST; HD-100546; PLANET AB HD 100546 is a well-studied Herbig Be star-disk system that likely hosts a close-in companion with compelling observational evidence for an embedded protoplanet at 68 AU. We present Atacama Large Millimeter/Submillimeter Array observations of the HD 100546 disk which resolve the gas and dust structure at (sub) millimeter wavelengths. The CO emission (at 345.795 GHz) originates from an extensive molecular disk (390 +/- 20 AU in radius) whereas the continuum emission is more compact (230 +/- 20 AU in radius), suggesting radial drift of the millimeter-sized grains. The CO emission is similar in extent to scattered light images indicating well-mixed gas and micrometer-sized grains in the disk atmosphere. Assuming azimuthal symmetry, a single-component power-law model cannot reproduce the continuum visibilities. The visibilities and images are better reproduced by a double-component model: a compact ring with a width of 21 AU centered at 26 AU and an outer ring with a width of 75 +/- 3 AU centered at 190 +/- 3 AU. The influence of a companion and protoplanet on the dust evolution is investigated. The companion at 10 AU facilitates the accumulation of millimeter-sized grains within a compact ring, approximate to 20-30 AU, by approximate to 10 Myr. The injection of a protoplanet at 1 Myr hastens the ring formation (approximate to 1.2 Myr) and also triggers the development of an outer ring (approximate to 100-200 AU). These observations provide additional evidence for the presence of a close-in companion and hint at dynamical clearing by a protoplanet in the outer disk. C1 [Walsh, Catherine; Juhasz, Attila; Pinilla, Paola; Harsono, Daniel; Mathews, Geoffrey S.; Hogerheijde, Michiel R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Harsono, Daniel] SRON Netherlands Inst Space Res, SRON, NL-9700 AV Groningen, Netherlands. [Mathews, Geoffrey S.] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 USA. [Dent, William R. F.] Joint ALMA Observ JAO, Santiago, Chile. [Dent, William R. F.] European So Observ, Santiago 19, Chile. [Birnstiel, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Meeus, Gwendolyn] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, E-28049 Madrid, Spain. [Nomura, Hideko] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Aikawa, Yuri] Kobe Univ, Dept Earth & Planetary Sci, Nada Ku, Kobe, Hyogo 6578501, Japan. [Millar, T. J.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Sandell, Goeran] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. RP Walsh, C (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. OI Millar, Tom/0000-0001-5178-3656; Hogerheijde, Michiel/0000-0001-5217-537X; Birnstiel, Tilman/0000-0002-1899-8783 FU Netherlands Organisation for Scientific Research (NWO) [639.041.335]; EU A-ERC [291141]; KNAW; NASA Origins of Solar Systems [NNX12AJ04G]; STFC; Netherlands Organization for Scientific Research (NWO); European ALMA Regional Center node in the Netherlands FX This Letter makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00863. S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The authors thank E. F. van Dishoeck, C. P. Dullemond, N. van der Marel, and M. Schmalzl for useful discussions, and G. D. Mulders for sharing the results of his hydrodynamical simulations. C. W. acknowledges support from the Netherlands Organisation for Scientific Research (NWO, program number 639.041.335). This work was also supported by EU A-ERC grant 291141 CHEMPLAN and a KNAW prize. T. B. acknowledges support from NASA Origins of Solar Systems grant NNX12AJ04G. Astrophysics at QUB is supported by a grant from the STFC. M. R. H., A. J., and G. S. M. acknowledge support from the Netherlands Organization for Scientific Research (NWO) to Allegro, the European ALMA Regional Center node in the Netherlands. NR 44 TC 35 Z9 35 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 10 PY 2014 VL 791 IS 1 AR L6 DI 10.1088/2041-8205/791/1/L6 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4JB UT WOS:000341302200006 ER PT J AU Bodaghee, A Tomsick, JA Krivonos, R Stern, D Bauer, FE Fornasini, FM Barriere, N Boggs, SE Christensen, FE Craig, WW Gotthelf, EV Hailey, CJ Harrison, FA Hong, J Mori, K Zhang, WW AF Bodaghee, Arash Tomsick, John A. Krivonos, Roman Stern, Daniel Bauer, Franz E. Fornasini, Francesca M. Barriere, Nicolas Boggs, Steven E. Christensen, Finn E. Craig, William W. Gotthelf, Eric V. Hailey, Charles J. Harrison, Fiona A. Hong, Jaesub Mori, Kaya Zhang, William W. TI INITIAL RESULTS FROM NuSTAR OBSERVATIONS OF THE NORMA ARM SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; novae, cataclysmic variables; stars: neutron; X-rays: binaries ID MAGNETIC CATACLYSMIC VARIABLES; X-RAY SURVEY; GALACTIC-CENTER; STAR-FORMATION; CATALOG; COMPLEX AB Results are presented for an initial survey of the Norma Arm gathered with the focusing hard X-Ray Telescope NuSTAR. The survey covers 0.2 deg(2) of sky area in the 3-79 keV range with a minimum and maximum raw depth of 15 ks and 135 ks, respectively. Besides a bright black-hole X-ray binary in outburst (4U 1630-47) and a new X-ray transient (NuSTAR J163433-473841), NuSTAR locates three sources from the Chandra survey of this region whose spectra are extended above 10 keV for the first time: CXOU J163329.5-473332, CXOU J163350.9-474638, and CXOU J163355.1-473804. Imaging, timing, and spectral data from a broad X-ray range (0.3-79 keV) are analyzed and interpreted with the aim of classifying these objects. CXOU J163329.5-473332 is either a cataclysmic variable or a faint low-mass X-ray binary. CXOU J163350.9-474638 varies in intensity on year-long timescales, and with no multi-wavelength counterpart, it could be a distant X-ray binary or possibly a magnetar. CXOU J163355.1-473804 features a helium-like iron line at 6.7 keV and is classified as a nearby cataclysmic variable. Additional surveys are planned for the Norma Arm and Galactic Center, and those NuSTAR observations will benefit from the lessons learned during this pilot study. C1 [Bodaghee, Arash; Tomsick, John A.; Krivonos, Roman; Barriere, Nicolas; Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bodaghee, Arash] Georgia Coll & State Univ, Milledgeville, GA 31061 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, Franz E.] Millennium Inst Astrophys, Santiago, Chile. [Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA. [Fornasini, Francesca M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Gotthelf, Eric V.; Hailey, Charles J.; Mori, Kaya] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Hong, Jaesub] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bodaghee, A (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. RI Boggs, Steven/E-4170-2015 OI Boggs, Steven/0000-0001-9567-4224 FU NASA [NNG08FD60C]; National Science Foundation Graduate Research Fellowship; BasalCATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1141218] FX This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology. 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; NASA's Astrophysics Data System Bibliographic Services; and the SIMBAD database operated at CDS, Strasbourg, France. F. M. F. acknowledges support from the National Science Foundation Graduate Research Fellowship. F. E. B. acknowledges support from BasalCATA PFB-06/2007, CONICYT-Chile (FONDECYT 1141218 and "EMBIGGEN" Anillo ACT1101), and Project IC120009 "Millennium Institute of Astrophysics (MAS)" of Iniciativa Cient ' ifica Milenio del Ministerio de Economia, Fomento y Turismo. NR 37 TC 3 Z9 3 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2014 VL 791 IS 1 AR 68 DI 10.1088/0004-637X/791/1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700068 ER PT J AU Bond, NA Gardner, JP de Mello, DF Teplitz, HI Rafelski, M Koekemoer, AM Coe, D Grogin, N Gawiser, E Ravindranath, S Scarlata, C AF Bond, Nicholas A. Gardner, Jonathan P. de Mello, Duilia F. Teplitz, Harry I. Rafelski, Marc Koekemoer, Anton M. Coe, Dan Grogin, Norman Gawiser, Eric Ravindranath, Swara Scarlata, Claudia TI THE REST-FRAME ULTRAVIOLET STRUCTURE OF 0.5 < z < 1.5 GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: formation; galaxies: high-redshift; galaxies: structure ID STAR-FORMING GALAXIES; ULTRA DEEP FIELD; GOODS-SOUTH FIELD; SIMILAR-TO 2; EXTRAGALACTIC LEGACY SURVEY; HIGH-REDSHIFT; VLT/FORS2 SPECTROSCOPY; ADVANCED CAMERA; CLUMP-CLUSTER; PART II AB We present the rest-frame UV wavelength dependence of the Petrosian-like half-light radius (r(50)), and the concentration parameter for a sample of 198 star-forming galaxies at 0.5 < z < 1.5. We find a similar to 5% decrease in r(50) from 1500 angstrom to 3000 angstrom, with half-light radii at 3000 ranging from 0.6 kpc to 6 kpc. We also find a decrease in concentration of similar to 0.07 (1.9 < C-3000 < 3.9). The lack of a strong relationship between r(50) and wavelength is consistent with a model in which clumpy star formation is distributed over length scales comparable to the galaxy's rest-frame optical light. While the wavelength dependence of r50 is independent of size at all redshifts, concentration decreases more sharply in the far-UV (similar to 1500 angstrom) for large galaxies at z similar to 1. This decrease in concentration is caused by a flattening of the inner similar to 20% of the light profile in disk-like galaxies, indicating that the central regions have different UV colors than the rest of the galaxy. We interpret this as a bulge component with older stellar populations and/or more dust. The size-dependent decrease in concentration is less dramatic at z similar to 2, suggesting that bulges are less dusty, younger, and/or less massive than the rest of the galaxy at higher redshifts. C1 [Bond, Nicholas A.; Gardner, Jonathan P.] NASA, Goddard Space Flight Ctr, Cosmol Lab, Greenbelt, MD 20771 USA. [de Mello, Duilia F.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Teplitz, Harry I.; Rafelski, Marc] CALTECH, IPAC, Pasadena, CA 91125 USA. [Koekemoer, Anton M.; Coe, Dan; Grogin, Norman] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Ravindranath, Swara] Interuniv Ctr Astron & Astrophys, Pune, Maharashtra, India. [Scarlata, Claudia] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. RP Bond, NA (reprint author), NASA, Goddard Space Flight Ctr, Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. OI Gawiser, Eric/0000-0003-1530-8713; Koekemoer, Anton/0000-0002-6610-2048 FU Space Telescope Science Institute [HST-GO-12534]; Association of Universities for Research in Astronomy, Inc., under NASA [NAS 5-26555] FX Support for program number HST-GO-12534 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. NR 48 TC 4 Z9 4 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2014 VL 791 IS 1 AR 18 DI 10.1088/0004-637X/791/1/18 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700018 ER PT J AU Klimchuk, JA Bradshaw, SJ AF Klimchuk, J. A. Bradshaw, S. J. TI ARE CHROMOSPHERIC NANOFLARES A PRIMARY SOURCE OF CORONAL PLASMA? SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: chromosphere; Sun: corona; Sun: UV radiation ID IMAGING SPECTROMETER OBSERVATIONS; ACTIVE-REGION LOOPS; DOPPLER SHIFTS; SPECTROSCOPIC OBSERVATIONS; TRANSITION REGION; TIME-DEPENDENCE; SOLAR CORONA; QUIET SUN; EMISSION; CORE AB It has been suggested that the hot plasma of the solar corona comes primarily from impulsive heating events, or nanoflares, that occur in the lower atmosphere, either in the upper part of the ordinary chromosphere or at the tips of type II spicules. We test this idea with a series of hydrodynamic simulations. We find that synthetic Fe XII (195) and Fe XIV (274) line profiles generated from the simulations disagree dramatically with actual observations. The integrated line intensities are much too faint; the blueshifts are much too fast; the blue-red asymmetries are much too large; and the emission is confined to low altitudes. We conclude that chromospheric nanoflares are not a primary source of hot coronal plasma. Such events may play an important role in producing the chromosphere and powering its intense radiation, but they do not, in general, raise the temperature of the plasma to coronal values. Those cases where coronal temperatures are reached must be relatively uncommon. The observed profiles of Fe XII and Fe XIV come primarily from plasma that is heated in the corona itself, either by coronal nanoflares or a quasi-steady coronal heating process. Chromospheric nanoflares might play a role in generating waves that provide this coronal heating. C1 [Klimchuk, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bradshaw, S. J.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. RP Klimchuk, JA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM James.A.Klimchuk@nasa.gov; stephen.bradshaw@rice.edu RI Klimchuk, James/D-1041-2012 OI Klimchuk, James/0000-0003-2255-0305 FU NASA Supporting Research and Technology Program FX This work was supported by the NASA Supporting Research and Technology Program. The authors benefited from participation in the International Space Science Institute team on Using Observables to Settle the Question of Steady versus Impulsive Coronal Heating, led by one of us (S.J.B.) and Helen Mason. NR 34 TC 16 Z9 16 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 AUG 10 PY 2014 VL 791 IS 1 AR 60 DI 10.1088/0004-637X/791/1/60 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700060 ER PT J AU Kushwaha, U Joshi, B Cho, KS Veronig, A Tiwari, SK Mathew, SK AF Kushwaha, Upendra Joshi, Bhuwan Cho, Kyung-Suk Veronig, Astrid Tiwari, Sanjiv Kumar Mathew, S. K. TI IMPULSIVE ENERGY RELEASE AND NON-THERMAL EMISSION IN A CONFINED M4.0 FLARE TRIGGERED BY RAPIDLY EVOLVING MAGNETIC STRUCTURES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: flares; Sun: X-rays, gamma rays ID CORONAL MASS EJECTIONS; DOUBLE-LOOP CONFIGURATION; X-RAY TELESCOPE; SOLAR-FLARES; EXTREME-ULTRAVIOLET; FLUX EMERGENCE; RECONNECTION; FIELD; ERUPTIONS; RHESSI AB We present observations of a confined M4.0 flare from NOAA 11302 on 2011 September 26. Observations at high temporal, spatial, and spectral resolution from the Solar Dynamics Observatory, Reuven Ramaty High Energy Solar Spectroscopic Imager, and Nobeyama Radioheliograph observations enabled us to explore the possible triggering and energy release processes of this flare despite its very impulsive behavior and compact morphology. The flare light curves exhibit an abrupt rise of non-thermal emission with co-temporal hard X-ray (HXR) and microwave (MW) bursts that peaked instantly without any precursor emission. This stage was associated with HXR emission up to 200 keV that followed a power law with photon spectral index (gamma) similar to 3. Another non-thermal peak, observed 32 s later, was more pronounced in the MW flux than the HXR profiles. Dual peaked structures in the MW and HXR light curves suggest a two-step magnetic reconnection process. Extreme ultraviolet (EUV) images exhibit a sequential evolution of the inner and outer core regions of magnetic loop systems while the overlying loop configuration remained unaltered. Combined observations in HXR, (E) UV, and Ha provide support for flare models involving the interaction of coronal loops. The magnetograms obtained by the Helioseismic and Magnetic Imager reveal emergence of magnetic flux that began similar to five hr before the flare. However, the more crucial changes in the photospheric magnetic flux occurred about one minute prior to the flare onset with opposite polarity magnetic transients appearing at the early flare location within the inner core region. The spectral, temporal, and spatial properties of magnetic transients suggest that the sudden changes in the small-scale magnetic field have likely triggered the flare by destabilizing the highly sheared pre-flare magnetic configuration. C1 [Kushwaha, Upendra; Joshi, Bhuwan; Mathew, S. K.] Udaipur Solar Observ, Phys Res Lab, Udaipur 313001, India. [Cho, Kyung-Suk] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Veronig, Astrid] Graz Univ, Inst Phys, Kanzelhohe Observ, A-8010 Graz, Austria. [Tiwari, Sanjiv Kumar] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Kushwaha, U (reprint author), Udaipur Solar Observ, Phys Res Lab, Udaipur 313001, India. EM upendra@prl.res.in RI Veronig, Astrid/B-8422-2009; OI Kushwaha, Upendra/0000-0001-6750-4578 FU "Development of Korea SpaceWeather Center" of KASI; KASI basic research funds; Austrian Science Fund (FWF) [P24092-N16]; NASA Postdoctoral Program at the NASAMarshall Space Flight Center FX We thank theSDO, RHESSI, NoRH, andGOESteams for their open data policy. SDO and RHESSI are NASA's missions under living with a star and small explorer programs, respectively. We are grateful to S. Couvidat of Stanford University for providing the SDO/HMI spectral data. We express our sincere gratitude to P. Venkatakrishnan (USO/PRL), Jongchul Chae (Seoul National University), and Yong-JaeMoon (Kyung-Hee University) for useful discussions. K. S. C. is supported by the "Development of Korea SpaceWeather Center" of KASI and the KASI basic research funds. A. V. gratefully acknowledges the Austrian Science Fund (FWF): P24092-N16. S. K. T. is supported by an appointment to the NASA Postdoctoral Program at the NASAMarshall Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. We sincerely thank the anonymous referee for providing constructive comments and suggestions that have enhanced the quality and presentation of this paper. NR 46 TC 3 Z9 3 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2014 VL 791 IS 1 AR 23 DI 10.1088/0004-637X/791/1/23 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700023 ER PT J AU Maseda, MV van der Wel, A Rix, HW da Cunha, E Pacifici, C Momcheva, I Brammer, GB Meidt, SE Franx, M van Dokkum, P Fumagalli, M Bell, EF Ferguson, HC Forster-Schreiber, NM Koekemoer, AM Koo, DC Lundgren, BF Marchesini, D Nelson, EJ Patel, SG Skelton, RE Straughn, AN Trump, JR Whitaker, KE AF Maseda, Michael V. van der Wel, Arjen Rix, Hans-Walter da Cunha, Elisabete Pacifici, Camilla Momcheva, Ivelina Brammer, Gabriel B. Meidt, Sharon E. Franx, Marijn van Dokkum, Pieter Fumagalli, Mattia Bell, Eric F. Ferguson, Henry C. Foerster-Schreiber, Natascha M. Koekemoer, Anton M. Koo, David C. Lundgren, Britt F. Marchesini, Danilo Nelson, Erica J. Patel, Shannon G. Skelton, Rosalind E. Straughn, Amber N. Trump, Jonathan R. Whitaker, Katherine E. TI THE NATURE OF EXTREME EMISSION LINE GALAXIES AT z=1-2: KINEMATICS AND METALLICITIES FROM NEAR-INFRARED SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: dwarf; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: starburst ID STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; HUBBLE-SPACE-TELESCOPE; GREATER-THAN 1; SIMILAR-TO 2; EXTRAGALACTIC LEGACY SURVEY; HIGH-REDSHIFT GALAXIES; GREEN PEA GALAXIES; LOW-MASS GALAXIES AB We present near-infrared spectroscopy of a sample of 22 Extreme Emission Line Galaxies at redshifts 1.3 < z < 2.3, confirming that these are low-mass (M* = 108-109M(circle dot)) galaxies undergoing intense starburst episodes (M*/SFR similar to 10-100 Myr). The sample is selected by [O iii] or Ha emission line flux and equivalent width using near-infrared grism spectroscopy from the 3D-HST survey. High-resolution NIR spectroscopy is obtained with LBT/LUCI and VLT/X-SHOOTER. The [Oiii]/H line ratio is high (greater than or similar to 5) and [N ii]/Ha is always significantly below unity, which suggests a low gas-phase metallicity. We are able to determine gas-phase metallicities for seven of our objects using various strong-line methods, with values in the range 0.05-0.30 Z similar to and with a median of 0.15 Z similar to; for three of these objects we detect [O iii].4363, which allows for a direct constraint on the metallicity. The velocity dispersion, as measured from the nebular emission lines, is typically similar to 50 km s-1. Combined with the observed star-forming activity, the Jeans and Toomre stability criteria imply that the gas fraction must be large (fgas - 2/3), consistent with the difference between our dynamical and stellar mass estimates. The implied gas depletion timescale (several hundred Myr) is substantially longer than the inferred mass-weighted ages (similar to 50 Myr), which further supports the emerging picture that most stars in low-mass galaxies form in short, intense bursts of star formation. C1 [Maseda, Michael V.; van der Wel, Arjen; Rix, Hans-Walter; da Cunha, Elisabete; Meidt, Sharon E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Pacifici, Camilla] Yonsei Univ, Yonsei Univ Observ, Seoul 120749, South Korea. [Momcheva, Ivelina; van Dokkum, Pieter; Nelson, Erica J.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Brammer, Gabriel B.; Ferguson, Henry C.; Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Franx, Marijn; Fumagalli, Mattia] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Foerster-Schreiber, Natascha M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Koo, David C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Koo, David C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Lundgren, Britt F.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Marchesini, Danilo] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. [Patel, Shannon G.] Carnegie Observ, Pasadena, CA 91101 USA. [Skelton, Rosalind E.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Straughn, Amber N.; Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Trump, Jonathan R.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Maseda, MV (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM maseda@mpia.de RI Skelton, Rosalind/S-1845-2016; OI Skelton, Rosalind/0000-0001-7393-3336; Koekemoer, Anton/0000-0002-6610-2048; da Cunha, Elisabete/0000-0001-9759-4797; Bell, Eric/0000-0002-5564-9873; Brammer, Gabriel/0000-0003-2680-005X FU KASI-Yonsei Joint Research Program for the Frontiers of Astronomy and Space Science - Korea Astronomy and Space Science Institute; NSF [AST-08-08133] FX M. V. M. is a member of the International Max Planck Research School for Astronomy and Cosmic Physics at the University of Heidelberg, IMPRS-HD, Germany. C. P. acknowledges support by the KASI-Yonsei Joint Research Program for the Frontiers of Astronomy and Space Science funded by the Korea Astronomy and Space Science Institute. D. C. K. acknowledges funding from NSF grant AST-08-08133. We would also like to thank R. Amorin for productive discussions and C. Berlind and F. Rice for their computational expertise. NR 96 TC 22 Z9 22 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2014 VL 791 IS 1 AR 17 DI 10.1088/0004-637X/791/1/17 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700017 ER PT J AU McCullough, PR Crouzet, N Deming, D Madhusudhan, N AF McCullough, P. R. Crouzet, N. Deming, D. Madhusudhan, N. TI WATER VAPOR IN THE SPECTRUM OF THE EXTRASOLAR PLANET HD 189733b. I. THE TRANSIT SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: atmospheres; stars: individual (HD 189733); techniques: spectroscopic ID HUBBLE-SPACE-TELESCOPE; NICMOS TRANSMISSION SPECTROSCOPY; MU-M; ATMOSPHERIC HAZE; GJ 1214B; STARS; ABSORPTION; TEMPERATURE; VARIABILITY; EXOPLANETS AB We report near-infrared spectroscopy of the gas giant planet HD 189733b in transit. We used the Hubble Space Telescope Wide Field Camera 3 (IIST WFC3) with its G141 grism covering 1.1 mu m to 1.7 mu m and spatially scanned the image across the detector at 2 '' s(-1). When smoothed to 75 nm bins, the local maxima of the transit depths in the 1.15 mu m and 1.4 mu m water vapor features are, respectively, 83 +/- 53 ppm and 200 +/- 47 ppm greater than the local minimum at 1.3 mu m. We compare the WFC3 spectrum with the composite transit spectrum of HD 189733b assembled by Pont et al., extending from 0.3 mu m to 24 mu m. Although the water vapor features in the WFC3 spectrum are compatible with the model of non-absorbing, Rayleigh-scattering dust in the planetary atmosphere, we also re-interpret the available data with a clear planetary atmosphere. In the latter interpretation, the slope of increasing transit depth with shorter wavelengths from the near infrared, through the visible, and into the ultraviolet is caused by unocculted star spots, with a smaller contribution of Rayleigh scattering by molecular hydrogen in the planet's atmosphere. At relevant pressures along the terminator, our model planetary atmosphere's temperature is similar to 700 K, which is below the condensation temperatures of sodium- and potassium-bearing molecules, causing the broad wings of the spectral lines of Na I and K I at 0.589 mu m and 0.769 mu m to be weak. C1 [McCullough, P. R.; Crouzet, N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [McCullough, P. R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Crouzet, N.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Deming, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Deming, D.] NASA, Astrobiol Inst, Virtual Planetary Lab, Washington, DC USA. [Madhusudhan, N.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA. [Madhusudhan, N.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP McCullough, PR (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM pmcc@stsci.edu OI Crouzet, Nicolas/0000-0001-7866-8738 FU HST [GO-12881]; Origins of Solar Systems [NNX10AG30G] FX This research used NASA's Astrophysics Data System Bibliographic Services and the SIMBAD database, operated at CDS, Strasbourg, France, and was funded in part by HST grant GO-12881 and Origins of Solar Systems grant NNX10AG30G. NR 65 TC 48 Z9 48 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2014 VL 791 IS 1 AR 55 DI 10.1088/0004-637X/791/1/55 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700055 ER PT J AU Sloan, GC Lagadec, E Zijlstra, AA Kraemer, KE Weis, AP Matsuura, M Volk, K Peeters, E Duley, WW Cami, J Bernard-Salas, J Kemper, F Sahai, R AF Sloan, G. C. Lagadec, E. Zijlstra, A. A. Kraemer, K. E. Weis, A. P. Matsuura, M. Volk, K. Peeters, E. Duley, W. W. Cami, J. Bernard-Salas, J. Kemper, F. Sahai, R. TI CARBON-RICH DUST PAST THE ASYMPTOTIC GIANT BRANCH: ALIPHATICS, AROMATICS, AND FULLERENES IN THE MAGELLANIC CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars ID SPITZER-SPACE-TELESCOPE; INFRARED-EMISSION FEATURES; 21 MU-M; GRAVITATIONAL LENSING EXPERIMENT.; SHORT-WAVELENGTH SPECTROMETER; POINT-SOURCE CATALOG; OGLE-III CATALOG; POST-AGB STARS; PLANETARY-NEBULAE; PROTOPLANETARY NEBULAE AB Infrared spectra of carbon-rich objects that have evolved off the asymptotic giant branch reveal a range of dust properties, including fullerenes, polycyclic aromatic hydrocarbons (PAHs), aliphatic hydrocarbons, and several unidentified features, including the 21 mu m emission feature. To test for the presence of fullerenes, we used the position and width of the feature at 18.7-18.9 mu m and examined other features at 17.4 and 6-9 mu m. This method adds three new fullerene sources to the known sample, but it also calls into question three previous identifications. We confirm that the strong 11 mu m features seen in some sources arise primarily from SiC, which may exist as a coating around carbonaceous cores and result from photo-processing. Spectra showing the 21 mu m feature usually show the newly defined Class D PAH profile at 7-9 mu m. These spectra exhibit unusual PAH profiles at 11-14 mu m, with weak contributions at 12.7 mu m, which we define as Class D1, or show features shifted to similar to 11.4, 12.4, and 13.2 mu m, which we define as Class D2. Alkyne hydrocarbons match the 15.8 mu m feature associated with 21 mu m emission. Sources showing fullerene emission but no PAHs have blue colors in the optical, suggesting a clear line of sight to the central source. Spectra with 21 mu m features and Class D2 PAH emission also show photometric evidence for a relatively clear line of sight to the central source. The multiple associations of the 21 mu m feature with aliphatic hydrocarbons suggest that the carrier is related to this material in some way. C1 [Sloan, G. C.; Lagadec, E.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Zijlstra, A. A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Kraemer, K. E.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA. [Weis, A. P.] Columbia Univ, Dept Astron & Astrophys, New York, NY 10027 USA. [Weis, A. P.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Matsuura, M.] UCL, Dept Phys & Astron, Astrophys Grp, London WC1E 6BT, England. [Volk, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Peeters, E.; Cami, J.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Peeters, E.; Cami, J.] SETI Inst, Mountain View, CA 94043 USA. [Duley, W. W.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Bernard-Salas, J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Kemper, F.] Acad Sinica, Inst Astron & Astrophys, NTU AS, Taipei 10617, Taiwan. [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sloan, GC (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. EM sloan@isc.astro.cornell.edu RI Kemper, Francisca/D-8688-2011; OI Kemper, Francisca/0000-0003-2743-8240; Kraemer, Kathleen/0000-0002-2626-7155 FU NASA [1257184]; California Institute of Technology under NASA [1407]; National Science Council of Taiwan [NSC100-2112-M-001-023-MY3] FX We thank the referee, A. P. Jones, for a thorough report that led to substantial improvements in this paper. We are grateful to P. R. Wood for providing the spectrum of LIN 49. G.C.S. was supported by NASA through Contract Number 1257184 issued by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. F.K. received support from the National Science Council of Taiwan, grant NSC100-2112-M-001-023-MY3. This research relied on the following resources: NASA's Astrophysics Data System, the Infrared Science Archive at the Infrared Processing and Analysis Center, operated by JPL, and the SIMBAD and VizieR databases, operated at the Centre de Donnees astronomiques de Strasbourg. NR 98 TC 15 Z9 15 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2014 VL 791 IS 1 AR 28 DI 10.1088/0004-637X/791/1/28 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700028 ER PT J AU Taquet, V Charnley, SB Sipila, O AF Taquet, Vianney Charnley, Steven B. Sipila, Olli TI MULTILAYER FORMATION AND EVAPORATION OF DEUTERATED ICES IN PRESTELLAR AND PROTOSTELLAR CORES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: molecules; stars: formation ID DENSE INTERSTELLAR CLOUDS; SOLAR-TYPE PROTOSTARS; WATER DEUTERIUM FRACTIONATION; COMPLEX ORGANIC-MOLECULES; GRAIN SURFACE-CHEMISTRY; STAR-FORMING REGIONS; LOW-MASS PROTOSTARS; O1 HALE-BOPP; IRAS 16293-2422; INFALL MOTIONS AB Extremely large deuteration of several molecules has been observed toward prestellar cores and low-mass protostars for a decade. New observations performed toward low-mass protostars suggest that water presents a lower deuteration in the warm inner gas than in the cold external envelope. We coupled a gas-grain astrochemical model with a one-dimensional model of a collapsing core to properly follow the formation and the deuteration of interstellar ices as well as their subsequent evaporation in the low-mass protostellar envelopes with the aim of interpreting the spatial and temporal evolutions of their deuteration. The astrochemical model follows the formation and the evaporation of ices with a multilayer approach and also includes a state-of-the-art deuterated chemical network by taking the spin states of H-2 and light ions into account. Because of their slow formation, interstellar ices are chemically heterogeneous and show an increase of their deuterium fractionation toward the surface. The differentiation of the deuteration in ices induces an evolution of the deuteration within protostellar envelopes. The warm inner region is poorly deuterated because it includes the whole molecular content of ices, while the deuteration predicted in the cold external envelope scales with the highly deuterated surface of ices. We are able to reproduce the observed evolution of water deuteration within protostellar envelopes, but we are still unable to predict the super-high deuteration observed for formaldehyde and methanol. Finally, the extension of this study to the deuteration of complex organics, important for the prebiotic chemistry, shows good agreement with the observations, suggesting that we can use the deuteration to retrace their mechanisms and their moments of formation. C1 [Taquet, Vianney; Charnley, Steven B.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20770 USA. [Taquet, Vianney; Charnley, Steven B.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20770 USA. [Sipila, Olli] Univ Helsinki, Dept Phys, FI-00014 Helsinki, Finland. RP Taquet, V (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Mailstop 691,8800 Greenbelt Rd, Greenbelt, MD 20770 USA. FU NASA's Origins of Solar Systems and Exobiology Programs; NASA postdoctoral program; Academy of Finland [250741] FX The kinetic data we used have been downloaded from the online database KIDA (Wakelam et al.2012; http://kida.obs.ubordeaux1.fr). This work was supported by NASA's Origins of Solar Systems and Exobiology Programs. V.T. acknowledges support from the NASA postdoctoral program. O.S. acknowledges support from the Academy of Finland grant 250741. NR 140 TC 25 Z9 25 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 AUG 10 PY 2014 VL 791 IS 1 AR 1 DI 10.1088/0004-637X/791/1/1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700001 ER PT J AU Zaccheo, TS Pernini, T Snell, HE Browell, EV AF Zaccheo, T. Scott Pernini, Timothy Snell, Hilary E. Browell, Edward V. TI Impact of atmospheric state uncertainties on retrieved XCO2 columns from laser differential absorption spectroscopy measurements SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE laser absorption spectroscopy; lidar; CO2 retrievals; ASCENDS ID CONSTRAINED MULTISPECTRUM ANALYSIS; SPEED DEPENDENCE; CO2; LIDAR; INTENSITIES; CM(-1) AB This work assesses the impact of uncertainties in atmospheric state knowledge on retrievals of carbon dioxide column amounts (XCO2) from laser differential absorption spectroscopy (LAS) measurements. LAS estimates of XCO2 columns are normally derived not only from differential absorption observations but also from measured or prior knowledge of atmospheric state that includes temperature, moisture, and pressure along the viewing path. In the case of global space-based monitoring systems, it is often difficult if not impossible to provide collocated in situ measurements of atmospheric state for all observations, so retrievals often rely on collocated remote-sensed data or values derived from numerical weather prediction (NWP) models to describe the atmospheric state. A radiative transfer-based simulation framework, combined with representative global upper-air observations and matched NWP profiles, was used to assess the impact of model differences on estimates of column CO2 and O-2 concentrations. These analyses focus on characterizing these errors for LAS measurements of CO2 in the 1.57-mu m region and of O-2 in the 1.27-mu m region. The results provide a set of signal-to-noise metrics that characterize the errors in retrieved values associated with uncertainties in atmospheric state and provide a method for selecting optimal differential absorption line pairs to minimize the impact of these noise terms. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. C1 [Zaccheo, T. Scott; Pernini, Timothy; Snell, Hilary E.] Atmospher & Environm Res Inc, Lexington, MA 02421 USA. [Browell, Edward V.] NASA, STARSS Affiliate 2, Langley Res Ctr, Yorktown, VA 23692 USA. RP Zaccheo, TS (reprint author), Atmospher & Environm Res Inc, 131 Hartwell Ave, Lexington, MA 02421 USA. EM szaccheo@aer.com FU NASA Langley Research Center, ASCENDS CarbonHawk Experiment Simulator (ACES) project - NASA Earth Science Technology Office, Instrument Incubator Program [NNL11AD10T]; Atmospheric and Environmental Research, Inc. management FX This work has been supported in part by a contract to AER from NASA Langley Research Center as part of the ASCENDS CarbonHawk Experiment Simulator (ACES) project funded under the NASA Earth Science Technology Office, Instrument Incubator Program (order # NNL11AD10T). The authors would like to thank a number of their colleagues at the NASA Langley Research Center: Narasimha Prasad for his hard work and dedication that enabled the ACES program to come to fruition, and F. Wallace Harrison, Syed Ismail, and Michael D. Obland for their continued support and insights that has allowed this work to move forward. Additionally, we would like to thank the anonymous JARS reviewer, whose in depth feedback have significantly strengthened the readability and content of this work. Finally, we would like to acknowledge Atmospheric and Environmental Research, Inc. management for their support of this effort over a number of years. NR 18 TC 2 Z9 2 U1 2 U2 10 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD AUG 8 PY 2014 VL 8 AR 083575 DI 10.1117/1.JRS.8.083575 PG 16 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AP8UE UT WOS:000342353900001 ER PT J AU Mikellides, IG Hofer, RR Katz, I Goebel, DM AF Mikellides, Ioannis G. Hofer, Richard R. Katz, Ira Goebel, Dan M. TI Magnetic shielding of Hall thrusters at high discharge voltages SO JOURNAL OF APPLIED PHYSICS LA English DT Article AB A series of numerical simulations and experiments have been performed to assess the effectiveness of magnetic shielding in a Hall thruster operating in the discharge voltage range of 300-700V (I-sp approximate to 2000-2700 s) at 6 kW, and 800V (I-sp approximate to 3000) at 9 kW. At 6 kW, the magnetic field topology with which highly effective magnetic shielding was previously demonstrated at 300V has been retained for all other discharge voltages; only the magnitude of the field has been changed to achieve optimum thruster performance. It is found that magnetic shielding remains highly effective for all discharge voltages studied. This is because the channel is long enough to allow hot electrons near the channel exit to cool significantly upon reaching the anode. Thus, despite the rise of the maximum electron temperature in the channel with discharge voltage, the electrons along the grazing lines of force remain cold enough to eliminate or reduce significantly parallel gradients of the plasma potential near the walls. Computed maximum erosion rates in the range of 300-700V are found not to exceed 10(-2) mm/kh. Such rates are similar to 3 orders of magnitude less than those observed in the unshielded version of the same thruster at 300V. At 9 kW and 800 V, saturation of the magnetic circuit did not allow for precisely the same magnetic shielding topology as that employed during the 6-kW operation since this thruster was not designed to operate at this condition. Consequently, the maximum erosion rate at the inner wall is found to be similar to 1 order of magnitude higher (similar to 10(-1) mm/kh) than that at 6 kW. At the outer wall, the ion energy is found to be below the sputtering yield threshold so no measurable erosion is expected. (C) 2014 AIP Publishing LLC. C1 [Mikellides, Ioannis G.; Hofer, Richard R.; Katz, Ira; Goebel, Dan M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mikellides, IG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Ioannis.G.Mikellides@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this paper was carried out by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and funded through the internal Research and Technology Development program. The authors wish to acknowledge Dr. Benjamin A. Jorns for providing the applied magnetic field measurements in the 9MS800 configuration of the H6 thruster. NR 22 TC 5 Z9 5 U1 0 U2 15 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD AUG 7 PY 2014 VL 116 IS 5 AR 053302 DI 10.1063/1.4892160 PG 11 WC Physics, Applied SC Physics GA AO2TM UT WOS:000341178900008 ER PT J AU Kobayashi, DR Farman, R Polovina, JJ Parker, DM Rice, M Balazs, GH AF Kobayashi, Donald R. Farman, Richard Polovina, Jeffrey J. Parker, Denise M. Rice, Marc Balazs, George H. TI "Going with the Flow'' or Not: Evidence of Positive Rheotaxis in Oceanic Juvenile Loggerhead Turtles (Caretta caretta) in the South Pacific Ocean Using Satellite Tags and Ocean Circulation Data SO PLOS ONE LA English DT Article ID CENTRAL NORTH PACIFIC; OLIVACEA SEA-TURTLES; ORIENTATION; MOVEMENT; BEHAVIOR; CURRENTS; HABITAT; DESIGN; MODEL AB The movement of juvenile loggerhead turtles (n = 42) out-fitted with satellite tags and released in oceanic waters off New Caledonia was examined and compared with ocean circulation data. Merging of the daily turtle movement data with drifter buoy movements, OSCAR (Ocean Surface Current Analyses - Real time) circulation data, and three different vertical strata (05 m, 0-40 m, 0-100 m) of HYCOM (HYbrid Coordinate Ocean Model) circulation data indicated the turtles were swimming against the prevailing current in a statistically significant pattern. This was not an artifact of prevailing directions of current and swimming, nor was it an artifact of frictional slippage. Generalized additive modeling was used to decompose the pattern of swimming into spatial and temporal components. The findings are indicative of a positive rheotaxis whereby an organism is able to detect the current flow and orient itself to swim into the current flow direction or otherwise slow down its movement. Potential mechanisms for the means and adaptive significance of rheotaxis in oceanic juvenile loggerhead turtles are discussed. C1 [Kobayashi, Donald R.; Polovina, Jeffrey J.; Balazs, George H.] NOAA, Pacific Islands Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96813 USA. [Farman, Richard] Aquarium Lagons, Noumea, New Caledonia. [Parker, Denise M.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Newport, OR USA. [Rice, Marc] Hawaii Preparatory Acad, Kamuela, HI USA. RP Kobayashi, DR (reprint author), NOAA, Pacific Islands Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96813 USA. EM Donald.Kobayashi@noaa.gov FU United States government to National Oceanic and Atmospheric Administration FX The funders were base funding and add-on funding from the United States government to National Oceanic and Atmospheric Administration and had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 45 TC 11 Z9 11 U1 0 U2 17 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD AUG 6 PY 2014 VL 9 IS 8 AR e103701 DI 10.1371/journal.pone.0103701 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM6SM UT WOS:000339995100025 PM 25098694 ER PT J AU Forouhar, S Borgentun, C Frez, C Briggs, RM Bagheri, M Canedy, CL Kim, CS Kim, M Bewley, WW Merritt, CD Abell, J Vurgaftman, I Meyer, JR AF Forouhar, S. Borgentun, C. Frez, C. Briggs, R. M. Bagheri, M. Canedy, C. L. Kim, C. S. Kim, M. Bewley, W. W. Merritt, C. D. Abell, J. Vurgaftman, I. Meyer, J. R. TI Reliable mid-infrared laterally-coupled distributed-feedback interband cascade lasers SO APPLIED PHYSICS LETTERS LA English DT Article ID HIGH-POWER AB We report on the performance and reliability of laterally-coupled distributed-feedback (DFB) interband cascade lasers designed to operate at 3.6 mu m wavelength. A two-step ridge etch process ensures single-transverse-mode operation with minimal lateral current spreading, and a secondorder Bragg grating etched alongside the ridge waveguide imposes single-mode DFB operation. Life tests performed on four randomly selected lasers, continuously operating at 40 degrees C with output power >10 mW, showed no measurable degradation after each laser was operated continuously for more than 1500 h. (C) 2014 AIP Publishing LLC. C1 [Forouhar, S.; Borgentun, C.; Frez, C.; Briggs, R. M.; Bagheri, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Canedy, C. L.; Kim, C. S.; Bewley, W. W.; Merritt, C. D.; Abell, J.; Vurgaftman, I.; Meyer, J. R.] Naval Res Lab, Washington, DC 20375 USA. [Kim, M.] Sotera Def Solut Inc, Columbia, MD 21046 USA. RP Forouhar, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM siamak.forouhar@jpl.nasa.gov NR 17 TC 17 Z9 17 U1 0 U2 13 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD AUG 4 PY 2014 VL 105 IS 5 AR 051110 DI 10.1063/1.4892655 PG 4 WC Physics, Applied SC Physics GA AO2LE UT WOS:000341153000010 ER PT J AU de Jeu, RAM Holmes, TRH Parinussa, RM Owe, M AF de Jeu, Richard A. M. Holmes, Thomas R. H. Parinussa, Robert M. Owe, Manfred TI A spatially coherent global soil moisture product with improved temporal resolution SO JOURNAL OF HYDROLOGY LA English DT Article DE Soil moisture; Dielectric constant; Passive microwave radiometry; Remote sensing ID VEGETATION OPTICAL DEPTH; PASSIVE MICROWAVE OBSERVATIONS; POLARIZATION DIFFERENCE INDEX; AMSR-E; SATELLITE-OBSERVATIONS; RETRIEVAL; MODEL; VALIDATION; CLIMATE; FIELDS AB Global soil moisture products that are completely independent of any type of ancillary data and solely rely on satellite observations are presented. Additionally, we further develop an existing downscaling technique that enhances the spatial resolution of such products to approximately 11 km. These products are based on internal modules of the Land Parameter Retrieval Model (LPRM), an algorithm that uses the radiative transfer equation to link soil moisture, vegetation optical depth and land surface temperature to observed brightness temperatures. The soil moisture product that is independent of any type of ancillary data uses the internally calculated dielectric constant as a soil moisture proxy. This data product is not influenced by errors associated with coarse-scale global soil property maps or by any other type of forcing (e.g. re-analysis) data and is therefore solely based on satellite microwave observations. The second step builds upon recent developments to increase the spatial resolution of the LPRM retrievals using a smoothing filter downscaling method. With this method we can attain a spatial resolution that can be more useful at the scale of local and regional hydrological studies as well. The steps presented in this paper were applied to observations from the Advanced Microwave Scanning Radiometer-Earth Observing System (AMSR-E). The newly derived data sets were validated using ground-based observations from the International Soil Moisture Network (ISMN). The internally calculated dielectric constant product results in significantly more days with valid retrievals than the original soil moisture data products, in particular over arid regions. The dielectric constant product resulted in similar correlations with in situ data as the original soil moisture data product. Together, these findings demonstrate the usefulness of this new dielectric constant product for the hydrological modeling community and climate studies. A case study on the Australian Fitzroy catchment demonstrated that the downscaled data product has a more detailed spatial description of soil moisture, especially during wet and dry conditions with more pronounced dry and wet regions within the catchment. The increased resolution data products could therefore improve runoff predictions and this study demonstrated the potential added value of a transitioning from a spatial resolution of 56 km toward a higher resolution of 11 km. The hydrological implications of these newly developed data records are not only linked to AMSR-E satellite data, but also to the next generation Soil Moisture Active and Passive (SMAP) mission where a 9 km spatial resolution is the target resolution for satellite soil moisture products. The new data products will not replace the current LPRM products, but will be added to the existing array of data products and will become publicly available through our data portals. (C) 2014 Elsevier B.V. All rights reserved. C1 [de Jeu, Richard A. M.; Parinussa, Robert M.] Vrije Univ Amsterdam, Dept Earth Sci Earth & Climate Cluster, NL-1081 HV Amsterdam, Netherlands. [Holmes, Thomas R. H.] ARS, USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [Owe, Manfred] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. RP de Jeu, RAM (reprint author), Vrije Univ Amsterdam, Dept Earth Sci Earth & Climate Cluster, De Boelelaan 1085, NL-1081 HV Amsterdam, Netherlands. EM r.a.m.de.jeu@vu.nl RI Holmes, Thomas/F-4512-2010 OI Holmes, Thomas/0000-0002-4651-0079 FU European Space Agency Climate Change Initiative for soil moisture [4000104814/11/I-NB]; European Commission [282672] FX This work has been undertaken as part of the European Space Agency Climate Change Initiative for soil moisture (http://www.esa-soilmoisture-cci.org/), Contract No. 4000104814/11/I-NB) Additionally, this work was funded by the European Commission's 7th Framework Project, under Grant Agreement Number 282672, EMBRACE Project. The authors would like to thank the International Soil Moisture Network for making the verification data available. Finally, the authors would like to thank Dr. I. van Meerveld for her valuable contribution to this manuscript. NR 70 TC 20 Z9 20 U1 2 U2 35 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 EI 1879-2707 J9 J HYDROL JI J. Hydrol. PD AUG 4 PY 2014 VL 516 SI SI BP 284 EP 296 DI 10.1016/j.jhydrol.2014.02.015 PG 13 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA AL3NT UT WOS:000339036100026 ER PT J AU Stephens, DB Vold, H AF Stephens, David B. Vold, Havard TI Order tracking signal processing for open rotor acoustics SO JOURNAL OF SOUND AND VIBRATION LA English DT Article ID SHAFT-SPEED INFORMATION; KALMAN; EXPLORATION; FILTER AB Counter-rotating open rotor acoustic measurements were processed using a two-shaft Vold-Kalman order tracking filter, providing new insight into the complicated noise generation mechanisms of this type of system. The multi-shaft formulation of the Vold-Kalman filter can determine a time-accurate output of shaft order tones associated with each rotor, even as the rotation rate of the two rotors varies. This is a major improvement over the usual short time Fourier transform method for many applications. It was found that the contribution from each rotor to the individual tones varies strongly as a function of shaft order and operating condition. The order tracking filter is also demonstrated as a robust tool for separating the tonal and broadband components of a signal for which the usual shaft phase averaging methods fail. Published by Elsevier Ltd. C1 [Stephens, David B.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Vold, Havard] ATA Engn Inc, San Diego, CA 92103 USA. RP Stephens, DB (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM david.stephens@nasa.gov; hvold@ata-e.com FU NASA Fixed Wing project; ATA Engineering, Inc. [SAA3-1239] FX This paper was funded by the NASA Fixed Wing project with Dr. Ruben Del Rosario as the project manager. The authors would also like to thank ATA Engineering, Inc., for their support and usage of proprietary software. The work was performed under the Space Act Agreement: SAA3-1239, ATA Engineering, Inc., "Joint Publication On Order Tracking Methods For Quantifying Noise From Open Rotors." The open rotor wind tunnel test was performed as a collaboration between the NASA Environmentally Responsible Aviation project and GE Aviation. NR 25 TC 2 Z9 2 U1 0 U2 4 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0022-460X EI 1095-8568 J9 J SOUND VIB JI J. Sound Vibr. PD AUG 4 PY 2014 VL 333 IS 16 BP 3818 EP 3830 DI 10.1016/j.jsv.2014.04.005 PG 13 WC Acoustics; Engineering, Mechanical; Mechanics SC Acoustics; Engineering; Mechanics GA AI4FY UT WOS:000336822300016 ER PT J AU Laurini, KC Gerstenmaier, WH AF Laurini, Kathleen C. Gerstenmaier, William H. TI The Global Exploration Roadmap and its significance for NASA SO SPACE POLICY LA English DT Article DE Global Exploration Roadmap; NASA; International cooperation AB The Global Exploration Roadmap reflects the collaborative effort of twelve space agencies to define a long-term human space exploration strategy which provides substantial benefits for improving the quality of life on Earth and is implementable and sustainable. Such a strategy is a necessary precondition to the government investments required to enable the challenging and rewarding missions that extend human presence into the solar system. The article introduces the international strategy and elaborates on NASA's leadership role in shaping that strategy. The publication of the roadmap, a reflection of the space landscape and multilateral agency-level dialog over the last four years, allows NASA to demonstrate its commitment to leading a long-term space exploration endeavor that delivers benefits, maintains strategic human spaceflight capabilities and expands human presence in space, with human missions to the surface of Mars as a driving goal. The road mapping process has clearly demonstrated the complementary interests of the participants and the potential benefits that can be gained through cooperation among nations to achieve a common goal. The present US human spaceflight policy is examined and it is shown that the establishment of a sustainable global space exploration strategy is fully consistent with that policy. Published by Elsevier Ltd. C1 [Laurini, Kathleen C.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Gerstenmaier, William H.] NASA, Washington, DC 20546 USA. RP Laurini, KC (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM Kathy.laurini-1@nasa.gov NR 21 TC 0 Z9 0 U1 3 U2 7 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-9646 EI 1879-338X J9 SPACE POLICY JI Space Policy PD AUG PY 2014 VL 30 IS 3 SI SI BP 149 EP 155 DI 10.1016/j.spacepol.2014.08.004 PN B PG 7 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA AY5HL UT WOS:000347603300004 ER PT J AU Neal, CR Schmidt, GK Ehrenfreund, P Carpenter, JD AF Neal, C. R. Schmidt, G. K. Ehrenfreund, P. Carpenter, J. D. TI Developing the global exploration roadmap: An example using the humans to the lunar surface theme SO SPACE POLICY LA English DT Article DE Space exploration; Lunar exploration; Global exploration roadmap; Test bed ID SPACE EXPLORATION; EPITHERMAL NEUTRONS; WATER ICE; MOON; CRATERS; PROJECT; SCIENCE; POLES; RADAR AB The development of the Global Exploration Roadmap (GER) by 12 space agencies participating in the International Space Exploration Coordination Group broadly outlines a pathway to send humans beyond low Earth orbit for the first time since Apollo. Three themes have emerged: Exploration of a Near-Earth Asteroid, Extended Duration Crew Missions, and Humans to the Lunar Surface. The lack of detail within each of these themes could mean that realizing the goals of the GER would be significantly delayed. The purpose of this paper is to demonstrate that many of the details needed to fully define and evaluate these themes in terms of scientific rationale, economic viability, and technical feasibility already exist and need to be mapped to the GER. Here, we use the Humans to the Lunar Surface theme as an example to illustrate how this process could work. By mapping documents from a variety of international stake-holders, this process can be used to cement buy-in from the current partners and attract new ones to this effort. (C) 2014 Published by Elsevier Ltd. C1 [Neal, C. R.] Univ Notre Dame, Dept Civil & Environm Engn & Earth Sci, Notre Dame, IN 46556 USA. [Schmidt, G. K.] NASA, Ames Res Ctr, SSERVI, Moffett Field, CA 94035 USA. [Ehrenfreund, P.] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA. [Carpenter, J. D.] ESA ESTEC, NL-2401 AZ Noordwijk, Netherlands. RP Neal, CR (reprint author), Univ Notre Dame, Dept Civil & Environm Engn & Earth Sci, Notre Dame, IN 46556 USA. EM cneal@nd.edu; gregory.k.schmidt@nasa.gov; pehren@gwu.edu; james.carpenter@esa.int NR 46 TC 1 Z9 1 U1 1 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-9646 EI 1879-338X J9 SPACE POLICY JI Space Policy PD AUG PY 2014 VL 30 IS 3 SI SI BP 156 EP 162 DI 10.1016/j.spacepol.2014.08.007 PN B PG 7 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA AY5HL UT WOS:000347603300005 ER PT J AU Ehrenfreund, P McKay, CP AF Ehrenfreund, P. McKay, C. P. CA COSPAR Panel Exploration PEX TI Activities of the COSPAR Panel on Exploration supporting the Global Exploration Roadmap SO SPACE POLICY LA English DT Editorial Material DE Space exploration; International cooperation; Solar system AB The Global Exploration Roadmap (GER) is driven by several goals and objectives that include space science, the search for life as well as preparatory science activities to enable human space exploration. The Committee on Space Research (COSPAR), through its Commissions and Panels provides an international forum that supports and promotes space exploration worldwide. COSPAR's Panel on Exploration (PEX) investigates a stepwise approach of preparatory research on Earth and in Low Earth Orbit (LEO) to facilitate a future global space exploration program. We summarize recent activities and workshops of PEX in support of the GER. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Ehrenfreund, P.] George Washington Univ, Elliott Sch Int Affairs, Inst Space Policy, Washington, DC 20052 USA. [McKay, C. P.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. RP Ehrenfreund, P (reprint author), George Washington Univ, Elliott Sch Int Affairs, Inst Space Policy, 1957 E St,Suite 403, Washington, DC 20052 USA. EM pehren@gwu.edu NR 10 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-9646 EI 1879-338X J9 SPACE POLICY JI Space Policy PD AUG PY 2014 VL 30 IS 3 SI SI BP 170 EP 173 DI 10.1016/j.spacepol.2014.07.006 PN B PG 4 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA AY5HL UT WOS:000347603300007 ER PT J AU Brown, ME Carroll, ML Escobar, VM AF Brown, Molly E. Carroll, Mark L. Escobar, Vanessa M. TI User needs and assessing the impact of low latency NASA Earth observation data availability on societal benefit SO SPACE POLICY LA English DT Article DE NASA; Latency; Earth observation; Applications; Operational; Satellite data AB Since the advent of NASA's Earth Observing System, knowledge of the practical benefits of Earth science data has grown considerably. The community using NASA Earth science observations in applications has grown significantly, with increasing sophistication to serve national interests. Data latency, or how quickly communities receive science observations after acquisition, can have a direct impact on the applications and usability of the information. This study was conducted to determine how users are incorporating NASA data into applications and operational processes to benefit society beyond scientific research, as well as to determine the need for data latency of less than 12 h. The results of the analysis clearly show the significant benefit to society of serving the needs of the agricultural, emergency response, environmental monitoring and weather communities who use rapidly delivered, accurate Earth science data. The study also showed the potential of expanding the communities who use low latency NASA science data products to provide new ways of transforming data into information. These benefits can be achieved with a clear and consistent NASA policy on product latency. Published by Elsevier Ltd. C1 [Brown, Molly E.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Carroll, Mark L.; Escobar, Vanessa M.] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA. RP Brown, ME (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA. EM molly.brown@nasa.gov RI Brown, Molly/E-2724-2010 OI Brown, Molly/0000-0001-7384-3314 NR 8 TC 0 Z9 0 U1 0 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-9646 EI 1879-338X J9 SPACE POLICY JI Space Policy PD AUG PY 2014 VL 30 IS 3 BP 135 EP 137 DI 10.1016/j.spacepol.2014.05.002 PN A PG 3 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA AY5HK UT WOS:000347603200003 ER PT J AU Burlaga, LF Ness, NF Richardson, JD AF Burlaga, L. F. Ness, N. F. Richardson, J. D. TI Heliosheath magnetic field and plasma observed by Voyager 2 during 2011 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID TERMINATION SHOCK; SOLAR-WIND; STRENGTH FLUCTUATIONS; AU; INTENSITIES; CYCLE AB We discuss magnetic field and plasma observations from Voyager 2 (V2) during 2011, when V2 was beginning to see the effects of increasing solar activity following the solar minimum in 2009. The magnetic field strength (B) profile showed large amplitude fluctuations that can be resolved into a linear increase of B with time and a sinusoidal variation of the period of 86.2 +/- 0.8 days. Voyager 2 was in a unipolar region in which the magnetic polarity was directed away from the Sun along the Parker spiral 96% of the time, indicating that V2 was poleward of the heliospheric current sheet throughout most of 2011. The distribution of B was lognormal, but a Gaussian distribution was observed when the linear variation of B was subtracted from the data. The distribution of daily increments of B was a q-Gaussian distribution with q = 1.1 +/- 0.1, which is less intermittent than normally observed in the heliosheath. However, the distribution of hourly increments of B was a q-Gaussian distribution with q = 1.5 +/- 0.03. The density, temperature, and velocity increased linearly from the beginning of 2011 to approximately day 254. The magnetic and thermal pressure tended to increase throughout the year, but the magnetic pressure dominated most of the time. The counting rate of > 70 MeV/nucleon particles increased rapidly during the first 250 days, but it leveled out during the rest of the year when B was stronger. The empirical CR-B relationship describes this behavior. C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Richardson, J. D.] MIT, Kalvi Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM lburlagahsp@verizon.net FU NASA [NNG14PN24P]; NASA from the JPL [959203]; [NNX12A63G] FX The data in this paper are from the magnetic field experiment on Voyager 2. N.F. Ness was partially supported by grant NNX12A63G to Catholic University of America. L. F. Burlaga was supported by NASA grant NNG14PN24P. J.D. Richardson was supported under NASA contract 959203 from the JPL to MIT. McClanahan and S. Kramer carried out the processing of the data. The zero-offset tables were computed by D. Berdichevsky using magnetic field rolls calibrations and "z axis calibration." We thank Edward Stone and his coinvestigators on the CRS experiment on V2 for making their data available for distribution on COHOweb. NR 32 TC 1 Z9 1 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG PY 2014 VL 119 IS 8 DI 10.1002/2014JA020297 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT3BJ UT WOS:000344809600004 ER PT J AU Collinson, GA Fedorov, A Futaana, Y Masunaga, K Hartle, R Stenberg, G Grebowsky, J Holmstrom, M Andre, N Barabash, S Zhang, TL AF Collinson, G. A. Fedorov, A. Futaana, Y. Masunaga, K. Hartle, R. Stenberg, G. Grebowsky, J. Holmstrom, M. Andre, N. Barabash, S. Zhang, T. L. TI The extension of ionospheric holes into the tail of Venus SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MAGNETIC-FIELDS; EXPRESS MISSION; SPACE PLASMAS; NIGHTSIDE; ANALYZER; ASPERA-4; FLOW; WAKE AB Ionospheric holes are Cytherian nightside phenomena discovered by the NASA Pioneer Venus Orbiter, featuring localized plasma depletions driven by prominent and unexplained enhancements in the draped interplanetary magnetic field. Observed only during solar maximum, the phenomenon remains unexplained, despite their frequent observation during the first 3 years of the mission and more than 30 years having elapsed since their first description in the literature. We present new observations by the European Space Agency Venus Express showing that ionospheric holes can extend much further into the tail than previously anticipated (1.2 to 2.4 planetary radii) and may be observed throughout the solar cycle and over a wide range of solar wind conditions. We find that ionospheric holes are a manifestation of a deeper underlying phenomenon: tubes of enhanced draped interplanetary magnetic field that emerge in pairs from below the ionosphere and stretch far down the tail. We speculate on two possible explanations for the magnetic fields underlying the phenomena: magnetic pileup due to stagnation of ionospheric flow and internal draping around a metallic core. C1 [Collinson, G. A.; Hartle, R.; Grebowsky, J.] NASA, Heliophys Sci Div, Goddard Spaceflight Ctr, Greenbelt, MD 20771 USA. [Collinson, G. A.; Futaana, Y.; Masunaga, K.; Stenberg, G.; Holmstrom, M.; Barabash, S.] Swedish Inst Space Phys, Inst Rymdfys, S-98128 Kiruna, Sweden. [Collinson, G. A.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Fedorov, A.; Andre, N.] Univ Toulouse, Inst Rech Astrophys & Planetol, Toulouse, France. [Masunaga, K.] Tohoku Univ, Dept Geophys, Sendai, Miyagi 980, Japan. [Zhang, T. L.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. RP Collinson, GA (reprint author), NASA, Heliophys Sci Div, Goddard Spaceflight Ctr, Greenbelt, MD 20771 USA. EM glyn.a.collinson@nasa.gov FU CNES FX We would like to thank Martin Wieser for his support and CNES for a travel grant which facilitated the survey. We also thank Elena Budnik and the AMDA team, Robin Ramsted, Menelaos Sarantos, and Alex Young for useful discussions. Venus Express data are available from the ESA planetary science archive. NR 38 TC 5 Z9 5 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG PY 2014 VL 119 IS 8 DI 10.1002/2014JA019851 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT3BJ UT WOS:000344809600067 ER PT J AU Denton, RE Takahashi, K Thomsen, MF Borovsky, JE Singer, HJ Wang, Y Goldstein, J Brandt, PC Reinisch, BW AF Denton, R. E. Takahashi, K. Thomsen, M. F. Borovsky, J. E. Singer, H. J. Wang, Y. Goldstein, J. Brandt, P. C. Reinisch, B. W. TI Evolution of mass density and O plus concentration at geostationary orbit during storm and quiet events SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INNER MAGNETOSPHERE; ELECTRON-DENSITIES; OUTER PLASMASPHERE; POLAR-CAP; ART.; FIELD; PLASMAPAUSE; IONS; IONOSPHERE; DYNAMICS AB We investigated mass density rho(m) and O+ concentration eta(O+) = n(O+)/n(e) (where n(O+) and n(e) are the O+ and electron density, respectively) during two events, one active and one more quiet. We found rho(m) from observations of Alfven wave frequencies measured by the GOES, and we investigated composition by combining measurements of rho(m) with measurements of ion density n(MPA, i) from the Magnetospheric Plasma Analyzer (MPA) instrument on Los Alamos National Laboratory spacecraft or n(e) from the Radio Plasma Imager instrument on the Imager forMagnetopause-to-Aurora Global Exploration spacecraft. Using a simple assumption for the He+ density at solar maximum based on a statistical study, we found eta(O+) values ranging from near zero to close to unity. For geostationary spacecraft that corotate with the Earth, sudden changes in density for both rho(m) and n(e) often appear between dusk and midnight magnetic local time, especially when Kp is significantly above zero. This probably indicates that the bulk (total) ions have energy below a few keV and that the satellites are crossing from closed or previously closed to open drift paths. During long periods that are geomagnetically quiet, the mass density varies little, but ne gradually refills leading to a gradual change in composition from low-density plasma that is relatively cold and heavy (high-average ion mass M = rho(m)/n(e)) to high-density plasma that is relatively cold and light (low M) plasmasphere-like plasma. During active periods we observe a similar daily oscillation in plasma properties from the dayside to the nightside, with cold and light high-density plasma (more plasmasphere-like) on the dayside and hotter and more heavy low-density plasma (more plasma sheet-like) on the nightside. The value of ne is very dependent on whether it is measured inside or outside a plasmaspheric plume, while rho(m) is not. All of our results were found at solar maximum; previous results suggest that there will be much less O+ at solar minimum under all conditions. C1 [Denton, R. E.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Takahashi, K.; Brandt, P. C.] Johns Hopkins Univ Appl Phys Lab, Laurel, MD USA. [Thomsen, M. F.] Los Alamos Natl Lab, Los Alamos, NM USA. [Borovsky, J. E.] Space Sci Inst, Boulder, CO USA. [Singer, H. J.] Natl Ocean & Atmospher Adm Space Weather Predict, Boulder, CO USA. [Wang, Y.] NASA Goddard Space Flight Ctr, Goddard Earth Sci & Technol Ctr, Greenbelt, MD USA. [Wang, Y.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. [Goldstein, J.] Southwest Res Inst, San Antonio, TX USA. [Reinisch, B. W.] Univ Massachusetts Lowell, Space Sci Lab, Lowell, MA USA. RP Denton, RE (reprint author), Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. EM richard.e.denton@dartmouth.edu RI Brandt, Pontus/N-1218-2016 OI Brandt, Pontus/0000-0002-4644-0306 FU NSF [AGS-1105790, ATM-0855924]; NASA [NNX10AQ60G, NNX11AO59G] FX Work at Dartmouth College was supported by NSF grant AGS-1105790 and NASA grants NNX10AQ60G (Living with a Star Targeted Research Plasmasphere focused science topic) and NNX11AO59G (Heliophysics Theory Program). Work at the Applied Physics Laboratory was supported by NSF grant ATM-0855924. We thank the reviewers for helpful comments. Supplementary materials for this paper include GOES magnetometer data, calculated Alfven frequencies and mass density, and IMAGE RPI electron density. Most LANL MPA data used in this study are available at CDAWeb. NR 44 TC 4 Z9 4 U1 1 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 AUG PY 2014 VL 119 IS 8 DI 10.1002/2014JA019888 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT3BJ UT WOS:000344809600028 ER PT J AU Fatemi, S Holmstrom, M Futaana, Y Lue, C Collier, MR Barabash, S Stenberg, G AF Fatemi, Shahab Holmstrom, Mats Futaana, Yoshifumi Lue, Charles Collier, Michael R. Barabash, Stas Stenberg, Gabriella TI Effects of protons reflected by lunar crustalmagnetic fields on the global lunar plasma environment SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MONOCHROMATIC WHISTLER WAVES; SOLAR-WIND; MAGNETIC-FIELDS; BOW SHOCK; ION-BEAM; WAKE; MOON; INSTABILITIES; SURFACE; KAGUYA AB Solar wind plasma interaction with lunar crustal magnetic fields is different than that of magnetized bodies like the Earth. Lunar crustal fields are, for typical solar wind conditions, not strong enough to form a (bow) shock upstream but rather deflect and perturb plasma and fields. Here we study the global effects of protons reflected from lunar crustal magnetic fields on the lunar plasma environment when the Moon is in the unperturbed solar wind. We employ a three-dimensional hybrid model of plasma and an observed map of reflected protons from lunar magnetic anomalies over the lunar farside. We observe that magnetic fields and plasma upstream over the lunar crustal fields compress to nearly 120% and 160% of the solar wind, respectively. We find that these disturbances convect downstream in the vicinity of the lunar wake, while their relative magnitudes decrease. In addition, solar wind protons are disturbed and heated at compression regions and their velocity distribution changes from Maxwellian to a non-Maxwellian. Finally, we show that these features persists, independent of the details of the ion reflection by the magnetic fields. C1 [Fatemi, Shahab; Holmstrom, Mats; Futaana, Yoshifumi; Lue, Charles; Barabash, Stas; Stenberg, Gabriella] Swedish Inst Space Phys, S-98128 Kiruna, Sweden. [Fatemi, Shahab] Lulea Univ Technol, Div Space Technol, Dept Comp Sci Elect & Space Engn, S-95187 Lulea, Sweden. [Lue, Charles] Umea Univ, Dept Phys, Umea, Sweden. [Collier, Michael R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Fatemi, S (reprint author), Swedish Inst Space Phys, S-98128 Kiruna, Sweden. EM shahab@irf.se RI Collier, Michael/I-4864-2013 OI Collier, Michael/0000-0001-9658-6605 FU National Graduate School of Space Technology (NGSST); Lulea University of Technology; Swedish National Space Board (SNSB); National Graduate School of Scientific Computing (NGSSC), Uppsala University, Sweden FX The work of Shahab Fatemi was supported by the National Graduate School of Space Technology (NGSST), Lulea University of Technology, the Swedish National Space Board (SNSB), and the National Graduate School of Scientific Computing (NGSSC), Uppsala University, Sweden. This research was conducted using resources provided by the Swedish National Infrastructure for Computing (SNIC) at the High Performance Computing Center North (HPC2N), Umea University, Sweden. The software used in this work was in part developed by the DOE NNSA-ASC OASCR Flash Center at the University of Chicago. The authors thank the International Space Science Institute (ISSI) Bern, Switzerland, for organizing a meeting when the topic of this paper was extensively discussed. We thank the teams who created and provided WIND magnetic field and plasma data used in this analysis, including K. W. Ogilvie, A.J. Lazarus, and R. Lepping. The authors also thank the reviewers for their valuable comments to improve this manuscript. NR 50 TC 10 Z9 10 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG PY 2014 VL 119 IS 8 DI 10.1002/2014JA019900 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT3BJ UT WOS:000344809600006 ER PT J AU Feynman, J Ruzmaikin, A AF Feynman, J. Ruzmaikin, A. TI The Centennial Gleissberg Cycle and its association with extendedminima SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID LONG-TERM VARIATION; MEAN-FIELD DYNAMO; SOLAR-WIND SPEED; DIFFERENTIAL ROTATION; GEOMAGNETIC-ACTIVITY; INTERPLANETARY FIELD; STELLAR DYNAMOS; MAGNETIC-FIELD; GRAND MINIMA; TIME SCALES AB The recent extended minimum of solar and geomagnetic variability (XSM) mirrors the XSMs in the nineteenth and twentieth centuries: 1810-1830 and 1900-1910. Such extended minima also were evident in aurorae reported from 450 A. D. to 1450 A. D. This paper argues that these minima are consistent with minima of the Centennial Gleissberg Cycles (CGCs), a 90-100 year variation observed on the Sun, in the solar wind, at the Earth, and throughout the heliosphere. The occurrence of the recent XSM is consistent with the existence of the CGC as a quasiperiodic variation of the solar dynamo. Evidence of CGCs is provided by the multicentury sunspot record, by the almost 150 year record of indexes of geomagnetic activity (1868 to present), by 1000 years of observations of aurorae (from 450 to 1450 A. D.) and millennial records of radionuclides in ice cores. The aa index of geomagnetic activity carries information about the two components of the solar magnetic field (toroidal and poloidal), one driven by flares and coronal mass ejections (related to the toroidal field) and the other driven by corotating interaction regions in the solar wind (related to the poloidal field). These two components systematically vary in their intensity and relative phase giving us information about centennial changes of the sources of solar dynamo during the recent CGC over the last century. The dipole and quadrupole modes of the solar magnetic field changed in relative amplitude and phase; the quadrupole mode became more important as the XSM was approached. Some implications for the solar dynamo theory are discussed. C1 [Feynman, J.; Ruzmaikin, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Ruzmaikin, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM alexander.ruzmaikin@jpl.nasa.gov FU Jet Propulsion Laboratory of the California Institute of Technology under National Aeronautics and Space Administration FX We thank reviewers for helpful, critical comments. 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. NR 79 TC 4 Z9 4 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG PY 2014 VL 119 IS 8 DI 10.1002/2013JA019478 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT3BJ UT WOS:000344809600002 ER PT J AU Raines, JM Gershman, DJ Slavin, JA Zurbuchen, TH Korth, H Anderson, BJ Solomon, SC AF Raines, Jim M. Gershman, Daniel J. Slavin, James A. Zurbuchen, Thomas H. Korth, Haje Anderson, Brian J. Solomon, Sean C. TI Structure and dynamics of Mercury'smagnetospheric cusp: MESSENGER measurements of protons and planetary ions SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MAGNETOPAUSE RECONNECTION RATE; MONTE-CARLO MODEL; SOLAR-WIND; MAGNETIC-FIELD; MERCURYS MAGNETOSPHERE; POLAR MAGNETOSPHERE; INNER HELIOSPHERE; PLASMA; SURFACE; EXOSPHERE AB The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft has observed the northern magnetospheric cusp of Mercury regularly since the probe was inserted into orbit about the innermost planet in March 2011. Observations from the Fast Imaging Plasma Spectrometer (FIPS) made at altitudes < 400 km in the planet's cusp have shown average proton densities (> 10 cm(-3)) that are exceeded only by those observed in the magnetosheath. These high plasma densities are also associated with strong diamagnetic depressions observed by MESSENGER's Magnetometer. Plasma in the cusp may originate from several sources: (1) Direct inflow from the magnetosheath, (2) locally produced planetary photoions and ions sputtered off the surface from solar wind impact and then accelerated upward, and (3) flow of magnetosheath and magnetospheric plasma accelerated from dayside reconnection X-lines. We surveyed 518 cusp passes by MESSENGER, focusing on the spatial distribution, energy spectra, and pitch-angle distributions of protons and Na+-group ions. Of those, we selected 77 cusp passes during which substantial Na+-group ion populations were present for a more detailed analysis. We find that Mercury's cusp is a highly dynamic region, both in spatial extent and plasma composition and energies. From the three-dimensional plasma distributions observed by FIPS, protons with mean energies of 1 keV were found flowing down into the cusp (i.e., source (1) above). The distribution of pitch angles of these protons showed a depletion in the direction away from the surface, indicating that ions within 40 degrees of the magnetic field direction are in the loss cone, lost to the surface rather than being reflected by the magnetic field. In contrast, Na+-group ions show two distinct behaviors depending on their energy. Low-energy (100-300 eV) ions appear to be streaming out of the cusp, showing pitch-angle distributions with a strong component antiparallel to the magnetic field (away from the surface). These ions appear to have been generated in the cusp and accelerated locally (i.e., source (2) above). Higher-energy (>= 1keV) Na+-group ions in the cusp exhibit much larger perpendicular components in their energy distributions. During active times, as judged by frequent, large-amplitude magnetic field fluctuations, many more Na+-group ions are measured at latitudes south of the cusp. In several cases, these Na+-group ions in the dayside magnetosphere are flowing northward toward the cusp. The high mean energy, pitch-angle distributions, and large number of Na+-group ions on dayside magnetospheric field lines are inconsistent with direct transport into the cusp of sputtered ions from the surface or newly photoionized particles. Furthermore, the highest densities and mean energies often occur together with high-amplitude magnetic fluctuations, attributed to flux transfer events along the magnetopause. These results indicate that high-energy Na+-group ions in the cusp are likely formed by ionization of escaping neutral Na in the outer dayside magnetosphere and the magnetosheath followed by acceleration and transport into the cusp by reconnection at the subsolar magnetopause (i.e., source 3 above). C1 [Raines, Jim M.; Gershman, Daniel J.; Slavin, James A.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Gershman, Daniel J.] NASA Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA. [Korth, Haje; Anderson, Brian J.] Johns Hopkins Univ Appl Phys Lab, Laurel, MD USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DE USA. RP Raines, JM (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM jraines@umich.edu RI Slavin, James/H-3170-2012 OI Slavin, James/0000-0002-9206-724X FU NASA Discovery Program [NAS5-97271, NASW-00002] FX The MESSENGER project is supported by the NASA Discovery Program under contracts NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. J.M.R. thanks D. Schriver and T. A. Cassidy for discussions helpful to this work. Data used in this study are available from the Planetary Data System. NR 59 TC 22 Z9 22 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG PY 2014 VL 119 IS 8 DI 10.1002/2014JA020120 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT3BJ UT WOS:000344809600039 ER PT J AU Selesnick, RS Baker, DN Jaynes, AN Li, X Kanekal, SG Hudson, MK Kress, BT AF Selesnick, R. S. Baker, D. N. Jaynes, A. N. Li, X. Kanekal, S. G. Hudson, M. K. Kress, B. T. TI Observations of the inner radiation belt: CRAND and trapped solar protons SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ENERGY; ZONE AB Measurements of inner radiation belt protons have been made by the Van Allen Probes Relativistic Electron-Proton Telescopes as a function of kinetic energy (24 to 76 MeV), equatorial pitch angle, and magnetic L shell, during late 2013 and early 2014. A probabilistic data analysis method reduces background from contamination by higher-energy protons. Resulting proton intensities are compared to predictions of a theoretical radiation belt model. Then trapped protons originating both from cosmic ray albedo neutron decay (CRAND) and from trapping of solar protons are evident in the measured distributions. An observed double-peaked distribution in L is attributed, based on the model comparison, to a gap in the occurrence of solar proton events during the 2007 to 2011 solar minimum. Equatorial pitch angle distributions show that trapped solar protons are confined near the magnetic equator but that CRAND protons can reach low altitudes. Narrow pitch angle distributions near the outer edge of the inner belt are characteristic of proton trapping limits. C1 [Selesnick, R. S.] Air Force Res Lab, Space Vehicles Directorate, Kirtland AFB, NM USA. [Baker, D. N.; Jaynes, A. N.; Li, X.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Li, X.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA. [Kanekal, S. G.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Hudson, M. K.; Kress, B. T.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. RP Selesnick, RS (reprint author), Air Force Res Lab, Space Vehicles Directorate, Kirtland AFB, NM USA. EM richard.selesnick@us.af.mil FU NASA [NNH14AX18I]; Air Force Research Laboratory under the Heliophysics Guest Investigators Program, at University of Colorado; College by RBSP-ECT through JHU/APL under prime NASA [967399, NAS5-01072]; NSF [ATM-1023332] FX The authors thank C. A. Kletzing for EMFISIS magnetic field data used in pitch angle determination and M. G. Henderson and G. D. Reeves for magnetic ephemeris data from the IGRF+OP77Q model. Van Allen Probes REPT and ephemeris data are available from the ECT Science Operations and Data Center, http://www.rbsp-ect.lanl.gov, and EMFISIS data from http://emfisis.physics.uiowa.edu. This work was supported in part by NASA agreement NNH14AX18I with the Air Force Research Laboratory under the Heliophysics Guest Investigators Program, at University of Colorado and Dartmouth College by RBSP-ECT funding through JHU/APL contract 967399 under prime NASA contract NAS5-01072, and by NSF grant ATM-1023332 to Dartmouth College. NR 21 TC 11 Z9 11 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG PY 2014 VL 119 IS 8 DI 10.1002/2014JA020188 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT3BJ UT WOS:000344809600035 ER PT J AU Voros, Z Facsko, G Khodachenko, M Honkonen, I Janhunen, P Palmroth, M AF Voeroes, Z. Facsko, G. Khodachenko, M. Honkonen, I. Janhunen, P. Palmroth, M. TI Windsock memory COnditioned RAM (CO-RAM) pressure effect: Forced reconnection in the Earth's magnetotail SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INTERPLANETARY MAGNETIC-FIELD; SOLAR-WIND; PLASMA SHEET; MAGNETOSPHERE; CLUSTER; INSTRUMENT; SUBSTORMS; TAIL; IMF; IDENTIFICATION AB Magnetic reconnection (MR) is a key physical concept explaining the addition of magnetic flux to the magnetotail and closed flux lines back-motion to the dayside magnetosphere. This scenario elaborated by Dungey (1963) can explain many aspects of solar wind-magnetosphere interaction processes, including substorms. However, neither the Dungey model nor its numerous modifications were able to explain fully the onset conditions for MR in the tail. In this paper, we introduce new onset conditions for forced MR in the tail. We call our scenario the "windsock memory conditioned ram pressure effect." Our nonflux transfer-associated forcing is introduced by a combination of the large-scale windsock motions exhibiting memory effects and solar wind dynamic pressure actions on the nightside magnetopause during northward oriented interplanetary magnetic field (IMF). Using global MHD Grand Unified Magnetosphere Ionosphere Coupling Simulation version 4 simulation results, upstream data from Wind, magnetosheath data from Cluster 1 and distant tail data from the two-probe Acceleration, Reconnection, Turbulence and Electrodynamics of the Moon's Interaction with the Sun mission, we show that the simultaneous occurrence of vertical windsock motions of the magnetotail and enhanced solar wind dynamic pressure introduces strong nightside disturbances, including enhanced electric fields and persistent vertical cross-tail shear flows. These perturbations, associated with a stream interaction region in the solar wind, drive MR in the tail during episodes of northward oriented interplanetary magnetic field (IMF). We detect MR indirectly, observing plasmoids in the tail and ground-based signatures of earthward moving fast flows. We also consider the application to solar system planets and close-in exoplanets, where the proposed scenario can elucidate some new aspects of solar/stellar wind-magnetosphere interactions. C1 [Voeroes, Z.; Khodachenko, M.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Voeroes, Z.] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria. [Facsko, G.] Hungarian Acad Sci, Geodet & Geophys Inst, Res Ctr Astron & Earth Sci, Sopron, Hungary. [Facsko, G.; Honkonen, I.; Janhunen, P.; Palmroth, M.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Khodachenko, M.] Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow, Russia. [Honkonen, I.] NASA GSFC, Greenbelt, MD USA. RP Voros, Z (reprint author), Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. EM zoltan.voeroes@oeaw.ac.at OI Voros, Zoltan/0000-0001-7597-238X FU Austrian Fond zur Forderung der wissenschaftlichen Forschung [P24740-N27, S11606-N16, Y398]; European Research Council under the European Community [200141-QuESpace]; ECLAT FP7 [263325]; OTKA of the Hungarian Scientific Research Fund [K75640]; NASA [NAS5-02099] FX The authors would like to thank A. Runov (UCLA, Los Angeles, USA); R. Nakamura, M. Panchenko, M. Volwerk, and T. L. Zhang (IWF, Graz Austria); Ch.J. Owen (MSSL, London, UK); J. Borovsky (University of Michigan, USA); and A. Kendl (University of Innsbruck, Austria) for very useful discussions and support. This work was supported by the Austrian Fond zur Forderung der wissenschaftlichen Forschung (projects P24740-N27, S11606-N16, and Y398). Part of the research has received funding from the European Research Council under the European Communitys Seventh Framework Programme (FP7/2007-2013)/ERC Starting grant 200141-QuESpace and from ECLAT FP7 grant 263325. Gabor Facsko was also supported by the OTKA grant K75640 of the Hungarian Scientific Research Fund. We acknowledge NASA contract NAS5-02099 and V. Angelopoulos for the use of data from the THEMIS/ARTEMIS mission. We acknowledge the use of Kyoto WDC AE index and geomagnetic observatory data from IQA (Canada), SKT, GHB, FHB, NAQ, and AMK (Greenland). Figure 1 was created by the Satellite Situation Center 4-D Orbit Viewer. The GUMICS-4 model developed at FMI represents a part of the computational modeling infrastructure of the EU FP7 project IMPEX (http://impex-FP7.oeaw.ac.at). NR 69 TC 4 Z9 4 U1 0 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG PY 2014 VL 119 IS 8 DI 10.1002/2014JA019857 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT3BJ UT WOS:000344809600019 ER PT J AU Wilson, LB Sibeck, DG Breneman, AW Le Contel, O Cully, C Turner, DL Angelopoulos, V Malaspina, DM AF Wilson, L. B., III Sibeck, D. G. Breneman, A. W. Le Contel, O. Cully, C. Turner, D. L. Angelopoulos, V. Malaspina, D. M. TI Quantified energy dissipation rates in the terrestrial bow shock: 2. Waves and dissipation SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ELECTROSTATIC SOLITARY WAVES; CYCLOTRON DRIFT INSTABILITY; QUASI-PERPENDICULAR SHOCK; HIGH MACH NUMBER; FAST MODE SHOCKS; PLASMA-WAVES; SOLAR-WIND; ANOMALOUS RESISTIVITY; NONLINEAR EVOLUTION; BEAM INSTABILITIES AB We present the first quantified measure of the energy dissipation rates, due to wave-particle interactions, in the transition region of the Earth's collisionless bow shock using data from the Time History of Events and Macroscale Interactions during Substorms spacecraft. Our results show that wave-particle interactions can regulate the global structure and dominate the energy dissipation of collisionless shocks. In every bow shock crossing examined, we observed both low-frequency (< 10 Hz) and high-frequency (greater than or similar to 10 Hz) electromagnetic waves throughout the entire transition region and into the magnetosheath. The low-frequency waves were consistent with magnetosonic-whistler waves. The high-frequency waves were combinations of ion-acoustic waves, electron cyclotron drift instability driven waves, electrostatic solitary waves, and whistler mode waves. The high-frequency waves had the following: (1) peak amplitudes exceeding delta B similar to 10 nT and delta E similar to 300 mV/m, though more typical values were delta B similar to 0.1-1.0 nT and delta B similar to 10-50 mV/m; (2) Poynting fluxes in excess of 2000 mu Wm(-2) (typical values were similar to 1-10 mu W m(-2)); (3) resistivities > 9000 Omega m; and (4) associated energy dissipation rates > 10 mu Wm(-3). The dissipation rates due to wave-particle interactions exceeded rates necessary to explain the increase in entropy across the shock ramps for similar to 90% of the wave burst durations. For similar to 22% of these times, the wave-particle interactions needed to only be = 0.1% efficient to balance the nonlinear wave steepening that produced the shock waves. These results show that wave-particle interactions have the capacity to regulate the global structure and dominate the energy dissipation of collisionless shocks. C1 [Wilson, L. B., III; Sibeck, D. G.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Breneman, A. W.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Le Contel, O.] Ecole Polytech, Lab Phys Plasmas, Palaiseau, France. [Cully, C.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Turner, D. L.; Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys Earth & Space Sci, Los Angeles, CA USA. [Malaspina, D. M.] Univ Colorado, Inst Geophys & Planetary Phys Earth & Space Sci, Boulder, CO 80309 USA. RP Wilson, LB (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM lynn.b.wilsoniii@gmail.com RI Wilson III, Lynn/D-4425-2012; Cully, Christopher/P-2539-2016 OI Wilson III, Lynn/0000-0002-4313-1970; FU Wind MODA grants; CNES; CNRS-INSU FX We would like to thank A.F.-Vinas, D. Bryant, D. A. Roberts, R. T. Wicks, R. Lysak, and M. L. Goldstein for useful discussions of the fundamental physics involved in our study. The work was partially supported by Wind MO&DA grants. The French involvement (SCM instruments) on THEMIS are supported by CNES and CNRS-INSU. The data used in this paper and the associated calibration software can be found at http://themis.ssl.berkeley.edu/index.shtml. NR 103 TC 7 Z9 7 U1 1 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG PY 2014 VL 119 IS 8 DI 10.1002/2014JA019930 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT3BJ UT WOS:000344809600032 ER PT J AU Wilson, LB Sibeck, DG Breneman, AW Le Contel, O Cully, C Turner, DL Angelopoulos, V Malaspina, DM AF Wilson, L. B., III Sibeck, D. G. Breneman, A. W. Le Contel, O. Cully, C. Turner, D. L. Angelopoulos, V. Malaspina, D. M. TI Quantified energy dissipation rates in the terrestrial bow shock: 1. Analysis techniques and methodology SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID QUASI-PERPENDICULAR SHOCKS; PHASE-SPACE SIGNATURES; ELECTRON CROSS-TALK; HIGH MACH NUMBER; HIGH-BETA; ISEE-2 OBSERVATIONS; RESOLVED LAYER; ELECTROMAGNETIC-WAVES; ANOMALOUS RESISTIVITY; ION DISTRIBUTIONS AB We present a detailed outline and discussion of the analysis techniques used to compare the relevance of different energy dissipation mechanisms at collisionless shock waves. We show that the low-frequency, quasi-static fields contribute less to ohmic energy dissipation, (-j.E), than their high-frequency counterparts. In fact, we found that high-frequency, large-amplitude (>100 mV/m and/or >1 nT) waves are ubiquitous in the transition region of collisionless shocks. We quantitatively show that their fields, through wave-particle interactions, cause enough energy dissipation to regulate the global structure of collisionless shocks. The purpose of this paper, part one of two, is to outline and describe in detail the background, analysis techniques, and theoretical motivation for our new results presented in the companion paper. The companion paper presents the results of our quantitative energy dissipation rate estimates and discusses the implications. Together, the two manuscripts present the first study quantifying the contribution that high-frequency waves provide, through wave-particle interactions, to the total energy dissipation budget of collisionless shock waves. C1 [Wilson, L. B., III; Sibeck, D. G.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Breneman, A. W.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Le Contel, O.] Ecole Polytech, Lab Phys Plasmas, Palaiseau, France. [Cully, C.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Turner, D. L.; Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys Earth & Space Sci, Los Angeles, CA USA. [Malaspina, D. M.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. RP Wilson, LB (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM lynn.b.wilsoniii@gmail.com RI Wilson III, Lynn/D-4425-2012; Cully, Christopher/P-2539-2016 OI Wilson III, Lynn/0000-0002-4313-1970; FU Wind MO grant; Wind DA grant; CNES; CNRS-INSU FX We would like to thank A.F.-Vinas, D. Bryant, D. A. Roberts, R. T. Wicks, R. Lysak, and M. L. Goldstein for useful discussions of the fundamental physics involved in our study. The work was partially supported by Wind MO and DA grants. The French involvement (SCM instruments) on THEMIS are supported by CNES and CNRS-INSU. The data used in this paper and the associated calibration software can be found at http://themis.ssl.berkeley.edu/index.shtml. NR 87 TC 5 Z9 5 U1 2 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG PY 2014 VL 119 IS 8 DI 10.1002/2014JA019929 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT3BJ UT WOS:000344809600031 ER PT J AU Mikouchi, T Komatsu, M Hagiya, K Ohsumi, K Zolensky, ME Hoffmann, V Martinez, J Hochleitner, R Kaliwoda, M Terada, Y Yagi, N Takata, M Satake, W Aoyagi, Y Takenouchi, A Karouji, Y Uesugi, M Yada, T AF Mikouchi, Takashi Komatsu, Mutsumi Hagiya, Kenji Ohsumi, Kazumasa Zolensky, Michael E. Hoffmann, Viktor Martinez, James Hochleitner, Rupert Kaliwoda, Melanie Terada, Yasuko Yagi, Naoto Takata, Masaki Satake, Wataru Aoyagi, Yuya Takenouchi, Atsushi Karouji, Yuzuru Uesugi, Masayuki Yada, Toru TI Mineralogy and crystallography of some Itokawa particles returned by the Hayabusa asteroidal sample return mission SO EARTH PLANETS AND SPACE LA English DT Article DE Itokawa; Hayabusa; Olivine; Plagioclase; SR-XRD; SR-XANES; LL chondrites ID ALMAHATA SITTA UREILITE; ORDINARY CHONDRITES; DUST PARTICLES; 2008 TC3; BRECCIA; REGOLITH; PYROXENE; HISTORY AB We studied seven Itokawa particles provided by the Japan Aerospace Exploration Agency (JAXA) as first International Announcement of Opportunity (AO) study mainly using electron and synchrotron radiation X-ray beam techniques. All the analyzed particles were collected from the first-touchdown site and composed of olivine and plagioclase with traces of Ca phosphate and chromite, and do not contain pyroxenes. Optical microscopy of these particles shows minor undulatory extinction of olivine and plagioclase, suggesting minor shock metamorphism (shock stage: S2). The electron microprobe analysis shows that olivine is Fo(70-73) and plagioclase is An(13-10)Or(5-7). The synchrotron radiation X-ray diffraction (SR-XRD) analysis of olivine crystals gives cell dimensions of a = 4.708 to 4.779 angstrom, b = 10.271 to 10.289 angstrom, c = 6.017 to 6.024 angstrom, corresponding to the Fo content of Fo(similar to 70) by Vegard's law. This composition matches the result obtained by the electron microprobe analysis. The olivine compositions of the analyzed particles are consistent with those of LL chondrites. The cell dimensions of two plagioclase crystals (a = 8.180 to 8.194 angstrom, b = 12.53 to 12.893 angstrom, c = 7.125 to 7.23 angstrom, a = 92.6 degrees to 93.00 degrees, beta = 116.36 degrees to 116.75 degrees, gamma = 90.03 degrees to 90.17 degrees) indicate that their equilibration temperatures are 800 degrees C +/- 10 degrees C. This temperature is near the peak metamorphic temperature recorded by equilibrated ordinary chondrites. The size of plagioclase crystals and the homogeneity of olivine compositions indicate that their petrologic type is >= 5. We also analyzed plagioclase by SR iron X-ray absorption near-edge structure (SR-XANES) and found that its Fe3+/(Fe2+ + Fe3+) ratio is approximately 0.5. Such high Fe3+ abundance indicates the formation under a relatively oxidizing environment. Thus, all these analyses have reconfirmed that the Itokawa particles returned by the Hayabusa spacecraft are very weakly shocked equilibrated LL chondrites, which matches the results of the preliminary examination team. C1 [Mikouchi, Takashi; Satake, Wataru; Aoyagi, Yuya; Takenouchi, Atsushi] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. [Komatsu, Mutsumi] Waseda Univ, Waseda Inst Adv Study, Shinjuku Ku, Tokyo 1698050, Japan. [Hagiya, Kenji] Univ Hyogo, Sch Sci, Kamigori, Hyogo 6781297, Japan. [Ohsumi, Kazumasa; Terada, Yasuko; Yagi, Naoto; Takata, Masaki] Japan Synchrotron Radiat Res Inst JASRI, Sayo, Hyogo 6795198, Japan. [Zolensky, Michael E.] NASA Johnson Space Ctr, Houston, TX 77058 USA. [Hoffmann, Viktor] Univ Munich LMU, Sect Geophys, Dept Earth & Environm Sci, D-80333 Munich, Germany. [Hoffmann, Viktor] Univ Tubingen, Dept Geosci, D-72074 Tubingen, Germany. [Martinez, James] ESCG Jacobs, Houston, TX 77058 USA. [Hochleitner, Rupert; Kaliwoda, Melanie] Mineral State Collect, D-80333 Munich, Germany. [Karouji, Yuzuru; Uesugi, Masayuki; Yada, Toru] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. RP Mikouchi, T (reprint author), Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. EM mikouchi@eps.s.u-tokyo.ac.jp FU Japanese Ministry of Education, Culture, Sports, Science and Technology [23360333]; SPring-8 long-term project [2010B1415]; KEK [2012G652]; NASA's Muses-C Program FX We thank JAXA for providing us with the Itokawa particles. Advice for the sample preparation and discussion with Dr. T. Nakamura was very helpful. We are grateful for the constructive reviews by Drs. A. Bischoff and T. Nakamura, and editorial handling by Dr. T. Okada. The electron microscopy was performed at the Electron Microbeam Analysis Facility for Mineralogy at the Department of Earth and Planetary Science, University of Tokyo. A part of this study was supported by the Grant-in-Aid for Scientific Research (B) by the Japanese Ministry of Education, Culture, Sports, Science and Technology No. 23360333 (TM). The SR-XRD work was supported by the SPring-8 long-term project (2010B1415) and SR-XANES work was by KEK 2012G652. MEZ was supported by NASA's Muses-C Program. NR 31 TC 6 Z9 6 U1 1 U2 6 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1880-5981 J9 EARTH PLANETS SPACE JI Earth Planets Space PD AUG 1 PY 2014 VL 66 AR 82 DI 10.1186/1880-5981-66-82 PG 9 WC Geosciences, Multidisciplinary SC Geology GA AQ9XS UT WOS:000343213300002 ER PT J AU Price, E Mielikainen, J Huang, ML Huang, BM Huang, HLA Lee, T AF Price, Erik Mielikainen, Jarno Huang, Melin Huang, Bormin Huang, Hung-Lung Allen Lee, Tsengdar TI GPU-Accelerated Longwave Radiation Scheme of the Rapid Radiative Transfer Model for General Circulation Models (RRTMG) SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Compute unified device architecture (CUDA); graphics processing unit (GPU); RRTMG_LW; radiative transfer; weather research and forecasting (WRF) ID ATMOSPHERIC SOUNDING INTERFEROMETER; CLIMATE MODELS; COOLING RATES; FLUXES AB Atmospheric radiative transfer models calculate radiative transfer of electromagnetic radiation through a planetary atmosphere. One of such models is the rapid radiative transfer model (RRTM), which evaluates longwave and shortwave atmospheric radiative fluxes and heating rates. The RRTM for general circulation models (GCMs), RRTMG, is an accelerated version based on the single-column reference of RRTM. The longwave radiation scheme of RRTM for GCMs (RRTMG_LW) is one model that utilizes the correlated-k approach to calculate longwave fluxes and heating rates for application to GCMs. In this paper, the feasibility of using graphics processing units (GPUs) to accelerate the RRTMG_LW in weather research and forecasting (WRF) model is examined. GPUs allow a substantial performance improvement in RRTMG_LW with a large number of parallel compute cores at low cost and power. Our GPU version of RRTMG_LW yields the bit-exact outputs as its original Fortran code. Our results show that NVIDIA's K40 GPU achieves a speedup of 127x as compared to its CPU counterpart running on one CPU core of Intel Xeon E5-2603, whereas the speedup for one CPU socket (4 cores) of the Xeon E5-2603 with respect to one CPU core is only : 3.2x. C1 [Price, Erik; Mielikainen, Jarno; Huang, Melin; Huang, Bormin; Huang, Hung-Lung Allen] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI 53706 USA. [Lee, Tsengdar] NASA Headquarters, Washington, DC 20546 USA. RP Huang, BM (reprint author), Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI 53706 USA. EM Bormin.Huang@ssec.wisc.edu FU National Aeronautics and Space Administration (NASA) [NNX11AL83G] FX This work was supported by the National Aeronautics and Space Administration (NASA) under Grant NNX11AL83G. (Corresponding author: B. Huang.) NR 43 TC 6 Z9 6 U1 1 U2 13 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD AUG PY 2014 VL 7 IS 8 BP 3660 EP 3667 DI 10.1109/JSTARS.2014.2315771 PG 8 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA AQ8DZ UT WOS:000343055200045 ER PT J AU Brzostek, ER Fisher, JB Phillips, RP AF Brzostek, Edward R. Fisher, Joshua B. Phillips, Richard P. TI Modeling the carbon cost of plant nitrogen acquisition: Mycorrhizal trade-offs and multipath resistance uptake improve predictions of retranslocation SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article DE terrestrial biosphere models; retranslocation; nitrogen cycling; mycorrhizae; plant carbon allocation; FUN model ID NORTHERN HARDWOOD FOREST; NUTRIENT USE EFFICIENCY; ELEVATED CO2; TEMPERATE FOREST; ECOSYSTEM PRODUCTIVITY; TERRESTRIAL ECOSYSTEMS; ECTOMYCORRHIZAL FUNGI; ARBUSCULAR MYCORRHIZA; DEPOSITION GRADIENT; SENESCING LEAVES AB Accurate projections of the future land carbon (C) sink by terrestrial biosphere models depend on how nutrient constraints on net primary production are represented. While nutrient limitation is nearly universal, current models do not have a C cost for plant nutrient acquisition. Also missing are symbiotic mycorrhizal fungi, which can consume up to 20% of net primary production and supply up to 50% of a plant's nitrogen (N) uptake. Here we integrate simultaneous uptake and mycorrhizae into a cutting-edge plant N modelFixation and Uptake of Nitrogen (FUN)that can be coupled into terrestrial biosphere models. The C cost of N acquisition varies as a function of mycorrhizal type, with plants that support arbuscular mycorrhizae benefiting when N is relatively abundant and plants that support ectomycorrhizae benefiting when N is strongly limiting. Across six temperate forested sites (representing arbuscular mycorrhizal- and ectomycorrhizal-dominated stands and 176 site years), including multipath resistance improved the partitioning of N uptake between aboveground and belowground sources. Integrating mycorrhizae led to further improvements in predictions of N uptake from soil (R-2=0.69 increased to R-2=0.96) and from senescing leaves (R-2=0.29 increased to R-2=0.73) relative to the original model. On average, 5% and 9% of net primary production in arbuscular mycorrhizal- and ectomycorrhizal-dominated forests, respectively, was needed to support mycorrhizal-mediated acquisition of N. To the extent that resource constraints to net primary production are governed by similar trade-offs across all terrestrial ecosystems, integrating these improvements to FUN into terrestrial biosphere models should enhance predictions of the future land C sink. C1 [Brzostek, Edward R.; Phillips, Richard P.] Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. [Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Fisher, Joshua B.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. RP Brzostek, ER (reprint author), Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. EM edbrzost@indiana.edu OI Fisher, Joshua/0000-0003-4734-9085 FU U.S. Department of Energy-Office of Biological and Environmental Research-Terrestrial Ecosystem Science Program [ER65415]; U.S. National Science Foundation Ecosystem Science Program; National Aeronautics and Space Administration FX The model input and output data are included as Appendix S2 in the supporting information. Funding was provided by the U.S. Department of Energy-Office of Biological and Environmental Research-Terrestrial Ecosystem Science Program (award ER65415) and by the U.S. National Science Foundation Ecosystem Science Program. We would like to acknowledge the researchers whose efforts to produce high-quality carbon and nitrogen budgets across forested ecosystems allowed us to validate the improvements to the model. We also thank M. Shi for the valuable comments on the structure of the model. J.B.F. carried out the research at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and at the Joint Institute for Regional Earth System Science and Engineering, University of California at Los Angeles. NR 89 TC 8 Z9 8 U1 5 U2 70 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 EI 2169-8961 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD AUG PY 2014 VL 119 IS 8 BP 1684 EP 1697 DI 10.1002/2014JG002660 PG 14 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA AQ7KK UT WOS:000342993200013 ER PT J AU Zak, M AF Zak, Michail TI Interference of probabilities in dynamics SO AIP ADVANCES LA English DT Article AB A new class of dynamical systems with a preset type of interference of probabilities is introduced. It is obtained from the extension of the Madelung equation by replacing the quantum potential with a specially selected feedback from the Liouville equation. It has been proved that these systems are different from both Newtonian and quantum systems, but they can be useful for modeling spontaneous collective novelty phenomena when emerging outputs are qualitatively different from the weighted sum of individual inputs. Formation of language and fast decision-making process as potential applications of the probability interference is discussed. (C) 2014 Author(s). C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Zak, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM michail.zak@gmail.com NR 5 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 2158-3226 J9 AIP ADV JI AIP Adv. PD AUG PY 2014 VL 4 IS 8 AR 087130 DI 10.1063/1.4893871 PG 13 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA AQ4YX UT WOS:000342808900030 ER PT J AU Kim, J Rim, T Lee, J Baek, CK Meyyappan, M Lee, JS AF Kim, Jungsik Rim, Taiuk Lee, Junyoung Baek, Chang-Ki Meyyappan, Meyya Lee, Jeong-Soo TI Threshold Voltage Variations Due to Oblique Single Grain Boundary in Sub-50-nm Polysilicon Channel SO IEEE TRANSACTIONS ON ELECTRON DEVICES LA English DT Article DE Grain boundary (GB); poly-silicon (poly-Si) channel; threshold voltage variation ID THIN-FILM TRANSISTORS; DEPENDENCE; LOCATION; SIZE AB We investigate the effect of single grain boundary (SGB) with arbitrary angles on the threshold voltage (V-th) variation in sub-50-nm polysilicon (poly-Si) channel devices using 3-D simulation. An SGB in the poly-Si channel causes changes in potential barrier profile resulting in the variation of V-th. As the planar devices scale down to 20-nm, oblique SGB can significantly increase the whole potential barrier profile and cause large V-th variation. However, due to superior gate controllability, the gate-all-around devices show relatively small increase of the conduction energy band, and thus mitigate the V-th variation even in 20-nm poly-Si channel. C1 [Kim, Jungsik] Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang 790784, South Korea. [Rim, Taiuk; Baek, Chang-Ki] Pohang Univ Sci & Technol, Dept Creat IT Engn, Pohang 790784, South Korea. [Rim, Taiuk; Baek, Chang-Ki] Pohang Univ Sci & Technol, Future IT Innovat Lab, Pohang 790784, South Korea. [Lee, Junyoung; Lee, Jeong-Soo] Pohang Univ Sci & Technol, Dept Elect Engn, Pohang 790784, South Korea. [Meyyappan, Meyya] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kim, J (reprint author), Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang 790784, South Korea. EM irijeori@postech.ac.kr; hacle@postech.ac.kr; covel123@postech.ac.kr; baekck@postech.ac.kr; m.meyyappan@nasa.gov; ljs6951@postech.ac.kr FU IT Consilience Creative Program [NIPA-2014-H0201-14-1001]; National IT Industry Promotion Agency [2011-0031638]; Center for Advanced Soft Electronics through the Ministry of Education, Science, and Technology, Global Frontier Research Program, Korea; Pohang University of Science and Technology, Pohang, Korea; Samsung Electronics Company, Ltd., Suwon, Korea FX This work was supported in part by the IT Consilience Creative Program under Grant NIPA-2014-H0201-14-1001, in part by National IT Industry Promotion Agency under Grant 2011-0031638, in part by Center for Advanced Soft Electronics through the Ministry of Education, Science, and Technology, Global Frontier Research Program, Korea, and in part by the Semiconductor Industry Collaborative Project between Pohang University of Science and Technology, Pohang, Korea, and Samsung Electronics Company, Ltd., Suwon, Korea. The review of this paper was arranged by Editor J. C. S. Woo. NR 23 TC 3 Z9 3 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9383 EI 1557-9646 J9 IEEE T ELECTRON DEV JI IEEE Trans. Electron Devices PD AUG PY 2014 VL 61 IS 8 BP 2705 EP 2710 DI 10.1109/TED.2014.2329848 PG 6 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA AQ6FS UT WOS:000342906200014 ER PT J AU Pettorelli, N Laurance, WF O'Brien, TG Wegmann, M Nagendra, H Turner, W AF Pettorelli, Nathalie Laurance, William F. O'Brien, Timothy G. Wegmann, Martin Nagendra, Harini Turner, Woody TI Satellite remote sensing for applied ecologists: opportunities and challenges SO JOURNAL OF APPLIED ECOLOGY LA English DT Review DE biodiversity; Earth observations; environmental management; natural capital; sensor; technology; wildlife management ID LAND-COVER CLASSIFICATIONS; PROTECTED AREAS; RAIN-FORESTS; INVASIVE PLANT; BIODIVERSITY; RESOLUTION; IMAGERY; SPACE; RADAR; CONSERVATION AB 1. Habitat loss and degradation, overexploitation, climate change and the spread of invasive species are drastically depleting the Earth's biological diversity, leading to detrimental impacts on ecosystem services and human well-being. 2. Our ability to monitor the state of biodiversity and the impacts of global environmental change on this natural capital is fundamental to designing effective adaptation and mitigation strategies for preventing further loss of biological diversity. This requires the scientific community to assess spatio-temporal changes in the distribution of abiotic conditions (e. g. temperature, rainfall) and in the distribution, structure, composition and functioning of ecosystems. 3. The potential for satellite remote sensing (SRS) to provide key data has been highlighted by many researchers, with SRS offering repeatable, standardized and verifiable information on long-term trends in biodiversity indicators. SRS permits one to address questions on scales inaccessible to ground-based methods alone, facilitating the development of an integrated approach to natural resource management, where biodiversity, pressures to biodiversity and consequences of management decisions can all be monitored. 4. Synthesis and applications. Here, we provide an interdisciplinary perspective on the prospects of satellite remote sensing (SRS) for ecological applications, reviewing established avenues and highlighting new research and technological developments that have a high potential to make a difference in environmental management. We also discuss current barriers to the ecological application of SRS-based approaches and identify possible ways to overcome some of these limitations. C1 [Pettorelli, Nathalie] Zool Soc London, Inst Zool, London NW1 4RY, England. [Laurance, William F.] James Cook Univ, Ctr Trop Environm & Sustainabil Sci, Cairns, Qld 4878, Australia. [Laurance, William F.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4878, Australia. [O'Brien, Timothy G.] Wildlife Conservat Soc, Mpala Res Ctr, Nanyuki 10400, Kenya. [Wegmann, Martin] Dept Geog & Geol, D-97074 Wurzburg, Germany. [Nagendra, Harini] Azim Premji Univ, Bangalore 560100, Karnataka, India. [Turner, Woody] NASA Headquarters, Div Earth Sci, Washington, DC 20546 USA. RP Pettorelli, N (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England. EM nathalie.pettorelli@ioz.ac.uk RI Research ID, CTBCC /O-3564-2014; James Cook University, TESS/B-8171-2012; OI Wegmann, Martin/0000-0003-0335-9601; Nagendra, Harini/0000-0002-1585-0724 NR 112 TC 42 Z9 42 U1 22 U2 159 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8901 EI 1365-2664 J9 J APPL ECOL JI J. Appl. Ecol. PD AUG PY 2014 VL 51 IS 4 BP 839 EP 848 DI 10.1111/1365-2664.12261 PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AQ5LP UT WOS:000342851000002 ER PT J AU Khazanov, G Sibeck, D Tel'nikhin, A Kronberg, T AF Khazanov, G. Sibeck, D. Tel'nikhin, A. Kronberg, T. TI Relativistic electron precipitation events driven by electromagnetic ion-cyclotron waves SO PHYSICS OF PLASMAS LA English DT Article ID EMIC WAVES; MAGNETOSPHERE; LOSSES; PLASMA; STORMS AB We adopt a canonical approach to describe the stochastic motion of relativistic belt electrons and their scattering into the loss cone by nonlinear EMIC waves. The estimated rate of scattering is sufficient to account for the rate and intensity of bursty electron precipitation. This interaction is shown to result in particle scattering into the loss cone, forming similar to 10 s microbursts of precipitating electrons. These dynamics can account for the statistical correlations between processes of energization, pitch angle scattering, and relativistic electron precipitation events, that are manifested on large temporal scales of the order of the diffusion time similar to tens of minutes. (C) 2014 AIP Publishing LLC. C1 [Khazanov, G.; Sibeck, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tel'nikhin, A.; Kronberg, T.] Altai State Univ, Dept Phys & Technol, Barnaul 656099, Russia. RP Khazanov, G (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM george.v.khazanov@nasa.gov RI feggans, john/F-5370-2012 FU NASA Van Allen Probes; NASA LWS Program; Altai State University (Russian Federation) FX Funding support for this study was provided by NASA Van Allen Probes (formerly known as the Radiation Belt Storm Probes (RBSP)) Project, the NASA LWS Program, and Altai State University (Russian Federation). NR 27 TC 1 Z9 1 U1 0 U2 9 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD AUG PY 2014 VL 21 IS 8 AR 082901 DI 10.1063/1.4892185 PG 8 WC Physics, Fluids & Plasmas SC Physics GA AQ4IZ UT WOS:000342760600056 ER PT J AU Mackey, J Dynys, F Sehirlioglu, A AF Mackey, Jon Dynys, Frederick Sehirlioglu, Alp TI Uncertainty analysis for common Seebeck and electrical resistivity measurement systems SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID THERMAL-CONDUCTIVITY; HIGH-TEMPERATURE; THERMOELECTRIC PROPERTIES; COEFFICIENT; THERMOPOWER; APPARATUS; POWER AB This work establishes the level of uncertainty for electrical measurements commonly made on thermoelectric samples. The analysis targets measurement systems based on the four probe method. Sources of uncertainty for both electrical resistivity and Seebeck coefficient were identified and evaluated. Included are reasonable estimates on the magnitude of each source, and cumulative propagation of error. Uncertainty for the Seebeck coefficient includes the cold-finger effect which has been quantified with thermal finite element analysis. The cold-finger effect, which is a result of parasitic heat transfer down the thermocouple probes, leads to an asymmetric over-estimation of the Seebeck coefficient. A silicon germanium thermoelectric sample has been characterized to provide an understanding of the total measurement uncertainty. The electrical resistivity was determined to contain uncertainty of +/- 7.0% across any measurement temperature. The Seebeck coefficient of the system is +1.0%/-13.1% at high temperature and +/- 1.0% near room temperature. The power factor has a combined uncertainty of +7.3%/-27.0% at high temperature and +/- 7.5% near room temperature. These ranges are calculated to be typical values for a general four probe Seebeck and resistivity measurement configuration. (C) 2014 AIP Publishing LLC. C1 [Mackey, Jon] Univ Akron, Dept Mech Engn, Akron, OH 44325 USA. [Dynys, Frederick] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Sehirlioglu, Alp] Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA. RP Mackey, J (reprint author), Univ Akron, Dept Mech Engn, Akron, OH 44325 USA. EM jam151@zips.uakron.edu FU NASA/USRA [04555-004] FX The authors of this work would like to thank the assistance of Tom Sabo, Ben Kowalski, and Ray Babuder from NASA Glenn Research Center (GRC), and funding provided by NASA/USRA Contract No. 04555-004. NR 33 TC 16 Z9 16 U1 3 U2 26 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 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD AUG PY 2014 VL 85 IS 8 AR 085119 DI 10.1063/1.4893652 PG 10 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA AQ6IH UT WOS:000342913500086 PM 25173324 ER PT J AU Hossain, F Siddique-E-Akbor, AHM Yigzaw, W Shah-Newaz, S Hossain, M Mazumder, LC Ahmed, T Shum, CK Lee, H Biancamaria, S Turk, FJ Limaye, A AF Hossain, Faisal Siddique-E-Akbor, A. H. M. Yigzaw, Wondmagegn Shah-Newaz, Sardar Hossain, Monowar Mazumder, Liton Chandra Ahmed, Tanvir Shum, C. K. Lee, Hyongki Biancamaria, Sylvain Turk, Francis J. Limaye, Ashutosh TI CROSSING THE "VALLEY OF DEATH" Lessons Learned from Implementing an Operational Satellite-Based Flood Forecasting System SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article C1 [Hossain, Faisal; Siddique-E-Akbor, A. H. M.; Yigzaw, Wondmagegn] Tennessee Technol Univ, Dept Civil & Environm Engn, Cookeville, TN 38505 USA. [Shah-Newaz, Sardar; Hossain, Monowar; Mazumder, Liton Chandra; Ahmed, Tanvir] Inst Water Modelling, Dhaka, Bangladesh. [Shum, C. K.] Ohio State Univ, Columbus, OH 43210 USA. [Shum, C. K.] Chinese Acad Sci, Inst Geodesy & Geophys, Beijing, Peoples R China. [Lee, Hyongki] Univ Houston, Houston, TX USA. [Biancamaria, Sylvain] CNRS, Lab Etud Geophys & Oceanog Spatiales, Toulouse, France. [Turk, Francis J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Limaye, Ashutosh] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Hossain, F (reprint author), Univ Washington, 201 More Hall,Box 352700, Seattle, WA 98105 USA. EM fhossain@uw.edu NR 12 TC 6 Z9 6 U1 1 U2 6 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD AUG PY 2014 VL 95 IS 8 BP 1201 EP 1207 DI 10.1175/BAMS-D-13-00176.1 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AQ1PD UT WOS:000342552400008 ER PT J AU Vinogradova, NT Ponte, RM Fukumori, I Wang, O AF Vinogradova, Nadya T. Ponte, Rui M. Fukumori, Ichiro Wang, Ou TI Estimating satellite salinity errors for assimilation of Aquarius and SMOS data into climate models SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID SEA-SURFACE SALINITY; OCEAN; CIRCULATION; PERFORMANCE AB Constraining dynamical systems with new information from ocean measurements, including observations of sea surface salinity (SSS) from Aquarius and SMOS, requires careful consideration of data errors that are used to determine the importance of constraints in the optimization. Here such errors are derived by comparing satellite SSS observations from Aquarius and SMOS with ocean model output and in situ data. The associated data error variance maps have a complex spatial pattern, ranging from less than 0.05 in the open ocean to 1-2 (units of salinity variance) along the coasts and high latitude regions. Comparing the data-model misfits to the data errors indicates that the Aquarius and SMOS constraints could potentially affect estimated SSS values in several ocean regions, including most tropical latitudes. In reference to the Aquarius error budget, derived errors are less than the total allocation errors for the Aquarius mission accuracy requirements in low and midlatitudes, but exceed allocation errors in high latitudes. C1 [Vinogradova, Nadya T.; Ponte, Rui M.] Atmospher & Environm Res Inc AER, Lexington, MA 02421 USA. [Fukumori, Ichiro; Wang, Ou] NASA, Jet Prop Lab, Pasadena, CA USA. RP Vinogradova, NT (reprint author), Atmospher & Environm Res Inc AER, Lexington, MA 02421 USA. EM nadya@aer.com FU NASA's Physical Oceanography Program; Ocean Surface Salinity Project [NNH10CC10C, NNH14CL48C]; Spanish National Program on Space FX This work was supported by NASA's Physical Oceanography Program and the Ocean Surface Salinity Project through contracts NNH10CC10C and NNH14CL48C to AER. Aquarius data are provided by NASA's Physical Oceanography Distributed Active Archive Center (PO.DAAC) and can be accessed at: http://podaac.jpl.nasa.gov/SeaSurfaceSalinity/Aquarius. SMOS data were produced by the Barcelona Expert Center (www.smos-bec.icm.csic.es), a joint initiative of the Spanish Research Council (CSIC) and the Technical University of Catalonia (UPC), mainly funded by the Spanish National Program on Space. SMOS data access: http://cp34-bec.cmima.csic.es/thredds/catalog/REPOI_001M025B/catalog.htm l. The in situ data used in this paper are available at http://www.metoffice.gov.uk/hadobs/en3/data/EN3_v2a/download_EN3_v2a.htm l. We thank our ECCO colleagues from MIT, Gael Forget and Patrick Heimbach, for all their efforts on the production of ECCO-version 4. We appreciate useful feedback and suggestions from two anonymous reviewers and the Associate Editor who helped us improve our manuscript. NR 28 TC 7 Z9 7 U1 3 U2 15 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 AUG PY 2014 VL 119 IS 8 BP 4732 EP 4744 DI 10.1002/2014JC009906 PG 13 WC Oceanography SC Oceanography GA AQ1CR UT WOS:000342519500003 ER PT J AU Tang, WQ Yueh, SH Fore, AG Hayashi, A Lee, T Lagerloef, G AF Tang, Wenqing Yueh, Simon H. Fore, Alexander G. Hayashi, Akiko Lee, Tong Lagerloef, Gary TI Uncertainty of Aquarius sea surface salinity retrieved under rainy conditions and its implication on the water cycle study SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID DIELECTRIC-CONSTANT; OCEAN ALGORITHM; MIXED-LAYER; ARGO; TEMPERATURE; VARIABILITY; BACKSCATTER; CHALLENGE; MODEL AB The uncertainty of Aquarius sea surface salinity (SSS) retrieved under rain is assessed. Rain not only has instantaneous impact on SSS but also interferes with the microwave remote sensing signals, making the task to retrieve SSS under rainy conditions difficult. A rain correction model is developed based on analysis of the L-band radiometer/scatterometer residual signals after accounting for roughness due to wind and flat surface emissivity. The combined active passive algorithm is used to retrieve SSS in parallel with (CAP_RC) or without rain correction (CAP). The CAP bias against individual ARGO floats increases with rain rate with slope of -0.14 PSU per mm h(-1), which reduced to near zero in CAP_RC. On the global monthly basis, CAP_RC is about 0.03 PSU higher than CAP. RMSD against ARGO is slightly smaller for CAP_RC than CAP. Regional biases are examined in areas with frequent rain events. As expected, results show that Delta SSS (CAP_RC-CAP) is highly correlated with the seasonal precipitation pattern, reaching about 0.2-0.3 PSU under heavy rain. However, Delta SSS shows no correlation with the difference pattern between ARGO and CAP or CAP_RC. This, along with regional analyses, suggests that the difference between ARGO and Aquarius' SSS is likely caused by the different spatial and temporal sampling, in addition to near surface stratification depicted by radiometer and ARGO at different depths. The effect of Delta SSS on water cycle in terms of mixed-layer salt storage tendency is about 10% in areas where evaporation-minus-precipitation is the dominant process driving the variability of near surface salinity. C1 [Tang, Wenqing; Yueh, Simon H.; Fore, Alexander G.; Hayashi, Akiko; Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Lagerloef, Gary] Earth & Space Res, Seattle, WA USA. RP Tang, WQ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Wenqing.Tang@jpl.nasa.gov FU National Aeronautics and Space Administration FX The work described in this paper carried out by the Jet Propulsion Laboratory, California Institute of Technology was under a contract with the National Aeronautics and Space Administration. The authors thank two anonymous reviewers for their comments for improving this article. Aquarius SSS data are available from http://podaac.jpl.nasa.gov; SSMI/S and WindSAT rain data are downloaded from www.remss.com; ARGO monthly gridded data from http://www.jamstec.go.jp/ARGO; ARGO individual floats data collocated with Aquarius from https://aquarius.esr.org/avds; and OAFlux evaporation from http://oaflux.whoi.edu. NR 32 TC 13 Z9 13 U1 1 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD AUG PY 2014 VL 119 IS 8 BP 4821 EP 4839 DI 10.1002/2014JC009834 PG 19 WC Oceanography SC Oceanography GA AQ1CR UT WOS:000342519500008 ER PT J AU Martin, ACH Boutin, J Hauser, D Dinnat, EP AF Martin, A. C. H. Boutin, J. Hauser, D. Dinnat, E. P. TI Active-passive synergy for interpreting ocean L-band emissivity: Results from the CAROLS airborne campaigns SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID SEA-SURFACE SALINITY; MICROWAVE RADIOMETRY; FIELD EXPERIMENTS; SMOS; RFI; MODEL AB The impact of the ocean surface roughness on the ocean L-band emissivity is investigated using simultaneous airborne measurements from an L-band radiometer (CAROLS) and from a C-band scatterometer (STORM) acquired in the Gulf of Biscay (off-the French Atlantic coasts) in November 2010. Two synergetic approaches are used to investigate the impact of surface roughness on the L-band brightness temperature (Tb). First, wind derived from the scatterometer measurements is used to analyze the roughness contribution to Tb as a function of wind and compare it with the one simulated by SMOS and Aquarius roughness models. Then residuals from this mean relationship are analyzed in terms of mean square slope derived from the STORM instrument. We show improvement of new radiometric roughness models derived from SMOS and Aquarius satellite measurements in comparison with prelaunch models. Influence of wind azimuth on Tb could not be evidenced from our data set. However, we point out the importance of taking into account large roughness scales (>20 cm) in addition to small roughness scale (5 cm) rapidly affected by wind to interpret radiometric measurements far from nadir. This was made possible thanks to simultaneous estimates of large and small roughness scales using STORM at small (7-16 degrees) and large (30 degrees) incidence angles. C1 [Martin, A. C. H.; Boutin, J.] Univ Paris 06, Sorbonne Univ, IRD, MNHN,LOCEAN IPSL, Paris, France. [Martin, A. C. H.] Natl Oceanog Ctr, Southampton, Hants, England. [Hauser, D.] Univ Paris 06, Sorbonne Univ, Univ Versailles St Quentin, CNRS,LATMOS IPSL, Guyancourt, France. [Dinnat, E. P.] Chapman Univ, Ctr Excellence Earth Syst Modeling & Observat, Orange, CA USA. [Dinnat, E. P.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. RP Martin, ACH (reprint author), Univ Paris 06, Sorbonne Univ, IRD, MNHN,LOCEAN IPSL, Paris, France. EM admartin@noc.ac.uk RI Dinnat, Emmanuel/D-7064-2012; Boutin, Jacqueline/M-2253-2016 OI Dinnat, Emmanuel/0000-0001-9003-1182; FU French Space Agency CNES/TOSCA; CNES/CNRS grant FX The authors acknowledge Mehrez Zribi, Pascal Fanise, and Mickael Parde for providing CAROLS measurements. The authors wish to thank the crew of the RV Cotes de la Manche as well as the technical teams from SAFIRE and DT-INSU. The authors also thank Gerard Caudal and Xiaobin Yin for very fruitful discussions, Joe Tenerelli for providing the Terrestrial Radiometry Analysis Package and Nicolas Martin for computation support. The authors thank Meteo France for providing data for the Gascogne Buoy and for providing us support during the airborne campaign. The authors also acknowledge Remote Sensing Systems for providing free and open access to SSMIS measurements. The development of the CAROLS instrument and the flight campaigns have been funded through the support of the French Space Agency CNES/TOSCA. Adrien Martin has been funded by a CNES/CNRS grant. NR 47 TC 2 Z9 2 U1 0 U2 4 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 AUG PY 2014 VL 119 IS 8 BP 4940 EP 4957 DI 10.1002/2014JC009890 PG 18 WC Oceanography SC Oceanography GA AQ1CR UT WOS:000342519500013 ER PT J AU Yueh, S Tang, WQ Fore, A Hayashi, A Song, YT Lagerloef, G AF Yueh, Simon Tang, Wenqing Fore, Alexander Hayashi, Akiko Song, Yuhe T. Lagerloef, Gary TI Aquarius geophysical model function and combined active passive algorithm for ocean surface salinity and wind retrieval SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID SEA-SURFACE; DIELECTRIC-CONSTANT; TEMPERATURE; CHALLENGE; WATER; ARGO AB This paper describes the updated Combined Active-Passive (CAP) retrieval algorithm for simultaneous retrieval of surface salinity and wind from Aquarius' brightness temperature and radar backscatter. Unlike the algorithm developed by Remote Sensing Systems (RSS), implemented in the Aquarius Data Processing System (ADPS) to produce Aquarius standard products, the Jet Propulsion Laboratory's CAP algorithm does not require monthly climatology SSS maps for the salinity retrieval. Furthermore, the ADPS-RSS algorithm fully uses the National Center for Environmental Predictions (NCEP) wind for data correction, while the CAP algorithm uses the NCEP wind only as a constraint. The major updates to the CAP algorithm include the galactic reflection correction, Faraday rotation, Antenna Pattern Correction, and geophysical model functions of wind or wave impacts. Recognizing the limitation of geometric optics scattering, we improve the modeling of the reflection of galactic radiation; the results are better salinity accuracy and significantly reduced ascending-descending bias. We assess the accuracy of CAP's salinity by comparison with ARGO monthly gridded salinity products provided by the Asia-Pacific Data-Research Center (APDRC) and Japan Agency for Marine-Earth Science and Technology (JAMSTEC). The RMS differences between Aquarius CAP and APDRC's or JAMSTEC's ARGO salinities are less than 0.2 psu for most parts of the ocean, except for the regions in the Intertropical Convergence Zone, near the outflow of major rivers and at high latitudes. C1 [Yueh, Simon; Tang, Wenqing; Fore, Alexander; Hayashi, Akiko; Song, Yuhe T.; Lagerloef, Gary] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Yueh, S (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Simon.Yueh@jpl.nasa.gov FU National Aeronautics and Space Administration FX The work described in this paper was carried out by the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. The Aquarius data were obtained from the NASA Physical Oceanography Distributed Active Archive Center, http://podaac.jpl.nasa.gov/aquarius. NR 38 TC 16 Z9 16 U1 1 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 AUG PY 2014 VL 119 IS 8 BP 5360 EP 5379 DI 10.1002/2014JC009939 PG 20 WC Oceanography SC Oceanography GA AQ1CR UT WOS:000342519500037 ER PT J AU Webster, MA Rigor, IG Nghiem, SV Kurtz, NT Farrell, SL Perovich, DK Sturm, M AF Webster, Melinda A. Rigor, Ignatius G. Nghiem, Son V. Kurtz, Nathan T. Farrell, Sinead L. Perovich, Donald K. Sturm, Matthew TI Interdecadal changes in snow depth on Arctic sea ice SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID THERMAL-CONDUCTIVITY; THICKNESS; PRODUCTS AB Snow plays a key role in the growth and decay of Arctic sea ice. In winter, it insulates sea ice from cold air temperatures, slowing sea ice growth. From spring to summer, the albedo of snow determines how much insolation is absorbed by the sea ice and underlying ocean, impacting ice melt processes. Knowledge of the contemporary snow depth distribution is essential for estimating sea ice thickness and volume, and for understanding and modeling sea ice thermodynamics in the changing Arctic. This study assesses spring snow depth distribution on Arctic sea ice using airborne radar observations from Operation IceBridge for 2009-2013. Data were validated using coordinated in situ measurements taken in March 2012 during the Bromine, Ozone, and Mercury Experiment (BROMEX) field campaign. We find a correlation of 0.59 and root-mean-square error of 5.8 cm between the airborne and in situ data. Using this relationship and Ice-Bridge snow thickness products, we compared the recent results with data from the 1937, 1954-1991 Soviet drifting ice stations. The comparison shows thinning of the snowpack, from 35.1 +/- 9.4 to 22.2 +/- 1.9 cm in the western Arctic, and from 32.8 +/- 9.4 to 14.5 +/- 1.9 cm in the Beaufort and Chukchi seas. These changes suggest a snow depth decline of 37 +/- 29% in the western Arctic and 56 +/- 33% in the Beaufort and Chukchi seas. Thinning is negatively correlated with the delayed onset of sea ice freezeup during autumn. C1 [Webster, Melinda A.; Rigor, Ignatius G.] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA. [Nghiem, Son V.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Kurtz, Nathan T.; Farrell, Sinead L.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. [Farrell, Sinead L.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Perovich, Donald K.] US Army Corps Engineers, Engn Res & Dev Ctr, Cold Reg Res & Engn Lab, Hanover, NH USA. [Sturm, Matthew] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. RP Webster, MA (reprint author), Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA. EM melindaw@uw.edu RI Farrell, Sinead/F-5586-2010 OI Farrell, Sinead/0000-0003-3222-2751 FU NASA Cryospheric Sciences Program FX Snow data from the 2012 BROMEX field campaign are available upon request. Meteorological data are available at http://www.esrl.noaa.gov/gmd/dv/. The IceBridge quick-look and standard snow depth products are available at https://nsidc.org/data/docs /daac/icebridge/evaluation_products/sea-ice-freeboard-snowdepththickness -quicklook-index.html and http://nsidc. org/data/idcsi2.html. The Soviet station snow data are available at http://dx.doi.org/10.7265/N5MS3QNJ. Ice Mass Balance buoy data are available at http://IMB.crrel.usace.army.mil. The sea ice freezeup product from passive microwave satellite data is available at http://neptune.gsfc.nasa.gov/csb/index.php? section=54. This research was supported by the National Aeronautics and Space Administration (NASA), and by contributors to the U.S. Interagency Arctic Buoy Program, which include the U.S. Coast Guard, NAVO, NIC, NOAA, NSF, and ONR. This is JISAO contribution 2225. The research carried out at the Jet Propulsion Laboratory, California Institute of Technology, was supported by the NASA Cryospheric Sciences Program. We thank Jacqueline A. Richter-Menge of the U.S. Army Cold Regions Research and Engineering Laboratory for the planning and coordination of the IceBridge flight operation with the BROMEX field campaign, and Stephen Warren for helpful discussions. We thank UMIAQ, the Barrow whaling community, and the Barrow Arctic Science Consortium for their assistance in the BROMEX field campaign. NR 42 TC 27 Z9 28 U1 4 U2 29 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 AUG PY 2014 VL 119 IS 8 BP 5395 EP 5406 DI 10.1002/2014JC009985 PG 12 WC Oceanography SC Oceanography GA AQ1CR UT WOS:000342519500039 ER PT J AU Chaussard, E Burgmann, R Shirzaei, M Fielding, EJ Baker, B AF Chaussard, E. Buergmann, R. Shirzaei, M. Fielding, E. J. Baker, B. TI Predictability of hydraulic head changes and characterization of aquifer-system and fault properties from InSAR-derived ground deformation SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID APERTURE RADAR INTERFEROMETRY; SANTA-CLARA-VALLEY; LAS-VEGAS VALLEY; LAND SUBSIDENCE; PRINCIPAL COMPONENTS; SURFACE DEFORMATION; HAYWARD FAULT; CALIFORNIA; BASIN; SAR AB We evaluate the benefits of space-derived ground deformation measurements for basin-wide characterization of aquifer-system properties and groundwater levels. We use Interferometric Synthetic Aperture Radar (InSAR) time series analysis of ERS, Envisat, and ALOS SAR data to resolve 1992-2011 ground deformation in the Santa Clara Valley, California. T-mode principal component analysis successfully isolates temporally variable deformation patterns embedded in the multidecadal time series. The data reveal uplift at 0.4 cm/yr between 1992 and 2000 and <0.1 cm/yr during 2000-2011, illustrating the end of the aquifer-system's poroelastic rebound following recovery of hydraulic heads after the 1960s low stand. In addition, seasonal elastic deformation with amplitude of up to 3 cm, in phase with head fluctuations, is observed over the confined aquifer sharply partitioned by the Quaternary Silver Creek Fault (SCF). Integration of this deformation with hydraulic head data enables characterization of the aquifer-system storativity and elastic skeletal specific storage. Modeling of the deformation partitioning across the SCF constrains the fault's last tectonic activity, hydraulic conductivity, and material composition. The SCF likely cuts the shallow confining clays and was last active since similar to 140 ka, it has a horizontal hydraulic conductivity several orders of magnitude lower than the surrounding aquifer-system, and is likely composed of clays, making it an effective barrier to across-fault fluid flow. Finally, we show that after a period of calibration, InSAR can be used to characterize basin-wide water level changes without well measurements with an accuracy of 70%, which demonstrates that it provides useful data for groundwater management. C1 [Chaussard, E.; Buergmann, R.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Chaussard, E.; Buergmann, R.] Univ Calif Berkeley, Berkeley Seismol Lab, Berkeley, CA 94720 USA. [Shirzaei, M.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Fielding, E. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Baker, B.] Santa Clara Valley Water Dist, San Jose, CA USA. RP Chaussard, E (reprint author), Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. EM estelle@seismo.berkeley.edu OI Chaussard, Estelle/0000-0002-2291-7085 FU National Aeronautics and Space Administration (NASA) [NNX12AQ32G]; Earth Surface and Interior focus area at NASA FX We thank the National Aeronautics and Space Administration (NASA) for support through grant NNX12AQ32G. We thank Thomas Burbey and Devin Galloway for their thoughtful comments prior to submission. We also thank the Associate Editor, Devin Galloway, and an anonymous reviewer for the reviews, which helped improve the quality of the manuscript. We thank the Santa Clara Valley Water District for the hydraulic head data. The ERS and Envisat original data are copyrighted by the European Space Agency and were provided through the WInSAR archive. The ALOS-PALSAR data are copyrighted by the Japanese Aerospace Exploration Agency (JAXA) and Ministry of Economy, Trade, and Industry and were made available by the U.S. Government Research Consortium through the Alaska Satellite Facility. Part of this research was supported by the Earth Surface and Interior focus area at NASA and performed at the Jet Propulsion Laboratory, California Institute of Technology. NR 94 TC 20 Z9 20 U1 3 U2 25 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD AUG PY 2014 VL 119 IS 8 BP 6572 EP 6590 DI 10.1002/2014JB011266 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ1AD UT WOS:000342512900025 ER PT J AU Force, DA AF Force, Dale A. TI Shaped, Fixed Antenna for One Gigabit per Second Data Rate Transmission from Earth Exploration Satellites in Low Earth Orbit SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE LA English DT Article C1 [Force, Dale A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Force, DA (reprint author), NASA, Glenn Res Ctr, Commun & Intelligent Syst Div, 21000 Brookpk Rd,MS 54-1, Cleveland, OH 44135 USA. EM Dale.A.Force@nasa.gov NR 10 TC 0 Z9 0 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0885-8985 EI 1557-959X J9 IEEE AERO EL SYS MAG JI IEEE Aerosp. Electron. Syst. Mag. PD AUG PY 2014 VL 29 IS 8 BP 4 EP 9 DI 10.1109/MAES.2014.120067 PG 6 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA AP7SZ UT WOS:000342278300002 ER PT J AU Solomonidou, A Hirtzig, M Coustenis, A Bratsolis, E Le Mouelic, S Rodriguez, S Stephan, K Drossart, P Sotin, C Jaumann, R Brown, RH Kyriakopoulos, K Lopes, RMC Bampasidis, G Stamatelopoulou-Seymour, K Moussas, X AF Solomonidou, A. Hirtzig, M. Coustenis, A. Bratsolis, E. Le Mouelic, S. Rodriguez, S. Stephan, K. Drossart, P. Sotin, C. Jaumann, R. Brown, R. H. Kyriakopoulos, K. Lopes, R. M. C. Bampasidis, G. Stamatelopoulou-Seymour, K. Moussas, X. TI Surface albedo spectral properties of geologically interesting areas on Titan SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID HUYGENS LANDING SITE; 5 MU-M; CASSINI VIMS; POSSIBLE ORIGIN; RADAR MAPPER; ATMOSPHERE; FEATURES; METHANE; MODEL; CRYOVOLCANISM AB We investigate the nature and possible formation processes of three areas on Titan's surface which have been suggested as geologically interesting: Hotei Regio, Tui Regio, and Sotra Patera. We also reanalyze the spectral characteristics of the Huygens Landing Site. We apply a statistical Principal Component Analysis (PCA) and a radiative transfer (RT) method on the Visual and Infrared Mapping Spectrometer Datacubes in order to retrieve the surface albedo of distinct spectral units in the near infrared. We have been able to exploit only a subset of the currently available Hotei Regio data, which are, in general, not optimal in terms of geometry for an analysis with a plane-parallel RT code. Our inferred surface albedos present generally higher values from 1 to 2 mu m and lower ones at 0.94 and in the 2.6-5 mu m region. The Regions of Interest (RoIs) within Hotei Regio, Tui Regio, and Sotra Patera are always significantly brighter than the surrounding areas. The largest variations are found longward of 2 mu m and mainly at 5 mu m. This higher surface albedo with respect to the surrounding area and, in general, the fact that the spectral behavior is different for each of these areas, is probably indicative of diverse chemical compositions and origins. We compare the spectral albedos with some suggested surface candidates on Titan (such as H2O, CO2, and CH4 ices, as well as tholin) and discuss possible chemical composition variations as well as other interpretations. C1 [Solomonidou, A.; Sotin, C.; Lopes, R. M. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Solomonidou, A.; Hirtzig, M.; Coustenis, A.; Drossart, P.; Bampasidis, G.] Paris VI Paris Diderot Univ, UPMC Univ, CNRS, LESIA,Observ Paris, Meudon, France. [Hirtzig, M.] Fdn Main Pate, Montrouge, France. [Bratsolis, E.; Bampasidis, G.; Moussas, X.] Univ Athens, Dept Phys, Athens, Greece. [Le Mouelic, S.] Univ Nantes, CNRS, UMR 6112, Lab Planetol & Geodynam,LPGNantes, Nantes, France. [Rodriguez, S.] Univ Paris 07, CNRS, CEA Saclay, Lab AIM,DSM,IRFU,SAp, Paris, France. [Stephan, K.; Jaumann, R.] DLR, Inst Planetary Res, Berlin, Germany. [Brown, R. H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Kyriakopoulos, K.] Univ Athens, Dept Geol & Geoenvironm, Athens, Greece. [Stamatelopoulou-Seymour, K.] Univ Patras, Dept Geol, Patras, Greece. [Stamatelopoulou-Seymour, K.] Concordia Univ, Dept Geog, Montreal, PQ, Canada. RP Solomonidou, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Anezina.Solomonidou@jpl.nasa.gov RI Lopes, Rosaly/D-1608-2016; Rodriguez, Sebastien/H-5902-2016 OI Lopes, Rosaly/0000-0002-7928-3167; Rodriguez, Sebastien/0000-0003-1219-0641 FU European Union (European Social Fund-ESF); Operational Program "Education and Lifelong Learning" of the National Strategic Reference Framework (NSRF)-Research Funding Program: Heracleitus II; NASA; French "Agence Nationale de la Recherche", France [11BS56002] FX This research has been cofinanced by the European Union (European Social Fund-ESF) and Greek national funds through the Operational Program "Education and Lifelong Learning" of the National Strategic Reference Framework (NSRF)-Research Funding Program: Heracleitus II. Investing in knowledge society through the European Social Fund. The research was also partly supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. A. C., S. L. M., S. R., C. S., P. D., and M. H. acknowledge financial support from the French "Agence Nationale de la Recherche" (ANR Project: CH4@Titan and/or ANR project "APOSTIC" 11BS56002), France. Part of the research was carried out by A. S. at the National and Kapodistrian University of Athens, Department of Geology and Geoenvironment. We thank Jason W. Barnes and an anonymous referee for their thorough and constructive reviews of the manuscript. NR 85 TC 11 Z9 11 U1 3 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG PY 2014 VL 119 IS 8 BP 1729 EP 1747 DI 10.1002/2014JE004634 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ0ZA UT WOS:000342510000001 ER PT J AU Heavens, NG Johnson, MS Abdou, WA Kass, DM Kleinbohl, A McCleese, DJ Shirley, JH Wilson, RJ AF Heavens, Nicholas G. Johnson, Morgan S. Abdou, Wedad A. Kass, David M. Kleinboehl, Armin McCleese, Daniel J. Shirley, James H. Wilson, R. John TI Seasonal and diurnal variability of detached dust layers in the tropical Martian atmosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID GENERAL-CIRCULATION MODEL; ORBITER CAMERA OBSERVATIONS; WATER-ICE CLOUDS; MARS; CRYSTALS; AGGREGATION; SIMULATION; STORMS; CYCLE; OCCULTATIONS AB Evidence for widespread nonuniform vertical mixing of dust in Mars's tropical atmosphere (in the form of features called "detached dust layers" or DDLs) is a challenge for atmospheric modeling. We characterize the seasonal, diurnal, and geographic variability of DDL activity in retrievals from observations by the Mars Climate Sounder onboard Mars Reconnaissance Orbiter. We find that dust injection above the boundary layer, which forms DDLs, is a spatially ubiquitous phenomenon in the tropics during the daytime, implying that it has a significant nontopographic component. DDL formation is more intense in northern spring and summer than in southern spring and summer but is still common when the zonal average dust distribution appears uniformly mixed. DDLs do not appear to follow the upwelling associated with Mars's Hadley circulation or the extant climatology of local dust storm activity in the tropics. Geographic variability in the nightside vertical dust distribution does not always correlate with the dayside vertical dust distribution, implying that there is spatial and seasonal variability in the efficiency of dust deposition/removal processes. Nighttime dust removal is especially efficient over the Tharsis Montes during northern spring and summer, which suggests some association between water ice clouds and removal. Intense injection combined with efficient removal results in a high amplitude of diurnal variability in the dust distribution at 15-30 km above the surface of the tropics during much of the Martian year. C1 [Heavens, Nicholas G.] Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA. [Johnson, Morgan S.] Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA. [Abdou, Wedad A.; Kass, David M.; Kleinboehl, Armin; McCleese, Daniel J.; Shirley, James H.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA. [Wilson, R. John] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. RP Heavens, NG (reprint author), Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA. EM nicholas.heavens@hamptonu.edu OI Heavens, Nicholas/0000-0001-7654-503X FU NASA Jet Propulsion Laboratory, California Institute of Technology [1471216] FX N.G. Heavens and M. S. Johnson acknowledge support from the NASA Jet Propulsion Laboratory, California Institute of Technology (subcontract 1471216). M. S. Johnson was hosted at Hampton University as part of the CREST Undergraduate Research Experience program. We thank Aymeric Spiga and an anonymous reviewer for their thorough reviews, which significantly improved this paper. All MRO-MCS data used to produce the results of this paper are freely available from NASA's Planetary Data System. Any analytical code is available from the first author by request. NOAA GFDL Mars model output is available from author Wilson by request. NR 56 TC 5 Z9 5 U1 1 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG PY 2014 VL 119 IS 8 BP 1748 EP 1774 DI 10.1002/2014JE004619 PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ0ZA UT WOS:000342510000002 ER PT J AU Jordan, AP Stubbs, TJ Wilson, JK Schwadron, NA Spence, HE Joyce, CJ AF Jordan, A. P. Stubbs, T. J. Wilson, J. K. Schwadron, N. A. Spence, H. E. Joyce, C. J. TI Deep dielectric charging of regolith within the Moon's permanently shadowed regions SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LUNAR PLASMA WAKE; SOLID DIELECTRICS; SPACECRAFT; BREAKDOWN; PROTON; ACCELERATION; ENVIRONMENT; FIELDS; PULSES; MODEL AB Energetic charged particles, such as galactic cosmic rays (GCRs) and solar energetic particles (SEPs), can penetrate deep within the lunar surface, resulting in deep dielectric charging. This charging process depends on the GCR and SEP currents, as well as on the regolith's electrical conductivity and permittivity. In permanently shadowed regions (PSRs) near the lunar poles, the discharging timescales are on the order of a lunation (similar to 20 days). We present the first predictions for deep dielectric charging of lunar regolith. To estimate the resulting subsurface electric fields, we develop a data-driven, one-dimensional, time-dependent model. For model inputs, we use GCR data from the Cosmic Ray Telescope for the Effects of Radiation on board the Lunar Reconnaissance Orbiter and SEP data from the Electron, Proton, and Alpha Monitor on the Advanced Composition Explorer. We find that during the recent solar minimum, GCRs create persistent electric fields up to similar to 700 V/m. We also find that large SEP events create transient but strong electric fields (>= 10(6) V/m) that may induce dielectric breakdown. Such breakdown would likely result in significant modifications to the physical and chemical properties of the lunar regolith within PSRs. C1 [Jordan, A. P.; Wilson, J. K.; Schwadron, N. A.; Spence, H. E.; Joyce, C. J.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Stubbs, T. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Jordan, AP (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. EM a.p.jordan@unh.edu RI Stubbs, Timothy/I-5139-2013 OI Stubbs, Timothy/0000-0002-5524-645X FU NASA [NNG11PA03C, NNX10AB17A] FX This work was supported by NASA grant NNG11PA03C and NNX10AB17A. The authors wish to thank Larry Townsend for helpful discussions. The authors also thank the ACE/EPAM team and its Principal Investigator Robert Gold of JHU/APL for providing the ACE data via CDAWeb at http://cdaweb.gsfc.nasa.gov/. LRO/CRaTER Level 2 data are available at the NASA Planetary Data System at http://pds.nasa.gov. The PSTAR and ESTAR results are available from the NIST website at http://www.nist.gov. NR 65 TC 5 Z9 5 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG PY 2014 VL 119 IS 8 BP 1806 EP 1821 DI 10.1002/2014JE004648 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ0ZA UT WOS:000342510000004 ER PT J AU Martinez, GM Renno, N Fischer, E Borlina, CS Hallet, B Juarez, MD Vasavada, AR Ramos, M Hamilton, V Gomez-Elvira, J Haberle, RM AF Martinez, G. M. Renno, N. Fischer, E. Borlina, C. S. Hallet, B. Juarez, M. de la Torre Vasavada, A. R. Ramos, M. Hamilton, V. Gomez-Elvira, J. Haberle, R. M. TI Surface energy budget and thermal inertia at Gale Crater: Calculations from ground-based measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID BOUNDARY-LAYER; EMISSION SPECTROMETER; TEMPERATURE SENSOR; MERIDIANI-PLANUM; MARTIAN SURFACE; LANDING SITES; MARS; ROVER; MODEL; WATER AB The analysis of the surface energy budget (SEB) yields insights into soil-atmosphere interactions and local climates, while the analysis of the thermal inertia (I) of shallow subsurfaces provides context for evaluating geological features. Mars orbital data have been used to determine thermal inertias at horizontal scales of similar to 10(4) m(2) to similar to 10(7) m(2). Here we use measurements of ground temperature and atmospheric variables by Curiosity to calculate thermal inertias at Gale Crater at horizontal scales of similar to 10(2) m(2). We analyze three sols representing distinct environmental conditions and soil properties, sol 82 at Rocknest (RCK), sol 112 at Point Lake (PL), and sol 139 at Yellowknife Bay (YKB). Our results indicate that the largest thermal inertia I = 452 J m(-2) K-1 s(-1/2) (SI units used throughout this article) is found at YKB followed by PL with I = 306 and RCK with I = 295. These values are consistent with the expected thermal inertias for the types of terrain imaged by Mastcam and with previous satellite estimations at Gale Crater. We also calculate the SEB using data from measurements by Curiosity's Rover Environmental Monitoring Station and dust opacity values derived from measurements by Mastcam. The knowledge of the SEB and thermal inertia has the potential to enhance our understanding of the climate, the geology, and the habitability of Mars. C1 [Martinez, G. M.; Renno, N.; Fischer, E.; Borlina, C. S.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Hallet, B.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Juarez, M. de la Torre; Vasavada, A. R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Ramos, M.] Univ Alcala de Henares, Dept Fis, Madrid, Spain. [Hamilton, V.] SW Res Inst, Dep Space Studies, Boulder, CO USA. [Gomez-Elvira, J.] Ctr Astrobiol, Madrid, Spain. [Haberle, R. M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Martinez, GM (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM gemartin@umich.edu RI Ramos, Miguel/K-2230-2014 OI Ramos, Miguel/0000-0003-3648-6818 FU JPL [1449038] FX This research is supported by a grant from JPL 1449038. German Martinez wants to thank Harvey Elliott for his contribution to improve this work. We want to thank Hanna Sizemore and the anonymous reviewer for their excellent suggestions to improve the paper. We also thank the REMS Team for their support of this investigation. NR 42 TC 13 Z9 13 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG PY 2014 VL 119 IS 8 BP 1822 EP 1838 DI 10.1002/2014JE004618 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ0ZA UT WOS:000342510000005 ER PT J AU Arney, G Meadows, V Crisp, D Schmidt, SJ Bailey, J Robinson, T AF Arney, Giada Meadows, Victoria Crisp, David Schmidt, Sarah J. Bailey, Jeremy Robinson, Tyler TI Spatially resolved measurements of H2O, HCl, CO, OCS, SO2, cloud opacity, and acid concentration in the Venus near-infrared spectral windows SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LOWER ATMOSPHERE; DEEP ATMOSPHERE; WATER-VAPOR; DARK SIDE; RUNAWAY GREENHOUSE; CARBON-MONOXIDE; NIGHT SIDE; LINE LIST; ABSORPTION; SPECTROSCOPY AB We observed Venus with the Apache Point Observatory 3.5 m telescope TripleSpec spectrograph (R = 3500, lambda = 0.96-2.47 mu m) on 1-3 March 2009 and on 25, 27, and 30 November and 2-4 December 2010. With these observations and synthetic spectra generated with the Spectral Mapping and Atmospheric Radiative Transfer model, we produce the first simultaneous maps of cloud opacity, acid concentration, water vapor (H2O), hydrogen chloride (HCl), carbon dioxide (CO), carbonyl sulfide (OCS), and sulfur dioxide (SO2) abundances in the Venusian lower atmosphere. Water measured at wavelengths near 1.18 mu m (near-surface) averages 29 +/- 2 ppm (2009) and 27 +/- 2 ppm (2010) and measured near 1.74 mu m (15-30 km) averages 33 +/- 2 ppm (2009) and 32 +/- 2 ppm (2010). Water in both these altitude ranges is spatially homogeneous. Water measured near 2.4 mu m (30-45 km) averages 34 +/- 2 ppm (2009) and 33 +/- 3 ppm (2010) and is spatially inhomogeneous and variable. HCl ismeasured near 1.74 mu m to be 0.41 +/- 0.04 ppm (2009) and 0.42 +/- 0.05 ppm (2010). CO and OCS (2.3-2.5 mu m; 30-45 km in altitude) are spatially inhomogeneous and show anticorrelation. CO (35 km) averages 25 +/- 3 ppm (2009) and 22 +/- 2 ppm (2010). OCS (36 km) averages 0.44 +/- 0.10 ppm (2009) and 0.57 +/- 0.12 ppm (2010). SO2 measurements average 140 +/- 37 ppm (2009) and 126 +/- 32 ppm (2010). Many species display a hemispherical dichotomy in their distribution. We find considerable spatial variability suggesting active processes with conservation between species. The most variable regions are just below the Venus cloud deck, and these may be related to changes in atmospheric circulation or virga events. C1 [Arney, Giada; Meadows, Victoria] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Arney, Giada; Meadows, Victoria] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA. [Arney, Giada; Meadows, Victoria; Crisp, David; Robinson, Tyler] NAI Virtual Planetary Lab, Seattle, WA USA. [Crisp, David] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Schmidt, Sarah J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Bailey, Jeremy] Univ New S Wales, Sch Phys, Sydney, NSW, Australia. [Robinson, Tyler] NASA Ames Explorat Ctr, Mountain View, CA USA. RP Arney, G (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA. EM giada@astro.washington.edu FU National Aeronautics and Space Administration through NASA Astrobiology Institute [NNH05ZDA001C, NNH12ZDA002C, NNA08CN87A, NNA13AA93A]; University of Washington eScience Institute FX Observational data are available upon request from the author. This work was performed as part of the NASA Astrobiology Institute's Virtual Planetary Laboratory Lead Team, supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under solicitations NNH05ZDA001C and NNH12ZDA002C and Cooperative Agreement NNA08CN87A and NNA13AA93A. This work was additionally supported in part by the University of Washington eScience Institute. We thank Y. Yung for useful discussions and are grateful for our reviewers B. Bezard and C.C.C. Tsang for their thoughtful comments and suggestions which helped to improve the quality of this manuscript. NR 81 TC 13 Z9 13 U1 0 U2 23 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG PY 2014 VL 119 IS 8 BP 1860 EP 1891 DI 10.1002/2014JE004662 PG 32 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ0ZA UT WOS:000342510000007 ER PT J AU Clifford, SM Farmer, J Carr, MH Marais, DD Bibring, JP Craddock, R Newsom, H AF Clifford, Stephen M. Farmer, Jack Carr, Michael H. Marais, Dave Des Bibring, Jean-Pierre Craddock, Robert Newsom, Horton TI Introduction to the Early Mars III Special Section and Key Questions from the Third International Conference on Early Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID STRATIGRAPHY; EVENTS C1 [Clifford, Stephen M.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Farmer, Jack] Arizona State Univ, Dept Geol, Tempe, AZ 85287 USA. [Carr, Michael H.] US Geol Survey, Menlo Pk, CA 94025 USA. [Marais, Dave Des] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bibring, Jean-Pierre] IAS, Orsay, France. [Craddock, Robert] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Sci, Washington, DC 20560 USA. [Newsom, Horton] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. RP Clifford, SM (reprint author), Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA. EM clifford@lpi.usra.edu NR 15 TC 0 Z9 0 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG PY 2014 VL 119 IS 8 BP 1892 EP 1894 DI 10.1002/2014JE004643 PG 3 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ0ZA UT WOS:000342510000008 ER PT J AU Zhang, G Ganguly, S Nemani, RR White, MA Milesi, C Hashimoto, H Wang, WL Saatchi, S Yu, YF Myneni, RB AF Zhang, Gong Ganguly, Sangram Nemani, Ramakrishna R. White, Michael A. Milesi, Cristina Hashimoto, Hirofumi Wang, Weile Saatchi, Sassan Yu, Yifan Myneni, Ranga B. TI Estimation of forest aboveground biomass in California using canopy height and leaf area index estimated from satellite data SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Aboveground biomass; Leaf area index; Canopy height; Landsat; Uncertainty assessment ID SYSTEM DATA RECORD; LAND-COVER; ACCURACY ASSESSMENT; CARBON STOCKS; LIDAR; SURFACE; EMISSIONS; MODEL; USA; DEFORESTATION AB Accurate characterization of variability and trends in forest biomass at local to national scales is required for accounting of global carbon sources and sinks and monitoring their dynamics. Here we present a new remote sensing based approach for estimating live forest aboveground biomass (AGB) based on a simple parametric model that combines high-resolution estimates of leaf area index (LAI) from the Landsat Thematic Mapper sensor and canopy maximum height from the Geoscience Laser Altimeter System (GLAS) sensor onboard ICESat, the Ice, Cloud, and land Elevation Satellite. We tested our approach with a preliminary uncertainty assessment over the forested areas of California spanning a broad range of climatic and land-use conditions and find our AGB estimates to be comparable to estimates of AGB from inventory records and other available satellite-estimated AGB maps at aggregated scales. Our study offers a high-resolution approach to map forest aboveground biomass at regional-to-continental scales and assess sources of uncertainties in the estimates. (C) 2014 Elsevier Inc All fights reserved. C1 [Zhang, Gong; Ganguly, Sangram] NASA, BAERI, Ames Res Ctr, Moffett Field, CA 94035 USA. [Nemani, Ramakrishna R.] NASA, Adv Supercomp Div, Ames Res Ctr, Moffett Field, CA 94035 USA. [White, Michael A.] Nat Publishing Grp, San Francisco, CA USA. [Milesi, Cristina; Hashimoto, Hirofumi; Wang, Weile] Calif State Univ Monterey Bay, NASA, Ames Res Ctr, Dept Sci & Environm Policy, Moffett Field, CA 94035 USA. [Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Yu, Yifan] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. [Myneni, Ranga B.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. RP Zhang, G (reprint author), NASA, BAERI, Ames Res Ctr, Moffett Field, CA 94035 USA. EM zhanggong07@gmail.com RI Myneni, Ranga/F-5129-2012; OI White, Michael/0000-0002-0238-8913 FU Carbon Monitoring System (CMS) program at NASA FX We acknowledge funding from the Carbon Monitoring System (CMS) program at NASA. We thank the anonymous reviewers and editors for their constructive comments and edits to the manuscript. We are particularly grateful to Dr. Ronald E. McRoberts for all his critical inputs in improving the manuscript. This research was performed using the NASA Earth Exchange (NEX) computing facilities. NR 58 TC 15 Z9 21 U1 6 U2 55 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 AUG PY 2014 VL 151 SI SI BP 44 EP 56 DI 10.1016/j.rse.2014.01.025 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AP7NM UT WOS:000342264000005 ER PT J AU Williams, CA Collatz, GJ Masek, J Huang, CQ Goward, SN AF Williams, Christopher A. Collatz, G. James Masek, Jeffrey Huang, Chengquan Goward, Samuel N. TI Impacts of disturbance history on forest carbon stocks and fluxes: Merging satellite disturbance mapping with forest inventory data in a carbon cycle model framework SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Net ecosystem productivity; Carbon sequestration; Landsat change detection; Forest inventory and analysis; Conterminous United States ID COARSE WOODY DEBRIS; WESTERN OREGON; UNITED-STATES; ECOSYSTEM PRODUCTION; LANDSAT RECORD; BUDGET MODEL; TIME-SERIES; AGE; DYNAMICS; USA AB Forest carbon stocks and fluxes are highly dynamic following stand-clearing disturbances from severe fire and harvest and this presents a significant challenge for continental carbon budget assessments. In this work we use forest inventory data to parameterize a carbon cycle model to represent post-disturbance carbon trajectories of carbon pools and fluxes for specific forest types growing in high and low site productivity class settings. We then apply these trajectories to landscapes and regions based on forest age distributions derived from either the FIA data or from Landsat time series stacks (1985-2006) for 54 representative scenes throughout most of the conterminous United States. We estimate the net carbon uptake in forests caused by post-disturbance growth and decomposition ("regrowth sink") for forested regions across the country. At the landscape scale, the prevailing condition of positive net ecosystem productivity (NEP) is in stark contrast to local patches with large sources, particularly in the west where fires and clear cuts create contiguous disturbed patches. At the continental scale, regional differences in disturbance rates reflect management patterns of high disturbance rates in the Southeastern and South Central states, and lower disturbance rates in the Northeast and Northern Lakes States. Despite low contemporary disturbance rates in the Northeast and Northern Lakes States (0.61 and 0.74% y(-1)), the regrowth sink there remains of moderate to large strength (88 and 57 g C m(-2) y(-1)) owing to the continued legacy from historical clearing. Large regrowth sinks are also found in the Southeast, South Central, and Pacific Southwest regions (85, 86, and 95 g C m(2) y(-1)) where disturbance rates also tend to be higher (1.59, 1.38, and 0.93% y(-1)). Overall, the Landsat-derived disturbance rates are elevated relative to FIA-derived rates (1.19 versus 0.93% y(-1)) particularly for western regions. The differences only modestly adjust regional- and continental-scale carbon budgets, reducing NEP from forest regrowth by about 8%. (C) 2013 Elsevier Inc. All rights reserved. C1 [Williams, Christopher A.] Clark Univ, Grad Sch Geog, Worcester, MA 01610 USA. [Collatz, G. James; Masek, Jeffrey] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Huang, Chengquan; Goward, Samuel N.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. RP Williams, CA (reprint author), 950 Main St, Worcester, MA 01610 USA. EM cwilliams@clarku.edu RI collatz, george/D-5381-2012; Masek, Jeffrey/D-7673-2012; OI Huang, Chengquan/0000-0003-0055-9798 FU NASA [NNH05ZDA001N]; North American Carbon Program FX We thank Charles (Chip) Scott and his team at the USFS National Inventory and Monitoring Applications Center for providing us with FIA data. We acknowledge the helpful discussions and comments from Warren Cohen, Richard Houghton, Nancy Thomas, Karen Schleeweis, Robert Kennedy, Scott Powell, Sean Healey, and Gretchen Moisen, as well as from five anonymous reviewers. We would also like to thank the organizers of this Special Issue, including Warren Cohen, Ronald McRoberts, and Dirk Pflugmacher, for giving us the opportunity to contribute following the ForestSAT 2012 Conference. This work was funded by NASA NNH05ZDA001N, North American Carbon Program. NR 50 TC 2 Z9 3 U1 5 U2 60 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 AUG PY 2014 VL 151 SI SI BP 57 EP 71 DI 10.1016/j.rse.2013.10.034 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AP7NM UT WOS:000342264000006 ER PT J AU Beck, JD Kinch, M Sun, XL AF Beck, Jeffrey D. Kinch, Mike Sun, Xiaoli TI Update on linear mode photon counting with the HgCdTe linear mode avalanche photodiode SO OPTICAL ENGINEERING LA English DT Article DE single photon counting; avalanche photodiode; HgCdTe; avalanche photodiode; mid-wavelength infrared; excess noise factor; photon detection efficiency; false event rate ID DIODES AB The behavior of the gain-voltage characteristic of the mid-wavelength infrared cutoff HgCdTe linear mode avalanche photodiode (e-APD) is discussed both experimentally and theoretically as a function of the width of the multiplication region. Data are shown that demonstrate a strong dependence of the gain at a given bias voltage on the width of the n(-) gain region. Geometrical and fundamental theoretical models are examined to explain this behavior. The geometrical model takes into account the gain-dependent optical fill factor of the cylindrical APD. The theoretical model is based on the ballistic ionization model being developed for the HgCdTe APD. It is concluded that the fundamental theoretical explanation is the dominant effect. A model is developed that combines both the geometrical and fundamental effects. The model also takes into account the effect of the varying multiplication width in the low bias region of the gain-voltage curve. It is concluded that the lower than expected gain seen in the first 2 x 8 HgCdTe linear mode photon counting APD arrays, and higher excess noise factor, was very likely due to the larger than typical multiplication region length in the photon counting APD pixel design. The implications of these effects on device photon counting performance are discussed. (C) 2014 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Beck, Jeffrey D.; Kinch, Mike] DRS Technol Inc, C4ISR Grp, Dallas, TX 75243 USA. [Sun, Xiaoli] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Beck, JD (reprint author), DRS Technol Inc, C4ISR Grp, 13544 N,Cent Expressway, Dallas, TX 75243 USA. EM jeff.beck@drs.com NR 14 TC 5 Z9 5 U1 1 U2 11 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 EI 1560-2303 J9 OPT ENG JI Opt. Eng. PD AUG PY 2014 VL 53 IS 8 AR 081906 DI 10.1117/1.OE.53.8.081906 PG 6 WC Optics SC Optics GA AO2YT UT WOS:000341195300008 ER PT J AU Dauler, EA Grein, ME Kerman, AJ Marsili, F Miki, S Nam, SW Shaw, MD Terai, H Verma, VB Yamashita, T AF Dauler, Eric A. Grein, Matthew E. Kerman, Andrew J. Marsili, Francesco Miki, Shigehito Nam, Sae Woo Shaw, Matthew D. Terai, Hirotaka Verma, Varun B. Yamashita, Taro TI Review of superconducting nanowire single-photon detector system design options and demonstrated performance SO OPTICAL ENGINEERING LA English DT Review DE photodetectors; detector arrays; quantum efficiency; optoelectronic packaging ID GIFFORD-MCMAHON CRYOCOOLER; EFFICIENCY; ARRAY AB We describe a number of methods that have been pursued to develop superconducting nanowire single-photon detectors (SNSPDs) with attractive overall performance, including three systems that operate with >70% system detection efficiency and high maximum counting rates at wavelengths near 1550 nm. The advantages and tradeoffs of various approaches to efficient optical coupling, electrical readout, and SNSPD design are described and contrasted. Optical interfaces to the detectors have been based on fiber coupling, either directly to the detector or through the substrate, using both single-mode and multimode fibers with different approaches to alignment. Recent advances in electrical interfaces have focused on the challenges of scalability and ensuring stable detector operation at high count rates. Prospects for further advances in these and other methods are also described, which may enable larger arrays and higher-performance SNSPD systems in the future. Finally, the use of some of these techniques to develop fully packaged SNSPD systems will be described and the performance available from these recently developed systems will be reviewed. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI. C1 [Dauler, Eric A.; Grein, Matthew E.; Kerman, Andrew J.] MIT, Lincoln Lab, Lexington, MA 02420 USA. [Marsili, Francesco; Shaw, Matthew D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Miki, Shigehito; Terai, Hirotaka; Yamashita, Taro] Natl Inst Informat & Communicat Technol, Kobe Adv Res Ctr, Nishi Ku, Kobe, Hyogo 6512492, Japan. [Nam, Sae Woo; Verma, Varun B.] NIST, Boulder, CO 80305 USA. RP Dauler, EA (reprint author), MIT, Lincoln Lab, 244 Wood St, Lexington, MA 02420 USA. EM edauler@LL.mit.edu FU Defense for Research and Engineering under Air Force Contract [FA8721-05-C-0002] FX The MIT Lincoln Laboratory portion of this work is sponsored by the Assistant Secretary of Defense for Research and Engineering under Air Force Contract FA8721-05-C-0002. Opinions, interpretations, conclusions, and recommendations are those of the author and are not necessarily endorsed by the U.S. government. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 30 TC 21 Z9 21 U1 6 U2 41 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 EI 1560-2303 J9 OPT ENG JI Opt. Eng. PD AUG PY 2014 VL 53 IS 8 AR 081907 DI 10.1117/1.OE.53.8.081907 PG 13 WC Optics SC Optics GA AO2YT UT WOS:000341195300009 ER PT J AU Cano, Z Postigo, AD Pozanenko, A Butler, N Thone, CC Guidorzi, C Kruhler, T Gorosabel, J Jakobsson, P Leloudas, G Malesani, D Hjorth, J Melandri, A Mundell, C Wiersema, K D'Avanzo, P Schulze, S Gomboc, A Johansson, A Zheng, W Kann, DA Knust, F Varela, K Akerlof, CW Bloom, J Burkhonov, V Cooke, E de Diego, JA Dhungana, G Farina, C Ferrante, FV Flewelling, HA Fox, OD Fynbo, J Gehrels, N Georgiev, L Gonzalez, JJ Greiner, J Guver, T Hatch, N Jelinek, M Kehoe, R Klose, S Klunko, E Kopae, D Kutyrev, A Krugly, Y Lee, WH Levan, A Linkov, V Matkin, A Minikulov, N Molotov, I Prochaska, JX Rieher, MG Roman-Zuniga, CG Rumyantsev, V Sanchez-Ramirez, R Steele, I Tanvir, NR Volnova, A Watson, AM Xu, D Yuan, F AF Cano, Z. de Ugarte Postigo, A. Pozanenko, A. Butler, N. Thoene, C. C. Guidorzi, C. Kruehler, T. Gorosabel, J. Jakobsson, P. Leloudas, G. Malesani, D. Hjorth, J. Melandri, A. Mundell, C. Wiersema, K. D'Avanzo, P. Schulze, S. Gomboc, A. Johansson, A. Zheng, W. Kann, D. A. Knust, F. Varela, K. Akerlof, C. W. Bloom, J. Burkhonov, V. Cooke, E. de Diego, J. A. Dhungana, G. Farina, C. Ferrante, F. V. Flewelling, H. A. Fox, O. D. Fynbo, J. Gehrels, N. Georgiev, L. Gonzalez, J. J. Greiner, J. Guever, T. Hatch, N. Jelinek, M. Kehoe, R. Klose, S. Klunko, E. Kopae, D. Kutyrev, A. Krugly, Y. Lee, W. H. Levan, A. Linkov, V. Matkin, A. Minikulov, N. Molotov, I. Prochaska, J. X. Rieher, M. G. Roman-Zuniga, C. G. Rumyantsev, V. Sanchez-Ramirez, R. Steele, I. Tanvir, N. R. Volnova, A. Watson, A. M. Xu, D. Yuan, F. TI A trio of gamma-ray burst supernovae: GRB 120729A, GRB 130215A/SN 2013ez, and GRB 130831A/SN 2013fu SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual: SN 2013ez; supernovae: general; supernovae: individual: SN 2013fu ID DIGITAL SKY SURVEY; CONTINUOUS ENERGY INJECTION; AFTERGLOW LIGHT CURVES; 25 APRIL 1998; HOST GALAXY; MILLISECOND PULSARS; OPTICAL AFTERGLOWS; IMAGE SUBTRACTION; BRIGHT SUPERNOVA; MAGNETIC-FIELDS AB We present optical and near-infrared (NIR) photometry for three gamma-ray burst supernovae (GRB-SNe): GRB 120729A, GRB 130215A/SN 2013ez, and GRB 130831A/SN 2013fu. For GRB 130215A/SN 2013ez, we also present optical spectroscopy at t-t(0) = 16.1 d, which covers rest-frame 3000-6250 angstrom. Based on Fell lambda 5169 and Sill lambda 6355, our spectrum indicates an unusually low expansion velocity of similar to 4000-6350 km s(-1), the lowest ever measured for a GRB-SN. Additionally, we determined the brightness and shape of each accompanying SN relative to a template supernova (SN 1998bw), which were used to estimate the amount of nickel produced via nucleosynthesis during each explosion. We find that our derived nickel masses are typical of other GRB-SNe, and greater than those of SNe Ibc that are not associated with GRBs. For GRB 130831A/SN 2013fu, we used our well-sampled R-band light curve (LC) to estimate the amount of ejecta mass and the kinetic energy of the SN, finding that these too are similar to other GRB-SNe. For GRB 130215A, we took advantage of contemporaneous optical/NIR observations to construct an optical/NIR bolometric LC of the afterglow. We fit the bolometric LC with the millisecond magnetar model of Zhang & Meszros (2001, ApJ, 552, L35), which considers dipole radiation as a source of energy injection to the forward shock powering the optical/NIR afterglow. Using this model we derive an initial spin period of P = 12 ms and a magnetic field of B = 1.1 x 10(15) G, which are commensurate with those found for proposed magnetar central engines of other long-duration GRBs. C1 [Cano, Z.; Jakobsson, P.; Johansson, A.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [de Ugarte Postigo, A.; Thoene, C. C.; Gorosabel, J.; Jelinek, M.] CSIC, IAA, E-18008 Granada, Spain. [de Ugarte Postigo, A.; Kruehler, T.; Leloudas, G.; Malesani, D.; Hjorth, J.; Fynbo, J.; Levan, A.; Xu, D.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Pozanenko, A.; Volnova, A.] Space Res Inst, Moscow 117997, Russia. [Butler, N.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Guidorzi, C.] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy. [Kruehler, T.] European So Observ, Santiago 19, Chile. [Gorosabel, J.] Univ Pais Vasco UPV EHU, ETS Ingn, Dept Fis Aplicada 1, Unidad Asociada Grp Ciencia Planetarias UPW EHU I, Bilbao 48013, Spain. [Gorosabel, J.] Basque Fdn Sci, Ikerbasque, Bilbao 48008, Spain. [Leloudas, G.] Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Melandri, A.; D'Avanzo, P.] INAF Brera Astron Observ, I-23807 Merate, LC, Italy. [Mundell, C.; Steele, I.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Wiersema, K.; Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Schulze, S.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Macul Santiago 7820436, Chile. [Schulze, S.] Millennium Ctr Supernova Sci, Santiago, Chile. [Gomboc, A.; Kopae, D.] Univ Ljubljana, Fac Math & Phys, Ljubljana 1000, Slovenia. [Zheng, W.; Bloom, J.; Fox, O. D.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kann, D. A.; Knust, F.; Varela, K.; Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kann, D. A.; Klose, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Akerlof, C. W.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Burkhonov, V.] Ulugh Beg Astron Inst, Tashkent, Uzbekistan. [Cooke, E.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [de Diego, J. A.; Georgiev, L.; Gonzalez, J. J.; Lee, W. H.; Roman-Zuniga, C. G.; Watson, A. M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Dhungana, G.; Ferrante, F. V.; Kehoe, R.] So Methodist Univ, Dept Phys, Dallas, TX 75275 USA. [Farina, C.] Isaac Newton Grp Telescopes, Santa Cruz De La Palma 38700, Canary Islands, Spain. [Flewelling, H. A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Gehrels, N.; Kutyrev, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Guever, T.] Istanbul Univ, Dept Astron & Space Sci, TR-34119 Istanbul, Turkey. Univ Amsterdam, Astron Inst, NL-1098 XH Amsterdam, Netherlands. [Hatch, N.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Klunko, E.] Russian Acad Sci, Inst Solar Terr Phys, Siberian Dept, Irkutsk 664033, Russia. [Krugly, Y.] Kharkov Natl Univ, Inst Astron, Kharkov, Ukraine. [Levan, A.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Linkov, V.] JSC Asron Sci Ctr, Moscow 125362, Russia. [Matkin, A.] Ussuriysk Astrophys Observ, S Gornotayozhnoe 692533, Russia. [Minikulov, N.] Acad Sci Tajikistan, Inst Astrophys, Dushanbe 734042, Tajikistan. [Molotov, I.] Keldysh Inst Appl Math, Moscow, Russia. [Prochaska, J. X.; Sanchez-Ramirez, R.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA. [Rieher, M. G.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. [Rumyantsev, V.] Taras Shevcheriko Natl Univ Kyiv, Crimean Astrophys Observ, Crimea, Ukraine. [Yuan, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. RP Cano, Z (reprint author), Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, Dunhagi 5, IS-107 Reykjavik, Iceland. EM zewcano@gmail.com RI Jakobsson, Pall/L-9950-2015; Jelinek, Martin/E-5290-2016; Roman-Zuniga, Carlos/F-6602-2016; Gonzalez, Jose/L-6687-2014; OI Sanchez-Ramirez, Ruben/0000-0002-7158-5099; Rumyantsev, Vasilij/0000-0003-1894-7019; Schulze, Steve/0000-0001-6797-1889; Guver, Tolga/0000-0002-3531-9842; de Ugarte Postigo, Antonio/0000-0001-7717-5085; Kruehler, Thomas/0000-0002-8682-2384; Jakobsson, Pall/0000-0002-9404-5650; Jelinek, Martin/0000-0003-3922-7416; Roman-Zuniga, Carlos/0000-0001-8600-4798; Gonzalez, Jose/0000-0002-3724-1583; Hatch, Nina/0000-0001-5600-0534; Thone, Christina/0000-0002-7978-7648 FU Icelandic Research Fund; Danish National Research Foundation; Spanish research project [AYA2012-39362-C02-02]; European Commission [FP7-PEOPLE-2012-CIG 322307]; European Commission; ASI [INAF I/004/11/]; RFBR [12-02-01336, 14-02-10015, 13-01-92204]; Max-Planck Institut fur Extraterrestrische Physik, Garching; Thuringer Landessternwarte Tautenburg; NASA [NNX13AJ67G, NNX09AH71G, NNX09AT02G, NNX10AI27G, NNX12AE66G]; ERC-StG [EGGS-278202]; Royal Society; Wolfson Foundation; Science and Technology Facilities Council; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; CONACyT [INFR-2009-01-122785, CB-2008-101958]; UNAM PAPIIT [IN113810]; UC MEXUS-CONACyT [CN 09-283]; CONICYT through FONDECYT [3140534]; Basal-CATA [PFB-06/2007]; Iniciativa Cientifica Milenio [P10-064-F]; Iniciativa Cientifica Milenio del Ministerio de Economa [IC120009]; Fomento y Turismo de Chile; Fondo de Innovacion para la Competitividad, del Ministerio de Economia, Fomento y Turismo de Chile; DFG [HA 1850/28-1]; [AYA2012-39727-C03-01] FX I am very grateful to Max de Pasquale for countless discussions regarding GRB physics, and Antonia Rowlinson for equally stimulating conversations regarding magnetars. We thank the referee for their insightful comments on the original manuscript. Z.C. gratefully acknowledges support by a Project Grant from the Icelandic Research Fund. The Dark Cosmology Centre is funded by the Danish National Research Foundation. The research activity of AdUP, CT, RSR, and JGor is supported by Spanish research project AYA2012-39362-C02-02. J.Gor and RSR are also supported by project AYA2012-39727-C03-01. AdUP acknowledges support by the European Commission under the Marie Curie Career Integration Grant programme (FP7-PEOPLE-2012-CIG 322307). T. K. acknowledges support by the European Commission under the Marie Curie Intra-European Fellowship Programme. The research activity of AM and PDA is supported by ASI grant INAF I/004/11/. A. P, A. V. acknowledge partial support by RFBR grants 12-02-01336, 14-02-10015, and A. M., I. M. acknowledge support by RFBR grant 13-01-92204. D. A. K. acknowledges support by the Max-Planck Institut fur Extraterrestrische Physik, Garching, and the Thuringer Landessternwarte Tautenburg. J.X.P. acknowledges support from NASA Swift Grant NNX13AJ67G. J.P.U.F. acknowledges support from the ERC-StG grant EGGS-278202. Based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. Based on observations made with the Gran Telescopio Canarias (GTC), instaled in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma. The Liverpool Telescope is operated by Liverpool John Moores University at the Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The Faulkes Telescopes are owned by Las Cumbres Observatory. C. G. M. acknowledges support from the Royal Society, the Wolfson Foundation and the Science and Technology Facilities Council. The ROTSE-IIIb telescope is operated by Southern Methodist University at McDonald Observatory, Ft. Davis, Texas. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. Additionally, we thank the RATIR project team and the staff of the Observatorio Astronmico Nacional on Sierra San Pedro Martir. RATIR is a collaboration between the University of California, the Universidad Nacional Autonoma de Mexico, NASA Goddard Space Flight Center, and Arizona State University, benefiting from the loan of an H2RG detector and hardware and software support from Teledyne Scientific and Imaging. RATIR, the automation of the Harold L. Johnson Telescope of the Observatorio Astronomico Nacional on Sierra San Pedro Martir, and the operation of both are funded through NASA grants NNX09AH71G, NNX09AT02G, NNX10AI27G, and NNX12AE66G, CONACyT grants INFR-2009-01-122785 and CB-2008-101958, UNAM PAPIIT grant IN113810, and UC MEXUS-CONACyT grant CN 09-283. S. S.; acknowledges support from CONICYT through FONDECYT grant 3140534, from Basal-CATA PFB-06/2007, Iniciativa Cientifica Milenio grant P10-064-F (Millennium Center for Supernova Science), and by Project IC120009 "Millennium Institute of Astrophysics (MAS)" of Iniciativa Cientifica Milenio del Ministerio de Economa, Fomento y Turismo de Chile, with input from "Fondo de Innovacion para la Competitividad, del Ministerio de Economia, Fomento y Turismo de Chile". Part of this work is based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to G. Hasinger (DFG grant HA 1850/28-1). NR 186 TC 14 Z9 14 U1 1 U2 13 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2014 VL 568 AR A19 DI 10.1051/0004-6361/201423920 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VZ UT WOS:000341185900080 ER PT J AU Fuente, A Cernicharo, J Caselli, P McCoey, C Johnstone, D Fich, M van Kempen, T Palau, A Yildiz, UA Tercero, B Lopez, A AF Fuente, A. Cernicharo, J. Caselli, P. McCoey, C. Johnstone, D. Fich, M. van Kempen, T. Palau, Aina Yildiz, U. A. Tercero, B. Lopez, A. TI The hot core towards the intermediate-mass protostar NGC 7129 FIRS 2 Chemical similarities with Orion KL SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; ISM: individual objects: NGC 7129 FIRS 2 ID LIMITED MILLIMETER SURVEY; GRAIN SURFACE-CHEMISTRY; MOLECULAR LINE SURVEY; SOLAR-TYPE PROTOSTAR; SUBMILLIMETER ARRAY; TENTATIVE DETECTION; ROTATIONAL SPECTRUM; ORGANIC-MOLECULES; 1ST DETECTION; SAGITTARIUS B2(N) AB Context. This paper is dedicated to the study of the chemistry of the intermediate-mass (IM) hot core NGC 7129 FIRS 2, probably the most compact warm core found in the 2-8 M-circle dot stellar mass range. Aims. Our aim is to determine the chemical composition of the IM hot core NGC 7129 FIRS 2, and to provide new insights on the chemistry of hot cores in a more general context. Methods. NGC 7129 FIRS 2 (hereafter, FIRS 2) is located at a distance of 1250 pc and high spatial resolution observations are required to resolve the hot core at its center. We present a molecular survey from 218 200 MHz to 221 800 MHz carried out with the IRAM Plateau de Bure Interferometer (PdBI). These observations were complemented with a long integration single-dish spectrum taken with the IRAM 30 m telescope in Pico de Veleta (Spain). We used a local thermodynamic equilibrium (LTE) single temperature code to model the whole dataset. Results. The interferometric spectrum is crowded with a total of approximate to 300 lines from which a few dozen remain unidentified. The spectrum has been modeled with a total of 20 species and their isomers, isotopologues, and deuterated compounds. Complex molecules like methyl formate (CH3OCHO), ethanol (CH3CH2OH), glycolaldehyde (CH2OHCHO), acetone (CH3COCH3), dimethyl ether (CH3OCH3), ethyl cyanide (CH3CH2CN), and the aGg' conformer of ethylene glycol (aGg'-(CH2OH)(2)) are among the detected species. The detection of vibrationally excited lines of CH3CN, CH3OCHO, CH3OH, OCS, HC3N, and CH3CHO proves the existence of gas and dust at high temperatures. The gas kinetic temperature estimated from the vibrational lines of CH3CN, similar to 405(-67)(+100) K, is similar to that measured in massive hot cores. Our data allow an extensive comparison of the chemistry in FIRS 2 and the Orion hot core. Conclusions. We find a quite similar chemistry in FIRS 2 and Orion. Most of the studied fractional molecular abundances agree within a factor of 5. Larger differences are only found for the deuterated compounds D2CO and CH2DOH and a few molecules (CH3CH2CN, SO2, HNCO and CH3CHO). Since the physical conditions are similar in both hot cores, only different initial conditions (warmer pre-collapse and collapse phase in the case of Orion) and/or different crossing times of the gas in the hot core can explain this behavior. We discuss these two scenarios. C1 [Fuente, A.] IGN, Observ Astron Nacl OAN, Alcala De Henares 28803, Spain. [Cernicharo, J.; Tercero, B.; Lopez, A.] Inst Ciencia Mat Madrid ICMM, Madrid 28049, Spain. [Caselli, P.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [McCoey, C.; Fich, M.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Joint Astron Ctr, Hilo, HI 96720 USA. [van Kempen, T.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Palau, Aina] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico. [Yildiz, U. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Fuente, A (reprint author), IGN, Observ Astron Nacl OAN, Apdo 112, Alcala De Henares 28803, Spain. EM a.fuente@oan.es RI Yildiz, Umut/C-5257-2011; Fuente, Asuncion/G-1468-2016 OI Yildiz, Umut/0000-0001-6197-2864; Fuente, Asuncion/0000-0001-6317-6343 FU Spanish MINECO [CSD2009-00038, AYA2009-07304, AYA2012-32032]; National Research Council of Canada; Natural Sciences and Engineering Research Council of Canada (NSERC); Spanish MICINN [AYA2011-30228-C03-02]; FEDER funds; AGAUR (Catalonia) [2009SGR1172] FX We thank the Spanish MINECO for funding support from grants CSD2009-00038, AYA2009-07304, and AYA2012-32032. D.J. is supported by the National Research Council of Canada and by a Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grant. A. P. is supported by the Spanish MICINN grant AYA2011-30228-C03-02 (co-funded with FEDER funds), and by the AGAUR grant 2009SGR1172 (Catalonia). NR 69 TC 15 Z9 15 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2014 VL 568 AR A65 DI 10.1051/0004-6361/201323074 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VZ UT WOS:000341185900022 ER PT J AU Messias, H Dye, S Nagar, N Orellana, G Bussmann, RS Calanog, J Dannerbauer, H Fu, H Ibar, E Inohara, A Ivison, RJ Negrello, M Riechers, DA Sheen, YK Aguirre, JE Amber, S Birkinshaw, M Bourne, N Bradford, CM Clements, DL Cooray, A De Zotti, G Demarco, R Dunne, L Eales, S Fleuren, S Kamenetzky, J Lupu, RE Maddox, SJ Marrone, DP Michalowski, MJ Murphy, EJ Nguyen, HT Omont, A Rowlands, K Smith, D Smith, M Valiante, E Vieira, JD AF Messias, Hugo Dye, Simon Nagar, Neil Orellana, Gustavo Bussmann, R. Shane Calanog, Jae Dannerbauer, Helmut Fu, Hai Ibar, Edo Inohara, Andrew Ivison, R. J. Negrello, Mattia Riechers, Dominik A. Sheen, Yun-Kyeong Aguirre, James E. Amber, Simon Birkinshaw, Mark Bourne, Nathan Bradford, Charles M. Clements, Dave L. Cooray, Asantha De Zotti, Gianfranco Demarco, Ricardo Dunne, Loretta Eales, Stephen Fleuren, Simone Kamenetzky, Julia Lupu, Roxana E. Maddox, Steve J. Marrone, Daniel P. Michalowski, Michal J. Murphy, Eric J. Nguyen, Hien T. Omont, Alain Rowlands, Kate Smith, Dan Smith, Matt Valiante, Elisabetta Vieira, Joaquin D. TI Herschel-ATLAS and ALMA HATLAS J142935.3-002836, a lensed major merger at redshift 1.027 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gravitational lensing: strong; galaxies: ISM; galaxies: kinematics and dynamics ID STAR-FORMING GALAXIES; SCIENCE DEMONSTRATION PHASE; DEGREE EXTRAGALACTIC SURVEY; SPITZER-SPACE-TELESCOPE; 1200-MU-M MAMBO SURVEY; DIGITAL SKY SURVEY; DEEP FIELD-SOUTH; SUBMILLIMETER GALAXIES; MOLECULAR GAS; INTERSTELLAR-MEDIUM AB Context. The submillimetre-bright galaxy population is believed to comprise, aside from local galaxies and radio-loud sources, intrinsically active star-forming galaxies, the brightest of which are lensed gravitationally. The latter enable studies at a level of detail beyond what is usually possible by the observation facility. Aims. This work focuses on one of these lensed systems, HATLAS J142935.3-002836 (H1429-0028), selected in the Herschel-ATLAS field. Gathering a rich, multi-wavelength dataset, we aim to confirm the lensing hypothesis and model the background source's morphology and dynamics, as well as to provide a full physical characterisation. Methods. Multi-wavelength high-resolution data is utilised to assess the nature of the system. A lensing-analysis algorithm that simultaneously fits different wavebands is adopted to characterise the lens. The background galaxy dynamical information is studied by reconstructing the 3D source plane of the ALMA CO (J: 4 -> 3) transition. Near-IR imaging from HST and Keck-AO allows to constrain rest-frame optical photometry independently for the foreground and background systems. Physical parameters (such as stellar and dust masses) are estimated via modelling of the spectral energy distribution taking source blending, foreground obscuration, and differential magnification into account. Results. The system comprises a foreground edge-on disk galaxy (at z(sp) = 0.218) with an almost complete Einstein ring around it. The background source (at z(sp) = 1.027) is magnified by a factor of p = 8-10 depending on wavelength. It is comprised of two components and a tens-of-kpc-long tidal tail resembling the Antenna merger. As a whole, the background source is a massive stellar system (1.32(0.41)(+0.63) x 10(11) M.) forming stars at a rate of 394 +/- 90 Mo yr(-1), and it has a significant gas reservoir M-ISM = 4.6 + 1.7 x 10(10) M-circle dot. Its depletion time due to star formation alone is thus expected to be T-sF = M-ISM/SFR = 117 +/- 51 Myr. The dynamical mass of one of the components is estimated to be 5.8 +/- 1.7 x 10(10) M., and, together with the photometric total mass estimate, it implies that H1429-0028 is a major merger system (1: 2.8+ 1). C1 [Messias, Hugo; Nagar, Neil; Orellana, Gustavo; Sheen, Yun-Kyeong; Demarco, Ricardo] Univ Concepcion, Barrio Univ, Concepcion, Chile. [Messias, Hugo] Univ Lisbon, Ctr Astron & Astrofis, Observatorio Astron Lisboa, P-1349018 Lisbon, Portugal. [Dye, Simon; Bourne, Nathan] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Bussmann, R. Shane] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Calanog, Jae; Inohara, Andrew; Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dannerbauer, Helmut] Univ Vienna, Inst Astrophys, A-1180 Vienna, Austria. [Fu, Hai] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Ibar, Edo] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile. [Ivison, R. J.; Dunne, Loretta; Maddox, Steve J.; Michalowski, Michal J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] European So Observ, Garching, Germany. [Negrello, Mattia; De Zotti, Gianfranco] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Riechers, Dominik A.; Cooray, Asantha] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Riechers, Dominik A.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Aguirre, James E.; Lupu, Roxana E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Amber, Simon] Open Univ, Milton Keynes MK7 6BJ, Bucks, England. [Birkinshaw, Mark] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Birkinshaw, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bradford, Charles M.; Nguyen, Hien T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Clements, Dave L.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Dunne, Loretta; Maddox, Steve J.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand. [Eales, Stephen; Smith, Matt; Valiante, Elisabetta] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Fleuren, Simone] Univ London, Sch Math Sci, London E1 4NS, England. [Kamenetzky, Julia] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Marrone, Daniel P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Murphy, Eric J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Omont, Alain] Univ Paris 06, Inst Astrophys Paris, UNIR 7095, CNRS, F-75014 Paris, France. [Rowlands, Kate] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Smith, Dan] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Vieira, Joaquin D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Vieira, Joaquin D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. RP Messias, H (reprint author), Univ Concepcion, Barrio Univ, Concepcion, Chile. EM hmessias@oal.ul.pt RI Lupu, Roxana/P-9060-2014; Ivison, R./G-4450-2011; OI Lupu, Roxana/0000-0003-3444-5908; Ivison, R./0000-0001-5118-1313; Marrone, Daniel/0000-0002-2367-1080; De Zotti, Gianfranco/0000-0003-2868-2595; Maddox, Stephen/0000-0001-5549-195X; Dye, Simon/0000-0002-1318-8343 FU CONYCIT-ALMA [31100008]; FCT [SFRH/BPD/97986/2013, PTDC/FIS-AST/2194/2012, PEst-OE/FIS/UI2751/2014]; NSF [AST-1313319]; CONICYT/FONDECYT [3130504]; FONDECYT [3130470]; BASAL centre for Astrophysics and Associated Technologies (CATA) and by FONDECYT [1130528] FX H.M. acknowledges the support by CONYCIT-ALMA through a post-doc scholarship under the project 31100008. HM acknowledges support by FCT via the post-doctoral fellowship SFRH/BPD/97986/2013 and the programs PTDC/FIS-AST/2194/2012 and PEst-OE/FIS/UI2751/2014. N.N. and R.D. acknowledge support from BASAL PFB-06/2007, Fondecyt 1100540 and Anillo ACT1101. J.A.C. and A. C. acknowledge support from NSF AST-1313319. E.I. acknowledges funding from CONICYT/FONDECYT postdoctoral project No: 3130504. R.J.I., S.J.M. and L.D. ackowledge support from the European Research Council in the form of Advanced Investigator grant, COSMICISM. Y.K.S. acknowledges support by FONDECYT Grant No. 3130470. R.D. acknowledges the support provided by the BASAL centre for Astrophysics and Associated Technologies (CATA) and by FONDECYT N. 1130528. K.R. acknowledges support from the European Research Council Starting Grant SEDmorph (P.I. Wild). This paper makes use of the following ALMA data: ADS/JAO. ALMA#2011.0.00476. S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This publication is based on data acquired with the Atacama Pathfinder Experiment (APEX). APEX is a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. We are grateful to the competent staff at the APEX base-camp in Sequitor, Chile and the Z-Spec instrument team. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, 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. Based in part on observations obtained at the Gemini Observatory (include additional acknowledgement here, see Sect. 1.2), which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovagao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). The Herschel-ATLAS is a project with Herschel, an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS website is http://www.h-atlas.org/. Based in part on observations carried out with the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.; The authors wish to recognise and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The authors thank the ALMA contact scientist Adam Leroy for the help throughout scheduling block preparation and quality assurance, and the help provided by Alexander J. Conley and Elisabete da Cunha handling, respectively, the MBBEMCEE and MAGPHYS codes. NR 143 TC 13 Z9 13 U1 1 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2014 VL 568 AR A92 DI 10.1051/0004-6361/201424410 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VZ UT WOS:000341185900134 ER PT J AU Oshagh, M Santos, NC Ehrenreich, D Haghighipour, N Figueira, P Santerne, A Montalto, M AF Oshagh, M. Santos, N. C. Ehrenreich, D. Haghighipour, N. Figueira, P. Santerne, A. Montalto, M. TI Impact of occultations of stellar active regions on transmission spectra Can occultation of a plage mimic the signature of a blue sky? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites: atmospheres; techniques: photometric; methods: data analysis; methods: numerical; stars: activity ID HUBBLE-SPACE-TELESCOPE; EXOPLANET HD 189733B; TIME-SERIES PHOTOMETRY; SPITZER OBSERVATIONS; EXTRASOLAR PLANET; TRANSITING PLANET; ATMOSPHERIC HAZE; LIGHT-CURVE; M DWARF; VARIABILITY AB Transmission spectroscopy during planetary transits, which is based on the measurements of the variations of the planet-to-star radius ratio as a function of wavelength, is a powerful technique to study the atmospheric properties of transiting planets. One of the main limitations of this technique is the effects of stellar activity, which up until now, have been taken into account only by assessing the effect of non-occulted stellar spots on the estimates of the planet-to-star radius ratio. In this paper, we study the impact of the occultation of a stellar spot and plage on the transmission spectra of transiting exoplanets for the first time. We simulated this effect by generating a large number of transit light curves for different transiting planets, stellar spectral types, and different wavelengths. Results of our simulations indicate that the anomalies inside the transit light curve can lead to a significant underestimation or overestimation of the planet-to-star radius ratio as a function of wavelength. At short wavelengths, the effect can reach to a difference of up to 10% in the planet-to-star radius ratio, mimicking the signature of light scattering in the planetary atmosphere. Atmospheric scattering has been proposed to interpret the increasing slopes of transmission spectra toward blue for exoplanets HD 189733b and GJ 3470b. Here, we show that these signatures can be alternatively interpreted by the occultation of stellar plages. Results also suggest that the best strategy to identify and quantify the effects of stellar activities on the transmission spectrum of a planet is to perform several observations during the transit epoch at the same wavelength. This will allow for identifying the possible variations in transit depth as a function of time due to stellar activity variability. C1 [Oshagh, M.; Santos, N. C.; Figueira, P.; Santerne, A.; Montalto, M.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Oshagh, M.; Santos, N. C.] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, P-4150762 Oporto, Portugal. [Oshagh, M.; Santos, N. C.; Figueira, P.; Santerne, A.; Montalto, M.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4169007 Oporto, Portugal. [Ehrenreich, D.] Univ Geneva, Observ Geneve, CH-1290 Sauverny, Switzerland. [Haghighipour, N.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Haghighipour, N.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. RP Oshagh, M (reprint author), Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Oporto, Portugal. EM moshagh@astro.up.pt RI Figueira, Pedro/J-4916-2013; Santos, Nuno/E-9957-2011; OI Figueira, Pedro/0000-0001-8504-283X; Oshagh, Mahmoudreza/0000-0002-0715-8789; Santos, Nuno/0000-0003-4422-2919; Santerne, Alexandre/0000-0002-3586-1316; Ehrenreich, David/0000-0001-9704-5405 NR 31 TC 18 Z9 18 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2014 VL 568 AR A99 DI 10.1051/0004-6361/201424059 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VZ UT WOS:000341185900104 ER PT J AU Santangelo, G Nisini, B Codella, C Lorenzani, A Yildiz, UA Antoniucci, S Bjerkeli, P Cabrit, S Giannini, T Kristensen, LE Liseau, R Mottram, JC Tafalla, M van Dishoeck, EF AF Santangelo, G. Nisini, B. Codella, C. Lorenzani, A. Yildiz, U. A. Antoniucci, S. Bjerkeli, P. Cabrit, S. Giannini, T. Kristensen, L. E. Liseau, R. Mottram, J. C. Tafalla, M. van Dishoeck, E. F. TI Water distribution in shocked regions of the NGC 1333-IRAS 4A protostellar outflow SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: low mass; ISM: jets and outflows; ISM: molecules; ISM: individual objects: NGC 1333-IRAS 4A; stars: formation ID STAR-FORMING REGIONS; LOW-MASS PROTOSTARS; YOUNG STELLAR OBJECTS; HERSCHEL-HIFI; MOLECULAR OUTFLOW; NGC-1333 IRAS-4; KEY PROGRAM; CO EMISSION; L1157; PACS AB Context. Water is a key molecule in protostellar environments because its line emission is very sensitive to both the chemistry and the physical conditions of the gas. Observations of H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observatory have highlighted the complexity of H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ line profiles, in which different kinematic components can be distinguished. Aims. The goal is to study the spatial distribution of H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ, in particular of the different kinematic components detected in H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ emission, at two bright shocked regions along IRAS 4A, one of the strongest H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ emitters among the Class 0 outflows. Methods. We obtained Herschel-PACS maps of the IRAS 4A outflow and HIFI observations of two shocked positions. The largest HIFI beam of 38'' at 557 GHz was mapped in several key water lines with different upper energy levels, to reveal possible spatial variations of the line profiles. A large velocity gradient (LVG) analysis was performed to determine the excitation conditions of the gas. Results. We detect four H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ lines and CO (16-15) at the two selected shocked positions. In addition, transitions from related outflow and envelope tracers are detected. Different gas components associated with the shock are identified in the H2O emission. In particular, at the head of the red lobe of the outflow, two distinct gas components with different excitation conditions are distinguished in the HIFI emission maps: a compact component, detected in the ground-state water lines, and a more extended one. Assuming that these two components correspond to two different temperature components observed in previous H2O and CO studies, the LVG analysis of the H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ emission suggests that the compact (about 32, corresponding to about 700 AU) component is associated with a hot (T similar to 1000 K) gas with densities n(H2) similar to (1-4) x 10(5) cm(-3), whereas the extended (10 ''-17 '', corresponding to 2400-4000 AU) one traces a warm (T similar to 300-500 K) and dense gas (n(H2) similar to (3-5) x 10(7) cm(-3)). Finally, using the CO (16-15) emission observed at R2 and assuming a typical CO/H-2 abundance of 10(-4), we estimate the H2O/H-2 abundance of the warm and hot components to be (7-10) x 10(-7) and (3-7) x 10(-5). Conclusions. Our data allowed us, for the first time, to resolve spatially the two temperature components previously observed with HIFI and PACS. We propose that the compact hot component may be associated with the jet that impacts the surrounding material, whereas the warm, dense, and extended component originates from the compression of the ambient gas by the propagating flow. C1 [Santangelo, G.; Codella, C.; Lorenzani, A.] Osserv Astrofis Arcetri, I-50125 Florence, Italy. [Santangelo, G.; Nisini, B.; Antoniucci, S.; Giannini, T.] Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. [Yildiz, U. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bjerkeli, P.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Bjerkeli, P.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Bjerkeli, P.] Univ Copenhagen, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark. [Bjerkeli, P.; Liseau, R.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. [Cabrit, S.] CNRS, Observ Paris, UMR 8112, LERMA, F-75014 Paris, France. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mottram, J. C.; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. RP Santangelo, G (reprint author), Osserv Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy. EM gina@arcetri.astro.it RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; OI Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Lorenzani, Andrea/0000-0002-4685-3434; Bjerkeli, Per/0000-0002-7993-4118; Antoniucci, Simone/0000-0002-0666-3847; Codella, Claudio/0000-0003-1514-3074 FU ASI project [01/005/11/0] FX Herschel activities at INAF are financially supported by the ASI project 01/005/11/0. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research. Groningen, The Netherlands and with major contributions from Germany, France and the US, Consortium members are Canada: CSA, U.Waterloo; France; CESR. LAB, LERMA, IRAM: Germany: ROSMA. MPIfR, MPS; Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetti- INAF; The Netherlands; SRON, TUD; Poland: CAMK, CHK: Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA): Sweden: Chalmers University of Technology - MC2. RSS & GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich. FHNW: USA; Caltech, JPL NHSC. NR 42 TC 8 Z9 8 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2014 VL 568 DI 10.1051/0004-6361/201424034 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VZ UT WOS:000341185900099 ER PT J AU Santos-Costa, D de Pater, I Sault, RJ Janssen, MA Levin, SM Bolton, SJ AF Santos-Costa, D. de Pater, I. Sault, R. J. Janssen, M. A. Levin, S. M. Bolton, S. J. TI Multifrequency analysis of the Jovian electron-belt radiation during the Cassini flyby of Jupiter SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiation mechanisms: non-thermal; methods: data analysis ID SYNCHROTRON-RADIATION; RADIO-EMISSION; 3-DIMENSIONAL RECONSTRUCTION; RELATIVISTIC ELECTRONS; VLA OBSERVATIONS; SL9 IMPACTS; SOLAR-WIND; GHZ; CM AB Aims. We examine Very Large Array (VLA) observations of Jupiter to present evidence of fluctuations in the emission produced by the electron belt in January 2001. Investigating the source of fluctuations will provide new opportunities to discuss the scenarios of temporal changes in Jupiter's synchrotron radiation (i.e., the electron belt) in future data analysis and modeling work. Methods. To discuss the electron belt dynamics during the Cassini flyby of Jupiter. we compare the radio measurements from 2-3 January 2001 with VLA observations obtained on 20-21 December 1988, when viewing geometry and array configuration are comparable. All data are scaled to a standard Earth-Jupiter distance of 4.04 AU for comparison purposes. Brightness distribution maps with identical spatial resolutions and cartography of the equatorial radiation are constructed and examined at the wavelengths of 21 cm and 90 cm. Results. Rotation-averaged maps show that the emission from the equatorial zones of maximum intensity is weaker by 5-40%. but the brightness distribution is spatially more extended on 2-3 January 2001. resulting in a total emission at both wavelengths stronger by similar to 35%. Between observation periods, the brightness distributions are observed to evolve differently during the planet rotation. Tomographic reconstructions of the equatorial radiation support our conclusion that the electron belt population was differently distributed around the planet in December 1988 and January 2001. Conclusions, Our analysis of VLA data sets suggests that the spatial distribution of the electron belt on 2-3 January 2001 is different from that usually observed. Our knowledge of solar activity at the time of the Cassini flyby of Jupiter suggests that the emission from the electron radiation belt was responding to external influences, most likely to solar wind structures rather than to solar radio flux, on a timescale of days to a couple of weeks. Combined results from a multisource data analysis including spacecraft and radio observations are needed to confirm this relationship. C1 [Santos-Costa, D.; Bolton, S. J.] SW Res Inst, Dept Space Sci, San Antonio, TX 78238 USA. [de Pater, I.] Univ Calif Berkeley, Berkeley Astron Dept, Berkeley, CA 94720 USA. [Sault, R. J.] Univ Melbourne, Melbourne, Vic 3010, Australia. [Janssen, M. A.; Levin, S. M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Santos-Costa, D (reprint author), SW Res Inst, Dept Space Sci, San Antonio, TX 78238 USA. EM dsantoscosta@swri.edu; imke@berkeley.edu; rsault@nrao.edu; michael.janssen@jpl.nasa.gov; steven.m.levin@jpl.nasa.gov; sbolton@swri.edu NR 48 TC 3 Z9 3 U1 1 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2014 VL 568 AR A61 DI 10.1051/0004-6361/201423896 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VZ UT WOS:000341185900077 ER PT J AU Sodor, A Chene, AN De Cat, P Bognar, Z Wright, DJ Marois, C Walker, GAH Matthews, JM Kallinger, T Rowe, JF Kuschnig, R Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D Weiss, WW AF Sodor, A. Chene, A. -N. De Cat, P. Bognar, Zs. Wright, D. J. Marois, C. Walker, G. A. H. Matthews, J. M. Kallinger, T. Rowe, J. F. Kuschnig, R. Guenther, D. B. Moffat, A. F. J. Rucinski, S. M. Sasselov, D. Weiss, W. W. TI MOST light-curve analysis of the gamma Doradus pulsator HR 8799, showing resonances and amplitude variations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: photometric; stars: individual: HR 8799; stars: oscillations ID RR LYRAE STARS; 1ST DETECTION; DEBRIS DISK; VEGA-LIKE; ASTEROSEISMOLOGY; FREQUENCIES; MODULATION; PHOTOMETRY; MULTISITE; PLANETS AB Context-The central star of the HR 8799 system is a gamma Dorados-type pulsator. The system harbours four planetary mass companions detected by direct imaging. and is a good solar system analogue. The masses of the companions are not accurately known because the estimation depends greatly on the age of the system, which is also not known with sufficient accuracy. Asteroseisrnic studies of the star might help to better constrain the age of HR 8799. We organized an extensive photometric and multi site spectroscopic observing campaign to study the pulsations of the central star. Aims. The aim of the present study is to investigate the pulsation properties of HR 8799 in detail via the ultra-precise 47 d nearly continuous photometry obtained with the Microvariability and Oscillations in STars (MOST) space telescope, and to find as many independent pulsation modes as possible, which is the prerequisite for an asteroseismic age determination. Methods. We carried out Fourier analysis of the wide band photometric time series. Results. We find that resonance and sudden amplitude changes characterize the pulsation of HR 8799. The dominant frequency is always at f(1) = 1.978 d(-1). Many multiples of one-ninth of the dominant frequency appear in the Fourier spectrum of the MOST data: n/9 f(1). where n =[1, 2, 3, 4. 5, 6,7, 8, 9, 10, 13, 14, 17, 18]. Our analysis also reveals that many of these peaks show strong amplitude decrease and phase variations even on the 47 d time scale. The dependencies between the pulsation frequencies of HR 8799 make the planned subsequent asteroseismic analysis rather difficult We point out some resemblance between the light curve of HR 8799 and the modulated pulsation light curves of Blazhko RR Lyrae stars. C1 [Sodor, A.; De Cat, P.; Wright, D. J.] Royal Observ Belgium, B-1180 Brussels, Belgium. [Sodor, A.; Bognar, Zs.] MTA CSFK, Konkoly Observ, H-1121 Budapest, Hungary. [Chene, A. -N.] Northern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. [Wright, D. J.] Univ New S Wales, Sch Phys, Dept Astrophys & Opt, Sydney, NSW 2052, Australia. [Marois, C.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Kallinger, T.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron IfA, A-1180 Vienna, Austria. [Rowe, J. F.] NASA Ames Res Pk, Moffett Field, CA 94035 USA. [Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rucinski, S. M.] Univ Toronto, David Dunlap Observ, Dept Astron & Astrophys, Richmond Hill, ON L4C 4Y6, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sodor, A (reprint author), Royal Observ Belgium, Ringlaan 3, B-1180 Brussels, Belgium. EM adam.sodor@oma.be OI Kallinger, Thomas/0000-0003-3627-2561 FU Belgian Federal Science Policy [M0/33/029]; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences; Austrian Science Fonds (EWE) [P22691-N16] FX A.S. acknowledges support by the Belgian Federal Science Policy (project M0/33/029, PI: P.D.C.) and by the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. WM. acknowledges support by the Austrian Science Fonds (EWE) P22691-N16. NR 26 TC 4 Z9 4 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2014 VL 568 AR A106 DI 10.1051/0004-6361/201423976 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VZ UT WOS:000341185900090 ER PT J AU Calabrese, E Hlozek, R Battaglia, N Bond, JR de Bernardis, F Devlin, MJ Hajian, A Henderson, S Hil, JC Kosowsky, A Louis, T McMahon, J Moodley, K Newburgh, L Niemack, MD Page, LA Partridge, B Sehgal, N Sievers, JL Spergel, DN Staggs, ST Switzer, ER Trac, H Wollack, EJ AF Calabrese, Erminia Hlozek, Renee Battaglia, Nick Bond, J. Richard de Bernardis, Francesco Devlin, Mark J. Hajian, Amir Henderson, Shawn Hil, J. Colin Kosowsky, Arthur Louis, Thibaut McMahon, Jeff Moodley, Kavilan Newburgh, Laura Niemack, Michael D. Page, Lyman A. Partridge, Bruce Sehgal, Neelima Sievers, Jonathan L. Spergel, David N. Staggs, Suzanne T. Switzer, Eric R. Trac, Hy Wollack, Edward J. TI Precision epoch of reionization studies with next-generation CMB experiments SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE CMBR polarisation; CMBR experiments; reionization; Sunyaev-Zeldovich effect ID MICROWAVE BACKGROUND POLARIZATION; SELF-REGULATED REIONIZATION; SOUTH-POLE TELESCOPE; SZ POWER SPECTRUM; SUNYAEV-ZELDOVICH; INHOMOGENEOUS REIONIZATION; COSMIC REIONIZATION; ANISOTROPIES; CONSTRAINTS; PROBE AB Future arcminute resolution polarization data from ground-based Cosmic Microwave Background (CMB) observations can be used to estimate the contribution to the temperature power spectrum from the primary anisotropies and to uncover the signature of reionization near l=1500 in the small angular-scale temperature measurements. Our projections are based on combining expected small-scale E-mode polarization measurements from Advanced ACTPol in the range 300 < l < 3000 with simulated temperature data from the full Planck mission in the low and intermediate l region, 2 < l < 2000 . We show that the six basic cosmological parameters determined from this combination of data will predict the underlying primordial temperature spectrum at high multipoles to better than 1% accuracy. Assuming an efficient cleaning from multi-frequency channels of most foregrounds in the temperature data, we investigate the sensitivity to the only residual secondary component, the kinematic Sunyaev-Zel'dovich (kSZ) term. The CMB polarization is used to break degeneracies between primordial and secondary terms present in temperature and, in effect, to remove from the temperature data all but the residual kSZ term. We estimate a 15 sigma detection of the diffuse homogeneous kSZ signal from expected AdvACT temperature data at l > 1500 , leading to a measurement of the amplitude of matter density fluctuations, sigma(8), at 1% precision. Alternatively, by exploring the reionization signal encoded in the patchy kSZ measurements, we bound the time and duration of the reionization with sigma(z(re)) = 1.1 and sigma(Delta z(re)) = 0.2 . We find that these constraints degrade rapidly with large beam sizes, which highlights the importance of arcminute-scale resolution for future CMB surveys. C1 [Calabrese, Erminia; Louis, Thibaut] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England. [Hlozek, Renee; Hil, J. Colin; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Battaglia, Nick; Trac, Hy] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Bond, J. Richard; Hajian, Amir; Switzer, Eric R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [de Bernardis, Francesco; Henderson, Shawn; Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Devlin, Mark J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [McMahon, Jeff] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Moodley, Kavilan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Newburgh, Laura] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Page, Lyman A.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Sehgal, Neelima] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Sievers, Jonathan L.] Univ KwaZulu Natal, Sch Chem & Phys, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Switzer, Eric R.; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Calabrese, E (reprint author), Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England. EM rminia.calabrese@astro.ox.ac.uk; rhlozek@astro.princeton.edu; nbattaglia@cmu.edu; bond@cita.utoronto.ca; fd63@cornell.edu; devlin@dept.physics.upenn.edu; ahajian@cita.utoronto.ca; swh76@cornell.edu; jhill@iastate.edu; kosowsky@pitt.edu; thibaut.louis@astro.ox.ac.uk; jeffmcm@umich.edu; moodleyk41@ukzn.ac.za; newburgh@di.utoronto.ca; niemack@cornell.edu; page@princeton.edu; bpartrid@haverford.edu; neelima.sehgal@stonybrook.edu; sieversj@ukzn.ac.za; dns@astro.princeton.edu; staggs@princeton.edu; eric.r.switzer@nasa.gov; hytrac@cmu.edu; edward.j.wollack@nasa.gov RI Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012; OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451; Sievers, Jonathan/0000-0001-6903-5074 FU U.S. National Science Foundation [AST-0408698, AST-0965625]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation (CFI); Parque Astronomico Atacama in northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT); ERC [259505]; NASA ATP [NNX14AB57G]; NSF [AST- 1312991]; [PHY-0855887]; [PHY-1214379] FX We acknowledge Graeme Addison and Sigurd Naess for useful discussions. This work was supported by the U.S. National Science Foundation through awards AST-0408698 and AST-0965625 for the ACT project, as well as awards PHY-0855887 and PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astronomico Atacama in northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT). Funding from ERC grant 259505 supports EC and TL. HT is supported by grants NASA ATP NNX14AB57G and NSF AST- 1312991. EC thanks Princeton Astrophysics for hospitality during this work. NR 63 TC 42 Z9 42 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD AUG PY 2014 IS 8 AR 010 DI 10.1088/1475-7516/2014/08/010 PG 21 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AP1RM UT WOS:000341848800010 ER PT J AU Raccanelli, A Bertacca, D Dore, O Maartens, R AF Raccanelli, Alvise Bertacca, Daniele Dore, Olivier Maartens, Roy TI Large-scale 3D galaxy correlation function and non-Gaussianity SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE power spectrum; redshift surveys; gravity; cosmological parameters from LSS ID PRIMORDIAL NON-GAUSSIANITY; REDSHIFT-SPACE; HALO BIAS; DISTORTIONS AB We investigate the properties of the 2-point galaxy correlation function at very large scales, including all geometric and local relativistic effects - wide-angle effects, redshift space distortions, Doppler terms and Sachs-Wolfe type terms in the gravitational potentials. The general three-dimensional correlation function has a nonzero dipole and octupole, in addition to the even multipoles of the flat-sky limit. We study how corrections due to primordial non-Gaussianity and General Relativity affect the multipolar expansion, and we show that they are of similar magnitude (when f(NL) is small), so that a relativistic approach is needed. Furthermore, we look at how large-scale corrections depend on the model for the growth rate in the context of modified gravity, and we discuss how a modified growth can affect the non-Gaussian signal in the multipoles. C1 [Raccanelli, Alvise; Dore, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Raccanelli, Alvise; Dore, Olivier] CALTECH, Pasadena, CA 91125 USA. [Bertacca, Daniele; Maartens, Roy] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Maartens, Roy] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. RP Raccanelli, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM alvise@caltech.edu; daniele.bertacca@gmail.com; Olivier.P.Dore@jpl.nasa.gov; roy.maartens@gmail.com OI Raccanelli, Alvise/0000-0001-6726-0438; Maartens, Roy/0000-0001-9050-5894 FU South African Square Kilometre Array Project; South African National Research Foundation; U.K. Science & Technology Facilities Council [ST/H002774/1, ST/K0090X/1] FX We thank Nicola Bartolo, Kazuya Koyama, Marc Manera, Sabino Matarrese, Will Percival, Ashley Ross, Lado Samushia and Gianmassimo Tasinato for helpful discussions. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The work of DB and RM was supported by the South African Square Kilometre Array Project and the South African National Research Foundation. RM was also supported by the U.K. Science & Technology Facilities Council (grant nos. ST/H002774/1 and ST/K0090X/1). NR 52 TC 20 Z9 20 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD AUG PY 2014 IS 8 AR 022 DI 10.1088/1475-7516/2014/08/022 PG 19 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AP1RM UT WOS:000341848800022 ER PT J AU Weaver, CP Mooney, S Allen, D Beller-Simms, N Fish, T Grambsch, AE Hohenstein, W Jacobs, K Kenney, MA Lane, MA Langner, L Larson, E McGinnis, DL Moss, RH Nichols, LG Nierenberg, C Seyller, EA Stern, PC Winthrop, R AF Weaver, C. P. Mooney, S. Allen, D. Beller-Simms, N. Fish, T. Grambsch, A. E. Hohenstein, W. Jacobs, K. Kenney, M. A. Lane, M. A. Langner, L. Larson, E. McGinnis, D. L. Moss, R. H. Nichols, L. G. Nierenberg, C. Seyller, E. A. Stern, P. C. Winthrop, R. TI From global change science to action with social sciences SO NATURE CLIMATE CHANGE LA English DT Editorial Material ID CLIMATE ADAPTATION C1 [Weaver, C. P.; Grambsch, A. E.] US EPA, Washington, DC 20460 USA. [Mooney, S.] Boise State Univ, Dept Econ, Boise, ID 83725 USA. [Mooney, S.] Natl Sci Fdn, Expt Program Stimulate Competit Res, Arlington, VA 22230 USA. [Allen, D.; Seyller, E. A.] US Global Change Res Program, Washington, DC 20006 USA. [Beller-Simms, N.; Nierenberg, C.] NOAA, Silver Spring, MD 20910 USA. [Fish, T.] US Dept Interior, Washington, DC 20240 USA. [Hohenstein, W.] USDA, Washington, DC 20250 USA. [Jacobs, K.] Univ Arizona, Ctr Climate Adaptat Sci & Solut, Tucson, AZ 85721 USA. [Jacobs, K.] Univ Arizona, Dept Soil Water & Environm Sci, Tucson, AZ 85721 USA. [Kenney, M. A.] Univ Maryland, Cooperat Inst Climate & Satellites Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Lane, M. A.; Stern, P. C.] CNR, Board Environm Change & Soc, Washington, DC 20001 USA. [Langner, L.] US Forest Serv, USDA, Washington, DC 20250 USA. [Larson, E.] NASA, Washington, DC 20546 USA. [McGinnis, D. L.] Montana State Univ, Billings, MT 59101 USA. [Moss, R. H.] Pacific NW Natl Lab, Joint Global Change Res Inst, College Pk, MD 20740 USA. [Moss, R. H.] Univ Maryland, College Pk, MD 20740 USA. [Nichols, L. G.] Natl Sci Fdn, Div Behav & Cognit Sci, Arlington, VA 22230 USA. [Winthrop, R.] Bureau Land Management, Washington, DC 20003 USA. RP Weaver, CP (reprint author), US EPA, 1200 Penn Ave NW, Washington, DC 20460 USA. EM weaver.chris@epa.gov RI Weaver, Christopher/G-3714-2010 OI Weaver, Christopher/0000-0003-4016-5451 NR 22 TC 30 Z9 30 U1 1 U2 27 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X EI 1758-6798 J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD AUG PY 2014 VL 4 IS 8 BP 656 EP 659 PG 4 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AO7YF UT WOS:000341568200010 ER PT J AU Stanford, SA Gonzalez, AH Brodwin, M Gettings, DP Eisenhardt, PRM Stern, D Wylezalek, D AF Stanford, S. A. Gonzalez, Anthony H. Brodwin, Mark Gettings, Daniel P. Eisenhardt, Peter R. M. Stern, Daniel Wylezalek, Dominika TI THE MASSIVE AND DISTANT CLUSTERS OF WISE SURVEY. II. INITIAL SPECTROSCOPIC CONFIRMATION OF z similar to 1 GALAXY CLUSTERS SELECTED FROM 10,000 deg(2) SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: clusters: individual; galaxies: distances and redshifts; galaxies: evolution ID POLE TELESCOPE SURVEY; STELLAR POPULATION SYNTHESIS; DATA RELEASE; SDSS-III; SPITZER; IRAC; EVOLUTION; DISCOVERY; UNIVERSE; SAMPLE AB We present optical and infrared imaging and optical spectroscopy of galaxy clusters which were identified as part of an all-sky search for high-redshift galaxy clusters, the Massive and Distant Clusters of WISE Survey (MaDCoWS). The initial phase of MaDCoWS combined infrared data from the all-sky data release of the Wide-field Infrared Survey Explorer (WISE) with optical data from the Sloan Digital Sky Survey to select probable z similar to 1 clusters of galaxies over an area of 10,000 deg(2). Our spectroscopy confirms 19 new clusters at 0.7 < z < 1.3, half of which are at z > 1, demonstrating the viability of using WISE to identify high-redshift galaxy clusters. The next phase of MaDCoWS will use the greater depth of the AllWISE data release to identify even higher redshift cluster candidates. C1 [Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Gonzalez, Anthony H.; Gettings, Daniel P.] Univ Florida, Dept Astron, Bryant Space Ctr 211, Gainesville, FL 32611 USA. [Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Eisenhardt, Peter R. M.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wylezalek, Dominika] European So Observ, D-85748 Garching, Germany. RP Stanford, SA (reprint author), Univ Calif Davis, Dept Phys, One Shields Ave, Davis, CA 95616 USA. FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; NASA Astrophysics Data Analysis Program (ADAP) [NNX12AE15G]; W.M. Keck Foundation FX This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration (NASA). Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration, a list of which can be found at https://www.sdss3.org/collaboration/institutions.php. We acknowledge using EzGal, available at www.baryons.org/ezgal/index.php, to calculate the colors displayed in the color-magnitude diagrams. S.A.S, M.B., D.P.G., and A.H.G. acknowledge support for this research from the NASA Astrophysics Data Analysis Program (ADAP) through grant NNX12AE15G. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. A.H.G and D.P.G. were Visiting Astronomers at Gemini 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. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias, on the island of La Palma. We thank the anonymous referee for comments which improved the final manuscript. NR 35 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2014 VL 213 IS 2 AR 25 DI 10.1088/0067-0049/213/2/25 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP0TM UT WOS:000341777400007 ER PT J AU Vrsnak, B Temmer, M Zic, T Taktakishvili, A Dumbovic, M Mostl, C Veronig, AM Mays, ML Odstrcil, D AF Vrsnak, B. Temmer, M. Zic, T. Taktakishvili, A. Dumbovic, M. Moestl, C. Veronig, A. M. Mays, M. L. Odstrcil, D. TI HELIOSPHERIC PROPAGATION OF CORONAL MASS EJECTIONS: COMPARISON OF NUMERICAL WSA-ENLIL plus CONE MODEL AND ANALYTICAL DRAG-BASED MODEL SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE magnetohydrodynamics (MHD); methods: analytical; methods: numerical; methods: statistical; solar-terrestrial relations; solar wind; Sun: coronal mass ejections (CMEs) ID AERODYNAMIC DRAG; SOLAR-WIND; ARRIVAL TIMES; CURRENT SHEET; 1 AU; EARTH; DYNAMICS; KINEMATICS; PLASMA; CMES AB Real-time forecasting of the arrival of coronal mass ejections (CMEs) at Earth, based on remote solar observations, is one of the central issues of space-weather research. In this paper, we compare arrival-time predictions calculated applying the numerical "WSA-ENLIL+Cone model" and the analytical "drag-based model" (DBM). Both models use coronagraphic observations of CMEs as input data, thus providing an early space-weather forecast two to four days before the arrival of the disturbance at the Earth, depending on the CME speed. It is shown that both methods give very similar results if the drag parameter Gamma = 0.1 is used in DBM in combination with a background solar-wind speed of w = 400 km s(-1). For this combination, the mean value of the difference between arrival times calculated by ENLIL and DBM is (Delta) over bar = 0.09 +/- 9.0 hr with an average of the absolute-value differences of vertical bar Delta vertical bar = 7.1 hr. Comparing the observed arrivals (O) with the calculated ones (C) for ENLIL gives O - C = -0.3 +/- 16.9 hr and, analogously, O - C = +1.1 +/- 19.1 hr for DBM. Applying Gamma = 0.2 with w = 450 km s(-1) in DBM, one finds O - C = - 1.7 +/- 18.3 hr, with an average of the absolute-value differences of 14.8 hr, which is similar to that for ENLIL, 14.1 hr. Finally, we demonstrate that the prediction accuracy significantly degrades with increasing solar activity. C1 [Vrsnak, B.; Zic, T.; Dumbovic, M.] Univ Zagreb, Fac Geodesy, Hvar Observ, HR-10000 Zagreb, Croatia. [Temmer, M.; Moestl, C.; Veronig, A. M.] Graz Univ, Inst Phys, Kanzelhohe Observ IGAM, A-8010 Graz, Austria. [Taktakishvili, A.; Mays, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Taktakishvili, A.; Mays, M. L.] Catholic Univ Amer, Washington, DC 20064 USA. [Moestl, C.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Odstrcil, D.] George Mason Univ, Fairfax, VA 22030 USA. RP Vrsnak, B (reprint author), Univ Zagreb, Fac Geodesy, Hvar Observ, Kacceva 26, HR-10000 Zagreb, Croatia. EM bvrsnak@geof.hr; manuela.temmer@uni-graz.at; tzic@geof.hr; aleksandre.taktakishvili-1@nasa.gov; mdumbovic@geof.hr; christian.moestl@uni-graz.at; astrid.veronig@uni-graz.at; m.leila.mays@nasa.gov; dusan.odstrcil@nasa.gov RI Veronig, Astrid/B-8422-2009; OI Zic, Tomislav/0000-0001-6372-8013; Temmer, Manuela/0000-0003-4867-7558; Moestl, Christian/0000-0001-6868-4152 FU European Commission's Seventh Framework Programme (FP7) [263252, 284461]; Austrian Science Fund (FWF) [V195-N16, P26174-N27]; Shota Rustaveli Foundation, Georgian National Science Foundation [DI/14/6-310/12]; Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme FX The research leading to these results has received funding from the European Commission's Seventh Framework Programme (FP7/2007-2013) under the grant agreement No. 263252 (COMESEP; www.comesep.eu) and No. 284461 (eHEROES; http://soteria-space.eu/eheroes/html/). M.T., A.V., and C.M. thank the Austrian Science Fund (FWF): V195-N16 and P26174-N27. A.T. greatly acknowledges Shota Rustaveli Foundation, Georgian National Science Foundation grant DI/14/6-310/12. This research was supported by a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme. NR 39 TC 15 Z9 15 U1 2 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2014 VL 213 IS 2 AR 21 DI 10.1088/0067-0049/213/2/21 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP0TM UT WOS:000341777400003 ER PT J AU McClelland, M Campbell, M Estlin, T AF McClelland, Mark Campbell, Mark Estlin, Tara TI Qualitative Relational Mapping for Mobile Robots with Minimal Sensing SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS LA English DT Article ID SIMULTANEOUS LOCALIZATION; NAVIGATION; SLAM; INFORMATION; MAP; CONSISTENCY; ORIENTATION; SPACE AB This paper presents a novel method for autonomous robotic navigation and mapping of large-scale spaces with minimal sensing. The proposed algorithm constructs a graph-based map that encodes the relative location of landmarks in the environment. Uncertainty in these locations is captured by imposing qualitative constraints on the relationships between landmarks observed by the robot. These relationships are represented in terms of the relative geometrical layout of landmark triplets. A novel measurement method based on camera imagery is presented that extends previous work from the field of qualitative spatial reasoning. Measurements are fused into the map using a deterministic approach based on iterative graph updates. The generation of these maps does not depend on estimates of robot egomotion, and it is consequently suitable for high-slip environments. Algorithm performance is evaluated using MonteCarlo simulations, and results are presented for an experiment using data gathered in the Jet Propulsion Laboratory, California Institute of Technology MarsYard. C1 [McClelland, Mark] Cornell Univ, Dept Mech & Aerosp Engn, Ithaca, NY 14853 USA. [Campbell, Mark] Cornell Univ, Sibley Sch Mech & Aerosp Engn, Dept Mech & Aerosp Engn, Ithaca, NY 14853 USA. [Estlin, Tara] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP McClelland, M (reprint author), Cornell Univ, Dept Mech & Aerosp Engn, Ithaca, NY 14853 USA. EM mjm496@cornell.edu; mc288@cornell.edu; Tara.Estlin@jpl.nasa.gov RI Campbell, Mark/F-8312-2013 OI Campbell, Mark/0000-0003-0775-4297 FU NASA Graduate Student Research Program; Cornell University; Jet Propulsion Laboratory, California Institute of Technology FX The research presented in this paper has been supported by a fellowship from the NASA Graduate Student Research Program. This work was performed by Cornell University and by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 25 TC 1 Z9 1 U1 0 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 1940-3151 EI 2327-3097 J9 J AEROSP INFORM SYST JI J. Aerosp. Inf. Syst. PD AUG PY 2014 VL 11 IS 8 BP 497 EP 511 DI 10.2514/1.I010155 PG 15 WC Engineering, Aerospace SC Engineering GA AP0YI UT WOS:000341792200002 ER PT J AU Pugh-Thomas, D AF Pugh-Thomas, Devin TI Spectroscopic properties and Judd-Ofelt analysis of BaY2F8:Sm3+ SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS LA English DT Article ID RARE-EARTH IONS; SPECTRAL PROPERTIES; OPTICAL-ABSORPTION; SINGLE-CRYSTALS; LBTAF GLASSES; LASER; SM3+; PHOTOLUMINESCENCE; INTENSITIES; CONVERSION AB Optical spectroscopy and Judd-Ofelt analysis were performed on a BaY2F8:Sm3+ crystal and used to guide the potential application of BaY2F8:Sm3+ as a laser material. Crystals were characterized by polarized absorption spectroscopy, fluorescence emission, and fluorescence lifetime measurements. The H-6(9/2) and H-6(7/2) manifolds are of most interest for visible lasers. This investigation seeks to capture the behavior of the samarium ion in a barium-yttrium-fluoride host from the UV-vis into the near-infrared wavelength regions. (C) 2014 Optical Society of America C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Pugh-Thomas, D (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM devin.pugh-thomas@nasa.gov FU NASA Internal Research and Development Fund FX Appreciation is extended to Drs. Brian M. Walsh and Archie L. Holmes for helpful discussions. Appreciation is extended to Dr. Arlete Cassanho of A.C. Materials for information on crystal growth. This investigation was supported by the NASA Internal Research and Development Fund. NR 31 TC 1 Z9 1 U1 3 U2 9 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0740-3224 EI 1520-8540 J9 J OPT SOC AM B JI J. Opt. Soc. Am. B-Opt. Phys. PD AUG PY 2014 VL 31 IS 8 BP 1777 EP 1785 DI 10.1364/JOSAB.31.001777 PG 9 WC Optics SC Optics GA AO8FU UT WOS:000341589700005 ER PT J AU Ting, WJ Chang, CH Chen, SE Chen, HC Shy, JT Drouin, BJ Daly, AM AF Ting, Wei-Jo Chang, Chun-Hung Chen, Shih-En Chen, Hsuan-Chen Shy, Jow-Tsong Drouin, Brian J. Daly, Adam M. TI Precision frequency measurement of N2O transitions near 4.5 mu m and above 150 mu m SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS LA English DT Article ID QUANTUM-CASCADE-LASER; NITROUS-OXIDE; ABSORPTION SPECTROSCOPY; ROTATIONAL TRANSITIONS; DIRECT LINK; COMB; MICROWAVE; SPECTRUM; SUBMILLIMETER; SPECTROMETER AB Frequency measurements are given for the 10(0)0 <-- 00(0)0 band of N2O near 4.5 mu m and for pure rotational transitions beyond 151.5 mu m. The infrared measurements utilize a periodically poled lithium niobate (PPLN) based difference frequency generation (DFG) source locked to the saturated absorption center of an N2O absorption line. The DFG frequency is calibrated by an optical frequency comb and an iodine hyperfine transition. We report 44 transitions ranging from J = 1 - 100 for both the P and R branches and the accuracy is better than 10 kHz for most transitions. In addition, 175 pure rotational transitions have been measured including 33 measurements with sub-Doppler precision (<= 3 kHz), and 142 Doppler limited measurements. These are combined with other precision rotational and vibrational measurements to provide improved quantum mechanical parameters, as well as frequency calibration tables for the N2O bands near 4.5 mu m. (C) 2014 Optical Society of America C1 [Ting, Wei-Jo; Chang, Chun-Hung; Chen, Shih-En; Shy, Jow-Tsong] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. [Chen, Hsuan-Chen; Shy, Jow-Tsong] Natl Tsing Hua Univ, Inst Photon Technol, Hsinchu 30013, Taiwan. [Shy, Jow-Tsong] Natl Tsing Hua Univ, Frontier Res Ctr Fundamental & Appl Sci Matters, Hsinchu 30013, Taiwan. [Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Shy, JT (reprint author), Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. EM shy@phys.nthu.edu.tw FU National Science Council; Ministry of Education of Taiwan; National Aeronautics and Space Administration FX The research at NTHU is supported by the National Science Council and the Ministry of Education of Taiwan. Portions of this research were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 51 TC 2 Z9 2 U1 5 U2 18 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0740-3224 EI 1520-8540 J9 J OPT SOC AM B JI J. Opt. Soc. Am. B-Opt. Phys. PD AUG PY 2014 VL 31 IS 8 BP 1954 EP 1963 DI 10.1364/JOSAB.31.001954 PG 10 WC Optics SC Optics GA AO8FU UT WOS:000341589700030 ER PT J AU Moore, AD Downs, ME Lee, SMC Feiveson, AH Knudsen, P Ploutz-Snyder, L AF Moore, Alan D., Jr. Downs, Meghan E. Lee, Stuart M. C. Feiveson, Alan H. Knudsen, Poul Ploutz-Snyder, Lori TI Peak exercise oxygen uptake during and following long-duration spaceflight SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE aerobic capacity; weightlessness; International Space Station ID MANNED SKYLAB MISSION; MIDDLE-AGED MEN; RED-BLOOD-CELL; BED-REST; CARDIOVASCULAR-RESPONSES; CARDIAC ATROPHY; SPACE-FLIGHT; ORTHOSTATIC INTOLERANCE; MAXIMAL EXERCISE; EXPERIMENT M-171 AB This investigation was designed to measure aerobic capacity ((V) over dot O-2peak) during and after long-duration International Space Station (ISS) missions. Astronauts (9 males, 5 females: 49 +/- 5 yr, 77.2 +/- 15.1 kg, 40.6 +/- 6.4 ml.kg(-1).min (-1) [mean +/- SD]) performed peak cycle tests similar to 90 days before flight, 15 days after launch, every similar to 30 days in-flight, and on recovery days 1 (R + 1), R + 10, and R + 30. Expired metabolic gas fractions, ventilation, and heart rate (HR) were measured. Data were analyzed using mixed-model linear regression. The main findings of this study were that (V) over dot O-2peak decreased early in-flight (similar to 17%) then gradually increased during flight but never returned to preflight levels. (V) over dot O-2peak was lower on R + 1 and R + 10 than preflight but recovered by R + 30. Peak HR was not different from preflight at any time during or following flight. A sustained decrease in (V) over dot O-2peak during and/or early postflight was not a universal finding in this study, since seven astronauts were able to attain their preflight (V) over dot O-2peak levels either at some time during flight or on R + 1. Four of these astronauts performed in-flight exercise at higher intensities compared with those who experienced a decline in (V) over dot O-2peak , and three had low aerobic capacities before flight. These data indicate that, while (V) over dot O-2peak may be difficult to maintain during long-duration ISS missions, aerobic deconditioning is not an inevitable consequence of long-duration spaceflight. C1 [Moore, Alan D., Jr.; Lee, Stuart M. C.] Technol & Engn Grp, Houston, TX USA. [Downs, Meghan E.] Univ Houston, Houston, TX USA. [Feiveson, Alan H.] NASA, Johnson Space Ctr, Houston, TX USA. [Knudsen, Poul] Danish Aerosp Co, Odense, Denmark. [Ploutz-Snyder, Lori] Univ Space Res Assoc, Houston, TX USA. RP Downs, ME (reprint author), Mail Code SK,1290 Hercules Ave, Houston, TX 77058 USA. EM meghan.e.everett@nasa.gov FU NASA Human Research Program FX This research was supported by the NASA Human Research Program. NR 48 TC 16 Z9 17 U1 1 U2 14 PU AMER PHYSIOLOGICAL SOC PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA SN 8750-7587 EI 1522-1601 J9 J APPL PHYSIOL JI J. Appl. Physiol. PD AUG 1 PY 2014 VL 117 IS 3 BP 231 EP 238 DI 10.1152/japplphysiol.01251.2013 PG 8 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA AO4LK UT WOS:000341309400005 PM 24970852 ER PT J AU Rauscher, BJ Boehm, N Cagiano, S Delo, GS Foltz, R Greenhouse, MA Hickey, M Hill, RJ Kan, E Lindler, D Mott, DB Waczynski, A Wen, YT AF Rauscher, Bernard J. Boehm, Nicholas Cagiano, Steve Delo, Gregory S. Foltz, Roger Greenhouse, Matthew A. Hickey, Michael Hill, Robert J. Kan, Emily Lindler, Don Mott, D. Brent Waczynski, Augustyn Wen, Yiting TI New and Better Detectors for the JWST Near-Infrared Spectrograph SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID WEBB-SPACE-TELESCOPE AB ESA and NASA recently selected two 5 mu m cutoff Teledyne H2RG sensor chip assemblies (S CA) for flight on the James Webb Space Telescope (JWST) Near Infrared Spectrograph (NIRSpec). These HgCdTe SCAs incorporate Teledyne's "improved barrier layer" design that eliminates the degradation that affected earlier JWST H2RGs. The better indium barrier, together with other design changes that Teledyne phased in from other programs over the years, has improved the performance and reliability of JWST's SCAs. In this article, we describe the measured performance characteristics that most directly affect scientific observations including read noise, total noise, dark current, quantum efficiency (QE), and image persistence. As part of measuring QE, we inferred the quantum yield over the full NIRSpec pass band of lambda = 0.6-5 mu m and found that it exceeds unity for photon energies E-gamma > (2.65 +/- .2)E-g, where E-g is the HgCdTe bandgap energy. This corresponds to lambda less than or similar to 2 mu m for NIRSpec's 5 mu m cutoff HgCdTe. C1 [Rauscher, Bernard J.; Cagiano, Steve; Foltz, Roger; Greenhouse, Matthew A.; Hickey, Michael; Kan, Emily; Mott, D. Brent; Waczynski, Augustyn; Wen, Yiting] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Boehm, Nicholas; Delo, Gregory S.] Global Sci & Technol Inc GST, Greenbelt, MD 20770 USA. [Hill, Robert J.] Conceptual Analyt LLC, Glenn Dale, MD USA. [Lindler, Don] Sigma Space Corp, Lanham, MD 20706 USA. RP Rauscher, BJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Bernard.J.Rauscher@nasa.gov FU NASA FX This work was supported by NASA as part of the James Webb Space Telescope Project. We are very grateful to John Auyeung, who manages JWST work at Teledyne, and to Eric Piquette, our HgCdTe lead at Teledyne. Both did a fantastic job making the new detectors possible! We also wish to thank Drs. Mike Regan and Peter McCullough of the Space Telescope Science Institute (STScI), both of whom read the manuscript and provided valuable feedback. NR 22 TC 10 Z9 10 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD AUG PY 2014 VL 126 IS 942 BP 739 EP 749 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO3KH UT WOS:000341227600002 ER PT J AU Pinzon, JE Tucker, CJ AF Pinzon, Jorge E. Tucker, Compton J. TI A Non-Stationary 1981-2012 AVHRR NDVI3g Time Series SO REMOTE SENSING LA English DT Article DE Advanced Very High Resolution Radiometer (AVHRR); Normalized Difference Vegetation Index (NDVI); Bayesian analysis; uncertainty; bias; climate variability; non-stationary ID HIGH-RESOLUTION RADIOMETER; NEAR-INFRARED CHANNELS; LAND DATA SET; SATELLITE DATA; INTERSATELLITE CALIBRATION; MONITORING VEGETATION; TROPOSPHERIC AEROSOL; ARCTIC TUNDRA; GLOBAL DATA; DATA RECORD AB The NDVI3g time series is an improved 8-km normalized difference vegetation index (NDVI) data set produced from Advanced Very High Resolution Radiometer (AVHRR) instruments that extends from 1981 to the present. The AVHRR instruments have flown or are flying on fourteen polar-orbiting meteorological satellites operated by the National Oceanic and Atmospheric Administration (NOAA) and are currently flying on two European Organization for the Exploitation of Meteorological Satellites (EUMETSAT) polar-orbiting meteorological satellites, MetOp-A and MetOp-B. This long AVHRR record is comprised of data from two different sensors: the AVHRR/2 instrument that spans July 1981 to November 2000 and the AVHRR/3 instrument that continues these measurements from November 2000 to the present. The main difficulty in processing AVHRR NDVI data is to properly deal with limitations of the AVHRR instruments. Complicating among-instrument AVHRR inter-calibration of channels one and two is the dual gain introduced in late 2000 on the AVHRR/3 instruments for both these channels. We have processed NDVI data derived from the Sea-Viewing Wide Field-of-view Sensor (SeaWiFS) from 1997 to 2010 to overcome among-instrument AVHRR calibration difficulties. We use Bayesian methods with high quality well-calibrated SeaWiFS NDVI data for deriving AVHRR NDVI calibration parameters. Evaluation of the uncertainties of our resulting NDVI values gives an error of +/- 0.005 NDVI units for our 1981 to present data set that is independent of time within our AVHRR NDVI continuum and has resulted in a non-stationary climate data set. C1 [Pinzon, Jorge E.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Tucker, Compton J.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA. RP Pinzon, JE (reprint author), NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA. EM jorge.e.pinzon@nasa.gov; compton.j.tucker@nasa.gov FU NASA [NNH08CD31C] FX This work was partially supported by NASA Applied Science grant NNH08CD31C from 2009 to 2012. We thank the financial support by George Collatz, Torry Johnson, and Molly Brown during the last year. We thank Edwin Pak for processing the AVHRR/3 input data to NDVI3g. Creating a consistent NDVI3g time series has been 8 years in the making and many insightful works using the data set on their analysis have contributed to its improvement. We thank supportive feedback from George Collatz, Ranga Myneni, Uma Bhatt, Martha Raynolds, Howard Epstein and Skip Walker and thank them for their comments on various parts of this article. We also thank the anonymous reviewers for their valuable remarks and suggestions. Lastly, two more important acknowledgments: first, since digital data are ephemeral and access to data involves infrastructure and economic support, we are in debt with Ramakrishna Nemani and his group at NASA Earth Exchange (NEX) for providing the infrastructure that supports data stewardship and makes it viable. Second, we have been fortunate to interact with the group at the SeaWiFS project. They not only provided us with high quality SeaWiFS data, but also shared valuable information related to calibration, data processing, and handling that is generally not included in scientific journal articles. NR 88 TC 112 Z9 118 U1 3 U2 42 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD AUG PY 2014 VL 6 IS 8 BP 6929 EP 6960 DI 10.3390/rs6086929 PG 32 WC Remote Sensing SC Remote Sensing GA AO7FV UT WOS:000341518700008 ER PT J AU Lee, HJ Zhang, SJ Bar-Cohen, Y Sherrit, S AF Lee, Hyeong Jae Zhang, Shujun Bar-Cohen, Yoseph Sherrit, Stewart TI High Temperature, High Power Piezoelectric Composite Transducers SO SENSORS LA English DT Review DE piezocomposites; high temperature; high power; transducer; sensor ID THERMAL-CONDUCTIVITY; ULTRASONIC TRANSDUCER; POLYMER COMPOSITES; PC-MUT; CERAMICS; BIMORPHS; SENSOR; PIEZOCOMPOSITES; CONNECTIVITY; STABILITY AB Piezoelectric composites are a class of functional materials consisting of piezoelectric active materials and non-piezoelectric passive polymers, mechanically attached together to form different connectivities. These composites have several advantages compared to conventional piezoelectric ceramics and polymers, including improved electromechanical properties, mechanical flexibility and the ability to tailor properties by using several different connectivity patterns. These advantages have led to the improvement of overall transducer performance, such as transducer sensitivity and bandwidth, resulting in rapid implementation of piezoelectric composites in medical imaging ultrasounds and other acoustic transducers. Recently, new piezoelectric composite transducers have been developed with optimized composite components that have improved thermal stability and mechanical quality factors, making them promising candidates for high temperature, high power transducer applications, such as therapeutic ultrasound, high power ultrasonic wirebonding, high temperature non-destructive testing, and downhole energy harvesting. This paper will present recent developments of piezoelectric composite technology for high temperature and high power applications. The concerns and limitations of using piezoelectric composites will also be discussed, and the expected future research directions will be outlined. C1 [Lee, Hyeong Jae; Bar-Cohen, Yoseph; Sherrit, Stewart] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lee, Hyeong Jae; Zhang, Shujun] Penn State Univ, Mat Res Inst, University Pk, PA 16802 USA. RP Lee, HJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM hjlee@jpl.nasa.gov; soz1@psu.edu; yoseph.bar-cohen@jpl.nasa.gov; stewart.sherrit@jpl.nasa.gov FU ONR; NIH [2P41EB002182-15A1.O] FX The authors thank to Thomas R. Shrout for the helpful discussions and his supports. Some of the research reported in this manuscript was conducted at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with National Aeronautics and Space Administration (NASA). Also, part of the reported research was supported by ONR and NIH under contract No. 2P41EB002182-15A1.O. NR 96 TC 8 Z9 8 U1 11 U2 88 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 1424-8220 J9 SENSORS-BASEL JI Sensors PD AUG PY 2014 VL 14 IS 8 BP 14526 EP 14552 DI 10.3390/s140814526 PG 27 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation SC Chemistry; Electrochemistry; Instruments & Instrumentation GA AO6YX UT WOS:000341499900060 PM 25111242 ER PT J AU Han, XG Funk, MR Shen, F Chen, YC Li, YY Campbell, CJ Dai, JQ Yang, XF Kim, JW Liao, YL Connell, JW Barone, V Chen, ZF Lin, Y Hu, LB AF Han, Xiaogang Funk, Michael R. Shen, Fei Chen, Yu-Chen Li, Yuanyuan Campbell, Caroline J. Dai, Jiaqi Yang, Xiaofeng Kim, Jae-Woo Liao, Yunlong Connell, John W. Barone, Veronica Chen, Zhongfang Lin, Yi Hu, Liangbing TI Scalable Holey Graphene Synthesis and Dense Electrode Fabrication toward High-Performance Ultracapacitors SO ACS NANO LA English DT Article DE scalable synthesis; facile processability; holey graphene; dense graphene electrode; ultracapacitor; supercapacitor; volumetric capacitance ID SCANNING-TUNNELING-MICROSCOPY; ORIENTED PYROLYTIC-GRAPHITE; ACTIVATED GRAPHENE; ENERGY-STORAGE; SUPERCAPACITOR ELECTRODES; MOLECULAR-MECHANICS; OXIDE; FILMS; OXIDATION; NANOMESH AB Graphene has attracted a lot of attention for ultracapacitor electrodes because of its high electrical conductivity, high surface area and superb chemical stability. However, poor volumetric capacitive performance of typical graphene-based electrodes has hindered their practical applications because of the extremely low density. Herein we report a scalable synthesis method of holey graphene (h-Graphene) in a single step without using any catalysts or special chemicals The film made of the as synthesized h-Graphene exhibited relatively strong mechanical strength, 2D hole morphology, high density, and facile processability. This scalable one-step synthesis method for h-Graphene is time environmentally friendly, and generally applicable to other two-dimensional materials The ultracapacitor electrodes based on remarkably improved volumetric capacitance with about 700% increase compared to that of regular graphene electrodes. h-Graphene was carried out to understand the excellent processability and improved ultracapacitor performance. efficient, the h-Graphene show a Modeling on individual cost-efficient, C1 [Han, Xiaogang; Shen, Fei; Chen, Yu-Chen; Li, Yuanyuan; Dai, Jiaqi; Yang, Xiaofeng; Hu, Liangbing] Univ Maryland, Dept Mat Sci & Engn, College Pk, MD 20742 USA. [Funk, Michael R.; Lin, Yi] Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA. [Funk, Michael R.; Connell, John W.] NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA. [Campbell, Caroline J.; Kim, Jae-Woo; Liao, Yunlong; Lin, Yi] Natl Inst Aerosp, Hampton, VA 23666 USA. [Barone, Veronica] Cent Michigan Univ, Adv Mat Program, Dept Phys & Sci, Mt Pleasant, MI 48859 USA. [Liao, Yunlong; Chen, Zhongfang] Univ Puerto Rico, Inst Funct Nanomat, Dept Chem, San Juan, PR 00931 USA. RP Lin, Y (reprint author), Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA. EM yi.lin@nianet.org; binghu@umd.edu RI Kim, Jae-Woo/A-8314-2008; Barone, Veronica/C-2634-2008; Chen, Zhongfang/A-3397-2008; Hu, Liangbing/N-6660-2013; Han, Xiaogang/D-6430-2015 OI Han, Xiaogang/0000-0002-4785-6506 FU NSF-CBET [1335944, 1335979]; Leading Edge Aeronautics Research for NASA (LEARN) program [NNX13AB88A]; NASA Pathways Intern Employment Program (IEP); LEARN; Department of Defense [W911NF-12-1-0083]; NASA [NNX10AM80H, NNX13AB22A] FX The authors thank Dr. W. Cao and Prof. H. Elsayed-Ali at Applied Research Center of Old Dominion University for their experimental assistance in acquiring TEM images. V.B. and L.H. gratefully acknowledge the support from NSF-CBET Grant Nos. 1335944 and 1335979, respectively. Y.L. and J.K. acknowledge the financial support from the Leading Edge Aeronautics Research for NASA (LEARN) program (Grant No. NNX13AB88A). M.F. is supported by the NASA Pathways Intern Employment Program (IEP). C.C. was a Langley Aerospace Research Summer Scholars (LARSS) Program scholar supported by LEARN. Z.C. acknowledges the support by Department of Defense (Grant No. W911NF-12-1-0083) and NASA (Grant Nos. NNX10AM80H and NNX13AB22A). We thank Prof. D. DeVoe, Dr. E. Kendall, and the Maryland Microfluidic Laboratory (MML) for providing access to the goniometer. NR 45 TC 50 Z9 50 U1 32 U2 246 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1936-0851 EI 1936-086X J9 ACS NANO JI ACS Nano PD AUG PY 2014 VL 8 IS 8 BP 8255 EP 8265 DI 10.1021/nn502635y PG 11 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA AO0IM UT WOS:000340992300072 PM 25093751 ER PT J AU Bishop, JL Quinn, R Dyar, MD AF Bishop, Janice L. Quinn, Richard Dyar, M. Darby TI Spectral and thermal properties of perchlorate salts and implications for Mars SO AMERICAN MINERALOGIST LA English DT Article DE Perchlorate; Mars; reflectance spectroscopy; differential scanning calorimetry; hydrated salts ID CRYSTAL-STRUCTURE; INFRARED-SPECTRA; EMISSION-SPECTROSCOPY; SOUTHERN HIGHLANDS; RAMAN-SPECTROSCOPY; PHASE-TRANSITIONS; MARTIAN SOIL; LANDING SITE; COMPLEXES; CHEMISTRY AB K+, Na2+, Mg2+, Fe2+, Fe3+, and Al3+ perchlorate salts were studied to provide spectral and thermal data for detecting and characterizing their possible presence on Mars. Spectral and thermal analyses are coordinated with structural analyses to understand how different cations and different hydration levels affect the mineral system. Near-infrared (NIR) spectral features for perchlorates are dominated by H2O bands that occur at 0.978-1.01, 1.17-1.19, 1.42-1.48, 1.93-1.99, and 2.40-2.45 mu m. Mid-IR spectral features are observed for vibrations of the tetrahedral ClO4- ion and occur as reflectance peaks at 1105-1130 cm(-1) (similar to 8.6-9 mu m), 760-825 cm(-1) (similar to 12-13 mu m), 630 cm(-1) (similar to 15.9 mu m), 460-495 (similar to 20-22 pm), and 130-215 (similar to 50-75 mu m). The spectral bands in both regions are sensitive to the type of cation present because the polarizing power is related to the band center for many of the spectral features. Band assignments were confirmed for many of the spectral features due to opposing trends in vibrational energies for the ClO4-, and H2O groups connected to different octahedral cations. Differential scanning calorimetry (DSC) data show variable patterns of water loss and thermal decomposition temperatures for perchlorates with different cations, consistent with changes in spectral features measured under varying hydration conditions. Results of the DSC analyses indicate that the bond energies of H2O in perchlorates are different for each cation and hydration state. Structural parameters are available for Mg perchlorates (Robertson and Bish 2010) and the changes in structure due to hydration state are consistent with DSC parameters and spectral features. Analyses of changes in the Mg perchlorate structures with H2O content inform our understanding of the effects of hydration on other perchlorates, for which the specific structures are less well defined. Spectra of the hydrated Fe2+ and Fe3+ perchlorates changed significantly upon heating to 100 degrees C or measurement under low-moisture conditions indicating that they are less stable than other perchlorates under dehydrated conditions. The perchlorate abundances observed by Phoenix and MSL are likely too low to be identified from orbit by CRISM, but may be sufficient to be identifiable by a VNIR imager on a future rover. C1 [Bishop, Janice L.; Quinn, Richard] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. [Bishop, Janice L.; Quinn, Richard] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Dyar, M. Darby] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. RP Bishop, JL (reprint author), Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. EM jbishop@seti.org FU NASA Astrobiology: Exobiology and Evolutionary Biology Program [NNX09AM93G, NNX13A167G] FX We are grateful for support from NASA Astrobiology: Exobiology and Evolutionary Biology Program grants NNX09AM93G and NNX13A167G. We also thank T. Hiroi at Brown University's RELAB for measuring many of the reflectance spectra used in the study and the helpful suggestions from two anonymous reviewers. NR 87 TC 7 Z9 7 U1 3 U2 29 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD AUG-SEP PY 2014 VL 99 IS 8-9 BP 1580 EP 1592 DI 10.2138/am.2014.4707 PG 13 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AN4TD UT WOS:000340580500008 ER PT J AU Pitman, KM Dobrea, EZN Jamieson, CS Dalton, JB Abbey, WJ Joseph, ECS AF Pitman, Karly M. Dobrea, Eldar Z. Noe Jamieson, Corey S. Dalton, James B., III Abbey, William J. Joseph, Emily C. S. TI Reflectance spectroscopy and optical functions for hydrated Fe-sulfates SO AMERICAN MINERALOGIST LA English DT Article DE Jarosite; szomolnokite; rhomboclase; optical constants; visible to near-infrared wavelength; laboratory diffuse reflectance spectroscopy ID THERMAL EMISSION-SPECTRA; SOLID-SOLUTION SERIES; PARTICULATE SURFACES; MARTIAN METEORITES; CRYSTAL-CHEMISTRY; NAKHLA METEORITE; SITE OCCUPANCY; MARS; MINERALS; JAROSITE AB Visible and near-infrared wavelength (VNIR, lambda = 0.35-5 mu m) laboratory diffuse reflectance spectra and corresponding optical functions (real and imaginary refractive indices) for several iron sulfates (natural K- and Na-jarosite, szomolnokite, rhomboclase) are presented. On Mars, jarosite has been identified in Meridiani Planum, Mawrth Vallis, Melas Chasma, and Eridania Basin; szomolnokite has been found as distinct layers at Columbus Crater and as outcrops at Juventae Chasma, and rhomboclase has been identified at Gusev Crater. Constraining the mineralogy and chemistry (Fe- vs. Mg-rich) of the sulfates on Mars may contribute to our understanding of the environmental and aqueous conditions present on Mars during their formation. The data presented here will help to constrain the mineralogy, abundance, and distribution of sulfates on the martian surface, which will lead to improvements in understanding the pressure, temperature, and humidity conditions and how active frost, groundwater, and atmospheric processes once were on Mars. C1 [Pitman, Karly M.; Dobrea, Eldar Z. Noe; Joseph, Emily C. S.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Jamieson, Corey S.] SETI Inst, Mountain View, CA 94043 USA. [Dalton, James B., III; Abbey, William J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pitman, KM (reprint author), Planetary Sci Inst, 1700 E Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA. EM pitman@psi.edu FU NASA's Mars Fundamental Research Program [NNX10AP78G] FX This work was supported by NASA's Mars Fundamental Research Program (NNX10AP78G: PI Pitman) and partly performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration. The authors thank Robert Anderson, Janice Bishop, Adrian Brown, Ed Cloutis, Ken Farley, Troy Hudson, Joel Hurowitz, Brendt Hyde, Penny King, and Melissa Lane for helpful comments, conversations, and assistance with samples and equipment. This is PSI Contribution No. 614. NR 84 TC 3 Z9 3 U1 1 U2 17 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD AUG-SEP PY 2014 VL 99 IS 8-9 BP 1593 EP 1603 DI 10.2138/am.2014.4730 PG 11 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AN4TD UT WOS:000340580500009 ER PT J AU Werdell, PJ Roesler, CS Goes, JI AF Werdell, P. Jeremy Roesler, Collin S. Goes, Joaquim I. TI Discrimination of phytoplankton functional groups using an ocean reflectance inversion model SO APPLIED OPTICS LA English DT Article ID INHERENT OPTICAL-PROPERTIES; CHLOROPHYLL-A CONCENTRATION; ABSORPTION-COEFFICIENTS; BACKSCATTERING RATIO; COLOR RADIOMETRY; LIGHT-ABSORPTION; CHESAPEAKE BAY; CASE-1 WATERS; SIZE CLASSES; ARABIAN SEA AB Ocean reflectance inversion models (ORMs) provide a mechanism for inverting the color of the water observed by a satellite into marine inherent optical properties (IOPs), which can then be used to study phytoplankton community structure. Most ORMs effectively separate the total signal of the collective phytoplankton community from other water column constituents; however, few have been shown to effectively identify individual contributions by multiple phytoplankton groups over a large range of environmental conditions. We evaluated the ability of an ORM to discriminate between Noctiluca miliaris and diatoms under conditions typical of the northern Arabian Sea. We: (1) synthesized profiles of IOPs that represent bio-optical conditions for the Arabian Sea; (2) generated remote-sensing reflectances from these profiles using Hydrolight; and (3) applied the ORM to the synthesized reflectances to estimate the relative concentrations of diatoms and N. miliaris. By comparing the estimates from the inversion model with those from synthesized vertical profiles, we identified those conditions under which the ORM performs both well and poorly. Even under perfectly controlled conditions, the absolute accuracy of ORM retrievals degraded when further deconstructing the derived total phytoplankton signal into subcomponents. Although the absolute magnitudes maintained biases, the ORM successfully detected whether or not Noctiluca miliaris appeared in the simulated water column. This quantitatively calls for caution when interpreting the absolute magnitudes of the retrievals, but qualitatively suggests that the ORM provides a robust mechanism for identifying the presence or absence of species. (C) 2014 Optical Society of America C1 [Werdell, P. Jeremy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Werdell, P. Jeremy] Univ Maine, Sch Marine Sci, Orono, ME 04469 USA. [Roesler, Collin S.] Bowdoin Coll, Dept Earth & Ocean Sci, Brunswick, ME 04011 USA. [Goes, Joaquim I.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. RP Werdell, PJ (reprint author), NASA, Goddard Space Flight Ctr, Code 616, Greenbelt, MD 20771 USA. EM jeremy.werdell@nasa.gov FU NASA Ocean Biology and Biogeochemistry Program [NNX11AE22G] FX Many thanks to Sean Bailey, Gene Feldman, Curt Mobley, Mary Jane Perry, Andrew Thomas, Huijie Xue, and Emmanuel Boss for their advice throughout the development of this manuscript. Thanks also to Susan Drapeau, Kelly Keebler, Helga do Rosario Gomes, Prahbu Matondkar, and colleagues at the National Institute of Oceanography, India for their support with field experiments and data analysis. Finally, many thanks to Stephane Maritorena and an anonymous reviewer for their exceptional comments and attention to detail. Support for this work was provided through the NASA Ocean Biology and Biogeochemistry Program under research grant NNX11AE22G. NR 74 TC 7 Z9 7 U1 4 U2 20 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD AUG 1 PY 2014 VL 53 IS 22 BP 4833 EP 4849 DI 10.1364/AO.53.004833 PG 17 WC Optics SC Optics GA AN8BC UT WOS:000340824800017 PM 25090312 ER PT J AU Roberts, LE Ward, RL Sutton, AJ Fleddermann, R de Vine, G Malikides, EA Wuchenich, DMR McClelland, DE Shaddock, DA AF Roberts, Lyle E. Ward, Robert L. Sutton, Andrew J. Fleddermann, Roland de Vine, Glenn Malikides, Emmanuel A. Wuchenich, Danielle M. R. McClelland, David E. Shaddock, Daniel A. TI Coherent beam combining using a 2D internally sensed optical phased array SO APPLIED OPTICS LA English DT Article ID ENHANCED HETERODYNE INTERFEROMETRY; FIBER AMPLIFIER; KW; LOCKING AB Coherent combination of multiple lasers using an optical phased array (OPA) is an effective way to scale optical intensity in the far field beyond the capabilities of single fiber lasers. Using an actively phase locked, internally sensed, 2D OPA we demonstrate over 95% fringe visibility of the interfered beam, lambda/120 RMS output phase stability over a 5 Hz bandwidth, and quadratic scaling of intensity in the far field using three emitters. This paper presents a new internally sensed OPA architecture that employs a modified version of digitally enhanced heterodyne interferometry (DEHI) based on code division multiplexing to measure and control the phase of each emitter. This internally sensed architecture can be implemented with no freespace components, offering improved robustness to shock and vibration exhibited by all-fiber devices. To demonstrate the concept, a single laser is split into three channels/emitters, each independently controlled using separate electro-optic modulators. The output phase of each channel is measured using DEHI to sense the small fraction of light that is reflected back into the fiber at the OPA's glass-air interface. The relative phase between emitters is used to derive the control signals needed to stabilize their relative path lengths and maintain coherent combination in the far field. (C) 2014 Optical Society of America C1 [Roberts, Lyle E.; Ward, Robert L.; Sutton, Andrew J.; Fleddermann, Roland; Malikides, Emmanuel A.; Wuchenich, Danielle M. R.; McClelland, David E.; Shaddock, Daniel A.] Australian Natl Univ, Dept Quantum Sci, Canberra, ACT 0200, Australia. [de Vine, Glenn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Roberts, LE (reprint author), Australian Natl Univ, Dept Quantum Sci, GPO Box 4, Canberra, ACT 0200, Australia. EM Lyle.Roberts@anu.edu.au RI McClelland, David/E-6765-2010; Shaddock, Daniel/A-7534-2011; Ward, Robert/I-8032-2014 OI McClelland, David/0000-0001-6210-5842; Shaddock, Daniel/0000-0002-6885-3494; Ward, Robert/0000-0001-5503-5241 NR 11 TC 1 Z9 1 U1 3 U2 12 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD AUG 1 PY 2014 VL 53 IS 22 BP 4881 EP 4885 DI 10.1364/AO.53.004881 PG 5 WC Optics SC Optics GA AN8BC UT WOS:000340824800022 PM 25090317 ER PT J AU Potter, C AF Potter, Christopher TI Regional analysis of MODIS satellite greenness trends for ecosystems of interior Alaska SO GISCIENCE & REMOTE SENSING LA English DT Article DE MODIS EVI; forest; tundra; wetlands; wildfire; Alaska ID POSTFIRE VEGETATION; FIRE DISTURBANCE; FOREST RECOVERY; BURN SEVERITY; TIME-SERIES; CLIMATE; VULNERABILITY; INDEXES; GROWTH; TUNDRA AB Trends in the growing season Moderate Resolution Imaging Spectroradiometer (MODIS) Enhanced Vegetation Index (EVI) time-series were analyzed for the time period from 2000 to 2010 to understand landscape-level patterns of vegetation change in ecosystems of interior Alaska. The analysis compared data-sets for Alaska vegetation cover types, wetland cover classes, wildfire boundaries since the 1940s, permafrost type, and elevation to identify the most likely combination of factors driving regional changes in habitat quality and ecosystem productivity. Approximately 48% of all ecosystem areas in interior Alaska were detected with significant (p < 0.05) positive or negative MODIS growing season EVI trends from 2000 to 2010. Three-quarters of these ecosystem areas (nearly 110,000 km(2)) were detected with significant positive growing season EVI trends. The vast majority of interior Alaska area detected with significant positive growing season EVI trends was classified as upland shrub cover, although non-forested wetlands (marshes, bogs, fens, and floodplains) were colocated on 13% of that total area. Evidence supports the hypothesis that temperature (warming) has markedly enhanced the rates of shrubland and tundra vegetation growth across interior Alaska over recent years. C1 NASA, Ames Res Ctr, Mountain View, CA 94035 USA. RP Potter, C (reprint author), NASA, Ames Res Ctr, Mail Stop 232-21, Mountain View, CA 94035 USA. EM chris.potter@nasa.gov FU NASA under the US National Climate Assessment FX This work was conducted with support from NASA under the US National Climate Assessment. NR 33 TC 6 Z9 7 U1 4 U2 21 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1548-1603 EI 1943-7226 J9 GISCI REMOTE SENS JI GISci. Remote Sens. PD AUG PY 2014 VL 51 IS 4 BP 390 EP 402 DI 10.1080/15481603.2014.933606 PG 13 WC Geography, Physical; Remote Sensing SC Physical Geography; Remote Sensing GA AN9TG UT WOS:000340951100003 ER PT J AU Kereszturi, A Blumberger, Z Jozsa, S May, Z Muller, A Szabo, M Toth, M AF Kereszturi, A. Blumberger, Z. Jozsa, S. May, Z. Mueller, A. Szabo, M. Toth, M. TI Alteration processes in the CV chondrite parent body based on analysis of NWA 2086 meteorite SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CARBONACEOUS CHONDRITE; AQUEOUS ALTERATION; MINERAL CHEMISTRY; ALLENDE METEORITE; CM CHONDRITES; SOLAR NEBULA; DARK RIMS; ORIGIN; INCLUSIONS; CHONDRULES AB Analysis of the NWA 2086 CV3 chondrite showed a matrix/chondrule ratio of 52%, similar to Bali, Mokoia, and Grosanaja. Nearly twice as many chondrule fragments as intact ones demonstrate that an early fragmentation phase occurred prior to final accretion. After this event, no substantial mechanical change or redeposition is evident. Rims with double-layered structures were identified around some chondrules, which, in at least one case, is attributed to an accretionary origin. The rim's outer parts with a diffuse appearance were formed by in situ chemical alteration. During this later process, Mg content decreased, Fe content increased, and olivine composition was homogenized, producing a rim composition close to that of the matrix. This alteration occasionally happened along fractures and at confined locations, and was probably produced by fluid interactions. Iron oxides are the best candidate for a small grain-sized alteration product; however, technical limitations in the available equipment did not allow exact phase identification. These results suggest that NWA 2086 came from a location (possible more deeply buried) in the CV parent body than Mokoia or Bali, and suffered less impact effects-although there is no evidence of sustained thermal alteration. This meteorite may represent a sample of the CV parent asteroid interior and provide a useful basis for comparison with other CV meteorites in the future. C1 [Kereszturi, A.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Thege Miklos Astron Inst, Astrophys & Geochem Lab, H-1121 Budapest, Hungary. [Blumberger, Z.] Eotvos Lorand Univ Sci, Hungarian Acad Sci, Fac Sci, Ctr Environm Sci, H-1117 Budapest, Hungary. [Jozsa, S.] Eotvos Lorand Univ Sci, Dept Petr & Geochem, Fac Sci, Hungarian Acad Sci, H-1117 Budapest, Hungary. [May, Z.] Hungarian Acad Sci, Chem Res Ctr, Inst Mat & Environm Chem, H-1025 Budapest, Hungary. [Mueller, A.; Szabo, M.; Toth, M.] Hungarian Acad Sci, Inst Geol & Geochem Res, Res Ctr Astron & Earth Sci, H-1112 Budapest, Hungary. [Kereszturi, A.] NASA, Astrobiol Inst, Thermodynam Disequilibrium & Evolut Focus Grp, Washington, DC USA. RP Kereszturi, A (reprint author), Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Thege Miklos Astron Inst, Astrophys & Geochem Lab, Konkoly 15-17, H-1121 Budapest, Hungary. EM kereszturi.akos@csfk.mta.hu FU Astrophysical and Geochemical Laboratory of CSFK, Hungary; Hungarian Academy of Sciences; COST [TD1308, TET_12_FR-1-2013-0023] FX This work was supported by the Astrophysical and Geochemical Laboratory of CSFK, Hungary, and also the Infrastructure and other related CSFK Fund of the Hungarian Academy of Sciences. The COST TD1308 and TET_12_FR-1-2013-0023 projects are also acknowledged. The authors thank the helpful suggestions from referees: M. Zolenksy, K. Fintor, an anonymous reviewer, and the editor T. Jull. NR 59 TC 5 Z9 5 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2014 VL 49 IS 8 BP 1350 EP 1364 DI 10.1111/maps.12336 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN8SZ UT WOS:000340875900004 ER PT J AU Jenniskens, P Rubin, AE Yin, QZ Sears, DWG Sandford, SA Zolensky, ME Krot, AN Blair, L Kane, D Utas, J Verish, R Friedrich, JM Wimpenny, J Eppich, GR Ziegler, K Verosub, KL Rowland, DJ Albers, J Gural, PS Grigsby, B Fries, MD Matson, R Johnston, M Silber, E Brown, P Yamakawa, A Sanborn, ME Laubenstein, M Welten, KC Nishiizumi, K Meier, MMM Busemann, H Clay, P Caffee, MW Schmitt-Kopplin, P Hertkorn, N Glavin, DP Callahan, MP Dworkin, JP Wu, QH Zare, RN Grady, M Verchovsky, S Emel'yanenko, V Naroenkov, S Clark, DL Girten, B Worden, PS AF Jenniskens, Peter Rubin, Alan E. Yin, Qing-Zhu Sears, Derek W. G. Sandford, Scott A. Zolensky, Michael E. Krot, Alexander N. Blair, Leigh Kane, Darci Utas, Jason Verish, Robert Friedrich, Jon M. Wimpenny, Josh Eppich, Gary R. Ziegler, Karen Verosub, Kenneth L. Rowland, Douglas J. Albers, Jim Gural, Peter S. Grigsby, Bryant Fries, Marc D. Matson, Robert Johnston, Malcolm Silber, Elizabeth Brown, Peter Yamakawa, Akane Sanborn, Matthew E. Laubenstein, Matthias Welten, Kees C. Nishiizumi, Kunihiko Meier, Matthias M. M. Busemann, Henner Clay, Patricia Caffee, Marc W. Schmitt-Kopplin, Phillipe Hertkorn, Norbert Glavin, Daniel P. Callahan, Michael P. Dworkin, Jason P. Wu, Qinghao Zare, Richard N. Grady, Monica Verchovsky, Sasha Emel'yanenko, Vacheslav Naroenkov, Sergey Clark, David L. Girten, Beverly Worden, Peter S. CA Novato Meteorite Consortium TI Fall, recovery, and characterization of the Novato L6 chondrite breccia SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID UNEQUILIBRATED ORDINARY CHONDRITES; PARK-FOREST METEORITE; INNER SOLAR-SYSTEM; COSMOGENIC NUCLIDES; EXPOSURE HISTORY; OXYGEN-ISOTOPE; CARBONACEOUS CHONDRITES; INNISFREE METEORITE; ASTEROIDAL SOURCE; STONY METEORITES AB The Novato L6 chondrite fragmental breccia fell in California on 17 October 2012, and was recovered after the Cameras for Allsky Meteor Surveillance (CAMS) project determined the meteor's trajectory between 95 and 46 km altitude. The final fragmentation from 42 to 22 km altitude was exceptionally well documented by digital photographs. The first sample was recovered before rain hit the area. First results from a consortium study of the meteorite's characterization, cosmogenic and radiogenic nuclides, origin, and conditions of the fall are presented. Some meteorites did not retain fusion crust and show evidence of spallation. Before entry, the meteoroid was 35 +/- 5 cm in diameter (mass 80 +/- 35 kg) with a cosmic-ray exposure age of 9 +/- 1 Ma, if it had a one-stage exposure history. A two-stage exposure history is more likely, with lower shielding in the last few Ma. Thermoluminescence data suggest a collision event within the last similar to 0.1 Ma. Novato probably belonged to the class of shocked L chondrites that have a common shock age of 470 Ma, based on the U, Th-He age of 420 +/- 220 Ma. The measured orbits of Novato, Jesenice, and Innisfree are consistent with a proposed origin of these shocked L chondrites in the Gefion asteroid family, perhaps directly via the 5: 2 mean-motion resonance with Jupiter. Novato experienced a stronger compaction than did other L6 chondrites of shock-stage S4. Despite this, a freshly broken surface shows a wide range of organic compounds. C1 [Jenniskens, Peter; Blair, Leigh; Albers, Jim; Gural, Peter S.; Grigsby, Bryant] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. [Jenniskens, Peter; Sears, Derek W. G.; Sandford, Scott A.; Girten, Beverly; Worden, Peter S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rubin, Alan E.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Yin, Qing-Zhu; Wimpenny, Josh; Verosub, Kenneth L.; Yamakawa, Akane; Sanborn, Matthew E.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Sears, Derek W. G.] BAER Inst, Mountain View, CA 94043 USA. [Zolensky, Michael E.; Fries, Marc D.] NASA, Johnson Space Ctr, Houston, TX 77801 USA. [Krot, Alexander N.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Kane, Darci] Buck Inst, Novato, CA 94945 USA. [Utas, Jason] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Verish, Robert] Meteorite Recovery Lab, Escondido, CA 92046 USA. [Friedrich, Jon M.] Fordham Univ, Dept Chem, Bronx, NY 10458 USA. [Friedrich, Jon M.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. [Eppich, Gary R.] Lawrence Livermore Natl Lab, Glenn Seaborg Inst, Livermore, CA 94550 USA. [Ziegler, Karen] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Rowland, Douglas J.] Univ Calif Davis, Ctr Mol & Genom Imaging, Davis, CA 95616 USA. [Matson, Robert] SAIC, San Diego, CA 92121 USA. [Johnston, Malcolm] US Geol Survey, Menlo Pk, CA 94025 USA. [Silber, Elizabeth; Brown, Peter; Clark, David L.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Laubenstein, Matthias] Inst Nazl Fis Nucl, Lab Nazl Gran Sasso, I-67010 Assergi, AQ, Italy. [Welten, Kees C.; Nishiizumi, Kunihiko] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Meier, Matthias M. M.] ETH, Dept Earth Sci, CH-8092 Zurich, Switzerland. [Meier, Matthias M. M.] Lund Univ, Dept Geol, SE-22362 Lund, Sweden. [Busemann, Henner; Clay, Patricia] Univ Manchester, SEAES, Manchester M13 9PL, Lancs, England. [Caffee, Marc W.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Schmitt-Kopplin, Phillipe; Hertkorn, Norbert] Helmholtz Zentrum Munchen, BGC, D-85764 Munich, Germany. [Schmitt-Kopplin, Phillipe] Tech Univ Munich, ALC, D-85354 Freising Weihenstephan, Germany. [Glavin, Daniel P.; Callahan, Michael P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Wu, Qinghao; Zare, Richard N.] Stanford Univ, Dept Chem, Stanford, CA 94305 USA. [Grady, Monica; Verchovsky, Sasha] Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. [Emel'yanenko, Vacheslav; Naroenkov, Sergey] Russian Acad Sci INASAN, Inst Astron, Moscow 119017, Russia. RP Jenniskens, P (reprint author), Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. EM petrus.m.jenniskens@nasa.gov RI Naroenkov, Sergey/I-5699-2013; Emel'yanenko, Vacheslav/A-4087-2014; Yin, Qing-Zhu/B-8198-2009; Caffee, Marc/K-7025-2015; Laubenstein, Matthias/C-4851-2013; Glavin, Daniel/D-6194-2012; Schmitt-Kopplin, Philippe/H-6271-2011; Dworkin, Jason/C-9417-2012; OI Eppich, Gary/0000-0003-2176-6673; Yin, Qing-Zhu/0000-0002-4445-5096; Caffee, Marc/0000-0002-6846-8967; Grady, Monica/0000-0002-4055-533X; Laubenstein, Matthias/0000-0001-5390-4343; Glavin, Daniel/0000-0001-7779-7765; Schmitt-Kopplin, Philippe/0000-0003-0824-2664; Dworkin, Jason/0000-0002-3961-8997; Busemann, Henner/0000-0002-0867-6908; Meier, Matthias/0000-0002-7179-4173; Rowland, Douglas/0000-0001-8059-6905; Clark, David/0000-0002-1203-764X; Sanborn, Matthew/0000-0003-3218-1195 FU NASA [NNX12AM14G, NNX08AO64G]; NASA Cosmochemistry program [NNG06GF95G, NNX11AJ51G, NNX11AC69G]; Swiss National Science Foundation (STFC) FX This consortium study was made possible thanks to the donation of meteorite N01 by Novato residents Lisa Webber and Glenn Rivera. Lynn Hofland of NASA Ames Research Center performed the tensile strength measurements. This work was supported by the NASA Near Earth Object Observation and Planetary Astronomy programs (NNX12AM14G and NNX08AO64G to P.J.), the NASA Cosmochemistry program (NNG06GF95G to A. R., NNX11AJ51G to Q.Z.Y. & A.N.K., and NNX11AC69G to K.N.), and the Swiss National Science Foundation (STFC). NR 124 TC 14 Z9 14 U1 0 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2014 VL 49 IS 8 BP 1388 EP 1425 DI 10.1111/maps.12323 PG 38 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN8SZ UT WOS:000340875900007 ER PT J AU Yin, QZ Zhou, Q Li, QL Li, XH Liu, Y Tang, GQ Krot, AN Jenniskens, P AF Yin, Qing-Zhu Zhou, Qin Li, Qiu-Li Li, Xian-Hua Liu, Yu Tang, Guo-Qiang Krot, Alexander N. Jenniskens, Peter TI Records of the Moon-forming impact and the 470 Ma disruption of the L chondrite parent body in the asteroid belt from U-Pb apatite ages of Novato (L6) SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ORDOVICIAN BIODIVERSIFICATION; FOSSIL METEORITES; SHOCK; CHROMITE; LEAD; OXYGEN; ORIGIN; EARTH; METAMORPHISM; AR-40-AR-39 AB Novato, a newly observed fall in the San Francisco Bay area, is a shocked and brecciated L6 ordinary chondrite containing dark and light lithologies. We have investigated the U-Pb isotope systematics of coarse Cl-apatite grains of metamorphic origin in Novato with a large geometry ion microprobe. The U-Pb systematics of Novato apatite reveals an upper intercept age of 4472 +/- 31 Ma and lower intercept age of 473 +/- 38 Ma. The upper intercept age is within error identical to the U-Pb apatite age of 4452 +/- 21 Ma measured in the Chelyabinsk LL5 chondrite. This age is interpreted to reflect a massive collisional resetting event due to a large impact associated with the peak arrival time at the primordial asteroid belt of ejecta debris from the Moon-forming giant impact on Earth. The lower intercept age is consistent with the most precisely dated Ar-Ar ages of 470 +/- 6 Ma of shocked L chondrites, and the fossil meteorites and extraterrestrial chromite relicts found in Ordovician limestones with an age of 467.3 +/- 1.6 Ma in Sweden and China. The lower intercept age reflects a major disturbance related to the catastrophic disruption of the L chondrite parent body most likely associated with the Gefion asteroid family, which produced an initially intense meteorite bombardment of the Earth in Ordovician period and reset and degassed at least approximately 35% of the L chondrite falls today. We predict that the 470 Ma impact event is likely to be found on the Moon and Mars, if not Mercury. C1 [Yin, Qing-Zhu] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Zhou, Qin] Chinese Acad Sci, Natl Astron Observ, Key Lab Lunar & Deep Space Explorat, Beijing 100012, Peoples R China. [Li, Qiu-Li; Li, Xian-Hua; Liu, Yu; Tang, Guo-Qiang] Chinese Acad Sci, Inst Geol & Geophys, State Key Lab Lithospher Evolut, Beijing 100029, Peoples R China. [Krot, Alexander N.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Jenniskens, Peter] SETI Inst, Mountain View, CA 94043 USA. [Jenniskens, Peter] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Yin, QZ (reprint author), Univ Calif Davis, Dept Earth & Planetary Sci, One Shields Ave, Davis, CA 95616 USA. EM qyin@ucdavis.edu RI liu, yu/P-1081-2014; Yin, Qing-Zhu/B-8198-2009; OI liu, yu/0000-0001-7195-7393; Yin, Qing-Zhu/0000-0002-4445-5096; Li, Qiuli/0000-0002-7280-5508 FU NSFC grants [41222023, 41221002] FX We sincerely thank Darci Kane for making the Novato N06 meteorite sample available for this study. We thank the reviewers, P. Claeys, P. Heck, and H. Hidaka, for their constructive comments and the associate editor Gretchen Benedix and executive editor A. J. Timothy Jull and the editorial office staff for their efficient handling of the manuscript. QLL and XHL acknowledge support from NSFC grants 41222023 and 41221002. NR 75 TC 5 Z9 5 U1 0 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2014 VL 49 IS 8 BP 1426 EP 1439 DI 10.1111/maps.12340 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN8SZ UT WOS:000340875900008 ER PT J AU Udom, I Zhang, YY Ram, MK Stefanakos, EK Hepp, AF Elzein, R Schlaf, R Goswami, DY AF Udom, Innocent Zhang, Yangyang Ram, Manoj K. Stefanakos, Elias K. Hepp, Aloysius F. Elzein, Radwan Schlaf, Rudy Goswami, D. Yogi TI A simple photolytic reactor employing Ag-doped ZnO nanowires for water purification SO THIN SOLID FILMS LA English DT Article DE Silver; Zinc oxide; Nanowires; Photoreactor; Water Purification ID PHOTOCATALYTIC DEGRADATION; METHYL-ORANGE; NANORODS; PHOTODEGRADATION; LIGHT; GROWTH; ARRAY; DISINFECTION; PERFORMANCE; SUSPENSIONS AB Well-aligned native zinc oxide (ZnO) and silver-doped ZnO (Ag-ZnO) films were deposited on borosilicate glass via a simple, low-cost, low-temperature, scalable hydrothermal process. The as-synthesized ZnO and Ag-ZnO films were characterized by X-ray diffraction; scanning electron microscopy, UV-visible spectroscopy, and Fourier transform infrared spectroscopy. A simple photolytic reactor was fabricated and later used to find the optimum experimental conditions for photocatalytic performance. The photodegradation of methyl orange in water was investigated using as-prepared ZnO and Ag-ZnO nanowires, and was compared to P25 (a commercial photocatalyst) in both visible and UV radiations. The P25 and Ag-ZnO showed a similar photodegradation performance under UV light, but Ag-ZnO demonstrated superior photocatalytic activity under visible irradiation. The optimized doping of Ag in Ag-ZnO enhanced photocatalytic activity in a simple reactor design and indicated potential applicability of Ag-ZnO for large-scale purification of water under solar irradiation. (C) 2014 Elsevier B.V. All rights reserved. C1 [Udom, Innocent; Zhang, Yangyang; Ram, Manoj K.; Stefanakos, Elias K.] Univ S Florida, Clean Energy Res Ctr, Coll Engn, Tampa, FL 33620 USA. [Elzein, Radwan; Schlaf, Rudy] Univ S Florida, Dept Elect Engn, Tampa, FL 33620 USA. [Hepp, Aloysius F.] Univ S Florida, Dept Chem & Biomed Engn, Tampa, FL 33620 USA. [Goswami, D. Yogi] NASA Glenn Res Ctr, Res & Technol Directorate, Cleveland, OH 44135 USA. RP Ram, MK (reprint author), Univ S Florida, Clean Energy Res Ctr, 4202 E Fowler Ave,ENB 118,Loc NTA102, Tampa, FL 33620 USA. EM mkram@usf.edu OI Ram, Manoj/0000-0002-6833-5566 FU National Aeronautics and Space Administration (NASA) - Harriett Jenkins Pre-doctoral Fellowship; State of Florida through the Florida Energy Systems Consortium (FESC) funds FX This work was supported by the National Aeronautics and Space Administration (NASA) - Harriett Jenkins Pre-doctoral Fellowship and the State of Florida through the Florida Energy Systems Consortium (FESC) funds. NR 42 TC 6 Z9 6 U1 3 U2 41 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0040-6090 J9 THIN SOLID FILMS JI Thin Solid Films PD AUG 1 PY 2014 VL 564 BP 258 EP 263 DI 10.1016/j.tsf.2014.05.057 PG 6 WC Materials Science, Multidisciplinary; Materials Science, Coatings & Films; Physics, Applied; Physics, Condensed Matter SC Materials Science; Physics GA AN8KD UT WOS:000340852200035 ER PT J AU Farnocchia, D Chesley, SR Tholen, DJ Micheli, M AF Farnocchia, D. Chesley, S. R. Tholen, D. J. Micheli, M. TI High precision predictions for near-Earth asteroids: the strange case of (3908) Nyx SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY LA English DT Article DE Astrometric treatment; Orbit determination; Asteroids; Yarkovsky effect; Orbital drift ID RADIATION PRESSURE; YARKOVSKY; CATALOG AB In November 2004 radar delay measurements of near-Earth asteroid (3908) Nyx obtained at the Arecibo radio telescope turned out to be away from the orbital prediction. We prove that this discrepancy was caused by a poor astrometric treatment and an incomplete dynamical model, which did not account for nongravitational perturbations. To improve the astrometric treatment, we remove known star catalog biases, apply suitable weights to the observations, and use an aggressive outlier rejection scheme. The main issue related to the dynamical model is having not accounted for the Yarkovsky effect. Including the Yarkovsky perturbation in the model makes the orbital prediction and the radar measurements statistically consistent by both reducing the offset and increasing the prediction uncertainty to a more realistic level. This analysis shows the sensitivity of high precision predictions to the astrometric treatment and the Yarkovsky effect. By using the full observational dataset we obtain a detection of the Yarkovsky effect acting on Nyx corresponding to an orbital drift m/year. In turn, we derive constraints on thermal inertia and bulk density. In particular, we find that the bulk density of Nyx is around 1 g/cm, possibly less. To make sure that our results are not corrupted by an asteroid impact or a close approach with a perturbing asteroid not included in our dynamical model, we show that the astrometry provides no convincing evidence of an impulsive variation of Nyx's velocity while crossing the main belt region. C1 [Farnocchia, D.; Chesley, S. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tholen, D. J.; Micheli, M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Farnocchia, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Davide.Farnocchia@jpl.nasa.gov OI Micheli, Marco/0000-0001-7895-8209 FU NASA Postdoctoral Program at the Jet Propulsion Laboratory; California Institute of Technology; NASA; U.S. National Science Foundation [AST 0709500, AST 1109940] FX We thank Fabrizio Bernardi for obtaining and measuring some of the observations in Table 5. DF was supported for this research by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. SC conducted this research at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. DT and MM were funded by Grants AST 0709500 and AST 1109940 from the U.S. National Science Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this sacred mountain. NR 28 TC 1 Z9 1 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0923-2958 EI 1572-9478 J9 CELEST MECH DYN ASTR JI Celest. Mech. Dyn. Astron. PD AUG PY 2014 VL 119 IS 3-4 SI SI BP 301 EP 312 DI 10.1007/s10569-014-9536-9 PG 12 WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications SC Astronomy & Astrophysics; Mathematics GA AN3NQ UT WOS:000340495600007 ER PT J AU da Costa, ET Mora, MF Willis, PA do Lago, CL Jiao, H Garcia, CD AF da Costa, Eric Tavares Mora, Maria F. Willis, Peter A. do Lago, Claudimir L. Jiao, Hong Garcia, Carlos D. TI Getting started with open-hardware: Development and control of microfluidic devices SO ELECTROPHORESIS LA English DT Article DE Open-source; PDMS; Valves ID MICROCHIP-CAPILLARY-ELECTROPHORESIS; CONTACTLESS CONDUCTIVITY DETECTION; IN-SITU ANALYSIS; ELECTROCHEMICAL DETECTION; MASS-SPECTROMETRY; MEMBRANE VALVES; FOOD ANALYSIS; PUMPS; INSTRUMENTATION; INTEGRATION AB Understanding basic concepts of electronics and computer programming allows researchers to get the most out of the equipment found in their laboratories. Although a number of platforms have been specifically designed for the general public and are supported by a vast array of on-line tutorials, this subject is not normally included in university chemistry curricula. Aiming to provide the basic concepts of hardware and software, this article is focused on the design and use of a simple module to control a series of PDMS-based valves. The module is based on a low-cost microprocessor (Teensy) and open-source software (Arduino). The microvalves were fabricated using thin sheets of PDMS and patterned using CO2 laser engraving, providing a simple and efficient way to fabricate devices without the traditional photolithographic process or facilities. Synchronization of valve control enabled the development of two simple devices to perform injection (1.6 +/- 0.4 mu L/stroke) and mixing of different solutions. Furthermore, a practical demonstration of the utility of this system for microscale chemical sample handling and analysis was achieved performing an on-chip acid-base titration, followed by conductivity detection with an open-source low-cost detection system. Overall, the system provided a very reproducible (98%) platform to perform fluid delivery at the microfluidic scale. C1 [da Costa, Eric Tavares; Garcia, Carlos D.] Univ Texas San Antonio, Dept Chem, San Antonio, TX 78248 USA. [da Costa, Eric Tavares; do Lago, Claudimir L.] Univ Sao Paulo, Dept Quim Fundamental, Inst Quim, Sao Paulo, Brazil. [Mora, Maria F.; Willis, Peter A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Jiao, Hong] HJ Sci & Technol, Berkeley, CA USA. RP Garcia, CD (reprint author), Univ Texas San Antonio, Dept Chem, One UTSA Circle, San Antonio, TX 78248 USA. EM carlos.garcia@utsa.edu RI do Lago, Claudimir/A-1852-2008; Mora, Maria/C-9753-2009; Institute of Chemistry - USP, Dept. of Chemistry/B-8988-2012; Willis, Peter/I-6621-2012; da Costa, Eric/D-5387-2012; Garcia, Carlos/A-8681-2008 OI do Lago, Claudimir/0000-0003-1542-4343; da Costa, Eric/0000-0003-4489-3501; Garcia, Carlos/0000-0002-7583-5585 FU NASA STTR [NNX13CP49C]; University of Texas at San Antonio; National Institutes of Health through the Research Centers at Minority Institutions [G12MD007591] FX The authors gratefully acknowledge the financial support provided by NASA STTR (Contract number: NNX13CP49C), The University of Texas at San Antonio, and the National Institutes of Health through the Research Centers at Minority Institutions (G12MD007591). NR 50 TC 10 Z9 10 U1 8 U2 66 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0173-0835 EI 1522-2683 J9 ELECTROPHORESIS JI Electrophoresis PD AUG PY 2014 VL 35 IS 16 SI SI BP 2370 EP 2377 DI 10.1002/elps.201400128 PG 8 WC Biochemical Research Methods; Chemistry, Analytical SC Biochemistry & Molecular Biology; Chemistry GA AN2DU UT WOS:000340394800013 PM 24823494 ER PT J AU Bakermans, C Skidmore, ML Douglas, S McKay, CP AF Bakermans, Corien Skidmore, Mark L. Douglas, Susanne McKay, Christopher P. TI Molecular characterization of bacteria from permafrost of the Taylor Valley, Antarctica SO FEMS MICROBIOLOGY ECOLOGY LA English DT Article DE 16S rRNA gene; rpoB; cold adaptation; psychrophiles ID MCMURDO DRY VALLEYS; 16S RIBOSOMAL-RNA; AT-15 DEGREES-C; SIBERIAN PERMAFROST; MICROBIAL DIVERSITY; COLD ADAPTATION; GROWTH TEMPERATURES; VICTORIA LAND; PSYCHROPHILIC ENZYMES; COMMUNITY STRUCTURE AB While bacterial communities from McMurdo Dry Valley soils have been studied using molecular techniques, data from permafrost are particularly scarce given the logistical difficulties of sampling. This study examined the molecular diversity and culturability of bacteria in permafrost from the Taylor Valley (TV), Antarctica. A 16S rRNA gene clone library was constructed to assess bacterial diversity, while a clone library of the RNA polymerase beta subunit (rpoB) gene was constructed to examine amino acid composition of an essential protein-coding gene. The 16S rRNA gene clone library was dominated by Acidobacteria from Gp6 and Gemmatimonadetes. The rpoB gene clone library (created with primers designed in this study) was also dominated by Acidobacteria. The ability of sequence analyses to garner additional information about organisms represented by TV sequences was explored. Specifically, optimum growth temperature was estimated from the stem GC content of the 16S rRNA gene, while potential cold adaptations within translated rpoB sequences were assessed. These analyses were benchmarked using known psychrophiles and mesophiles. Bioinformatic analyses suggested that many TV sequences could represent organisms capable of activity at low temperatures. Plate counts confirmed that c. 10(3) cells per gram permafrost remained viable and were culturable, while laboratory respiration assays demonstrated that microbial activity occurred at -5 degrees C and peaked at 15 degrees C. C1 [Bakermans, Corien] Penn State Univ, Altoona Coll, Altoona, PA 16601 USA. [Skidmore, Mark L.] Montana State Univ, Bozeman, MT 59717 USA. [Douglas, Susanne] Planetary Sci Inst, Tucson, AZ USA. [McKay, Christopher P.] NASA Ames Res Ctr, Moffett Field, CA USA. RP Bakermans, C (reprint author), Penn State Univ, Altoona Coll, 3000 Ivyside Pk, Altoona, PA 16601 USA. EM cub21@psu.edu FU Penn State; NASA; NSF [0525567, 0636770]; NASA Astrobiology Science and Technology for Exploring Planets (ASTEP) program FX This study was supported by internal grants from Penn State to C.B. C.B. was also partially supported by a NASA Montana Space Grant and NSF 0525567. M. S. was partially supported by NSF Grants 0525567 and 0636770. Sample collection was supported by a NASA International Polar Year grant to Dr Leslie Tamppari, which supported C.P.M. S.D. was supported by the NASA Astrobiology Science and Technology for Exploring Planets (ASTEP) program. Many thanks to Penn State Altoona undergraduate students S. Gorman, S. Abbott, F. Wendt, and E. Malmberg. NR 109 TC 8 Z9 8 U1 1 U2 41 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0168-6496 EI 1574-6941 J9 FEMS MICROBIOL ECOL JI FEMS Microbiol. Ecol. PD AUG PY 2014 VL 89 IS 2 SI SI BP 331 EP 346 DI 10.1111/1574-6941.12310 PG 16 WC Microbiology SC Microbiology GA AN4CM UT WOS:000340535200011 PM 24592998 ER PT J AU Guilbert, J Beckage, B Winter, JM Horton, RM Perkins, T Bomblies, A AF Guilbert, Justin Beckage, Brian Winter, Jonathan M. Horton, Radley M. Perkins, Timothy Bomblies, Arne TI Impacts of Projected Climate Change over the Lake Champlain Basin in Vermont SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID FOREST ECOSYSTEMS; MODEL PROJECTIONS; PRECIPITATION; TEMPERATURE; HUMIDITY; DATABASE; UTILITY; TRENDS; ICE AB The Lake Champlain basin is a critical ecological and socioeconomic resource of the northeastern United States and southern Quebec, Canada. While general circulation models (GCMs) provide an overview of climate change in the region, they lack the spatial and temporal resolution necessary to fully anticipate the effects of rising global temperatures associated with increasing greenhouse gas concentrations. Observed trends in precipitation and temperature were assessed across the Lake Champlain basin to bridge the gap between global climate change and local impacts. Future shifts in precipitation and temperature were evaluated as well as derived indices, including maple syrup production, days above 32.2 degrees C (90 degrees F), and snowfall, relevant to managing the natural and human environments in the region. Four statistically downscaled, bias-corrected GCM simulations were evaluated from the Coupled Model Intercomparison Project phase 5 (CMIP5) forced by two representative concentration pathways (RCPs) to sample the uncertainty in future climate simulations. Precipitation is projected to increase by between 9.1 and 12.8 mm yr(-1) decade(-1) during the twenty-first century while daily temperatures are projected to increase between 0.43 degrees and 0.49 degrees C decade(-1). Annual snowfall at six major ski resorts in the region is projected to decrease between 46.9% and 52.4% by the late twenty-first century. In the month of July, the number of days above 32.2 degrees C in Burlington, Vermont, is projected to increase by over 10 days during the twenty-first century. C1 [Guilbert, Justin; Bomblies, Arne] Univ Vermont, Sch Engn, Burlington, VT USA. [Beckage, Brian; Perkins, Timothy] Univ Vermont, Dept Plant Biol, Burlington, VT USA. [Winter, Jonathan M.; Horton, Radley M.] Columbia Univ, Earth Inst, Ctr Climate Syst Res, New York, NY USA. [Horton, Radley M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Guilbert, J (reprint author), 23 Mansfield Ave, Burlington, VT 05401 USA. EM jguilber@uvm.edu FU Vermont EPSCoR through NSF [EPS-1101317] FX This work was supported by Vermont EPSCoR through NSF Award EPS-1101317. Many thanks are given to Levi Brekke, Ed Maurer, and Tom Pruitt for their assistance with the BCCA data used in this analysis. NR 34 TC 6 Z9 6 U1 1 U2 33 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD AUG PY 2014 VL 53 IS 8 BP 1861 EP 1875 DI 10.1175/JAMC-D-13-0338.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN3TS UT WOS:000340512200001 ER PT J AU Swimmer, Y Campora, CE Mcnaughton, L Musyl, M Parga, M AF Swimmer, Y. Campora, C. Empey Mcnaughton, L. Musyl, M. Parga, M. TI Post-release mortality estimates of loggerhead sea turtles (Caretta caretta) caught in pelagic longline fisheries based on satellite data and hooking location SO AQUATIC CONSERVATION-MARINE AND FRESHWATER ECOSYSTEMS LA English DT Article DE bycatch; telemetry; post-release mortality; sea turtles ID CIRCLE HOOKS; TRACKING TURTLES; BYCATCH; MARINE; CATCH; SURVIVAL; CAPTURE; REDUCE; DEATH; OCEAN AB 1. There are few reliable estimates of post-release mortality for sea turtle species because of the many challenges and costs associated with tracking animals released at sea. In this study, the likelihood of sea turtle mortality as a result of interactions with longline fishing gear was estimated based on satellite telemetry data, such as the number of days an animal was successfully tracked, or days at liberty (DAL) and dive depth data, as well as anatomical hooking locations. 2. Pop-up satellite archival tags were deployed on 29 loggerhead sea turtles (Caretta caretta) caught by the North Pacific US-based pelagic longline fishery operating from California and Hawaii between 2002 and 2006. Loggerhead turtles were catagorized by observers as shallow-hooked (55%) if the animal was entangled in the line or the hook was in the flipper, jaw or mouth and could be removed, or deep-hooked (45%) if the hook was ingested and could not be removed. The vertical movements of turtles were used to infer potential mortalities. 3. Of the 25 tags that reported data, the DAL ranged from 3 to 243 days (mean = 68 days). The DAL was shorter (by nearly 50%) for shallow-hooked (mean = 48 days, range: 3 to 127) compared to deep-hooked turtles (mean = 94 days, range: 5 to 243), but these changes were not statistically significant (P = 0.0658). 4. Although aspects of these analyses may be considered speculative, these data provide empirical evidence to indicate that deep-hooking is not linked to shorter DAL. 5. DAL, anatomical hooking location, and gear removal were evaluated with inferences about the extent of injuries and rates of infection to estimate an overall post-release mortality rate of 28% (95% bootstrap CI: 16-52%). 6. This range of estimates is consistent with those used to shape some US fisheries management plans, suggesting that conservation goals are being achieved at the expected level and ideally striking a balance between the interests of industry and those of protected species. Copyright (C) 2013 John Wiley & Sons, Ltd. C1 [Swimmer, Y.] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. [Campora, C. Empey] Biolintec Consulting LLC, Kailua, HI USA. [Mcnaughton, L.; Musyl, M.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA. [Musyl, M.] Pelag Res Grp LLC, Honolulu, HI USA. [Parga, M.] SUBMON, Barcelona, Spain. RP Swimmer, Y (reprint author), Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. EM yonat.swimmer@noaa.gov FU University of Hawaii Pelagic Fisheries Research Program [658847]; Pacific Islands Fisheries Science Center (NOAA, US National Marine Fisheries Service) FX We thank the fisheries observers, coordinators, vessel owners and crew involved in this project. We are also grateful to C. Boggs, L. Nakamura, D. Lau and J. Sibert for extensive technical and administrative assistance. This project was funded by the University of Hawaii Pelagic Fisheries Research Program (Grant #658847) and the Pacific Islands Fisheries Science Center (NOAA, US National Marine Fisheries Service). All research was conducted in accordance with the protocols and handling guidelines set forth by the University of Hawaii Animal Care and Use Committee (IACUC Protocol #00-037-2). The views expressed herein are those of the authors and do not necessarily reflect the views of NOAA of any of its subdivisions. NR 45 TC 6 Z9 6 U1 4 U2 39 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1052-7613 EI 1099-0755 J9 AQUAT CONSERV JI Aquat. Conserv.-Mar. Freshw. Ecosyst. PD AUG PY 2014 VL 24 IS 4 BP 498 EP 510 DI 10.1002/aqc.2396 PG 13 WC Environmental Sciences; Marine & Freshwater Biology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA AN0BR UT WOS:000340247200005 ER PT J AU Olsen, JL Coyer, JA Chesney, B AF Olsen, Jeanine L. Coyer, James A. Chesney, Bryant TI Numerous mitigation transplants of the eelgrass Zostera marina in southern California shuffle genetic diversity and may promote hybridization with Zostera pacifica SO BIOLOGICAL CONSERVATION LA English DT Article DE Admixture; Diversity; Genetics; Hybridization; Management; Transplants ID COASTAL BAY SYSTEM; GENOTYPIC DIVERSITY; POPULATION-STRUCTURE; MICROSATELLITE LOCI; CLONAL ORGANISMS; F-STATISTICS; RECOVERY; DISTANCE; DISTURBANCE; DOMINANCE AB Intensive human pressures along the southern California coast have led to >50 mitigation transplants of eelgrass over the past 30 years. We analyzed diversity and population structure of Zostera marina and Zostera pacifica at 36 locations to identify potential management units and further develop transplant guidelines. Normalized allelic diversity of Z. marina was uniformly moderate to high (4.78; 3.48-6.44) and nearly twofold higher than mainland Z. pacifica (2.70; 1.74-4.89). More than half of the Z. marina populations exhibited strongly significant inbreeding coefficients coupled with strong linkage disequilibrium attributable to transplant effects; neither attribute was found in Z. pacifica. Both species were characterized by high genotypic diversity and an absence of large clones. A Bayesian analysis of population structure suggested 6 potential management units for Z. marina and 3 for Z. pacifica; some units included disjunct locations associated with transplants. Hybridization between Z. marina and Z. pacifica Was documented at Newport Bay Entrance Channel and south San Diego Bay. The presence of two species requires management plans for each, as well as avoidance of potential transplant-induced hybridization. Although transplant admixtures elevate diversity, shuffling among locations may potentially reduce the genetic potential necessary to ensure rapid adaptation, even though overall transplant success has been successful. Given that transplants will continue (from both plants and seeds), we recommend that the current requirement for "two additional distinct donor sites" be restricted to within a management unit for small, routine mitigations and expanded to among-management units for wholesale de novo restorations. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Olsen, Jeanine L.] Univ Groningen, Ctr Ecol & Evolutionary Studies, Marine Benth Ecol & Evolut Grp, NL-9700 CC Groningen, Netherlands. [Coyer, James A.] Cornell Univ, Shoals Marine Lab, Portsmouth, NH 03801 USA. [Chesney, Bryant] Natl Marine Fisheries Serv, NOAA, Habitat Conservat Div, Long Beach, CA 90802 USA. RP Olsen, JL (reprint author), Univ Groningen, Ctr Ecol & Evolutionary Studies, Marine Benth Ecol & Evolut Grp, Postbus 11103,Nijenborgh 7, NL-9700 CC Groningen, Netherlands. EM j.l.olsen@rug.nl FU NOAA - USA via Western Regional Acquisition Division, Southwest Region, NMFS, Long Beach, CA [NFFR5400-11-04308] FX We thank Adam Obaza, Eric Chavez and the Santa Barbara Channelkeeper for the California collections: and Lydia Ladah for the Mexican collections. We also thank Jan Veldsink for technical assistance in the laboratory and Per Palsboll for discussions about linkage disequilibrium. This work was supported by NOAA - USA Grant (NFFR5400-11-04308) to JLO via the Western Regional Acquisition Division, Southwest Region, NMFS, Long Beach, CA. The views expressed herein do not necessarily reflect the view of those organizations. NR 80 TC 6 Z9 6 U1 3 U2 36 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD AUG PY 2014 VL 176 BP 133 EP 143 DI 10.1016/j.biocon.2014.05.001 PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AM9TI UT WOS:000340223500015 ER PT J AU Fletcher, JM Teran, OJ Rockwell, TK Oskin, ME Hudnut, KW Mueller, KJ Spelz, RM Akciz, SO Masana, E Faneros, G Fielding, EJ Leprince, S Morelan, AE Stock, J Lynch, DK Elliott, AJ Gold, P Liu-Zeng, J Gonzalez-Ortega, A Hinojosa-Corona, A Gonzalez-Garcia, J AF Fletcher, John M. Teran, Orlando J. Rockwell, Thomas K. Oskin, Michael E. Hudnut, Kenneth W. Mueller, Karl J. Spelz, Ronald M. Akciz, Sinan O. Masana, Eulalia Faneros, Geoff Fielding, Eric J. Leprince, Sebastien Morelan, Alexander E. Stock, Joann Lynch, David K. Elliott, Austin J. Gold, Peter Liu-Zeng, Jing Gonzalez-Ortega, Alejandro Hinojosa-Corona, Alejandro Gonzalez-Garcia, Javier TI Assembly of a large earthquake from a complex fault system: Surface rupture kinematics of the 4 April 2010 El Mayor-Cucapah (Mexico) M-w 7.2 earthquake SO GEOSPHERE LA English DT Article ID SAN-ANDREAS FAULT; GULF-OF-CALIFORNIA; AMERICA PLATE BOUNDARY; LAGUNA-SALADA FAULT; ANGLE NORMAL-FAULT; SOUTHERN-CALIFORNIA; BAJA-CALIFORNIA; SHEAR ZONE; EASTERN CALIFORNIA; DIPPING FAULTS AB The 4 April 2010 moment magnitude (M-w) 7.2 El Mayor-Cucapah earthquake revealed the existence of a previously unidentified fault system in Mexico that extends similar to 120 km from the northern tip of the Gulf of California to the U.S.-Mexico border. The system strikes northwest and is composed of at least seven major faults linked by numerous smaller faults, making this one of the most complex surface ruptures ever documented along the Pacific-North America plate boundary. Rupture propagated bilaterally through three distinct kinematic and geomorphic domains. Southeast of the epicenter, a broad region of distributed fracturing, liquefaction, and discontinuous fault rupture was controlled by a buried, southwest-dipping, dextral-normal fault system that extends similar to 53 km across the southern Colorado River delta. Northwest of the epicenter, the sense of vertical slip reverses as rupture propagated through multiple strands of an imbricate stack of east-dipping dextral-normal faults that extend similar to 55 km through the Sierra Cucapah. However, some coseismic slip (10-30 cm) was partitioned onto the west-dipping Laguna Salada fault, which extends parallel to the main rupture and defines the western margin of the Sierra Cucapah. In the northernmost domain, rupture terminates on a series of several north-northeast-striking cross-faults with minor offset (<8 cm) that cut uplifted and folded sediments of the northern Colorado River delta in the Yuha Desert. In the Sierra Cucapah, primary rupture occurred on four major faults separated by one fault branch and two accommodation zones. The accommodation zones are distributed in a left-stepping en echelon geometry, such that rupture passed systematically to structurally lower faults. The structurally lowest fault that ruptured in this event is inclined as shallowly as similar to 20. Net surface offsets in the Sierra Cucapah average similar to 200 cm, with some reaching 300-400 cm, and rupture kinematics vary greatly along strike. Nonetheless, instantaneous extension directions are consistently oriented similar to 085 and the dominant slip direction is similar to 310, which is slightly (similar to 10) more westerly than the expected azimuth of relative plate motion, but considerably more oblique to other nearby historical ruptures such as the 1992 Landers earthquake. Complex multifault ruptures are common in the central portion of the Pacific North American plate margin, which is affected by restraining bend tectonics, gravitational potential energy gradients, and the inherently three-dimensional strain of the transtensional and transpressional shear regimes that operate in this region. C1 [Fletcher, John M.; Teran, Orlando J.; Gonzalez-Ortega, Alejandro; Hinojosa-Corona, Alejandro; Gonzalez-Garcia, Javier] Ctr Inves Cient & Educ Super Ensenada, Dept Geol, Ensenada 22860, Baja California, Mexico. [Rockwell, Thomas K.; Faneros, Geoff] San Diego State Univ, Dept Geol Sci, San Diego, CA 92182 USA. [Oskin, Michael E.; Morelan, Alexander E.; Elliott, Austin J.; Gold, Peter] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Hudnut, Kenneth W.; Lynch, David K.] US Geol Survey, Pasadena, CA 91106 USA. [Mueller, Karl J.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Spelz, Ronald M.] Univ Autonoma Baja California, Fac Ciencias Marinas, Ensenada 22860, Baja California, Mexico. [Akciz, Sinan O.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. [Masana, Eulalia] Univ Barcelona, Dept Geodinam & Geofis, E-08028 Barcelona, Spain. [Fielding, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Leprince, Sebastien; Stock, Joann] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Liu-Zeng, Jing] China Earthquake Adm, Inst Geol, State Key Lab Earthquake Dynam, Beijing 100029, Peoples R China. RP Fletcher, JM (reprint author), Ctr Inves Cient & Educ Super Ensenada, Dept Geol, Carretera Tijuana Ensenada,3918 Zona Playitas, Ensenada 22860, Baja California, Mexico. EM jfletche@cicese.mx RI Masana, Eulalia/I-2122-2015; Hudnut, Kenneth/B-1945-2009; Liu-Zeng, Jing/F-8582-2011; Hinojosa-Corona, Alejandro/L-5422-2015; OI Masana, Eulalia/0000-0001-8315-7561; Hudnut, Kenneth/0000-0002-3168-4797; Hinojosa-Corona, Alejandro/0000-0002-2282-337X; Rockwell, Thomas/0000-0001-5319-6447; Stock, Joann Miriam/0000-0003-4816-7865 FU CONACYT (Consejo Nacional de Ciencia y Tecnologia) [81463]; SCEC (Southern California Earthquake Center) [1697]; National Science Foundation [EAR-0529922]; GEER (Geotechnical Extreme Events Reconnaissance) Foundation; Keck Institute for Space Studies; Gordon and Betty Moore Foundation; National Aeronautics and Space Administration (NASA) Earth Surface and Interior focus area; NASA FX This work was financed by CONACYT (Consejo Nacional de Ciencia y Tecnologia) grant 81463, SCEC (Southern California Earthquake Center) grant 1697, and National Science Foundation grant EAR-0529922; the GEER (Geotechnical Extreme Events Reconnaissance) Foundation provided funding for initial field work. S. Leprince was supported in part by the Keck Institute for Space Studies and by the Gordon and Betty Moore Foundation. Part of this study was sponsored by the National Aeronautics and Space Administration (NASA) Earth Surface and Interior focus area and performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Enlightening discussions with Paul Wetmore and Francisco Suarez helped refine ideas about tectonics of the Big Bend domain and the kinematics of faulting in the Colorado River delta, respectively. We thank John Galetzka, Kate Scharer, David Bowman, Roman Manjarrez, and Maria Oturno for help with field work. We also thank Jose Mojarro, Sergio Arregui, and Luis Gradilla for technical support. NR 82 TC 21 Z9 21 U1 2 U2 27 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 1553-040X J9 GEOSPHERE JI Geosphere PD AUG PY 2014 VL 10 IS 4 BP 797 EP 827 DI 10.1130/GES00933.1 PG 31 WC Geosciences, Multidisciplinary SC Geology GA AM6GK UT WOS:000339961500010 ER PT J AU Murri, GB AF Murri, Gretchen B. TI Effect of data reduction and fiber-bridging on Mode I delamination characterization of unidirectional composites SO JOURNAL OF COMPOSITE MATERIALS LA English DT Article DE Composites; fracture toughness; fatigue; Paris Law; delamination; strain energy release rate; R-curve AB Reliable delamination characterization data for laminated composites are needed for input in analytical models of structures to predict delamination onset and growth. The double-cantilevered beam specimen is used to measure fracture toughness, G(Ic), and strain energy release rate, G(Imax), for delamination onset and growth in laminated composites under Mode I loading. The current study was conducted as part of an ASTM Round Robin activity to evaluate a proposed testing standard for Mode I fatigue delamination propagation. Static and fatigue tests were conducted on specimens of IM7/977-3 and G40-800/5276-1 graphite/epoxies, and S2/5216 glass/epoxy double-cantilevered beam specimens to evaluate the draft standard "Standard Test Method for Mode I Fatigue Delamination Propagation of Unidirectional Fiber-Reinforced Polymer Matrix Composites." Static results were used to generate a delamination resistance curve, G(IR), for each material, which was used to determine the effects of fiber-bridging on the delamination growth data. All three materials were tested in fatigue at a cyclic G(Imax) level equal to 90% of the fracture toughness, G(Ic), to determine the delamination growth rate. Two different data reduction methods, a two-point and a seven-point fit, were used and the resulting Paris Law equations were compared. Growth rate results were normalized by the delamination resistance curve for each material and compared to the non-normalized results. Paris Law exponents were found to decrease by 5.7 to 47.6% due to normalizing the growth data. Additional specimens of the IM7/977-3 material were tested at three lower cyclic G(Imax) levels to compare the effect of loading level on delamination growth rates. The IM7/977-3 tests were also used to determine the delamination threshold curve for that material. The results show that tests at a range of loading levels are necessary to describe the complete delamination behavior of this material. C1 NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Murri, GB (reprint author), NASA Langley Res Ctr, 2W Reid St,MS188E, Hampton, VA 23681 USA. EM gretchen.b.murri@nasa.gov NR 11 TC 7 Z9 7 U1 3 U2 12 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0021-9983 EI 1530-793X J9 J COMPOS MATER JI J. Compos Mater. PD AUG PY 2014 VL 48 IS 19 BP 2413 EP 2424 DI 10.1177/0021998313498791 PG 12 WC Materials Science, Composites SC Materials Science GA AM9MZ UT WOS:000340207000010 ER PT J AU Porcar-Castell, A Tyystjarvi, E Atherton, J van der Tol, C Flexas, J Pfundel, EE Moreno, J Frankenberg, C Berry, JA AF Porcar-Castell, Albert Tyystjarvi, Esa Atherton, Jon van der Tol, Christiaan Flexas, Jaume Pfuendel, Erhard E. Moreno, Jose Frankenberg, Christian Berry, Joseph A. TI Linking chlorophyll a fluorescence to photosynthesis for remote sensing applications: mechanisms and challenges SO JOURNAL OF EXPERIMENTAL BOTANY LA English DT Review DE Gross primary production; GPP; leaf level; photosystem II; photosystem I; PSII; PSI; photosynthesis dynamics; pulse amplitude modulation; PAM; PSII connectivity; remote sensing; solar-induced fluorescence; sun-induced fluorescence; SIF ID THERMAL-ENERGY DISSIPATION; LIGHT-USE EFFICIENCY; PHOTOCHEMICAL REFLECTANCE INDEX; PIGMENT-PROTEIN COMPLEXES; PINUS-SYLVESTRIS L.; THYLAKOID MEMBRANE ORGANIZATION; PHOTOSYSTEM-II FLUORESCENCE; ADJUSTED VEGETATION INDEX; GROSS PRIMARY PRODUCTION; CARBON-DIOXIDE UPTAKE AB Chlorophyll a fluorescence (ChlF) has been used for decades to study the organization, functioning, and physiology of photosynthesis at the leaf and subcellular levels. ChlF is now measurable from remote sensing platforms. This provides a new optical means to track photosynthesis and gross primary productivity of terrestrial ecosystems. Importantly, the spatiotemporal and methodological context of the new applications is dramatically different compared with most of the available ChlF literature, which raises a number of important considerations. Although we have a good mechanistic understanding of the processes that control the ChlF signal over the short term, the seasonal link between ChlF and photosynthesis remains obscure. Additionally, while the current understanding of in vivo ChlF is based on pulse amplitude-modulated (PAM) measurements, remote sensing applications are based on the measurement of the passive solar-induced chlorophyll fluorescence (SIF), which entails important differences and new challenges that remain to be solved. In this review we introduce and revisit the physical, physiological, and methodological factors that control the leaf-level ChlF signal in the context of the new remote sensing applications. Specifically, we present the basis of photosynthetic acclimation and its optical signals, we introduce the physical and physiological basis of ChlF from the molecular to the leaf level and beyond, and we introduce and compare PAM and SIF methodology. Finally, we evaluate and identify the challenges that still remain to be answered in order to consolidate our mechanistic understanding of the remotely sensed SIF signal. C1 [Porcar-Castell, Albert; Atherton, Jon] Univ Helsinki, Dept Forest Sci, FIN-00014 Helsinki, Finland. [Tyystjarvi, Esa] Univ Turku, Dept Biochem, FI-20014 Turku, Finland. [van der Tol, Christiaan] Univ Twente, Fac ITC, NL-7524 AE Enschede, Netherlands. [Flexas, Jaume] Univ Illes Balears, Palma De Mallorca 07122, Spain. [Pfuendel, Erhard E.] Heinz Walz GmbH, D-91090 Effeltrich, Germany. [Moreno, Jose] Univ Valencia, Fac Phys, Dept Earth Phys & Thermodynam, E-46100 Valencia, Spain. [Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Berry, Joseph A.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. RP Porcar-Castell, A (reprint author), Univ Helsinki, Dept Forest Sci, POB 27, FIN-00014 Helsinki, Finland. EM joan.porcar@helsinki.fi RI Flexas, Jaume/C-1898-2012; Tyystjarvi, Esa/B-2360-2015; van der Tol, Christiaan/A-2403-2010; Frankenberg, Christian/A-2944-2013; OI Tyystjarvi, Esa/0000-0001-6808-7470; van der Tol, Christiaan/0000-0002-2484-8191; Frankenberg, Christian/0000-0002-0546-5857; Porcar-Castell, Albert/0000-0003-1357-9982 FU Academy of Finland [1138884, 272041, 259075]; University of Helsinki [490116] FX This work has been supported by the Academy of Finland [grant nos 1138884 and 272041 to AP-C and 259075 to ET], and the University of Helsinki (grant no 490116). This review idea originated from discussions during a Workshop organized by the Keck Institute for Space Studies 'New Methods for Measurements of Photosynthesis from Space'. The availability of results from ongoing preparatory studies for the ESA FLEX mission is acknowledged. We thank Professor Kari Heliovaara for help in preparing Figs 2, 4, and 7. NR 270 TC 64 Z9 65 U1 30 U2 207 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-0957 EI 1460-2431 J9 J EXP BOT JI J. Exp. Bot. PD AUG PY 2014 VL 65 IS 15 BP 4065 EP 4095 DI 10.1093/jxb/eru191 PG 31 WC Plant Sciences SC Plant Sciences GA AM6EB UT WOS:000339954300001 PM 24868038 ER PT J AU di Lauro, C Lattanzi, F Brown, LR Soon, K Mantz, AW Smith, MAH AF di Lauro, Carlo Lattanzi, Franca Brown, Linda R. Soon, Keeyoon Mantz, Arlan W. Smith, Mary Ann H. TI The V-4, V-9, V-10 and V-6+V-11 bands of (CH3CH3)-C-12-C-13 between 1345 and 1557 cm(-1) SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE Line positions; Intensities; (CH3CH3)-C-12-C-13; Cold temperature; Coriolis coupling; Torsional splitting; K-doubling ID STIMULATED RAMAN-SPECTRUM; INTERNAL-ROTATION; LINE PARAMETERS; MU-M; ETHANE; C2H6; (C2H6)-C-12; MOLECULE; REGION; TITAN AB The infrared spectrum of (CH3CH3)-C-12-C-13 is measured between 1345 and 1560 cm(-1) using high resolution FTIR with a C-13-enriched gas sample cooled to 130.3 K. The three fundamentals v(4), v(9) and v(10) (at 1374, 1470 and 1468 cm-1 respectively) and one combination band v(6) + v(11) at 1473 cm-1 are analyzed for the first time. The transitions of v10 (an infrared inactive "g" mode of the ethane) are observed through its resonant coupling with v9 (corresponding to a "u" mode of normal ethane). Transitions of v(6) + v(11) are seen due to its strong coupling to v9. In general, torsional splitting produces two components (as in normal ethane), but in both v9 and v50, there is an additional small splitting of these components with degenerate torsional symmetry wherever the interacting v(10) levels become infrared active (from "g 4-* u" mixing); this mechanism is investigated. Several e-type resonances with AE = 2 and Ak = +1 are observed within v9 and between v(9) and v(10) while the strong interaction between v(9) and v(6) + v(11) plays a role in tuning pairs of levels into resonance. As in normal ethane, a detectable K-doubling occurs in the levels k= 2, e = 1 of v(9), and the parallel band v4 shows an intensity bias, with the R-transitions markedly stronger than the P-transitions, due to its x,y-Coriolis coupling with v9. The spectrum is analyzed by adopting an appropriate Hamiltonian model, and vibration-rotation-torsion parameters of the four mentioned vibrational states are determined by the least squares process using 1350 observed transition line positions (RMS deviation 3.24 x 10-3 cm-I). The values of rotational and torsional parameters of the vibrational ground state are also improved or determined anew, from data of the present spectrum. Two supplemental files are provided. One shows the fit of line positions, and the other gives the measured positions and intensities at 130 K (with known quantum assignments and lower state energies) so that lines of this molecule can be identified in planetary spectra. (C) 2014 Elsevier Inc. All rights reserved. C1 [di Lauro, Carlo; Lattanzi, Franca] Univ Naples Federico II, I-80131 Naples, Italy. [Brown, Linda R.; Soon, Keeyoon] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mantz, Arlan W.] Connecticut Coll, Dept Phys Astron & Geophys, New London, CT 06320 USA. [Smith, Mary Ann H.] NASA Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. RP Brown, LR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM linda.r.brown@jpl.nasa.gov RI Sung, Keeyoon/I-6533-2015 NR 34 TC 2 Z9 2 U1 1 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 EI 1096-083X J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD AUG PY 2014 VL 302 BP 36 EP 49 DI 10.1016/j.jms.2014.06.001 PG 14 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA AM7CF UT WOS:000340021600006 ER PT J AU Kim, JH Chun, HY Sharman, RD Trier, SB AF Kim, Jung-Hoon Chun, Hye-Yeong Sharman, Robert D. Trier, Stanley B. TI The Role of Vertical Shear on Aviation Turbulence within Cirrus Bands of a Simulated Western Pacific Cyclone SO MONTHLY WEATHER REVIEW LA English DT Article ID CLEAR-AIR TURBULENCE; MESOSCALE CONVECTIVE SYSTEM; UPPER-LEVEL OUTFLOW; CLOUD BANDS; MODEL; ENVIRONMENT; WEATHER; MECHANISMS AB At 0300 UTC 9 September 2010, commercial aircraft traveling between Tokyo and Hawaii encountered regions of moderate and severe intensity turbulence at about 12-km elevation in or just above banded structures in the cirrus anvil associated with an oceanic cyclone located off the east coast of Japan. The generation mechanisms of the cirrus bands and turbulence are investigated using the Advanced Research Weather Research and Forecasting Model with five nested domains having a finest horizontal grid spacing of 370 m. The simulation reproduces the satellite-observed patterns of cloud brightness, including the bands, and suggests that synoptic-scale vertical shear within the anvil cloud layer and radiative effects, including long-wave cooling at cloud top and warming at cloud base, act together to produce banded structures within the southern edge of the cirrus cloud shield. The character of the bands within the nearly neutral or convectively unstable layer of the cirrus shield is similar to boundary layer rolls in that the vertical wind shear vectors are nearly parallel to the cirrus bands. The strong vertical shear aligned with the banded convection leads to flow deformations and mixing near the cloud top, resulting in localized moderate and severe turbulence. The estimated maximum value of the cube root of eddy dissipation rate within the bands is similar to 0.7 m(2/3) s(-1), consistent with severe turbulence levels experienced by large aircraft. C1 [Kim, Jung-Hoon] Oak Ridge Associated Univ, NASA, Ames Res Ctr, Moffett Field, CA USA. [Kim, Jung-Hoon; Chun, Hye-Yeong] Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea. [Sharman, Robert D.; Trier, Stanley B.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Kim, JH (reprint author), NASA, Aviat Syst Div, Ames Res Ctr, Mail Code 210-10, Moffett Field, CA 94035 USA. EM jung-hoon.kim@nasa.gov FU Korean Meteorological Administration Research and Development Program [CATER_2012-2011]; NOAA [NA-09NWS4670001]; Federal Aviation Administration (FAA) Aviation Weather Research Program FX This work was supported by the Korean Meteorological Administration Research and Development Program under Grant CATER_2012-2011 (HYC and JHK), NOAA Grant NA-09NWS4670001, and by the Federal Aviation Administration (FAA) Aviation Weather Research Program (RDS and SBT). The views expressed are those of the authors and do not necessarily represent the official policy or position of the FAA. The authors thank Melissa Thomas (Delta Air Lines) for a helpful review of a previous version of the manuscript and for informative discussions concerning real-time observations of the relation of cirrus bands to aviation turbulence. The authors also appreciate the informative comments from two anonymous reviewers, which helped clarify aspects of the paper. NR 44 TC 5 Z9 5 U1 3 U2 6 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 AUG PY 2014 VL 142 IS 8 BP 2794 EP 2813 DI 10.1175/MWR-D-14-00008.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AM6YZ UT WOS:000340013200013 ER PT J AU Gregg, WW Casey, NW Rousseaux, CS AF Gregg, Watson W. Casey, Nancy W. Rousseaux, Cecile S. TI Sensitivity of simulated global ocean carbon flux estimates to forcing by reanalysis products SO OCEAN MODELLING LA English DT Article DE Reanalysis; Ocean; Carbon; Fluxes; Models ID ANTHROPOGENIC CARBON; GAS-EXCHANGE; WIND-SPEED; SYSTEM; MODEL; VARIABILITY; PACIFIC; DUST AB Reanalysis products from MERRA, NCEP2, NCEPI, and ECMWF were used to force an established ocean biogeochemical model to estimate air-sea carbon fluxes (FCO2) and partial pressure of carbon dioxide (pCO(2)) in the global oceans. Global air-sea carbon fluxes and pCO(2) were relatively insensitive to the choice of forcing reanalysis. All global FCO2 estimates from the model forced by the four different reanalyses were within 20% of in situ estimates (MERRA and NCEP1 were within 7%), and all models exhibited statistically significant positive correlations with in situ estimates across the 12 major oceanographic basins. Global pCO(2) estimates were within 1% of in situ estimates with ECMWF being the outlier at 0.6%. Basin correlations were similar to FCO2. There were, however, substantial departures among basin estimates from the different reanalysis forcings. The high latitudes and tropics had the largest ranges in estimated fluxes among the reanalyses. Regional pCO(2) differences among the reanalysis forcings were muted relative to the FCO2 results. No individual reanalysis was uniformly better or worse in the major oceanographic basins. The results provide information on the characterization of uncertainty in ocean carbon models due to choice of reanalysis forcing. Published by Elsevier Ltd. This is an open access article under the CC BY license (http://creativecommon-s.org/licenses/by/3.0/). C1 [Gregg, Watson W.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Casey, Nancy W.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Rousseaux, Cecile S.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. RP Gregg, WW (reprint author), NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM watson.gregg@nasa.gov; nancy.casey@ssaihq.com; cecile.s.rousseaux@nasa.gov RI Rousseaux, Cecile/E-8811-2012 OI Rousseaux, Cecile/0000-0002-3022-2988 FU NASA FX We thank the NASA/MERRA Project, the NOAA/NCEP Project and the ECMWF Project for the data sets and public availability. We also thank the Lamont-Doherty Earth Observatory for in situ pCO2 data and flux estimates. We thank three anonymous reviewers for insights. This work was supported by NASA Modeling and Analysis Program (MAP) and Carbon Monitoring System (CMS) Programs. NR 24 TC 2 Z9 2 U1 0 U2 7 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1463-5003 EI 1463-5011 J9 OCEAN MODEL JI Ocean Model. PD AUG PY 2014 VL 80 BP 24 EP 35 DI 10.1016/j.ocemod.2014.05.002 PG 12 WC Meteorology & Atmospheric Sciences; Oceanography SC Meteorology & Atmospheric Sciences; Oceanography GA AN0YQ UT WOS:000340310300003 ER PT J AU Elham, A van Tooren, MJL Sobieszczanski-Sobieski, J AF Elham, Ali van Tooren, Michel J. L. Sobieszczanski-Sobieski, Jaroslaw TI Bilevel Optimization Strategy for Aircraft Wing Design Using Parallel Computing SO AIAA JOURNAL LA English DT Article ID SHAPE AB A new bilevel optimization strategy for wing design is developed, in which the optimizations of the wing-planform and wing-airfoil shapes are decoupled from each other. The design of the wing-planform shape and the shape of the airfoils in several spanwise positions are considered as the goal of the optimization. In the new approach, the design problem is decomposed into a series of subproblems based on the design variables. The design variables defining the wing-planform shape are optimized in a top-level optimization, and the design variables defining the shape of airfoils in several spanwise positions are optimized in several sublevel optimizations. To take into account the influence of the airfoil shape in a specific spanwise position on the shape of the airfoils in other spanwise positions, a series of design variables are added to the design vector of the top-level optimization. The top-level optimizer is responsible for the consistency of the optimization. Using this approach, the number of design variables in the top-level optimization is reduced; the airfoils in several spanwise positions are optimized in parallel; and, instead of complex three-dimensional aerodynamic and structural solvers, much simpler and faster two-dimensional airfoil analysis tools can be used. C1 [Elham, Ali] Delft Univ Technol, Fac Aerosp Engn, NL-2629 HS Delft, Netherlands. [van Tooren, Michel J. L.] Univ S Carolina, Ronald E McNair Ctr Aerosp Innovat & Res, Columbia, SC 29201 USA. [Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23601 USA. RP Elham, A (reprint author), Delft Univ Technol, Fac Aerosp Engn, Kluyverweg 1, NL-2629 HS Delft, Netherlands. EM A.Elham@tudelft.nl; vantooren@cec.se.edu; ysobieskiy@gmail.com NR 49 TC 2 Z9 2 U1 0 U2 9 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD AUG PY 2014 VL 52 IS 8 BP 1770 EP 1783 DI 10.2514/1.J052696 PG 14 WC Engineering, Aerospace SC Engineering GA AM1XG UT WOS:000339642000015 ER PT J AU Horvath, C Envia, E Podboy, GG AF Horvath, Csaba Envia, Edmane Podboy, Gary G. TI Limitations of Phased Array Beamforming in Open Rotor Noise Source Imaging SO AIAA JOURNAL LA English DT Article C1 [Horvath, Csaba; Envia, Edmane; Podboy, Gary G.] NASA John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. RP Horvath, C (reprint author), Budapest Univ Technol & Econ, Budapest, Hungary. EM horvath@ara.bme.hu FU Environmentally Responsible Aviation Project of the NASA Integrated Systems Research Program; Fixed Wing Project of the NASA Fundamental Aeronautics Program; Hungarian Fund for Science and Research [K 83807]; relates to the scientific program of the projects "Development of quality-oriented and harmonized R + D + 1 strategy and the functional model at BME" [TAMOP-4.2.1/B-09/1/KMR-2010-0002]; "Talent care and cultivation in the scientific workshops of BME" [TAMOP-4.2.2/B-10/1-2010-0009] FX This testing and research was funded by the Environmentally Responsible Aviation Project of the NASA Integrated Systems Research Program and the Fixed Wing Project of the NASA Fundamental Aeronautics Program. A portion of the study and the publication of the work was supported by the Hungarian Fund for Science and Research under Contract No. K 83807 and relates to the scientific program of the projects "Development of quality-oriented and harmonized R + D + 1 strategy and the functional model at BME" and "Talent care and cultivation in the scientific workshops of BME" under Grants No. TAMOP-4.2.1/B-09/1/KMR-2010-0002 and No. TAMOP-4.2.2/B-10/1-2010-0009, respectively. NR 16 TC 9 Z9 9 U1 1 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD AUG PY 2014 VL 52 IS 8 BP 1810 EP 1817 DI 10.2514/1.J052952 PG 8 WC Engineering, Aerospace SC Engineering GA AM1XG UT WOS:000339642000021 ER PT J AU Borkowski, KJ Reynolds, SP Green, DA Hwang, U Petre, R Krishnamurthy, K Willett, R AF Borkowski, Kazimierz J. Reynolds, Stephen P. Green, David A. Hwang, Una Petre, Robert Krishnamurthy, Kalyani Willett, Rebecca TI NONUNIFORM EXPANSION OF THE YOUNGEST GALACTIC SUPERNOVA REMNANT G1.9+0.3 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (G1.9+0.3); ISM: supernova remnants; X-rays: ISM ID HIGH-VELOCITY FEATURES; IA SUPERNOVAE; EXPLOSION MECHANISM; MODELS; EJECTA; CONSTRAINTS AB We report measurements of the X-ray expansion of the youngest Galactic supernova remnant, G1.9+0.3, using Chandra observations in 2007, 2009, and 2011. The measured rates strongly deviate from uniform expansion, decreasing radially by about 60% along the X-ray bright SE-NW axis from 0.84% +/- 0.06% yr(-1) to 0.52% +/- 0.03% yr(-1). This corresponds to undecelerated ages of 120-190 yr, confirming the young age of G1.9+0.3 and implying a significant deceleration of the blast wave. The synchrotron-dominated X-ray emission brightens at a rate of 1.9% +/- 0.4% yr(-1). We identify bright outer and inner rims with the blast wave and reverse shock, respectively. Sharp density gradients in either the ejecta or ambient medium are required to produce the sudden deceleration of the reverse shock or the blast wave implied by the large spread in expansion ages. The blast wave could have been decelerated recently by an encounter with a modest density discontinuity in the ambient medium, such as may be found at a wind termination shock, requiring strong mass loss in the progenitor. Alternatively, the reverse shock might have encountered an order-of-magnitude density discontinuity within the ejecta, such as may be found in pulsating delayed-detonation Type Ia models. We demonstrate that the blast wave is much more decelerated than the reverse shock in these models for remnants at ages similar to G1.9+0.3. Similar effects may also be produced by dense shells possibly associated with high-velocity features in Type Ia spectra. Accounting for the asymmetry of G1.9+0.3 will require more realistic three-dimensional Type Ia models. C1 [Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Green, David A.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Hwang, Una] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krishnamurthy, Kalyani] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA. [Willett, Rebecca] Univ Wisconsin, Dept Elect & Comp Engn, Madison, WI 53706 USA. RP Borkowski, KJ (reprint author), N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. EM kborkow@unity.ncsu.edu RI Green, David/E-9609-2010; OI Green, David/0000-0003-3189-9998; Willett, Rebecca/0000-0002-8109-7582 FU NASA through Chandra General Observer Program [SAO G01-12098A, SAO G01-12098B] FX This work was supported by NASA through Chandra General Observer Program grants SAO G01-12098A and B. NR 24 TC 4 Z9 4 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 1 PY 2014 VL 790 IS 2 AR L18 DI 10.1088/2041-8205/790/2/L18 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5KO UT WOS:000339897100004 ER PT J AU Piro, L Troja, E Gendre, B Ghisellini, G Ricci, R Bannister, K Fiore, F Kidd, LA Piranomonte, S Wieringa, MH AF Piro, Luigi Troja, Eleonora Gendre, Bruce Ghisellini, Gabriele Ricci, Roberto Bannister, Keith Fiore, Fabrizio Kidd, Lauren A. Piranomonte, Silvia Wieringa, Mark H. TI A HOT COCOON IN THE ULTRALONG GRB 130925A: HINTS OF A POPIII-LIKE PROGENITOR IN A LOW-DENSITY WIND ENVIRONMENT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma-ray burst: individual (GRB130925A); stars: Population III ID GAMMA-RAY BURSTS; POPULATION-III STARS; MASSIVE STARS; 1ST STARS; SWIFT; JETS; AFTERGLOWS; SUPERNOVA; EMISSION; CONNECTION AB GRB 130925A is a peculiar event characterized by an extremely long gamma-ray duration (approximate to 7 ks), as well as dramatic flaring in the X-rays for approximate to 20 ks. After this period, its X-ray afterglow shows an atypical soft spectrum with photon index Gamma similar to 4, as observed by Swift and Chandra, until approximate to 10(7) s, when XMM-Newton observations uncover a harder spectral shape with Gamma similar to 2.5, commonly observed in gamma-ray burst (GRB) afterglows. We find that two distinct emission components are needed to explain the X-ray observations: a thermal component, which dominates the X-ray emission for several weeks, and a non-thermal component, consistent with a typical afterglow. A forward shock model well describes the broadband (from radio to X-rays) afterglow spectrum at various epochs. It requires an ambient medium with a very low-density wind profile, consistent with that expected from a low-metallicity blue supergiant (BSG). The thermal component has a remarkably constant size and a total energy consistent with those expected by a hot cocoon surrounding the relativistic jet. We argue that the features observed in this GRB (its ultralong duration, the thermal cocoon, and the low-density wind environment) are associated with a low metallicity BSG progenitor and, thus, should characterize the class of ultralong GRBs. C1 [Piro, Luigi] INAF Ist Astrofis Planetol Spaziali, I-00133 Rome, Italy. [Troja, Eleonora; Kidd, Lauren A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gendre, Bruce] ARTEMIS, UMR 7250, F-06304 Nice 4, France. [Ghisellini, Gabriele] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Ricci, Roberto] INAF Ist Radioastron, I-40129 Bologna, Italy. [Bannister, Keith] CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia. [Fiore, Fabrizio; Piranomonte, Silvia] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy. [Wieringa, Mark H.] CSIRO Astron & Space Sci, Narrabri, NSW 2390, Australia. RP Piro, L (reprint author), INAF Ist Astrofis Planetol Spaziali, Via Fosso Cavaliere 100, I-00133 Rome, Italy. OI Piranomonte, Silvia/0000-0002-8875-5453; Bannister, Keith/0000-0003-2149-0363; Ghisellini, Gabriele/0000-0002-0037-1974; Gendre, Bruce/0000-0002-9077-2025; Fiore, Fabrizio/0000-0002-4031-4157 NR 42 TC 20 Z9 20 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 1 PY 2014 VL 790 IS 2 AR L15 DI 10.1088/2041-8205/790/2/L15 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5KO UT WOS:000339897100001 ER PT J AU Tremblay, GR Gladders, MD Baum, SA O'Dea, CP Bayliss, MB Cooke, KC Dahle, H Davis, TA Florian, M Rigby, JR Sharon, K Soto, E Wuyts, E AF Tremblay, Grant R. Gladders, Michael D. Baum, Stefi A. O'Dea, Christopher P. Bayliss, Matthew B. Cooke, Kevin C. Dahle, Hakon Davis, Timothy A. Florian, Michael Rigby, Jane R. Sharon, Keren Soto, Emmaris Wuyts, Eva TI A 30 kpc CHAIN OF "BEADS ON A STRING" STAR FORMATION BETWEEN TWO MERGING EARLY TYPE GALAXIES IN THE CORE OF A STRONG-LENSING GALAXY CLUSTER SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (SDSS J1531+3414); galaxies; interactions; galaxies: star formation; gravitational lensing: strong ID COLOR-MAGNITUDE RELATIONS; GIANT ARCS; PROJECT; CONSTRAINTS; EVOLUTION; ORIGIN; SCALES; GAS; LAW AB New Hubble Space Telescope ultraviolet and optical imaging of the strong-lensing galaxy cluster SDSS J1531+3414 (z = 0.335) reveals two centrally dominant elliptical galaxies participating in an ongoing major merger. The interaction is at least somewhat rich in cool gas, as the merger is associated with a complex network of 19 massive superclusters of young stars (or small tidal dwarf galaxies) separated by similar to 1 kpc in projection from one another, combining to an estimated total star formation rate of similar to 5 M-circle dot yr(-1). The resolved young stellar superclusters are threaded by narrow Ha, [O-II], and blue excess filaments arranged in a network spanning similar to 27 kpc across the two merging galaxies. This morphology is strongly reminiscent of the well-known " beads on a string" mode of star formation observed on kiloparsecscales in the arms of spiral galaxies, resonance rings, and in tidal tails between interacting galaxies. Nevertheless, the arrangement of this star formation relative to the nuclei of the two galaxies is difficult to interpret in a dynamical sense, as no known " beads on a string" systems associated with kiloparsec-scale tidal interactions exhibit such lopsided morphology relative to the merger participants. In this Letter, we present the images and follow-up spectroscopy and discuss possible physical interpretations for the unique arrangement of the young stellar clusters. While we suggest that this morphology is likely to be dynamically short-lived, a more quantitative understanding awaits necessary multiwavelength follow-up, including optical integral field spectroscopy, ALMA submillimeter interferometry, and Chandra X-ray imaging. C1 [Tremblay, Grant R.; Davis, Timothy A.] European So Observ, D-85748 Garching, Germany. [Gladders, Michael D.; Florian, Michael] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Gladders, Michael D.; Florian, Michael] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Baum, Stefi A.; O'Dea, Christopher P.; Cooke, Kevin C.] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Baum, Stefi A.; O'Dea, Christopher P.; Cooke, Kevin C.] Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA. [Bayliss, Matthew B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dahle, Hakon] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Sharon, Keren] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Soto, Emmaris] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Wuyts, Eva] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Tremblay, GR (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM grant.tremblay@eso.org RI Rigby, Jane/D-4588-2012; OI Rigby, Jane/0000-0002-7627-6551; Davis, Timothy/0000-0003-4932-9379; Cooke, Kevin/0000-0002-2200-9845; Tremblay, Grant/0000-0002-5445-5401; Florian, Michael/0000-0001-5097-6755 FU European Community [229517]; NASA [HST-GO-13003]; Association of Universities for Research in Astronomy, Inc., under NASA [NAS5-26555]; Alfred P. Sloan Foundation; SDSS; Participating Institutions; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We thank Professors Francoise Combes, Eric Emsellem, and Tim de Zeeuw for thoughtful discussions. We also thank the anonymous referee whose feedback improved this work. G. R. T. and T. A. D. acknowledge support from a European Southern Observatory (ESO) Fellowship partially funded by the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No. 229517. Support for program number HST-GO-13003 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This Letter is based on observations by the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute. We also present results from the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. NR 35 TC 5 Z9 5 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 AUG 1 PY 2014 VL 790 IS 2 AR L26 DI 10.1088/2041-8205/790/2/L26 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5KO UT WOS:000339897100012 ER PT J AU Xiao, H Mechoso, CR Sun, RY Han, J Pan, HL Park, S Hannay, C Bretherton, C Teixeira, J AF Xiao, Heng Mechoso, C. Roberto Sun, Ruiyu Han, Jongil Pan, Hua-Lu Park, Sungsu Hannay, Cecile Bretherton, Chris Teixeira, Joao TI Diagnosis of the marine low cloud simulation in the NCAR community earth system model (CESM) and the NCEP global forecast system (GFS)-modular ocean model v4 (MOM4) coupled model SO CLIMATE DYNAMICS LA English DT Article DE Marine low clouds; Stratocumulus; Shallow cumulus; Climate modeling; CESM; GFS; Parameterization; Stratocumulus to cumulus transition ID BOUNDARY-LAYER CLOUDS; GENERAL-CIRCULATION MODELS; ATMOSPHERE MODEL; SOUTHEAST PACIFIC; SEASONAL CYCLE; PART I; CLIMATE SIMULATIONS; CUMULUS CONVECTION; VERTICAL DIFFUSION; TROPICAL PACIFIC AB We present a diagnostic analysis of the marine low cloud climatology simulated by two state-of-the-art coupled atmosphere-ocean models: the National Center for Atmospheric Research community earth system model version 1 (CESM1) and the National Center for Environmental Predictions global forecasting system-modular ocean model version 4 (GFS-MOM4) coupled model. In the CESM1, the coastal stratocumulus (Sc)-topped planetary boundary layers (PBLs) in the subtropical Eastern Pacific are well-simulated but the climatological transition from Sc to shallow cumulus (Cu) is too abrupt and occurs too close to the coast. By contrast, in the GFS-MOM4 the coastal Sc amount and PBL depth are severely underestimated while the transition from Sc to shallow Cu is "delayed" and offshore Sc cover is too extensive in the subtropical Eastern Pacific. We discuss the possible connections between these differences in the simulations and differences in the parameterizations of shallow convection and boundary layer turbulence in the two models. C1 [Xiao, Heng; Mechoso, C. Roberto] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Sun, Ruiyu; Han, Jongil; Pan, Hua-Lu] NOAA, Natl Ctr Environm Predict, Silver Spring, MD USA. [Park, Sungsu; Hannay, Cecile] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Bretherton, Chris] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Teixeira, Joao] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Xiao, H (reprint author), Pacific NW Natl Lab, Atmospher Sci & Global Change Div, POB 999, Richland, WA 99352 USA. EM Heng.Xiao@pnnl.gov FU NOAA MAPP/CPO; U.S. DOE OBER [KP/501021/58166]; US Department of Energy [DE-AC05-76RL01830]; National Science Foundation FX This work is supported by the NOAA MAPP/CPO program as part of the Sc-Cu Climate Process Team through grants to UCLA, NCAR, NCEP, UW and JPL. HX was supported by U.S. DOE OBER grant KP/501021/58166 at PNNL. We also acknowledge helpful suggestions from all four anonymous reviewers. Pacific Northwest National Laboratory is operated by Battelle Memorial Institute for the US Department of Energy under Contract No. DE-AC05-76RL01830. The National Center for Atmospheric Research is sponsored by the National Science Foundation. NR 69 TC 3 Z9 3 U1 0 U2 11 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD AUG PY 2014 VL 43 IS 3-4 BP 737 EP 752 DI 10.1007/s00382-014-2067-y PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AM5LG UT WOS:000339899500010 ER PT J AU Minson, SE Simons, M Beck, JL Ortega, F Jiang, J Owen, SE Moore, AW Inbal, A Sladen, A AF Minson, S. E. Simons, M. Beck, J. L. Ortega, F. Jiang, J. Owen, S. E. Moore, A. W. Inbal, A. Sladen, A. TI Bayesian inversion for finite fault earthquake source models - II: the 2011 great Tohoku-oki, Japan earthquake SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE Inverse theory; Probability distributions; Earthquake source observations; Computational seismology ID WAVE-FORM INVERSION; NORTHEASTERN JAPAN; STRUCTURAL CHARACTERISTICS; NORTHERN HONSHU; PACIFIC COAST; TRENCH AXIS; ARC REGION; SLIP; RUPTURE; REFLECTION AB We present a fully Bayesian inversion of kinematic rupture parameters for the 2011 M(w)9 Tohoku-oki, Japan earthquake. Albeit computationally expensive, this approach to kinematic source modelling has the advantage of producing an ensemble of slip models that are consistent with physical a priori constraints, realistic data uncertainties, and realistic but simplistic uncertainties in the physics of the kinematic forward model, all without being biased by non-physical regularization constraints. Combining 1 Hz kinematic GPS, static GPS offsets, seafloor geodesy and near-field and far-field tsunami data into a massively parallel Monte Carlo simulation, we construct an ensemble of samples of the posterior probability density function describing the evolution of fault rupture. We find that most of the slip is concentrated in a depth range of 10-20 km from the trench, and that slip decreases towards the trench with significant displacements at the toe of wedge occurring in just a small region. Estimates of static stress drop and rupture velocity are ambiguous. Due to the spatial compactness of the fault rupture, the duration of the entire rupture was less than approximately 150 s. C1 [Minson, S. E.; Simons, M.; Ortega, F.; Jiang, J.; Inbal, A.] CALTECH, Div Geol & Planetary Sci, Seismol Lab, Pasadena, CA 91125 USA. [Beck, J. L.] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. [Owen, S. E.; Moore, A. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sladen, A.] Univ Nice, CNRS UMR 7329, Geoazur, Observ Cote Azur,IRD,UPMC, Valbonne, France. RP Minson, SE (reprint author), CALTECH, Div Geol & Planetary Sci, Seismol Lab, Pasadena, CA 91125 USA. EM minson@gps.caltech.edu RI Ortega-Culaciati, Francisco Hernan/A-2587-2014; Sladen, Anthony/A-2532-2017; OI Ortega-Culaciati, Francisco Hernan/0000-0002-2983-8646; Sladen, Anthony/0000-0003-4126-0020; Jiang, Junle/0000-0002-8796-5846; Simons, Mark/0000-0003-1412-6395 FU National Science Foundation [EAR-0941374] FX The CATMIP MCMC simulations were executed on NASA's Pleiades supercomputer. This work is supported by the National Science Foundation through grant number EAR-0941374 and is Caltech Seismological Laboratory contribution 10087. NR 52 TC 18 Z9 18 U1 2 U2 21 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0956-540X EI 1365-246X J9 GEOPHYS J INT JI Geophys. J. Int. PD AUG PY 2014 VL 198 IS 2 BP 922 EP 940 DI 10.1093/gji/ggu170 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AM2YN UT WOS:000339717700018 ER PT J AU Mukhanov, O Johnson, M Kleinsasser, A AF Mukhanov, Oleg Johnson, Mark Kleinsasser, Alan TI SPECIAL ISSUE ON THE 2013 INTERNATIONAL SUPERCONDUCTIVE ELECTRONICS CONFERENCE (ISEC) SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Editorial Material C1 [Mukhanov, Oleg] Hypres Inc, Elmsford, NY 10523 USA. [Johnson, Mark] D Wave Syst Inc, Burnaby, BC V5C 4M9, Canada. [Kleinsasser, Alan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mukhanov, O (reprint author), Hypres Inc, 175 Clearbrook Rd, Elmsford, NY 10523 USA. NR 0 TC 0 Z9 0 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD AUG PY 2014 VL 24 IS 4 AR 0002101 DI 10.1109/TASC.2014.2332671 PG 1 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA AM7ZZ UT WOS:000340089200001 ER PT J AU Wang, H Long, L Kumar, A Wang, WQ Schemm, JKE Zhao, M Vecchi, GA Larow, TE Lim, YK Schubert, SD Shaevitz, DA Camargo, SJ Henderson, N Kim, D Jonas, JA Walsh, KJE AF Wang, Hui Long, Lindsey Kumar, Arun Wang, Wanqiu Schemm, Jae-Kyung E. Zhao, Ming Vecchi, Gabriel A. Larow, Timothy E. Lim, Young-Kwon Schubert, Siegfried D. Shaevitz, Daniel A. Camargo, Suzana J. Henderson, Naomi Kim, Daehyun Jonas, Jeffrey A. Walsh, Kevin J. E. TI How Well Do Global Climate Models Simulate the Variability of Atlantic Tropical Cyclones Associated with ENSO? SO JOURNAL OF CLIMATE LA English DT Article ID GENERAL-CIRCULATION MODELS; SEA-SURFACE TEMPERATURE; NORTH-ATLANTIC; EL-NINO; HURRICANE ACTIVITY; CMIP5 MODELS; FORECAST; GCM; PRECIPITATION; OSCILLATION AB The variability of Atlantic tropical cyclones (TCs) associated with El Nino-Southern Oscillation (ENSO) in model simulations is assessed and compared with observations. The model experiments are 28-yr simulations forced with the observed sea surface temperature from 1982 to 2009. The simulations were coordinated by the U.S. Climate Variability and Predictability Research Program (CLIVAR) Hurricane Working Group and conducted with five global climate models (GCMs) with a total of 16 ensemble members. The model performance is evaluated based on both individual model ensemble means and multimodel ensemble mean. The latter has the highest anomaly correlation (0.86) for the interannual variability of TCs. Previous observational studies show a strong association between ENSO and Atlantic TC activity, as well as distinctions during eastern Pacific (EP) and central Pacific (CP) El Nino events. The analysis of track density and TC origin indicates that each model has different mean biases. Overall, the GCMs simulate the variability of Atlantic TCs well with weaker activity during EP El Nino and stronger activity during La Nina. For CP El Nino, there is a slight increase in the number of TCs as compared with EP El Nino. However, the spatial distribution of track density and TC origin is less consistent among the models. Particularly, there is no indication of increasing TC activity over the U.S. southeast coastal region during CP El Nino as in observations. The difference between the models and observations is likely due to the bias of the models in response to the shift of tropical heating associated with CP El Nino, as well as the model bias in the mean circulation. C1 [Wang, Hui; Long, Lindsey; Kumar, Arun; Wang, Wanqiu; Schemm, Jae-Kyung E.] NOAA, NWS, NCEP, Climate Predict Ctr, College Pk, MD 20740 USA. [Wang, Hui; Long, Lindsey] Innovim, Greenbelt, MD USA. [Zhao, Ming; Vecchi, Gabriel A.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Larow, Timothy E.] Florida State Univ, Ctr Ocean Atmospher Predict Studies, Tallahassee, FL 32306 USA. [Lim, Young-Kwon; Schubert, Siegfried D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Lim, Young-Kwon] IM Syst Grp, Goddard Earth Sci Technol & Res, Greenbelt, MD USA. [Shaevitz, Daniel A.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [Camargo, Suzana J.; Henderson, Naomi; Kim, Daehyun] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Jonas, Jeffrey A.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Jonas, Jeffrey A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Walsh, Kevin J. E.] Univ Melbourne, Sch Earth Sci, Parkville, Vic 3052, Australia. RP Wang, H (reprint author), NOAA, Climate Predict Ctr, NCWCP, 5830 Univ Res Court, College Pk, MD 20740 USA. EM hui.wang@noaa.gov RI Camargo, Suzana/C-6106-2009; Vecchi, Gabriel/A-2413-2008; Zhao, Ming/C-6928-2014; OI Camargo, Suzana/0000-0002-0802-5160; Vecchi, Gabriel/0000-0002-5085-224X; Walsh, Kevin/0000-0002-1860-510X FU U.S. CLIVAR FX This work was carried out as part of a Hurricane Working Group activity supported by the U.S. CLIVAR. The authors thank the Lamont-Doherty Earth Observatory of Columbia University for archiving model data and making them accessible online. The authors also thank Prof. Kerry A. Emanuel, Dr. Christopher W. Landsea, Mr. Bill Mohan, an anonymous reviewer, and the editor for their insightful and constructive comments and suggestions. NR 50 TC 11 Z9 11 U1 4 U2 30 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD AUG 1 PY 2014 VL 27 IS 15 BP 5673 EP 5692 DI 10.1175/JCLI-D-13-00625.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AM2SY UT WOS:000339702300001 ER PT J AU Xia, YL Ek, MB Mocko, D Peters-Lidard, CD Sheffield, J Dong, JR Wood, EF AF Xia, Youlong Ek, Michael B. Mocko, David Peters-Lidard, Christa D. Sheffield, Justin Dong, Jiarui Wood, Eric F. TI Uncertainties, Correlations, and Optimal Blends of Drought Indices from the NLDAS Multiple Land Surface Model Ensemble SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID ASSIMILATION SYSTEM NLDAS; UNITED-STATES; 20TH-CENTURY DROUGHT; MONITOR AB This study analyzed uncertainties and correlations over the United States among four ensemble-mean North American Land Data Assimilation System (NLDAS) percentile-based drought indices derived from monthly mean evapotranspiration ET, total runoff Q, top 1-m soil moisture SM1, and total column soil moisture SMT. The results show that the uncertainty is smallest for SM1, largest for SMT, and moderate for ET and Q. The strongest correlation is between SM1 and SMT, and the weakest correlation is between ET and Q. The correlation between ET and SM1 (SMT) is strongest in arid-semiarid regions, and the correlation between Q and SM1 (SMT) is strongest in more humid regions in the Pacific Northwest and the Southeast. Drought frequency analysis shows that SM1 has the most frequent drought occurrence, followed by SMT, Q, and ET. The study compared the NLDAS drought indices (a research product) with the U.S. Drought Monitor (USDM; an operational product) in terms of drought area percentage derived from each product. It proposes an optimal blend of NLDAS drought indices by searching for weights for each index that minimizes the RMSE between NLDAS and USDM drought area percentage for a 10-yr period (2000-09) with a cross validation. It reconstructed a 30-yr (1980-2009) Objective Blended NLDAS Drought Index (OBNDI) and monthly drought percentage. Overall, the OBNDI performs the best with the smallest RMSE, followed by SM1 and SMT. It should be noted that the contribution to OBNDI from different variables varies with region. So a single formula is probably not the best representation of a blended index. The representation of a blended index using the multiple formulas will be addressed in a future study. C1 [Xia, Youlong; Dong, Jiarui] Environm Modeling Ctr, IMSG, College Pk, MD 20740 USA. [Xia, Youlong; Ek, Michael B.; Dong, Jiarui] NOAA, NCEP, EMC, IMSG, College Pk, MD 20740 USA. [Mocko, David; Peters-Lidard, Christa D.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Mocko, David] SAIC, Greenbelt, MD USA. [Sheffield, Justin; Wood, Eric F.] Princeton Univ, Dept Environm & Civil Engn, Princeton, NJ 08544 USA. RP Xia, YL (reprint author), NOAA, NCEP, EMC, IMSG, 5830 Univ Res Court, College Pk, MD 20740 USA. EM youlong.xia@noaa.gov RI Peters-Lidard, Christa/E-1429-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876 FU NOAA Climate Program Office's Modeling, Analysis, Prediction, and Projection (MAPP) program FX This study is sponsored by the NOAA Climate Program Office's Modeling, Analysis, Prediction, and Projection (MAPP) program. We thank Dr. Kingtse Mo from Climate Prediction Center, who provided SPI3 and SPI6 derived from CPC gauge precipitation data used in NLDAS-2. Y.X. thanks Dr. Weiyu Yang from EMC and three anonymous reviewers, whose comments and suggestions greatly improved the quality of this manuscript. NR 27 TC 10 Z9 11 U1 1 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD AUG PY 2014 VL 15 IS 4 BP 1636 EP 1650 DI 10.1175/JHM-D-13-058.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AM2QX UT WOS:000339697000020 ER PT J AU Zhou, T Nijssen, B Huffman, GJ Lettenmaier, DP AF Zhou, Tian Nijssen, Bart Huffman, George J. Lettenmaier, Dennis P. TI Evaluation of Real-Time Satellite Precipitation Data for Global Drought Monitoring SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID CONTERMINOUS UNITED-STATES; ANALYSIS TMPA; TRENDS; RAINFALL; SCALES AB The Tropical Rainfall Measuring Mission (TRMM) Multi-satellite Precipitation Analysis (TMPA) near-real-time (RT) data are considered less accurate than the TMPA research quality (RP) data because of the simplified data processing algorithm and the lack of gauge adjustments. However, for near-real-time hydrological applications, such as drought nowcasting, the RT data must play a key role given latency considerations and consistency is essential with products like RP, which have a long-term climatology. The authors used a bivariate test to examine the consistency between the monthly RT and RP precipitation estimates for 12 yr (2000-12) and found that, for over 75% of land cells globally, RT and RP were statistically consistent at 0.05 significance level. The inconsistent grid cells are spatially clustered in western North America, northern South America, central Africa, and most of Australia. The authors also show that RT generally increases with time relative to RP in northern South America and western Australia, while in western North America and eastern Australia, RT decreases relative to RP. In other areas such as the eastern part of North America, Eurasia, and southern part of the South America, the RT data are statistically consistent with the RP data and are appropriate for global- or macroscale hydrological applications. C1 [Zhou, Tian; Nijssen, Bart; Lettenmaier, Dennis P.] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA. [Huffman, George J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lettenmaier, DP (reprint author), Univ Washington, Dept Civil & Environm Engn, 202D Wilson Ceram Lab,Box 352700, Seattle, WA 98195 USA. EM dennisl@uw.edu RI Zhou, Tian/F-8659-2015; Nijssen, Bart/B-1013-2012; Huffman, George/F-4494-2014 OI Zhou, Tian/0000-0003-1582-4005; Nijssen, Bart/0000-0002-4062-0322; Huffman, George/0000-0003-3858-8308 FU NASA [NNX10AG87G] FX This study was supported by NASA Grant NNX10AG87G to the University of Washington. The authors thank David Bolvin for thoughtful comments, Huilin Gao for data sharing, and Faisal Hossain for his suggestions on an earlier draft of the manuscript. NR 25 TC 10 Z9 10 U1 2 U2 17 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD AUG PY 2014 VL 15 IS 4 BP 1651 EP 1660 DI 10.1175/JHM-D-13-0128.1 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AM2QX UT WOS:000339697000021 ER PT J AU Kitching, TD Heavens, AF Alsing, J Erben, T Heymans, C Hildebrandt, H Hoekstra, H Jaffe, A Kiessling, A Mellier, Y Miller, L van Waerbeke, L Benjamin, J Coupon, J Fu, L Hudson, MJ Kilbinger, M Kuijken, K Rowe, BTP Schrabback, T Semboloni, E Velander, M AF Kitching, T. D. Heavens, A. F. Alsing, J. Erben, T. Heymans, C. Hildebrandt, H. Hoekstra, H. Jaffe, A. Kiessling, A. Mellier, Y. Miller, L. van Waerbeke, L. Benjamin, J. Coupon, J. Fu, L. Hudson, M. J. Kilbinger, M. Kuijken, K. Rowe, B. T. P. Schrabback, T. Semboloni, E. Velander, M. TI 3D cosmic shear: cosmology from CFHTLenS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; cosmological parameters ID WEAK-LENSING SURVEYS; GALAXY SHAPE MEASUREMENT; MATTER POWER SPECTRUM; HUBBLE-SPACE-TELESCOPE; DARK ENERGY; INTRINSIC ALIGNMENTS; PRECISION COSMOLOGY; COVARIANCE-MATRIX; HALO MODEL; CONSTRAINTS AB This paper presents the first application of 3D cosmic shear to a wide-field weak lensing survey. 3D cosmic shear is a technique that analyses weak lensing in three dimensions using a spherical harmonic approach, and does not bin data in the redshift direction. This is applied to CFHTLenS, a 154 square degree imaging survey with a median redshift of 0.7 and an effective number density of 11 galaxies per square arcminute usable for weak lensing. To account for survey masks we apply a 3D pseudo-C-a"" approach on weak lensing data, and to avoid uncertainties in the highly non-linear regime, we separately analyse radial wavenumbers k a parts per thousand currency sign 1.5 and 5.0 h Mpc(-1), and angular wavenumbers a"" a parts per thousand 400-5000. We show how one can recover 2D and tomographic power spectra from the full 3D cosmic shear power spectra and present a measurement of the 2D cosmic shear power spectrum, and measurements of a set of 2-bin and 6-bin cosmic shear tomographic power spectra; in doing so we find that using the 3D power in the calculation of such 2D and tomographic power spectra from data naturally accounts for a minimum scale in the matter power spectrum. We use 3D cosmic shear to constrain cosmologies with parameters Omega(M), Omega(B), sigma(8), h , n(s), w(0) and w(a). For a non-evolving dark energy equation of state, and assuming a flat cosmology, lensing combined with Wilkinson Microwave Anisotropy Probe 7 results in h = 0.78 +/- 0.12, Omega(M) = 0.252 +/- 0.079, sigma(8) = 0.88 +/- 0.23 and w = -1.16 +/- 0.38 using only scales k a parts per thousand currency sign 1.5 h Mpc(-1). We also present results of lensing combined with first year Planck results, where we find no tension with the results from this analysis, but we also find no significant improvement over the Planck results alone. We find evidence of a suppression of power compared to Lambda cold dark matter (LCDM) on small scales 1.5 < k a parts per thousand currency sign 5.0 h Mpc(-1) in the lensing data, which is consistent with predictions of the effect of baryonic feedback on the matter power spectrum. C1 [Kitching, T. D.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Heavens, A. F.; Alsing, J.; Jaffe, A.] Univ London Imperial Coll Sci Technol & Med, Imperial Ctr Inference & Cosmol, London SW7 2AZ, England. [Erben, T.; Hildebrandt, H.; Schrabback, T.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Heymans, C.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Hildebrandt, H.; van Waerbeke, L.; Benjamin, J.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Hoekstra, H.; Kuijken, K.; Schrabback, T.; Semboloni, E.; Velander, M.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [Kiessling, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mellier, Y.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Mellier, Y.; Kilbinger, M.] CEA, Irfu, SAp Saclay, Lab AIM, F-91191 Gif Sur Yvette, France. [Miller, L.; Velander, M.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Coupon, J.] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland. [Fu, L.] Shanghai Normal Univ, Shanghai Key Lab Astrophys, Shanghai 200234, Peoples R China. [Hudson, M. J.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Hudson, M. J.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 1Y5, Canada. [Rowe, B. T. P.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Schrabback, T.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. RP Kitching, TD (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM t.kitching@ucl.ac.uk RI Hudson, Michael/H-3238-2012; Fu, Liping/B-3051-2012; OI Hudson, Michael/0000-0002-1437-3786; Kiessling, Alina/0000-0002-2590-1273; Rowe, Barnaby/0000-0002-7042-9174; Kilbinger, Martin/0000-0001-9513-7138; Hoekstra, Henk/0000-0002-0641-3231 FU Royal Society University FX We thank Dipak Munshi, Andy Taylor, Fergus Simpson, Stephen Feeney, Hiranya Peiris, Licia Verde, Raul Jimenez, Jason McEwen and Mark Cropper for useful discussions. We thank Anthony Lewis and the developers of CAMB, and the PPF module for making their code public. We thank Eric Tittley and Mark Holliman for system administration on several machines used in this work. We made use of CosmoCalc http://www.astro.ucla. edu/wright/CosmoCalc.html (Wright 2006) during development. We thank WMAP for providing their MCMC chains available for download http://lambda.gsfc.nasa.gov, and Eiichiro Komatsu for providing supplementary data products to the main WMAP data release. We thank ESA Planck for providing their MCMC chains available for download http://pla.esac.esa.int/pla/aio/planckProducts.html. TDK acknowledges support from a Royal Society University Research Fellowship. NR 81 TC 47 Z9 47 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2014 VL 442 IS 2 BP 1326 EP 1349 DI 10.1093/mnras/stu934 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL8XM UT WOS:000339423100032 ER PT J AU Goncalves, TS Basu-Zych, A Overzier, RA Perez, L Martin, DC AF Goncalves, Thiago S. Basu-Zych, Antara Overzier, Roderik A. Perez, Laura Martin, D. Christopher TI Molecular gas properties of UV-bright star-forming galaxies at low redshift SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: formation; galaxies: ISM; galaxies: starburst ID LYMAN BREAK GALAXY; ULTRAVIOLET-LUMINOUS GALAXIES; MASS-METALLICITY RELATION; CO-TO-H-2 CONVERSION FACTOR; DIGITAL SKY SURVEY; ULTRA DEEP FIELD; NEARBY GALAXIES; FORMATION LAW; SUBMILLIMETER GALAXIES; DISK GALAXIES AB Lyman break analogues (LBAs) are a population of star-forming galaxies at low redshift (z similar to 0.2) selected in the ultraviolet (UV). These objects present higher star formation rates and lower dust extinction than other galaxies with similar masses and luminosities in the local universe. In this work, we present results from a survey with the Combined Array for Research in Millimeter-wave Astronomy (CARMA) array to detect CO(1-0) emission in LBAs, in order to analyse the properties of the molecular gas in these galaxies. Our results show that LBAs follow the same Schmidt-Kennicutt law as local galaxies. On the other hand, they have higher gas fractions (up to 66 per cent) and faster gas depletion time-scales (below 1 Gyr). These characteristics render these objects more akin to high-redshift star-forming galaxies. We conclude that LBAs are a great nearby laboratory for studying the cold interstellar medium in low-metallicity, UV-bright compact star-forming galaxies. C1 [Goncalves, Thiago S.] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, RJ, Brazil. [Basu-Zych, Antara] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Overzier, Roderik A.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Perez, Laura] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Martin, D. Christopher] CALTECH, Pasadena, CA 91125 USA. RP Goncalves, TS (reprint author), Univ Fed Rio de Janeiro, Observ Valongo, Ladeira Pedro Antonio 43, BR-20080090 Rio De Janeiro, RJ, Brazil. EM tsg@astro.ufrj.br FU CAPES (Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior) FX We thank the anonymous referee for suggestions that helped improve this paper. We would also like to thank Andrew Baker and Tim Heckman for useful comments. TSG gratefully acknowledges CAPES (Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior) for financial support. Support for CARMA construction was derived from the states of California, Illinois, and Maryland, the James S. McDonnell Foundation, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the University of Chicago, 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 81 TC 5 Z9 5 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2014 VL 442 IS 2 BP 1429 EP 1439 DI 10.1093/mnras/stu852 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL8XM UT WOS:000339423100039 ER PT J AU Huang, H Cao, YW Xie, GD Ren, YX Yan, Y Bao, CJ Ahmed, N Neifeld, MA Dolinar, SJ Willner, AE AF Huang, Hao Cao, Yinwen Xie, Guodong Ren, Yongxiong Yan, Yan Bao, Changjing Ahmed, Nisar Neifeld, Mark A. Dolinar, Samuel J. Willner, Alan E. TI Crosstalk mitigation in a free-space orbital angular momentum multiplexed communication link using 4x4 MIMO equalization SO OPTICS LETTERS LA English DT Article ID ATMOSPHERIC-TURBULENCE; SINGLE-PHOTON; TRANSMISSION; FIBER; POLARIZATION; SYSTEMS; LIGHT AB We demonstrate crosstalk mitigation using 4 x 4 multiple-input-multiple-output (MIMO) equalization on an orbital angular momentum (OAM) multiplexed free-space data link with heterodyne detection. Four multiplexed OAM beams, each carrying a 20 Gbit/s quadrature phase-shift keying signal, propagate through weak turbulence. The turbulence induces inter-channel crosstalk among each beam and degrades the signal performance. Experimental results demonstrate that with the assistance of MIMO processing, the signal quality and the bit-error-rate (BER) performance can be improved. The power penalty can be reduced by >4 dB at a BER of 3.8 x 10(-3). (C) 2014 Optical Society of America C1 [Huang, Hao; Cao, Yinwen; Xie, Guodong; Ren, Yongxiong; Yan, Yan; Bao, Changjing; Ahmed, Nisar; Willner, Alan E.] Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA. [Neifeld, Mark A.] Univ Arizona, Dept Elect & Comp Engn, Tucson, AZ 85721 USA. [Dolinar, Samuel J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Huang, H (reprint author), Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA. EM haoh@usc.edu FU DARPA under the InPho (Information in a Photon) program FX We acknowledge the support of DARPA under the InPho (Information in a Photon) program. NR 24 TC 19 Z9 20 U1 0 U2 23 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 AUG 1 PY 2014 VL 39 IS 15 BP 4360 EP 4363 DI 10.1364/OL.39.004360 PG 4 WC Optics SC Optics GA AM5EL UT WOS:000339878900020 PM 25078177 ER PT J AU Ackermann, M Ajello, M Albert, A Baldini, L Ballet, J Barbiellini, G Bastieri, D Bellazzini, R Bissaldi, E Blandford, RD Bloom, ED Bottacini, E Brandt, TJ Bregeon, J Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caragiulo, M Caraveo, PA Cavazzuti, E Charles, E Chekhtman, A Cheung, CC Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Corbel, S D'Ammando, F de Angelis, A den Hartog, PR de Palma, F Dermer, CD Desiante, R Digel, SW Di Venere, L Silva, EDE Donato, D Drell, PS Drlica-Wagner, A Favuzzi, C Ferrara, EC Focke, WB Franckowiak, A Fuhrmann, L Fukazawa, Y Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Hadasch, D Harding, AK Hayashida, M Hays, E Hewitt, JW Hill, AB Hou, X Jean, P Jogler, T Johannesson, G Johnson, AS Johnson, WN Kerr, M Knodlseder, J Kuss, M Larsson, S Latronico, L Lemoine-Goumard, M Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Manfreda, A Martin, P Massaro, F Mayer, M Mazziotta, MN McEnery, JE Michelson, PF Mitthumsiri, W Mizuno, T Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nemmen, R Nuss, E Ohsugi, T Omodei, N Orienti, M Orlando, E Ormes, JF Paneque, D Panetta, JH Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Porter, TA Raino, S Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Reposeur, T Parkinson, PMS Schaal, M Schulz, A Sgro, C Siskind, EJ Spandre, G Spinelli, P Stawarz, L Suson, DJ Takahashi, H Tanaka, T Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Torres, DF Tosti, G Troja, E Uchiyama, Y Vianello, G Winer, BL Wolff, MT Wood, DL Wood, KS Wood, M Charbonnel, S Corbet, RHD Aquino, ID Edlin, JP Mason, E Schwarz, GJ Shore, SN Starrfield, S Teyssier, F AF Ackermann, M. Ajello, M. Albert, A. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bellazzini, R. Bissaldi, E. Blandford, R. D. Bloom, E. D. Bottacini, E. Brandt, T. J. Bregeon, J. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caragiulo, M. Caraveo, P. A. Cavazzuti, E. Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Corbel, S. D'Ammando, F. de Angelis, A. den Hartog, P. R. de Palma, F. Dermer, C. D. Desiante, R. Digel, S. W. Di Venere, L. do Couto e Silva, E. Donato, D. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Ferrara, E. C. Focke, W. B. Franckowiak, A. Fuhrmann, L. Fukazawa, Y. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Hadasch, D. Harding, A. K. Hayashida, M. Hays, E. Hewitt, J. W. Hill, A. B. Hou, X. Jean, P. Jogler, T. Johannesson, G. Johnson, A. S. Johnson, W. N. Kerr, M. Knoedlseder, J. Kuss, M. Larsson, S. Latronico, L. Lemoine-Goumard, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Manfreda, A. Martin, P. Massaro, F. Mayer, M. Mazziotta, M. N. McEnery, J. E. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nemmen, R. Nuss, E. Ohsugi, T. Omodei, N. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Porter, T. A. Raino, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Reposeur, T. Parkinson, P. M. Saz Schaal, M. Schulz, A. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Stawarz, L. Suson, D. J. Takahashi, H. Tanaka, T. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Uchiyama, Y. Vianello, G. Winer, B. L. Wolff, M. T. Wood, D. L. Wood, K. S. Wood, M. Charbonnel, S. Corbet, R. H. D. Aquino, I. De Gennaro Edlin, J. P. Mason, E. Schwarz, G. J. Shore, S. N. Starrfield, S. Teyssier, F. CA Fermi-LAT Collaboration TI Fermi establishes classical novae as a distinct class of gamma-ray sources SO SCIENCE LA English DT Article ID V407 CYGNI; EMISSION; ACCELERATION; SUBCLASS; OUTBURST AB A classical nova results from runaway thermonuclear explosions on the surface of a white dwarf that accretes matter from a low-mass main-sequence stellar companion. In 2012 and 2013, three novae were detected in gamma rays and stood in contrast to the first gamma-ray-detected nova V407 Cygni 2010, which belongs to a rare class of symbiotic binary systems. Despite likely differences in the compositions and masses of their white dwarf progenitors, the three classical novae are similarly characterized as soft-spectrum transient gamma-ray sources detected over 2- to 3-week durations. The gamma-ray detections point to unexpected high-energy particle acceleration processes linked to the mass ejection from thermonuclear explosions in an unanticipated class of Galactic gamma-ray sources. C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA. [Albert, A.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; den Hartog, P. R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. 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[Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Donato, D.; Hewitt, J. W.; Nemmen, R.; Corbet, R. H. D.] CRESST, Greenbelt, MD 20771 USA. [Donato, D.; McEnery, J. E.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Donato, D.; McEnery, J. E.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Drlica-Wagner, A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Fuhrmann, L.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Hadasch, D.; Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. 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EM teddy.cheung@nrl.navy.mil; pierre.jean@irap.omp.eu; shore@df.unipi.it RI Orlando, E/R-5594-2016; Di Venere, Leonardo/C-7619-2017; Torres, Diego/O-9422-2016; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Reimer, Olaf/A-3117-2013; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Massaro, Francesco/L-9102-2016 OI Di Venere, Leonardo/0000-0003-0703-824X; mason, elena/0000-0003-3877-0484; SPINELLI, Paolo/0000-0001-6688-8864; Hill, Adam/0000-0003-3470-4834; Torres, Diego/0000-0002-1522-9065; Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Bissaldi, Elisabetta/0000-0001-9935-8106; Massaro, Francesco/0000-0002-1704-9850 FU Naval Research Laboratory by a Karles' Fellowship; NASA through DPR program [S-15633-Y]; NASA through Guest Investigator program [11-FERMI11-0030, 12-FERMI12-0026]; NASA; NSF FX The Fermi-LAT Collaboration acknowledges support for LAT development, operation, and data analysis from NASA and the Department of Energy (United States), CEA/Irfu and IN2P3/CNRS (France), Agenzia Spaziale Italiana and INFN (Italy), MEXT, KEK, and JAXA (Japan), and the K. A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board (Sweden). Science analysis support in the operations phase from INAF (Italy) and CNES (France) is also gratefully acknowledged. We acknowledge with thanks the variable star observations from the American Association of Variable Star Observers International Database contributed by observers worldwide and used in this research and the dedicated observers of the Astronomical Ring for Access to Spectroscopy (ARAS) group for their tireless and selfless efforts. C.C.C. was supported at the Naval Research Laboratory by a Karles' Fellowship and by NASA through DPR S-15633-Y and Guest Investigator programs 11-FERMI11-0030 and 12-FERMI12-0026. S. S. was supported by NASA and NSF grants to Arizona State University. The Fermi-LAT data reported in this paper are available from http://fermi.gsfc.nasa.gov/ssc/data/access. NR 28 TC 35 Z9 36 U1 1 U2 32 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD AUG 1 PY 2014 VL 345 IS 6196 BP 554 EP 558 DI 10.1126/science.1253947 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM2AU UT WOS:000339651300043 ER PT J AU Mellon, MT Mckay, CP Heldmann, JL AF Mellon, Michael T. Mckay, Christopher P. Heldmann, Jennifer L. TI Polygonal ground in the McMurdo Dry Valleys of Antarctica and its relationship to ice-table depth and the recent Antarctic climate history SO ANTARCTIC SCIENCE LA English DT Article DE Beacon Valley; ground ice; permafrost; polygon ID MIOCENE GLACIER ICE; BEACON VALLEY; PERMAFROST DISTRIBUTION; REGION; MARS; SUBLIMATION; STABILITY; ORIGIN; CREEP; SNOW AB The occurrence of dry permafrost overlying ice-rich permafrost is unique to the Antarctic Dry Valleys on Earth and to the high latitudes of Mars. The stability and distribution of this ice are poorly understood and fundamental to understanding the Antarctic climate as far back as a few million years. Polygonal patterned ground is nearly ubiquitous in these regions and is integrally linked to the history of the icy permafrost and climate. We examined the morphology of polygonal ground in Beacon Valley and the Beacon Heights region of the Antarctic Dry Valleys, and show that polygon size is correlated with ice-table depth (the boundary between dry and ice-rich permafrost). A numerical model of seasonal stress in permafrost shows that the ice-table depth is a dominant factor. Remote sensing and field observations of polygon size are therefore important tools for investigating subsurface ice. Polygons are long-lived landforms and observed characteristics indicate no major fluctuations in the ice-table depth during their development. We conclude that the Beacon Valley and Beacon Heights polygons have developed for at least 10(4) years to achieve their present mature-stage morphology and that the ice-table depth has been stable for a similar length of time. C1 [Mellon, Michael T.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Mckay, Christopher P.; Heldmann, Jennifer L.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Mellon, MT (reprint author), SW Res Inst, Dept Space Studies, 1050 Walnut St, Boulder, CO 80302 USA. EM mellon@boulder.swri.edu RI Mellon, Michael/C-3456-2016 FU NASA Planetary Geology and Geophysics programme [NNX08AE33G]; NASA ASTEP programme; NSF Office of Polar Programs FX This work was supported in part by the NASA Planetary Geology and Geophysics programme through grant NNX08AE33G. We also acknowledge support from the NASA ASTEP programme. Field work in the Antarctic Dry Valleys was supported by the NSF Office of Polar Programs. We thank Jaakko Putkonen and an anonymous reviewer for their constructive and thorough comments. NR 44 TC 4 Z9 4 U1 1 U2 13 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0954-1020 EI 1365-2079 J9 ANTARCT SCI JI Antarct. Sci. PD AUG PY 2014 VL 26 IS 4 BP 413 EP 426 DI 10.1017/S0954102013000710 PG 14 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA AL8GX UT WOS:000339377300012 ER PT J AU Johnston, SL Blue, RS Jennings, RT Tarver, WJ Gray, GW AF Johnston, Smith L. Blue, Rebecca S. Jennings, Richard T. Tarver, William J. Gray, Gary W. TI Astronaut Medical Selection During the Shuttle Era: 1981-2011 SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE spaceflight; medical standards; crewmembers; medical screening AB Introduction: U.S. astronauts undergo extensive job-related screening and medical examinations prior to selection in order to identify candidates optimally suited for careers in spaceflight. Screening medical standards evolved over many years and after extensive spaceflight experience. These standards assess health-related risks for each astronaut candidate, minimizing the potential for medical impact on future mission success. This document discusses the evolution of the Shuttleera medical selection standards and the most common reasons for medical disqualification of applicants. Methods: Data for astronaut candidate finalists were compiled from medical records and NASA archives from the period of 1978 to 2004 and were retrospectively reviewed for medically disqualifying conditions. Results: During Shuttle selection cycles, a total of 372 applicants were disqualified due to 425 medical concerns. The most common disqualifying conditions included visual, cardiovascular, psychiatric, and behavioral disorders. During this time period, three major expert panel reviews resulted in refinements and alterations to selection standards for future cycles. Discussion: Shuttle-era screening, testing, and specialist evaluations evolved through periodic expert reviews, evidence-based medicine, and astronaut medical care experience. The Shuttle medical program contributed to the development and implementation of NASA and international standards, longitudinal data collection, improved medical care, and occupational surveillance models. The lessons learned from the Shuttle program serve as the basis for medical selection for the ISS, exploration-class missions, and for those expected to participate in commercial spaceflight. C1 [Johnston, Smith L.; Blue, Rebecca S.; Jennings, Richard T.; Tarver, William J.; Gray, Gary W.] NASA, Houston, TX USA. RP Blue, RS (reprint author), Univ Texas Med Branch, Dept Prevent Med & Community Hlth, 301 Univ Blvd, Galveston, TX 77555 USA. EM rsblue@utmb.edu NR 11 TC 0 Z9 0 U1 2 U2 3 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD AUG PY 2014 VL 85 IS 8 BP 823 EP 827 DI 10.3357/ASEM.3968.2014 PG 5 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AL9IU UT WOS:000339455600006 PM 25199124 ER PT J AU Anderson, JL Mertens, CJ Grajewski, B Luo, LA Tseng, CY Cassinelli, RT AF Anderson, Jeri L. Mertens, Christopher J. Grajewski, Barbara Luo, Lian Tseng, Chih-Yu Cassinelli, Rick T., II TI Flight Attendant Radiation Dose from Solar Particle Events SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE absorbed dose; effective dose; conceptus; reproductive health ID MODEL DEVELOPMENT; EXPOSURE; VALIDATION; ALTITUDES; AIRCREW AB Introduction: Research has suggested that work as a flight attendant may be related to increased risk for reproductive health effects. Air cabin exposures that may influence reproductive health include radiation dose from galactic cosmic radiation and solar particle events. This paper describes the assessment of radiation dose accrued during solar particle events as part of a reproductive health study of flight attendants. Methods: Solar storm data were obtained from the National Oceanic and Atmospheric Administration Space Weather Prediction Center list of solar proton events affecting the Earth environment to ascertain storms relevant to the two study periods (1992-1996 and 1999-2001). Radiation dose from exposure to solar energetic particles was estimated using the NAIRAS model in conjunction with galactic cosmic radiation dose calculated using the CARI-6P computer program. Results: Seven solar particle events were determined to have potential for significant radiation exposure, two in the first study period and five in the second study period, and over-lapped with 24,807 flight segments. Absorbed (and effective) flight segment doses averaged 6.5 mu Gy (18 mu Sv) and 3.1 mu Gy (8.3 mu Sv) for the first and second study periods, respectively. Maximum doses were as high as 440 mu Gy (1.2 mSv) and 20 flight segments had doses greater than 190 mu Gy (0.5 mSv). Discussion: During solar particle events, a pregnant flight attendant could potentially exceed the equivalent dose limit to the conceptus of 0.5 mSv in a month recommended by the National Council on Radiation Protection and Measurements. C1 [Anderson, Jeri L.] NIOSH, Cincinnati, OH 45226 USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Anderson, JL (reprint author), NIOSH, 4676 Columbia Pkwy,MS R-14, Cincinnati, OH 45226 USA. EM JLAnderson@cdc.gov NR 22 TC 2 Z9 2 U1 2 U2 8 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD AUG PY 2014 VL 85 IS 8 BP 828 EP 832 DI 10.3357/ASEM.3989.2014 PG 5 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AL9IU UT WOS:000339455600007 PM 25199125 ER PT J AU Watson, JT Bigelow, KA AF Watson, Jordan T. Bigelow, Keith A. TI Trade-offs among Catch, Bycatch, and Landed Value in the American Samoa Longline Fishery SO CONSERVATION BIOLOGY LA English DT Article DE Albacore; longline; nontarget species; observer data; sea turtles; sharks; trade-offs ID EASTERN PACIFIC-OCEAN; HORIZONTAL MOVEMENTS; DEPTH DISTRIBUTION; PELAGIC FISHES; BY-CATCH; TUNA; CLOSURES; BEHAVIOR; TIME; CONSERVATION AB The interspecific preferences of fishes for different depths and habitats suggest fishers could avoid unwanted catches of some species while still effectively targeting other species. In pelagic longline fisheries, albacore (Thunnus alalunga) are often caught in relatively cooler, deeper water (>100 m) than many species of conservation concern (e. g., sea turtles, billfishes, and some sharks) that are caught in shallower water (<100 m). From 2007 to 2011, we examined the depth distributions of hooks for 1154 longline sets (3,406,946 hooks) and recorded captures by hook position on 2642 sets (7,829,498 hooks) in the American Samoa longline fishery. Twenty-three percent of hooks had a settled depth <100 m. Individuals captured in the 3 shallowest hook positions accounted for 18.3% of all bycatch. We analyzed hypothetical impacts for 25 of the most abundant species caught in the fishery by eliminating the 3 shallowest hook positions under scenarios with and without redistribution of these hooks to deeper depths. Distributions varied by species: 45.5% (n = 10) of green sea turtle (Chelonia mydas), 59.5% (n = 626) of shortbill spearfish (Tetrapturus angustirostris), 37.3% (n = 435) of silky shark (Carcharhinus falciformis), and 42.6% (n = 150) of oceanic whitetip shark (C. longimanus) were caught on the 3 shallowest hooks. Eleven percent (n = 20,435) of all tuna and 8.5% (n = 10,374) of albacore were caught on the 3 shallowest hooks. Hook elimination reduced landed value by 1.6-9.2%, and redistribution of hooks increased average annual landed value relative to the status quo by 5-11.7%. Based on these scenarios, redistribution of hooks to deeper depths may provide an economically feasible modification to longline gear that could substantially reduce bycatch for a suite of vulnerable species. Our results suggest that this method may be applicable to deep-set pelagic longline fisheries worldwide. C1 [Watson, Jordan T.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA. [Watson, Jordan T.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA. [Bigelow, Keith A.] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. RP Watson, JT (reprint author), Univ Hawaii, Joint Inst Marine & Atmospher Res, 1000 Pope Rd, Honolulu, HI 96822 USA. EM jordan.watson@noaa.gov FU Fisheries Disaster Relief Program; Joint Institute for Marine and Atmospheric Research [NA09OAR4320075]; National Oceanic and Atmospheric Administration (NOAA) [NA09OAR4320075] FX We thank captains and crews of American Samoa based longline vessels and observers for TDR deployments. We thank S. Kostelnik and R. Kupfer for TDR data management, E. Fletcher for programming support, and E. Forney and J. Willson for data access. C. Boggs, D. Curran, P. Dalzell, M. Pan, Y. Swimmer, and 2 anonymous reviewers provided valuable input. This project was partially funded by the Fisheries Disaster Relief Program and by Cooperative Agreement NA09OAR4320075 between the Joint Institute for Marine and Atmospheric Research and the National Oceanic and Atmospheric Administration (NOAA). The views expressed herein are those of the authors and do not necessarily reflect the views of NOAA or any of its subdivisions. NR 48 TC 7 Z9 7 U1 2 U2 27 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD AUG PY 2014 VL 28 IS 4 BP 1012 EP 1022 DI 10.1111/cobi.12268 PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AL9ZB UT WOS:000339501100013 PM 24628499 ER PT J AU Desai, SD Bertiger, W Haines, BJ AF Desai, Shailen D. Bertiger, Willy Haines, Bruce J. TI Self-consistent treatment of tidal variations in the geocenter for precise orbit determination SO JOURNAL OF GEODESY LA English DT Article DE Reference frame; Geocenter; Ocean tides; Precise orbit determination; GPS ID MEAN SEA-LEVEL; GLOBAL POSITIONING SYSTEM; OCEAN TIDES; ALTIMETER MISSIONS; GEOSAT ALTIMETRY; TIME-SERIES; TOPEX/POSEIDON; SATELLITE; JASON-1; GPS AB We show that the current levels of accuracy being achieved for the precise orbit determination (POD) of low-Earth orbiters demonstrate the need for the self-consistent treatment of tidal variations in the geocenter. Our study uses as an example the POD of the OSTM/Jason-2 satellite altimeter mission based upon Global Positioning System (GPS) tracking data. Current GPS-based POD solutions are demonstrating root-mean-square (RMS) radial orbit accuracy and precision of cm and 1 mm, respectively. Meanwhile, we show that the RMS of three-dimensional tidal geocenter variations is mm, but can be as large as 15 mm, with the largest component along the Earth's spin axis. Our results demonstrate that GPS-based POD of Earth orbiters is best performed using GPS satellite orbit positions that are defined in a reference frame whose origin is at the center of mass of the entire Earth system, including the ocean tides. Errors in the GPS-based POD solutions for OSTM/Jason-2 of mm (3D RMS) and mm (radial RMS) are introduced when tidal geocenter variations are not treated consistently. Nevertheless, inconsistent treatment is measurable in the OSTM/Jason-2 POD solutions and manifests through degraded post-fit tracking data residuals, orbit precision, and relative orbit accuracy. For the latter metric, sea surface height crossover variance is higher by when tidal geocenter variations are treated inconsistently. C1 [Desai, Shailen D.; Bertiger, Willy; Haines, Bruce J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Desai, SD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 238-600, Pasadena, CA 91109 USA. EM shailen.desai@jpl.nasa.gov NR 48 TC 3 Z9 3 U1 2 U2 9 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 AUG PY 2014 VL 88 IS 8 BP 735 EP 747 DI 10.1007/s00190-014-0718-8 PG 13 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA AL8WV UT WOS:000339421400002 ER PT J AU Kolli, KK Effat, MA Peelukhana, SV Succop, P Back, LH Leesar, MA Helmy, TA Imran, A Banerjee, RK AF Kolli, Kranthi K. Effat, M. A. Peelukhana, Srikara V. Succop, Paul Back, Lloyd H. Leesar, M. A. Helmy, T. A. Imran, Arif Banerjee, R. K. TI Hyperemia-Free Delineation of Epicardial and Microvascular Impairments Using a Basal Index SO ANNALS OF BIOMEDICAL ENGINEERING LA English DT Article DE Coronary disease; FFR; CFR; CDP; Catheterization; Hyperemia-free index ID FRACTIONAL FLOW RESERVE; PRESSURE-DROP COEFFICIENT; CORONARY LESION SEVERITY; HEMODYNAMIC END-POINTS; PORCINE MODEL; CARDIAC-CATHETERIZATION; INTRAVENOUS ADENOSINE; HEART-RATE; STENOSIS; INTRACORONARY AB The assessment of functional coronary lesion severity using intracoronary hemodynamic parameters like the pressure-derived fractional flow reserve and the flow-derived coronary flow reserve are known to rely critically on the establishment of maximal hyperemia. We evaluated a hyperemia-free index, basal pressure drop coefficient (bCDP), that combines pressure and velocity for simultaneous assessment of the status of both epicardial and microvascular circulations. In 23 pigs, simultaneous measurements of distal coronary arterial pressure and flow were performed using a dual-sensor tipped guidewire in the settings of both normal and abnormal microcirculation with the presence of epicardial lesions of area stenosis (AS) < 50% and AS > 50%. The bCDP, a parameter based on fundamental fluid dynamics principles, was calculated as the transtenotic pressure-drop divided by the dynamic pressure in the distal vessel, measured under baseline (without hyperemia) conditions. The group mean values of bCDP for normal (84 +/- A 18) and abnormal (124.5 +/- A 15.6) microcirculation were significantly different. Similarly, the mean values of bCDP from AS < 50% (72.5 +/- A 16.1) and AS > 50% (136 +/- A 17.2) were also significantly different (p < 0.05). The bCDP could significantly distinguish between lesions of AS < 50% to AS > 50% under normal microcirculation (52.1 vs. 85.8; p < 0.05) and abnormal microcirculation (84.9 vs. 172; p < 0.05). Further, the bCDP correlated linearly and significantly with the hyperemic parameters FFR (r = 0.42, p < 0.05) and CDP (r = 0.50, p < 0.05). The bCDP is a promising clinical diagnostic parameter that can independently assess the severity of epicardial stenosis and microvascular impairment. We believe that it has an immediate appeal for detection of coronary artery disease if validated clinically. C1 [Kolli, Kranthi K.; Peelukhana, Srikara V.; Banerjee, R. K.] Univ Cincinnati, Dept Mech & Mat Engn, Cincinnati, OH 45221 USA. [Effat, M. A.; Helmy, T. A.; Imran, Arif] Univ Cincinnati, Div Cardiovasc Dis, Cincinnati, OH USA. [Kolli, Kranthi K.; Effat, M. A.; Peelukhana, Srikara V.; Helmy, T. A.; Imran, Arif; Banerjee, R. K.] Vet Affairs Med Ctr, Cincinnati, OH 45267 USA. [Succop, Paul] Univ Cincinnati, Dept Environm Hlth, Cincinnati, OH USA. [Back, Lloyd H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Leesar, M. A.] Univ Alabama Birmingham, Div Cardiovasc Dis, Birmingham, AL 35294 USA. RP Banerjee, RK (reprint author), Univ Cincinnati, Dept Mech & Mat Engn, 598 Rhodes Hall,POB 210072, Cincinnati, OH 45221 USA. EM rupak.banerjee@uc.edu FU Great Rivers Affiliate; National-Scientific Development Grant of American Heart Association [0755236B, 0335270N]; Department of Veteran Affairs Merit Review Grant [I01CX000342] FX The authors are grateful to Dr. Mahesh Krishnamoorthy, Dr. Subhashish Das Gupta, Marwan Al-Rjoub and Bhaskar Konala of Transport in Engineering and Medicine Laboratory at University of Cincinnati for their assistance during the experiments. This study is supported by Grant-In-Aid of Great Rivers Affiliate, National-Scientific Development Grant of American Heart Association (Grant reference #s: 0755236B and 0335270N) and a Department of Veteran Affairs Merit Review Grant (I01CX000342). NR 36 TC 1 Z9 1 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0090-6964 EI 1573-9686 J9 ANN BIOMED ENG JI Ann. Biomed. Eng. PD AUG PY 2014 VL 42 IS 8 BP 1681 EP 1690 DI 10.1007/s10439-014-1020-x PG 10 WC Engineering, Biomedical SC Engineering GA AL8OP UT WOS:000339399000009 PM 24806315 ER PT J AU Flagey, N Noriega-Crespo, A Petric, A Geballe, TR AF Flagey, N. Noriega-Crespo, A. Petric, A. Geballe, T. R. TI PALOMAR/TRIPLESPEC OBSERVATIONS OF SPITZER/MIPSGAL 24 mu m CIRCUMSTELLAR SHELLS: UNVEILING THE NATURES OF THEIR CENTRAL SOURCES SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; stars: early-type; stars: emission-line, Be; stars: late-type; stars: variables: S Doradus; stars: Wolf-Rayet ID WOLF-RAYET STARS; LUMINOUS BLUE VARIABLES; INNER GALACTIC PLANE; INFRARED CLASSIFICATION SPECTROSCOPY; H-ALPHA SURVEY; MASSIVE STARS; SPECTRAL-ANALYSES; COMPACT BUBBLES; RED SUPERGIANTS; BAND SPECTRA AB We present near-IR spectroscopic observations of the central sources in 17 circumstellar shells from a sample of more than 400 "bubbles" discovered in the Spitzer/MIPSGAL 24 mu m survey of the Galactic plane and in the Cygnus-X region. To identify the natures of these shells, we have obtained J, H, and K band spectra with a resolution of similar to 2600 of the stars at their centers. We observed 14 MIPSGAL bubbles (MBs), WR149, and 2 objects in the Cygnus-X region (WR138a and BD+43 3710), our sample being about 2.5 mag fainter in the K band than previous studies of the central sources of MBs. We use spectroscopic diagnostics and spectral libraries of late- and early-type stars to constrain the natures of our targets. We find five late-type giants. The equivalent widths of their CO 2.29 mu m features allow us to determine the spectral types of the stars and hence derive the extinction along the line of sight, distance, and physical size of the shells. We also find 12 early-type stars: in 9 MBs and the 3 comparison objects. We find that the subtype inferred from the near-IR for WR138a (WN9h) and WR149 (WN5h) agrees with that derived from optical observations. A careful analysis of the literature and the environment of BD+43 3710 allows us to rule out the carbon star interpretation previously suggested. Our near-IR spectrum suggests that it is a B5 supergiant. At the centers of the nine MBs, we find a WC5-6 star possibly of low mass, a candidate O5-6 V star, a B0 supergiant, a B/A-type giant, and five luminous blue variable (LBV) candidates. We also report the detections of emission lines arising from at least two shells with typical extents (similar to 10 ''), in agreement with those in the mid-IR. We summarize the findings on the natures of the MBs since their discovery, with 30% of them now known. Most MBs with central sources detected in the near- to mid-IR have been identified and are red and blue giants, supergiants, or stars evolving toward these phases, including, in particular, a handful of newly discovered Wolf-Rayet stars and a significant number of LBV candidates. C1 [Flagey, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Flagey, N.] Inst Astron, Hilo, HI 96720 USA. [Noriega-Crespo, A.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Noriega-Crespo, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Petric, A.] CALTECH, Pasadena, CA 91125 USA. [Petric, A.; Geballe, T. R.] Gemini North Observ, Hilo, HI 96720 USA. RP Flagey, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM nflagey@jpl.nasa.gov FU Gemini Observatory FX The Hale Telescope at Palomar Observatory is operated as part of a collaborative agreement between the California Institute of Technology and its divisions, Caltech Optical Observatories and the Jet Propulsion Laboratory (operated for NASA), and Cornell University. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. N.F. thanks Francois Ochsenbein for providing the plate scale of the BD charts, Paul Crowther for his help with some identifications, and the referee, Dr. Vasilii V. Gvaramadze, for valuable comments that clarified and improved this paper. T.R.G.s research is supported by the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina, Australia, Brazil, Canada, Chile, and the United States of America. NR 71 TC 10 Z9 10 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD AUG PY 2014 VL 148 IS 2 AR 34 DI 10.1088/0004-6256/148/2/34 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL7OQ UT WOS:000339324400010 ER PT J AU Archer, A Barnacka, A Beilicke, M Benbow, W Berger, K Bird, R Biteau, J Buckley, JH Bugaev, V Byrum, K Cardenzana, JV Cerruti, M Chen, W Chen, X Ciupik, L Connolly, MP Cui, W Dickinson, HJ Dumm, J Eisch, JD Falcone, A Federici, S Feng, Q Finley, JP Fleischhack, H Fortson, L Furniss, A Galante, N Griffin, S Griffiths, ST Grube, J Gyuk, G Hakansson, N Hanna, D Holder, J Hughes, G Johnson, CA Kaaret, P Kar, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Kumar, S Lang, MJ Maier, G McArthur, S McCann, A Meagher, K Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Park, N Perkins, JS Pohl, M Popkow, A Prokoph, H Pueschel, E Quinn, J Ragan, K Rajotte, J Reyes, LC Reynolds, PT Richards, GT Roache, E Sembroski, GH Shahinyan, K Smith, AW Staszak, D Telezhinsky, I Tucci, JV Tyler, J Varlotta, A Vincent, S Wakely, SP Weinstein, A Welsing, R Wilhelm, A Williams, DA Zajczyk, A Zitzer, B AF Archer, A. Barnacka, A. Beilicke, M. Benbow, W. Berger, K. Bird, R. Biteau, J. Buckley, J. H. Bugaev, V. Byrum, K. Cardenzana, J. V. Cerruti, M. Chen, W. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Dickinson, H. J. Dumm, J. Eisch, J. D. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fleischhack, H. Fortson, L. Furniss, A. Galante, N. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hakansson, N. Hanna, D. Holder, J. Hughes, G. Johnson, C. A. Kaaret, P. Kar, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Kumar, S. Lang, M. J. Maier, G. McArthur, S. McCann, A. Meagher, K. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Pueschel, E. Quinn, J. Ragan, K. Rajotte, J. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Sembroski, G. H. Shahinyan, K. Smith, A. W. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Varlotta, A. Vincent, S. Wakely, S. P. Weinstein, A. Welsing, R. Wilhelm, A. Williams, D. A. Zajczyk, A. Zitzer, B. TI VERY-HIGH ENERGY OBSERVATIONS OF THE GALACTIC CENTER REGION BY VERITAS IN 2010-2012 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astroparticle physics; black hole physics; Galaxy: center; gamma rays: galaxies; methods: data analysis; radiation mechanisms: non-thermal ID SGR-A-ASTERISK; GAMMA-RAY SOURCE; MOLECULAR CLOUDS; MAGIC TELESCOPE; SOURCE CATALOG; DARK-MATTER; CRAB-NEBULA; EMISSION; VARIABILITY; DISCOVERY AB The Galactic center is an interesting region for high-energy (0.1-100 GeV) and very-high-energy (E > 100 GeV) gamma-ray observations. Potential sources of GeV/TeV gamma-ray emission have been suggested, e.g., the accretion of matter onto the supermassive black hole, cosmic rays from a nearby supernova remnant (e.g., Sgr A East), particle acceleration in a plerion, or the annihilation of dark matter particles. The Galactic center has been detected by EGRET and by Fermi/LAT in the MeV/GeV energy band. At TeV energies, the Galactic center was detected with moderate significance by the CANGAROO and Whipple 10 m telescopes and with high significance by H.E.S.S., MAGIC, and VERITAS. We present the results from three years of VERITAS observations conducted at large zenith angles resulting in a detection of the Galactic center on the level of 18 standard deviations at energies above similar to 2.5 TeV. The energy spectrum is derived and is found to be compatible with hadronic, leptonic, and hybrid emission models discussed in the literature. Future, more detailed measurements of the high-energy cutoff and better constraints on the high-energy flux variability will help to refine and/or disentangle the individual models. C1 [Archer, A.; Beilicke, M.; Buckley, J. H.; Bugaev, V.; Chen, W.; Krawczynski, H.; Zajczyk, A.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Barnacka, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Benbow, W.; Cerruti, M.; Galante, N.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Khassen, Y.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin, Ireland. [Biteau, J.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Biteau, J.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Federici, S.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Chen, X.; Federici, S.; Fleischhack, H.; Hughes, G.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.; Wilhelm, A.] DESY, D-15738 Zeuthen, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kar, P.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Bishopstown, Cork, Ireland. RP Archer, A (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA. EM beilicke@physics.wustl.edu RI Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755; Pueschel, Elisa/0000-0002-0529-1973; Cui, Wei/0000-0002-6324-5772; Barnacka, Anna/0000-0001-5655-4158; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the UK FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. NR 61 TC 6 Z9 6 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2014 VL 790 IS 2 AR 149 DI 10.1088/0004-637X/790/2/149 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800066 ER PT J AU Bayliss, MB Rigby, JR Sharon, K Wuyts, E Florian, M Gladders, MD Johnson, T Oguri, M AF Bayliss, Matthew B. Rigby, Jane R. Sharon, Keren Wuyts, Eva Florian, Michael Gladders, Michael D. Johnson, Traci Oguri, Masamune TI THE PHYSICAL CONDITIONS, METALLICITY AND METAL ABUNDANCE RATIOS IN A HIGHLY MAGNIFIED GALAXY AT z=3.6252 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: star formation; gravitational lensing: strong ID STAR-FORMING GALAXIES; GRAVITATIONALLY LENSED GALAXY; STELLAR POPULATION SYNTHESIS; LYMAN-BREAK GALAXY; GIANT ARCS SURVEY; SIMILAR-TO 2; INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; H-II REGIONS; ULTRAVIOLET-SPECTRUM AB We present optical and near-IR imaging and spectroscopy of SGAS J105039.6+001730, a strongly lensed galaxy at z = 3.6252 magnified by >30x, and derive its physical properties. We measure a stellar mass of log(M-*/M-circle dot) = 9.5 +/- 0.35, star formation rates from [O II] lambda lambda 3727 and H beta of 55 +/- 25 and 84 +/- 24 M-circle dot yr(-1), respectively, an electron density of n(e) <= 10(3) cm(-2), an electron temperature of T-e <= 14,000 K, and a metallicity of 12 + log(O/H) = 8.3 +/- 0.1. The strong C III] lambda lambda 1907,1909 emission and abundance ratios of C, N, O, and Si are consistent with well-studied starbursts at z similar to 0 with similar metallicities. Strong P Cygni lines and He II lambda 1640 emission indicate a significant population of Wolf-Rayet stars, but synthetic spectra of individual populations of young, hot stars do not reproduce the observed integrated P Cygni absorption features. The rest-frame UV spectral features are indicative of a young starburst with high ionization, implying either (1) an ionization parameter significantly higher than suggested by rest-frame optical nebular lines, or (2) differences in one or both of the initial mass function and the properties of ionizing spectra of massive stars. We argue that the observed features are likely the result of a superposition of star forming regions with different physical properties. These results demonstrate the complexity of star formation on scales smaller than individual galaxies, and highlight the importance of systematic effects that result from smearing together the signatures of individual star forming regions within galaxies. C1 [Bayliss, Matthew B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Sharon, Keren; Johnson, Traci] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Wuyts, Eva] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Florian, Michael; Gladders, Michael D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Florian, Michael; Gladders, Michael D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Oguri, Masamune] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Oguri, Masamune] Univ Tokyo, Kavli Inst Phys & Math Universe Kavli IPMU WPI, Chiba 2778583, Japan. RP Bayliss, MB (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM mbayliss@cfa.harvard.edu RI Rigby, Jane/D-4588-2012; Oguri, Masamune/C-6230-2011 OI Rigby, Jane/0000-0002-7627-6551; FU National Science Foundation [AST-1009012]; NASA from the Space Telescope Science Institute [HST-GO-13003.01]; NASA [NAS5-26555]; JSPS [23740161]; FIRST program "Subaru Measurements of Images and Redshifts (SuMIRe)," World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan FX We thank Sally Heap and Dan Stark for interesting and helpful discussions that improved this paper, as well as the anonymous referee who provided very thoughtful and constructive feedback. This work was supported by the National Science Foundation through grant AST-1009012, by NASA through grant HST-GO-13003.01 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555, and also by the FIRST program "Subaru Measurements of Images and Redshifts (SuMIRe)," World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and Grant-in-Aid for Scientific Research from the JSPS (23740161). NR 103 TC 22 Z9 22 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2014 VL 790 IS 2 AR 144 DI 10.1088/0004-637X/790/2/144 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800061 ER PT J AU Boyajian, TS von Braun, K van Belle, G McAlister, HA ten Brummelaar, TA Kane, SR Muirhead, PS Jones, J White, R Schaefer, G Ciardi, D Henry, T Lopez-Morales, M Ridgway, S Gies, D Jao, WC Rojas-Ayala, B Parks, JR Sturmann, L Sturmann, J Turner, NH Farrington, C Goldfinger, PJ Berger, DH AF Boyajian, Tabetha S. von Braun, Kaspar van Belle, Gerard McAlister, Harold A. ten Brummelaar, Theo A. Kane, Stephen R. Muirhead, Philip S. Jones, Jeremy White, Russel Schaefer, Gail Ciardi, David Henry, Todd Lopez-Morales, Mercedes Ridgway, Stephen Gies, Douglas Jao, Wei-Chun Rojas-Ayala, Barbara Parks, J. Robert Sturmann, Laszlo Sturmann, Judit Turner, Nils H. Farrington, Chris Goldfinger, P. J. Berger, David H. TI STELLAR DIAMETERS AND TEMPERATURES. II. MAIN-SEQUENCE K- AND M-STARS (vol 757, pg 112, 2012) SO ASTROPHYSICAL JOURNAL LA English DT Correction ID LOW-MASS STARS; NEARBY RED DWARFS; INFRARED PHOTOMETRY; SOLAR NEIGHBORHOOD; UBV PHOTOMETRY; STANDARD STARS; ECLIPSING BINARIES; MAGNETIC ACTIVITY; UVBY PHOTOMETRY; BETA PHOTOMETRY C1 [Boyajian, Tabetha S.; McAlister, Harold A.; Jones, Jeremy; White, Russel; Henry, Todd; Gies, Douglas; Jao, Wei-Chun; Rojas-Ayala, Barbara; Parks, J. Robert] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA. [Boyajian, Tabetha S.; McAlister, Harold A.; Jones, Jeremy; White, Russel; Henry, Todd; Gies, Douglas; Jao, Wei-Chun; Parks, J. Robert] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [von Braun, Kaspar; Kane, Stephen R.; Ciardi, David] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [van Belle, Gerard] Lowell Observ, Flagstaff, AZ 86001 USA. [ten Brummelaar, Theo A.; Schaefer, Gail; Sturmann, Laszlo; Sturmann, Judit; Turner, Nils H.; Farrington, Chris; Goldfinger, P. J.] Mt Wilson Observ, CHARA Array, Mount Wilson, CA 91023 USA. [Muirhead, Philip S.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Lopez-Morales, Mercedes] CSIC, IEEC, Inst Ciencies Espai, E-08193 Barcelona, Spain. [Lopez-Morales, Mercedes] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Ridgway, Stephen] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Rojas-Ayala, Barbara] Amer Museum Nat Hist, Dept Astrophys, Div Phys Sci, New York, NY 10024 USA. [Berger, David H.] Syst Planning Corp, Arlington, VA 22201 USA. RP Boyajian, TS (reprint author), Georgia State Univ, Ctr High Angular Resolut Astron, POB 4106, Atlanta, GA 30302 USA. RI Rojas-Ayala, Barbara/G-4382-2015; Muirhead, Philip/H-2273-2014; OI Rojas-Ayala, Barbara/0000-0002-0149-1302; Muirhead, Philip/0000-0002-0638-8822; Boyajian, Tabetha/0000-0001-9879-9313 NR 217 TC 0 Z9 0 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2014 VL 790 IS 2 AR 166 DI 10.1088/0004-637X/790/2/166 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800083 ER PT J AU Brosius, JW Daw, AN Rabin, DM AF Brosius, Jeffrey W. Daw, Adrian N. Rabin, D. M. TI PERVASIVE FAINT Fe XIX EMISSION FROM A SOLAR ACTIVE REGION OBSERVED WITH EUNIS-13: EVIDENCE FOR NANOFLARE HEATING SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: flares; Sun: UV radiation ID CORONAL DIAGNOSTIC SPECTROMETER; EXTREME-ULTRAVIOLET SPECTRUM; HIGH TIME RESOLUTION; X-RAY TELESCOPE; HOT PLASMA; CHROMOSPHERIC EVAPORATION; RESONANT ABSORPTION; SOUNDING ROCKET; ATOMIC DATABASE; ENERGY-RELEASE AB We present spatially resolved EUV spectroscopic measurements of pervasive, faint Fe XIX 592.2 angstrom line emission in an active region observed during the 2013 April 23 flight of the Extreme Ultraviolet Normal Incidence Spectrograph (EUNIS-13) sounding rocket instrument. With cooled detectors, high sensitivity, and high spectral resolution, EUNIS-13 resolves the lines of Fe XIX at 592.2 angstrom(formed at temperature T approximate to 8.9MK) and Fe XII at 592.6 angstrom (T approximate to 1.6MK). The Fe XIX line emission, observed over an area in excess of 4920 arcsec(2) (2.58 x 10(9) km(2), more than 60% of the active region), provides strong evidence for the nanoflare heating model of the solar corona. No GOES events occurred in the region less than 2 hr before the rocket flight, but a microflare was observed north and east of the region with RHESSI and EUNIS during the flight. The absence of significant upward velocities anywhere in the region, particularly the microflare, indicates that the pervasive Fe XIX emission is not propelled outward from the microflare site, but is most likely attributed to localized heating (not necessarily due to reconnection) consistent with the nanoflare heating model of the solar corona. Assuming ionization equilibrium we estimate Fe XIX/Fe XII emission measure ratios of similar to 0.076 just outside the AR core and similar to 0.59 in the core. C1 [Brosius, Jeffrey W.] Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Daw, Adrian N.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Rabin, D. M.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Brosius, JW (reprint author), Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA. EM Jeffrey.W.Brosius@nasa.gov FU NASA Heliophysics Division through its Low Cost Access to Space program FX EUNIS-13 was supported by the NASA Heliophysics Division through its Low Cost Access to Space program. CHIANTI is a collaborative project involving George Mason University, the University of Michigan (USA), and the University of Cambridge (UK). We thank Dr. Gordon Holman for assistance with creating the RHESSI image, and the anonymous referee for valuable comments that helped improve the manuscript. NR 68 TC 19 Z9 19 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2014 VL 790 IS 2 AR 112 DI 10.1088/0004-637X/790/2/112 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800029 ER PT J AU Desjardins, TD Gallagher, SC Hornschemeier, AE Mulchaey, JS Walker, LM Brandt, WN Charlton, JC Johnson, KE Tzanavaris, P AF Desjardins, Tyler D. Gallagher, Sarah C. Hornschemeier, Ann E. Mulchaey, John S. Walker, Lisa May Brandt, William N. Charlton, Jane C. Johnson, Kelsey E. Tzanavaris, Panayiotis TI SOME LIKE IT HOT: LINKING DIFFUSE X-RAY LUMINOSITY, BARYONIC MASS, AND STAR FORMATION RATE IN COMPACT GROUPS OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: groups: general; X-rays: galaxies ID CHANDRA MULTIWAVELENGTH PROJECT; NORMAL ELLIPTIC GALAXIES; NORTH POLAR SPUR; SPECTRAL ENERGY-DISTRIBUTIONS; NEAR-INFRARED PROPERTIES; ACTIVE GALACTIC NUCLEUS; ALL-SKY SURVEY; REDSHIFT SURVEY; INTERSTELLAR-MEDIUM; SCALING RELATIONS AB We present an analysis of the diffuse X-ray emission in 19 compact groups (CGs) of galaxies observed with Chandra. The hottest, most X-ray luminous CGs agree well with the galaxy cluster X-ray scaling relations in L-X-T and L-X-sigma, even in CGs where the hot gas is associated with only the brightest galaxy. Using Spitzer photometry, we compute stellar masses and classify Hickson CGs 19, 22, 40, and 42, and RSCGs 32, 44, and 86 as fossil groups using a new definition for fossil systems that includes a broader range of masses. We find that CGs with total stellar and Hi masses greater than or similar to 10(11.3) M-circle dot are often X-ray luminous, while lower-mass CGs only sometimes exhibit faint, localized X-ray emission. Additionally, we compare the diffuse X-ray luminosity against both the total UV and 24 m star formation rates of each CG and optical colors of the most massive galaxy in each of the CGs. The most X-ray luminous CGs have the lowest star formation rates, likely because there is no cold gas available for star formation, either because the majority of the baryons in these CGs are in stars or the X-ray halo, or due to gas stripping from the galaxies in CGs with hot halos. Finally, the optical colors that trace recent star formation histories of the most massive group galaxies do not correlate with the X-ray luminosities of the CGs, indicating that perhaps the current state of the X-ray halos is independent of the recent history of stellar mass assembly in the most massive galaxies. C1 [Desjardins, Tyler D.; Gallagher, Sarah C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Hornschemeier, Ann E.; Tzanavaris, Panayiotis] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Mulchaey, John S.] Carnegie Observ, Pasadena, CA 91101 USA. [Walker, Lisa May; Johnson, Kelsey E.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Brandt, William N.; Charlton, Jane C.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Tzanavaris, Panayiotis] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Desjardins, TD (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. RI Brandt, William/N-2844-2015 OI Brandt, William/0000-0002-0167-2453 FU Natural Science and Engineering Research Council of Canada; Ontario Early Researcher Award Program; NASA ADP grant [NNX10AC99G]; NSF grant [AST-1108604]; NSF [AST-0908984]; ACIS [SAO SV4-74018]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX T.D.D. and S.C.G. thank the Natural Science and Engineering Research Council of Canada and the Ontario Early Researcher Award Program for support. W.N.B. is supported by NASA ADP grant NNX10AC99G and NSF grant AST-1108604 for support. J.C.C. thanks NSF for funding under award AST-0908984. This work was partially supported by the ACIS Instrument Team contract SAO SV4-74018 (PI: G. Garmire). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Based on observations obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. NR 141 TC 8 Z9 8 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2014 VL 790 IS 2 AR 132 DI 10.1088/0004-637X/790/2/132 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800049 ER PT J AU Fabrycky, DC Lissauer, JJ Ragozzine, D Rowe, JF Steffen, JH Agol, E Barclay, T Batalha, N Borucki, W Ciardi, DR Ford, EB Gautier, TN Geary, JC Holman, MJ Jenkins, JM Li, J Morehead, RC Morris, RL Shporer, A Smith, JC Still, M Van Cleve, J AF Fabrycky, Daniel C. Lissauer, Jack J. Ragozzine, Darin Rowe, Jason F. Steffen, Jason H. Agol, Eric Barclay, Thomas Batalha, Natalie Borucki, William Ciardi, David R. Ford, Eric B. Gautier, Thomas N. Geary, John C. Holman, Matthew J. Jenkins, Jon M. Li, Jie Morehead, Robert C. Morris, Robert L. Shporer, Avi Smith, Jeffrey C. Still, Martin Van Cleve, Jeffrey TI ARCHITECTURE OF KEPLER'S MULTI-TRANSITING SYSTEMS. II. NEW INVESTIGATIONS WITH TWICE AS MANY CANDIDATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: statistical; planetary systems; planets and satellites: detection; planets and satellites: dynamical evolution and stability ID PLANET SYSTEMS; ORBITAL ECCENTRICITIES; MULTIPLANET SYSTEMS; TIMING OBSERVATIONS; SUPER-EARTH; DYNAMICS; CONFIRMATION; STABILITY; MIGRATION; HARPS AB We report on the orbital architectures of Kepler systems having multiple-planet candidates identified in the analysis of data from the first six quarters of Kepler data and reported by Batalha et al. (2013). These data show 899 transiting planet candidates in 365 multiple-planet systems and provide a powerful means to study the statistical properties of planetary systems. Using a generic mass-radius relationship, we find that only two pairs of planets in these candidate systems (out of 761 pairs total) appear to be on Hill-unstable orbits, indicating similar to 96% of the candidate planetary systems are correctly interpreted as true systems. We find that planet pairs show little statistical preference to be near mean-motion resonances. We identify an asymmetry in the distribution of period ratios near first-order resonances (e.g., 2:1, 3:2), with an excess of planet pairs lying wide of resonance and relatively few lying narrow of resonance. Finally, based upon the transit duration ratios of adjacent planets in each system, we find that the interior planet tends to have a smaller transit impact parameter than the exterior planet does. This finding suggests that the mode of the mutual inclinations of planetary orbital planes is in the range 1 degrees.0-2 degrees.2, for the packed systems of small planets probed by these observations. C1 [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Lissauer, Jack J.; Rowe, Jason F.; Barclay, Thomas; Batalha, Natalie; Borucki, William; Jenkins, Jon M.; Li, Jie; Morris, Robert L.; Smith, Jeffrey C.; Van Cleve, Jeffrey] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ragozzine, Darin; Geary, John C.; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rowe, Jason F.; Li, Jie; Morris, Robert L.; Smith, Jeffrey C.; Van Cleve, Jeffrey] SETI Inst, Mountain View, CA 94043 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Steffen, Jason H.] CIERA Northwestern Univ, Evanston, IL 60208 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Ford, Eric B.; Morehead, Robert C.] Penn State Univ, Davey Lab 525, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Ford, Eric B.; Morehead, Robert C.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Ford, Eric B.; Morehead, Robert C.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA. [Gautier, Thomas N.; Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [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. RP Fabrycky, DC (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM fabrycky@uchicago.edu OI /0000-0002-0802-9145; Ciardi, David/0000-0002-5741-3047; /0000-0001-6545-639X; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NASA through Hubble Fellowship [HF-51272.01-A]; NASA [NAS 5-26555]; NSF [0645416]; National Aeronautics and Space Administration [NNX08AR04G]; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; National Science Foundation [0707203, DGE-0802270] FX Funding for this mission is provided by NASA's Science Mission Directorate. We thank the entire Kepler team for the many years of work that is making the Kepler mission so successful. We thank Emily Fabrycky, Doug Lin, Man-Hoi Lee, Scott Tremaine, and Tsevi Mazeh for helpful conversations and insightful comments. D.C F. acknowledges support for this work was provided by NASA through Hubble Fellowship grant No. HF-51272.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. E.A. was supported by NSF Career grant 0645416. E.B.F acknowledges support by the National Aeronautics and Space Administration under grant NNX08AR04G issued through the Kepler Participating Scientist Program, and the Center for Exoplanets and Habitable Worlds, which is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. This material is based upon work supported by the National Science Foundation under grant No. 0707203. R.C.M. was support by the National Science Foundation Graduate Research Fellowship under grant No. DGE-0802270. NR 40 TC 107 Z9 107 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 AUG 1 PY 2014 VL 790 IS 2 AR 146 DI 10.1088/0004-637X/790/2/146 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800063 ER PT J AU Farnocchia, D Chesley, SR Chodas, PW Tricarico, P Kelley, MSP Farnham, TL AF Farnocchia, Davide Chesley, Steven R. Chodas, Paul W. Tricarico, Pasquale Kelley, Michael S. P. Farnham, Tony L. TI TRAJECTORY ANALYSIS FOR THE NUCLEUS AND DUST OF COMET C/2013 A1 (SIDING SPRING) SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; comets: individual (C/2013 A1); methods: analytical; radiation: dynamics ID MARS; FORCES AB Comet C/2013 A1 (Siding Spring) will experience a high velocity encounter with Mars on 2014 October 19 at a distance of 135,000 km +/- 5000 km from the planet center. We present a comprehensive analysis of the trajectory of both the comet nucleus and the dust tail. The nucleus of C/2013 A1 cannot impact on Mars even in the case of unexpectedly large nongravitational perturbations. Furthermore, we compute the required ejection velocities for the dust grains of the tail to reach Mars as a function of particle radius and density and heliocentric distance of the ejection. A comparison between our results and the most current modeling of the ejection velocities suggests that impacts are possible only for millimeter to centimeter size particles released more than 13AU from the Sun. However, this level of cometary activity that far from the Sun is considered extremely unlikely. The arrival time of these particles spans a 20-minute time interval centered at 2014 October 19 at 20: 09 TDB, i.e., around the time that Mars crosses the orbital plane of C/2013 A1. Ejection velocities larger than currently estimated by a factor >2 would allow impacts for smaller particles ejected as close as 3AU from the Sun. These particles would reach Mars from 19:13 TDB to 20:40 TDB. C1 [Farnocchia, Davide; Chesley, Steven R.; Chodas, Paul W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tricarico, Pasquale] Planetary Sci Inst, Tucson, AZ 85719 USA. [Kelley, Michael S. P.; Farnham, Tony L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Farnocchia, D (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Davide.Farnocchia@jpl.nasa.gov OI Kelley, Michael/0000-0002-6702-7676; Chesley, Steven/0000-0003-3240-6497 NR 15 TC 15 Z9 15 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 AUG 1 PY 2014 VL 790 IS 2 AR 114 DI 10.1088/0004-637X/790/2/114 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800031 ER PT J AU Fuskeland, U Wehus, IK Eriksen, HK Naess, SK AF Fuskeland, U. Wehus, I. K. Eriksen, H. K. Naess, S. K. TI SPATIAL VARIATIONS IN THE SPECTRAL INDEX OF POLARIZED SYNCHROTRON EMISSION IN THE 9 yr WMAP SKY MAPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; Galaxy: structure; methods: statistical; polarization; radio continuum: general ID COMPONENT SEPARATION; MICROWAVE; POWER AB We estimate the spectral index, beta, of polarized synchrotron emission as observed in the 9 yr Wilkinson Microwave Anisotropy Probe sky maps using two methods, linear regression ("T-T plot") and maximum likelihood. We partition the sky into 24 disjoint sky regions and evaluate the spectral index for all polarization angles between 0. and 85 degrees in steps of 5 degrees. Averaging over polarization angles, we derive a mean spectral index of beta(all-sky) = -2.99 +/- 0.01 in the frequency range of 23-33 GHz. We find that the synchrotron spectral index steepens by 0.14 from low to high Galactic latitudes, in agreement with previous studies, with mean spectral indices of beta(plane) = -2.98 +/- 0.01 and beta(high-lat) = -3.12 +/- 0.04. In addition, we find a significant longitudinal variation along the Galactic plane with a steeper spectral index toward the Galactic center and anticenter than toward the Galactic spiral arms. This can be well modeled by an offset sinusoidal, beta(l) = -2.85 + 0.17 sin(2l - 90 degrees). Finally, we study synchrotron emission in the BICEP2 field, in an attempt to understand whether the claimed detection of large-scale B-mode polarization could be explained in terms of synchrotron contamination. Adopting a spectral index of beta = -3.12, typical for high Galactic latitudes, we find that the most likely bias corresponds to about 2% of the reported signal (r = 0.003). The flattest index allowed by the data in this region is beta = -2.5, and under the assumption of a straight power-law frequency spectrum, we find that synchrotron emission can account for at most 20% of the reported BICEP2 signal. C1 [Fuskeland, U.; Eriksen, H. K.; Naess, S. K.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Wehus, I. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wehus, I. K.; Naess, S. K.] Univ Oxford, DWB, Oxford OX1 3RH, England. RP Fuskeland, U (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, NO-0315 Oslo, Norway. EM unnif@astro.uio.no; i.k.wehus@fys.uio.no; h.k.k.eriksen@astro.uio.no; s.k.nass@astro.uio.no FU ERC [StG2010-257080, 259505]; NASA FX The computations presented in this paper were carried out on Abel, a cluster owned and maintained by the University of Oslo and NOTUR. This project was supported by the ERC Starting Grant StG2010-257080. I. K. W. acknowledges support from ERC grant 259505. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) software and analysis package. NR 28 TC 23 Z9 23 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2014 VL 790 IS 2 AR 104 DI 10.1088/0004-637X/790/2/104 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800021 ER PT J AU Gatuzz, E Garcia, J Mendoza, C Kallman, TR Bautista, MA Gorczyca, TW AF Gatuzz, E. Garcia, J. Mendoza, C. Kallman, T. R. Bautista, M. A. Gorczyca, T. W. TI PHYSICAL PROPERTIES OF THE INTERSTELLAR MEDIUM USING HIGH-RESOLUTION CHANDRA SPECTRA: O K-EDGE ABSORPTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; ISM: abundances; ISM: atoms; X-rays: binaries; X-rays: ISM ID X-RAY SPECTROSCOPY; XMM-NEWTON OBSERVATION; NEUTRON-STAR; ATOMIC OXYGEN; SCORPIUS X-1; 4U 1820-30; CYG X-2; SHELL PHOTOABSORPTION; CROSS-SECTIONS; LOW/HARD STATE AB Chandra high-resolution spectra toward eight low-mass Galactic binaries have been analyzed with a photoionization model that is capable of determining the physical state of the interstellar medium. Particular attention is given to the accuracy of the atomic data. Hydrogen column densities are derived with a broadband fit that takes into account pileup effects, and in general are in good agreement with previous results. The dominant features in the oxygen-edge region are OI and OII K alpha absorption lines whose simultaneous fits lead to average values of the ionization parameter of log xi = -2.90 and oxygen abundance of A(O) = 0.70. The latter is given relative to the standard by Grevesse & Sauval, but rescaling with the revision by Asplund et al. would lead to an average abundance value fairly close to solar. The low average oxygen column density (N-O = 9.2 x 10(17) cm(-2)) suggests a correlation with the low ionization parameters, the latter also being in evidence in the column density ratios N(O II)/N(O I) and N(O III)/N(O I) that are estimated to be less than 0.1. We do not find conclusive evidence for absorption by any other compound but atomic oxygen in our oxygen-edge region analysis. C1 [Gatuzz, E.; Mendoza, C.] Inst Venezolano Invest Cient, Ctr Fis, Caracas 1020A, Venezuela. [Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mendoza, C.; Bautista, M. A.; Gorczyca, T. W.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gatuzz, E (reprint author), Inst Venezolano Invest Cient, Ctr Fis, POB 20632, Caracas 1020A, Venezuela. EM egatuzz@ivic.gob.ve; javier@head.cfa.harvard.edu; claudio@ivic.gob.ve; timothy.r.kallman@nasa.gov; manuel.bautista@wmich.edu; thomas.gorczyca@wmich.edu OI Mendoza, Claudio/0000-0002-2854-4806 FU National Science Foundation [AST-1313265] FX Part of this work was carried out by Efrain Gatuzz during a visit in 2014 January to the Laboratory of High Energy Astrophysics, NASA Goddard Space Flight Center, Greenbelt, Maryland, USA. Their hospitality and financial support are gratefully acknowledged. Manuel Bautista has received financial support from the National Science Foundation through grant AST-1313265. We would also like to thank Dr. Frits Paerels for comments at the refereeing stage that led to substantial improvements of the arguments presented and thus of the final quality of the paper. NR 51 TC 8 Z9 8 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2014 VL 790 IS 2 AR 131 DI 10.1088/0004-637X/790/2/131 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800048 ER PT J AU Kassin, SA Brooks, A Governato, F Weiner, BJ Gardner, JP AF Kassin, Susan A. Brooks, Alyson Governato, Fabio Weiner, Benjamin J. Gardner, Jonathan P. TI KINEMATIC EVOLUTION OF SIMULATED STAR-FORMING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: fundamental parameters; galaxies: kinematics and dynamics; galaxies: spiral ID COSMOLOGICAL ZOOM SIMULATIONS; INITIAL MASS FUNCTION; TULLY-FISHER RELATION; NEARBY GALAXIES; STELLAR FEEDBACK; FORMATION LAW; HYDRODYNAMIC SIMULATIONS; PHYSICAL-PROPERTIES; MOLECULAR-HYDROGEN; DWARF GALAXIES AB Recent observations have shown that star-forming galaxies like our own Milky Way evolve kinematically into ordered thin disks over the last similar to 8 billion years since z = 1.2, undergoing a process of "disk settling." For the first time, we study the kinematic evolution of a suite of four state of the art "zoom in" hydrodynamic simulations of galaxy formation and evolution in a fully cosmological context and compare with these observations. Until now, robust measurements of the internal kinematics of simulated galaxies were lacking because the simulations suffered from low resolution, overproduction of stars, and overly massive bulges. The current generation of simulations has made great progress in overcoming these difficulties and is ready for a kinematic analysis. We show that simulated galaxies follow the same kinematic trends as real galaxies: they progressively decrease in disordered motions (sigma(g)) and increase in ordered rotation (V-rot) with time. The slopes of the relations between both sigma(g) and V-rot with redshift are consistent between the simulations and the observations. In addition, the morphologies of the simulated galaxies become less disturbed with time, also consistent with observations. This match between the simulated and observed trends is a significant success for the current generation of simulations, and a first step in determining the physical processes behind disk settling. C1 [Kassin, Susan A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Brooks, Alyson] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Governato, Fabio] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Weiner, Benjamin J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Gardner, Jonathan P.] Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Kassin, SA (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM kassin@stsci.edu OI Kassin, Susan/0000-0002-3838-8093 FU NSF [AST-0607819]; NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center FX F.G. acknowledges support from NSF grant AST-0607819. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. A.B. thanks Jay Gallagher for helpful conversations. NR 54 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2014 VL 790 IS 2 AR 89 DI 10.1088/0004-637X/790/2/89 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800006 ER PT J AU Mahapatra, DP Chutjian, A Machacek, JR Mangina, RS AF Mahapatra, D. P. Chutjian, A. Machacek, J. R. Mangina, R. S. TI SIZE DISTRIBUTION OF POSSIBLE DUST CARRIERS FOR THE EXTENDED RED EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction ID AROMATIC-HYDROCARBON CLUSTERS; SILICON NANOPARTICLES; BLUE LUMINESCENCE; INTERSTELLAR-MEDIUM; GRAINS; INJECTION; RECTANGLE; NGC-7023; SYSTEM AB Power-law size distributions expected to be applicable to possible carriers of extended red emission (ERE) have been examined using Monte Carlo (MC) simulations. Si nanoparticles and some polycyclic aromatic hydrocarbon complexes such as oligoacene and oligorylenes with energy gaps close to 2 eV have been considered. In the simplest case of unit quantum efficiency, the MC-generated size distributions are used to obtain photoluminescence (PL) spectra that are then corrected for dust extinction and reddening effects for comparison with observed ERE spectra. It is shown that a power-law size distribution with a decay exponent of alpha = 7/2, which closely agrees with starlight extinction data, fails to produce an ERE-like spectrum. However, size distributions with decay exponents of alpha = 19/12 and 3/2 are found to lead to acceptable spectra. Results indicate that energetic photon-induced breakup and competing aggregation effects dominate collisional effects in producing the observed steady-statemass distribution. It is shown that the peak wavelength of emission critically depends on the band gap, rather than cluster mass, which for oligoacenes and oligorylenes is widely different. The peak wavelength is also shown to be insensitive to dust attenuation. C1 [Mahapatra, D. P.; Chutjian, A.; Machacek, J. R.; Mangina, R. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mahapatra, DP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM ara.chutjian@jpl.nasa.gov RI Machacek, Joshua/A-5316-2011 FU NASA through the NASA Senior Research Associate Program FX We thank M. P. Das for helpful discussions. D.P.M. acknowledges support from NASA through the NASA Senior Research Associate Program managed by the Oak Ridge Associated Universities, USA. This research was carried out at JPL/Caltech under contract with the National Aeronautics and Space Administration. NR 31 TC 0 Z9 0 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2014 VL 790 IS 2 AR 140 DI 10.1088/0004-637X/790/2/140 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800057 ER PT J AU Ressler, SM Katsuda, S Reynolds, SP Long, KS Petre, R Williams, BJ Winkler, PF AF Ressler, Sean M. Katsuda, Satoru Reynolds, Stephen P. Long, Knox S. Petre, Robert Williams, Brian J. Winkler, P. Frank TI MAGNETIC FIELD AMPLIFICATION IN THE THIN X-RAY RIMS OF SN 1006 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; ISM: individual objects (SN 1006); ISM: magnetic fields; ISM: supernova remnants; X-rays: ISM ID YOUNG SUPERNOVA-REMNANTS; DIFFUSIVE SHOCK ACCELERATION; SMALL-SCALE STRUCTURE; PARTICLE-ACCELERATION; SYNCHROTRON EMISSION; CHANDRA OBSERVATIONS; NORTHEASTERN LIMB; MAXIMUM ENERGY; CASSIOPEIA-A; FILAMENTS AB Several young supernova remnants, including SN 1006, emit synchrotron X-rays in narrow filaments, hereafter thin rims, along their periphery. The widths of these rims imply 50-100 G fields in the region immediately behind the shock, far larger than expected for the interstellar medium compressed by unmodified shocks, assuming electron radiative losses limit rim widths. However, magnetic field damping could also produce thin rims. Here we review the literature on rim width calculations, summarizing the case for magnetic field amplification. We extend these calculations to include an arbitrary power-law dependence of the diffusion coefficient on energy, D. E. Loss-limited rim widths should shrink with increasing photon energy, while magnetic-damping models predict widths almost independent of photon energy. We use these results to analyze Chandra observations of SN 1006, in particular the southwest limb. We parameterize the FWHM in terms of energy as FWHM alpha E-nu(mE) Filament widths in SN 1006 decrease with energy; m(E) similar to -0.3 to -0.8, implying magnetic field amplification by factors of 10-50, above the factor of four expected in strong unmodified shocks. For SN 1006, the rapid shrinkage rules out magnetic damping models. It also favors short mean free paths (small diffusion coefficients) and strong dependence of D on energy (mu >= 1). C1 [Ressler, Sean M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Katsuda, Satoru] Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. [Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Petre, Robert; Williams, Brian J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. RP Ressler, SM (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. FU National Aeronautics and Space Administration through Chandra grant by the Chandra X-Ray Observatory Center [GO2-13066]; NASA [NAS8-03060] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra grant Number GO2-13066, 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 37 TC 11 Z9 11 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2014 VL 790 IS 2 AR 85 DI 10.1088/0004-637X/790/2/85 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800002 ER PT J AU Veilleux, S Teng, SH Rupke, DSN Maiolino, R Sturm, E AF Veilleux, S. Teng, S. H. Rupke, D. S. N. Maiolino, R. Sturm, E. TI HALF-MEGASECOND CHANDRA SPECTRAL IMAGING OF THE HOT CIRCUMGALACTIC NEBULA AROUND QUASAR MRK 231 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: starburst; ISM: jets and outflows; quasars: individual (Mrk 231); X-rays: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; X-RAY-EMISSION; ABSORPTION-LINE QUASAR; MERGER NGC 6240; XMM-NEWTON; INTERSTELLAR-MEDIUM; MOLECULAR OUTFLOWS; ELLIPTIC GALAXIES; STAR-FORMATION; CHEMICAL ENRICHMENT AB A deep 400 ks ACIS-S observation of the nearest quasar known, Mrk 231, is combined with archival 120 ks data to carry out the first ever spatially resolved spectral analysis of a hot X-ray-emitting circumgalactic nebula around a quasar. The 65 x 50 kpc X-ray nebula shares no resemblance with the tidal debris seen at optical wavelengths. One notable exception is the small tidal arc similar to 3.5 kpc south of the nucleus where excess soft X-ray continuum emission and Si XIII 1.8 keV line emission are detected, consistent with star formation and its associated alpha-element enhancement, respectively. An X-ray shadow is also detected at the location of the 15 kpc northern tidal tail. The hard X-ray continuum emission within similar to 6 kpc of the center is consistent with being due entirely to the bright central active galactic nucleus. The soft X-ray spectrum of the outer (greater than or similar to 6 kpc) portion of the nebula is best described as the sum of two thermal components with temperatures similar to 3 and similar to 8 million K and spatially uniform super-solar alpha-element abundances, relative to iron. This result implies enhanced star formation activity over similar to 10(8) yr, accompanied by redistribution of the metals on a large scale. The low-temperature thermal component is not present within similar to 6 kpc of the nucleus, suggesting extra heating in this region from the circumnuclear starburst, the central quasar, or the optically identified greater than or similar to 3 kpc quasar-driven outflow. The soft X-ray emission is weaker in the western quadrant, coincident with a deficit of H alpha and some of the largest columns of neutral gas outflowing from the nucleus. Shocks may heat the gas to high temperatures at this location, consistent with the tentative similar to 2 sigma detection of extended Fe XXV 6.7 keV line emission. C1 [Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Veilleux, S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Teng, S. H.] NASA Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Rupke, D. S. N.] Dept Phys, Rhodes Coll, Memphis, TN 38112 USA. [Maiolino, R.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Maiolino, R.] Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Sturm, E.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Veilleux, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM veilleux@astro.umd.edu OI Veilleux, Sylvain/0000-0002-3158-6820 FU NASA [GO2-13129X]; NASA Postdoctoral Program (NPP) Fellowship; Alexander von Humboldt Foundation FX We thank the anonymous referee for thoughtful and constructive comments that improved this paper. Support for this work was provided by NASA through Chandra contract GO2-13129X (S. V.) and the NASA Postdoctoral Program (NPP) Fellowship (S. H. T., S. V.). S. V. acknowledges support from the Alexander von Humboldt Foundation for a "renewed visit" to Germany and thanks the host institution, MPE Garching, where a portion of this paper was written. He is also grateful to R. Mushotzky for discussions of the interpretation of the elemental abundances. This work has made use of NASA's Astrophysics Data System Abstract Service and the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 104 TC 4 Z9 4 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2014 VL 790 IS 2 AR 116 DI 10.1088/0004-637X/790/2/116 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800033 ER PT J AU Whitaker, KE Rigby, JR Brammer, GB Gladders, MD Sharon, K Teng, SH Wuyts, E AF Whitaker, Katherine E. Rigby, Jane R. Brammer, Gabriel B. Gladders, Michael D. Sharon, Keren Teng, Stacy H. Wuyts, Eva TI RESOLVED STAR FORMATION ON SUB-GALACTIC SCALES IN A MERGER AT z=1.7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: interactions; galaxies: starburst; gravitational lensing: strong ID SIMILAR-TO 2; INITIAL MASS FUNCTION; H-II REGIONS; GRAVITATIONALLY LENSED GALAXIES; INTEGRAL FIELD SPECTROSCOPY; SUPERMASSIVE BLACK-HOLES; HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; LESS-THAN 1.5; FORMING GALAXIES AB We present a detailed analysis of Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) G141 grism spectroscopy for seven star-forming regions of the highly magnified lensed starburst galaxy RCSGA 032727-132609 at z = 1.704. We measure the spatial variations of the extinction in RCS0327 through the observed H gamma/H beta emission line ratios, finding a constant average extinction of E(B - V)(gas) = 0.40 +/- 0.07. We infer that the star formation is enhanced as a result of an ongoing interaction, with measured star formation rates derived from demagnified, extinction-corrected H beta line fluxes for the individual star-forming clumps falling >1-2 dex above the star formation sequence. When combining the HST/WFC3 [O III] lambda 5007/H beta emission line ratio measurements with [N II]/H alpha line ratios from Wuyts et al., we find that the majority of the individual star-forming regions fall along the local "normal" abundance sequence. With the first detections of the He I lambda 5876 and He II lambda 4686 recombination lines in a distant galaxy, we probe the massive-star content of the star-forming regions in RCS0327. The majority of the star-forming regions have a He I lambda 5876 to H beta ratio consistent with the saturated maximum value, which is only possible if they still contain hot O-stars. Two regions have lower ratios, implying that their last burst of new star formation ended similar to 5 Myr ago. Together, the He I lambda 5876 and He II lambda 4686 to H beta line ratios provide indirect evidence for the order in which star formation is stopping in individual star-forming knots of this high-redshift merger. We place the spatial variations of the extinction, star formation rate and ionization conditions in the context of the star formation history of RCS0327. C1 [Whitaker, Katherine E.; Rigby, Jane R.; Teng, Stacy H.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Brammer, Gabriel B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gladders, Michael D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Gladders, Michael D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Sharon, Keren] Univ Michigan, Dept Astron & Astrophys, Ann Arbor, MI 48109 USA. [Wuyts, Eva] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. RP Whitaker, KE (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA. EM kate.whitaker@nasa.gov RI Rigby, Jane/D-4588-2012; OI Rigby, Jane/0000-0002-7627-6551; Brammer, Gabriel/0000-0003-2680-005X FU NASA Postdoctoral Program at the Goddard Space Flight Center; NASA [NAS 5-26555, NAS5-26555]; NASA from the Space Telescope Science Institute [12726] FX The authors acknowledge Alaina Henry for insightful discussions, and Alejo Stark for his help with the AGN analysis. We thank the anonymous referee for useful comments and a careful reading of the paper. K.E.W. is supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This research is based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program 12726. Support for program number 12726 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. We thank Gary Ferland and Claus Leitherer for making the Cloudy and Starbust99 tools publicly available. NR 115 TC 10 Z9 10 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2014 VL 790 IS 2 AR 143 DI 10.1088/0004-637X/790/2/143 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800060 ER PT J AU Williams, BJ Borkowski, KJ Reynolds, SP Ghavamian, P Raymond, JC Long, KS Blair, WP Sankrit, R Winkler, PF Hendrick, SP AF Williams, Brian J. Borkowski, Kazimierz J. Reynolds, Stephen P. Ghavamian, Parviz Raymond, John C. Long, Knox S. Blair, William P. Sankrit, Ravi Winkler, P. Frank Hendrick, Sean P. TI SPITZER OBSERVATIONS OF THE TYPE IA SUPERNOVA REMNANT N103B: KEPLER'S OLDER COUSIN? SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: supernova remnants ID LARGE-MAGELLANIC-CLOUD; RESOLUTION X-RAY; SN 1006; COSMIC SILICATES; DUST; PROGENITOR; EMISSION; STARS; SHOCK; IDENTIFICATION AB We report results from Spitzer observations of SNR 0509-68.7, also known as N103B, a young Type Ia supernova remnant (SNR) in the Large Magellanic Cloud (LMC) that shows interaction with a dense medium in its western hemisphere. Our images show that N103B has strong IR emission from warm dust in the post-shock environment. The post-shock gas density we derive, 45 cm(-3), is much higher than in other Type Ia remnants in the LMC, though a lack of spatial resolution may bias measurements toward regions of higher than average density. This density is similar to that in Kepler's SNR, a Type Ia interacting with a circumstellar medium (CSM). Optical images show Ha emission along the entire periphery of the western portion of the shock, with [O III] and [S II] lines emitted from a few dense clumps of material where the shock has become radiative. The dust is silicate in nature, though standard silicate dust models fail to reproduce the "18 mu m" silicate feature that peaks instead at 17.3 mu m. We propose that the dense material is circumstellar material lost from the progenitor system, as with Kepler. If the CSM interpretation is correct, this remnant would become the second member, along with Kepler, of a class of Type Ia remnants characterized by interaction with a dense CSM hundreds of years post-explosion. A lack of N enhancement eliminates symbiotic asymptotic giant branch progenitors. The white dwarf companion must have been relatively unevolved at the time of the explosion. C1 [Williams, Brian J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Ghavamian, Parviz] Towson Univ, Dept Phys Chem & Geosci, Towson, MD 21252 USA. [Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Long, Knox S.] STScI, Baltimore, MD 21218 USA. [Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Sankrit, Ravi] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. [Hendrick, Sean P.] Millersville Univ Pennsylvania, Dept Phys, Millersville, PA 17551 USA. RP Williams, BJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM brian.j.williams@nasa.gov FU Spitzer Guest Observer [RSA 1265236, RSA 1328682] FX We thank R. Chris Smith for providing the optical images from CTIO. This work was supported through Spitzer Guest Observer Grants RSA 1265236 and RSA 1328682. NR 54 TC 7 Z9 7 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2014 VL 790 IS 2 AR 139 DI 10.1088/0004-637X/790/2/139 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800056 ER PT J AU Suggs, RM Moser, DE Cooke, WJ Suggs, RJ AF Suggs, R. M. Moser, D. E. Cooke, W. J. Suggs, R. J. TI The flux of kilogram-sized meteoroids from lunar impact monitoring SO ICARUS LA English DT Article DE Meteors; Moon; Photometry; Near-Earth Objects; Cratering ID CAMERA NETWORK; MOON; FLASHES; EARTH; STREAMS; SURFACE; SEARCH; STARS AB The flashes from meteoroid impacts on the Moon are useful in determining the flux of impactors with masses as low as a few tens of grams. A routine monitoring program at NASA's Marshall Space Flight Center has recorded over 300 impacts since 2006. A selection of 126 flashes recorded during periods of photometric skies was analyzed, creating the largest and most homogeneous dataset of lunar impact flashes to date. Standard CCD photometric techniques were applied to the video and the luminous energy, kinetic energy, and mass are estimated for each impactor. Shower associations were determined for most of the impactors and a range of luminous efficiencies was considered. The flux to a limiting energy of 2.5 x 10(-6) kT TNT or 1.05 x 10(7) J is 1.03 x 10(-7) km(-2) h(-1) and the flux to a limiting mass of 30 g is 6.14 x 10(-1) m(-2) yr(-1) at the Moon. Comparisons made with measurements and models of the meteoroid population indicate that the flux of objects in this size range is slightly lower (but within the error bars) than flux at this size from the power law distribution determined for the near Earth object and fireball population by Brown et al. (Brown, P.G., Spalding, R., ReVelle, D., Tagliaferri, E., Worden, S. [2002]. Nature 420, 294-296). Size estimates for the crater detected by Lunar Reconnaissance Orbiter from a large impact observed on March 17, 2013 are also briefly discussed. Published by Elsevier Inc. C1 [Suggs, R. M.; Cooke, W. J.; Suggs, R. J.] NASA, George C Marshall Space Flight Ctr, Meteoroid Environm Off, Nat Environm Branch, Huntsville, AL 35812 USA. [Moser, D. E.] MITS Dynet, George C Marshall Space Flight Ctr, Meteoroid Environm Off, Nat Environm Branch, Huntsville, AL 35812 USA. RP Suggs, RM (reprint author), NASA, George C Marshall Space Flight Ctr, Meteoroid Environm Off, Nat Environm Branch, EV44 Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM rob.suggs@nasa.gov FU NASA Meteoroid Environment Office, Marshall Space Flight Center Engineering Directorate; International Space Station Program, Constellation Program; Space Shuttle Program FX The authors gratefully acknowledge the NASA Meteoroid Environment Office, Marshall Space Flight Center Engineering Directorate, the International Space Station Program, Constellation Program, and Space Shuttle Program for financial support for this work. We appreciate the dedication of the following personnel who operated the telescopes and helped analyze the data: Richard Altstatt, Victoria Coffey, Anne Diekmann, Heather Koehler, and Leigh Smith. We also thank Peter Gural for providing the LunarScan software which was essential in performing this work and Rhiannon Blaauw who developed the meteor shower catalog for us. Thanks also to George Varros and Dave Clark for independent confirmation of 3 of the flashes. We owe a huge debt of gratitude to Wesley Swift who helped assemble the observatories and developed the initial photometric analysis software as well as collecting and analyzing some of the data. NR 62 TC 16 Z9 16 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 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2014 VL 238 BP 23 EP 36 DI 10.1016/j.icarus.2014.04.032 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL8CV UT WOS:000339366400003 ER PT J AU Burger, MH Killen, RM McClintock, WE Merkel, AW Vervack, RJ Cassidy, TA Sarantos, M AF Burger, Matthew H. Killen, Rosemary M. McClintock, William E. Merkel, Aimee W. Vervack, Ronald J., Jr. Cassidy, Timothy A. Sarantos, Menelaos TI Seasonal variations in Mercury's dayside calcium exosphere SO ICARUS LA English DT Article DE Mercury; Mercury, atmosphere; Spectroscopy; Atmospheres, structure ID INPUT FUNCTION; SODIUM; ATMOSPHERE; IMPACTS; MODEL; FLUX AB The Mercury Atmospheric and Surface Composition Spectrometer on the MESSENGER spacecraft has observed calcium emission in Mercury's exosphere on a near-daily basis since March 2011. During MESSENGER's primary and first extended missions (March 2011 - March 2013) the dayside calcium exosphere was measured over eight Mercury years. We have simulated these data with a Monte Carlo model of exospheric source processes to show that (a) there is a persistent source of energetic calcium located in the dawn equatorial region, (b) there is a seasonal dependence in the calcium source rate, and (c) there are no obvious year-to-year variations in the near-surface dayside calcium exosphere. (C) 2014 Elsevier Inc. All rights reserved. C1 [Burger, Matthew H.] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21251 USA. [Killen, Rosemary M.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McClintock, William E.; Merkel, Aimee W.; Cassidy, Timothy A.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Vervack, Ronald J., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Sarantos, Menelaos] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA. RP Burger, MH (reprint author), Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21251 USA. EM Matthew.Burger@nasa.gov RI Vervack, Ronald/C-2702-2016 OI Vervack, Ronald/0000-0002-8227-9564 NR 27 TC 14 Z9 14 U1 2 U2 9 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 AUG PY 2014 VL 238 BP 51 EP 58 DI 10.1016/j.icarus.2014.04.049 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL8CV UT WOS:000339366400005 ER PT J AU Zimmerman, MI Farrell, WM Poppe, AR AF Zimmerman, M. I. Farrell, W. M. Poppe, A. R. TI Grid-free 2D plasma simulations of the complex interaction between the solar wind and small, near-Earth asteroids SO ICARUS LA English DT Article DE Asteroids; Solar wind ID LUNAR PHOTOELECTRON SHEATH; PONDED DEPOSITS; DUST; VACUUM; EXPANSION; 433-EROS; SPACE; MOON; WAKE AB We present results from a new grid-free 2D plasma simulation code applied to a small, unmagnetized body immersed in the streaming solar wind plasma. The body was purposely modeled as an irregular shape in order to examine photoemission and solar wind plasma flow in high detail on the dayside, night-side, terminator and surface-depressed 'pocket' regions. Our objective is to examine the overall morphology of the various plasma interaction regions that form around a small body like a small near-Earth asteroid (NEA). We find that the object obstructs the solar wind flow and creates a trailing wake region downstream, which involves the interplay between surface charging and ambipolar plasma expansion. Photoemission is modeled as a steady outflow of electrons from illuminated portions of the surface, and under direct illumination the surface forms a non-monotonic or "double-sheath" electric potential upstream of the body, which is important for understanding trajectories and equilibria of lofted dust grains in the presence of a complex asteroid geometry. The largest electric fields are found at the terminators, where ambipolar plasma expansion in the body-sized nightside wake merges seamlessly with the thin photoelectric sheath on the dayside. The pocket regions are found to be especially complex, with nearby sunlit regions of positive potential electrically connected to unlit negative potentials and forming adjacent natural electric dipoles. For objects near the surface, we find electrical dissipation times (through collection of local environmental solar wind currents) that vary over at least 5 orders of magnitude: from 39 mu s inside the near-surface photoelectron cloud under direct sunlight to >> 1 s inside the particle-depleted nightside wake and shadowed pocket regions. (C) 2014 Elsevier Inc. All rights reserved. C1 [Zimmerman, M. I.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Poppe, A. R.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Zimmerman, M. I.; Farrell, W. M.; Poppe, A. R.] NASA, Lunar Sci Inst, Ames Res Ctr, Moffett Field, CA 94089 USA. RP Zimmerman, MI (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM Michael.Zimmerman@jhuapl.edu RI Farrell, William/I-4865-2013 FU NASA; NASA Lunar Science Institute; DREAM Virtual Institute [NNX09AG78A] 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. Support by the NASA Lunar Science Institute and DREAM Virtual Institute through Grant NNX09AG78A are gratefully acknowledged. M. Zimmerman thanks W. Farrell and T. Stubbs at NASA/GSFC for providing additional computing resources. NR 41 TC 4 Z9 4 U1 0 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2014 VL 238 BP 77 EP 85 DI 10.1016/j.icarus.2014.02.029 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL8CV UT WOS:000339366400008 ER PT J AU Fletcher, LN Greathouse, TK Orton, GS Irwin, PGJ Mousis, O Sinclair, JA Giles, RS AF Fletcher, Leigh N. Greathouse, T. K. Orton, G. S. Irwin, P. G. J. Mousis, O. Sinclair, J. A. Giles, R. S. TI The origin of nitrogen on Jupiter and Saturn from the N-15/N-14 ratio SO ICARUS LA English DT Article DE Jupiter; Saturn; Atmospheres, composition ID PROBE MASS-SPECTROMETER; GIANT PLANETS; CASSINI/CIRS OBSERVATIONS; CLOUD STRUCTURE; SOLAR-SYSTEM; ISOTOPIC FRACTIONATION; JOVIAN ATMOSPHERE; TITANS ATMOSPHERE; UPPER TROPOSPHERE; VOLATILES AB The Texas Echelon cross Echelle Spectrograph (TEXES), mounted on NASA's Infrared Telescope Facility (IRTF), was used to map mid-infrared ammonia absorption features on both Jupiter and Saturn in February 2013. Ammonia is the principle reservoir of nitrogen on the giant planets, and the ratio of isotopologues (N-15/N-14) can reveal insights into the molecular carrier (e.g., as N-2 or NH3) of nitrogen to the forming protoplanets, and hence the source reservoirs from which these worlds accreted. We targeted two spectral intervals (900 and 960 cm(-1)) that were relatively clear of terrestrial atmospheric contamination and contained close features of (NH3)-N-14 and (NH3)-N-15, allowing us to derive the ratio from a single spectrum without ambiguity due to radiometric calibration (the primary source of uncertainty in this study). We present the first ground-based determination of Jupiter's N-15/N-14 ratio (in the range from 1.4 x 10(-3) to 2.5 x 10(-3)), which is consistent with both previous space-based studies and with the primordial value of the protosolar nebula. On Saturn, we present the first upper limit on the N-15/N-14 ratio of no larger than 2.0 x 10(-3) for the 900-cm(-1) channel and a less stringent requirement that the ratio be no larger than 2.8 x 10(-3) for the 960-cm(-1) channel (1 sigma-confidence). Specifically, the data rule out strong N-15-enrichments such as those observed in Titan's atmosphere and in cometary nitrogen compounds. To the extent possible with ground-based radiometric uncertainties, the saturnian and jovian N-15/N-14 ratios appear indistinguishable, implying that N-15-enriched ammonia ices could not have been a substantial contributor to the bulk nitrogen inventory of either planet. This result favours accretion of primordial N-2 on both planets, either in the gas phase from the solar nebula, or as ices formed at very low temperatures. Finally, spatially-resolved TEXES observations are used to derive zonal contrasts in tropospheric temperatures, phosphine and (NH3)-N-14 on both planets, allowing us to relate thermal conditions and chemical compositions to phenomena observed at visible wavelengths in 2013 (e.g., Jupiter's faint equatorial red colouration event and wave activity in the equatorial belts, plus the remnant warm band on Saturn following the 2010-11 springtime storm). (C) 2014 Elsevier Inc. All rights reserved. C1 [Fletcher, Leigh N.; Irwin, P. G. J.; Sinclair, J. A.; Giles, R. S.] Univ Oxford, Clarendon Lab, Dept Phys, Oxford OX1 3PU, England. [Greathouse, T. K.] SW Res Inst, Div 15, San Antonio, TX 78228 USA. [Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mousis, O.] Univ Franche Comte, Inst UTINAM, CNRS INSU, UMR 6213, F-25030 Besancon, France. RP Fletcher, LN (reprint author), Univ Oxford, Clarendon Lab, Dept Phys, Parks Rd, Oxford OX1 3PU, England. EM fletcher@atm.ox.ac.uk RI Fletcher, Leigh/D-6093-2011; OI Fletcher, Leigh/0000-0001-5834-9588; Irwin, Patrick/0000-0002-6772-384X; Giles, Rohini/0000-0002-7665-6562 FU Royal Society Research Fellowship at the University of Oxford; National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program [NNX-08AE38A]; Science and Technology Facilities Council (STFC); CNES; NASA FX Fletcher was supported by a Royal Society Research Fellowship at the University of Oxford. Fletcher, Greathouse and Orton were visiting astronomers at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement No. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. The UK authors acknowledge the support of the Science and Technology Facilities Council (STFC). Mousis acknowledges support from CNES. A portion of this work was performed by Orton at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. We are extremely grateful to John Lacy and Matt Richter for their assistance in understanding the performance of the TEXES instrument and the uncertainties related to calibration, and to Tobias Owen for helpful discussions. We thank Thierry Fouchet and one anonymous reviewer for their helpful critiques of the manuscript. NR 75 TC 10 Z9 10 U1 3 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2014 VL 238 BP 170 EP 190 DI 10.1016/j.icarus.2014.05.007 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL8CV UT WOS:000339366400015 ER PT J AU Altobelli, N Lopez-Paz, D Pilorz, S Spilker, LJ Morishima, R Brooks, S Leyrat, C Deau, E Edgington, S Flandes, A AF Altobelli, Nicolas Lopez-Paz, David Pilorz, S. Spilker, Linda J. Morishima, R. Brooks, S. Leyrat, C. Deau, E. Edgington, S. Flandes, A. TI Two numerical models designed to reproduce Saturn ring temperatures as measured by Cassini-CIRS SO ICARUS LA English DT Article DE Saturn, rings; Planetary rings; Infrared observations ID THERMAL INFRARED-EMISSION; DENSE PLANETARY RINGS; SELF-GRAVITY WAKES; MAIN RINGS; MULTILAYER MODEL; SOLAR ELEVATION; VIMS; SIMULATIONS; PARTICLES; DEPENDENCE AB We present two numerical models designed to reproduce the temperatures of the illuminated Saturn rings as measured by the CASSINI-CIRS instrument. Our models are constrained by all available temperature measurements performed on the illuminated rings since SOI. Both models reproduce well the variations of temperature under any illumination and observation geometry. One model is derived from a purely numerical data mining approach, relying on the implementation of a Neural Network that treats the data set globally. This model is used as a test of coverage completeness of the observational parameter space, driving our ability to characterize the rings thermal response. The second (analytical) model is derived using simple physical considerations, by treating the rings as a surface rather than as a collection of individual particles, combined with an empirical anisotropy function to describe the temperature resulting from the Sun's and Saturn's heating. The thermal response of this ring-surface is parameterized by its Bond albedo and emissivity, thermal relaxation time and a set of geometrical parameters quantifying the anisotropy of the temperature measurements depending on azimuth and elevation of the observer with respect to the ring plane, as well as on the solar elevation. Both models provide formulae to predict the ring temperature, that will ease the benchmarking of future physical models against data. The physical model is applied to fit the temperature of tens of different radial slices, allowing us to constrain the combined emissivity and albedo, thermal relaxation time and anisotropy parameters of the ring slabs with the highest radial resolution achieved so far with CIRS. Using for the first time all observation geometries available for illuminated rings, we are confident that our values are as unbiased as possible against observation geometry. The thermal relaxation time appears to be short, a few tens of minutes, and independent of the radial distance across the whole ring. A study of the temperature anisotropy suggests inter-particle shadowing is important in the B ring and in the outer A ring regions. (C) 2014 Elsevier Inc. All rights reserved. C1 [Altobelli, Nicolas; Lopez-Paz, David] ESA ESAC, Madrid, Spain. [Pilorz, S.; Spilker, Linda J.; Morishima, R.; Brooks, S.; Deau, E.; Edgington, S.; Flandes, A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Leyrat, C.] Observ Paris, F-75014 Paris, France. RP Altobelli, N (reprint author), ESA ESAC, Madrid, Spain. EM nicolas.altobelli@sciops.esa.int NR 33 TC 3 Z9 3 U1 1 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2014 VL 238 BP 205 EP 220 DI 10.1016/j.icarus.2014.04.031 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL8CV UT WOS:000339366400017 ER PT J AU Beck, J Welch, T Mitra, P Reiff, K Sun, XL Abshire, J AF Beck, Jeff Welch, Terry Mitra, Pradip Reiff, Kirk Sun, Xiaoli Abshire, James TI A Highly Sensitive Multi-element HgCdTe e-APD Detector for IPDA Lidar Applications SO JOURNAL OF ELECTRONIC MATERIALS LA English DT Article DE HgCdTe; APD; NEP; IPDA; CO2; lidar ID ELECTRON AVALANCHE PHOTODIODE AB An HgCdTe electron avalanche photodiode (e-APD) detector has been developed for lidar receivers, one application of which is integrated path differential absorption lidar measurements of such atmospheric trace gases as CO2 and CH4. The HgCdTe APD has a wide, visible to mid-wave-infrared, spectral response, high dynamic range, substantially improved sensitivity, and an expected improvement in operational lifetime. A demonstration sensor-chip assembly consisting of a 4.3 mu m cutoff HgCdTe 4 x 4 APD detector array with 80 mu m pitch pixels and a custom complementary metal-oxide-semiconductor readout integrated circuit was developed. For one typical array the APD gain was 654 at 12 V with corresponding gain normalized dark currents ranging from 1.2 fA to 3.2 fA. The 4 x 4 detector system was characterized at 77 K with a 1.55 mu m wavelength, 1 mu s wide, laser pulse. The measured unit gain detector photon conversion efficiency was 91.1%. At 11 V bias the mean measured APD gain at 77 K was 307.8 with sigma/mean uniformity of 1.23%. The average, noise-bandwidth normalized, system noise-equivalent power (NEP) was 1.04 fW/Hz(1/2) with a sigma/mean of 3.8%. The measured, electronics-limited, bandwidth of 6.8 MHz was more than adequate for 1 mu s pulse detection. The system had an NEP (3 MHz) of 0.4 fW/Hz(1/2) at 12 V APD bias and a linear dynamic range close to 1000. A gain-independent quantum-limited SNR of 80% of full theoretical was indicative of a gain-independent excess noise factor very close to 1.0 and the expected APD mode quantum efficiency. C1 [Beck, Jeff; Welch, Terry; Mitra, Pradip] DRS Technol Inc, Grp C4ISR, Dallas, TX 75243 USA. [Reiff, Kirk] Analog Digital Integrated Circuits, Longwood, FL USA. [Sun, Xiaoli; Abshire, James] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Beck, J (reprint author), DRS Technol Inc, Grp C4ISR, Dallas, TX 75243 USA. EM jeff.beck@drs.com FU NASA ESTO IIP-10 program FX The authors would like to acknowledge the important contributions of DRS employees James McCurdy (testing), Chris Kamilar (electronics), Mark Skokan (fanout array design), Richard Scritchfield (consulting), Drew Gordon (software), Patty Benken (array fabrication), and Towfik Teherani (management support). This work was supported by the NASA ESTO IIP-10 program managed by Parminder Ghuman and Irene Bibyk. NR 8 TC 5 Z9 5 U1 1 U2 22 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0361-5235 EI 1543-186X J9 J ELECTRON MATER JI J. Electron. Mater. PD AUG PY 2014 VL 43 IS 8 BP 2970 EP 2977 DI 10.1007/s11664-014-3164-8 PG 8 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA AL7SH UT WOS:000339334800028 ER PT J AU Downs, ME Hackney, KJ Martin, D Caine, TL Cunningham, D O'Connor, DP Ploutz-Snyder, LL AF Downs, Meghan E. Hackney, Kyle J. Martin, David Caine, Timothy L. Cunningham, David O'Connor, Daniel P. Ploutz-Snyder, Lori L. TI Acute Vascular and Cardiovascular Responses to Blood Flow-Restricted Exercise SO MEDICINE AND SCIENCE IN SPORTS AND EXERCISE LA English DT Article DE BLOOD FLOW-RESTRICTED EXERCISE; ARTERIAL BLOOD FLOW; CARDIOVASCULAR RESPONSE TO RESISTANCE EXERCISE; HEMODYNAMIC RESPONSE TO RESISTANCE EXERCISE ID INTENSITY RESISTANCE EXERCISE; NEAR-INFRARED SPECTROSCOPY; MUSCLE METABOREFLEX; NONINVASIVE MEASUREMENT; ARTERIAL STIFFNESS; DOPPLER ULTRASOUND; INDOCYANINE GREEN; DYNAMIC EXERCISE; CARDIAC-OUTPUT; PRESSOR REFLEX AB Blood flow-restricted resistance exercise improves muscle strength; however, the cardiovascular response is not well understood. Purpose: This investigation measured local vascular responses, tissue oxygen saturation (StO(2)), and cardiovascular responses during supine unilateral leg press and heel raise exercise in four conditions: high load with no occlusion cuff, low load with no occlusion cuff, and low load with occlusion cuff pressure set at 1.3 times resting diastolic blood pressure (BFRDBP) or at 1.3 times resting systolic blood pressure (BFRSBP). Methods: Subjects (N = 13) (men/women, 5/8, 31.8 +/- 12.5 yr, 68.3 +/- 12.1 kg, mean +/- SD) performed three sets of leg press and heel raise to fatigue with 90-s rest. Artery diameter, velocity time integral, and stroke volume were measured using two-dimensional and Doppler ultrasound at rest and immediately after exercise. HR was monitored using a three-lead ECG. Finger blood pressure was acquired by photoplethysmography. Vastus lateralis StO(2) was measured using near-infrared spectroscopy. A repeated-measures ANOVA was used to analyze exercise work and StO(2). Multilevel modeling was used to evaluate the effect of exercise condition on vascular and cardiovascular variables. Statistical significance was set a priori at P < 0.05. Results: Artery diameter did not change from baseline during any of the exercise conditions. Blood flow increased after exercise in each condition except BFRSBP. StO(2) decreased during exercise and recovered to baseline levels during rest only in low load with no occlusion cuff and high load with no occlusion cuff. HR, stroke volume, and cardiac output (Q) over dot responses to exercise were blunted in blood flow-restricted exercise. Blood pressure was elevated during rest intervals in blood flow-restricted exercise. Conclusions: Our results demonstrate that cuff pressure alters the hemodynamic responses to resistance exercise. These findings warrant further evaluations in individuals presenting cardiovascular risk factors. C1 [Downs, Meghan E.; O'Connor, Daniel P.] Univ Houston, Dept Hlth & Human Performance, Houston, TX USA. [Hackney, Kyle J.; Martin, David; Caine, Timothy L.] Wyle Sci Technol & Engn Grp, Human Performance & Engn Div, Houston, TX USA. [Hackney, Kyle J.] Syracuse Univ, Dept Exercise Sci, Syracuse, NY USA. [Cunningham, David; Ploutz-Snyder, Lori L.] Univ Space Res Assoc, Houston, TX USA. RP Ploutz-Snyder, LL (reprint author), NASA, Johnson Space Ctr, 2101 NASA Pkwy,B261,SK3, Houston, TX 77058 USA. EM lori.ploutz-snyder-1@nasa.gov FU National Aeronautics and Space Administration-Human Research Program FX This study was funded by the National Aeronautics and Space Administration-Human Research Program. NR 45 TC 8 Z9 8 U1 6 U2 30 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0195-9131 EI 1530-0315 J9 MED SCI SPORT EXER JI Med. Sci. Sports Exerc. PD AUG PY 2014 VL 46 IS 8 BP 1489 EP 1497 DI 10.1249/MSS.0000000000000253 PG 9 WC Sport Sciences SC Sport Sciences GA AL6RF UT WOS:000339259700003 PM 24389514 ER PT J AU Saylor, RD Wolfe, GM Meyers, TP Hicks, BB AF Saylor, Rick D. Wolfe, Glenn M. Meyers, Tilden P. Hicks, Bruce B. TI A corrected formulation of the Multi layer Model (MLM) for inferring gaseous dry deposition to vegetated surfaces SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Dry deposition; Nitric acid; Sulfur dioxide; Ozone; Multi-layer model; Canopy; CASTNet ID IONIZATION MASS-SPECTROMETER; CLEAN-AIR STATUS; TRENDS NETWORK; HNO3; ATMOSPHERE; SULFUR AB The Multilayer Model (MLM) has been used for many years to infer dry deposition fluxes from measured trace species concentrations and standard meteorological measurements for national networks in the U.S., including the U.S. Environmental Protection Agency's Clean Air Status and Trends Network (CASTNet). MLM utilizes a resistance analogy to calculate deposition velocities appropriate for whole vegetative canopies, while employing a multilayer integration to account for vertically varying meteorology, canopy morphology and radiative transfer within the canopy. However, the MLM formulation, as it was originally presented and as it has been subsequently employed, contains a non-physical representation related to the leaf-level quasi-laminar boundary layer resistance that affects the calculation of the total canopy resistance. In this note, the non-physical representation of the canopy resistance as originally formulated in MLM is discussed and a revised, physically consistent, formulation is suggested as a replacement. The revised canopy resistance formulation reduces estimates of HNO3 deposition velocities by as much as 38% during mid-day as compared to values generated by the original formulation. Inferred deposition velocities for SO2 and O-3 are not significantly altered by the change in formulation (<3%). Inferred deposition loadings of oxidized and total nitrogen from CASTNet data may be reduced by 10 20% and 5-10%, respectively, for the Eastern U. S. when employing the revised formulation of MLM as compared to the original formulation. Published by Elsevier Ltd. This is an open access article under the CC BY license (http://creativecommons.org/licenses/by/3.0/). C1 [Saylor, Rick D.; Meyers, Tilden P.] NOAA, Air Resources Lab, Atmospher Turbulence & Diffus Div, Oak Ridge, TN 37830 USA. [Wolfe, Glenn M.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. [Wolfe, Glenn M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Hicks, Bruce B.] Metcorps, Norris, TN 37828 USA. RP Saylor, RD (reprint author), NOAA, Air Resources Lab, Atmospher Turbulence & Diffus Div, 456 S Illinois Ave, Oak Ridge, TN 37830 USA. EM Rick.Saylor@noaa.gov RI Wolfe, Glenn/D-5289-2011; Meyers, Tilden/C-6633-2016 FU U.S. Weather Research Program within the NOAA/OAR Office of Weather and Air Quality FX One author (RS) performed this work with support from the U.S. Weather Research Program within the NOAA/OAR Office of Weather and Air Quality. NR 21 TC 3 Z9 3 U1 2 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD AUG PY 2014 VL 92 BP 141 EP 145 DI 10.1016/j.atmosenv.2014.03.056 PG 5 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AL0IO UT WOS:000338810800015 ER PT J AU Lee, J Kim, J Lee, YG AF Lee, Jaehwa Kim, Jhoon Lee, Yun Gon TI Simultaneous retrieval of aerosol properties and clear-sky direct radiative effect over the global ocean from MODIS SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Aerosol; Direct radiative effect; Radiative forcing; Ocean; MODIS ID OPTICAL-PROPERTIES; ATMOSPHERE; CERES; TOP; INSTRUMENT; AERONET AB A unified satellite algorithm is presented to simultaneously retrieve aerosol properties (aerosol optical depth; AOD and aerosol type) and clear-sky shortwave direct radiative effect (hereafter, DREA) over ocean. The algorithm is applied to Moderate Resolution Imaging spectroradiometer (MODIS) observations for a period from 2003 to 2010 to assess the DREA over the global ocean. The simultaneous retrieval utilizes lookup table (LUT) containing both spectral reflectances and solar irradiances calculated using a single radiative transfer model with the same aerosol input data. This study finds that aerosols cool the top-of-atmosphere (TOA) and bottom-of-atmosphere (BOA) by 5.2 +/- 0.5 W/m(2) and 8.3 W/m(2), respectively, and correspondingly warm the atmosphere (hereafter, ATM) by 3.1 W/m(2). These quantities, solely based on the MODIS observations, are consistent with those of previous studies incorporating chemical transport model simulations and satellite observations. However, the DREAs at BOA and ATM are expected to be less accurate compared to that of TOA due to low sensitivity in retrieving aerosol type information, which is related with the atmospheric heating by aerosols, particularly in low AOD conditions; consequently, the uncertainties could not be quantified. Despite the issue in the aerosol type information, the present method allows us to confine the DREA attributed only to fine-mode dominant aerosols, which are expected to be mostly anthropogenic origin, in the range from -1.1 W/m(2) to -1.3 W/m(2) at TOA. Improvements in size-resolved AOD and SSA retrievals from current and upcoming satellite instruments are suggested to better assess the DREA, particularly at BOA and ATM, where aerosol absorptivity induces substantial uncertainty. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Lee, Jaehwa; Kim, Jhoon; Lee, Yun Gon] Yonsei Univ, Inst Earth Astron & Atmosphere, Dept Atmospher Sci, Brain Korea Program 21, Seoul 120749, South Korea. [Lee, Jaehwa] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Lee, Jaehwa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lee, Yun Gon] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea. RP Kim, J (reprint author), Yonsei Univ, Inst Earth Astron & Atmosphere, Dept Atmospher Sci, Brain Korea Program 21, Seoul 120749, South Korea. EM jhoonkim1@gmail.com OI Lee, Jaehwa/0000-0002-5029-476X FU Korea Meteorological Administration Research and Development Program [CATER 2012-2065]; Brain Korea 21 (BK21) program FX We thank the MODIS science team for providing valuable data used in this study. We also thank the principal investigators and their staff for establishing and maintaining the AERONET sites used in this investigation. This work was supported by the Korea Meteorological Administration Research and Development Program under Grant CATER 2012-2065. This research was partially supported by the Brain Korea 21 (BK21) program for Jhoon Kim and Jaehwa Lee. NR 25 TC 2 Z9 2 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD AUG PY 2014 VL 92 BP 309 EP 317 DI 10.1016/j.atmosenv.2014.04.021 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AL0IO UT WOS:000338810800033 ER PT J AU Flynn, CM Pickering, KE Crawford, JH Lamsal, L Krotkov, N Herman, J Weinheimer, A Chen, G Liu, X Szykman, J Tsay, SC Loughner, C Hains, J Lee, P Dickerson, RR Stehr, JW Brent, L AF Flynn, Clare M. Pickering, Kenneth E. Crawford, James H. Lamsal, Lok Krotkov, Nickolay Herman, Jay Weinheimer, Andrew Chen, Gao Liu, Xiong Szykman, James Tsay, Si-Chee Loughner, Christopher Hains, Jennifer Lee, Pius Dickerson, Russell R. Stehr, Jeffrey W. Brent, Lacey TI Relationship between column-density and surface mixing ratio: Statistical analysis of O-3 and NO2 data from the July 2011 Maryland DISCOVER-AQ mission SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Ozone; Nitrogen oxides; DISCOVER-AQ; Column-surface relationship; Aircraft measurement campaign; Measurement-model comparison ID TROPOSPHERIC OZONE; AIR-POLLUTANTS; UNITED-STATES; PART I; MODEL; SATELLITE; POLLUTION; LAYER; OMI AB To investigate the ability of column (or partial column) information to represent surface air quality, results of linear regression analyses between surface mixing ratio data and column abundances for O-3 and NO2 are presented for the July 2011 Maryland deployment of the DISCOVER-AQ mission. Data collected by the P-3B aircraft, ground-based Pandora spectrometers, Aura/OMI satellite instrument, and simulations for July 2011 from the CMAQ air quality model during this deployment provide a large and varied data set, allowing this problem to be approached from multiple perspectives. O-3 columns typically exhibited a statistically significant and high degree of correlation with surface data (R-2 > 0.64) in the P-3B data set, a moderate degree of correlation (0.16 < R-2 < 0.64) in the CMAQ data set, and a low degree of correlation (R-2 < 0.16) in the Pandora and OMI data sets. NO2 columns typically exhibited a low to moderate degree of correlation with surface data in each data set. The results of linear regression analyses for O-3 exhibited smaller errors relative to the observations than NO2 regressions. These results suggest that O-3 partial column observations from future satellite instruments with sufficient sensitivity to the lower troposphere can be meaningful for surface air quality analysis. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Flynn, Clare M.; Pickering, Kenneth E.; Dickerson, Russell R.; Stehr, Jeffrey W.; Brent, Lacey] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Pickering, Kenneth E.; Krotkov, Nickolay; Tsay, Si-Chee] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Crawford, James H.; Chen, Gao] NASA Langley Res Ctr, Hampton, VA USA. [Lamsal, Lok] NASA Goddard Space Flight Ctr, GESTAR, Greenbelt, MD USA. [Herman, Jay] NASA Goddard Space Flight Ctr, UMBC, Greenbelt, MD USA. [Weinheimer, Andrew] NCAR Atmospher Chem Div, Boulder, CO USA. [Liu, Xiong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Szykman, James] EPA, Off Res & Dev, Washington, DC USA. [Loughner, Christopher] NASA Goddard Space Flight Ctr, ESSIC, Greenbelt, MD USA. [Hains, Jennifer] Maryland Dept Environm, Baltimore, MD 21224 USA. [Lee, Pius] NOAA Air Resources Lab, Silver Spring, MD USA. RP Flynn, CM (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. EM cflynn@atmos.umd.edu RI Liu, Xiong/P-7186-2014; Krotkov, Nickolay/E-1541-2012; Lee, Pius/D-5201-2016; Pickering, Kenneth/E-6274-2012; Dickerson, Russell/F-2857-2010; OI Liu, Xiong/0000-0003-2939-574X; Krotkov, Nickolay/0000-0001-6170-6750; Dickerson, Russell/0000-0003-0206-3083; Herman, Jay/0000-0002-9146-1632; Loughner, Christopher/0000-0002-3833-2014 FU NASA Earth Venture-1 DISCOVER-AQ project [NNX10AR39G] FX Funding for this work was provided by the NASA Earth Venture-1 DISCOVER-AQ project (NASA Grant NNX10AR39G). The authors thank Donald Lenschow for providing estimates of PBL height during the deployment. NR 34 TC 10 Z9 10 U1 4 U2 44 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD AUG PY 2014 VL 92 BP 429 EP 441 DI 10.1016/j.atmosenv.2014.04.041 PG 13 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AL0IO UT WOS:000338810800045 ER PT J AU Dietrich, JP Van Gaest, AL Strickland, SA Arkoosh, MR AF Dietrich, Joseph P. Van Gaest, Ahna L. Strickland, Stacy A. Arkoosh, Mary R. TI The impact of temperature stress and pesticide exposure on mortality and disease susceptibility of endangered Pacific salmon SO CHEMOSPHERE LA English DT Article DE Salmon; Malathion; Disease susceptibility; Temperature; Multiple stressors ID JUVENILE COHO SALMON; CHINOOK SALMON; CLIMATE-CHANGE; RIVER TEMPERATURE; RISK-ASSESSMENT; TOXICITY; CONSERVATION; MIXTURES; INSECTICIDES; ECOSYSTEMS AB Anthropogenic stressors, including chemical contamination and temperature stress, may contribute to increased disease susceptibility in aquatic animals. Specifically, the organophosphate pesticide malathion has been detected in surface waters inhabited by threatened and endangered salmon. In the presence of increasing water temperatures, malathion may increase susceptibility to disease and ultimately threaten salmon survival. This work examines the effect of acute and sublethal exposures to malathion on ocean-type subyearling Chinook salmon held under two temperature regimes. Chinook salmon were exposed to malathion at optimal (11 degrees C) or elevated (19 and 20 degrees C) temperatures. The influence of temperature on the acute toxicity of malathion was determined by generating 96-h lethal concentration (LC) curves. A disease challenge assay was also used to assess the effects of sublethal malathion exposure. The malathion concentration that resulted in 50% mortality (LC50: 274.1 mu g L-1) of the Chinook salmon at 19 degrees C was significantly less than the LC50 at 11 degrees C (364.2 mu g L-1). Mortality increased 11.2% in Chinook salmon exposed to malathion at the elevated temperature and challenged with Aeromonas salmonicida compared to fish held at the optimal temperature and exposed to malathion or the carrier control. No difference in disease challenge mortality was observed among malathion-exposed and unexposed fish at the optimal temperature. The interaction of co-occurring stressors may have a greater impact on salmon than if they occur in isolation. Ecological risk assessments considering the effects of an individual stressor on threatened and endangered salmon may underestimate risk when additional stressors are present in the environment. Published by Elsevier Ltd. C1 [Dietrich, Joseph P.; Van Gaest, Ahna L.; Strickland, Stacy A.; Arkoosh, Mary R.] NOAA, Environm & Fisheries Sci Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Dietrich, JP (reprint author), NOAA, Environm & Fisheries Sci Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2032 SE OSU Dr, Newport, OR 97365 USA. EM joseph.dietrich@noaa.gov; vangaest@gmail.com; sas70@me.com; mary.arkoosh@noaa.gov FU National Oceanic and Atmospheric Administration, Office of Protected Resources FX Funds were provided internally by the National Oceanic and Atmospheric Administration, Office of Protected Resources. Individuals at the Office of Protected Resources provided input into study design and objectives, but did not participate in the collection, analysis, interpretation of the data, preparation of the manuscript, or decision to submit the manuscript. All experiments with the lab-raised salmon were in accordance with the U.S. Government Principles for the Utilization and Care of Vertebrate Animals Used in Testing. Research. and Training for the humane treatment of fish to alleviate suffering. NR 52 TC 9 Z9 9 U1 6 U2 63 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-6535 EI 1879-1298 J9 CHEMOSPHERE JI Chemosphere PD AUG PY 2014 VL 108 BP 353 EP 359 DI 10.1016/j.chemosphere.2014.01.079 PG 7 WC Environmental Sciences SC Environmental Sciences & Ecology GA AJ7MU UT WOS:000337881600046 PM 24559935 ER PT J AU Wan, ZM Hong, Y Khan, S Gourley, J Flamig, Z Kirschbaum, D Tang, GQ AF Wan, Zhanming Hong, Yang Khan, Sadiq Gourley, Jonathan Flamig, Zachary Kirschbaum, Dalia Tang, Guoqiang TI A cloud-based global flood disaster community cyber-infrastructure: Development and demonstration SO ENVIRONMENTAL MODELLING & SOFTWARE LA English DT Article DE Flood; Cloud; Crowdsourcing; Web GIS AB Flood disasters have significant impacts on the development of communities globally. This study describes a public cloud-based flood cyber-infrastructure (CyberFlood) that collects, organizes, visualizes, and manages several global flood databases for authorities and the public in real-time, providing location-based eventful visualization as well as statistical analysis and graphing capabilities. In order to expand and update the existing flood inventory, a crowdsourcing data collection methodology is employed for the public with smartphones or Internet to report new flood events, which is also intended to engage citizen-scientists so that they may become motivated and educated about the latest developments in satellite remote sensing and hydrologic modeling technologies. Our shared vision is to better serve the global water community with comprehensive flood information, aided by the state-of-the-art cloud computing and crowd-sourcing technology. The CyberFlood presents an opportunity to eventually modernize the existing paradigm used to collect, manage, analyze, and visualize water-related disasters. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Wan, Zhanming; Hong, Yang; Khan, Sadiq] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA. [Wan, Zhanming; Hong, Yang; Khan, Sadiq; Flamig, Zachary] Natl Weather Ctr, Hydrometeorol & Remote Sensing Lab HyDROS, Norman, OK 73072 USA. [Wan, Zhanming; Hong, Yang; Khan, Sadiq; Flamig, Zachary] Natl Weather Ctr, Adv Radar Res Ctr, Norman, OK 73072 USA. [Gourley, Jonathan; Flamig, Zachary] NOAA, Natl Severe Storms Lab, Natl Weather Ctr, Norman, OK 73069 USA. [Kirschbaum, Dalia] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tang, Guoqiang] Tsinghua Univ, Dept Hydraul Engn, Beijing 100084, Peoples R China. RP Hong, Y (reprint author), Natl Weather Ctr, Adv Radar Res Ctr, HyDROS Lab, 4610 Suites,120 David L Boren Blvd, Norman, OK 73072 USA. EM zwan@ou.edu; yanghong@ou.edu RI Gourley, Jonathan/C-7929-2016; Hong, Yang/D-5132-2009; OI Gourley, Jonathan/0000-0001-7363-3755; Hong, Yang/0000-0001-8720-242X; Tang, Guoqiang/0000-0002-0923-583X FU Hydrometeorology & Remote Sensing Lab (HyDROS); Advanced Radar Research Center (ARRC) at the University of Oklahoma FX The first author would like to acknowledge the seed money support from Hydrometeorology & Remote Sensing Lab (HyDROS) and Advanced Radar Research Center (ARRC) at the University of Oklahoma. NR 15 TC 11 Z9 11 U1 4 U2 38 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1364-8152 EI 1873-6726 J9 ENVIRON MODELL SOFTW JI Environ. Modell. Softw. PD AUG PY 2014 VL 58 BP 86 EP 94 DI 10.1016/j.envsoft.2014.04.007 PG 9 WC Computer Science, Interdisciplinary Applications; Engineering, Environmental; Environmental Sciences SC Computer Science; Engineering; Environmental Sciences & Ecology GA AL0OI UT WOS:000338825800007 ER PT J AU Ruzmaikin, A Lee, JN Wu, DL AF Ruzmaikin, Alexander Lee, Jae N. Wu, Dong L. TI Patterns of carbon monoxide in the middle atmosphere and effects of solar variability SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Middle atmosphere; Solar variability ID CYCLE AB We determine the spatial-time patterns of zonally averaged carbon monoxide (CO) in the middle atmosphere by applying Principle Component Analysis to the CO data obtained from the Microwave Limb Sounder (MLS) measurements on the Aura satellite in 2004-2012. The first two principal components characterize more than 90% of the CO variability. Both principal components are localized in the low thermosphere near the mesopause. The first principal component is asymmetric relative to the poles. It has opposite signs in the Northern and Southern Hemisphere at mid to high latitudes and strongly oscillates with an annual periodicity. The second principal component has the same sign in both hemispheres and oscillates mainly with a semi-annual frequency. Both principal components are modulated by the 11-year solar cycle and display short-term variations. To test possible correlations of these variations with the short term solar ultraviolet (UV) variability we use the simultaneous measurements of the UV solar radiance from the Solar-Stellar Irradiance Comparison Experiment (SOLSTICE) on the Solar Radiation and Climate Experiment (SORCE) satellite to investigate the correlation between CO in the middle atmosphere and solar UV in 2004-2012. Using a wavelet coherence technique a weak, intermittent 27-day signal is detected in high-frequency parts of the CO principal components. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Ruzmaikin, Alexander] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lee, Jae N.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Wu, Dong L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ruzmaikin, A (reprint author), CALTECH, 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 the National Aeronautics and Space Administration; NASA LWS FX We thank two reviewers for helpful critical comments. 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 acknowledge the NASA LWS grant on observational study of solar variability impacts on the troposphere, stratosphere and mesosphere. NR 16 TC 4 Z9 4 U1 0 U2 6 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD AUG 1 PY 2014 VL 54 IS 3 BP 320 EP 326 DI 10.1016/j.asr.2013.06.033 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA AL0IE UT WOS:000338809800005 ER PT J AU Gao, J Vissers, MR Sandberg, M Li, D Cho, HM Bockstiegel, C Mazin, BA Leduc, HG Chaudhuri, S Pappas, DP Irwin, KD AF Gao, J. Vissers, M. R. Sandberg, M. Li, D. Cho, H. M. Bockstiegel, C. Mazin, B. A. Leduc, H. G. Chaudhuri, S. Pappas, D. P. Irwin, K. D. TI Properties of TiN for Detector and Amplifier Applications SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Kinetic inductance detector; Parametric amplifier; Two-level system; Titanium nitride ID BAND AB We have experimentally explored and carefully characterized the important properties of TiN, including the resistivity, nonlinear kinetic inductance, the anomalous electro-dynamical response, and the two-level-system induced frequency shift and noise. We suggest that some of these properties, which are not well understood and are different from conventional superconductors, need further study and special consideration in kinetic inductance detector and parametric amplifier applications. C1 [Gao, J.; Vissers, M. R.; Sandberg, M.; Li, D.; Cho, H. M.; Bockstiegel, C.; Pappas, D. P.; Irwin, K. D.] NIST, Boulder, CO 80305 USA. [Mazin, B. A.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. [Leduc, H. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chaudhuri, S.] CALTECH, Pasadena, CA 91125 USA. RP Gao, J (reprint author), NIST, Boulder, CO 80305 USA. EM jgao@boulder.nist.gov RI Mazin, Ben/B-8704-2011 OI Mazin, Ben/0000-0003-0526-1114 NR 20 TC 2 Z9 2 U1 1 U2 20 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 136 EP 141 DI 10.1007/s10909-014-1089-5 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800002 ER PT J AU Giachero, A Day, P Falferi, P Faverzani, M Ferri, E Giordano, C Marghesin, B Mattedi, F Mezzena, R Nizzolo, R Nucciotti, A AF Giachero, A. Day, P. Falferi, P. Faverzani, M. Ferri, E. Giordano, C. Marghesin, B. Mattedi, F. Mezzena, R. Nizzolo, R. Nucciotti, A. TI Critical Temperature Tuning of Ti/TiN Multilayer Films Suitable for Low Temperature Detectors SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE MKIDs; Superconductive microresonator; Neutrino physics AB We present our current progress on the design and test of Ti/TiN multilayer for use in kinetic inductance detectors. Sensors based on sub-stoichiometric TiN film are commonly used in several applications. However, it is difficult to control the targeted critical temperature , to maintain precise control of the nitrogen incorporation process and to obtain a production uniformity. To avoid these problems we investigated multilayer Ti/TiN films that show a high uniformity coupled with high quality factor, kinetic inductance and inertness of TiN. These features are ideal to realize superconductive microresonator detectors for astronomical instruments application but also for the field of neutrino physics. Using pure Ti and stoichiometric TiN, we developed and tested different multilayer configurations, in terms of number of Ti/TiN layers and in terms of different interlayer thicknesses. The target was to reach a critical temperature around K in order to have a low energy gap and slower recombination time (i.e. low generation-recombination noise). The results prove that the superconductive transition can be tuned in the K temperature range by properly choosing the Ti thickness in the nm range, and the TiN thickness in the nm range. C1 [Giachero, A.; Faverzani, M.; Ferri, E.; Nizzolo, R.; Nucciotti, A.] Univ Milano Bicocca, Milan, Italy. [Giachero, A.; Faverzani, M.; Ferri, E.; Nizzolo, R.; Nucciotti, A.] INFN Milano Bicocca, Milan, Italy. [Day, P.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Falferi, P.] Fdn Bruno Kessler, CNR, Ist Foton & Nanotecnol, Trento, Italy. [Giordano, C.; Marghesin, B.; Mattedi, F.] Fdn Bruno Kessler, Trento, Italy. [Mezzena, R.] Univ Trento, Dipartimento Fis, Trento, Italy. RP Giachero, A (reprint author), Univ Milano Bicocca, Milan, Italy. EM Andrea.Giachero@mib.infn.it RI Giachero, Andrea/I-1081-2013; Nucciotti, Angelo/I-8888-2012; Ferri, Elena/L-8531-2014; Falferi, Paolo/C-3439-2015; Mezzena, Renato/K-1802-2015; Faverzani, Marco/K-3865-2016 OI Giachero, Andrea/0000-0003-0493-695X; Nucciotti, Angelo/0000-0002-8458-1556; Ferri, Elena/0000-0003-1425-3669; Falferi, Paolo/0000-0002-1929-4710; Mezzena, Renato/0000-0001-9891-0472; Faverzani, Marco/0000-0001-8119-2953 FU Fondazione Cariplo [2010-2351] FX This work is supported by Fondazione Cariplo through the project Development of Microresonator Detectors for Neutrino Physics (Grant International Recruitment Call 2010, ref. 2010-2351). NR 15 TC 1 Z9 1 U1 0 U2 10 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 155 EP 160 DI 10.1007/s10909-013-1078-0 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800005 ER PT J AU Kellaris, N Daal, M Epland, M Pepin, M Kamaev, O Cushman, P Kramer, E Sadoulet, B Mirabolfathi, N Golwala, S Runyan, M AF Kellaris, N. Daal, M. Epland, M. Pepin, M. Kamaev, O. Cushman, P. Kramer, E. Sadoulet, B. Mirabolfathi, N. Golwala, S. Runyan, M. TI Sub-Kelvin Thermal Conductivity and Radioactivity of Some Useful Materials in Low Background Cryogenic Experiments SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Ti 15-3-3-3; Vespel; Graphite; Kapton; Thermal Conductivity; Radioactivity AB We present measurements of the thermal conductivity between 0.05 and 1 K, and radioactive contamination levels, for some thermally isolating materials. TIMET Ti 15-3-3-3, Mersen grade 2020 graphite, Vespel SP-1, Vespel SP-22, Vespel SCP-5000, Vespel SCP-5050, Graphlite CFRP, and a Kapton/epoxy composite are all investigated. Thermal conductivities were measured using a single-heater longitudinal heat flow method. Material radioactivity was determined for the materials at a low background counting facility using a high-purity gamma detector and GEANT4 Monte Carlo simulations. C1 [Kellaris, N.; Daal, M.; Kramer, E.; Sadoulet, B.; Mirabolfathi, N.; Runyan, M.] Univ Calif Berkeley, Dept Phys, CDMS Expt, Berkeley, CA 94720 USA. [Epland, M.; Pepin, M.; Cushman, P.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Kamaev, O.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada. [Golwala, S.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Runyan, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kellaris, N (reprint author), Univ Calif Berkeley, Dept Phys, CDMS Expt, Berkeley, CA 94720 USA. EM nicholaskellaris@berkeley.edu FU Department of Energy; National Science Foundation FX The authors would like to thank Curbell Plastics and Tech-Etch for donating test samples. This work was funded by the Department of Energy and the National Science Foundation. NR 9 TC 1 Z9 1 U1 2 U2 5 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 201 EP 208 DI 10.1007/s10909-013-1048-6 PG 8 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800012 ER PT J AU Karasik, BS McKitterick, CB Prober, DE AF Karasik, Boris S. McKitterick, Christopher B. Prober, Daniel E. TI Prospective Performance of Graphene HEB for Ultrasensitive Detection of Sub-mm Radiation SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Graphene; Hot-electron bolometer; Noise thermometry ID HOT-ELECTRON BOLOMETER; NOISE; NANOBOLOMETERS; MIXER; BAND AB Noise equivalent power and time constant of a submillimeter wave hot-electron bolometer (HEB) made from monolayer graphene are analyzed using the lowest electron-phonon thermal conductance data reported to date. Frequency-domain multiplexed Johnson Noise Thermometry (JNT) is used for the detector readout. Planar microantennas or waveguides can provide efficient coupling of the graphene microdevice to radiation. The results show that the graphene HEB detector can be radiation background limited at very low level corresponding to the photon noise on a space telescope with cryogenically cooled mirror. Beside the high sensitivity, absence of a hard power saturation limit, higher operating temperature, and the ability to read 1,000s of elements with a single broadband amplifier will be the advantages of such a detector. C1 [Karasik, Boris S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [McKitterick, Christopher B.; Prober, Daniel E.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [McKitterick, Christopher B.; Prober, Daniel E.] Yale Univ, Dept Appl Phys, New Haven, CT 06520 USA. RP Karasik, BS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM boris.s.karasik@jpl.nasa.gov FU National Aeronautics and Space Administration; NSF [DMR-0907082]; IBM; Yale University FX The work at the Jet Propulsion Laboratory, California Institute of Technology, was carried out under a contract with the National Aeronautics and Space Administration. The work at Yale was supported by NSF Grant DMR-0907082, an IBM Faculty Grant, and by Yale University. NR 28 TC 4 Z9 4 U1 1 U2 21 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 249 EP 254 DI 10.1007/s10909-014-1087-7 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800019 ER PT J AU McKitterick, C Vora, H Du, X Karasik, B Prober, D AF McKitterick, Christopher B. Vora, Heli Du, Xu Karasik, Boris S. Prober, Daniel E. TI Graphene Microbolometers with Superconducting Contacts for Terahertz Photon Detection SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Graphene; Hot-electron bolometer; Terahertz AB We report on noise and thermal conductance measurements taken in order to determine an upper bound on the performance of graphene as a terahertz photon detector. The main mechanism for sensitive terahertz detection in graphene is bolometric heating of the electron system. To study the properties of a device using this mechanism to detect terahertz photons, we perform Johnson noise thermometry measurements on graphene samples. These measurements probe the electron-phonon behavior of graphene on silicon dioxide at low temperatures. Because the electron-phonon coupling is weak in graphene, superconducting contacts with large gap are used to confine the hot electrons and prevent their out-diffusion. We use niobium nitride leads with a K to contact the graphene. We find these leads make good ohmic contact with very low contact resistance. Our measurements find an electron-phonon thermal conductance that depends quadratically on temperature above 4 K and is compatible with single terahertz photon detection. C1 [McKitterick, Christopher B.; Prober, Daniel E.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [McKitterick, Christopher B.; Prober, Daniel E.] Yale Univ, Dept Appl Phys, New Haven, CT 06520 USA. [Vora, Heli; Du, Xu] SUNY Stony Brook, Dept Phys, Stony Brook, NY 11790 USA. [Karasik, Boris S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP McKitterick, CB (reprint author), Yale Univ, Dept Phys, New Haven, CT 06520 USA. EM chris.mckitterick@yale.edu; daniel.prober@yale.edu FU NSF [DMR-0907082]; IBM; Yale University; National Aeronautics and Space Administration; AFOSR-YIP Award [FA9550-10-1-0090] FX The work at Yale was supported by NSF Grant DMR-0907082, an IBM Faculty Grant, and by Yale University. The work at Jet Propulson Laboratory was carried out under a contract with the National Aeronautics and Space Administration. X. Du and H. Vora acknowledge support from AFOSR-YIP Award No. FA9550-10-1-0090. NR 26 TC 6 Z9 6 U1 4 U2 39 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 291 EP 298 DI 10.1007/s10909-014-1127-3 PG 8 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800026 ER PT J AU Beyer, AD Kenyon, ME Bumble, B Runyan, MC Echternach, PE Holmes, WA Bock, JJ Bradford, CM AF Beyer, A. D. Kenyon, M. E. Bumble, B. Runyan, M. C. Echternach, P. E. Holmes, W. A. Bock, J. J. Bradford, C. M. TI Comparing Transition-Edge Sensor Response Times in a Modified Contact Scheme with Different Support Beams SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Infrared detector; Sub-mm detector; Superconducting device; Transition-edge sensor AB We present measurements of the thermal conductance, G, and effective time constants, , of three transition-edge sensors (TESs) populated in arrays operated from 80-87 mK with T 120 mK. Our TES arrays include several variations of thermal architecture enabling determination of the architecture that demonstrates the minimum noise equivalent power, the lowest , and the trade-offs among designs. The three TESs we report here have identical Mo/Cu bilayer thermistors and wiring structures, while the thermal architectures are: (1) a TES with straight support beams of 1 mm length, (2) a TES with meander support beams of total length 2 mm and with two phonon-filter blocks per beam, and (3) a TES with meander support beams of total length 2 mm and with six phonon-filter blocks per beam. Our wiring scheme aims to lower the thermistor normal state resistance R and increase the sharpness of the transition dlogR/dlogT at the transition temperature T. We find an upper limit of given by (), and G values of 200 fW/K for (1), 15 fW/K for (2), and 10 fW/K for (3). The value of can be improved by slightly increasing the length of our thermistors. C1 [Beyer, A. D.; Kenyon, M. E.; Bumble, B.; Runyan, M. C.; Echternach, P. E.; Holmes, W. A.; Bock, J. J.; Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Beyer, AD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM andrew.d.beyer@jpl.nasa.gov NR 7 TC 0 Z9 0 U1 1 U2 3 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 299 EP 303 DI 10.1007/s10909-013-1027-y PG 5 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800027 ER PT J AU Morgan, KM Busch, SE Eckart, ME Kilbourne, CA McCammon, D AF Morgan, K. M. Busch, S. E. Eckart, M. E. Kilbourne, C. A. McCammon, D. TI Large Area Transition Edge Sensor X-ray Microcalorimeters for Diffuse X-ray Background Studies SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Transition edge sensors; Microcalorimeters; X-ray astronomy ID CHARGE-TRANSFER; SOLAR-WIND; EMISSION AB We are developing transition edge sensor (TES) mirocalorimeters with large area (0.72 mm) absorbers to study the keV diffuse X-ray background. The goal is to develop a 2 cm array of 256 pixels for a sounding rocket payload. We present a pixel design which includes a Mo/Au bilayer TES coupled to a large (850 x 850 x 0.2 m) gold absorber. Our simulations indicate that such a design can achieve energy resolution as good as 1.6 eV FWHM in our target bandpass of 0.05-1 keV. Additionally, thermal modelling shows that for typical gold layers, the position-dependent variation of the pulse shape over the large area of the absorber is not expected to significantly degrade this energy resolution. An array of devices will be fabricated in late 2013 to test this design. C1 [Morgan, K. M.; McCammon, D.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Busch, S. E.; Eckart, M. E.; Kilbourne, C. A.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Busch, S. E.] NASA, Postdoctoral Program, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eckart, M. E.] CRESST, Baltimore, MD 21250 USA. [Eckart, M. E.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. RP Morgan, KM (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. EM kmmorgan2@wisc.edu RI Morgan, Kelsey/J-5053-2016 OI Morgan, Kelsey/0000-0002-6597-1030 FU NASA Office of the Chief Technologist's Space Technology Research Fellowship; NASA [NNX09AF09G]; NASA FX This work was supported by a NASA Office of the Chief Technologist's Space Technology Research Fellowship. Supported in part by NASA grant NNX09AF09G. This research was in part supported by appointment (S. E. Busch) to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 14 TC 1 Z9 1 U1 1 U2 13 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 331 EP 336 DI 10.1007/s10909-013-1011-6 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800032 ER PT J AU Smith, SJ Adams, JS Bandler, SR Busch, SE Chervenak, JA Eckart, ME Finkbeiner, FM Kelley, RL Kilbourne, CA Lee, SJ Porst, JP Porter, FS Sadleir, JE AF Smith, S. J. Adams, J. S. Bandler, S. R. Busch, S. E. Chervenak, J. A. Eckart, M. E. Finkbeiner, F. M. Kelley, R. L. Kilbourne, C. A. Lee, S. J. Porst, J. -P. Porter, F. S. Sadleir, J. E. TI Characterization of Mo/Au Transition-Edge Sensors with Different Geometric Configurations SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Transition-edge sensor; Microcalorimeter; Weak-link; Proximity effect ID X-RAY MICROCALORIMETERS AB Mo/Au transition-edge sensors exhibit weak-link behavior in the measured temperature, and field, dependence of the critical current . This is a consequence of the longitudinal proximitization between the Nb electrical bias contacts and the bilayer. Understanding how weak-link superconductivity impacts the resistive transition and the detector energy resolution is of great interest. In this contribution we present studies of for three devices that have different geometries of metallic depositions on top of the sensor used for noise mitigation and X-ray absorption. Results show that these features change the measured compared to the previously seen measurements on devices without additional deposition layers. Measurements of the small signal transition parameters and also reveal differences between designs that impact the measured response to X-rays and energy resolution. C1 [Smith, S. J.; Adams, J. S.; Bandler, S. R.; Busch, S. E.; Chervenak, J. A.; Eckart, M. E.; Finkbeiner, F. M.; Kelley, R. L.; Kilbourne, C. A.; Lee, S. J.; Porst, J. -P.; Porter, F. S.; Sadleir, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smith, S. J.; Adams, J. S.; Eckart, M. E.] CRESST, Baltimore, MD 21250 USA. [Smith, S. J.; Adams, J. S.; Eckart, M. E.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Bandler, S. R.] CRESST, College Pk, MD 20742 USA. [Bandler, S. R.] Univ Maryland, College Pk, MD 20742 USA. [Busch, S. E.; Lee, S. J.] NASA, Postdoctoral Program Fellow, Greenbelt, MD USA. [Finkbeiner, F. M.] Wyle Informat Syst, Mclean, VA 22102 USA. [Porst, J. -P.] CRESST, Columbia, MD 21044 USA. [Porst, J. -P.] USRA, Columbia, MD 21044 USA. RP Smith, SJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM stephen.j.smith@nasa.gov RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Lee, Sang Jun/A-3892-2015; Porter, Frederick/D-3501-2012 OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106; Lee, Sang Jun/0000-0002-8199-3993; Porter, Frederick/0000-0002-6374-1119 FU NASA FX This research was in part supported by an appointment (Busch and Lee) to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 12 TC 6 Z9 6 U1 3 U2 19 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 356 EP 362 DI 10.1007/s10909-013-1031-2 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800036 ER PT J AU Kenyon, M Beyer, AD Bumble, B Echternach, PM Holmes, WA Bradford, CM AF Kenyon, M. Beyer, A. D. Bumble, B. Echternach, P. M. Holmes, W. A. Bradford, C. M. TI Toward a Detector/Readout Architecture for the Background-Limited Far-IR/Submm Spectrograph (BLISS) SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Transition-edge sensor; Far-IR spectrometer; Submm spectrometer AB We have built and tested 32-element linear arrays of absorber-coupled transition-edge sensors (TESs) read out with a time-division SQUID multiplexer. This detector/readout architecture is designed for the background-limited far-IR/submm spectrograph (BLISS) which is a broadband (35-433 m), grating spectrometer consisting of six wavebands each with a modest resolution of R 700. Since BLISS requires the effective noise equivalent power (NEP) of the TESs to equal 1 10 W/Hz, our detectors consist of very long (1-2 mm), narrow (0.4 m), and thin (0.25 m) SiN support beams that reduce the thermal conductance G between the substrate and the optical absorber. The thermistors of our lowest noise TESs consist of iridium with mK. We have measured the electrical properties of arrays of these Ir TESs with various meander and straight support beams and absorber shapes and found that G is 30 fW/K (meander) and 110 fW/K (straight), the electrical NEP is 2-3 10 W/Hz (meander and straight), and the response time is 10-30 ms (meander) and 2-5 ms (straight). To reduce spurious or "dark" power from heating the arrays, we mounted the arrays into light-tight niobium boxes and added custom L/R and L/C low-pass chip filters into these boxes to intercept dark power from the bias and readout circuit. We found the average dark power equals 1.3 and 4.6 fW for the boxes with L/R and L/C chip filters, respectively. We have built arrays with mK using molybdenum/copper bilayers and are working to lower the dark power by an order of magnitude so we can demonstrate NEP 10 W/Hz with these arrays. PACS numbers: 85.25.Pb; 95.85.Gn; 95.85.Fm; 63.22.+m. C1 [Kenyon, M.; Beyer, A. D.; Bumble, B.; Echternach, P. M.; Holmes, W. A.; Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kenyon, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mkenyon@jpl.nasa.gov FU National Aeronautics and Space Administration FX This research was carried out at the Jet Propulsion Laboratory and Caltech under contract with the National Aeronautics and Space Administration. NR 9 TC 0 Z9 0 U1 0 U2 3 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 376 EP 382 DI 10.1007/s10909-013-1020-5 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800039 ER PT J AU Sadleir, JE Lee, SJ Smith, SJ Busch, SE Bandler, SR Adams, JS Eckart, ME Chervenak, JA Kelley, RL Kilbourne, CA Porter, FS Porst, JP AF Sadleir, John E. Lee, Sang-Jun Smith, Stephen J. Busch, Sarah E. Bandler, Simon R. Adams, Joseph S. Eckart, Megan E. Chervenak, James A. Kelley, Richard L. Kilbourne, Caroline A. Porter, Frederick S. Porst, Jan-Patrick TI The Magnetically-Tuned Transition-Edge Sensor SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Low temperature detectors; Supeconductivity; Magnetic field dependence; Superconducting resistive transition width; Superconducting weak-links AB We present the first measurements on the proposed magnetically-tuned superconducting transition-edge sensor and compare the modified resistive transition with the theoretical prediction (Sadleir et al., IEEE Trans App Supercond 23:2101405, 2013). A TES's resistive transition is customarily characterized in terms of the unitless device parameters and corresponding to the resistive response to changes in temperature and current respectively. We present a new relationship between measured IV quantities (sensor current and voltage ) and the parameters and and use these relations to confirm we have stably biased a TES with negative parameter with magnetic tuning. Motivated by access to this new unexplored parameter space, we investigate the conditions for bias stability of a TES taking into account both self and externally applied magnetic fields. C1 [Sadleir, John E.; Lee, Sang-Jun; Smith, Stephen J.; Busch, Sarah E.; Bandler, Simon R.; Adams, Joseph S.; Eckart, Megan E.; Chervenak, James A.; Kelley, Richard L.; Kilbourne, Caroline A.; Porter, Frederick S.; Porst, Jan-Patrick] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sadleir, JE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM john.e.sadleir@nasa.gov RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Lee, Sang Jun/A-3892-2015; Porter, Frederick/D-3501-2012 OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106; Lee, Sang Jun/0000-0002-8199-3993; Porter, Frederick/0000-0002-6374-1119 NR 7 TC 0 Z9 0 U1 2 U2 13 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 392 EP 399 DI 10.1007/s10909-014-1194-5 PG 8 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800041 ER PT J AU Lindeman, MA Eom, BH Day, PK Swenson, LJ Wernis, R LeDuc, HG Zmuidzinas, J AF Lindeman, M. A. Eom, B. H. Day, P. K. Swenson, L. J. Wernis, Rebecca LeDuc, H. G. Zmuidzinas, J. TI AC Bolometer Theory and Measurements of Kinetic Inductance Bolometer-Resonators SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Alternating current; Bolometer; Calorimeter; Kinetic inductance; Theory; Alpha; Beta; Response; Noise AB AC bolometer theory is built on the established matrix formalism for quantum calorimeters and bolometers. The bolometer is represented by a 3 3 matrix with complex valued parameters. The bolometer matrix is used to model the behavior of the devices including the response to signal and noise, feedback, pulse response times, stability, and bolometer impedance. The effects of a current dependent bolometer impedance are included. The matrix simplifies theoretical computations of AC devices, including demodulation and the interactions between signals at different frequencies. This theory is applied to measurements of bolometers, each consisting of a kinetic inductance device suspended on a silicon nitride membrane. These measurements and analysis facilitate the optimization of the design and performance of these novel AC bolometers. C1 [Lindeman, M. A.; Eom, B. H.; Day, P. K.; LeDuc, H. G.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Swenson, L. J.; Wernis, Rebecca; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA. RP Lindeman, MA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM mark.a.lindeman@jpl.nasa.gov NR 9 TC 3 Z9 3 U1 0 U2 6 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 511 EP 517 DI 10.1007/s10909-013-1008-1 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800059 ER PT J AU Faverzani, M Day, PK Falferi, P Ferri, E Giachero, A Giordano, C LeDuc, HG Marghesin, B Mezzena, R Nizzolo, R Nucciotti, A AF Faverzani, M. Day, P. K. Falferi, P. Ferri, E. Giachero, A. Giordano, C. LeDuc, H. G. Marghesin, B. Mezzena, R. Nizzolo, R. Nucciotti, A. TI Development of Superconducting Microresonators for a Neutrino Mass Experiment SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE MKID detectors; Neutrino mass; Holmium ID KINETIC INDUCTANCE DETECTORS; REDUCTION; ARRAYS; DECAY AB The determination of the neutrino mass is still an open issue in particle physics. The calorimetric measurement of the energy released in a nuclear beta decay allows to measure all the released energy, except the fraction carried away by the neutrino: a finite neutrino mass m causes the energy spectrum to be truncated at Q m, where Q is the transition energy. The electron capture of Ho (Q 2.5 keV) results to be an ideal decay. In order to achieve enough statistics, a large number of detectors (10) is required. Superconducting microwave microresonators are detectors suitable for large-scale multiplexed frequency domain readout, with theoretical energy and time resolution of eV and s. Our aim is to develop arrays of microresonator detectors applicable to the calorimetric measurement of the energy spectra of Ho. Currently, a study aimed to the selection of the best design and material for the detectors is in progress. In this contribution, a comparison between the measurements (critical temperature, gap parameter, quasiparticle recombination time and X-ray energy spectra) made with stoichiometric, sub-stoichiometric TiN and Ti/TiN multilayer films are presented. C1 [Faverzani, M.; Ferri, E.; Giachero, A.; Nizzolo, R.; Nucciotti, A.] Univ Milano Bicocca, Milan, Italy. [Faverzani, M.; Ferri, E.; Giachero, A.; Nucciotti, A.] INFN Milano Bicocca, Milan, Italy. [Day, P. K.; LeDuc, H. G.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Falferi, P.] CNR Fdn Bruno Kessler, Ist Foton & Nanotecnol, Trento, Italy. [Giordano, C.; Marghesin, B.] FBK, Trento, Italy. [Mezzena, R.] Univ Trento, Dipartimento Fis, Trento, Italy. RP Faverzani, M (reprint author), Univ Milano Bicocca, Milan, Italy. EM marco.faverzani@mib.infn.it RI Giachero, Andrea/I-1081-2013; Nucciotti, Angelo/I-8888-2012; Ferri, Elena/L-8531-2014; Falferi, Paolo/C-3439-2015; Mezzena, Renato/K-1802-2015; Faverzani, Marco/K-3865-2016 OI Giachero, Andrea/0000-0003-0493-695X; Nucciotti, Angelo/0000-0002-8458-1556; Ferri, Elena/0000-0003-1425-3669; Falferi, Paolo/0000-0002-1929-4710; Mezzena, Renato/0000-0001-9891-0472; Faverzani, Marco/0000-0001-8119-2953 FU Fondazione Cariplo through project Development of Microresonator Detectors for Neutrino Physics [2010-2351] FX This work is supported by Fondazione Cariplo through the project Development of Microresonator Detectors for Neutrino Physics (Grant 2010-2351). NR 16 TC 3 Z9 3 U1 0 U2 11 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 530 EP 537 DI 10.1007/s10909-013-1051-y PG 8 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800062 ER PT J AU Hokin, MS McCammon, D Morgan, KM Bandler, SR Lee, SJ Moseley, SH Smith, SJ AF Hokin, M. S. McCammon, D. Morgan, K. M. Bandler, S. R. Lee, S. J. Moseley, S. H. Smith, S. J. TI Narrow Line X-Ray Calibration Source for High Resolution Microcalorimeters SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Microcalorimeters; Calibration; Fiber-optics; Lasers; X-ray detectors AB We are developing a narrow line calibration source for use with X-ray microcalorimeters. At energies below 300 eV fluorescent lines are intrinsically broad, making calibration of high resolution detectors difficult. This source consists of a 405 nm (3 eV) laser diode coupled to an optical fiber. The diode is pulsed to create approximately one hundred photons in a few microseconds. If the pulses are short compared to the rise time of the detector, they will be detected as single events with a total energy in the soft X-ray range. Poisson fluctuations in photon number per pulse create a comb of X-ray lines with 3 eV spacing, so detectors with energy resolution better than 2 eV are required to resolve the individual lines. Our currently unstabilized diode has a multimode width less than 1 nm, giving a 300 eV event a FWHM less than 0.1 eV. By varying the driving voltage, or pulse width, the source can produce a comb centered on a wide range of energies. The calibration events are produced at precisely known times. This allows continuous calibration of a flight mission without contaminating the observed spectrum and with minimal deadtime. C1 [Hokin, M. S.; McCammon, D.; Morgan, K. M.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Bandler, S. R.; Lee, S. J.; Moseley, S. H.; Smith, S. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hokin, MS (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. EM mhokin@wisc.edu RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Lee, Sang Jun/A-3892-2015; Morgan, Kelsey/J-5053-2016 OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106; Lee, Sang Jun/0000-0002-8199-3993; Morgan, Kelsey/0000-0002-6597-1030 FU NASA [NNX09AF09G]; NASA office of the Chief Technologist's Space Technology Research Fellowship FX This work was supported in part by NASA grant NNX09AF09G. K.M. Morgan is supported by a NASA office of the Chief Technologist's Space Technology Research Fellowship. NR 2 TC 1 Z9 1 U1 0 U2 5 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 566 EP 570 DI 10.1007/s10909-013-1029-9 PG 5 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800067 ER PT J AU Akamatsu, H Gottardi, L Adams, J Bandler, S Bruijn, M Chervenak, J Eckart, M Finkbeiner, F den Hartog, R Hoevers, H Kelley, R Kilbourne, C van der Kuur, J van den Linden, AJ Porter, F Sadleir, J Smith, S Kiviranta, M AF Akamatsu, H. Gottardi, L. Adams, J. Bandler, S. Bruijn, M. Chervenak, J. Eckart, M. Finkbeiner, F. den Hartog, R. Hoevers, H. Kelley, R. Kilbourne, C. van der Kuur, J. van den Linden, A. J. Porter, F. Sadleir, J. Smith, S. Kiviranta, M. TI Performance of TES X-ray Microcalorimeters with AC Bias Read-Out at MHz Frequencies SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE X-ray; Transition edge sensor; Microcalorimeter ID ABSORBER DESIGN AB At SRON we are developing Frequency Domain Multiplexing for the read-out of superconducting transition edge sensor microcalorimeters for future X-ray astrophysical missions. We will report on the performance of Goddard Space Flight Center pixels under AC bias in the MHz frequency range. Superconducting flux transformers are used to improve the impedance matching between the low ohmic TESs and the SQUID. We connected 5 pixels to the LC filters with resonant frequencies ranging between 1 and 5 MHz. For X-ray photons of 6 keV we measured a best X-ray energy resolution of 3.6 eV at 1.4 MHz, consistent with the integrated Noise Equivalent Power. In addition, we improved the electrical circuit by optimizing the coupling ratio of the impedance matching transformer. In addition, we improved electrical circuit for impedance matching; modified transformer coupling ratio. As a result, we got the integrated noise equivalent power resolution of 2.7 eV at 2.5 MHz. A characterization of the detector response as a function of the AC bias voltage, bias frequency and the applied magnetic field is presented. C1 [Akamatsu, H.; Gottardi, L.; Bruijn, M.; den Hartog, R.; Hoevers, H.; van der Kuur, J.; van den Linden, A. J.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Adams, J.; Bandler, S.; Chervenak, J.; Eckart, M.; Finkbeiner, F.; Kelley, R.; Kilbourne, C.; Porter, F.; Sadleir, J.; Smith, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kiviranta, M.] VTT, Espoo, Finland. RP Akamatsu, H (reprint author), SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM h.akamatsu@sron.nl RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Porter, Frederick/D-3501-2012 OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106; Porter, Frederick/0000-0002-6374-1119 FU NWO, the Netherlands Organization for Scientific Research FX The authors would like to thank Martijn Schoemans, Dick Boersma, Marcel van Litsenburg and Robert Huiting for their precious technical help. We also thank an anonymous referees for constructive comments. SRON is supported financially by NWO, the Netherlands Organization for Scientific Research. NR 10 TC 3 Z9 3 U1 0 U2 8 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 591 EP 596 DI 10.1007/s10909-014-1130-8 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800071 ER PT J AU Lee, SJ Bandler, SR Busch, SE Adams, JS Chervenak, JA Eckart, ME Ewin, AJ Finkbeiner, FM Kelley, RL Kilbourne, CA Porst, JP Porter, FS Sadleir, JE Smith, SJ Wassel, EJ AF Lee, S. J. Bandler, S. R. Busch, S. E. Adams, J. S. Chervenak, J. A. Eckart, M. E. Ewin, A. J. Finkbeiner, F. M. Kelley, R. L. Kilbourne, C. A. Porst, J. -P. Porter, F. S. Sadleir, J. E. Smith, S. J. Wassel, E. J. TI High Count-Rate Studies of Small-Pitch Transition-Edge Sensor X-ray Microcalorimeters SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Low temperature detector; Transition-edge sensor; X-ray spectroscopy; High count-rate; Signal processing AB We are developing kilo-pixel arrays of small-pitch transition-edge sensors for high spectral-resolving, high count-rate applications in astrophysics and solar physics measurements. We have fabricated and tested pixels that are m in size on a silicon substrate with an X-ray flux of counts per second (cps) per pixel. The X-ray pulses were recorded and analyzed in various ways to obtain high throughput with good energy resolution. We have demonstrated 2.3 eV FWHM resolution with 99.6 % throughput for a 6-keV X-ray flux of 100 cps. C1 [Lee, S. J.; Bandler, S. R.; Busch, S. E.; Adams, J. S.; Chervenak, J. A.; Eckart, M. E.; Ewin, A. J.; Finkbeiner, F. M.; Kelley, R. L.; Kilbourne, C. A.; Porst, J. -P.; Porter, F. S.; Sadleir, J. E.; Smith, S. J.; Wassel, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bandler, S. R.] CRESST, College Pk, MD 20742 USA. [Bandler, S. R.] Univ Maryland, College Pk, MD 20742 USA. [Adams, J. S.; Eckart, M. E.; Smith, S. J.] CRESST, Baltimore, MD 21250 USA. [Adams, J. S.; Eckart, M. E.; Smith, S. J.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Finkbeiner, F. M.] Wyle Informat Syst, Mclean, VA 22102 USA. [Porst, J. -P.] CRESST, Columbia, MD 21044 USA. [Porst, J. -P.] USRA, Columbia, MD 21044 USA. [Wassel, E. J.] MEI Technol Inc, Lanham, MD 20706 USA. RP Lee, SJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM quantization@gmail.com RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Lee, Sang Jun/A-3892-2015; Porter, Frederick/D-3501-2012 OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106; Lee, Sang Jun/0000-0002-8199-3993; Porter, Frederick/0000-0002-6374-1119 FU NASA Postdoctoral Program at Goddard Space Flight Center; NASA FX This research was supported in part by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center (S. J. Lee and S. E. Busch), administered by Oak Ridge Associated Universities through a contract with NASA. NR 14 TC 3 Z9 3 U1 0 U2 7 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2014 VL 176 IS 3-4 BP 597 EP 603 DI 10.1007/s10909-013-1071-7 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AK1WY UT WOS:000338210800072 ER PT J AU Islam, T Srivastava, PK Rico-Ramirez, MA Dai, Q Han, DW Gupta, M AF Islam, Tanvir Srivastava, Prashant K. Rico-Ramirez, Miguel A. Dai, Qiang Han, Dawei Gupta, Manika TI An exploratory investigation of an adaptive neuro fuzzy inference system (ANFIS) for estimating hydrometeors from TRMM/TMI in synergy with TRMM/PR SO ATMOSPHERIC RESEARCH LA English DT Article DE Liquid water contents; Ice water contents; Global precipitation measurement (GPM); Rain rate retrieval; Passive microwave radiometry; Precipitation radar ID PRECIPITATION RADAR; PROFILING ALGORITHM; CLOUD PROPERTIES; NETWORK AB The authors have investigated an adaptive neuro fuzzy inference system (ANFIS) for the estimation of hydrometeors from the TRMM microwave imager (TMI). The proposed algorithm, named as Hydro-Rain algorithm, is developed in synergy with the TRMM precipitation radar (PR) observed hydrometeor information. The method retrieves rain rates by exploiting the synergistic relations between the TMI and PR observations in twofold steps. First, the fundamental hydrometeor parameters, liquid water path (LWP) and ice water path (IWP), are estimated from the TMI brightness temperatures. Next, the rain rates are estimated from the retrieved hydrometeor parameters (LWP and IWP). A comparison of the hydrometeor retrievals by the Hydro-Rain algorithm is done with the TRMM PR 2A25 and GPROF 2A12 algorithms. The results reveal that the Hydro-Rain algorithm has good skills in estimating hydrometeor paths LWP and IWP, as well as surface rain rate. An examination of the Hydro-Rain algorithm is also conducted on a super typhoon case, in which the Hydro-Rain has shown very good performance in reproducing the typhoon field. Nevertheless, the passive microwave based estimate of hydrometeors appears to suffer in high rain rate regimes, and as the rain rate increases, the discrepancies with hydrometeor estimates tend to increase as well. (C) 2014 Elsevier B.V. All rights reserved. C1 [Islam, Tanvir] NOAA, NESDIS, Ctr Weather & Climate Predict, College Pk, MD USA. [Islam, Tanvir] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. [Islam, Tanvir; Srivastava, Prashant K.; Rico-Ramirez, Miguel A.; Dai, Qiang; Han, Dawei] Univ Bristol, Dept Civil Engn, Bristol, Avon, England. [Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Gupta, Manika] Indian Inst Technol Delhi, Dept Civil Engn, New Delhi, India. RP Islam, T (reprint author), NOAA, NESDIS, STAR, Ctr Weather & Climate Predict, 5830 Univ Res Ct, College Pk, MD 20740 USA. EM tanvir.islam@noaa.gov RI Islam, Tanvir/F-6922-2011; Rico-Ramirez, Miguel/H-3248-2014; OI Rico-Ramirez, Miguel/0000-0002-8885-4582; Islam, Tanvir/0000-0003-2429-3074 NR 20 TC 10 Z9 10 U1 1 U2 12 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0169-8095 EI 1873-2895 J9 ATMOS RES JI Atmos. Res. PD AUG-SEP PY 2014 VL 145 BP 57 EP 68 DI 10.1016/j.atmosres.2014.03.019 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ8UK UT WOS:000337983100005 ER PT J AU Newell, PT Tsurutani, BT AF Newell, P. T. Tsurutani, B. T. TI Introduction to this special issue: "Sun-Earth system exploration: Moderate and extreme disturbances" SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Editorial Material C1 [Newell, P. T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Newell, PT (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM Patrick.Newell@jhuapl.edu NR 0 TC 0 Z9 0 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD AUG PY 2014 VL 115 SI SI BP 1 EP 1 DI 10.1016/j.jastp.2014.02.004 PG 1 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AJ8VR UT WOS:000337986700001 ER PT J AU Mannucci, AJ Crowley, G Tsurutani, BT Verkhoglyadova, OP Komjathy, A Stephens, P AF Mannucci, A. J. Crowley, G. Tsurutani, B. T. Verkhoglyadova, O. P. Komjathy, A. Stephens, P. TI Interplanetary magnetic field B-y control of prompt total electron content increases during superstorms SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Ionosphere; Geomagnetic storms ID LOW-LATITUDE IONOSPHERE; TRANSPOLAR POTENTIAL SATURATION; GEOMAGNETIC STORMS; THERMOSPHERE MODEL; NOVEMBER 2003; HILL MODEL; ELECTRODYNAMICS; EQUATORIAL; TUTORIAL; CONVECTION AB Large magnitude increases in ionospheric total electron content (TEC) that occur over 1-3 h on the dayside are a significant manifestation of the main phases of superstorms. For the largest superstorms of solar cycle 23 (based on the Dst index), ground networks of GPS receivers measured peak total electron content increases greater than a factor of 2 relative to quiet time TEC averaged over the broad latitude band +/- 40 degrees for local times 1200-1600 LT. Near 30 degrees latitude, the Halloween storms of October 29-30, 2003 appeared to produce storm-time TEC exceeding quiet time values by a factor of 5 within 2-3 h of storm onset, at 1300 LT. The physical cause of these large positive phase ionospheric storms is usually attributed to prompt penetration electric fields (PPEFs) initiated by Region 1 current closure through the ionosphere (Nopper and Carovillano, 1978 mechanism). An unresolved question is what determines variation of the TEC response for different superstorms. It has been suggested that the cross polar cap potential and Region I currents are significant factors in determining PPEF in the equatorial ionosphere, which are related to the solar wind reconnection electric field estimated by Kan-Lee and others. In this paper, we show evidence that suggests B-y may be a significant factor controlling the TEC response during the main phase of superstorms. We analyzed the interplanetary conditions during the period that TEC was increasing for eight superstorms. We find that increasing daytime TEC during superstorms only occurs for large reconnection electric fields when B-y magnitude is less than B-z. The data suggest that B-z is a far more important factor in the TEC response than the reconnection electric field. We also find that TEC decreases following its peak storm-time value for two superstorms, even though B-z remains large and B-y magnitudes are less than B-z. Such decreases during the geomagnetic disturbance may indicate the role of magnetospheric shielding currents, or of changes in the thermosphere that have developed over the prolonged period of large solar wind electric field. Further analysis is warranted covering a wider range of storm intensities on the role of B-y in affecting the daytime TEC response for a range of storm intensities. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Mannucci, A. J.; Tsurutani, B. T.; Verkhoglyadova, O. P.; Komjathy, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Crowley, G.] Atmospher & Space Technol Res Associates, Boulder, CO USA. [Stephens, P.] Google Inc, Santa Monica, CA USA. RP Mannucci, AJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM anthony.j.mannucci@jpl.nasa.gov OI Verkhoglyadova, Olga/0000-0002-9295-9539 NR 60 TC 11 Z9 11 U1 3 U2 19 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD AUG PY 2014 VL 115 SI SI BP 7 EP 16 DI 10.1016/j.jastp.2014.01.001 PG 10 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AJ8VR UT WOS:000337986700003 ER PT J AU Verkhoglyadova, OP Tsurutani, BT Mannucci, AJ Mlynczak, MG Hunt, LA Paxton, LJ AF Verkhoglyadova, O. P. Tsurutani, B. T. Mannucci, A. J. Mlynczak, M. G. Hunt, L. A. Paxton, L. J. TI Ionospheric TEC, thermospheric cooling and Sigma[O/N-2] compositional changes during the 6-17 March 2012 magnetic storm interval (CAWSES II) SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Ionosphere; Thermosphere; Geomagnetic storms ID LOW-LATITUDE; SOLAR; MODEL; TIMED/GUVI; SUPERSTORM AB A series of four geomagnetic storms (the minimum SYM-H similar to-148 nT) occurred during the March 6-17, 2012 in the ascending phase of the solar cycle 24. This interval was selected by CAWSES II for its campaign. The GPS total electron content (TEC) database and JPL's Global Ionospheric Maps (GIM) were used to study vertical TEC (VTEC) for different local times and latitude ranges. The largest response to geomagnetic activity is shown in increases of the low-latitude dayside VTEC. Several GPS sites feature post-afternoon VTEC "bite-outs". During Sudden Impulse (SI+) event on March 8th a peak daytime VTEC restores to about quiet-time values. It is shown that the TIMED/SABER zonal flux of nitric oxide (NO) infrared cooling radiation correlates well with auroral heating. A factor of similar to 5 cooling increase is noted in some storms. The cooling radiation intensifies in the auroral zone and spreads towards the equator. Effects of the storm appear at lower latitudes similar to 18.6 h later. The column density ratio Sigma[O/N-2] is analyzed based on TIMED/GUVI measurements. Both increases (at low latitudes) and decreases (from auroral to middle latitudes) in the ratio occurs during the geomagnetic storms. We suggest that the column density ratio could be enhanced at low to middle latitudes on the dayside partially due to the superfountain effect (atomic oxygen uplift due to ion-neutral drag). It is suggested that decreases in the [O/N-2] ratio at high to middle-latitudes may be caused by high thermospheric temperatures. During SI+ s, there is an increase in Sigma[O/N-2] ratio at auroral latitudes. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Verkhoglyadova, O. P.; Tsurutani, B. T.; Mannucci, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Verkhoglyadova, O. P.] UAH, Ctr Space & Aeron Res, Huntsville, AL USA. [Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Hunt, L. A.] Sci Syst & Applicat Inc, Hampton, VA USA. [Paxton, L. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Verkhoglyadova, OP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Olga.Verkhoglyadova@jpl.nasa.gov RI Paxton, Larry/D-1934-2015; OI Paxton, Larry/0000-0002-2597-347X; Verkhoglyadova, Olga/0000-0002-9295-9539 NR 42 TC 4 Z9 4 U1 0 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD AUG PY 2014 VL 115 SI SI BP 41 EP 51 DI 10.1016/j.jastp.2013.11.009 PG 11 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AJ8VR UT WOS:000337986700007 ER PT J AU Moore, TE Fok, MC Garcia-Sage, K AF Moore, T. E. Fok, M. -C. Garcia-Sage, K. TI The ionospheric outflow feedback loop SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Ionosphere; Feedback; Magnetosphere ID ION OUTFLOW; MAGNETOSPHERE; POLAR; FIELD; WIND; CIRCULATION; PLASMA; REGION; EISCAT; WAVES AB Following a long period of observation and investigation beginning in the early 1970s, it has been firmly established that Earth's magnetosphere is defined as much by the geogenic plasma within it as by the geomagnetic field. This plasma is not confined to the ionosphere proper, defined as the region within a few density scale heights of the F-region plasma density peak. Rather, it fills the flux tubes on which it is created, and circulates throughout the magnetosphere in a pattern driven by solar wind plasma that becomes magnetically connected to the ionosphere by reconnection through the dayside magnetopause. Under certain solar wind conditions, plasma and field energy is stored in the magnetotail rather than being smoothly recirculated back to the dayside. Its release into the downstream solar wind is produced by magnetotail disconnection of stored plasma and fields both continuously and in the form of discrete plasmoids, with associated generation of energetic Earthward-moving bursty bulk flows and injection fronts. A new generation of global circulation models is showing us that outflowing ionospheric plasmas, especially O+, load the system in a different way than the resistive F-region load of currents dissipating energy in the plasma and atmospheric neutral gas. The extended ionospheric load is reactive to the primary dissipation, forming a time-delayed feedback loop within the system. That sets up or intensifies bursty transient behaviors that would be weaker or absent if the ionosphere did not "strike back" when stimulated. Understanding this response appears to be a necessary, if not sufficient, condition for us to gain accurate predictive capability for space weather. However, full predictive understanding of outflow and incorporation into global simulations requires a clear observational and theoretical identification of the causal mechanisms of the outflows. This remains elusive and requires a dedicated mission effort. Published by Elsevier Ltd. C1 [Moore, T. E.; Fok, M. -C.; Garcia-Sage, K.] NASA, Goddard SFC, Greenbelt, MD 20771 USA. RP Moore, TE (reprint author), NASA, Goddard SFC, Greenbelt, MD 20771 USA. FU NASA Postdoctoral Program; Magnetospheric Multiscale (MMS) at NASA Goddard Space Flight Center FX The authors gratefully acknowledge support by the NASA Postdoctoral Program, and the Magnetospheric Multiscale (MMS) at NASA Goddard Space Flight Center. NR 37 TC 7 Z9 7 U1 2 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD AUG PY 2014 VL 115 SI SI BP 59 EP 66 DI 10.1016/j.jastp.2014.02.002 PG 8 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AJ8VR UT WOS:000337986700009 ER PT J AU Keesee, AM Elfritz, JG Fok, MC McComas, DJ Scime, EE AF Keesee, A. M. Elfritz, J. G. Fok, M. -C. McComas, D. J. Scime, E. E. TI Superposed epoch analyses of ion temperatures during CME- and CIR/HSS-driven storms SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Magnetosphere; Geomagnetic storm; CME; High speed stream; Corotating interaction region; Ion temperature ID PLASMA SHEET; GEOMAGNETIC STORMS; TWINS; MODEL AB Coronal mass ejections (CMEs) and corotating interaction regions associated with high speed solar wind streams (CIR/HSSs) drive geomagnetic storms in the terrestrial magnetosphere. Each type of storm driver yields different dynamics of storm evolution. We present results from comparative superposed epoch analyses of global ion temperatures calculated from TWINS energetic neutral atom (ENA) data and simulations using the comprehensive ring current model (CRCM). During the June 2008-April 2012 timeframe, 48 geomagnetic storms (minimum Dst <= -40 nT) occurred. Of these, 21 storms were CME-driven and 15 were driven by CIR/HSSs. Superposed epoch analysis results demonstrate that ion temperatures increase during the recovery phase of CIR/HSS-driven storms, while ions are rapidly heated at the commencement of CME-driven storms then cool over the main phase, particularly for intense (minimum Dst <= -78 nT) CME-driven storms. Higher energy ions are convected to lower L-shells during CME-driven storms, while CIR/HSS-driven storms tend to have average ion temperatures that are higher on the dayside than nightside. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Keesee, A. M.; Elfritz, J. G.; Scime, E. E.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Fok, M. -C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McComas, D. J.] SW Res Inst, San Antonio, TX 78228 USA. [McComas, D. J.] Univ Texas San Antonio, San Antonio, TX 78249 USA. RP Keesee, AM (reprint author), W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. EM amy.keesee@mail.wvu.edu RI Keesee, Amy/J-8194-2014 OI Keesee, Amy/0000-0002-9719-3229 FU NASA EPSCoR [NNX10AN08A]; NSF [AGS-1113478]; WVU FX This work was carried out as a part of the TWINS NASA Explorer mission; work at WVU was supported under subcontract to the Southwest Research Institute, NASA EPSCoR grant NNX10AN08A and NSF grant AGS-1113478. We would like to thank members of the TWINS science team for helpful discussions regarding the TWINS ENA data. We gratefully acknowledge the use of solar wind data and geomagnetic indices provided by OMNIWeb and Kyoto World Data Center for Geomagnetism. NR 27 TC 7 Z9 7 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD AUG PY 2014 VL 115 SI SI BP 67 EP 78 DI 10.1016/j.jastp.2013.08.009 PG 12 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AJ8VR UT WOS:000337986700010 ER PT J AU Huang, YS Richmond, AD Deng, Y Chamberlin, PC Qian, LY Solomon, SC Roble, RG Xiao, Z AF Huang, Yanshi Richmond, Arthur D. Deng, Yue Chamberlin, Phillip C. Qian, Liying Solomon, Stanley C. Roble, Raymond G. Xiao, Zuo TI Wavelength dependence of solar irradiance enhancement during X-class flares and its influence on the upper atmosphere SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Solar flare; FISM; TIE-GCM ID GENERAL-CIRCULATION MODEL; EUV EXPERIMENT; THERMOSPHERE; IONOSPHERE AB The wavelength dependence of solar irradiance enhancement during flare events is one of the important factors in determining how the Thermosphere-Ionosphere (T-I) system responds to flares. To investigate the wavelength dependence of flare enhancement, the Flare Irradiance Spectral Model (FISM) was run for 61 X-class flares. The absolute and the percentage increases of solar irradiance at flare peaks, compared to pre-flare conditions, have clear wavelength dependences. The 0-14 nm irradiance increases much more (similar to 680% on average) than that in the 14-25 nm waveband (similar to 65% on average), except at 24 nm (similar to 220%). The average percentage increases for the 25-105 nm and 122-190 nm wavebands are similar to 120% and similar to 35%, respectively. The influence of 6 different wavebands (0-14 nm, 14-25 nm, 25-105 nm, 105-120 nm, 121.56 nm, and 122-175 nm) on the thermosphere was examined for the October 28th, 2003 flare (X17-class) event by coupling FISM with the National Center for Atmospheric Research (NCAR) Thermosphere-Ionosphere-Electrodynamics General Circulation Model (TIE-GCM) under geomagnetically quiet conditions (Kp=1). While the enhancement in the 0-14 nm waveband caused the largest enhancement of the globally integrated solar heating, the impact of solar irradiance enhancement on the thermosphere at 400 km is largest for the 25-105 nm waveband (EUV), which accounts for about 33 K of the total 45 K temperature enhancement, and similar to 7.4% of the total similar to 11.5% neutral density enhancement. The effect of 122-175 nm flare radiation on the thermosphere is rather small. The study also illustrates that the high-altitude thermospheric response to the flare radiation at 0-175 nm is almost a linear combination of the responses to the individual wavebands. The upper thermospheric temperature and density enhancements peaked 3-5 h after the maximum flare radiation. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Huang, Yanshi] Univ New Mexico, Dept Elect & Comp Engn, Albuquerque, NM 87131 USA. [Richmond, Arthur D.; Qian, Liying; Solomon, Stanley C.; Roble, Raymond G.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Deng, Yue] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. [Chamberlin, Phillip C.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Xiao, Zuo] Peking Univ, Dept Geophys, Beijing 100871, Peoples R China. RP Huang, YS (reprint author), Univ New Mexico, Dept Elect & Comp Engn, Albuquerque, NM 87131 USA. EM huangys@unm.edu; richmond@hao.ucar.edu; yuedeng@uta.edu; phillip.c.chamberlin@nasa.gov; lqian@ucar.edu; stans@ucar.edu; roble@hao.ucar.ed; zxiao@pku.eud.cn RI Solomon, Stanley/J-4847-2012; Chamberlin, Phillip/C-9531-2012; OI Solomon, Stanley/0000-0002-5291-3034; Chamberlin, Phillip/0000-0003-4372-7405; Richmond, Arthur/0000-0002-6708-1023 FU National Science Foundation [ATM0955629]; Air Force Office of Scientific Research [1210429]; National Science Foundation FX We acknowledge the LASP Interactive Solar Irradiance Data center for FISM data. This research was supported by the National Science Foundation through grant ATM0955629 and by the Air Force Office of Scientific Research through grant 1210429. Part of this work was conducted while Y.H. and Y.D. were visitors in the Advanced Study Program at the National Center for Atmospheric Research (NCAR). NCAR is sponsored by the National Science Foundation. NR 40 TC 0 Z9 0 U1 0 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD AUG PY 2014 VL 115 SI SI BP 87 EP 94 DI 10.1016/j.jastp.2013.10.011 PG 8 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AJ8VR UT WOS:000337986700012 ER PT J AU Pendyala, VRR Jacobs, G Ma, WP Klettlinger, JLS Yen, CH Davis, BH AF Pendyala, Venkat Ramana Rao Jacobs, Gary Ma, Wenping Klettlinger, Jennifer L. S. Yen, Chia H. Davis, Burtron H. TI Fischer-Tropsch synthesis: Effect of catalyst particle (sieve) size range on activity, selectivity, and aging of a Pt promoted Co/Al2O3 catalyst SO CHEMICAL ENGINEERING JOURNAL LA English DT Article DE Fischer-Tropsch synthesis; Cobalt catalysts; Sieve size; Activity; Selectivity ID CO/SIO2 CATALYSTS; COBALT CATALYSTS; SUPPORT; DISPERSION; REDUCIBILITY AB The effect of cobalt-alumina catalyst particle (sieve) size range on the performance of a traditional cobalt catalyst (platinum promoted cobalt/alumina) was investigated during Fischer-Tropsch synthesis (FTS) using a continuously stirred tank reactor (CSTR). In this study, the catalyst was sieved into four different size ranges: 20-63, 63-106, 106-180 and 180-355 mu m. CO conversion varied with varying sieve size range under similar reaction conditions. With increasing catalyst sieve size, the CO conversion decreased, except for the smallest sieve size range (20-63 mu m). These results are consistent with the view that, for the larger sieve size range, losses in CO conversion beyond catalyst aging may be explained by filling of the interior of the catalyst particle with heavy wax, thereby blocking available catalytically active sites. The adverse selectivities are directly the result of significant deactivation, since in FT synthesis, selectivity is a function of CO conversion. The loss in CO conversion for the 20-63 mu m range catalyst was higher compared to the other three catalysts; due to the presence of heavy wax (Polywax 3000), the results suggest that the small particles tended to flocculate to larger clusters or were small enough to move at the speed of the liquid. (C) 2014 Elsevier B.V. All rights reserved. C1 [Pendyala, Venkat Ramana Rao; Jacobs, Gary; Ma, Wenping; Davis, Burtron H.] Univ Kentucky, Ctr Appl Energy Res, Lexington, KY 40511 USA. [Klettlinger, Jennifer L. S.; Yen, Chia H.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Davis, BH (reprint author), Univ Kentucky, Ctr Appl Energy Res, 2540 Res Pk Dr, Lexington, KY 40511 USA. EM burtron.davis@uky.edu RI Jacobs, Gary/M-5349-2015 OI Jacobs, Gary/0000-0003-0691-6717 FU Commonwealth of Kentucky (USA); NASA (USA) [NNX11A175A] FX This work carried out at the CAER was supported by the Commonwealth of Kentucky (USA) and a NASA (USA) grant (Relating FTS catalyst properties to performance no: NNX11A175A). NR 20 TC 6 Z9 6 U1 7 U2 53 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 1385-8947 EI 1873-3212 J9 CHEM ENG J JI Chem. Eng. J. PD AUG 1 PY 2014 VL 249 BP 279 EP 284 DI 10.1016/j.cej.2014.03.100 PG 6 WC Engineering, Environmental; Engineering, Chemical SC Engineering GA AJ3GI UT WOS:000337554100033 ER PT J AU Fonollosa, J Rodriguez-Lujan, I Shevade, AV Homer, ML Ryan, MA Huerta, R AF Fonollosa, Jordi Rodriguez-Lujan, Irene Shevade, Abhijit V. Homer, Margie L. Ryan, Margaret A. Huerta, Ramon TI Human activity monitoring using gas sensor arrays SO SENSORS AND ACTUATORS B-CHEMICAL LA English DT Article DE Activity monitoring; Gas sensors; e-Nose; Support vector machines; Remote sensing; Home monitoring ID HOME GAIT ASSESSMENT; PHYSICAL-ACTIVITY; ELECTRONIC NOSE; RECOGNITION; SYSTEM; CALIBRATION; REGRESSION; NETWORKS AB A chemical detection system made of a gas sensor array and algorithms intended to monitor human activity was tested in a NASA spacecraft cabin simulator. Such a chemical-based monitoring system, if extended to home settings, would allow the autonomous detection of emergency situations, thereby postponing the moving of elderly people to assisted living facilities and improving their quality of life. Moreover, in contrast to other monitoring systems based on wearable sensors or video cameras, a monitoring system based on measuring changes in air composition induced by human activities would be non-invasive and would not raise privacy concerns when installed in homes. The third generation of the JPL sensor array was adapted in a small, compact and portable system and deployed in a spacecraft-like room for four weeks while volunteers were performing daily routines. The system was able to predict the total number of people and the level of activity performed in the room, while detecting unexpectedly high concentrations of volatiles. (C) 2014 Elsevier B.V. All rights reserved. C1 [Fonollosa, Jordi; Rodriguez-Lujan, Irene; Huerta, Ramon] Univ Calif San Diego, BioCircuits Inst, La Jolla, CA 92093 USA. [Shevade, Abhijit V.; Homer, Margie L.; Ryan, Margaret A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Fonollosa, J (reprint author), Univ Calif San Diego, BioCircuits Inst, La Jolla, CA 92093 USA. EM fonollosa@ucsd.edu RI Huerta, Ramon/J-4316-2012; Huerta, Ramon/C-9296-2013; Rodriguez-Lujan, Irene/E-8619-2016; Fonollosa, Jordi/L-2303-2014 OI Huerta, Ramon/0000-0003-3925-5169; Huerta, Ramon/0000-0003-3925-5169; Rodriguez-Lujan, Irene/0000-0001-9512-9162; Fonollosa, Jordi/0000-0001-8854-8588 FU Jet Propulsion LaboratoryJet Propulsion Laboratory [2012-1455933] FX This work has been supported by the Jet Propulsion Laboratory under the contract number 2012-1455933. The authors want to dedicate this paper to the memory of their former colleague and friend at UCSD, Dr. Alexander Vergara, who passed away in March 2014. NR 45 TC 7 Z9 7 U1 6 U2 48 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-4005 J9 SENSOR ACTUAT B-CHEM JI Sens. Actuator B-Chem. PD AUG PY 2014 VL 199 BP 398 EP 402 DI 10.1016/j.snb.2014.03.102 PG 5 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation SC Chemistry; Electrochemistry; Instruments & Instrumentation GA AI5AO UT WOS:000336878000054 ER PT J AU Kramar, M Airapetian, V Mikic, Z Davila, J AF Kramar, M. Airapetian, V. Mikic, Z. Davila, J. TI 3D Coronal Density Reconstruction and Retrieving the Magnetic Field Structure during Solar Minimum SO SOLAR PHYSICS LA English DT Article DE Corona, quiet, structures; Magnetic fields, corona ID EMISSION-LINE POLARIZATION; WHITE-LIGHT IMAGES; WHOLE SUN MONTH; ELECTRON-DENSITY; RADIOLOGICAL APPLICATIONS; VECTOR TOMOGRAPHY; MHD MODEL; REPRESENTATION; CALIBRATION; INTEGRALS AB Measurement of the coronal magnetic field is a crucial ingredient in understanding the nature of solar coronal phenomena at all scales. We employed STEREO/COR1 data obtained during a deep minimum of solar activity in February 2008 (Carrington Rotation CR 2066) to retrieve and analyze the three-dimensional (3D) coronal electron density in the range of heights from 1.5 to 4 R-aS (TM) using a tomography method. With this, we qualitatively deduced structures of the coronal magnetic field. The 3D electron-density analysis is complemented by the 3D STEREO/EUVI emissivity in the 195 band obtained by tomography for the same CR. A global 3D MHD model of the solar corona was used to relate the reconstructed 3D density and emissivity to open/closed magnetic-field structures. We show that the density-maximum locations can serve as an indicator of current-sheet position, while the locations of the density-gradient maximum can be a reliable indicator of coronal-hole boundaries. We find that the magnetic-field configuration during CR 2066 has a tendency to become radially open at heliocentric distances greater than 2.5 R-aS (TM). We also find that the potential-field model with a fixed source surface is inconsistent with the boundaries between the regions with open and closed magnetic-field structures. This indicates that the assumption of the potential nature of the coronal global magnetic field is not satisfied even during the deep solar minimum. Results of our 3D density reconstruction will help to constrain solar coronal-field models and test the accuracy of the magnetic-field approximations for coronal modeling. C1 [Kramar, M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Kramar, M.; Airapetian, V.; Davila, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mikic, Z.] Predict Sci Inc, San Diego, CA 92121 USA. RP Kramar, M (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave NE, Washington, DC 20064 USA. EM kramar@cua.edu FU NASA [NNG11PL10A 670.008, SCEX22013D]; NSF [AGS0819971] FX The work of MK has been supported by the NASA Cooperative Agreement NNG11PL10A 670.008 to the Catholic University of America and NSF National Space Weather Program grant AGS0819971. VA acknowledges support from NASA grant SCEX22013D. The authors thank the anonymous referee for the insightful review of the manuscript. NR 55 TC 8 Z9 8 U1 0 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD AUG PY 2014 VL 289 IS 8 BP 2927 EP 2944 DI 10.1007/s11207-014-0525-7 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH7SS UT WOS:000336334900007 ER PT J AU Panesar, NK Innes, DE Schmit, DJ Tiwari, SK AF Panesar, N. K. Innes, D. E. Schmit, D. J. Tiwari, S. K. TI On the Structure and Evolution of a Polar Crown Prominence/Filament System SO SOLAR PHYSICS LA English DT Article DE Prominences, quiescent; Prominences, dynamics; Corona, coronal cavities ID CORONAL MASS EJECTIONS; SOLAR PROMINENCES; QUIESCENT PROMINENCES; MAGNETIC-STRUCTURE; FILAMENT; CAVITY; DYNAMICS; HINODE; MODELS; FIELDS AB Polar crown prominences, that partially circle the Sun's poles between 60A degrees and 70A degrees latitude, are made of chromospheric plasma. We aim to diagnose the 3D dynamics of a polar crown prominence using high-cadence EUV images from the Solar Dynamics Observatory (SDO)/AIA at 304, 171, and 193 and the Ahead spacecraft of the Solar Terrestrial Relations Observatory (STEREO-A)/EUVI at 195 . Using time series across specific structures, we compare flows across the disk in 195 with the prominence dynamics seen on the limb. The densest prominence material forms vertical columns that are separated by many tens of Mm and connected by dynamic bridges of plasma that are clearly visible in 304/171 two-colour images. We also observe intermittent but repetitious flows with velocity 15 km s(-1) in the prominence that appear to be associated with EUV bright points on the solar disk. The boundary between the prominence and the overlying cavity appears as a sharp edge. We discuss the structure of the coronal cavity seen both above and around the prominence. SDO/HMI and GONG magnetograms are used to infer the underlying magnetic topology. The evolution and structure of the prominence with respect to the magnetic field seems to agree with the filament-linkage model. C1 [Panesar, N. K.; Innes, D. E.; Schmit, D. J.; Tiwari, S. K.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Panesar, N. K.] Inst Astrophys Gottingen, Fak Phys, D-37077 Gottingen, Germany. [Tiwari, S. K.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Panesar, NK (reprint author), Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany. EM panesar@mps.mpg.de FU NASA FX We would like to thank the referee for his/her constructive comments. SDO data are courtesy of the NASA/SDO AIA and HMI science teams. STEREO data are courtesy of the STEREO Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) team. GONG magnetogram data obtained by the Global Oscillation Network Group (GONG) project, managed by the National Solar Observatory, which is operated by AURA, Inc. under a cooperative agreement with the National Science Foundation. NKP acknowledges the facilities provided by the MPS. One of the authors, SKT, is supported by an appointment to the NASA Postdoctoral Program at the NASA Marshall Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 65 TC 2 Z9 2 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 AUG PY 2014 VL 289 IS 8 BP 2971 EP 2991 DI 10.1007/s11207-014-0504-z PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH7SS UT WOS:000336334900010 ER PT J AU Richardson, IG von Rosenvinge, TT Cane, HV Christian, ER Cohen, CMS Labrador, AW Leske, RA Mewaldt, RA Wiedenbeck, ME Stone, EC AF Richardson, I. G. von Rosenvinge, T. T. Cane, H. V. Christian, E. R. Cohen, C. M. S. Labrador, A. W. Leske, R. A. Mewaldt, R. A. Wiedenbeck, M. E. Stone, E. C. TI > 25 MeV Proton Events Observed by the High Energy Telescopes on the STEREO A and B Spacecraft and/or at Earth During the First similar to aEuro parts per thousand Seven Years of the STEREO Mission SO SOLAR PHYSICS LA English DT Article DE Solar energetic particles; STEREO; SOHO ID CORONAL MASS EJECTIONS; SOLAR-FLARE PARTICLES; III RADIO-BURSTS; INTERPLANETARY SHOCKS; INNER HELIOSPHERE; PEAK INTENSITIES; GNEVYSHEV GAP; COSMIC-RAYS; 1 AU; PROPAGATION AB Using observations from the High Energy Telescopes (HETs) on the STEREO A and B spacecraft and similar observations from near-Earth spacecraft, we summarize the properties of more than 200 individual > 25 MeV solar proton events, some detected by multiple spacecraft, that occurred from the beginning of the STEREO mission in October 2006 to December 2013, and provide a catalog of these events and their solar sources and associations. Longitudinal dependencies of the electron and proton peak intensities and delays to onset and peak intensity relative to the solar event have been examined for 25 three-spacecraft particle events. Expressed as Gaussians, peak intensities fall off with longitude with sigma=47 +/- 14(a similar to) for 0.7 -aEuro parts per thousand 4 MeV electrons, and sigma=43 +/- 13(a similar to) for 14 -aEuro parts per thousand 24 MeV protons. Several particle events are discussed in more detail, including one on 3 November 2011, in which similar to aEuro parts per thousand 25 MeV protons filled the inner heliosphere within 90 minutes of the solar event, and another on 7 March 2012, in which we demonstrate that the first of two coronal mass ejections that erupted from an active region within similar to aEuro parts per thousand 1 hour was associated with particle acceleration. Comparing the current Solar Cycle 24 with the previous cycle, the first > 25 MeV proton event was detected at Earth in the current solar cycle around one year after smoothed sunspot minimum, compared with a delay of only two months in Cycle 23. Otherwise, solar energetic particle event occurrence rates were reasonably similar during the rising phases of Cycles 23 and 24. However, the rate declined in 2013, reflecting the decline in sunspot number since the peak in the northern-hemisphere sunspot number in November 2011. Observations in late 2013 suggest that the rate may be rising again in association with an increase in the southern sunspot number. C1 [Richardson, I. G.; von Rosenvinge, T. T.; Christian, E. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Richardson, I. G.] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Richardson, I. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Cane, H. V.] Bruny Isl Radio Spectrometer, Bruny Island, Tas, Australia. [Cohen, C. M. S.; Labrador, A. W.; Leske, R. A.; Mewaldt, R. A.; Stone, E. C.] CALTECH, Pasadena, CA 91125 USA. [Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Richardson, IG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM ian.g.richardson@nasa.gov; tycho.t.vonrosenvinge@nasa.gov; hcane@utas.edu.au; eric.r.christian@nasa.gov; cohen@srl.caltech.edu; labrador@srl.caltech.edu; ral@srl.caltech.edu; rmewaldt@srl.caltech.edu; mark.e.wiedenbeck@jpl.nasa.gov; ecs@srl.caltech.edu OI Richardson, Ian/0000-0002-3855-3634 FU NASA; University of California, Berkeley, under NASA [SA2715-26309, NAS5-03131]; German Bundesminister fur Wirtschaft through the Deutsches Zentrum fur Luft- und Raumfahrt (DLR) [50 OC 1302] FX We thank Janet Luhmann of the University of California, Berkeley, for her steadfast support as the Principal Investigator of the STEREO/IMPACT investigation. The work at GSFC, Caltech and JPL was supported by NASA (Caltech and JPL were funded under subcontract SA2715-26309 from the University of California, Berkeley, under NASA Contract NAS5-03131). The LASCO CME catalog at http://cdaw.gsfc.nasa.gov/CME_list/ is generated and maintained at the CDAW Data Center by NASA and The Catholic University of America in cooperation with the Naval Research Laboratory. We particularly appreciate the efforts by S. Yashiro and colleagues to generate daily summary movies of SOHO and STEREO observations (http://cdaw.gsfc.nasa.gov/stereo/daily_movies/), which were very helpful in verifying the solar sources of the SEP events. The CACTUS CME catalog is maintained by the Solar Influences Data Analysis Center at the Royal Observatory of Belgium. The SOHO/ERNE data were obtained from the Space Research Laboratory, University of Turku (http://www.srl.utu.fi/erne_data/). The SOHO/EPHIN project is supported under grant No. 50 OC 1302 by the German Bundesminister fur Wirtschaft through the Deutsches Zentrum fur Luft- und Raumfahrt (DLR). SOHO is a project of international cooperation between ESA and NASA. NR 75 TC 54 Z9 54 U1 0 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD AUG PY 2014 VL 289 IS 8 BP 3059 EP 3107 DI 10.1007/s11207-014-0524-8 PG 49 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH7SS UT WOS:000336334900015 ER PT J AU Jouanny, I Sennour, M Berger, MH Filipov, VB Ievdokyrnova, A Paderno, VN Sayir, A AF Jouanny, I. Sennour, M. Berger, M. H. Filipov, V. B. Ievdokyrnova, A. Paderno, V. N. Sayir, A. TI Effect of Zr substitution by Ti on growth direction and interface structure of LaB6-TixZr1-xB2 directionally solidified eutectics SO JOURNAL OF THE EUROPEAN CERAMIC SOCIETY LA English DT Article DE DSE; Boride; Interfaces; Crystallographic orientation ID COMPOSITE; CRYSTALLOGRAPHY; DIBORIDES; ZIRCONIUM; FEATURES; ALLOYS AB Boride ceramics were directionally solidified around LaB6-(TixZr1-x)B-2 eutectic compositions. The directionally solidified rods were composed of LaB6 rich concentric belts surrounding large eutectic regions with a dense and uniform distribution of (TixZr1-x)B-2 fibers of 0.6 mu m in diameter inside a LaB6 matrix. The di- and hexa-boride mole fractions at eutectic points have been more accurately defined for x = 0-0.76. Fiber growth directions were modified by the addition of titanium. Diboride (subscript 2) fibers grew along [0 0 0 1](2) for x = 0 and along ((1) over bar 1 0 0)(2) for x not equal 0. The orientation of the hexaboride (subscript 6) matrix was unchanged with or without titanium addition. The favored crystallographic orientation relationship was: [0 0 1](6)//[0 0 0 1](2) and (1 1 0)(6)//(1 1 (2) over bar 0)(2) and ((1) over bar 1 0)(6)//((1) over bar 1 0 0)(2) for any x value. The dominant interfaces were {1 1 0}(6)//{1 1 (2) over bar 0}(2) for x = 0 and (0 0 1)(6)//(0 0 0 1)(2) for x not equal 0, the latter being expected to be energetically more favorable, as predicted by a 2D geometrical model. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Jouanny, I.; Sennour, M.; Berger, M. H.] MINES ParisTech, Ctr Mat, UMR CNRS 7633, F-91003 Evry, France. [Filipov, V. B.; Ievdokyrnova, A.; Paderno, V. N.] Natl Acad Sci Ukraine, Frantsevitch Inst Problems Mat Sci, Kiev, Ukraine. [Sayir, A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Berger, MH (reprint author), MINES ParisTech, Ctr Mat, BP 87, F-91003 Evry, France. EM marie-helene.berger@mines-paristech.fr RI Berger, Marie-Helene/B-9785-2013 FU Air Force Office of Scientific Research [FA9550-09-1-0312] FX Supported by the Air Force Office of Scientific Research under grant AFOSR No. FA9550-09-1-0312. NR 19 TC 0 Z9 0 U1 3 U2 20 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0955-2219 EI 1873-619X J9 J EUR CERAM SOC JI J. Eur. Ceram. Soc. PD AUG PY 2014 VL 34 IS 9 SI SI BP 2101 EP 2109 DI 10.1016/j.jeurceramsoc.2014.01.026 PG 9 WC Materials Science, Ceramics SC Materials Science GA AH1HZ UT WOS:000335872500009 ER PT J AU Tanner, A Gaier, T Imbriale, W Kangaslahti, P Lambrigtsen, B Lim, B AF Tanner, Alan Gaier, Todd Imbriale, William Kangaslahti, Pekka Lambrigtsen, Bjorn Lim, Boon TI A Dual-Gain Design for the Geostationary Synthetic Thinned Array Radiometer SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Aperture synthesis; interferometer array; microwave radiometer ID GEOSTAR DEMONSTRATOR INSTRUMENT AB Anew geometry for synthetic aperture radiometers is presented which increases the distance between adjacent elements in the array without changing the visibility sample density in the u-v plane. This provides room for higher elemental antenna gain, which improves both the overall system sensitivity and alias rejection in the synthesized image-both critical requirements for the Earth observing application. The geometry is derived from the simple Y-array geometry by shifting alternate elements within an otherwise linear array arm into two or more rows of antennas. The resulting system largely retains the same hexagonal sample grid in the u-v plane of the visibility function, yet allows for an elemental antenna aperture that is physically larger than the u-v sample spacing. Only the shortest visibility baselines are lost, and a small dedicated low-gain array must be added to the system to recover these baselines. The radiometer is thus divided between a large high-gain array and a small low-gain array. Since the sensitivity (delta-T) of the system is dominated by that of the large array, this approach greatly improves the overall system sensitivity-in this letter, by a factor of 9 (or, equivalently, factor 81 integration time). C1 [Tanner, Alan; Gaier, Todd; Imbriale, William; Kangaslahti, Pekka; Lambrigtsen, Bjorn; Lim, Boon] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tanner, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 9 TC 2 Z9 2 U1 0 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD AUG PY 2014 VL 11 IS 8 BP 1340 EP 1344 DI 10.1109/LGRS.2013.2293318 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AD2VY UT WOS:000333095200006 ER PT J AU Le Vine, DM de Matthaeis, P Ruf, CS AF Le Vine, David M. de Matthaeis, Paolo Ruf, Christopher S. TI Aquarius RFI Detection and Mitigation Algorithm: Assessment and Examples SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Interference; microwave radiometry; remote sensing ID L-BAND; SURFACE SALINITY; RADIOMETER; SPACE AB Aquarius is an L-band radiometer system designed to map sea surface salinity from space. This is a sensitive measurement, and protection from radio frequency interference (RFI) is important for success. An initial look at the performance of the Aquarius RFI detection and mitigation algorithm is reported together with examples of the global distribution of RFI at the L-band. To protect against RFI, Aquarius employs rapid sampling (10 ms) and a "glitch" detection algorithm that looks for outliers among the samples. Samples identified as RFI are removed, and the remainder is averaged to produce an RFI-free signal for the salinity retrieval algorithm. The RFI detection algorithm appears to work well over the ocean with modest rates for false alarms (5%) and missed detection. The global distribution of RFI coincides well with population centers and is consistent with observations reported by the Soil Moisture and Ocean Salinity mission. C1 [Le Vine, David M.; de Matthaeis, Paolo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ruf, Christopher S.] Univ Michigan, Ann Arbor, MI 48109 USA. RP Le Vine, DM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Ruf, Christopher/I-9463-2012 NR 21 TC 15 Z9 15 U1 2 U2 27 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2014 VL 52 IS 8 BP 4574 EP 4584 DI 10.1109/TGRS.2013.2282595 PG 11 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AC5ZC UT WOS:000332598500008 ER PT J AU Friedline, AW Zachariah, MM Johnson, K Thomas, KJ Middaugh, AN Garimella, R Powell, DR Vaishampayan, PA Rice, CV AF Friedline, Anthony W. Zachariah, Malcolm M. Johnson, Karen Thomas, Kieth J., III Middaugh, Amy N. Garimella, Ravindranath Powell, Douglas R. Vaishampayan, Parag A. Rice, Charles V. TI Water Behavior in Bacterial Spores by Deuterium NMR Spectroscopy SO JOURNAL OF PHYSICAL CHEMISTRY B LA English DT Article ID BACILLUS-SUBTILIS SPORES; CALCIUM DIPICOLINATE TRIHYDRATE; NUCLEAR-MAGNETIC-RESONANCE; ACID-SOLUBLE PROTEINS; SOLAR UV-RADIATION; SOLID-STATE NMR; H-2 NMR; HEAT-RESISTANCE; CA2+-DIPICOLINIC ACID; DYNAMIC STRUCTURE AB Dormant bacterial spores are able to survive long periods of time without nutrients, withstand harsh environmental conditions, and germinate into metabolically active bacteria when conditions are favorable. Numerous factors influence this hardiness, including the spore structure and the presence of compounds to protect DNA from damage. It is known that the water content of the spore core plays a role in resistance to degradation, but the exact state of water inside the core is a subject of discussion. Two main theories present themselves: either the water in the spore core is mostly immobile and the core and its components are in a glassy state, or the core is a gel with mobile water around components which themselves have limited mobility. Using deuterium solid-state NMR experiments, we examine the nature of the water in the spore core. Our data show the presence of unbound water, bound water, and deuterated biomolecules that also contain labile deuterons. Deuterium-hydrogen exchange experiments show that most of these deuterons are inaccessible by external water. We believe that these unreachable deuterons are in a chemical bonding state that prevents exchange. Variable-temperature NMR results suggest that the spore core is more rigid than would be expected for a gel-like state. However, our rigid core interpretation may only apply to dried spores whereas a gel core may exist in aqueous suspension. Nonetheless, the gel core, if present, is inaccessible to external water. C1 [Friedline, Anthony W.; Zachariah, Malcolm M.; Johnson, Karen; Thomas, Kieth J., III; Middaugh, Amy N.; Garimella, Ravindranath; Powell, Douglas R.; Rice, Charles V.] Univ Oklahoma, Dept Chem & Biochem, Stephenson Life Sci Res Ctr, Norman, OK 73019 USA. [Vaishampayan, Parag A.] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA. RP Rice, CV (reprint author), Univ Oklahoma, Dept Chem & Biochem, Stephenson Life Sci Res Ctr, 101 Stephenson Pkwy, Norman, OK 73019 USA. EM rice@ou.edu FU National Institutes of Health [1R01GM090064-01]; NASA EPSCoR Research Infrastructure Development (RID) grant [NN07AL49A]; University of Oklahoma FX This work is supported by the National Institutes of Health (1R01GM090064-01), a NASA EPSCoR Research Infrastructure Development (RID) grant (NN07AL49A), and the University of Oklahoma. We also wish to express our gratitude to Dr. Kasthuri Venkateswaran, California Institute of Technology, Jet Propulsion Laboratory, NASA, for insights and helpful discussions. NR 59 TC 5 Z9 5 U1 3 U2 12 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1520-6106 J9 J PHYS CHEM B JI J. Phys. Chem. B PD JUL 31 PY 2014 VL 118 IS 30 BP 8945 EP 8955 DI 10.1021/jp5025119 PG 11 WC Chemistry, Physical SC Chemistry GA AM5VX UT WOS:000339930200004 PM 24950158 ER PT J AU Jensen, ELN Akeson, R AF Jensen, Eric L. N. Akeson, Rachel TI Misaligned protoplanetary disks in a young binary star system SO NATURE LA English DT Article ID ON CIRCUMSTELLAR DISK; T-TAURI STARS; PLANETARY ORBITS; ACCRETION DISCS; TRIPLE SYSTEM; V4046 SGR; MU-M; EVOLUTION; PERTURBATIONS; OBLIQUITIES AB Many extrasolar planets follow orbits that differ from the nearly coplanar and circular orbits found in our Solar System; their orbits may be eccentric(1) or inclined with respect to the host star's equator(2,3), and the population of giant planets orbiting close to their host stars suggests appreciable orbital migration(4). There is at present no consensus on what produces such orbits. Theoretical explanations often invoke interactions with a binary companion star in an orbit that is inclined relative to the planet's orbital plane(4,5). Such mechanisms require significant mutual inclinations between the planetary and binary star orbital planes. The protoplanetary disks in a few young binaries are misaligned(6-12), but often the measurements of these mis-alignments are sensitive only to a small portion of the inner disk, and the three-dimensional misalignment of the bulk of the planet-forming disk mass has hitherto not been determined. Here we report that the protoplanetary disks in the young binary system HK Tauri are misaligned by 60 to 68 degrees, such that one or both of the disks are significantly inclined to the binary orbital plane. Our results demonstrate that the necessary conditions exist for misalignment-driven mechanisms to modify planetary orbits, and that these conditions are present at the time of planet formation, apparently because of the binary formation process. C1 [Jensen, Eric L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Akeson, Rachel] CALTECH, IPAC, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. RP Jensen, ELN (reprint author), Swarthmore Coll, Dept Phys & Astron, 500 Coll Ave, Swarthmore, PA 19081 USA. EM ejensen1@swarthmore.edu OI Jensen, Eric/0000-0002-4625-7333 NR 47 TC 28 Z9 28 U1 2 U2 6 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JUL 30 PY 2014 VL 511 IS 7511 BP 567 EP + DI 10.1038/nature13521 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM0VT UT WOS:000339566300029 PM 25079553 ER PT J AU Molotch, NP Meromy, L AF Molotch, Noah P. Meromy, Leah TI Physiographic and climatic controls on snow cover persistence in the Sierra Nevada Mountains SO HYDROLOGICAL PROCESSES LA English DT Article; Proceedings Paper CT Eastern Snow Conference (ESC) CY JUN 04-06, 2013 CL Huntsville, CANADA DE snow hydrology; remote sensing; water resources ID WESTERN UNITED-STATES; RIO-GRANDE HEADWATERS; TELEMETRY SNOTEL DATA; SUB-ALPINE FOREST; WATER EQUIVALENT; SPATIAL-DISTRIBUTION; THEMATIC MAPPER; GRAIN-SIZE; MODEL; VARIABILITY AB The persistence of snow cover across mountainous landscapes influences land-atmosphere energy exchange, water availability, the partitioning of snowmelt into various hydrologic pathways, vegetation productivity, and fluxes of nutrients. Understanding the processes controlling snow cover persistence has been limited as relationships between physiography, climate, and snow persistence are nonlinear and difficult to characterize empirically. The work detailed herein uses 7 years of remotely sensed snow cover persistence observed from the Moderate Resolution Imaging Spectroradiometer over the Sierra Nevada Mountains as a dependent variable in binary regression tree models with a suite of independent variables comprised of both physiographic and climatic metrics. Annual snow cover persistence over 2001-2007 revealed significant inter-annual variability, with domain-average snow persistence values exceeding 4.01 (i. e. early April) in the wettest year of 2005 and reaching as low as 2.90 (i. e. late February) in the driest year of 2007. Regression tree models revealed that elevation was the most important explanatory variable regarding snow cover persistence, ranking first in the hierarchical models in 10 out of 13 watersheds. Precipitation (Feather and Owens River basins) and temperature (Kern River basin) were the first-ranking variables in the remaining three watersheds. Second, the order variables of importance included vegetation, which ranked between 2nd and 5th in 10 of 13 watersheds, and slope, which ranked 4th and 5th in 12 of the 13 watersheds. Interestingly, solar radiation and aspect were of tertiary importance but were more influential in watersheds with north-south orientation (e. g. in the Feather, Mokelumne and Stanislaus watersheds). These results have implications for understanding the sensitivity of snow cover persistence to changes in climate as watersheds where elevation and/or temperature strongly influence snow cover persistence may be more sensitive to future warming. Further work is needed to identify associated ecosystem sensitivities to future changes in snow cover persistence. Copyright (C) 2014 John Wiley & Sons, Ltd. C1 [Molotch, Noah P.; Meromy, Leah] Univ Colorado, Inst Arctic & Alpine Res, Dept Geog, Boulder, CO 80303 USA. [Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Molotch, NP (reprint author), Univ Colorado, Inst Arctic & Alpine Res, Dept Geog, Boulder, CO 80303 USA. EM Noah.Molotch@colorado.edu RI Zhang, Jianming/A-2994-2011; Molotch, Noah/C-8576-2009 OI Zhang, Jianming/0000-0001-7053-7696; FU NASA [NNX08AH18G, NNX11AK35A, NNX11AK35G, NNX10AO97G]; NSF [EAR 1032295, EAR 1141764]; USDA [2012-67003-19802]; NOAA RISA Western Water Assessment fund; United States American Recovery and Reinvestment Act fund FX This research was supported by NASA grants NNX08AH18G, NNX11AK35A, NNX11AK35G and NNX10AO97G, NSF grants EAR 1032295 and EAR 1141764, USDA grant 2012-67003-19802, the NOAA RISA Western Water Assessment and United States American Recovery and Reinvestment Act funds. Part of NPM's contributions for this study was carried out on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 86 TC 2 Z9 2 U1 3 U2 40 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0885-6087 EI 1099-1085 J9 HYDROL PROCESS JI Hydrol. Process. PD JUL 30 PY 2014 VL 28 IS 16 SI SI BP 4573 EP 4586 DI 10.1002/hyp.10254 PG 14 WC Water Resources SC Water Resources GA AM2YO UT WOS:000339717800004 ER PT J AU Sugg, JW Perry, LB Hall, DK Riggs, GA Badurek, CA AF Sugg, Johnathan W. Perry, L. Baker Hall, Dorothy K. Riggs, George A. Badurek, Christopher A. TI Satellite perspectives on the spatial patterns of new snowfall in the Southern Appalachian Mountains SO HYDROLOGICAL PROCESSES LA English DT Article; Proceedings Paper CT Eastern Snow Conference (ESC) CY JUN 04-06, 2013 CL Huntsville, CANADA DE fractional snow cover; MODIS; synoptic-scale circulation; Southern Appalachian Mountains ID FLOW SNOWFALL; NEW-ZEALAND; MODIS; COVER; ALBEDO; PRECIPITATION; TURKEY; PRODUCTS; TERRAIN; FORESTS AB The Southern Appalachian Mountains (SAM) are a heavily forested mid-latitude mountain region that provide an ideal location for assessing the suitability of satellite-derived snow maps and explicitly linking atmospheric circulation to the spatial patterns of new snowfall. Although a variety of synoptic-scale circulation regimes contribute to mean annual snowfall, which ranges from roughly 25 cm in the lowest valleys to over 250 cm at the highest elevations, atmospheric circulation processes have largely been absent from efforts seeking to quantify the spatial patterns of new snowfall. In this paper, we examine the suitability of fractional snow cover (FSC) maps from the Moderate Resolution Imaging Spectroradiometer (MODIS) and determine the spatial extent of snowfall according to synoptic-scale circulation. FSC maps are analysed after 122 snow events from 2006 to 2012 to provide a suitability analysis of MODIS products for use in the SAM. For each event, we calculate FSC distribution and total snow-covered area and compare it with available in situ observations. Results indicate that the SAM presents unique meteorological, physical, and spectral characteristics that are ideal for evaluating the suitability of MODIS for measuring snow cover. Out of 122 observed snow events, 63 are considered suitable for analysis with the FSC maps. The highest FSC values are observed after Gulf/Atlantic lows and south-eastward tracking clipper systems. We conclude that MODIS data can be successfully used to link broader atmospheric circulation processes of snowfall with the spatial patterns of snow cover. Copyright (C) 2014 John Wiley & Sons, Ltd. C1 [Sugg, Johnathan W.] Univ N Carolina, Dept Geog, Chapel Hill, NC 27599 USA. [Perry, L. Baker; Badurek, Christopher A.] Appalachian State Univ, Dept Geog & Planning, Boone, NC 28608 USA. [Hall, Dorothy K.; Riggs, George A.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Riggs, George A.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Sugg, JW (reprint author), Univ N Carolina, Dept Geog, Chapel Hill, NC 27599 USA. EM jwsugg@live.unc.edu RI Badurek, Christopher/A-8114-2015 OI Badurek, Christopher/0000-0001-5741-4333 FU North Carolina Space Grant; Appalachian State University Department of Geography and Planning; Office of Student Research; Cratis D. Williams Graduate School FX The authors thank the following data sources: the NASA's REVERB ECHO Data Portal, the NWS COOP network, National Oceanic and Atmospheric Administration's Hydrometeorological Prediction Center, the State Climate Office of North Carolina, and the University of Wisconsin-Madison Space Science and Engineering Center. Funding support was provided by the North Carolina Space Grant, Appalachian State University Department of Geography and Planning, Office of Student Research, and the Cratis D. Williams Graduate School. The authors declare no conflict of interest. NR 37 TC 1 Z9 1 U1 2 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0885-6087 EI 1099-1085 J9 HYDROL PROCESS JI Hydrol. Process. PD JUL 30 PY 2014 VL 28 IS 16 SI SI BP 4602 EP 4613 DI 10.1002/hyp.10196 PG 12 WC Water Resources SC Water Resources GA AM2YO UT WOS:000339717800006 ER PT J AU Parker, ET Zhou, MS Burton, AS Glavin, DP Dworkin, JP Krishnamurthy, R Fernandez, FM Bada, JL AF Parker, Eric T. Zhou, Manshui Burton, Aaron S. Glavin, Daniel P. Dworkin, Jason P. Krishnamurthy, Ramanarayanan Fernandez, Facundo M. Bada, Jeffrey L. TI A Plausible Simultaneous Synthesis of Amino Acids and Simple Peptides on the Primordial Earth SO ANGEWANDTE CHEMIE-INTERNATIONAL EDITION LA English DT Article DE amino acids; cyanamide; mass spectrometry; peptides; polymerization ID SPARK DISCHARGE EXPERIMENT; PREBIOTIC CHEMISTRY; MURCHISON METEORITE; HYDROLYSIS; EVOLUTION; CYANAMIDE; ATMOSPHERE; OCEAN AB Following his seminal work in 1953, Stanley Miller conducted an experiment in 1958 to study the polymerization of amino acids under simulated early Earth conditions. In the experiment, Miller sparked a gas mixture of CH4, NH3, and H2O, while intermittently adding the plausible prebiotic condensing reagent cyanamide. For unknown reasons, an analysis of the samples was not reported. We analyzed the archived samples for amino acids, dipeptides, and diketopiperazines by liquid chromatography, ion mobility spectrometry, and mass spectrometry. A dozen amino acids, 10 glycine-containing dipeptides, and 3 glycine-containing diketopiperazines were detected. Miller's experiment was repeated and similar polymerization products were observed. Aqueous heating experiments indicate that Strecker synthesis intermediates play a key role in facilitating polymerization. These results highlight the potential importance of condensing reagents in generating diversity within the prebiotic chemical inventory. C1 [Parker, Eric T.; Zhou, Manshui; Fernandez, Facundo M.] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA. [Burton, Aaron S.] NASA, Astromat Res & Explorat Sci Directorate, Johnson Space Ctr, Houston, TX 77058 USA. [Glavin, Daniel P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Krishnamurthy, Ramanarayanan] Scripps Res Inst, Dept Chem, La Jolla, CA 92037 USA. [Bada, Jeffrey L.] Univ Calif San Diego, Scripps Inst Oceanog, Geophys Res Div, La Jolla, CA 92093 USA. RP Fernandez, FM (reprint author), Georgia Inst Technol, Sch Chem & Biochem, 901 Atlantic Dr NW, Atlanta, GA 30332 USA. EM facundo.fernandez@chemistry.gatech.edu; jbada@ucsd.edu RI Burton, Aaron/H-2212-2011; Glavin, Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012; OI Burton, Aaron/0000-0002-7137-1605; Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997; Krishnamurthy, Ramanarayanan/0000-0001-5238-610X FU Center for Chemical Evolution at the Georgia Institute of Technology by NSF [CHE-1004570]; Center for Chemical Evolution at the Georgia Institute of Technology by NASA Astrobiology Program (NSF) [CHE-100457]; Marine Biology Laboratory's NASA Planetary Biology Internship Program; NASA Postdoctoral Program at the Goddard Space Flight Center; NASA FX This research was supported by the Center for Chemical Evolution at the Georgia Institute of Technology, jointly supported by the NSF and the NASA Astrobiology Program (NSF CHE-1004570). E.T.P. acknowledges financial support from the Marine Biology Laboratory's NASA Planetary Biology Internship Program. A.S.B. acknowledges support from the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. J.P.D. and D.P.G. acknowledge the Goddard Center for Astrobiology and the NASA Astrobiology Institute. We are appreciative of the Mandeville Special Collections at the Geisel Library on the campus of the University of California, San Diego for archiving Miller's original laboratory notebooks and providing assistance with retrieving them. NR 42 TC 12 Z9 15 U1 8 U2 75 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 1433-7851 EI 1521-3773 J9 ANGEW CHEM INT EDIT JI Angew. Chem.-Int. Edit. PD JUL 28 PY 2014 VL 53 IS 31 BP 8132 EP 8136 DI 10.1002/anie.201403683 PG 5 WC Chemistry, Multidisciplinary SC Chemistry GA AN3WZ UT WOS:000340520700026 PM 24966137 ER PT J AU Gronoff, G Rahmati, A SimonWedlund, C Mertens, CJ Cravens, TE Kallio, E AF Gronoff, Guillaume Rahmati, Ali SimonWedlund, Cyril Mertens, Christopher J. Cravens, Thomas E. Kallio, Esa TI The precipitation of keV energetic oxygen ions at Mars and their effects during the comet Siding Spring approach SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LYMAN-ALPHA OBSERVATIONS; C/2013 A1; PICKUP IONS; C/1996 B2; IONOSPHERE; HYAKUTAKE; DEGRADATION; ATMOSPHERE; SPACECRAFT; TRANSPORT AB Comet Siding Spring C/2013 A1 will pass Mars on 19 October 2014, entailing particle and dust precipitation in the Martian upper atmosphere and a potential dust hazard for orbiters. An estimate of the flux of energetic O+ ions picked up by the solar wind from the cometary coma is shown, with an increase of the O+ flux above 50 keV by 2 orders of magnitude. While the ionization of Mars' upper atmosphere by precipitating O+ ions is expected to be negligible compared to solar EUV-XUV ionization, it is of the same order of magnitude at 110 km altitude during the cometary passage, leading to detectable increases in ionospheric densities. Cometary O+ pickup ion precipitation is expected to be the major nightside ionization source, creating a temporary ionosphere and a global airglow. These effects are dependent on the solar and cometary activities at the time of the encounter. C1 [Gronoff, Guillaume; Mertens, Christopher J.] NASA Langley Res Ctr, Sci Directorate, Chem & Dynam Branch, Hampton, VA 23681 USA. [Gronoff, Guillaume] SSAI, Hampton, VA USA. [Rahmati, Ali; Cravens, Thomas E.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [SimonWedlund, Cyril; Kallio, Esa] Aalto Univ, Sch Elect Engn, Dept Radio Sci & Engn, Aalto, Finland. RP Gronoff, G (reprint author), NASA Langley Res Ctr, Sci Directorate, Chem & Dynam Branch, Hampton, VA 23681 USA. EM Guillaume.P.Gronoff@nasa.gov RI Kallio, Esa/F-9410-2014; OI Kallio, Esa/0000-0002-9791-804X; Gronoff, Guillaume/0000-0002-0331-7076 NR 49 TC 9 Z9 9 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2014 VL 41 IS 14 BP 4844 EP 4850 DI 10.1002/2014GL060902 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AN4CU UT WOS:000340536000006 ER PT J AU Poppe, AR Sarantos, M Halekas, JS Delory, GT Saito, Y Nishino, M AF Poppe, A. R. Sarantos, M. Halekas, J. S. Delory, G. T. Saito, Y. Nishino, M. TI Anisotropic solar wind sputtering of the lunar surface induced by crustal magnetic anomalies SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID FIELDS; EXOSPHERE; REGOLITH; ATOMS AB The lunar exosphere is generated by several processes each of which generates neutral distributions with different spatial and temporal variability. Solar wind sputtering of the lunar surface is a major process for many regolith-derived species and typically generates neutral distributions with a cosine dependence on solar zenith angle. Complicating this picture are remanent crustal magnetic anomalies on the lunar surface, which decelerate and partially reflect the solar wind before it strikes the surface. We use Kaguya maps of solar wind reflection efficiencies, Lunar Prospector maps of crustal field strengths, and published neutral sputtering yields to calculate anisotropic solar wind sputtering maps. We feed these maps to a Monte Carlo neutral exospheric model to explore three-dimensional exospheric anisotropies and find that significant anisotropies should be present in the neutral exosphere depending on selenographic location and solar wind conditions. Better understanding of solar wind/crustal anomaly interactions could potentially improve our results. C1 [Poppe, A. R.; Halekas, J. S.; Delory, G. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Poppe, A. R.; Sarantos, M.; Halekas, J. S.; Delory, G. T.] NASA Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Mountain View, CA USA. [Sarantos, M.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA. [Sarantos, M.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Saito, Y.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Tokyo, Japan. [Nishino, M.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. RP Poppe, AR (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM poppe@ssl.berkeley.edu OI Poppe, Andrew/0000-0001-8137-8176; Halekas, Jasper/0000-0001-5258-6128 FU NASA's Lunar Atmospheric and Dust Environment Explorer (LADEE) Guest Investigator program [NNX13AO71G, NNX13AO74G]; NASA's Solar System Exploration Research Virtual Institute FX The authors gratefully acknowledge support from NASA's Lunar Atmospheric and Dust Environment Explorer (LADEE) Guest Investigator program, grants NNX13AO71G (A. R. P. and J.S.H.) and NNX13AO74G (M. S.). The authors also acknowledge support by NASA's Solar System Exploration Research Virtual Institute. This publication is SSERVI contribution SSERVI-2014-097. The Kaguya data used in this study are available upon request to the authors, while the Lunar Prospector data can be found in the NASA Planetary Data System (PDS). NR 37 TC 5 Z9 5 U1 1 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2014 VL 41 IS 14 BP 4865 EP 4872 DI 10.1002/2014GL060523 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AN4CU UT WOS:000340536000009 ER PT J AU Schorghofer, N AF Schorghofer, Norbert TI Migration calculations for water in the exosphere of the Moon: Dusk-dawn asymmetry, heterogeneous trapping, and D/H fractionation SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LUNAR POLAR-REGIONS; SOLAR-WIND; PARENT MOLECULES; ICE; SURFACE; POLES; VOLATILES; MERCURY AB Water ice is trapped in permanently shadowed craters near the lunar poles, where it is thought to have arrived from an exogenic or endogenic source via ballistic hops. We use a model of the migration of water molecules in the lunar exosphere to investigate three problems: (1) A strong continuous source would lead to an enhanced concentration of H2O at the morning terminator but not at the evening terminator. Hence, spectral features observed at both terminators do not suggest that there is diurnal migration of volatiles. (2) Cold trapping after a comet impact leads to an unequal partitioning between the two hemispheres depending on the latitude of the impact but to nearly equal partitioning with respect to longitude. (3) The D/H fractionation as the water molecules migrate toward the poles is small. Hence, the isotopic composition of ice deposits in the cold traps can be related to that of the source. C1 [Schorghofer, Norbert] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Schorghofer, Norbert] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. RP Schorghofer, N (reprint author), Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. EM norbert@hawaii.edu FU National Aeronautics and Space Administration through the NASA Astrobiology Institute [NNA09DA77A] FX This material is based upon work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative agreement NNA09DA77A issued through the Office of Space Science. The author is also grateful for the hospitality of the International Space Science Institute (ISSI) in Bern and the Keck Institute for Space Studies (KISS) at Caltech. NR 28 TC 5 Z9 5 U1 1 U2 3 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 JUL 28 PY 2014 VL 41 IS 14 BP 4888 EP 4893 DI 10.1002/2014GL060820 PG 6 WC Geosciences, Multidisciplinary SC Geology GA AN4CU UT WOS:000340536000012 ER PT J AU Qiu, JX Crow, WT Nearing, GS Mo, XG Liu, SX AF Qiu, Jianxiu Crow, Wade T. Nearing, Grey S. Mo, Xingguo Liu, Suxia TI The impact of vertical measurement depth on the information content of soil moisture times series data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SEQUENTIAL ASSIMILATION; ERS SCATTEROMETER; NEAR-SURFACE; VALIDATION; PRODUCTS; FILTER AB Using a decade of ground-based soil moisture observations acquired from the United States Department of Agriculture's Soil Climate Analysis Network (SCAN), we calculate the mutual information (MI) content between multiple soil moisture variables and near-future vegetation condition to examine the existence of emergent drought information in vertically integrated (surface to 60 cm) soil moisture observations (theta(0-60) ([cm])) not present in either superficial soil moisture observations (theta(5) ([cm])) or a simple low-pass transformation of theta(5). Results suggest that while theta(0-60) is indeed more valuable than theta(5) for predicting near-future vegetation anomalies, the enhanced information content in theta(0-60) soil moisture can be effectively duplicated by the low-pass transformation of theta(5). This implies that, for drought monitoring applications, the shallow vertical penetration depth of microwave-based theta(5) retrievals does not represent as large a practical limitation as commonly perceived. C1 [Qiu, Jianxiu; Mo, Xingguo; Liu, Suxia] Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, Key Lab Water Cycle & Related Land Surface Proc, Beijing, Peoples R China. [Qiu, Jianxiu; Crow, Wade T.] ARS, USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [Nearing, Grey S.] NASA Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD USA. RP Crow, WT (reprint author), ARS, USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. EM Wade.Crow@ars.usda.gov RI Qiu, Jianxiu/O-6255-2016 OI Qiu, Jianxiu/0000-0002-1275-4171 FU Natural Science Foundation of China [31171451]; Key Project for the Strategic Science Plan in IGSNRR, CAS [2012ZD003]; Chinese Scholarship Council; NASA Terrestrial Ecology Program [NNH09ZDA001N] FX The soil moisture data set for this paper is available at USDA SCAN website (see http://www.wcc.nrcs.usda.gov/scan/), and MODIS surface reflectance and land cover data are available at http://modis.gsfc.nasa.gov. Thanks to the Natural Science Foundation of China grant (31171451), the Key Project for the Strategic Science Plan in IGSNRR, CAS (2012ZD003), and the Chinese Scholarship Council for supporting the first author to conduct research at the USDA-ARS Hydrology and Remote Sensing Laboratory. This work was also partially supported by a grant from the NASA Terrestrial Ecology Program (NNH09ZDA001N) to W. T. Crow. NR 29 TC 5 Z9 5 U1 4 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2014 VL 41 IS 14 BP 4997 EP 5004 DI 10.1002/2014GL060017 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AN4CU UT WOS:000340536000025 ER PT J AU Kwok, R AF Kwok, R. TI Simulated effects of a snow layer on retrieval of CryoSat-2 sea ice freeboard SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB The impact of a snow layer on the location of the tracking point (RP) for ranging to the sea ice surface in CryoSat-2 synthetic aperture interferometric radar altimeter waveforms is simulated. With a range resolution of similar to 47 cm, the response of the air-snow (a-s) interface broadens the response of the snow-ice (s-i) interface and displaces the RP toward the altimeter. This effect is largest when the strengths of their returns are comparable and when snow thicknesses are > 20 cm. On the other hand, the RP is displaced away from the altimeter when the reduced propagation speed in the snow layer is not accounted for. This analysis examines the dependence of these competing corrections on snow thickness and the relative scattering strengths of the interfaces and the sensitivity of two different tracking approaches (leading edge and centroid) to these snow parameters. Expected errors depend on a better understanding of the relative scattering strengths of the interfaces and snow layer. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 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 I thank Shirley Pang for the software support during the course of this study. Data from Operation IceBridge are provided by the National Snow and Ice Data Center. R. K. performed this work at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 9 TC 9 Z9 9 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2014 VL 41 IS 14 BP 5014 EP 5020 DI 10.1002/2014GL060993 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AN4CU UT WOS:000340536000027 ER PT J AU Liang, Q Newman, PA Daniel, JS Reimann, S Hall, BD Dutton, G Kuijpers, LJM AF Liang, Qing Newman, Paul A. Daniel, John S. Reimann, Stefan Hall, Bradley D. Dutton, Geoff Kuijpers, Lambert J. M. TI Constraining the carbon tetrachloride (CCl4) budget using its global trend and inter-hemispheric gradient SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EMISSIONS; TRANSPORT; STRATOSPHERE; TROPOSPHERE; CHLORINE; FUTURE; GASES AB Carbon tetrachloride (CCl4) is a major anthropogenic ozone-depleting substance and greenhouse gas and has been regulated under the Montreal Protocol. However, the near-zero 2007-2012 emissions estimate based on the UNEP reported production and feedstock usage cannot be reconciled with the observed slow decline of atmospheric concentrations and the inter-hemispheric gradient (IHG) for CCl4. Our 3-D model simulations suggest that the observed IHG (1.5 +/- 0.2 ppt for 2000-2012) is primarily caused by ongoing current emissions, while ocean and soil losses and stratosphere-troposphere exchange together contribute a small negative gradient (similar to 0 - -0.3 ppt). Using the observed CCl4 global trend and IHG, we deduce that the mean global emissions for the 2000-2012 period are 39(34)(45) Gg/yr (similar to 30% of the peak 1980s emissions) and a corresponding total lifetime of 35(37)(32) years. C1 [Liang, Qing; Newman, Paul A.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. [Liang, Qing] Univ Space Res Assoc, GESTAR, Columbia, MD USA. [Daniel, John S.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO USA. [Reimann, Stefan] Empa, Fed Labs Mat Sci & Technol, Dubendorf, Switzerland. [Hall, Bradley D.; Dutton, Geoff] NOAA, Earth Syst Res Lab, Global Monitoring Div, Boulder, CO USA. [Dutton, Geoff] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Kuijpers, Lambert J. M.] Tech Univ Eindhoven, NL-5600 MB Eindhoven, Netherlands. RP Liang, Q (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. EM Qing.Liang-1@nasa.gov RI Liang, Qing/B-1276-2011; Daniel, John/D-9324-2011; Reimann, Stefan/A-2327-2009; Manager, CSD Publications/B-2789-2015 OI Reimann, Stefan/0000-0002-9885-7138; NR 30 TC 8 Z9 8 U1 1 U2 25 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 JUL 28 PY 2014 VL 41 IS 14 BP 5307 EP 5315 DI 10.1002/2014GL060754 PG 9 WC Geosciences, Multidisciplinary SC Geology GA AN4CU UT WOS:000340536000052 ER PT J AU Carlson, AE Hoffmayer, ER Tribuzio, CA Sulikowski, JA AF Carlson, Amy E. Hoffmayer, Eric R. Tribuzio, Cindy A. Sulikowski, James A. TI The Use of Satellite Tags to Redefine Movement Patterns of Spiny Dogfish (Squalus acanthias) along the US East Coast: Implications for Fisheries Management SO PLOS ONE LA English DT Article ID ATLANTIC BLUEFIN TUNA; SEA-SURFACE TEMPERATURE; SHARKS CARCHARODON-CARCHARIAS; DIEL VERTICAL MIGRATION; LIGHT-BASED GEOLOCATION; OFFSHORE FORAGING AREA; BOTTOM-TRAWL SURVEY; STATE-SPACE MODEL; GULF-OF-MEXICO; PACIFIC-OCEAN AB Spiny dogfish (Squalus acanthias) are assumed to be a highly migratory species, making habitual north-south migrations throughout their northwestern Atlantic United States (U.S.) range. Also assumed to be a benthic species, spiny dogfish stock structure is estimated through Northeast Fisheries Science Center (NEFSC) bottom-trawl surveys. Recent anomalies in population trends, including a recent four-fold increase in estimated spawning stock biomass, suggest alternative movement patterns could exist for this shark species. To obtain a better understanding of the horizontal and vertical movement dynamics of this species, Microwave Telemetry pop-up satellite archival X-Tags were attached to forty adult spiny dogfish at the northern (Gulf of Maine) and southern (North Carolina) extents of their core U.S. geographic range. Reconstructed geolocation tracks ranging in lengths from two to 12 months suggest that the seasonal migration patterns appear to be local in nature to each respective northern and southern deployment site, differing from previously published migration paradigms. Differences in distance and direction traveled between seasonal geolocations possibly indicate separate migratory patterns between groups. Kernel utilization distribution models also suggest strong separate core home ranges. Significant differences in seasonal temperature and depths between the two regions further substantiate the possibility of separate regional movement patterns between the two groups. Vertical utilization also suggests distinct diel patterns and that this species may not utilize the benthos as previously thought, potentially decreasing availability to benthic gear. C1 [Carlson, Amy E.; Sulikowski, James A.] Univ New England, Ctr Marine Sci, Biddeford, ME 04005 USA. [Hoffmayer, Eric R.] Southeast Fisheries Sci Ctr, Mississippi Labs, Natl Marine Fisheries Serv, Pascagoula, MS USA. [Tribuzio, Cindy A.] Alaska Fisheries Sci Ctr, Auke Bay Labs, Natl Marine Fisheries Serv, Juneau, AK USA. RP Carlson, AE (reprint author), Univ New England, Ctr Marine Sci, Biddeford, ME 04005 USA. EM acarlson1@une.edu FU Saltonstall-Kennedy (S-K) Grant Program [NA09NMF4270099, NA10NMF4270203]; Sturdivant Island Tuna Association FX This project was supported by awards from the Saltonstall-Kennedy (S-K) Grant Program (NA09NMF4270099 and NA10NMF4270203) and Sturdivant Island Tuna Association to J.A.S. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 112 TC 8 Z9 8 U1 6 U2 47 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 JUL 28 PY 2014 VL 9 IS 7 AR e103384 DI 10.1371/journal.pone.0103384 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM6RZ UT WOS:000339993700066 PM 25068584 ER PT J AU McConnell, JR Maselli, OJ Sigl, M Vallelonga, P Neumann, T Anschutz, H Bales, RC Curran, MAJ Das, SB Edwards, R Kipfstuhl, S Layman, L Thomas, ER AF McConnell, J. R. Maselli, O. J. Sigl, M. Vallelonga, P. Neumann, T. Anschutz, H. Bales, R. C. Curran, M. A. J. Das, S. B. Edwards, R. Kipfstuhl, S. Layman, L. Thomas, E. R. TI Antarctic-wide array of high-resolution ice core records reveals pervasive lead pollution began in 1889 and persists today SO SCIENTIFIC REPORTS LA English DT Article ID COATS LAND; LAW DOME; SNOW; GREENLAND; AD; ISOTOPES; CLIMATE AB Interior Antarctica is among the most remote places on Earth and was thought to be beyond the reach of human impacts when Amundsen and Scott raced to the South Pole in 1911. Here we show detailed measurements from an extensive array of 16 ice cores quantifying substantial toxic heavy metal lead pollution at South Pole and throughout Antarctica by 1889 - beating polar explorers by more than 22 years. Unlike the Arctic where lead pollution peaked in the 1970s, lead pollution in Antarctica was as high in the early 20th century as at any time since industrialization. The similar timing and magnitude of changes in lead deposition across Antarctica, as well as the characteristic isotopic signature of Broken Hill lead found throughout the continent, suggest that this single emission source in southern Australia was responsible for the introduction of lead pollution into Antarctica at the end of the 19th century and remains a significant source today. An estimated 660 t of industrial lead have been deposited over Antarctica during the past 130 years as a result of mid-latitude industrial emissions, with regional-to-global scale circulation likely modulating aerosol concentrations. Despite abatement efforts, significant lead pollution in Antarctica persists into the 21st century. C1 [McConnell, J. R.; Maselli, O. J.; Sigl, M.; Layman, L.] Desert Res Inst, Reno, NV 89512 USA. [Vallelonga, P.] Univ Copenhagen, Ctr Ice & Climate, DK-1168 Copenhagen, Denmark. [Neumann, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Anschutz, H.] Norwegian Geotech Inst, Oslo, Norway. [Bales, R. C.] Univ Calif, Merced, CA USA. [Curran, M. A. J.] Australian Antarctic Div, Kingston, Tas, Australia. [Das, S. B.] Woods Hole Oceanog Inst, Woods Hole, MA USA. [Edwards, R.] Curtin Univ, Perth, WA, Australia. [Kipfstuhl, S.] Helmholtz Zentrum Polar & Meeresforsch, Alfred Wegener Inst, Bremerhaven, Germany. [Thomas, E. R.] British Antarctic Survey, Cambridge, England. RP McConnell, JR (reprint author), Desert Res Inst, Reno, NV 89512 USA. EM Joe.McConnell@dri.edu RI Maselli, Olivia/A-6687-2013; Neumann, Thomas/D-5264-2012; Vallelonga, Paul/I-9650-2016; Edwards, Ross/B-1433-2013 OI Vallelonga, Paul/0000-0003-1055-7235; Edwards, Ross/0000-0002-9233-8775 FU U. S. National Science Foundation Division of Polar Programs [9903744, 0538427, 0538416, 0968391, 1142166, 0632031]; instrument grants [0216552, 0421412]; national research programs FX The data reported in this paper are tabulated in the Supplementary Information. This work primarily was supported by the U. S. National Science Foundation Division of Polar Programs (research grants 9903744, 0538427, 0538416, 0968391, 1142166, 0632031; instrument grants 0216552, 0421412). We gratefully acknowledge the national research programs for their support and the efforts of field teams and others for help in collecting the ice cores in the array. The authors also thank the WAIS Divide Science Coordination Office for the collection and distribution of the WAIS Divide ice cores, Ice Drilling and Design and Operations for drilling support, the National Ice Core Laboratory for curating many of the cores used in this study; Raytheon Polar Service for logistics support in Antarctica; and the 109th New York Air National Guard for airlift in Antarctic. NR 32 TC 13 Z9 13 U1 5 U2 39 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 JUL 28 PY 2014 VL 4 AR 5848 DI 10.1038/srep05848 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM0CT UT WOS:000339511300001 PM 25068819 ER PT J AU Goldstein, ME AF Goldstein, M. E. TI Effect of free-stream turbulence on boundary layer transition SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Review DE boundary layer transition; free-stream turbulence; boundary layer streaks ID VORTICAL DISTURBANCES; KLEBANOFF MODES; INSTABILITY; FLOW; DISTORTION; EVOLUTION AB This paper is concerned with the transition to turbulence in flat plate boundary layers due to moderately high levels of free-stream turbulence. The turbulence is assumed to be generated by an (idealized) grid and matched asymptotic expansions are used to analyse the resulting flow over a finite thickness flat plate located in the downstream region. The characteristic Reynolds number R-Lambda based on the mesh size. and free-stream velocity is assumed to be large, and the turbulence intensity e is assumed to be small. The asymptotic flow structure is discussed for the generic case where the turbulence Reynolds number epsilon R-Lambda and the plate thickness and are held fixed (at O(1) and O(Lambda), respectively) in the limit as R-Lambda -> infinity and epsilon -> 0. But various limiting cases are considered in order to explain the relevant transition mechanisms. It is argued that there are two types of streak-like structures that can play a role in the transition process: (i) those that appear in the downstream region and are generated by streamwise vorticity in upstream flow and (ii) those that are concentrated near the leading edge and are generated by plate normal vorticity in upstream flow. The former are relatively unaffected by leading edge geometry and are usually referred to as Klebanoff modes while the latter are strongly affected by leading edge geometry and are more streamwise vortex-like in appearance. C1 NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Goldstein, ME (reprint author), NASA Glenn Res Ctr, 2100 Brookpk Rd, Cleveland, OH 44135 USA. EM marvin.e.goldstein@nasa.gov FU NASA Aerosciences Project FX This work was supported by the NASA Aerosciences Project. NR 35 TC 4 Z9 4 U1 3 U2 8 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-503X EI 1471-2962 J9 PHILOS T R SOC A JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci. PD JUL 28 PY 2014 VL 372 IS 2020 SI SI AR 20130354 DI 10.1098/rsta.2013.0354 PG 18 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AK5AW UT WOS:000338437200012 ER PT J AU Rind, D Jonas, J Balachandran, NK Schmidt, GA Lean, J AF Rind, D. Jonas, J. Balachandran, N. K. Schmidt, G. A. Lean, J. TI The QBO in two GISS global climate models: 1. Generation of the QBO SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID QUASI-BIENNIAL OSCILLATION; GRAVITY-WAVE PARAMETERIZATION; DOUBLED CO2 CLIMATE; EARTH SYSTEM MODEL; MIDDLE ATMOSPHERE; CIRCULATION MODEL; TROPICAL PRECIPITATION; CUMULUS CONVECTION; SIMULATED CLIMATE; EQUATORIAL WAVES AB The adjustment of parameterized gravity waves associated with model convection and finer vertical resolution has made possible the generation of the quasi-biennial oscillation (QBO) in two Goddard Institute for Space Studies (GISS) models, GISS Middle Atmosphere Global Climate Model III and a climate/middle atmosphere version of Model E2. Both extend from the surface to 0.002 hPa, with 2 degrees x 2.5 degrees resolution and 102 layers. Many realistic features of the QBO are simulated, including magnitude and variability of its period and amplitude. The period itself is affected by the magnitude of parameterized convective gravity wave momentum fluxes and interactive ozone (which also affects the QBO amplitude and variability), among other forcings. Although varying sea surface temperatures affect the parameterized momentum fluxes, neither aspect is responsible for the modeled variation in QBO period. Both the parameterized and resolved waves act to produce the respective easterly and westerly wind descent, although their effect is offset in altitude at each level. The modeled and observed QBO influences on tracers in the stratosphere, such as ozone, methane, and water vapor are also discussed. Due to the link between the gravity wave parameterization and the models' convection, and the dependence on the ozone field, the models may also be used to investigate how the QBO may vary with climate change. C1 [Rind, D.; Schmidt, G. A.] NASA, Goddard Space Flight Ctr, Inst Space Studies, New York, NY 10025 USA. [Jonas, J.; Balachandran, N. K.] Columbia Univ, Ctr Climate Change Res, New York, NY USA. [Lean, J.] US Naval Res Lab, Washington, DC USA. RP Rind, D (reprint author), NASA, Goddard Space Flight Ctr, Inst Space Studies, New York, NY 10025 USA. EM david.h.rind@nasa.gov RI Schmidt, Gavin/D-4427-2012 OI Schmidt, Gavin/0000-0002-2258-0486 FU NASA Glory Mission; NASA Modeling, Analysis and Prediction program FX This paper was improved substantially by the knowledgeable suggestions of three anonymous reviewers. We thank them greatly for all their efforts. The work was funded by the NASA Glory Mission. Climate modeling at GISS is supported by the NASA Modeling, Analysis and Prediction program and 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 and the NASA program at Ames Research Center. Data from these runs are available from Jeff Jonas (jeffjonas88@gmail.com). NR 81 TC 6 Z9 6 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2014 VL 119 IS 14 BP 8798 EP 8824 DI 10.1002/2014JD021678 PG 27 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN2GQ UT WOS:000340402800017 ER PT J AU Hansell, RA Tsay, SC Pantina, P Lewis, JR Ji, Q Herman, JR AF Hansell, R. A. Tsay, S. -C. Pantina, P. Lewis, J. R. Ji, Q. Herman, J. R. TI Spectral derivative analysis of solar spectroradiometric measurements: Theoretical basis SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID INFRARED RADIOMETRIC MEASUREMENTS; TRANSMITTANCE MEASUREMENTS; MICROPHYSICAL PROPERTIES; RADIATIVE IMPACTS; RETRIEVAL METHOD; TROPICAL CIRRUS; SOUTHEAST-ASIA; OPTICAL DEPTH; CLOUDS; AEROSOLS AB Spectral derivative analysis, a commonly used tool in analytical spectroscopy, is described for studying cirrus clouds and aerosols using hyperspectral, remote sensing data. The methodology employs spectral measurements from the 2006 Biomass-burning Aerosols in Southeast Asia field study to demonstrate the approach. Spectral peaks associated with the first two derivatives of measured/modeled transmitted spectral fluxes are examined in terms of their shapes, magnitudes, and positions from 350 to 750nm, where variability is largest. Differences in spectral features between media are mainly associated with particle size and imaginary term of the complex refractive index. Differences in derivative spectra permit cirrus to be conservatively detected at optical depths near the optical thin limit of similar to 0.03 and yield valuable insight into the composition and hygroscopic nature of aerosols. Biomass-burning smoke aerosols/cirrus generally exhibit positive/negative slopes, respectively, across the 500-700 nm spectral band. The effect of cirrus in combined media is to increase/decrease the slope as cloud optical thickness decreases/increases. For thick cirrus, the slope tends to 0. An algorithm is also presented which employs a two model fit of derivative spectra for determining relative contributions of aerosols/clouds to measured data, thus enabling the optical thickness of the media to be partitioned. For the cases examined, aerosols/clouds explain similar to 83%/17% of the spectral signatures, respectively, yielding a mean cirrus cloud optical thickness of 0.08 +/- 0.03, which compared reasonably well with those retrieved from a collocated Micropulse Lidar Network Instrument (0.09 +/- 0.04). This method permits extracting the maximum informational content from hyperspectral data for atmospheric remote sensing applications. C1 [Hansell, R. A.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Hansell, R. A.; Tsay, S. -C.; Pantina, P.; Lewis, J. R.; Ji, Q.; Herman, J. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pantina, P.] Sci Syst & Applicat Inc, Lanham, MD USA. [Lewis, J. R.; Herman, J. R.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Ji, Q.] Sigma Space Corp, Greenbelt, MD USA. RP Hansell, RA (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM Richard.A.Hansell@nasa.gov OI Herman, Jay/0000-0002-9146-1632 FU NASA Radiation Sciences Program; NASA Earth Observing System and Radiation Sciences Program FX This work is supported by the NASA Radiation Sciences Program managed by Hal B. Maring. Both AERONET and MPLNET are funded by the NASA Earth Observing System and Radiation Sciences Program. We would like to thank B. Holben for establishing and maintaining the AERONET site at Phimai and for the valuable discussions. We acknowledge the MODTRAN developers (a joint collaboration of Spectral Sciences, Inc. and the U. S. Air Force) for their RTM code and M. Hess for making the OPAC database publicly available. We would like to thank G. Fager at PANalytical NIR (formerly ASD) for his technical support of our FieldSpec Pro instrument and D. Feldman and T. O'Haven for their MODTRANwrapper and signal-processing codes (terpconnect.umd.edu/similar to toh/spectrum/SignalProcessingTools.html), respectively. We also thank B. Baum, P. Yang, A. Heymsfield, and C. Schmitt for their ice cloud scattering models. Lastly, we thank the reviewers for their helpful and insightful comments. NR 57 TC 1 Z9 1 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2014 VL 119 IS 14 BP 8908 EP 8924 DI 10.1002/2013JD021423 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN2GQ UT WOS:000340402800023 ER PT J AU Wood, NB L'Ecuyer, TS Heymsfield, AJ Stephens, GL Hudak, DR Rodriguez, P AF Wood, Norman B. L'Ecuyer, Tristan S. Heymsfield, Andrew J. Stephens, Graeme L. Hudak, David R. Rodriguez, Peter TI Estimating snow microphysical properties using collocated multisensor observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID PARTICLE TERMINAL VELOCITIES; ICE-CLOUD PARTICLES; VIDEO DISDROMETER; FALL SPEEDS; PRECIPITATION; CRYSTALS; MICROWAVE; UNCERTAINTIES; CIRRUS; AREA AB The ability of ground-based in situ and remote sensing observations to constrain microphysical properties for dry snow is examined using a Bayesian optimal estimation retrieval method. Power functions describing the variation of mass and horizontally projected area with particle size and a parameter related to particle shape are retrieved from near-Rayleigh radar reflectivity, particle size distribution, snowfall rate, and size-resolved particle fall speeds. Algorithm performance is explored in the context of instruments deployed during the Canadian CloudSat CALIPSO Validation Project, but the algorithm is adaptable to other similar combinations of sensors. Critical estimates of observational and forward model uncertainties are developed and used to quantify the performance of the method using synthetic cases developed from actual observations of snow events. In addition to illustrating the technique, the results demonstrate that this combination of sensors provides useful constraints on the mass parameters and on the coefficient of the area power function but only weakly constrains the exponent of the area power function and the shape parameter. Information content metrics show that about two independent quantities are measured by the suite of observations and that the method is able to resolve about eight distinct realizations of the state vector containing the mass and area power function parameters. Alternate assumptions about observational and forward model uncertainties reveal that improved modeling of particle fall speeds could contribute substantial improvements to the performance of the method. C1 [Wood, Norman B.] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI 53706 USA. [L'Ecuyer, Tristan S.] Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI USA. [Heymsfield, Andrew J.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Stephens, Graeme L.] NASA, Jet Prop Lab, Pasadena, CA USA. [Hudak, David R.; Rodriguez, Peter] Environm Canada, Cloud Phys & Severe Weather Res Sect, King City, ON, Canada. RP Wood, NB (reprint author), Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI 53706 USA. EM norman.wood@ssec.wisc.edu RI L'Ecuyer, Tristan/E-5607-2012 OI L'Ecuyer, Tristan/0000-0002-7584-4836 FU National Aeronautics and Space Administration; JPL CloudSat Office; NASA Global Precipitation Measurement program [NN-X13AH73G] FX Parts of this research by N.B.W. and T. S. L. were performed at the University of Wisconsin-Madison and at Colorado State University for the Jet Propulsion Laboratory, California Institute of Technology, sponsored by the National Aeronautics and Space Administration. A.J.H. acknowledges support from the JPL CloudSat Office and NASA Global Precipitation Measurement program contract NN-X13AH73G. Thanks to G.-J. Huang of Colorado State University (2DVD data), F. Fabry of McGill University (VertiX data), and L. Bliven of NASA Goddard Space Flight Center (SVI data) for making their C3VP data sets available and sharing their expertise. Other data used in the analyses, including the relevant FD12P and DFIR observations, are available from the authors. Thanks to two anonymous reviewers and S. Nesbitt of University of Illinois Urbana-Champaign for their thoughtful comments and suggestions. NR 48 TC 12 Z9 12 U1 0 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2014 VL 119 IS 14 BP 8941 EP 8961 DI 10.1002/2013JD021303 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN2GQ UT WOS:000340402800025 ER PT J AU Lebsock, M Su, H AF Lebsock, Matthew Su, Hui TI Application of active spaceborne remote sensing for understanding biases between passive cloud water path retrievals SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID COMMUNITY ATMOSPHERE MODEL; DROPLET EFFECTIVE RADIUS; OPTICAL DEPTH; A-TRAIN; PART II; ALGORITHM; OCEAN; PRECIPITATION; RADAR; SURFACE AB Bias between the Advanced Microwave Scanning Radiometer-EOS (AMSR-E) version 2 and the Moderate Resolution Imaging Spectroradiometer (MODIS) collection 5.1 cloud liquid water path (W-c) products are explored with the aid of coincident active observations from the CloudSat radar and the CALIPSO lidar. In terms of detection, the active observations provide precise separation of cloudy from clear sky and precipitating from nonprecipitating clouds. In addition, they offer a unique quantification of precipitation water path (W-p) in warm clouds. They also provide an independent quantification of W-c that is based on an accurate surface reference technique, which is an independent arbiter between the two passive approaches. The results herein establish the potential for CloudSat and CALIPSO to provide an independent assessment of bias between the conventional passive remote sensing methods from reflected solar and emitted microwave radiation. After applying a common data filter to the observations to account for sampling biases, AMSR-E is biased high relative to MODIS in the global mean by 26.4 gm(-2). The RMS difference in the regional patterns is 32.4 gm(-2), which highlights a large geographical dependence in the bias which is related to the tropical transitions from stratocumulus to cumulus cloud regimes. The contributions of four potential sources for this bias are investigated by exploiting the active observations: (1) bias in MODIS related to solar zenith angle dependence accounts for -2.3 gm(-2), (2) bias in MODIS due to undersampling of cloud edges accounts for 4.2 gm(-2), (3) a wind speed and water vapor-dependent "clear-sky biase" in the AMSR-E retrieval accounts for 6.3 gm(-2), and (4) evidence suggests that much of the remaining 18 gm(-2) bias is related to the assumed partitioning of the observed emission signal between cloud and precipitation water in the AMSR-E retrieval. This is most evident through the correlations between the regional mean patterns of W-p and the W-c bias within the latitudes of 30 degrees N and 30 degrees S, suggesting that the assumption of a regionally invariant cloud/precipitation partitioning in the AMSR-E algorithm is the likely causal factor. C1 [Lebsock, Matthew; Su, Hui] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Lebsock, M (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM matthew.d.lebsock@jpl.nasa.gov FU NASA FX The research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Funding was provided by the NASA Making Earth System Data Records for Use in Research Environments. CloudSat data were acquired through the CloudSat Data Processing Center at Colorado State University and can be accessed through their Web site http://www.cloudsat.cira.colostate.edu. MODIS products were obtained from the Goddard Distributed Active Archive Center. AMSR-E data were acquired from the National Snow and Ice Data Center. We are especially grateful to the three anonymous reviewers who helped clarify the limitations of the non-overlapping AMSR-E and CloudSat footprints and the importance of the cloud/precipitation partitioning in the AMSR-E results. NR 47 TC 11 Z9 11 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 JUL 27 PY 2014 VL 119 IS 14 BP 8962 EP 8979 DI 10.1002/2014JD021568 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN2GQ UT WOS:000340402800026 ER PT J AU Jethva, H Torres, O Ahn, C AF Jethva, Hiren Torres, Omar Ahn, Changwoo TI Global assessment of OMI aerosol single-scattering albedo using ground-based AERONET inversion SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OPTICAL-PROPERTIES; NON-SPHERICITY; DUST; ABSORPTION; SATELLITE; INSTRUMENT; AIRCRAFT; NETWORK; DEPTH; SUN AB We compare the aerosol single-scattering albedo (SSA) retrieved by the near-UV two-channel algorithm (OMAERUV) applied to the Aura/Ozone Monitoring Instrument (OMI) measurements with an equivalent inversion made by the ground-based Aerosol Robotic Network (AERONET). A recent upgrade of the OMAERUV algorithm incorporates a modified carbonaceous aerosol model, a Cloud-Aerosol Lidar with Orthogonal Polarization-based aerosol height climatology, and a robust aerosol-type identification. This paper is the first comprehensive effort to globally compare the OMI-retrieved SSA with that of AERONET using all available sites spanning the regions of biomass burning, dust, and urban pollution. An analysis of the colocated retrievals over 269 sites reveals that about 46% (69%) of OMI-AERONET matchups agree within the absolute difference of +/- 0.03 (+/- 0.05) for all aerosol types. The comparison improves to 52% (77%) when only "smoke" and "dust" aerosol types were identified by the OMAERUV algorithm. Regionally, the agreement between the two inversions was robust over the biomass burning sites of South America, Sahel, Indian subcontinent, and oceanic/coastal sites followed by a reasonable agreement over Northeast Asia. Over the desert regions, OMI tends to retrieve higher SSA, particularly over the Arabian Peninsula. Globally, the OMI-AERONET matchups agree mostly within +/- 0.03 for the aerosol optical depth (440 nm) and UV-aerosol index larger than 0.4 and 1.0, respectively. Possible sources of uncertainty in the OMI retrieval can be the subpixel cloud contamination, assumptions of the surface albedo, and spectral aerosol absorption. We expect further refinement in the OMAERUV algorithm which stands uniquely in characterizing aerosol absorption from space. C1 [Jethva, Hiren] Univ Space Res Assoc, Columbia, MD 21046 USA. [Jethva, Hiren; Torres, Omar] NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA. [Ahn, Changwoo] Sci Syst & Applicat Inc, Lanham, MD USA. RP Jethva, H (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA. EM hiren.t.jethva@nasa.gov RI Torres, Omar/G-4929-2013 NR 37 TC 20 Z9 20 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2014 VL 119 IS 14 BP 9020 EP 9040 DI 10.1002/2014JD021672 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN2GQ UT WOS:000340402800029 ER PT J AU Schmitt, MP Rai, AK Bhattacharya, R Zhu, DM Wolfe, DE AF Schmitt, Michael P. Rai, Amarendra K. Bhattacharya, Rabi Zhu, Dongming Wolfe, Douglas E. TI "Multilayer thermal barrier coating (TBC) architectures utilizing rare earth doped YSZ and rare earth pyrochlores" SO SURFACE & COATINGS TECHNOLOGY LA English DT Article DE Thermal barrier coating; TBC; Pyrochlore; Multilayer; Rare earth ID CONDUCTIVITY AB To allow for increased gas turbine efficiencies, new insulating thermal barrier coatings (TBCs) must be developed to protect the underlying metallic components from higher operating temperatures. This work focused on using rare earth doped (Yb and Gd) yttria stabilized zirconia (t' low-k) and Gd2Zr2O7 pyrochlores (GZO) combined with novel nanolayered and thick layered microstructures to enable operation beyond the 1200 degrees C stability limit of current 7 wt.% yttria stabilized zirconia (7YSZ) coatings. It was observed that the layered system can reduce the thermal conductivity by similar to 45% with respect to YSZ after 20 h of testing at 1316 degrees C. The erosion rate of GZO is shown to be an order to magnitude higher than YSZ and t' low-k, but this can be reduced by almost 57% when utilizing a nanolayered structure. Lastly, the thermal instability of the layered system is investigated and thought is given to optimization of layer thickness. (C) 2014 Elsevier B.V. All rights reserved. C1 [Schmitt, Michael P.; Wolfe, Douglas E.] Penn State Univ, Appl Res Lab, University Pk, PA 16802 USA. [Schmitt, Michael P.; Wolfe, Douglas E.] Penn State Univ, Dept Mat Sci & Engn, University Pk, PA 16802 USA. [Rai, Amarendra K.; Bhattacharya, Rabi] UES Inc, Dayton, OH 45432 USA. [Zhu, Dongming] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Wolfe, DE (reprint author), Penn State Univ, Appl Res Lab, University Pk, PA 16802 USA. EM dew125@arl.psu.edu FU DOE STTR Phase II [DE-SC0005356]; Eric Walker fellowship program of the Applied Research Laboratory at the Pennsylvania State University FX The authors would like to thank Anna Stump for help with sample preparation and microscopy and Ethan Lucas for help with coating erosion testing. This work was funded in part under DOE STTR Phase II award No. DE-SC0005356 and the Eric Walker fellowship program of the Applied Research Laboratory at the Pennsylvania State University. Any opinions, findings, conclusions, or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the DOE. NR 19 TC 13 Z9 13 U1 6 U2 50 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0257-8972 J9 SURF COAT TECH JI Surf. Coat. Technol. PD JUL 25 PY 2014 VL 251 BP 56 EP 63 DI 10.1016/j.surfcoat.2014.03.049 PG 8 WC Materials Science, Coatings & Films; Physics, Applied SC Materials Science; Physics GA AJ8XT UT WOS:000337992100008 ER PT J AU Henderson, BL Gudipati, MS AF Henderson, Bryana L. Gudipati, Murthy S. TI Plume Composition and Evolution in Multicomponent Ices Using Resonant Two-Step Laser Ablation and Ionization Mass Spectrometry SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID MOLECULAR-DYNAMICS SIMULATIONS; KNUDSEN-LAYER FORMATION; DESORPTION IONIZATION; ORGANIC-SOLIDS; UV-MALDI; ION YIELDS; 248 NM; MATRIX; CLUSTERS; MECHANISMS AB The composition and evolution of plumes generated in a resonant infrared (IR) laser desorption of low-temperature ices is investigated via a recently developed two-step laser desorption and ionization mass spectrometry (2S-LAIMS) technique where a neutral plume is ejected by an IR laser pulse and ionized by a UV laser pulse for analysis via time-of-flight mass spectrometry. By varying the delay between the lasers, we can construct a complete time-resolved model of the ejected plume components. We found that water ices containing mixtures of polar and nonpolar analytes displayed complex mass spectral profiles that varied as the plume evolved. In these samples, the low-volatility polar analytes and clusters were restricted to the early part of the plume, whereas volatile or nonpolar analytes were spread throughout the plume. The distributions of low-volatility polar species, clusters, and impurities from the copper substrate were well-represented by single Maxwell-like distributions centered at high velocities (600-800 m s(-1)), while nonpolar, volatile species contained two distinct components, indicating both ablation and thermal desorption processes. Characterization of plume distributions can therefore provide new insight into an analyte's chemical identity and can aid in assignment of otherwise ambiguous signals in the mass spectra. C1 [Henderson, Bryana L.; Gudipati, Murthy S.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA. RP Gudipati, MS (reprint author), CALTECH, Jet Prop Lab, Div Sci, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM gudipati@jpl.nasa.gov RI Gudipati, Murthy/F-7575-2011 FU JPL's DRDF; JPL's RTD; NASA Spitzer Science Center; NASA; Europa Clipper Pre-Project; National Aeronautics and Space Administration; NASA Postdoctoral Program for an NPP fellowship FX This research was enabled through partial funding from JPL's DRDF and R&TD funding for infrastructure of the "Ice Spectroscopy Laboratory" at JPL, NASA Spitzer Science Center, NASA funding through Planetary Atmospheres, and the Europa Clipper Pre-Project. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. B.L.H. acknowledges funding from the NASA Postdoctoral Program for an NPP fellowship. We thank Dr. Robert Wagner (Karlsruhe Institute of Technology, Germany) for assisting with the LabVIEW software integration of the experimental setup. B.L.H. is a NASA Postdoctoral Fellow at the Jet Propulsion Laboratory. M.S.G. is also a Senior Research Scientist at the IPST, University of Maryland at College Park. NR 47 TC 2 Z9 2 U1 1 U2 8 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD JUL 24 PY 2014 VL 118 IS 29 BP 5454 EP 5463 DI 10.1021/jp503111k PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA AM0MU UT WOS:000339540500011 PM 24990519 ER PT J AU Liao, YL Chen, ZF Connell, JW Fay, CC Park, C Kim, JW Lin, Y AF Liao, Yunlong Chen, Zhongfang Connell, John W. Fay, Catharine C. Park, Cheol Kim, Jae-Woo Lin, Yi TI Chemical Sharpening, Shortening, and Unzipping of Boron Nitride Nanotubes SO ADVANCED FUNCTIONAL MATERIALS LA English DT Article ID WALLED CARBON NANOTUBES; GRAPHENE NANORIBBONS; POLYMERIC COMPOSITES; FACILE SYNTHESIS; BN NANOTUBES; NANOSHEETS; FUNCTIONALIZATION; PURIFICATION; SOLUBILIZATION; OXIDATION AB Boron nitride nanotubes (BNNTs), the one-dimensional member of the boron nitride nanostructure family, are generally accepted to be highly inert to oxidative treatments and can only be covalently modified by highly reactive species. Conversely, it is discovered that the BNNTs can be chemically dispersed and their morphology modified by a relatively mild method: simply sonicating the nanotubes in aqueous ammonia solution. The dispersed nanotubes are significantly corroded, with end-caps removed, tips sharpened, and walls thinned. The sonication treatment in aqueous ammonia solution also removes amorphous BN impurities and shortened BNNTs, resembling various oxidative treatments of carbon nanotubes. Importantly, the majority of BNNTs are at least partially longitudinally cut, or "unzipped". Entangled and freestanding BN nanoribbons (BNNRs), resulting from the unzipping, are found to be similar to 5-20 nm in width and up to a few hundred nanometers in length. This is the first chemical method to obtain BNNRs from BNNT unzipping. This method is not derived from known carbon nanotube unzipping strategies, but is unique to BNNTs because the use of aqueous ammonia solutions specifically targets the B-N bond network. This study may pave the way for convenient processing of BNNTs, previously thought to be highly inert, toward controlling their dispersion, purity, lengths, and electronic properties. C1 [Liao, Yunlong; Kim, Jae-Woo; Lin, Yi] Natl Inst Aerosp, Hampton, VA 23666 USA. [Liao, Yunlong; Chen, Zhongfang] Univ Puerto Rico, Dept Phys, Dept Chem, San Juan, PR 00931 USA. [Connell, John W.; Fay, Catharine C.; Park, Cheol] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Park, Cheol] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA. [Lin, Yi] Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA. RP Liao, YL (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. EM zhongfangchen@gmail.com; john.w.connell@nasa.gov; yi.lin@nianet.org RI Kim, Jae-Woo/A-8314-2008; Chen, Zhongfang/A-3397-2008 FU Department of Defense [W911NF-12-1-0083]; NASA [NNX10AM80H, NNX13AB22A]; US Air Force Office of Scientific Research - Low Density Materials program [FA9550-11-1-0042] FX We thank Dr. W. Cao and Prof. H. Elsayed-Ali (Applied Research Center, Old Dominion University) for assistance in HR-TEM imaging and C. Chamberlain (NASA Langley Research Center) for TGA measurements. Y. Liao was an exchange student resident from University of Puerto Rico, who is supported by Department of Defense (Grant W911NF-12-1-0083) and NASA (Grant Nos. NNX10AM80H and NNX13AB22A) to conduct research at National Institute of Aerospace and NASA Langley Research Center. C. Park acknowledges the financial support in part by US Air Force Office of Scientific Research - Low Density Materials program (Grant No. FA9550-11-1-0042). NR 56 TC 12 Z9 12 U1 2 U2 81 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 1616-301X EI 1616-3028 J9 ADV FUNCT MATER JI Adv. Funct. Mater. PD JUL 23 PY 2014 VL 24 IS 28 BP 4497 EP 4506 DI 10.1002/adfm.201400599 PG 10 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA AM2XE UT WOS:000339713900014 ER PT J AU Williams, JC Meador, MAB McCorkle, L Mueller, C Wilmoth, N AF Williams, Jarrod C. Meador, Mary Ann B. McCorkle, Linda Mueller, Carl Wilmoth, Nathan TI Synthesis and Properties of Step-Growth Polyamide Aerogels Cross-linked with Triacid Chlorides SO CHEMISTRY OF MATERIALS LA English DT Article ID SYNDIOTACTIC POLYSTYRENE AEROGELS; POLYIMIDE AEROGELS; POLYACRYLAMIDE-GELS; MECHANICALLY STRONG; SILICA AEROGELS; CARBON AEROGELS; ADSORPTION; STRENGTH AB We report the first synthesis of step-growth aromatic polyamide (PA) aerogels made using amine end-capped polyamide oligomers cross-linked with 1,3,5-benzenetricarbonyl trichloride (BTC). Isophthaloyl chloride (IPC) or terephthaloyl chloride (TPC) were combined with m-phenylenediamine (mPDA) in N-methylpyrrolidinone (NMP) to give amine-capped polyamide oligomers formulated with up to 40 repeat units. Addition of the cross-linker, BTC, typically induces gelation in under 5 min. Solvent exchange of the resulting gels into ethanol followed by supercritical CO2 drying gives colorless aerogels with densities ranging from 0.06 to 0.33 g/cm(3), compressive moduli between 5 and 312 MPa, and surface areas as high as 385 m(2)/g. Dielectric properties were also measured in the X-band frequency range. It was found that relative dielectric constant decreased with density as seen with other aerogels with the lowest relative dielectric constant being 1.15 for aerogels with densities of 0.06 g/cm(3). Because of their superior mechanical properties, these aerogels can be utilized in a number of aerospace related applications, such as insulation for rovers, habitats, deployable structures, and extravehicular activity suits, as well as low dielectric substrates for antennas and other electronics. Because of potentially lower cost relative to polyimide and other polymer aerogels, they also have potential for use in more terrestrial applications as well, such as insulation for refrigeration, building and construction, and protective clothing. C1 [Williams, Jarrod C.] NASA Glenn Res Ctr, NASA Postdoctoral Program, Cleveland, OH 44135 USA. [Meador, Mary Ann B.] NASA Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. [McCorkle, Linda] Ohio Aerosp Inst, Cleveland, OH 44142 USA. [Mueller, Carl] Qinetiq NA, Waltham, MA 02451 USA. [Wilmoth, Nathan] Vantage Partners LLC, Brookpark, OH 44142 USA. RP Williams, JC (reprint author), NASA Glenn Res Ctr, NASA Postdoctoral Program, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM jarrod.c.williams@nasa.gov; maryann.meador@nasa.gov OI Meador, Mary Ann/0000-0003-2513-7372 NR 34 TC 21 Z9 22 U1 7 U2 75 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0897-4756 EI 1520-5002 J9 CHEM MATER JI Chem. Mat. PD JUL 22 PY 2014 VL 26 IS 14 BP 4163 EP 4171 DI 10.1021/cm5012313 PG 9 WC Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA AL9OU UT WOS:000339471400018 ER PT J AU Gastaldello, F Limousin, M Foex, G Munoz, RP Verdugo, T Motta, V More, A Cabanac, R Buote, DA Eckert, D Ettori, S Fritz, A Ghizzardi, S Humphrey, PJ Meneghetti, M Rossetti, M AF Gastaldello, F. Limousin, M. Foex, G. Munoz, R. P. Verdugo, T. Motta, V. More, A. Cabanac, R. Buote, D. A. Eckert, D. Ettori, S. Fritz, A. Ghizzardi, S. Humphrey, P. J. Meneghetti, M. Rossetti, M. TI Dark matter-baryons separation at the lowest mass scale: the Bullet Group SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: strong; galaxies: groups: individual: SL2S J08544-0121; dark matter; X-rays: galaxies: clusters ID GALAXY CLUSTER MERGER; SAMPLE; DYNAMICS; RELEASE AB We report on the X-ray observation of a strong lensing selected group, SL2S J08544-0121, with a total mass of 2.4 +/- 0.6 x 10(14) M-circle dot which revealed a separation of 124 +/- 20 kpc between the X-ray emitting collisional gas and the collisionless galaxies and dark matter (DM), traced by strong lensing. This source allows to put an order of magnitude estimate to the upper limit to the interaction cross-section of DM of 10 cm(2) g(-1). It is the lowest mass object found to date showing a DM-baryons separation, and it reveals that the detection of bullet-like objects is not rare and confined to mergers of massive objects opening the possibility of a statistical detection of DM-baryons separation with future surveys. C1 [Gastaldello, F.; Eckert, D.; Fritz, A.; Ghizzardi, S.; Rossetti, M.] INAF IASF Milano, I-20133 Milan, Italy. [Gastaldello, F.; Buote, D. A.; Humphrey, P. J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Limousin, M.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Limousin, M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Foex, G.; Motta, V.] Univ Valparaiso, Inst Fis & Astron, Valparaiso 2360102, Chile. [Munoz, R. P.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile. [Verdugo, T.] Ctr Invest Astron, Merida 5101A, Venezuela. [More, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [More, A.] Univ Tokyo, Kavli IPMU, Kashiwa, Chiba 2778583, Japan. [Cabanac, R.] Univ Toulouse UPS, CNRS, Inst Rech Astrophys & Planetol, F-65000 Tarbes, France. [Eckert, D.] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland. [Ettori, S.; Meneghetti, M.] INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Ettori, S.; Meneghetti, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Meneghetti, M.] JPL, Pasadena, CA 91109 USA. [Rossetti, M.] Univ Milan, Dip Fis, I-20133 Milan, Italy. RP Gastaldello, F (reprint author), INAF IASF Milano, Via E Bassini 15, I-20133 Milan, Italy. EM gasta@lambrate.inaf.it RI Gastaldello, Fabio/N-4226-2015; Ettori, Stefano/N-5004-2015; Meneghetti, Massimo/O-8139-2015; OI Gastaldello, Fabio/0000-0002-9112-0184; Ettori, Stefano/0000-0003-4117-8617; Meneghetti, Massimo/0000-0003-1225-7084; Ghizzardi, Simona/0000-0003-0879-7328; Verdugo, Tomas/0000-0003-4062-6123 FU INAF-ASI [I/023/05/0, I/088/06/0, I/032/10/0]; INAF through VIPERS; FONDECYT [1120741, 3130750]; ECOS-CONICYT [C12U02]; CONACYT [165365, 203489]; INFN project [PD51]; [ASI/INAF/I/023/12/0] FX FG is supported by INAF-ASI through grant I/023/05/0, I/088/06/0 and I/032/10/0. AF is supported by INAF through VIPERS grants PRIN 2008/2010. VM acknowledges the support of FONDECYT 1120741. RM acknowledges the support of FONDECYT 3130750. RC, GF, ML, VM acknowledge the support of ECOS-CONICYT C12U02. TV acknowledges support from CONACYT through grant 165365 and 203489. MM acknowledges financial contribution from the agreement ASI/INAF/I/023/12/0 and from INFN project PD51. NR 30 TC 10 Z9 10 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2014 VL 442 IS 1 BP L76 EP L80 DI 10.1093/mnrasl/slu058 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ2DP UT WOS:000348045200017 ER PT J AU Ramsay, G Hakala, P Howell, SB AF Ramsay, Gavin Hakala, Pasi Howell, Steve B. TI Red giant pulsations from the suspected symbiotic star StHA 169 detected in Kepler data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: symbiotic; Stars: individual: StHa 169; ultraviolet: stars ID PERIOD-LUMINOSITY RELATIONS; LARGE-MAGELLANIC-CLOUD; CH-CYGNI; WHITE-DWARF; PHOTOMETRIC CALIBRATION; RS OPHIUCHI; SPACED DATA; VARIABILITY; CATALOG; FIELD AB We present Kepler and Swift observations of StHa 169 which is currently classified as a symbiotic binary. The Kepler light curve shows quasi-periodic behaviour with a mean period of 34 d and an amplitude of a few per cent. Using Swift data, we find a relatively strong UV source at the position of StHa 169 but no X-ray counterpart. Using a simple two-component blackbody fit to model the combined Swift and 2MASS spectral energy distribution and an assessment of the previously published optical spectrum, we find that the source has a hot (similar to 10 000 K) component and a cooler (similar to 3700 K) component. The Kepler light is dominated by the cool component and we attribute the variability to pulsations in a red giant star. If we remove this approximate month long modulation from the light curve, we find no evidence for additional variability in the light curve. The hotter source is assigned to a late B or early A main-sequence star. We briefly discuss the implications of these findings and conclude that StHA 169 is a red giant plus main-sequence binary. C1 [Ramsay, Gavin] Armagh Observ, Armagh BT61 9DG, North Ireland. [Hakala, Pasi] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94095 USA. RP Ramsay, G (reprint author), Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland. EM gar@arm.ac.uk FU NASA, Science Mission Directorate; NASA [NAS5 26555]; NASA Office of Space Science [NAG5 7584]; Northern Ireland Government through the Department of Culture, Arts and Leisure FX Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate. The Kepler data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5 26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NAG5 7584 and by other grants and contracts. This work made use of PYKE, a software package for the reduction and analysis of Kepler data. This open source software project is developed and distributed by the NASA Kepler Guest Observer Office. Armagh Observatory is supported by the Northern Ireland Government through the Department of Culture, Arts and Leisure. We thank the anonymous referee for a useful report. NR 36 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2014 VL 442 IS 1 BP 489 EP 494 DI 10.1093/mnras/stu800 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RW UT WOS:000338765400044 ER PT J AU Dutta, P Chengalur, JN Roy, N Goss, WM Arjunwadkar, M Minter, AH Brogan, CL Lazio, TJW AF Dutta, Prasun Chengalur, Jayaram N. Roy, Nirupam Goss, W. M. Arjunwadkar, Mihir Minter, Anthony H. Brogan, Crystal L. Lazio, T. J. W. TI The structure function of Galactic H I opacity fluctuations on au scales based on MERLIN, VLA and VLBA data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE turbulence; ISM: atoms; ISM: general; ISM: structure; radio lines: ISM ID DIFFUSE INTERSTELLAR-MEDIUM; POWER SPECTRUM ANALYSIS; COLD NEUTRAL MEDIUM; ATOMIC-STRUCTURE; MAGNETIC-FIELDS; TURBULENCE; HYDROGEN; ABSORPTION; EMISSION; GAS AB We use MERLIN, VLA and VLBA observations of Galactic H I absorption towards 3C 138 to estimate the structure function of the H I opacity fluctuations at au scales. Using Monte Carlo simulations, we show that there is likely to be a significant bias in the estimated structure function at signal-to-noise ratios characteristic of our observations, if the structure function is constructed in the manner most commonly used in the literature. We develop a new estimator that is free from this bias and use it to estimate the true underlying structure function slope on length-scales ranging from 5 to 40 au. From a power-law fit to the structure function, we derive a slope of 0.81(-0.13)(+0.14), i.e. similar to the value observed at parsec scales. The estimated upper limit for the amplitude of the structure function is also consistent with the measurements carried out at parsec scales. Our measurements are hence consistent with the H I opacity fluctuation in the Galaxy being characterized by a power-law structure function over length-scales that span six orders of magnitude. This result implies that the dissipation scale has to be smaller than a few au if the fluctuations are produced by turbulence. This inferred smaller dissipation scale implies that the dissipation occurs either in (i) regions with densities greater than or similar to 10(3) cm(-3) (i. e. similar to that inferred for 'tiny scale' atomic clouds or (ii) regions with a mix of ionized and atomic gas (i. e. the observed structure in the atomic gas has a magnetohydrodynamic origin). C1 [Dutta, Prasun; Chengalur, Jayaram N.; Arjunwadkar, Mihir] Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Roy, Nirupam] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Goss, W. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Minter, Anthony H.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Brogan, Crystal L.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dutta, P (reprint author), Natl Ctr Radio Astrophys, Post Bag 3, Pune 411007, Maharashtra, India. EM prasun@ncra.tifr.res.in OI Arjunwadkar, Mihir/0000-0002-7653-8494 FU DST - INSPIRE fellowship [IFA-13 PH-54]; Alexander von Humboldt Foundation; Jansky Fellowship of the National Radio Astronomy Observatory; National Aeronautics and Space Administration FX The authors are grateful to K. Subramanian, A. Deshpande, N. Kanekar, S. Bharadwaj and S. Bhatnagar for useful discussions. This paper reports results from observations with MERLIN, VLA and VLBA. MERLIN is a National Facility operated by the University of Manchester at Jodrell Bank Observatory on behalf of PPARC/STFC. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. PD would like to acknowledge the DST - INSPIRE fellowship [IFA-13 PH-54 dated 2013 Aug 01] used while doing this research. NR acknowledges support from the Alexander von Humboldt Foundation and the Jansky Fellowship of the National Radio Astronomy Observatory. 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 33 TC 3 Z9 4 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2014 VL 442 IS 1 BP 647 EP 655 DI 10.1093/mnras/stu881 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RW UT WOS:000338765400055 ER PT J AU Thakur, N Gopalswamy, N Xie, H Makela, P Yashiro, S Akiyama, S Davila, JM AF Thakur, N. Gopalswamy, N. Xie, H. Maekelae, P. Yashiro, S. Akiyama, S. Davila, J. M. TI GROUND LEVEL ENHANCEMENT IN THE 2014 JANUARY 6 SOLAR ENERGETIC PARTICLE EVENT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE acceleration of particles; shock waves; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: particle emission; Sun: radio radiation ID CORONAL MASS EJECTIONS; SHOCK FORMATION; RELEASE TIMES; CYCLE 24; SECCHI AB We present a study of the 2014 January 6 solar energetic particle event which produced a small ground level enhancement (GLE), making it the second GLE of this unusual solar cycle 24. This event was primarily observed by the South Pole neutron monitors (increase of similar to 2.5%) while a few other neutron monitors recorded smaller increases. The associated coronal mass ejection (CME) originated behind the western limb and had a speed of 1960 km s(-1). The height of the CME at the start of the associated metric type II radio burst, which indicates the formation of a strong shock, was measured to be 1.61 Rs using a direct image from STEREO-A/EUVI. The CME height at the time of the GLE particle release (determined using the South Pole neutron monitor data) was directly measured as 2.96 Rs based on STEREO-A/COR1 white-light observations. These CME heights are consistent with those obtained for GLE71, the only other GLE of the current cycle, as well as cycle-23 GLEs derived using back-extrapolation. GLE72 is of special interest because it is one of only two GLEs of cycle 24, one of two behind-the-limb GLEs, and one of the two smallest GLEs of cycles 23 and 24. C1 [Thakur, N.; Gopalswamy, N.; Xie, H.; Maekelae, P.; Yashiro, S.; Akiyama, S.; Davila, J. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Thakur, N.; Xie, H.; Maekelae, P.; Yashiro, S.; Akiyama, S.] Catholic Univ Amer, Washington, DC 20064 USA. RP Thakur, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. OI Makela, Pertti/0000-0002-8182-4559 FU European Union [213007]; National Science Foundation; NASA's LWS TRT program FX We thank Dr. P. Evenson of Bartol Neutron Monitor Network for the neutron monitor asymptotic directions and useful discussions. We thank Dr. T. Kuwabara of Bartol for his help with the conversion of the IMF directions for Figure 3. We acknowledge the NMDB database (www.nmdb.eu), founded under the European Union's FP7 programme (contract No. 213007) for providing data. Neutron monitors of the Bartol Research Institute are supported by the National Science Foundation. STEREO is a mission in NASA's Solar Terrestrial Probes program. SOHO is a project of international collaboration between ESA and NASA. This work was supported by NASA's LWS TR&T program. NR 29 TC 18 Z9 18 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2014 VL 790 IS 1 AR L13 DI 10.1088/2041-8205/790/1/L13 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5ED UT WOS:000339878100013 ER PT J AU An, HJ Kaspi, VM Beloborodov, AM Kouveliotou, C Archibald, RF Boggs, SE Christensen, FE Craig, WW Gotthelf, EV Grefenstette, BW Hailey, CJ Harrison, FA Madsen, KK Mori, K Stern, D Zhang, WW AF An, Hongjun Kaspi, Victoria M. Beloborodov, Andrei M. Kouveliotou, Chryssa Archibald, Robert F. Boggs, Steven E. Christensen, Finn E. Craig, William W. Gotthelf, Eric V. Grefenstette, Brian W. Hailey, Charles J. Harrison, Fiona A. Madsen, Kristin K. Mori, Kaya Stern, Daniel Zhang, William W. TI NuSTAR OBSERVATIONS OF X-RAY BURSTS FROM THE MAGNETAR 1E 1048.1-5937 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (1E 1048.1-5937); stars: magnetars; stars: neutron; X-rays: bursts ID SOFT GAMMA-REPEATERS; NEUTRON-STARS; SGR 1627-41; PULSAR; 1E-1048.1-5937; VARIABILITY; SGR-1900+14; QUIESCENCE; EMISSION; OUTBURST AB We report the detection of eight bright X-ray bursts from the 6.5 s magnetar 1E 1048.1-5937, during a 2013 July observation campaign with the Nuclear Spectroscopic Telescope Array. We study the morphological and spectral properties of these bursts and their evolution with time. The bursts resulted in count rate increases by orders of magnitude, sometimes limited by the detector dead time, and showed blackbody spectra with kT 6-8 keV in the T90 duration of 1-4 s, similar to earlier bursts detected from the source. We find that the spectra during the tail of the bursts can be modeled with an absorbed blackbody with temperature decreasing with flux. The burst flux decays followed a power law of index 0.8-0.9. In the burst tail spectra, we detect a 13 keV emission feature, similar to those reported in previous bursts from this source as well as from other magnetars observed with the Rossi X-ray Timing Explorer. We explore possible origins of the spectral feature such as proton cyclotron emission, which implies a magnetic field strength of B 2x10(15) G in the emission region. However, the consistency of the energy of the feature in different objects requires further explanation. C1 [An, Hongjun; Kaspi, Victoria M.; Archibald, Robert F.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Beloborodov, Andrei M.; Gotthelf, Eric V.; Hailey, Charles J.; Mori, Kaya] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP An, HJ (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; An, Hongjun/0000-0002-6389-9012; Madsen, Kristin/0000-0003-1252-4891 FU National Aeronautics and Space Administration; NSERC Discovery Grant; FQRNT Centre de Recherche Astrophysique du Quebec; R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR); Canada Research Chairs Program; Lorne Trottier Chair in Astrophysics and Cosmology; NASA [NNX10AI72G, NNX13AI34G] FX This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). V. M. K. acknowledges support from an NSERC Discovery Grant, the FQRNT Centre de Recherche Astrophysique du Quebec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. A. M. B. acknowledges the support by NASA grants NNX10AI72G and NNX13AI34G. NR 37 TC 11 Z9 11 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 60 DI 10.1088/0004-637X/790/1/60 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800060 ER PT J AU Ballard, S Chaplin, WJ Charbonneau, D Desert, JM Fressin, F Zeng, L Werner, MW Davies, GR Aguirre, VS Basu, S Christensen-Dalsgaard, J Metcalfe, TS Stello, D Bedding, TR Campante, TL Handberg, R Karoff, C Elsworth, Y Gilliland, RL Hekker, S Huber, D Kawaler, SD Kjeldsen, H Lund, MN Lundkvist, M AF Ballard, Sarah Chaplin, William J. Charbonneau, David Desert, Jean-Michel Fressin, Francois Zeng, Li Werner, Michael W. Davies, Guy R. Aguirre, Victor Silva Basu, Sarbani Christensen-Dalsgaard, Jorgen Metcalfe, Travis S. Stello, Dennis Bedding, Timothy R. Campante, Tiago L. Handberg, Rasmus Karoff, Christoffer Elsworth, Yvonne Gilliland, Ronald L. Hekker, Saskia Huber, Daniel Kawaler, Steven D. Kjeldsen, Hans Lund, Mikkel N. Lundkvist, Mia TI KEPLER-93b: A TERRESTRIAL WORLD MEASURED TO WITHIN 120 km, AND A TEST CASE FOR A NEW SPITZER OBSERVING MODE SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; methods: observational; planetary systems; stars: individual (KOI 69, KIC 3544595) ID TRANSIT TIMING VARIATIONS; STELLAR EVOLUTION CODE; FINE GUIDANCE SENSOR; CIRCLE-PLUS PLANET; EARTH-SIZED PLANET; SOLAR-TYPE STARS; SUN-LIKE STAR; EXTRASOLAR PLANET; SPACE-TELESCOPE; HABITABLE ZONE AB We present the characterization of the Kepler-93 exoplanetary system, based on three years of photometry gathered by the Kepler spacecraft. The duration and cadence of the Kepler observations, in tandem with the brightness of the star, enable unusually precise constraints on both the planet and its host. We conduct an asteroseismic analysis of the Kepler photometry and conclude that the star has an average density of 1.652 +/- 0.006 g cm(-3). Its mass of 0.911 +/- 0.033M(circle dot) renders it one of the lowest-mass subjects of asteroseismic study. An analysis of the transit signature produced by the planet Kepler-93b, which appears with a period of 4.72673978 +/- 9.7 x 10(-7) days, returns a consistent but less precise measurement of the stellar density, 1.72(-0.28)(+0.02) g cm(-3). The agreement of these two values lends credence to the planetary interpretation of the transit signal. The achromatic transit depth, as compared between Kepler and the Spitzer Space Telescope, supports the same conclusion. We observed seven transits of Kepler-93b with Spitzer, three of which we conducted in a new observing mode. The pointing strategy we employed to gather this subset of observations halved our uncertainty on the transit radius ratio R-P/R-star. We find, after folding together the stellar radius measurement of 0.919 +/- 0.011R(circle dot) with the transit depth, a best-fit value for the planetary radius of 1.481 +/- 0.019 R-circle plus. The uncertainty of 120 km on our measurement of the planet's size currently renders it one of the most precisely measured planetary radii outside of the solar system. Together with the radius, the planetary mass of 3.8 +/- 1.5 M-circle plus. corresponds to a rocky density of 6.3 +/- 2.6 g cm(-3). After applying a prior on the plausible maximum densities of similarly sized worlds between 1 and 1.5 R-circle plus, we find that Kepler-93b possesses an average density within this group. C1 [Ballard, Sarah] Univ Washington, Seattle, WA 98195 USA. [Chaplin, William J.; Davies, Guy R.; Campante, Tiago L.; Handberg, Rasmus; Elsworth, Yvonne; Hekker, Saskia] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Chaplin, William J.; Davies, Guy R.; Aguirre, Victor Silva; Christensen-Dalsgaard, Jorgen; Metcalfe, Travis S.; Campante, Tiago L.; Handberg, Rasmus; Karoff, Christoffer; Elsworth, Yvonne; Kjeldsen, Hans; Lund, Mikkel N.; Lundkvist, Mia] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Charbonneau, David; Fressin, Francois; Zeng, Li] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Desert, Jean-Michel] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Werner, Michael W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Metcalfe, Travis S.] Space Sci Inst, Boulder, CO 80301 USA. [Stello, Dennis; Bedding, Timothy R.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Hekker, Saskia] Max Planck Inst Stromungsforsch, D-37077 Gottingen, Germany. [Hekker, Saskia] Univ Amsterdam, Astron Inst, NL-1012 WX Amsterdam, Netherlands. [Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA. [Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. RP Ballard, S (reprint author), Univ Washington, Seattle, WA 98195 USA. EM sarahba@uw.edu OI Zeng, Li/0000-0003-1957-6635; Davies, Guy/0000-0002-4290-7351; Metcalfe, Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965; Bedding, Tim/0000-0001-5222-4661; Basu, Sarbani/0000-0002-6163-3472; Lund, Mikkel Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571; Handberg, Rasmus/0000-0001-8725-4502 FU NASA through the Sagan Fellowship Program; NASA; NASA's Science Mission Directorate; Kepler Participatory Science [NNX12AC77G, NNX09AB53G]; John Templeton Foundation; UK Science and Technology Facilities Council (STFC); NSF [AST-1105930]; NASA [NNX13AE70G, NNX13AE91G, NNX14AB92G]; Danish National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) - European Research Council [267864]; Netherlands Organisation for Scientific Research (NWO); European Research Council under the European Community's Seventh Framework Programme/ERC [338251]; Australian Research Council; International Space Science Institute (ISSI) FX This work was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. It was conducted with 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. We thank the Spitzer team at the Infrared Processing and Analysis Center in Pasadena, California, and in particular Nancy Silbermann for scheduling the Spitzer observations of this program. This work is also based on observations made with Kepler, which was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. The authors would like to thank the many people who generously gave so much their time to make this Mission a success. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. S. Ballard thanks Geoffrey Marcy for helpful discussions about the RV signature of Kepler-93. We acknowledge support through Kepler Participatory Science Awards NNX12AC77G and NNX09AB53G, awarded to D.C. This publication was made possible in part through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. W.J.C., T.L.C., G.R.D., Y.E. and A.M. acknowledge the support of the UK Science and Technology Facilities Council (STFC). S. Basu acknowledges support from NSF grant AST-1105930 and NASA grant NNX13AE70G. Funding for the StellarAstrophysics Centre is provided by The Danish National Research Foundation (grant agreement No. DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement No. 267864). S.H. acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO). The research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 338251 (StellarAges). T.S.M. acknowledges NASA grant NNX13AE91G. D.S. is supported by the Australian Research Council. D.H. acknowledges support by an appointment to the NASA Postdoctoral Program at Ames Research Center administered by Oak Ridge Associated Universities, and NASA grant NNX14AB92G issued through the Kepler Participating Scientist Program. Computational time on Kraken at the National Institute of Computational Sciences was provided through NSF TeraGrid allocation TG-AST090107. We are also grateful for support from the International Space Science Institute (ISSI). NR 108 TC 20 Z9 20 U1 0 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 12 DI 10.1088/0004-637X/790/1/12 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800012 ER PT J AU Chung, SM Kochanek, CS Assef, R Brown, MJI Stern, D Jannuzi, BT Gonzalez, AH Hickox, RC Moustakas, J AF Chung, Sun Mi Kochanek, Christopher S. Assef, Roberto Brown, Michael J. I. Stern, Daniel Jannuzi, Buell T. Gonzalez, Anthony H. Hickox, Ryan C. Moustakas, John TI A UV TO MID-IR STUDY OF AGN SELECTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: distances and redshifts; quasars: general ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; WIDE-FIELD SURVEY; QUASAR LUMINOSITY FUNCTION; 7TH DATA RELEASE; X-RAY SURVEY; DEEP FIELD; MIDINFRARED SELECTION; PHOTOMETRIC REDSHIFTS; BOOTES FIELD AB We classify the spectral energy distributions (SEDs) of 431,038 sources in the 9 deg(2) Bootes field of the NOAO Deep Wide-Field Survey (NDWFS). There are up to 17 bands of data available per source, including ultraviolet (GALEX), optical (NDWFS), near-IR (NEWFIRM), and mid-infrared (IRAC and MIPS) data, as well as spectroscopic redshifts for similar to 20,000 objects, primarily from the AGN and Galaxy Evolution Survey. We fit galaxy, active galactic nucleus (AGN), stellar, and brown dwarf templates to the observed SEDs, which yield spectral classes for the Galactic sources and photometric redshifts and galaxy/AGN luminosities for the extragalactic sources. The photometric redshift precision of the galaxy and AGN samples are sigma/(1 + z) = 0.040 and sigma/(1 + z) = 0.169, respectively, with the worst 5% outliers excluded. On the basis of the chi(2)(nu) of the SED fit for each SED model, we are able to distinguish between Galactic and extragalactic sources for sources brighter than I = 23.5 mag. We compare the SED fits for a galaxy-only model and a galaxy-AGN model. Using known X-ray and spectroscopic AGN samples, we confirm that SED fitting can be successfully used as a method to identify large populations of AGNs, including spatially resolved AGNs with significant contributions from the host galaxy and objects with the emission line ratios of "composite" spectra. We also use our results to compare with the X-ray, mid-IR, optical color, and emission line ratio selection techniques. For an F-ratio threshold of F > 10, we find 16,266 AGN candidates brighter than I = 23.5 mag and a surface density of similar to 1900 AGN deg(-2). C1 [Chung, Sun Mi; Kochanek, Christopher S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Assef, Roberto] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jannuzi, Buell T.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Jannuzi, Buell T.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Hickox, Ryan C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. RP Chung, SM (reprint author), Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA. RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 FU Gemini-CONICYT [32120009] FX The authors thank the Bootes collaborations for contributing to the various Bootes photometric catalogs. The work of D.S. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. R.J.A. was supported by Gemini-CONICYT grant number 32120009. NR 82 TC 8 Z9 9 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 54 DI 10.1088/0004-637X/790/1/54 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800054 ER PT J AU Cohen, O Drake, JJ Glocer, A Garraffo, C Poppenhaeger, K Bell, JM Ridley, AJ Gombosi, TI AF Cohen, O. Drake, J. J. Glocer, A. Garraffo, C. Poppenhaeger, K. Bell, J. M. Ridley, A. J. Gombosi, T. I. TI MAGNETOSPHERIC STRUCTURE AND ATMOSPHERIC JOULE HEATING OF HABITABLE PLANETS ORBITING M-DWARF STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics ( MHD); planets and satellites: atmospheres; planets and satellites: magnetic fields; planets and satellites: terrestrial planets ID MAIN-SEQUENCE STARS; RESISTIVE MHD SIMULATIONS; EARTH-LIKE EXOPLANETS; EJECTION CME ACTIVITY; MASS-LOSS RATES; X-RAY-EMISSION; HOT JUPITERS; OHMIC DISSIPATION; MAGNETIC-FIELD; HD 209458B AB We study the magnetospheric structure and the ionospheric Joule Heating of planets orbiting M-dwarf stars in the habitable zone using a set ofmagnetohydrodynamic models. The stellarwind solution is used to drive amodel for the planetary magnetosphere, which is coupled with a model for the planetary ionosphere. Our simulations reveal that the space environment around close-in habitable planets is extreme, and the stellar wind plasma conditions change from sub-to super-Alfv ' enic along the planetary orbit. As a result, themagnetospheric structure changes dramatically with a bow shock forming in the super-Alfv ' enic sectors, while no bow shock forms in the sub-Alfv ' enic sectors. The planets reside most of the time in the sub-Alfv ' enic sectors with poor atmospheric protection. A significant amount of Joule Heating is provided at the top of the atmosphere as a result of the intense stellar wind. For the steady-state solution, the heating is about 0.1%-3% of the total incoming stellar irradiation, and it is enhanced by 50% for the time-dependent case. The significant Joule Heating obtained here should be considered in models for the atmospheres of habitable planets in terms of the thickness of the atmosphere, the top-side temperature and density, the boundary conditions for the atmospheric pressure, and particle radiation and transport. Here we assume constant ionospheric Pedersen conductance similar to that of the Earth. The conductance could be greater due to the intense EUV radiation leading to smaller heating rates. We plan to quantify the ionospheric conductance in future study. C1 [Cohen, O.; Drake, J. J.; Garraffo, C.; Poppenhaeger, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Glocer, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bell, J. M.] Natl Inst Aerosp, Ctr Planetary Atmospheres & Flight Sci, Hampton, VA 23666 USA. [Ridley, A. J.; Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Glocer, Alex/C-9512-2012; Gombosi, Tamas/G-4238-2011; Ridley, Aaron/F-3943-2011; OI Glocer, Alex/0000-0001-9843-9094; Gombosi, Tamas/0000-0001-9360-4951; Ridley, Aaron/0000-0001-6933-8534; Poppenhaeger, Katja/0000-0003-1231-2194; Cohen, Ofer/0000-0003-3721-0215 FU NASA ESS; NASA ESTO-CT; NSF KDI; DoDMURI; NASA HEC Pleiades system [SMD-13-4076]; NASA [NAS8-03060] FX We thank an unknown referee for comments and suggestions. The work presented here was funded by the Smithsonian Institution Consortium for Unlocking the Mysteries of the Universe grant " Lessons from Mars: Are Habitable Atmospheres on Planets around M Dwarfs Viable?," and by the Smithsonian Institute Competitive Grants Program for Science (CGPS) grant " Can Exoplanets Around Red Dwarfs Maintain Habitable Atmospheres?." Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoDMURI. The simulations were performed on the NASA HEC Pleiades system under award SMD-13-4076. J. J. D. was supported by NASA contract NAS8-03060 to the Chandra X-ray Center during the course of this research and thanks the Director, H. Tananbaum, for continuing support and encouragement. NR 86 TC 24 Z9 24 U1 0 U2 12 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 JUL 20 PY 2014 VL 790 IS 1 AR 57 DI 10.1088/0004-637X/790/1/57 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800057 ER EF