FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Behrangi, A Casey, SPF Lambrigtsen, BH AF Behrangi, Ali Casey, Sean P. F. Lambrigtsen, Bjorn H. TI Three-dimensional distribution of cloud types over the USA and surrounding areas observed by CloudSat SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID PRECIPITATION ESTIMATION; CLASSIFICATION-SYSTEM; NEURAL-NETWORK; AVHRR IMAGERY; MISSION AB The vertical and horizontal distributions of the cloud types across different seasons and over the contiguous USA and surrounding areas are studied. The study is performed by collecting two years (2007 and 2008) of data from the CloudSat 2B-CLDCLASS product that uses effective radar reflectivity factor Ze, the presence of precipitation and ancillary data such as surface topography and the model-predicted temperature profile to classify clouds into seven distinct types. Considerable seasonal variations of the horizontal distribution of the cloud-type fractions are observed in the study area among different seasons and for both daytime and night-time CloudSat observations. It was found that during spring and summer, deep convective (Dc) clouds are observed much more frequently during night-time than during daytime over both the land and ocean. For the studied area and during daytime, low clouds were more frequent (up to similar to 50%) over the land and less frequent over the ocean compared with night-time observations. Analysis of the vertical distribution of cloud layers reveals that the fraction of cloudy scenes with two or more distinct cloud layers is the highest (up to 30%) over the northwest corner of the USA and the southwest corner of Canada and the nearby oceans. The southwest corner of the USA and the nearby east Pacific Ocean appeared to have the lowest fraction (<0.05%) of cloudy scenes with two or more distinct cloud layers. Over the land, approximately 18% of the total cloudy scenes are classified as two-layer clouds, whereas over the ocean, two-layer clouds are less frequent and range from 13% to 17% with a stronger seasonal dependency. Only about 2-3% of the total cloudy scenes are classified as multilayer clouds, with three or more distinct layers over both the land and ocean. The vertical distribution of cloud-top heights over both the land and ocean shows two distinct peaks. Over the land, the lower peak, at around 2 km, is almost independent of season, whereas the higher peak is seasonally dependent and varies between similar to 8 km (during winter) and similar to 11 km (during summer). Over the ocean, the lower peak is also observed near 2 km (or less), whereas the higher peak ranges approximately from 11 km (during winter) to 12 km (during summer). C1 [Behrangi, Ali; Casey, Sean P. F.; Lambrigtsen, Bjorn H.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM ali.behrangi@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this article was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. (C) 2011 California Institute of Technology. Government sponsorship is acknowledged. NR 16 TC 1 Z9 1 U1 3 U2 9 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PY 2012 VL 33 IS 16 BP 4856 EP 4870 DI 10.1080/01431161.2011.639404 PG 15 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 917JE UT WOS:000302169400002 ER PT J AU Kokkalis, P Mamouri, RE Todua, M Didebulidze, GG Papayannis, A Amiridis, V Basart, S Perez, C Baldasano, JM AF Kokkalis, P. Mamouri, R. E. Todua, M. Didebulidze, G. G. Papayannis, A. Amiridis, V. Basart, S. Perez, C. Baldasano, J. M. TI Ground-, satellite- and simulation-based analysis of a strong dust event over Abastumani, Georgia, during May 2009 SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID OPTICAL-PROPERTIES; AIR-QUALITY; AEROSOL; LIDAR; VALIDATION; ALGORITHM; INVERSION; AREAS; SPAIN; CYCLE AB A strong dust event over Abastumani, Georgia, during May 2009 was studied using light detection and ranging (lidar), satellite and sun photometric measurements. High aerosol optical depth (AOD) values (0.45-0.57) at 500 nm were measured over the closest Aerosol Robotic Network (AERONET) site (Erdemli, Turkey), whereas over Georgia, the AOD measured by the Moderate Resolution Imaging Spectroradiometer (MODIS) was about 0.9 at 550 nm. The AERONET data analysis showed a mean aerosol effective radius of about 2.5 mu m, whereas the mean value of the Angstrom exponent (alpha) (wavelength pair 440/870 nm) was smaller than 1, indicating the dominance of large aerosols. The aerosol lidar over Abastumani showed the existence of a strong particle load from the near ground up to a height of 3.5 km. The BSC-DREAM8b forecast model showed that the dust aerosols travelled from the Saharan and the Arabic deserts to the studied area, even reaching southern Russia, covering a total distance of about 5500 km, in the height region from about 2 to 11.5 km. C1 [Kokkalis, P.; Mamouri, R. E.; Papayannis, A.] Natl Tech Univ Athens, Dept Phys, Laser Remote Sensing Lab, GR-15773 Athens, Greece. [Todua, M.; Didebulidze, G. G.] Ilia State Univ, Georgian Natl Astrophys Observ, Tbilisi, Rep of Georgia. [Amiridis, V.] Natl Observ Athens, Inst Space Applicat & Remote Sensing, Athens, Greece. [Basart, S.; Baldasano, J. M.] Barcelona Supercomp Ctr, Div Earth Sci, Barcelona, Spain. [Perez, C.] Columbia Univ, Earth Inst, NASA Goddard Inst Space Studies, New York, NY USA. [Perez, C.] Int Res Inst Climate & Soc, New York, NY USA. [Baldasano, J. M.] Univ Politecn Cataluna, Environm Modelling Lab, Project Engn Dept, Barcelona, Spain. RP Papayannis, A (reprint author), Natl Tech Univ Athens, Dept Phys, Laser Remote Sensing Lab, Zografou Campus, GR-15773 Athens, Greece. EM apdlidar@central.ntua.gr RI Amiridis, Vassilis/G-6769-2012; Kokkalis, Panagiotis/I-8531-2014; OI Amiridis, Vassilis/0000-0002-1544-7812; Basart, Sara/0000-0002-9821-8504; Perez Garcia-Pando, Carlos/0000-0002-4456-0697 NR 35 TC 7 Z9 7 U1 1 U2 7 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PY 2012 VL 33 IS 16 BP 4886 EP 4901 DI 10.1080/01431161.2011.644593 PG 16 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 917JE UT WOS:000302169400004 ER PT J AU Raja, MKRV Wu, XQ Yu, FF AF Raja, M. K. Rama Varma Wu, Xiangqian Yu, Fangfang TI Assessment of MetOp-A Advanced Very High Resolution Radiometer (AVHRR) short-wave infrared channel measurements using Infrared Atmospheric Sounding Interferometer (IASI) observations and line-by-line radiative transfer model simulations SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID LAND-SURFACE TEMPERATURE; CALIBRATION; RADIANCES; NOAA-16 AB MetOp-A satellite-based hyper-spectral Infrared Atmospheric Sounding Interferometer (IASI) observations are used to evaluate the accuracy of the broadband short-wave infrared (SWIR) atmospheric window channel (channel 3B) centred at 3.74 mu m of the Advanced Very High Resolution Radiometer (AVHRR) carried on the same platform. To complement the partial spectral coverage of IASI, line-by-line radiative transfer model (LBLRTM)-simulated IASI spectra are used. The comparisons result in significant negative AVHRR minus IASI bias in radiance (similar to-0.04 mW m(-2) sr(-1) cm(-1)) with scene temperature dependency in which the absolute value of the bias linearly increases with increasing temperature. It is demonstrated that the negative bias and the scene temperature dependency of the bias are the results of significant absorption in the portion of AVHRR spectral band not seen by IASI, leading to the conclusion that MetOp-A AVHRR channel 3B is not purely an 'atmospheric window' channel. C1 [Raja, M. K. Rama Varma] NASA, NPP OMPS Sci Operat Ctr, Goddard Space Flight Ctr, Lanham, MD 20706 USA. [Yu, Fangfang] NOAA, Sensor Phys Branch, ERT Syst Inc, NESDIS,STAR, Camp Springs, MD 20746 USA. RP Raja, MKRV (reprint author), NASA, NPP OMPS Sci Operat Ctr, Goddard Space Flight Ctr, Lanham, MD 20706 USA. EM ramavarmaraja.mundakkara-kovilakom@nasa.gov RI Yu, Fangfang/E-7942-2011; Wu, Xiangqian/F-5634-2010 OI Yu, Fangfang/0000-0001-8343-0863; Wu, Xiangqian/0000-0002-7804-5650 FU I.M. Systems Group, Inc.; NOAA/NESDIS/STAR; NOAA [IA1-1016] FX The authors are grateful to Dr Michael Weinreb of NOAA/NESDIS/SOCC for helpful discussions during the course of the work. M. K. Rama Varma Raja also gratefully acknowledges the helpful discussions during the course of the reported work with Dr Changyong Cao (NOAA/NESDIS/STAR), Dr Likun Wang (Dell Services Federal Government@NOAA/NESDIS/STAR) and Dr Ruiyue Chen (I. M. Systems Group, Inc.@NOAA/NESDIS/STAR). M. K. Rama Varma Raja gratefully acknowledges the support received from I.M. Systems Group, Inc., during the course of this work. This work was funded by the NOAA/NESDIS/STAR cal/val project and the NOAA Science Data Stewardship project through the interagency agreement IA1-1016. The contents are solely the opinions of the authors and do not constitute a statement of policy, decision or position on behalf of the NOAA or the US Government. NR 20 TC 1 Z9 1 U1 0 U2 2 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PY 2012 VL 33 IS 16 BP 5240 EP 5250 DI 10.1080/01431161.2012.656766 PG 11 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 917JE UT WOS:000302169400022 ER PT J AU Tkacik, DS Luna-Cruz, Y Clinton, N Spak, S Ryan, J AF Tkacik, Daniel S. Luna-Cruz, Yaitza Clinton, Nicholas Spak, Scott Ryan, John TI Atmospheric correction for MASTER image data using localized modelled and observed meteorology and trace gases SO REMOTE SENSING LETTERS LA English DT Article ID ARCTAS-CARB PERIOD; OZONE; MODIS; CALIFORNIA; ALGORITHM AB Atmospheric correction for remote sensing-based studies typically does not use information from spatio-temporally resolved meteorological models. We assessed the effect of using observations and mesoscale weather and chemical transport models on multispectral retrievals of land and ocean properties. We performed two atmospheric corrections on image data acquired by the Moderate Resolution Imaging Spectroradiometer (MODIS)/Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) airborne simulator over Monterey Bay, California. One correction used local atmospheric profiles of meteorology and trace gases at overpass and the other used the 1976 US Standard default atmospheric profile in the MODTRAN4 radiative transfer model. We found only minor impacts from atmospheric correction in the Fluorescence Line Height index of ocean chlorophyll, but substantive differences in retrievals of surface temperature and the Normalized Difference Vegetation Index. Improvements in sea surface temperature retrieval were validated by in situ measurements. Results indicate that spatio-temporally specific atmospheric correction factors from mesoscale models can improve retrievals of surface properties from remotely sensed image data. C1 [Clinton, Nicholas] NASA, Airborne Sensor Facil, Ames Res Ctr, Moffett Field, CA 94035 USA. [Tkacik, Daniel S.] Carnegie Mellon Univ, Dept Civil & Environm Engn, Pittsburgh, PA 15213 USA. [Luna-Cruz, Yaitza] Howard Univ, Ctr Atmospher Sci, NOAA, Washington, DC 20059 USA. [Spak, Scott] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA USA. [Ryan, John] Monterey Bay Aquarium Res Inst, Moss Landing, CA USA. RP Clinton, N (reprint author), NASA, Airborne Sensor Facil, Ames Res Ctr, Moffett Field, CA 94035 USA. EM nicholas.clinton@nasa.gov RI Spak, Scott/B-7331-2008; Tkacik, Daniel/G-5630-2011 OI Spak, Scott/0000-0002-8545-1411; FU National Aeronautics and Space Administration (NASA); National Suborbital Education and Research Center (NSERC) FX This research was supported by the National Aeronautics and Space Administration (NASA) and the National Suborbital Education and Research Center (NSERC) during the 2009 Student Airborne Research Program (SARP). In situ data collection was supported by R. Kudela (University of California, Santa Cruz). NR 22 TC 0 Z9 0 U1 2 U2 9 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 2150-704X J9 REMOTE SENS LETT JI Remote Sens. Lett. PY 2012 VL 3 IS 3 BP 201 EP 209 DI 10.1080/01431161.2010.551550 PG 9 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 918KH UT WOS:000302247900003 ER PT J AU Raynolds, MK Walker, DA Epstein, HE Pinzon, JE Tucker, CJ AF Raynolds, Martha K. Walker, Donald A. Epstein, Howard E. Pinzon, Jorge E. Tucker, Compton J. TI A new estimate of tundra-biome phytomass from trans-Arctic field data and AVHRR NDVI SO REMOTE SENSING LETTERS LA English DT Article ID VEGETATION; ALASKA; REFLECTANCE; ECOSYSTEMS; TRENDS; MODIS AB It is often assumed that the Normalized Difference Vegetation Index (NDVI) can be equated to aboveground plant biomass, but such a relationship has never been quantified at a global biome scale. We sampled aboveground plant biomass (phytomass) at representative zonal sites along two trans-Arctic transects, one in North America and one in Eurasia, and compared these data to satellite-derived NDVI. The results showed a remarkably strong correlation between total aboveground phytomass sampled at the peak of summer and the maximum annual NDVI (R-2 = 0.94, p < 0.001). The relationship was almost identical for the North America and Eurasia transects. The NDVI-phytomass relationship was used to make an aboveground phytomass map of the tundra biome. The approach uses a new and more accurate NDVI data set for the Arctic (GIMMS3g) and a sampling protocol that employs consistent methods for site selection, clip harvest and sorting and weighing of plant material. Extrapolation of the results to zonal landscape-level phytomass estimates provides valuable data for monitoring and modelling tundra vegetation. C1 [Raynolds, Martha K.; Walker, Donald A.] Univ Alaska, Inst Arctic Biol, Fairbanks, AK 99775 USA. [Epstein, Howard E.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. [Pinzon, Jorge E.; Tucker, Compton J.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. RP Raynolds, MK (reprint author), Univ Alaska, Inst Arctic Biol, Fairbanks, AK 99775 USA. EM mkraynolds@alaska.edu FU US National Science Foundation [OPP-0120736, ARC-0531180, ARC-0425517, ARC-0902175]; National Aeronautics and Space Administration [NNG6GE00A, NNX09AK56G] FX Uma S. Bhatt (UAF-GI) has been instrumental in validating the GIMMS3g NDVI data. Many people made the work possible along these remote transects, in particular the Earth Cryosphere Institute in Russia, the Aurora Institute in Canada and the field teams. This work is part of the Greening of the Arctic initiative of the International Polar Year, with funding from the US National Science Foundation (grants OPP-0120736, ARC-0531180, ARC-0425517, ARC-0902175) and the National Aeronautics and Space Administration (grants NNG6GE00A, NNX09AK56G). NR 23 TC 40 Z9 45 U1 4 U2 39 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 2150-704X EI 2150-7058 J9 REMOTE SENS LETT JI Remote Sens. Lett. PY 2012 VL 3 IS 5 BP 403 EP 411 DI 10.1080/01431161.2011.609188 PG 9 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 918KM UT WOS:000302248400004 ER PT J AU Signorini, SR McClain, CR AF Signorini, Sergio R. McClain, Charles R. TI Subtropical gyre variability as seen from satellites SO REMOTE SENSING LETTERS LA English DT Article ID CHLOROPHYLL-A CONCENTRATION; NORTH PACIFIC; PHYTOPLANKTON BIOMASS; ATLANTIC-OCEAN; GROWTH AB A satellite multi-sensor approach is used to analyse the biological response of open ocean regions of the subtropical gyres to changes in physical forcing. Thirteen years (19982010) of Sea-viewing Wide Field-of-view Sensor (SeaWiFS) chlorophyll-a (chl-a) data, combined with concurrent satellite records of sea-surface temperature (SST) and sea level height, were analysed to investigate the seasonal and inter-annual variability of chl-a concentration within these immense so-called ocean deserts. The seasonal variability of chl-a within the gyres is driven mostly by the warming/cooling of surface waters. Summer warming promotes shallower mixed layers and lower chl-a due to a reduction of vertical mixing and consequently a decrease in nutrient supply. The opposite happens during the winter cooling period. Therefore, long-term trends in SST have the potential to cause an impact on the inter-annual variability of chl-a. Our analyses show that, during the 13 whole years of SeaWiFS data record, the North Pacific, Indian Ocean and North Atlantic gyres experienced a decrease in chl-a of 9%, 12% and 11%, respectively, with corresponding SST increases of 0.27 degrees C, 0.42 degrees C and 0.32 degrees C, respectively. The South Pacific and South Atlantic gyres also showed warming trends but with weak positive trends in chl-a that are not statistically significant. We hypothesize that the warming of surface waters in these two gyres is counterbalanced by other interacting physical- and biological-driving mechanisms, as indicated in previous studies. C1 [Signorini, Sergio R.; McClain, Charles R.] NASA, Ocean Ecol Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Signorini, Sergio R.] SAIC, Sci Support Div, Beltsville, MD 20705 USA. RP Signorini, SR (reprint author), NASA, Ocean Ecol Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM sergio.signorini@nasa.gov FU NASA FX We acknowledge the NASA Ocean Biology and Biogeochemistry Programme for supporting this work. NR 17 TC 8 Z9 8 U1 3 U2 14 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 2150-704X J9 REMOTE SENS LETT JI Remote Sens. Lett. PY 2012 VL 3 IS 6 BP 471 EP 479 DI 10.1080/01431161.2011.625053 PG 9 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 918IZ UT WOS:000302244100002 ER PT J AU Chen, YS Malkovskiy, A Wang, XQ Lebron-Colon, M Sokolov, AP Perry, K More, K Pang, Y AF Chen, Yusheng Malkovskiy, Andrey Wang, Xiao-Qian Lebron-Colon, Marisabel Sokolov, Alexei P. Perry, Kelly More, Karren Pang, Yi TI Selection of Single-Walled Carbon Nanotube with Narrow Diameter Distribution by Using a PPE-PPV Copolymer SO ACS MACRO LETTERS LA English DT Article ID SEPARATION; DISPERSION; POLYMERS; FUNCTIONALIZATION; RECOGNITION; TRANSISTORS; ENRICHMENT AB Electronic and mechanic properties Of single-walled carbon nanotubes (SWNTs) are uniquely dependent on the tube's chiralities and diameters. Isolation of different. type SWNTs remains one of the fundamental and challenging issues in nanotube science. Herein, we demonstrate that SWNTs can be effectively enriched to a narrow diameter range by sequential treatment of the HiPco sample with nitric acid and a pi-conjugated copolymer poly(phenyleneethynylene) (PPE)-co-poly(phenylenevinylene) (PPV). On the basis of Raman, fluorescence, and microscopic evidence, the nitric acid is found to selectively remove the SWNTsof small diameter. The polymer not only effectively dispersed carbon nanotubes but also exhibited a good selectivity toward a few SWNTs. The reported approach thus offers a new methodology to isolate SWNTs, which has the potential to operate in a relatively large scale. C1 [Chen, Yusheng; Pang, Yi] Univ Akron, Dept Chem, Akron, OH 44325 USA. [Malkovskiy, Andrey] Univ Akron, Dept Polymer Sci, Akron, OH 44325 USA. [Wang, Xiao-Qian] Clark Atlanta Univ, Dept Phys, Dept Chem, Atlanta, GA 30314 USA. [Wang, Xiao-Qian] Clark Atlanta Univ, Ctr Funct Nanoscale Mat, Atlanta, GA 30314 USA. [Lebron-Colon, Marisabel] NASA Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. [Sokolov, Alexei P.; Perry, Kelly; More, Karren] Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA. RP Pang, Y (reprint author), Univ Akron, Dept Chem, Akron, OH 44325 USA. EM yp5@uakron.edu RI More, Karren/A-8097-2016 OI More, Karren/0000-0001-5223-9097 FU AFOSR [FA9550-10-1-0254]; Materials Science and Engineering Division; Office of Basic Energy Sciences, U.S. Department of Energy FX This work was supported by AFOSR (Grant FA9550-10-1-0254). APS acknowledges partial support from the Materials Science and Engineering Division and the SHaRE user Facility, which are sponsored by the Office of Basic Energy Sciences, U.S. Department of Energy. NR 37 TC 23 Z9 24 U1 3 U2 25 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 2161-1653 J9 ACS MACRO LETT JI ACS Macro Lett. PD JAN PY 2012 VL 1 IS 1 BP 246 EP 251 DI 10.1021/mz2001093 PG 6 WC Polymer Science SC Polymer Science GA 913YR UT WOS:000301913800055 ER PT J AU Xie, Y Yang, P Kattawar, GW Minnis, P Hu, YX Wu, DL AF Xie, Yu Yang, Ping Kattawar, George W. Minnis, Patrick Hu, Yongxiang Wu, Dong L. TI Determination of ice cloud models using MODIS and MISR data SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID IN-SITU OBSERVATIONS; BULK SCATTERING PROPERTIES; MULTIANGLE IMAGING SPECTRORADIOMETER; POLARIZED-LIGHT SCATTERING; SATELLITE-BASED RETRIEVAL; CIRRUS CLOUDS; OPTICAL-THICKNESS; RADIATIVE PROPERTIES; PART I; MICROPHYSICAL PROPERTIES AB Representation of ice clouds in radiative transfer simulations is subject to uncertainties associated with the shapes and sizes of ice crystals within cirrus clouds. In this study, we examined several ice cloud models consisting of smooth, roughened, homogeneous and inhomogeneous hexagonal ice crystals with various aspect ratios. The sensitivity of the bulk scattering properties and solar reflectances of cirrus clouds to specific ice cloud models is investigated using the improved geometric optics method (IGOM) and the discrete ordinates radiative transfer (DISORT) model. The ice crystal habit fractions in the ice cloud model may significantly affect the simulations of cloud reflectances. A new algorithm was developed to help determine an appropriate ice cloud model for application to the satellite-based retrieval of ice cloud properties. The ice cloud particle size retrieved from Moderate Resolution Imaging Spectroradiometer (MODIS) data, collocated with Multi-angle Imaging Spectroradiometer (MISR) observations, is used to infer the optical thicknesses of ice clouds for nine MISR viewing angles. The relative differences between view-dependent cloud optical thickness and the averaged value over the nine MISR viewing angles can vary from -0.5 to 0.5 and are used to evaluate the ice cloud models. In the case for 2 July 2009, the ice cloud model with mixed ice crystal habits is the best fit to the observations (the root mean square (RMS) error of cloud optical thickness reaches 0.365). This ice cloud model also produces consistent cloud property retrievals for the nine MISR viewing configurations within the measurement uncertainties. C1 [Xie, Yu; Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Kattawar, George W.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Minnis, Patrick; Hu, Yongxiang] NASA Langley Res Ctr, Hampton, VA 23681 USA. [Wu, Dong L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Xie, Y (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM xieyupku@tamu.edu RI Yang, Ping/B-4590-2011; Hu, Yongxiang/K-4426-2012; Wu, Dong/D-5375-2012; Minnis, Patrick/G-1902-2010 OI Minnis, Patrick/0000-0002-4733-6148 FU NASA [NNX09AP63G, NNX10AL55G]; Office of Naval Research [N00014-06-1-0069, N00014-11-1-0154]; NASA SMD FX This study was partly supported by NASA grants NNX09AP63G and NNX10AL55G. George W. Kattawar's research was supported by the Office of Naval Research under contracts N00014-06-1-0069 and N00014-11-1-0154. Patrick Minnis was supported by the NASA SMD Radiation Sciences Program through the Clouds and the Earth's Radiant Energy System Project. The work by Dong L. Wu was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 79 TC 4 Z9 4 U1 0 U2 7 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PY 2012 VL 33 IS 13 BP 4219 EP 4253 DI 10.1080/01431161.2011.642323 PG 35 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 917IX UT WOS:000302168500012 ER PT J AU Mace, TH AF Mace, Thomas H. TI At-sea detection of marine debris: Overview of technologies, processes, issues, and options SO MARINE POLLUTION BULLETIN LA English DT Article DE Marine debris; Remote sensing; Radar; Hyperspectral; Sampling; Derelict fishing gear AB At-sea detection of marine debris presents a difficult problem, as the debris items are often relatively small and partially submerged. However, they may accumulate in water parcel boundaries or eddy lines. The application of models, satellite radar and multispectral data, and airborne remote sensing (particularly radar) to focus the search on eddies and convergence zones in the open ocean appear to be a productive avenue of investigation. A multistage modeling and remote sensing approach is proposed for the identification of areas of the open ocean where debris items are more likely to congregate. A path forward may best be achieved through the refinement of the Ghost Net procedures with the addition of a final search stage using airborne radar from an UAS simulator aircraft to detect zones of potential accumulation for direct search. Sampling strategies, direct versus indirect measurements, remote sensing resolution, sensor/platform considerations, and future state are addressed. Published by Elsevier Ltd. C1 NASA Dryden Flight Res Ctr, Edwards AFB, CA 93523 USA. RP Mace, TH (reprint author), NASA Dryden Flight Res Ctr, POB 273, Edwards AFB, CA 93523 USA. EM thomas.h.mace@nasa.gov NR 10 TC 16 Z9 16 U1 5 U2 34 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-326X EI 1879-3363 J9 MAR POLLUT BULL JI Mar. Pollut. Bull. PY 2012 VL 65 IS 1-3 BP 23 EP 27 DI 10.1016/j.marpolbul.2011.08.042 PG 5 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 913SE UT WOS:000301896900004 PM 21939986 ER PT J AU Lissauer, JJ AF Lissauer, Jack J. TI Exoplanets: Birth of a new field of study SO NEW ASTRONOMY REVIEWS LA English DT Editorial Material C1 NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP Lissauer, JJ (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA. EM Jack.J.Lissauer@nasa.gov NR 2 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD JAN PY 2012 VL 56 IS 1 BP 1 EP 1 DI 10.1016/j.newar.2011.07.001 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 913WJ UT WOS:000301907800001 ER PT J AU Lee, YH Adams, PJ AF Lee, Y. H. Adams, P. J. TI A Fast and Efficient Version of the TwO-Moment Aerosol Sectional (TOMAS) Global Aerosol Microphysics Model SO AEROSOL SCIENCE AND TECHNOLOGY LA English DT Article ID KINETIC COLLECTION EQUATION; CLOUD CONDENSATION NUCLEI; SULFURIC-ACID; NUCLEATION EVENTS; SIZE DISTRIBUTION; BOUNDARY-LAYER; CCN; SIMULATION; WATER; PARAMETERIZATION AB This study develops more computationally efficient versions of the TwO-Moment Aerosol Sectional (TOMAS) microphysics algorithms, collectively called "Fast TOMAS." Several methods for speeding up the algorithm were attempted, but only reducing the number of size sections was adopted. Fast TOMAS models, coupled to the GISS GCM II-prime, require a new coagulation algorithm with less restrictive size resolution assumptions but only minor changes in other processes. Fast TOMAS models have been evaluated in a box model against analytical solutions of coagulation and condensation and in a 3-D model against the original TOMAS (TOMAS-30) model. Condensation and coagulation in the Fast TOMAS models agree well with the analytical solution but show slightly more bias than the TOMAS-30 box model. In the 3-D model, errors resulting from decreased size resolution in each process (i.e., emissions, cloud processing/wet deposition, microphysics) are quantified in a series of model sensitivity simulations. Errors resulting from lower size resolution in condensation and coagulation, defined as the microphysics error, affect number and mass concentrations by only a few percent. The microphysics error in CN70/CN100 (number concentrations of particles larger than 70/100 nm diameter), proxies for cloud condensation nuclei, range from -5% to 5% in most regions. The largest errors are associated with decreasing the size resolution in the cloud processing/wet deposition calculations, defined as cloud-processing error, and range from -20% to 15% in most regions for CN70/CN100 concentrations. Overall, the Fast TOMAS models increase the computational speed by 2 to 3 times with only small numerical errors stemming from condensation and coagulation calculations when compared to TOMAS-30. The faster versions of the TOMAS model allow for the longer, multi-year simulations required to assess aerosol effects on cloud lifetime and precipitation. C1 [Lee, Y. H.; Adams, P. J.] Columbia Univ, NASA Goddard Inst Space Studies, New York, NY 10025 USA. [Lee, Y. H.; Adams, P. J.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. [Adams, P. J.] Carnegie Mellon Univ, Dept Engn & Publ Policy, Pittsburgh, PA 15213 USA. RP Lee, YH (reprint author), Columbia Univ, NASA Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM Yunha.lee.00@gmail.com RI Adams, Peter/D-7134-2013; Lee, Yunha/Q-7222-2016 OI Adams, Peter/0000-0003-0041-058X; Lee, Yunha/0000-0001-7478-2672 FU Environmental Protection Agency (EPA STAR) [83337401] FX This study was supported by the Environmental Protection Agency (EPA STAR Award 83337401). NR 44 TC 17 Z9 19 U1 0 U2 13 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0278-6826 EI 1521-7388 J9 AEROSOL SCI TECH JI Aerosol Sci. Technol. PY 2012 VL 46 IS 6 BP 678 EP 689 DI 10.1080/02786826.2011.643259 PG 12 WC Engineering, Chemical; Engineering, Mechanical; Environmental Sciences; Meteorology & Atmospheric Sciences SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 912CT UT WOS:000301773000008 ER PT S AU Perchonok, MH Cooper, MR Catauro, PM AF Perchonok, Michele H. Cooper, Maya R. Catauro, Patricia M. BE Doyle, MP Klaenhammer, TR TI Mission to Mars: Food Production and Processing for the Final Frontier SO ANNUAL REVIEW OF FOOD SCIENCE AND TECHNOLOGY, VOL 3 SE Annual Review of Food Science and Technology LA English DT Review; Book Chapter DE space food; bioregenerative food system; food production; NASA; space exploration ID SPACE MISSIONS; CANNED FRUITS; LIFE-SUPPORT; VITAMIN-C; VEGETABLES; QUALITY; SYSTEMS; CAROTENOIDS; ENVIRONMENT; NUTRITION AB The food systems of the National Aeronautics and Space Administration (NASA) have evolved tremendously since the early manned spaceflights of the 1960s. To date, NASA's mission focus has been limited to exploration of low Earth orbit (LEO), and the agency's prepackaged food systems have been adequate to enable success of their parent programs. With NASA's mission focus increasing to achieve manned space exploration of the Martian surface, the agency is considering a significant departure from the prepackaged food systems of current and past space programs. NASA's Advanced Food Technology (AFT) project is presently investigating the introduction of a bioregenerative food system to support long duration habitat missions to the Martian surface. A bioregenerative food system is expected to impart less of a burden on critical mission resources, such as mass and volume, than a prepackaged, shelf-stable system. This review provides an introduction to past and present spaceflight food systems, and provides a broad examination of the research conducted to date to enable crop production and food processing on the Martian surface. C1 [Perchonok, Michele H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Cooper, Maya R.; Catauro, Patricia M.] Lockheed Martin Informat Syst & Global Serv, Houston, TX 77058 USA. RP Perchonok, MH (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM michele.h.perchonok@nasa.gov; maya.cooper@nasa.gov; patricia.catauro@nasa.gov NR 69 TC 3 Z9 3 U1 8 U2 48 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA SN 1941-1413 BN 978-0-8243-4903-5 J9 ANNU REV FOOD SCI T JI Annu. Rev. Food Sci. Technol. PY 2012 VL 3 BP 311 EP 330 DI 10.1146/annurev-food-022811-101222 PG 20 WC Food Science & Technology SC Food Science & Technology GA BZJ97 UT WOS:000301795100016 PM 22136130 ER PT J AU Gyawali, M Arnott, WP Zaveri, RA Song, C Moosmuller, H Liu, L Mishchenko, MI Chen, LWA Green, MC Watson, JG Chow, JC AF Gyawali, M. Arnott, W. P. Zaveri, R. A. Song, C. Moosmueller, H. Liu, L. Mishchenko, M. I. Chen, L. -W. A. Green, M. C. Watson, J. G. Chow, J. C. TI Photoacoustic optical properties at UV, VIS, and near IR wavelengths for laboratory generated and winter time ambient urban aerosols SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID LIGHT-ABSORPTION MEASUREMENTS; SINGLE SCATTERING ALBEDO; BLACK CARBON; ATMOSPHERIC AEROSOLS; MEXICO-CITY; SPECTRAL ABSORPTION; ORGANIC-CARBON; BROWN CARBON; ANGSTROM EXPONENT; SIZE DISTRIBUTION AB We present the laboratory and ambient photoacoustic (PA) measurement of aerosol light absorption coefficients at ultraviolet wavelength (i.e., 355 nm) and compare with measurements at 405, 532, 870, and 1047 nm. Simultaneous measurements of aerosol light scattering coefficients were achieved by the integrating reciprocal nephelometer within the PA's acoustic resonator. Absorption and scattering measurements were carried out for various laboratory-generated aerosols, including salt, incense, and kerosene soot to evaluate the instrument calibration and gain insight on the spectral dependence of aerosol light absorption and scattering. Ambient measurements were obtained in Reno, Nevada, between 18 December 2009 and 18 January 2010. The measurement period included days with and without strong ground level temperature inversions, corresponding to highly polluted (freshly emitted aerosols) and relatively clean (aged aerosols) conditions. Particulate matter (PM) concentrations were measured and analyzed with other tracers of traffic emissions. The temperature inversion episodes caused very high concentration of PM2.5 and PM10 (particulate matter with aerodynamic diameters less than 2.5 mu m and 10 mu m, respectively) and gaseous pollutants: carbon monoxide (CO), nitric oxide (NO), and nitrogen dioxide (NO2). The diurnal change of absorption and scattering coefficients during the polluted (inversion) days increased approximately by a factor of two for all wavelengths compared to the clean days. The spectral variation in aerosol absorption coefficients indicated a significant amount of absorbing aerosol from traffic emissions and residential wood burning. The analysis of single scattering albedo (SSA), Angstrom exponent of absorption (AEA), and Angstrom exponent of scattering (AES) for clean and polluted days provides evidences that the aerosol aging and coating process is suppressed by strong temperature inversion under cloudy conditions. In general, measured UV absorption coefficients were found to be much larger for biomass burning aerosol than for typical ambient aerosols. C1 [Gyawali, M.; Arnott, W. P.] Univ Nevada, Dept Phys, Reno, NV 89557 USA. [Zaveri, R. A.; Song, C.] Pacific NW Natl Lab, Atmospher Sci & Global Change Div, Richland, WA 99352 USA. [Moosmueller, H.; Chen, L. -W. A.; Green, M. C.; Watson, J. G.; Chow, J. C.] Desert Res Inst, Reno, NV 89512 USA. [Liu, L.; Mishchenko, M. I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Gyawali, M (reprint author), Univ Nevada, Dept Phys, 1664 N Virginia St, Reno, NV 89557 USA. EM madhug@unr.edu RI Mishchenko, Michael/D-4426-2012; Chen, Lung-Wen/J-5792-2015; OI Chen, Lung-Wen/0000-0002-2311-7506; Zaveri, Rahul/0000-0001-9874-8807; Moosmuller, Hans/0000-0002-1021-8877 FU NASA EPSCoR [NNX10AR89A]; NASA ROSES [NNX11AB79G]; US Department of Energy's Atmospheric System Research (ASR) at Pacific Northwest National Laboratory [DE-AC06-76RLO 1830] FX This material is based upon work supported by NASA EPSCoR under Cooperative Agreement No. NNX10AR89A, by NASA ROSES under Grant No. NNX11AB79G, and by the US Department of Energy's Atmospheric System Research (ASR) Program under Contract DE-AC06-76RLO 1830 at Pacific Northwest National Laboratory. NR 79 TC 27 Z9 27 U1 2 U2 66 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 5 BP 2587 EP 2601 DI 10.5194/acp-12-2587-2012 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 909FH UT WOS:000301547500022 ER PT J AU Mitchard, ETA Saatchi, SS White, LJT Abernethy, KA Jeffery, KJ Lewis, SL Collins, M Lefsky, MA Leal, ME Woodhouse, IH Meir, P AF Mitchard, E. T. A. Saatchi, S. S. White, L. J. T. Abernethy, K. A. Jeffery, K. J. Lewis, S. L. Collins, M. Lefsky, M. A. Leal, M. E. Woodhouse, I. H. Meir, P. TI Mapping tropical forest biomass with radar and spaceborne LiDAR in Lope National Park, Gabon: overcoming problems of high biomass and persistent cloud SO BIOGEOSCIENCES LA English DT Article ID CARBON STORAGE; AMAZON; DEFORESTATION; COMMONS; AFRICA; STOCKS; REDD AB Spatially-explicit maps of aboveground biomass are essential for calculating the losses and gains in forest carbon at a regional to national level. The production of such maps across wide areas will become increasingly necessary as international efforts to protect primary forests, such as the REDD+ (Reducing Emissions from Deforestation and forest Degradation) mechanism, come into effect, alongside their use for management and research more generally. However, mapping biomass over high-biomass tropical forest is challenging as (1) direct regressions with optical and radar data saturate, (2) much of the tropics is persistently cloud-covered, reducing the availability of optical data, (3) many regions include steep topography, making the use of radar data complex, (5) while LiDAR data does not suffer from saturation, expensive aircraft-derived data are necessary for complete coverage. We present a solution to the problems, using a combination of terrain-corrected L-band radar data (ALOS PALSAR), spaceborne LiDAR data (ICESat GLAS) and ground-based data. We map Gabon's Lope National Park (5000 km(2)) because it includes a range of vegetation types from savanna to closed-canopy tropical forest, is topographically complex, has no recent contiguous cloud-free high-resolution optical data, and the dense forest is above the saturation point for radar. Our 100 m resolution biomass map is derived from fusing spaceborne LiDAR (7142 ICESat GLAS footprints), 96 ground-based plots (average size 0.8 ha) and an unsupervised classification of terrain-corrected ALOS PALSAR radar data, from which we derive the aboveground biomass stocks of the park to be 78 Tg C (173MgC ha(-1)). This value is consistent with our field data average of 181 Mg Cha(-1), from the field plots measured in 2009 covering a total of 78 ha, and which are independent as they were not used for the GLAS-biomass estimation. We estimate an uncertainty of +/-25% on our carbon stock value for the park. This error term includes uncertainties resulting from the use of a generic tropical allometric equation, the use of GLAS data to estimate Lorey's height, and the necessity of separating the landscape into distinct classes. As there is currently no spaceborne LiDAR satellite in operation (GLAS data is available for 2003-2009 only), this methodology is not suitable for change-detection. This research underlines the need for new satellite LiDAR data to provide the potential for biomass-change estimates, although this need will not be met before 2015. C1 [Mitchard, E. T. A.; Woodhouse, I. H.; Meir, P.] Univ Edinburgh, Sch GeoSci, Edinburgh EH8 9XP, Midlothian, Scotland. [Saatchi, S. S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [White, L. J. T.; Jeffery, K. J.] Agence Natl Parcs Nationaux, Libreville, Gabon. [White, L. J. T.; Abernethy, K. A.; Jeffery, K. J.] Univ Stirling, Sch Nat Sci, Stirling FK9 4LA, Scotland. [White, L. J. T.; Abernethy, K. A.; Jeffery, K. J.] CENAREST, Inst Rech Ecol Tropicale, Libreville, Gabon. [Lewis, S. L.] Univ Leeds, Sch Geog, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. [Collins, M.] London Sch Econ, Grantham Res Inst Climate Change & Environm, London WC2A 2AE, England. [Lefsky, M. A.] Colorado State Univ, Nat Resource Ecol Lab, Ft Collins, CO 80523 USA. [Leal, M. E.] Missouri Bot Garden, St Louis, MO 63166 USA. [Lewis, S. L.] UCL, Dept Geog, London, England. RP Mitchard, ETA (reprint author), Univ Edinburgh, Sch GeoSci, Edinburgh EH8 9XP, Midlothian, Scotland. EM edward.mitchard@ed.ac.uk RI Woodhouse, Iain/B-1790-2009; Lewis, Simon/I-9025-2012; Meir, Patrick/J-8344-2012; Jeffery, Kathryn/G-2530-2013; OI Jeffery, Kathryn/0000-0002-2632-0008; Mitchard, Edward/0000-0002-5690-4055; Abernethy, Katharine/0000-0002-0393-9342; Lewis, Simon/0000-0002-8066-6851 FU Gatsby Plants PhD Studentship fo Edward Mitchard; Gordon and Betty Moore Foundation; Packard Foundation; Royal Society FX This work is dedicated to the memory of Fabiane Lima de Oliveira, who passed away in Gabon in 2009 after falling ill whilst on fieldwork for this project. Her deep knowledge and love of the forest was highly respected by all who she met. She is greatly missed by family, friends and the scientific community. ESA provided the ALOS PALSAR radar data at cost price through a Category 1 Application. These data were ultimately collected and processed by JAXA. ICESat GLAS data were provided by NASA. SRTM data were provided by NASA and processed by CGIAR-CSI (http://srtm.csi.cgiar.org). Funding for this work was provided by a Gatsby Plants PhD Studentship fo Edward Mitchard, with the fieldwork being funded by a grant from the Gordon and Betty Moore Foundation and the Packard Foundation. Simon Lewis is supported by a Royal Society University Research Fellowship. The Gabonese Agence Nationale des Parcs Nationaux, the Station d'Etudes des Gorilles et Chimpanzes, and Etienne Massard provided essential logistical support to the fieldwork effort. NR 43 TC 62 Z9 63 U1 8 U2 86 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1726-4170 J9 BIOGEOSCIENCES JI Biogeosciences PY 2012 VL 9 IS 1 BP 179 EP 191 DI 10.5194/bg-9-179-2012 PG 13 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 891PL UT WOS:000300229000013 ER PT J AU Halekas, JS Poppe, A Delory, GT Farrell, WM Horanyi, M AF Halekas, J. S. Poppe, A. Delory, G. T. Farrell, W. M. Horanyi, M. TI Solar wind electron interaction with the dayside lunar surface and crustal magnetic fields: Evidence for precursor effects SO EARTH PLANETS AND SPACE LA English DT Article DE Moon; solar wind; precursor effects; wave-particle interactions ID DOUBLE-LAYER; CONICS; PLASMA; ACCELERATION; PROSPECTOR; DYNAMICS; SPACE; DUST AB Electron distributions measured by Lunar Prospector above the dayside lunar surface in the solar wind often have an energy dependent loss cone, inconsistent with adiabatic magnetic reflection. Energy dependent reflection suggests the presence of downward parallel electric fields below the spacecraft, possibly indicating the presence of a standing electrostatic structure. Many electron distributions contain apparent low energy (< 100 eV) upward-going conics (58% of the time) and beams (12% of the time), primarily in regions with non-zero crustal magnetic fields, implying the presence of parallel electric fields and/or wave-particle interactions below the spacecraft. Some, but not all, of the observed energy dependence comes from the energy gained during reflection from a moving obstacle; correctly characterizing electron reflection requires the use of the proper reference frame. Non-adiabatic reflection may also play a role, but cannot fully explain observations. In cases with upward-going beams, we observe partial isotropization of incoming solar wind electrons, possibly indicating streaming and/or whistler instabilities. The Moon may therefore influence solar wind plasma well upstream from its surface. Magnetic anomaly interactions and/or non-monotonic near surface potentials provide the most likely candidates to produce the observed precursor effects, which may help ensure quasi-neutrality upstream from the Moon. C1 [Halekas, J. S.; Poppe, A.; Delory, G. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Halekas, J. S.; Poppe, A.; Delory, G. T.; Farrell, W. M.; Horanyi, M.] NASA, Ames Res Ctr, Lunar Sci Inst, Moffett Field, CA 94035 USA. [Horanyi, M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Horanyi, M.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Halekas, JS (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM jazzman@ssl.berkeley.edu RI Farrell, William/I-4865-2013; OI Horanyi, Mihaly/0000-0002-5920-9226; Halekas, Jasper/0000-0001-5258-6128 NR 35 TC 16 Z9 16 U1 0 U2 11 PU TERRA SCIENTIFIC PUBL CO PI TOKYO PA 2003 SANSEI JIYUGAOKA HAIMU, 5-27-19 OKUSAWA, SETAGAYA-KU, TOKYO, 158-0083, JAPAN SN 1343-8832 J9 EARTH PLANETS SPACE JI Earth Planets Space PY 2012 VL 64 IS 2 BP 73 EP 82 DI 10.5047/eps.2011.03.008 PG 10 WC Geosciences, Multidisciplinary SC Geology GA 913BT UT WOS:000301847100004 ER PT J AU Prevot, T Homola, JR Martin, LH Mercer, JS Cabrall, CD AF Prevot, Thomas Homola, Jeffrey R. Martin, Lynne H. Mercer, Joey S. Cabrall, Christopher D. TI Toward Automated Air Traffic Control-Investigating a Fundamental Paradigm Shift in Human/Systems Interaction SO INTERNATIONAL JOURNAL OF HUMAN-COMPUTER INTERACTION LA English DT Article AB Predicted air traffic increases over the next 25 years may create a significant capacity problem that the United States' National Airspace System will be unable to accommodate. The concept of introducing automated separation assurance was proposed to help solve this problem. However, the introduction of such a concept involves a fundamental paradigm shift in which automation is allowed to perform safety-critical tasks that today are strictly the air traffic controllers' domain. Moving toward automated air traffic control, therefore, requires a careful and thorough investigation. As part of an ongoing series, three human-in-the-loop simulation studies were conducted at the NASA Ames Research Center with the overarching goal of determining whether the automated separation assurance concept can be integrated into air traffic control operations in an acceptable and safe manner. These studies investigated a range of issues including the proper levels of automation for given capacity targets, off-nominal operations from both air and ground perspectives, and sustained near-full mission operations with many tasks allocated to the automation in the presence of convective weather and scheduling constraints. Overall, it was found that the concept has the potential to solve the envisioned airspace capacity problem. The automation was largely effective and robust, and the function allocation of tasks between controllers and automation was generally acceptable. However, feedback and results also showed that further technological development is necessary to improve trajectory prediction and conflict detection accuracy. The need for further procedural development to govern controller/automation and air/ground interactions was also highlighted. These and other considerations are addressed as the automated separation assurance concept is further tested and pursued through subsequent studies. C1 [Prevot, Thomas; Homola, Jeffrey R.; Martin, Lynne H.; Mercer, Joey S.; Cabrall, Christopher D.] San Jose State Univ, Ames Res Ctr, NASA, Moffett Field, CA 94035 USA. RP Prevot, T (reprint author), San Jose State Univ, Ames Res Ctr, NASA, Moffett Field, CA 94035 USA. EM thomas.prevot@nasa.gov RI Cabrall, Christopher/M-7455-2015 OI Cabrall, Christopher/0000-0003-1357-0160 NR 34 TC 20 Z9 20 U1 0 U2 10 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1044-7318 J9 INT J HUM-COMPUT INT JI Int. J. Hum.-Comput. Interact. PY 2012 VL 28 IS 2 SI SI BP 77 EP 98 DI 10.1080/10447318.2012.634756 PG 22 WC Computer Science, Cybernetics; Ergonomics SC Computer Science; Engineering GA 912ZF UT WOS:000301840400002 ER PT J AU Vu, KPL Strybel, TZ Battiste, V Lachter, J Dao, AQV Brandt, S Ligda, S Johnson, A AF Vu, Kim-Phuong L. Strybel, Thomas Z. Battiste, Vernol Lachter, Joel Dao, Arik-Quang V. Brandt, Summer Ligda, Sarah Johnson, Andwalter TI Pilot Performance in Trajectory-Based Operations Under Concepts of Operation That Vary Separation Responsibility Across Pilots, Air Traffic Controllers, and Automation SO INTERNATIONAL JOURNAL OF HUMAN-COMPUTER INTERACTION LA English DT Article ID SITUATION AWARENESS; SYSTEMS AB The Next Generation Air Transportation System (NextGen) will revolutionize the air traffic management system in the United States. NextGen will involve human operators interacting with new technologies in a complex system, making human factors and human-computer interaction considerations a major concern. The present study reports data from a human-in-the-loop simulation that evaluated pilot performance, workload, and situation awareness under one of three plausible NextGen concepts of operation. The concepts of operation differed with respect to the allocation of separation responsibility across human pilots and air traffic controllers (ATCs), and automation. Pilots were asked to employ trajectory-based operations to perform weather avoidance maneuvers, an interval management task, and a continuous descent approach. Depending on the concept being tested, they were also given the responsibility of separation assurance (Concept 1) or received conflict resolutions from an ATC (Concept 2) or automated system (Concept 3). Overall, pilot performance on the various flight tasks was worse in Concept 3 than in Concepts 1 and 2. Although pilot workload did not differ across the three concepts, pilot situation awareness was highest in Concept 1, in which the pilots were given the most responsibilities. These findings suggest that keeping pilots engaged in separation assurance tasks may be preferable to having them rely on automation alone. C1 [Vu, Kim-Phuong L.] Calif State Univ Long Beach, Dept Psychol, Long Beach, CA 90840 USA. [Battiste, Vernol; Lachter, Joel; Dao, Arik-Quang V.; Brandt, Summer; Ligda, Sarah] San Jose State Univ Fdn, San Jose, CA USA. [Johnson, Andwalter] NASA, Ames Res Ctr, Flight Deck Display Res Lab, Moffett Field, CA 94035 USA. RP Vu, KPL (reprint author), Calif State Univ Long Beach, Dept Psychol, 1250 N Bellflower Blvd, Long Beach, CA 90840 USA. EM kvu8@csulb.edu FU NASA [NNA06CN30A, NNX09AU66A]; Metrics for Situation Awareness, Workload; Group 5 University Research Center: Center for Human Factors in Advanced Aeronautics Technologies FX The simulation described in the article was supported in part by NASA cooperative agreement NNA06CN30A, Metrics for Situation Awareness, Workload, and Performance in Separation Assurance Systems. Preparation of this article was supported by NASA cooperative agreement NNX09AU66A, Group 5 University Research Center: Center for Human Factors in Advanced Aeronautics Technologies. We thank members of the FDDRL, CHAAT, SERL, and HISEL laboratories at NASA Ames, California State University Long Beach, California State University Northridge, and Purdue University, respectively, for their contributions to the simulation. NR 38 TC 11 Z9 11 U1 0 U2 5 PU LAWRENCE ERLBAUM ASSOC INC-TAYLOR & FRANCIS PI PHILADELPHIA PA 325 CHESTNUT STREET, STE 800, PHILADELPHIA, PA 19106 USA SN 1044-7318 J9 INT J HUM-COMPUT INT JI Int. J. Hum.-Comput. Interact. PY 2012 VL 28 IS 2 SI SI BP 107 EP 118 DI 10.1080/10447318.2012.634761 PG 12 WC Computer Science, Cybernetics; Ergonomics SC Computer Science; Engineering GA 912ZF UT WOS:000301840400004 ER PT J AU Prinzel, LJ Kramer, LJ Shelton, KJ Arthur, JJ Bailey, RE Norman, RM Ellis, KL Barmore, BE AF Prinzel, Lawrence J., III Kramer, Lynda J. Shelton, Kevin J. Arthur, Jarvis J. Bailey, Randall E. Norman, Robert M. Ellis, Kyle L. Barmore, Bryan E. TI Flight Deck Interval Management Delegated Separation Using Equivalent Visual Operations SO INTERNATIONAL JOURNAL OF HUMAN-COMPUTER INTERACTION LA English DT Article AB The Next Generation Air Transportation System (NextGen) concept termed, "Equivalent Visual Operations" (EVO) represents a fundamentally different operational approach to current issues confronting commercial aviation. Synthetic and enhanced flight vision system (S/EVS) technologies are critical enabling technologies to EVO. Research was conducted that evaluated concepts for flight-deck-based interval management operations, integrated with S/EVS. One of the concepts tested involves delegated flight-deck-based separation, in which the flight crews were paired with another aircraft and responsible for spacing and maintaining separation from the paired aircraft termed "equivalent visual separation." The operation required the flight crews to acquire and maintain an "equivalent visual contact" as well as to conduct manual landings in low-visibility conditions utilizing S/EVS and other flight deck technologies. The article describes results that evaluated the concept of EVO delegated separation, including an off-nominal scenario in which the lead aircraft was not able to conform to the assigned spacing resulting in a loss of separation. The results demonstrated that delegated separation improved flight deck situation awareness without an increase in mental workload. Implications for NextGen and future research directions are described. C1 [Prinzel, Lawrence J., III; Kramer, Lynda J.; Shelton, Kevin J.; Arthur, Jarvis J.; Bailey, Randall E.; Norman, Robert M.; Ellis, Kyle L.; Barmore, Bryan E.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Norman, Robert M.] Boeing Res & Technol, Seattle, WA USA. RP Prinzel, LJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM lawrence.j.prinzel@nasa.gov FU NASA Langley Research Center FX The article reflects the views and opinions of the authors, and any statements made herein do not necessarily reflect those of NASA, other federal agencies, or Boeing. We acknowledge the significant support provided by many Federal Systems contractors, at NASA Langley Research Center, most notably Jerry Karwac, Wei Anderson, Victoria Chung, Sean Kenney, Miguel Alvarez, Tod Lewis, Danette Allen, Lisa Rippy, Brent Weathered, and Terry Abbott. NR 34 TC 1 Z9 1 U1 1 U2 2 PU LAWRENCE ERLBAUM ASSOC INC-TAYLOR & FRANCIS PI PHILADELPHIA PA 325 CHESTNUT STREET, STE 800, PHILADELPHIA, PA 19106 USA SN 1044-7318 J9 INT J HUM-COMPUT INT JI Int. J. Hum.-Comput. Interact. PY 2012 VL 28 IS 2 SI SI BP 119 EP 130 DI 10.1080/10447318.2012.634764 PG 12 WC Computer Science, Cybernetics; Ergonomics SC Computer Science; Engineering GA 912ZF UT WOS:000301840400005 ER PT J AU Huang, HG Liu, Q Liu, QH Qin, WH AF Huang, Huaguo Liu, Qiang Liu, Qinhuo Qin, Wenhan TI Validating theoretical simulations of thermal emission hot spot effects on maize canopies SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID SURFACE-TEMPERATURE; COMPONENT TEMPERATURES; BRIGHTNESS TEMPERATURE; INFRARED OBSERVATIONS; ANGULAR VARIATIONS; VIEWING ANGLE; CROP CANOPIES; DIRECTIONALITY; MODEL; SOIL AB This is a development of some of our previous work on the analysis of thermal emission hot spot effects. In that work, which was a simulation study, a curve-fitting model was proposed to derive the hot spot amplitude and half width. Based on the curve-fitting model, a new algorithm that predicts the component temperature differences from the hot spot amplitude is presented. In this study, the objectives are to evaluate the accuracy of the curve-fitting model and the new prediction algorithm using both airborne measurements based on the wide-angle infrared dual-mode line/area array scanner (WiDAS) system and ground measurements. Based on a prior knowledge of crop structure parameters (e.g. the leaf area index (LAI), leaf angle distribution (LAD) and leaf dimensions), validation results indicate that the curve-fitting model and the prediction algorithm can accurately retrieve the hot spot amplitude and half width (R-2 > 0.90 and root mean square error (RMSE) < 0.15 K), and predict leaf and soil temperature differences from directional signals of both airborne and ground data (bias < 1 K). The error of prior knowledge can significantly affect the prediction accuracy of leaf temperature difference. Also discussed are the limitations of the model and future research and application. C1 [Huang, Huaguo] Beijing Forestry Univ, Coll Forestry, Minist Educ, Key Lab Silviculture & Conservat, Beijing 100083, Peoples R China. [Liu, Qiang; Liu, Qinhuo; Qin, Wenhan] Inst Remote Sensing Applicat Chinese Acad Sci & B, State Key Lab Remote Sensing Sci, Beijing 100101, Peoples R China. [Qin, Wenhan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Huang, HG (reprint author), Beijing Forestry Univ, Coll Forestry, Minist Educ, Key Lab Silviculture & Conservat, Beijing 100083, Peoples R China. EM huaguo.huang@gmail.com RI rslab, water/O-7043-2015 FU Chinese State Key Basic Research Project [2007CB714402]; Chinese Natural Science Foundation Project [40801135, 40730525]; Beijing Forestry University [BLYX200917]; Chinese State Key Basic Research Project 'Synthetic Retrieval of Territorial Ecological Variables Using both Active and Passive Remote Sensing Approaches' [2007CB714400]; 'WATER: Watershed Airborne Telemetry Experiment Research' under CAS [KZCX2-XB2-09] FX This work is supported by the Chinese State Key Basic Research Project (2007CB714402), the Chinese Natural Science Foundation Project (40801135; 40730525) and the Innovation Project of Beijing Forestry University (BLYX200917). We appreciate useful suggestions received from Klaus V. Gadow and the anonymous reviewers. The experiment was jointly supported by the Chinese State Key Basic Research Project 'Synthetic Retrieval of Territorial Ecological Variables Using both Active and Passive Remote Sensing Approaches' (grant number 2007CB714400), and by the 'WATER: Watershed Airborne Telemetry Experiment Research' (grant number KZCX2-XB2-09) under the auspices of the CAS Action Plan for West Development Programme. NR 41 TC 2 Z9 3 U1 4 U2 11 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PY 2012 VL 33 IS 3 SI SI BP 746 EP 761 DI 10.1080/01431161.2011.577827 PG 16 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 907BH UT WOS:000301392300006 ER PT J AU Mayr, HG Schatten, KH AF Mayr, Hans G. Schatten, Kenneth H. TI Nonlinear oscillators in space physics SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Wave-driven quasi-biennial oscillation; Intra-seasonal bimonthly oscillation; Semidiurnal pseudo-tide; 22-year solar dynamo ID DOPPLER-SPREAD PARAMETERIZATION; QUASI-BIENNIAL OSCILLATION; WAVE MOMENTUM DEPOSITION; FLUX-TRANSPORT DYNAMO; LARGE-SCALE DYNAMICS; GRAVITY-WAVES; MIDDLE ATMOSPHERE; LOWER THERMOSPHERE; INTRASEASONAL OSCILLATIONS; EQUATORIAL OSCILLATIONS AB We discuss dynamical systems that produce an oscillation without an external time dependent source. Numerical results are presented for nonlinear oscillators in the Earth's atmosphere, foremost the quasi-biennial oscillation (QBO). These fluid dynamical oscillators, like the solar dynamo, have in common that one of the variables in a governing equation is strongly nonlinear and that the nonlinearity, to first order, has a particular form, of 3rd or odd power. It is shown that this form of nonlinearity can produce the fundamental frequency of the internal oscillation, which has a period that is favored by the dynamical condition of the fluid. The fundamental frequency maintains the oscillation, with no energy input to the system at that particular frequency. Nonlinearities of 2nd or even power could not maintain the oscillation. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Mayr, Hans G.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Schatten, Kenneth H.] Ai Solut Inc, Lanham, MD 20706 USA. RP Mayr, HG (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-3,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM hans.g.mayr@nasa.gov NR 38 TC 1 Z9 1 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD JAN PY 2012 VL 74 BP 44 EP 50 DI 10.1016/j.jastp.2011.09.008 PG 7 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 910BK UT WOS:000301612000004 ER PT J AU Ma, Q Tipping, RH Lavrentieva, NN AF Ma, Q. Tipping, R. H. Lavrentieva, N. N. TI Theoretical studies of N-2-broadened half-widths of H2O lines involving high j states SO MOLECULAR PHYSICS LA English DT Article DE energy levels and wave functions of H2O states; Robert-Bonamy theory; theoretically calculated half-widths and shifts; rules governing spectroscopic parameters of H2O lines; HITRAN ID ROBERT-BONAMY FORMALISM; WATER-VAPOR; PARAMETERS; HITRAN; SHIFTS; LIST AB Based on the properties of the energy levels and wave functions of H2O states, one can categorize H2O lines into individually defined groups such that within the same group, the energy levels and the wave functions associated with two paired lines have an identity property while those associated with different pairs have a similarity property. Meanwhile, by thoroughly analyzing processes used to calculate N-2-broadened half-widths, it was found that the 'Fourier series' of W-L1K1K1'((a))(t; j(f) tau f) and W-L1K1K1'((a)) (t; j(i) tau(i)), and a factor P-222(j(f) tau(f) j(i) tau(i)) are the key items in the Robert-Bonamy formalism to distinguish contributions to ReS2(r(c)) among different transitions of j(f) tau(f) <- j(i) tau(i). However, these items are completely determined by the energy levels and the wave functions associated with their initial and final states and they must bear the latter's features as well. Thus, it becomes obvious that for two paired lines in the same group, their calculated half-widths must be almost identical and the values associated with different pairs must vary smoothly as their ji values vary. Thus, the pair identity and the smooth variation rules are established within individual groups of lines. One can use these rules to screen half-width data listed in HITRAN and to improve the data accuracies. C1 [Ma, Q.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Ma, Q.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. [Tipping, R. H.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Lavrentieva, N. N.] VE Zuev Inst Atmospher Opt SB RAS, Tomsk 634021, Russia. RP Ma, Q (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM qma@giss.nasa.gov RI Lavrentieva, Nina/A-4010-2014 FU NASA [NNG06GB23G, NNX09AB62G, FCCS-547, NNH08ZDA001N-ACLAB]; US Department of Energy [DE-AI02-93ER61744]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX Two of the authors (Q. Ma and R.H. Tipping) acknowledge financial support from NASA under grants NNG06GB23G, NNX09AB62G, and FCCS-547. Q. Ma wishes to acknowledge financial support from the Biological and Environmental Research Program (BER), US Department of Energy, Interagency Agreement No. DE-AI02-93ER61744 and financial support from NASA under grant NNH08ZDA001N-ACLAB. 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 17 TC 5 Z9 5 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0026-8976 J9 MOL PHYS JI Mol. Phys. PY 2012 VL 110 IS 6 BP 307 EP 331 DI 10.1080/00268976.2011.646333 PG 25 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 912BM UT WOS:000301769500001 ER PT J AU Hollis, BR Borrelli, S AF Hollis, Brian R. Borrelli, Salvatore TI Aerothermodynamics of blunt body entry vehicles SO PROGRESS IN AEROSPACE SCIENCES LA English DT Review DE Blunt body entry vehicles; Turbulent flow on blunt bodies; Rarefied flow; Radiation transport ID CREW EXPLORATION VEHICLE; LUNAR-RETURN CONDITIONS; SHOCK-LAYER RADIATION; CAVITIES AB In this chapter, the aerothermodynamic phenomena of blunt body entry vehicles are discussed. Four topics will be considered that present challenges to current computational modeling techniques for blunt body environments: turbulent flow, non-equilibrium flow, rarefied flow, and radiation transport. Examples of comparisons between computational tools to ground and flight-test data will be presented in order to illustrate the challenges existing in the numerical modeling of each of these phenomena and to provide test cases for evaluation of computational fluid dynamics (CFD) code predictions. Published by Elsevier Ltd. C1 [Hollis, Brian R.] NASA, Langley Res Ctr, Hampton, VA 23666 USA. [Borrelli, Salvatore] CIRA Italian Aerosp Res Ctr, I-81083 Capua, CE, Italy. RP Hollis, BR (reprint author), NASA, Langley Res Ctr, Hampton, VA 23666 USA. EM brian.r.hollis@nasa.gov NR 42 TC 5 Z9 5 U1 0 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0376-0421 J9 PROG AEROSP SCI JI Prog. Aeosp. Sci. PD JAN-FEB PY 2012 VL 48-49 SI SI BP 42 EP 56 DI 10.1016/j.paerosci.2011.09.005 PG 15 WC Engineering, Aerospace SC Engineering GA 912RK UT WOS:000301817100005 ER PT J AU Walpot, LMG Wright, MJ Noeding, P Schrijer, F AF Walpot, Louis M. G. Wright, Michael J. Noeding, Peter Schrijer, Ferry TI Base flow investigation of the Apollo AS-202 Command Module SO PROGRESS IN AEROSPACE SCIENCES LA English DT Review DE Re-entry vehicles; Base flows; Thermal protection; Computational fluid dynamics AB A major contributor to the overall vehicle mass of re-entry vehicles is the afterbody thermal protection system. This is due to the large acreage (equal or bigger than that of the forebody) to be protected. The present predictive capabilities for base flows are comparatively lower than those for windward flowfields and offer therefore a substantial potential for improving the design of future re-entry vehicles. To that end, it is essential to address the accuracy of high fidelity CFD tools exercised in the US and EU, which motivates a thorough investigation of the present status of hypersonic flight afterbody heating. This paper addresses the predictive capabilities of afterbody flow fields of re-entry vehicles investigated in the frame of the NATO/RTO-RTG-043 task group. First, the verification of base flow topologies on the basis of available wind-tunnel results performed under controlled supersonic conditions (i.e. cold flows devoid of reactive effects) is performed. Such tests address the detailed characterization of the base flow with particular emphasis on separation/reattachment and their relation to Mach number effects. The tests have been performed on an Apollo-like re-entry capsule configuration. Second, the tools validated in the frame of the previous effort are exercised and appraised against flight-test data collected during the Apollo AS-202 re-entry. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Wright, Michael J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Noeding, Peter] EADS Astrium, Bremen, Germany. [Schrijer, Ferry] Delft Univ Technol, Delft, Netherlands. EM louis.walpot@aoes.com FU European Space Agency FX The authors would like to thank Rafael Molina of the European Space Agency for providing his support, Stan van Gemert, COO, for enabling and managing the computational infrastructure at ADES and the CEO, Paul Pearson, for the support to the AVT making this work possible. Also many thanks to Greg Byshenk and Alessio Terpin, for building an optimized cost-performance cluster environment and Marco van Duijn. NR 11 TC 2 Z9 2 U1 1 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0376-0421 J9 PROG AEROSP SCI JI Prog. Aeosp. Sci. PD JAN-FEB PY 2012 VL 48-49 SI SI BP 57 EP 74 DI 10.1016/j.paerosci.2011.06.006 PG 18 WC Engineering, Aerospace SC Engineering GA 912RK UT WOS:000301817100006 ER PT S AU Doney, SC Ruckelshaus, M Duffy, JE Barry, JP Chan, F English, CA Galindo, HM Grebmeier, JM Hollowed, AB Knowlton, N Polovina, J Rabalais, NN Sydeman, WJ Talley, LD AF Doney, Scott C. Ruckelshaus, Mary Duffy, J. Emmett Barry, James P. Chan, Francis English, Chad A. Galindo, Heather M. Grebmeier, Jacqueline M. Hollowed, Anne B. Knowlton, Nancy Polovina, Jeffrey Rabalais, Nancy N. Sydeman, William J. Talley, Lynne D. BE Carlson, CA Giovannoni, SJ TI Climate Change Impacts on Marine Ecosystems SO ANNUAL REVIEW OF MARINE SCIENCE, VOL 4 SE Annual Review of Marine Science LA English DT Review; Book Chapter DE trophic structure; hypoxia; diversity; food webs ID CALIFORNIA CURRENT SYSTEM; OCEAN ACIDIFICATION; NORTHEAST PACIFIC; BIOLOGICAL INVASIONS; SPECIES INTERACTIONS; ANTARCTIC PENINSULA; THERMAL TOLERANCE; CONTINENTAL-SHELF; CARBON-DIOXIDE; WARMER OCEAN AB In marine ecosystems, rising atmospheric CO2 and climate change are associated with concurrent shifts in temperature, circulation, stratification, nutrient input, oxygen content, and ocean acidification, with potentially wide-ranging biological effects. Population-level shifts are occurring because of physiological intolerance to new environments, altered dispersal patterns, and changes in species interactions. Together with local climate-driven invasion and extinction, these processes result in altered community structure and diversity, including possible emergence of novel ecosystems. Impacts are particularly striking for the poles and the tropics, because of the sensitivity of polar ecosystems to sea-ice retreat and poleward species migrations as well as the sensitivity of coral-algal symbiosis to minor increases in temperature. Midlatitude upwelling systems, like the California Current, exhibit strong linkages between climate and species distributions, phenology, and demography. Aggregated effects may modify energy and material flows as well as biogeochemical cycles, eventually impacting the overall ecosystem functioning and services upon which people and societies depend. C1 [Doney, Scott C.] Woods Hole Oceanog Inst, Marine Chem & Geochem Dept, Woods Hole, MA 02543 USA. [Ruckelshaus, Mary] Stanford Univ, Nat Capital Project, Stanford, CA 94305 USA. [Ruckelshaus, Mary] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA. [Duffy, J. Emmett] Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. [Barry, James P.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. [Chan, Francis] Oregon State Univ, Corvallis, OR 97331 USA. [English, Chad A.] Commun Partnership Sci & Sea, Silver Spring, MD 20910 USA. [Galindo, Heather M.] Commun Partnership Sci & Sea, Seattle, WA 98195 USA. [Grebmeier, Jacqueline M.] Univ Maryland, Chesapeake Biol Lab, Ctr Environm Sci, Solomons, MD 20688 USA. [Hollowed, Anne B.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Seattle, WA 98115 USA. [Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Polovina, Jeffrey] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. [Rabalais, Nancy N.] Louisiana Univ Marine Consortium, Chauvin, LA 70344 USA. [Sydeman, William J.] Farallon Inst, Petaluma, CA 94975 USA. [Talley, Lynne D.] Univ Calif San Diego, La Jolla, CA 92093 USA. RP Doney, SC (reprint author), Woods Hole Oceanog Inst, Marine Chem & Geochem Dept, Woods Hole, MA 02543 USA. EM sdoney@whoi.edu; mary.ruckelshaus@stanford.edu; jeduffy@vims.edu; barry@mbari.org; chanft@science.oregonstate.edu; cenglish@compassonline.org; hgalindo@compassonline.org; jgrebmei@umces.edu; anne.hollowed@noaa.gov; knowlton@si.edu; jeffrey.polovina@noaa.gov; nrabalais@lumcon.edu; wsydeman@comcast.net; ltalley@ucsd.edu RI Doney, Scott/F-9247-2010; Grebmeier, Jacqueline/L-9805-2013 OI Doney, Scott/0000-0002-3683-2437; Grebmeier, Jacqueline/0000-0001-7624-3568 NR 165 TC 541 Z9 549 U1 134 U2 957 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA SN 1941-1405 BN 978-0-8243-4504-4 J9 ANNU REV MAR SCI JI Annu. Rev. Mar. Sci. PY 2012 VL 4 BP 11 EP 37 DI 10.1146/annurev-marine-041911-111611 PG 27 WC Geochemistry & Geophysics; Marine & Freshwater Biology; Oceanography SC Geochemistry & Geophysics; Marine & Freshwater Biology; Oceanography GA BYW27 UT WOS:000300634900003 PM 22457967 ER PT J AU Appourchaux, T Benomar, O Gruberbauer, M Chaplin, WJ Garcia, RA Handberg, R Verner, GA Antia, HM Campante, TL Davies, GR Deheuvels, S Hekker, S Howe, R Salabert, D Bedding, TR White, TR Houdek, G Aguirre, VS Elsworth, YP Van Cleve, J Clarke, BD Hall, JR Kjeldsen, H AF Appourchaux, T. Benomar, O. Gruberbauer, M. Chaplin, W. J. Garcia, R. A. Handberg, R. Verner, G. A. Antia, H. M. Campante, T. L. Davies, G. R. Deheuvels, S. Hekker, S. Howe, R. Salabert, D. Bedding, T. R. White, T. R. Houdek, G. Aguirre, V. Silva Elsworth, Y. P. Van Cleve, J. Clarke, B. D. Hall, J. R. Kjeldsen, H. TI Oscillation mode linewidths of main-sequence and subgiant stars observed by Kepler SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; asteroseismology; stars: solar-type ID SOLAR-LIKE OSCILLATIONS; SUN-LIKE STAR; STELLAR OSCILLATIONS; ASTEROSEISMOLOGY; AMPLITUDES AB Context. Solar-like oscillations have been observed by Kepler and CoRoT in several solar-type stars. Aims. We study the variations in the stellar p-mode linewidth as a function of effective temperature. Methods. We study a time series of nine months of Kepler data. We analyse the power spectra of 42 cool main-sequence stars and subgiants using both maximum likelihood estimators and Bayesian estimators to recover individual mode characteristics such as frequencies, linewidths, and mode heights. Results. We report on the mode linewidth at both maximum power and maximum mode height for these 42 stars as a function of effective temperature. Conclusions. We show that the mode linewidth at either maximum mode height or maximum amplitude follows a scaling relation with effective temperature, which is a combination of a power law and a lower bound. The typical power-law index is about 13 for the linewidth derived from the maximum mode height, and about 16 for the linewidth derived from the maximum amplitude, while the lower bound is about 0.3 mu Hz and 0.7 mu Hz, respectively. We stress that this scaling relation is only valid for cool main-sequence stars and subgiants, and does not have any predictive power outside the temperature range of these stars. C1 [Appourchaux, T.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France. [Appourchaux, T.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Benomar, O.; Bedding, T. R.; White, T. R.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Gruberbauer, M.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Chaplin, W. J.; Hekker, S.; Howe, R.; Elsworth, Y. P.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Garcia, R. A.; Verner, G. A.; Davies, G. R.] CEA DSM CNRS Univ Paris Diderot, Lab AIM, IRFU SAp, Ctr Saclay, F-91191 Gif Sur Yvette, France. [Handberg, R.; Campante, T. L.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, Aarhus C 8, Denmark. [Antia, H. M.] Tata Inst Fundamental Res, Bombay 45, Maharashtra, India. [Campante, T. L.] Univ Porto, DFA Fac Ciencias, Ctr Astrofis, P-4150762 Oporto, Portugal. [Deheuvels, S.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Salabert, D.] Univ Nice Sophia Antipolis, CNRS UMR 6202, Observ Cote Azur, F-06304 Nice 4, France. [Houdek, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Aguirre, V. Silva] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Clarke, B. D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hall, J. R.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Appourchaux, T (reprint author), Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, Batiment 121, F-91405 Orsay, France. EM thierry.appourchaux@ias.u-psud.fr OI Antia, H. M./0000-0001-7549-9684; Davies, Guy/0000-0002-4290-7351; Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776; Handberg, Rasmus/0000-0001-8725-4502 FU NASA's Science Mission Directorate; National Science Foundation [NSF PHY05-51164]; UK Science and Technology Facilities Council (STFC); European Community [269194]; NSERC; Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO); Austrian Science Fund (FWF) [P21205-N16]; Centre National d'Etudes Spatiales (CNES) FX The authors wish to thank the entire Kepler team, without whom these results would not be possible. Funding for this Discovery mission is provided by NASA's Science Mission Directorate. We also thank all funding councils and agencies that have supported the activities of KASC Working Group 1, as well as the International Space Science Institute (ISSI). This research was supported in part by the National Science Foundation under Grant No. NSF PHY05-51164. W.J.C., G. A. V., and Y.E. acknowledge financial support from the UK Science and Technology Facilities Council (STFC). R. A. G. and G. R. D. has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 269194. M. G. received financial support from an NSERC Vanier scholarship. This work employed computational facilities provided by ACEnet, the regional high performance computing consortium for universities in Atlantic Canada. SH acknowledges funding from the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO). G. H. acknowledges support by the Austrian Science Fund (FWF) project P21205-N16. R. H. acknowledges computing support from the National Solar Observatory. D. S. acknowledges the financial support from the Centre National d'Etudes Spatiales (CNES). NR 37 TC 29 Z9 29 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2012 VL 537 AR A134 DI 10.1051/0004-6361/201118496 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894HD UT WOS:000300416800134 ER PT J AU Bethermin, M Dore, O Lagache, G AF Bethermin, M. Dore, O. Lagache, G. TI Where stars form and live at high redshift: clues from the infrared SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: star formation; galaxies: statistics; galaxies: halos; dark matter; infrared: galaxies ID STELLAR MASS FUNCTION; DARK-MATTER HALOES; DIGITAL SKY SURVEY; LESS-THAN 2; LUMINOSITY FUNCTION; FORMATION HISTORY; GALAXY FORMATION; GAS CLOUDS; EVOLUTION; SAMPLE AB The relation between dark matter halos and the loci of star formation at high redshift is a pressing question in contemporary cosmology. Matching the abundance of halos to the abundance of infrared (IR) galaxies, we explore the link between dark matter halo mass (M-h), stellar mass (M-*) and star-formation rate (SFR) up to a redshift of 2. Our findings are five-fold. First, we find a strong evolution of the relation between M-* and SFR as a function of redshift with an increase of sSFR = SFR/M-* by a factor similar to 30 between z = 0 and z = 2.3. Second, we observe a decrease of sSFR with stellar mass. These results reproduce observed trends at redshift z > 0.3. Third, we find that the star formation is most efficient in dark matter halos with M-h similar or equal to 5 x 10(11) M-circle dot, with hints of an increase of this mass with redshift. Fourth, we find that SFR/M-h increases by a factor similar to 15 between z = 0 and z = 2.3. Finally we find that the SFR density is dominated by halo masses close to similar to 7 x 10(11) M-circle dot at all redshift, with a rapid decrease at lower and higher halo masses. Despite its simplicity, our novel use of IR observations unveils some characteristic mass-scales governing star formation at high redshift. C1 [Bethermin, M.] Univ Paris Diderot, CNRS, Lab AIM Paris Saclay, CEA,DSM,Irfu, Saclay, France. [Bethermin, M.; Lagache, G.] Inst Astrophys Spatiale IAS, F-91405 Orsay, France. [Bethermin, M.; Lagache, G.] Univ Paris 11, Paris, France. [Bethermin, M.; Lagache, G.] CNRS, UMR8617, F-75700 Paris, France. [Dore, O.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Bethermin, M (reprint author), Univ Paris Diderot, CNRS, Lab AIM Paris Saclay, CEA,DSM,Irfu, Saclay, France. EM matthieu.bethermin@cea.fr OI Bethermin, Matthieu/0000-0002-3915-2015 FU ERC-StG [UPGAL 240039]; NASA FX We thank Andrew Wetzel, whose questions stimulated this work, Mark Sargent, Emanuele Daddi and Lingyu Wang for their insightful comments, Gil Holder for his special perspective. M.B. acknowledge financial support from ERC-StG grant UPGAL 240039. Part of this research was carried out at JPL/Caltech under a contract from NASA. NR 48 TC 23 Z9 23 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2012 VL 537 AR L5 DI 10.1051/0004-6361/201118607 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894HD UT WOS:000300416800162 ER PT J AU Creevey, OL Dogan, G Frasca, A Thygesen, AO Basu, S Bhattacharya, J Biazzo, K Brandao, IM Bruntt, H Mazumdar, A Niemczura, E Shrotriya, T Sousa, SG Stello, D Subramaniam, A Campante, TL Handberg, R Mathur, S Bedding, TR Garcia, RA Regulo, C Salabert, D Molenda-Zakowicz, J Quirion, PO White, TR Bonanno, A Chaplin, WJ Christensen-Dalsgaard, J Christiansen, JL Elsworth, Y Fanelli, MN Karoff, C Kinemuchi, K Kjeldsen, H Gai, N Monteiro, MJPFG Suarez, C AF Creevey, O. L. Dogan, G. Frasca, A. Thygesen, A. O. Basu, S. Bhattacharya, J. Biazzo, K. Brandao, I. M. Bruntt, H. Mazumdar, A. Niemczura, E. Shrotriya, T. Sousa, S. G. Stello, D. Subramaniam, A. Campante, T. L. Handberg, R. Mathur, S. Bedding, T. R. Garcia, R. A. Regulo, C. Salabert, D. Molenda-Zakowicz, J. Quirion, P. -O. White, T. R. Bonanno, A. Chaplin, W. J. Christensen-Dalsgaard, J. Christiansen, J. L. Elsworth, Y. Fanelli, M. N. Karoff, C. Kinemuchi, K. Kjeldsen, H. Gai, N. Monteiro, M. J. P. F. G. Suarez, C. TI Fundamental properties of five Kepler stars using global asteroseismic quantities and ground-based observations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: oscillations; stars: fundamental parameters; stars: atmospheres; asteroseismology; stars: solar-type; stars: general ID SOLAR-TYPE STARS; EQUATION-OF-STATE; ELODIE ECHELLE SPECTRA; PARAMETERS T-EFF; 1ST 4 MONTHS; RED GIANTS; OSCILLATION PARAMETERS; AUTOMATIC-DETERMINATION; ONLINE DETERMINATION; STELLAR PARAMETERS AB We present an asteroseismic study of the solar-like stars KIC 11395018, KIC 10273246, KIC 10920273, KIC 10339342, and KIC 11234888 using short-cadence time series of more than eight months from the Kepler satellite. For four of these stars, we derive atmospheric parameters from spectra acquired with the Nordic Optical Telescope. The global seismic quantities (average large frequency separation and frequency of maximum power), combined with the atmospheric parameters, yield the mean density and surface gravity with precisions of 2% and similar to 0.03 dex, respectively. We also determine the radius, mass, and age with precisions of 2-5%, 7-11%, and similar to 35%, respectively, using grid-based analyses. Coupling the stellar parameters with photometric data yields an asteroseismic distance with a precision better than 10%. A v sin i measurement provides a rotational period-inclination correlation, and using the rotational periods from the recent literature, we constrain the stellar inclination for three of the stars. An Li abundance analysis yields an independent estimate of the age, but this is inconsistent with the asteroseismically determined age for one of the stars. We assess the performance of five grid-based analysis methods and find them all to provide consistent values of the surface gravity to similar to 0.03 dex when both atmospheric and seismic constraints are at hand. The different grid-based analyses all yield fitted values of radius and mass to within 2.4 sigma, and taking the mean of these results reduces it to 1.5 sigma. The absence of a metallicity constraint when the average large frequency separation is measured with a precision of 1% biases the fitted radius and mass for the stars with non-solar metallicity (metal-rich KIC 11395018 and metal-poor KIC 10273246), while including a metallicity constraint reduces the uncertainties in both of these parameters by almost a factor of two. We found that including the average small frequency separation improves the determination of the age only for KIC 11395018 and KIC 11234888, and for the latter this improvement was due to the lack of strong atmospheric constraints. C1 [Creevey, O. L.; Salabert, D.] IAC Inst Astrofis Canarias, Tenerife 38200, Spain. [Creevey, O. L.; Salabert, D.] Univ La Laguna, E-38206 Tenerife, Spain. [Creevey, O. L.; Salabert, D.] Univ Nice, Observ Cote Azur, Lab Cassiopae, CNRS UMR 6202, F-06304 Nice 4, France. [Dogan, G.; Thygesen, A. O.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Dogan, G.] High Altitude Observ, NCAR, Boulder, CO 80307 USA. [Frasca, A.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Thygesen, A. O.] Nord Optic Telescope, Santa Cruz de La Palma 38700, CA, Spain. [Basu, S.; Gai, N.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Bhattacharya, J.] Indian Inst Technol, Dept Phys, Kanpur 208016, Uttar Pradesh, India. [Biazzo, K.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Brandao, I. M.; Sousa, S. G.; Campante, T. L.; Monteiro, M. J. P. F. G.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Campante, T. L.; Regulo, C.; Monteiro, M. J. P. F. G.] Univ Porto, Dept Fis & Astron, Fac Ciencias, P-4169007 Oporto, Portugal. [Mazumdar, A.] Homi Bhabha Ctr Sci Educ TIFR, Mumbai 400088, Maharashtra, India. [Niemczura, E.] Univ Wroclaw, Inst Astronomiczny, PL-51622 Wroclaw, Poland. [Shrotriya, T.] Indian Inst Sci Educ & Res Pune, Pune 411021, Maharashtra, India. [White, T. R.] Univ Sydney, Sydney Inst Astron SIfA, Sch Phys, Sydney, NSW, Australia. [Subramaniam, A.] Indian Inst Technol, Madras 600036, Tamil Nadu, India. [Garcia, R. A.] Univ Paris Diderot, CEA DSM CNRS, Lab AIM, F-91191 Gif Sur Yvette, France. [Quirion, P. -O.] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. [Elsworth, Y.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Christiansen, J. L.] NASA Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Fanelli, M. N.] NASA Ames Reseach Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Gai, N.] Dezhou Univ, Dept Phys, Dezhou 253023, Peoples R China. [Suarez, C.] Inst Astrofis Andalucia CSIC, Granada 3004, Spain. RP Creevey, OL (reprint author), IAC Inst Astrofis Canarias, C Via Lactea S-N, Tenerife 38200, Spain. EM ocreevey@oca.eu RI Sousa, Sergio/I-7466-2013; Brandao, Isa/M-5172-2013; Monteiro, Mario J.P.F.G./B-4715-2008; OI Karoff, Christoffer/0000-0003-2009-7965; Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776; Handberg, Rasmus/0000-0001-8725-4502; Mazumdar, Anwesh/0000-0003-2409-2942; Frasca, Antonio/0000-0002-0474-0896; Bedding, Timothy/0000-0001-5943-1460; Sousa, Sergio/0000-0001-9047-2965; Brandao, Isa/0000-0002-1153-0942; Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Biazzo, Katia/0000-0002-1892-2180; Amby, Thomas Mellergaard/0000-0002-8116-1097; Bonanno, Alfio/0000-0003-3175-9776; Suarez, Juan Carlos/0000-0003-3649-8384 FU Henri Poincare Fellowship; Australian Research Council; China State Scholarship Fund; Ministry of Science and Technology of the Peoples Republic of China [2007CB815406]; National Natural Science Foundation of China [10773003, 10933002]; UK Science and Technology Facilities Council (STFC); International Space Science Institute (ISSI); FCT/MCTES, Portugal; MNiSW [NN203 302635]; Danish Council for Independent Research; National Initiative on Undergraduate Science (NIUS); Fundacao para a Ciencia e Tecnologia (Portugal) [SFRH/BPD/47611/2008]; Polish Ministry [N N203 405139]; Spanish Ministry of Science and Innovation (MICINN) [AYA 2010-20982-C02-02]; [SFRH/BD/41213/2007] FX All of the authors acknowledge the Kepler team for their years of work to provide excellent data. Funding for this Discovery mission is provided by NASA's Science Mission Directorate. This article is based on observations made with the Nordic Optical Telescope operated on the island of La Palma in the Spanish Observatorio del Roque de los Muchachos. We thank Othman Benomar and Frederic Thevenin for useful discussions, and we also thank the referee for very constructive comments which has greatly improved the manuscript. Part of this research was carried out while O.L.C. was a Henri Poincare Fellow at the Observatoire de la Cote d'Azur. The Henri Poincare Fellowship is funded the Conseil General des Alpes-Maritimes and the Observatoire de la Cote d'Azur. D. St acknowledges support from the Australian Research Council. N.G. acknowledges the China State Scholarship Fund that allowed her to spend a year at Yale. She also acknowledges grant 2007CB815406 of the Ministry of Science and Technology of the Peoples Republic of China and grants 10773003 and 10933002 from the National Natural Science Foundation of China. W.J.C. and Y.E. acknowledge the financial support of the UK Science and Technology Facilities Council (STFC), and the International Space Science Institute (ISSI). I.M.B. is supported by the grant SFRH/BD/41213/2007 funded by FCT/MCTES, Portugal. E.N. acknowledges financial support of the NN203 302635 grant from the MNiSW. G.D., H.B., and C.K. acknowledge financial support from The Danish Council for Independent Research and thank Frank Grundahl and Thomas Amby Ottosen for suggestions regarding the NOT proposal. J.B., A.M., A.S., and T.S. acknowledge support from the National Initiative on Undergraduate Science (NIUS) undertaken by the Homi Bhabha Centre for Science Education - Tata Institute of Fundamental Research (HBCSE-TIFR), Mumbai, India. S.G.S. acknowledges the support from grant SFRH/BPD/47611/2008 from the Fundacao para a Ciencia e Tecnologia (Portugal). J.M.Z. acknowledges the Polish Ministry grant number N N203 405139. D. Sa. acknowledges funding by the Spanish Ministry of Science and Innovation (MICINN) under the grant AYA 2010-20982-C02-02. NR 113 TC 20 Z9 20 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2012 VL 537 AR A111 DI 10.1051/0004-6361/201117037 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894HD UT WOS:000300416800111 ER PT J AU Ehrenreich, D Vidal-Madjar, A Widemann, T Gronoff, G Tanga, P Barthelemy, M Lilensten, J Etangs, ALD Arnold, L AF Ehrenreich, D. Vidal-Madjar, A. Widemann, T. Gronoff, G. Tanga, P. Barthelemy, M. Lilensten, J. Etangs, A. Lecavelier des Arnold, L. TI Transmission spectrum of Venus as a transiting exoplanet SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiative transfer; planets and satellites: atmospheres; astrobiology; planetary systems; scattering; planets and satellites: individual: Venus ID MOLECULAR SPECTROSCOPIC DATABASE; HUBBLE-SPACE-TELESCOPE; METAL-RICH ATMOSPHERE; EXTRASOLAR PLANET; RAYLEIGH-SCATTERING; CROSS-SECTION; HD 189733B; GJ 1214B; EARTH; ALTITUDE AB On 5-6 June 2012, Venus will be transiting the Sun for the last time before 2117. This event is an unique opportunity to assess the feasibility of the atmospheric characterisation of Earth-size exoplanets near the habitable zone with the transmission spectroscopy technique and provide an invaluable proxy for the atmosphere of such a planet. In this letter, we provide a theoretical transmission spectrum of the atmosphere of Venus that could be tested with spectroscopic observations during the 2012 transit. This is done using radiative transfer across Venus' atmosphere, with inputs from in-situ missions such as Venus Express and theoretical models. The transmission spectrum covers a range of 0.1-5 mu m and probes the limb between 70 and 150 km in altitude. It is dominated in UV by carbon dioxide absorption producing a broad transit signal of similar to 20 ppm as seen from Earth, and from 0.2 to 2.7 mu m by Mie extinction (similar to 5 ppm at 0.8 mu m) caused by droplets of sulfuric acid composing an upper haze layer above the main deck of clouds. These features are not expected for a terrestrial exoplanet and could help discriminating an Earth-like habitable world from a cytherean planet. C1 [Ehrenreich, D.; Barthelemy, M.; Lilensten, J.] UJF Grenoble 1, CNRS INSU, IPAG, UMR 5274, Grenoble, France. [Vidal-Madjar, A.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, Paris, France. [Widemann, T.] Univ Paris Diderot, UPMC, Observ Paris, LESIA, Meudon, France. [Gronoff, G.] NASA, Langley Res Ctr, Sci Directorate, Chem & Dynam Branch, Hampton, VA 23665 USA. [Tanga, P.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Cassiopee,UMR 6202, Nice, France. [Arnold, L.] CNRS OAMP, Observ Haute Provence, St Michel lObservatoire, France. RP Ehrenreich, D (reprint author), UJF Grenoble 1, CNRS INSU, IPAG, UMR 5274, Grenoble, France. EM david.ehrenreich@obs.ujf-grenoble.fr OI Gronoff, Guillaume/0000-0002-0331-7076; Tanga, Paolo/0000-0002-2718-997X; Ehrenreich, David/0000-0001-9704-5405 NR 41 TC 13 Z9 13 U1 3 U2 14 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 JAN PY 2012 VL 537 AR L2 DI 10.1051/0004-6361/201118400 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894HD UT WOS:000300416800159 ER PT J AU Lohne, T Augereau, JC Ertel, S Marshall, JP Eiroa, C Mora, A Absil, O Stapelfeldt, K Thebault, P Bayo, A del Burgo, C Danchi, W Krivov, AV Lebreton, J Letawe, G Magain, P Maldonado, J Montesinos, B Pilbratt, GL White, GJ Wolf, S AF Loehne, T. Augereau, J. -C. Ertel, S. Marshall, J. P. Eiroa, C. Mora, A. Absil, O. Stapelfeldt, K. Thebault, P. Bayo, A. del Burgo, C. Danchi, W. Krivov, A. V. Lebreton, J. Letawe, G. Magain, P. Maldonado, J. Montesinos, B. Pilbratt, G. L. White, G. J. Wolf, S. TI Modelling the huge, Herschel-resolved debris ring around HD 207129 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE interplanetary medium; stars: individual: HD 207129 ID EDGEWORTH-KUIPER BELT; MAIN-SEQUENCE STARS; BETA-PICTORIS DISK; VEGA-TYPE STARS; SUN-LIKE STARS; CIRCUMSTELLAR DISK; OPTICAL-CONSTANTS; SOLAR-SYSTEM; NEARBY STARS; DUST GRAINS AB Debris disks, which are inferred from the observed infrared excess to be ensembles of dust, rocks, and probably planetesimals, are common features of stellar systems. As the mechanisms of their formation and evolution are linked to those of planetary bodies, they provide valuable information. The few well-resolved debris disks are even more valuable because they can serve as modelling benchmarks and help resolve degeneracies in modelling aspects such as typical grain sizes and distances. Here, we present an analysis of the HD 207129 debris disk, based on its well-covered spectral energy distribution and Herschel/PACS images obtained in the framework of the DUNES (DUst around NEarby Stars) programme. We use an empirical power-law approach to the distribution of dust and we then model the production and removal of dust by means of collisions, direct radiation pressure, and drag forces. The resulting best-fit model contains a total of nearly 10(-2) Earth masses in dust, with typical grain sizes in the planetesimal belt ranging from 4 to 7 mu m. We constrain the dynamical excitation to be low, which results in very long collisional lifetimes and a drag that notably fills the inner gap, especially at 70 mu m. The radial distribution stretches from well within 100 AU in an unusual, outward-rising slope towards a rather sharp outer edge at about 170-190 AU. The inner edge is therefore smoother than that reported for Fomalhaut, but the contribution from the extended halo of barely bound grains is similarly small. Both slowly self-stirring and planetary perturbations could potentially have formed and shaped this disk. C1 [Loehne, T.; Krivov, A. V.] Univ Jena, Astrophys Inst & Univ, D-07745 Jena, Germany. [Augereau, J. -C.; Pilbratt, G. L.] IPAG, UJF Grenoble 1, CNRS INSU, F-38041 Grenoble, France. [Ertel, S.; Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. [Marshall, J. P.; Eiroa, C.] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, Madrid 28049, Spain. [Mora, A.] ESA ESAC Gaia SOC, Madrid, Spain. [Absil, O.; Letawe, G.; Magain, P.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Montesinos, B.] Ctr Astrobiol CAB CSIC INTA, Dept Astrofis, Madrid 28691, Spain. [Stapelfeldt, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Thebault, P.] Observ Paris, LESIA, F-92195 Meudon, France. [Bayo, A.] European So Observ, Santiago 19, Chile. [del Burgo, C.] UNINOVA CA3, P-2825149 Monte De Caparica, Caparica, Portugal. [Pilbratt, G. L.] ESTEC SRE SA, ESA Astrophys, NL-2201 AZ Noordwijk, Netherlands. [Pilbratt, G. L.] ESTEC SRE SA, Fundamental Phys Missions Div, NL-2201 AZ Noordwijk, Netherlands. [White, G. J.] Open Univ, Dept Phys & Astrophys, Milton Keynes MK7 6AA, Bucks, England. [White, G. J.] Rutherford Appleton Lab, Chilton OX11 0QX, England. [Danchi, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lohne, T (reprint author), Univ Jena, Astrophys Inst & Univ, Schillergasshen 2-3, D-07745 Jena, Germany. EM tloehne@astro.uni-jena.de RI Stapelfeldt, Karl/D-2721-2012; Montesinos, Benjamin/C-3493-2017 OI Marshall, Jonathan/0000-0001-6208-1801; Montesinos, Benjamin/0000-0002-7982-2095 FU Deutsche Forschungsgemeinschaft [Lo 1715/1-1, Kr 2164/9-1, Wo 857/7-1]; Spanish grant [AYA 2008-01727.]; Portuguese Fundacao para a Ciencia e a Tecnologia [PEst-OE/EEI/UI0066/2011] FX Parts of our work were funded by the Deutsche Forschungsgemeinschaft (grants Lo 1715/1-1, Kr 2164/9-1, and Wo 857/7-1). C. Eiroa, J. Maldonado, J. P. Marshall, and B. Montesinos are partly supported by Spanish grant AYA 2008-01727. A. Mora acknowledges support from the Portuguese Fundacao para a Ciencia e a Tecnologia (grant PEst-OE/EEI/UI0066/2011). We thank Harald Mutschke for a discussion about refractive indices. NR 73 TC 42 Z9 42 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2012 VL 537 AR A110 DI 10.1051/0004-6361/201117731 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894HD UT WOS:000300416800110 ER PT J AU Mosser, B Elsworth, Y Hekker, S Huber, D Kallinger, T Mathur, S Belkacem, K Goupil, MJ Samadi, R Barban, C Bedding, TR Chaplin, WJ Garcia, RA Stello, D De Ridder, J Middour, CK Morris, RL Quintana, EV AF Mosser, B. Elsworth, Y. Hekker, S. Huber, D. Kallinger, T. Mathur, S. Belkacem, K. Goupil, M. J. Samadi, R. Barban, C. Bedding, T. R. Chaplin, W. J. Garcia, R. A. Stello, D. De Ridder, J. Middour, C. K. Morris, R. L. Quintana, E. V. TI Characterization of the power excess of solar-like oscillations in red giants with Kepler SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: oscillations; stars: interiors; stars: evolution; stars: mass-loss; stars: late-type; methods: data analysis ID MAIN-SEQUENCE STARS; 1ST 4 MONTHS; STELLAR OSCILLATIONS; COROT; PARAMETERS; AMPLITUDES; MODES; ASTEROSEISMOLOGY; GRANULATION; EXCITATION AB Context. The space mission Kepler provides us with long and uninterrupted photometric time series of red giants. This allows us to examine their seismic global properties and to compare these with theoretical predictions. Aims. We aim to describe the oscillation power excess observed in red giant oscillation spectra with global seismic parameters, and to investigate empirical scaling relations governing these parameters. From these scalings relations, we derive new physical properties of red giant oscillations. Methods. Various different methods were compared in order to validate the processes and to derive reliable output values. For consistency, a single method was then used to determine scaling relations for the relevant global asteroseismic parameters: mean mode height, mean height of the background signal superimposed on the oscillation power excess, width of the power excess, bolometric amplitude of the radial modes and visibility of non-radial modes. A method for deriving oscillation amplitudes is proposed, which relies on the complete identification of the red giant oscillation spectrum. Results. The comparison of the different methods has shown the important role of the way the background is modelled. The convergence reached by the collaborative work enables us to derive significant results concerning the oscillation power excess. We obtain several scaling relations, and identify the influence of the stellar mass and the evolutionary status. The effect of helium burning on the red giant interior structure is confirmed: it yields a strong mass-radius relation for clump stars. We find that none of the amplitude scaling relations motivated by physical considerations predict the observed mode amplitudes of red giant stars. In parallel, the degree-dependent mode visibility exhibits important variations. Both effects seem related to the significant influence of the high mode mass of non-radial mixed modes. A family of red giants with very weak dipole modes is identified, and its properties are analyzed. Conclusions. The clear correlation between the power densities of the background signal and of the stellar oscillation induces important consequences to be considered for deriving a reliable theoretical relation of the mode amplitude. As a by-product of this work, we have verified that red giant asteroseismology delivers new insights for stellar and Galactic physics, given the evidence for mass loss at the tip of the red giant branch. C1 [Mosser, B.; Belkacem, K.; Goupil, M. J.; Samadi, R.; Barban, C.] Univ Paris 07, Observ Paris, Univ Paris 06, CNRS,LESIA, F-92195 Meudon, France. [Elsworth, Y.; Hekker, S.; Chaplin, W. J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Huber, D.; Bedding, T. R.; Stello, D.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Kallinger, T.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Kallinger, T.; De Ridder, J.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Mathur, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Belkacem, K.] Univ Paris 11, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. [Garcia, R. A.] Univ Paris Diderot IRFU SAp, CEA DSM CNRS, Lab AIM, F-91191 Gif Sur Yvette, France. [Middour, C. K.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. [Morris, R. L.; Quintana, E. V.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Mosser, B (reprint author), Univ Paris 07, Observ Paris, Univ Paris 06, CNRS,LESIA, F-92195 Meudon, France. EM benoit.mosser@obspm.fr OI Kallinger, Thomas/0000-0003-3627-2561; Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776 FU NASA's Science Mission Directorate; UK Science and Technology Facilities Council; Netherlands Organisation for Scientific Research (NWO); National Science Foundation; Australian Research Council; FWO-Flanders [O6260 - G.0728.11] FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. YE, SH and WJC acknowledge financial support from the UK Science and Technology Facilities Council. SH acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO). NCAR is supported by the National Science Foundation. DS and TRB acknowledge support by the Australian Research Council. TK acknowledges the support of the FWO-Flanders under project O6260 - G.0728.11. NR 46 TC 65 Z9 65 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2012 VL 537 AR A30 DI 10.1051/0004-6361/201117352 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894HD UT WOS:000300416800030 ER PT J AU Penin, A Dore, O Lagache, G Bethermin, M AF Penin, A. Dore, O. Lagache, G. Bethermin, M. TI Modeling the evolution of infrared galaxies: clustering of galaxies in the cosmic infrared background SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE infrared: galaxies; large scale structure of Universe; galaxies: high-redshift ID STAR-FORMING GALAXIES; MULTIBAND IMAGING PHOTOMETER; SPITZER-SPACE-TELESCOPE; GOODS FIELDS; LUMINOSITY FUNCTIONS; NUMBER COUNTS; IRAS GALAXIES; POWER SPECTRA; MU-M; ANISOTROPY AB Context. Star-forming galaxies are highly biased tracers of the underlying dark matter density field. Their clustering can be studied through the cosmic infrared background (CIB) anisotropies. These anisotropies have been measured from 100 mu m to 2 mm in the past few years. Aims. In this paper, we present a fully parametric model allowing joint analysis of these recent observations. Methods. To develop a coherent model at various wavelengths, we rely on two building blocks. The first one is a parametric model that describes the redshift evolution of the luminosity function of star-forming galaxies. It compares favorably to measured differential number counts and luminosity functions. The second is a halo model-based description of the clustering of galaxies. Starting from a fiducial model, we investigate parameter degeneracies using a Fisher analysis. We then discuss how halos of different masses and redshifts and how LIRGs and ULIRGs contribute to the CIB angular power spectra. Results. From the Fisher analysis, we conclude that we cannot constrain the parameters of the model of evolution of galaxies using clustering data only. The use of combined data of C-l, counts, and luminosity functions improves the constraints slightly but does not remove any degeneracies. In contrast, the measurement of the anisotropies allows us to set interesting constraints on the halo model parameters, even if some strong degeneracies remain. Using our fiducial model, we establish that the 1-halo and 2-halo terms are not sensitive to the same mass regime. We also illustrate how the 1-halo term can be misinterpreted with the Poisson noise term. Conclusions. We present a new model of the clustering of infrared galaxies. Our framework allows a coherent and joint analysis of various probes of infrared galaxies: number counts, luminosity functions, and clustering measurements; however, such a model has a few limitations, such as the parameters of the halo occupation that suffer from strong degeneracies. C1 [Penin, A.; Lagache, G.; Bethermin, M.] Univ Paris 11, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France. [Penin, A.; Lagache, G.; Bethermin, M.] CNRS, F-91405 Orsay, France. [Dore, O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dore, O.] CALTECH, Pasadena, CA 91125 USA. RP Penin, A (reprint author), Univ Paris 11, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France. EM aurelie.penin@ias.u-psud.fr OI Bethermin, Matthieu/0000-0002-3915-2015 FU National Aeronautics and Space Administration FX 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 authors would like to thank Mathieu Langer for very useful comments that improved this manuscript. NR 48 TC 21 Z9 21 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2012 VL 537 AR A137 DI 10.1051/0004-6361/201117489 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894HD UT WOS:000300416800137 ER PT J AU Roelfsema, PR Helmich, FP Teyssier, D Ossenkopf, V Morris, P Olberg, M Shipman, R Risacher, C Akyilmaz, M Assendorp, R Avruch, IM Beintema, D Biver, N Boogert, A Borys, C Braine, J Caris, M Caux, E Cernicharo, J Coeur-Joly, O Comito, C de Lange, G Delforge, B Dieleman, P Dubbeldam, L de Graauw, T Edwards, K Fich, M Flederus, F Gal, C di Giorgio, A Herpin, F Higgins, DR Hoac, A Huisman, R Jarchow, C Jellema, W de Jonge, A Kester, D Klein, T Kooi, J Kramer, C Laauwen, W Larsson, B Leinz, C Lord, S Lorenzani, A Luinge, W Marston, A Martin-Pintado, J McCoey, C Melchior, M Michalska, M Moreno, R Muller, H Nowosielski, W Okada, Y Orleanski, P Phillips, TG Pearson, J Rabois, D Ravera, L Rector, J Rengel, M Sagawa, H Salomons, W Sanchez-Suarez, E Schieder, R Schloder, F Schmulling, F Soldati, M Stutzki, J Thomas, B Tielens, AGGM Vastel, C Wildeman, K Xie, Q Xilouris, M Wafelbakker, C Whyborn, N Zaal, P Bell, T Bjerkeli, P de Beck, E Cavalie, T Crockett, NR Hily-Blant, P Kama, M Kaminski, T Lefloch, B Lombaert, R De Luca, M Makai, Z Marseille, M Nagy, Z Pacheco, S van der Wiel, MHD Wang, S Yildiz, U AF Roelfsema, P. R. Helmich, F. P. Teyssier, D. Ossenkopf, V. Morris, P. Olberg, M. Shipman, R. Risacher, C. Akyilmaz, M. Assendorp, R. Avruch, I. M. Beintema, D. Biver, N. Boogert, A. Borys, C. Braine, J. Caris, M. Caux, E. Cernicharo, J. Coeur-Joly, O. Comito, C. de Lange, G. Delforge, B. Dieleman, P. Dubbeldam, L. de Graauw, Th Edwards, K. Fich, M. Flederus, F. Gal, C. di Giorgio, A. Herpin, F. Higgins, D. R. Hoac, A. Huisman, R. Jarchow, C. Jellema, W. de Jonge, A. Kester, D. Klein, T. Kooi, J. Kramer, C. Laauwen, W. Larsson, B. Leinz, C. Lord, S. Lorenzani, A. Luinge, W. Marston, A. Martin-Pintado, J. McCoey, C. Melchior, M. Michalska, M. Moreno, R. Mueller, H. Nowosielski, W. Okada, Y. Orleanski, P. Phillips, T. G. Pearson, J. Rabois, D. Ravera, L. Rector, J. Rengel, M. Sagawa, H. Salomons, W. Sanchez-Suarez, E. Schieder, R. Schloeder, F. Schmuelling, F. Soldati, M. Stutzki, J. Thomas, B. Tielens, A. G. G. M. Vastel, C. Wildeman, K. Xie, Q. Xilouris, M. Wafelbakker, C. Whyborn, N. Zaal, P. Bell, T. Bjerkeli, P. de Beck, E. Cavalie, T. Crockett, N. R. Hily-Blant, P. Kama, M. Kaminski, T. Lefloch, B. Lombaert, R. De Luca, M. Makai, Z. Marseille, M. Nagy, Z. Pacheco, S. van der Wiel, M. H. D. Wang, S. Yildiz, U. TI In-orbit performance of Herschel-HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: observational; space vehicles: instruments; instrumentation: spectrographs ID ASTRONOMY AB Aims. In this paper the calibration and in-orbit performance of the Heterodyne Instrument for the Far-Infrared (HIFI) is described. Methods. The calibration of HIFI is based on a combination of ground and in-flight tests. Dedicated ground tests to determine those instrument parameters that can only be measured accurately using controlled laboratory stimuli were carried out in the instrument level test (ILT) campaign. Special in-flight tests during the commissioning phase (CoP) and performance verification (PV) allowed the determination of the remaining instrument parameters. The various instrument observing modes, as specified in astronomical observation templates (AOTs), were validated in parallel during PV by observing selected celestial sources. Results. The initial calibration and in-orbit performance of HIFI has been established. A first estimate of the calibration budget is given. The overall in-flight instrument performance agrees with the original specification. Issues remain at only a few frequencies. C1 [Roelfsema, P. R.; Helmich, F. P.; Ossenkopf, V.; Olberg, M.; Shipman, R.; Risacher, C.; Assendorp, R.; Avruch, I. M.; Beintema, D.; de Lange, G.; Dieleman, P.; Dubbeldam, L.; Flederus, F.; Huisman, R.; Jellema, W.; de Jonge, A.; Kester, D.; Laauwen, W.; Luinge, W.; Salomons, W.; Thomas, B.; Wildeman, K.; Wafelbakker, C.; Zaal, P.; Kama, M.; Marseille, M.; Nagy, Z.; van der Wiel, M. H. D.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Teyssier, D.; Marston, A.] ESA, European Space Astron Ctr, Madrid 28691, Spain. [Ossenkopf, V.; Akyilmaz, M.; Gal, C.; Kramer, C.; Mueller, H.; Okada, Y.; Schieder, R.; Schloeder, F.; Schmuelling, F.; Stutzki, J.; Makai, Z.] Univ Cologne, KOSMA, Inst Phys 1, D-50937 Cologne, Germany. [Morris, P.; Boogert, A.; Borys, C.; Hoac, A.; Lord, S.; Rector, J.; Xie, Q.] CALTECH, NHSC, Pasadena, CA 91125 USA. [Olberg, M.; Bjerkeli, P.] Chalmers, S-41296 Gothenburg, Sweden. [Caris, M.; Comito, C.; Klein, T.; Leinz, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Caux, E.; Coeur-Joly, O.; Rabois, D.; Ravera, L.; Vastel, C.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Caux, E.; Coeur-Joly, O.; Rabois, D.; Ravera, L.; Vastel, C.] IRAP, CNRS, F-31028 Toulouse 4, France. [Jarchow, C.; Rengel, M.; Sagawa, H.; Cavalie, T.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Delforge, B.] UCP, UPMC, Lab Etud Rayonnement & Matiere Astrophys, OP,ENS,UMR CNRS INSU 8112, F-75231 Paris 05, France. [Lorenzani, A.] Osservatorio Astrofis Arcetri INAF, I-50100 Florence, Italy. [di Giorgio, A.] Inst Fis Spazio Interplanetario INAF, I-00133 Rome, Italy. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Melchior, M.; Soldati, M.] ETH, Astron Inst, CH-8093 Zurich, Switzerland. [Cernicharo, J.; Martin-Pintado, J.; Sanchez-Suarez, E.] Ctr Astrobiol INTA CSIC, Madrid 28850, Spain. [Edwards, K.; Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [de Graauw, Th; Whyborn, N.] Joint Alma Observ, Santiago, Chile. [Tielens, A. G. G. M.; Yildiz, U.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Kooi, J.; Phillips, T. G.; Bell, T.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Michalska, M.; Nowosielski, W.; Orleanski, P.] Polish Acad Sci, Space Res Ctr, PL-00716 Warsaw, Poland. [Higgins, D. R.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Braine, J.; Herpin, F.] Univ Bordeaux, Observ Aquitain Sci Univers, F-33271 Floirac, France. [Braine, J.; Herpin, F.] CNRS, UMR 5804, Lab Astrophys Bordeaux, F-33271 Floirac, France. [Xilouris, M.] Natl Observ Athens, Athens, Greece. [Pearson, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Biver, N.; Moreno, R.; De Luca, M.] UPMC, Ecole Normale Super, Observ Paris, LERMA LRA,UMR CNRS 8112, F-75231 Paris 05, France. [Avruch, I. M.; Nagy, Z.; van der Wiel, M. H. D.] Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands. [de Beck, E.; Lombaert, R.] Katholieke Univ Leuven, Inst Astron, Dept Phys & Astron, B-3001 Louvain, Belgium. [Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Hily-Blant, P.; Lefloch, B.; Pacheco, S.] UJF Grenoble, Inst Planetol & Astrophys Grenoble IPAG UMR 5274, CNRS INSU, F-38041 Grenoble, France. [Kama, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Kaminski, T.] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-87100 Torun, Poland. RP Roelfsema, PR (reprint author), Univ Groningen, SRON Netherlands Inst Space Res, Landleven 12, NL-9747 AD Groningen, Netherlands. EM p.r.roelfsema@sron.nl RI Yildiz, Umut/C-5257-2011; Xilouris, Emmanuel/K-9459-2013; van der Wiel, Matthijs/M-4531-2014; Martin-Pintado, Jesus/H-6107-2015; OI Yildiz, Umut/0000-0001-6197-2864; van der Wiel, Matthijs/0000-0002-4325-3011; Martin-Pintado, Jesus/0000-0003-4561-3508; Lorenzani, Andrea/0000-0002-4685-3434; Bjerkeli, Per/0000-0002-7993-4118; Mueller, Holger/0000-0002-0183-8927; De Beck, Elvire/0000-0002-7441-7189; Kama, Mihkel/0000-0003-0065-7267 FU Deutsches Zentrum fur Luft- und Raumfahrt (DLR) [50OF00053]; Max-Planck-Society; CNES; National Aeronautics and Space Administration; Science and High Education Ministry of Poland [N203 393334] FX 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: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; The Netherlands: SRON, TUD; Poland: CAMK, CBK; 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. This work has been partially supported by grant 50OF00053 of the Deutsches Zentrum fur Luft- und Raumfahrt (DLR) and by central resources of the Max-Planck-Society. This work has been partly supported by CNES. A part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work has been partly supported by grant N203 393334 of the Science and High Education Ministry of Poland NR 22 TC 151 Z9 151 U1 0 U2 8 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 JAN PY 2012 VL 537 AR A17 DI 10.1051/0004-6361/201015120 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894HD UT WOS:000300416800017 ER PT J AU Rosenberg, MJF Berne, O Boersma, C Allamandola, LJ Tielens, AGGM AF Rosenberg, M. J. F. Berne, O. Boersma, C. Allamandola, L. J. Tielens, A. G. G. M. TI Coupled blind signal separation and spectroscopic database fitting of the mid-infrared PAH features (vol 532, pg A128, 2011) SO ASTRONOMY & ASTROPHYSICS LA English DT Correction DE astrochemistry; infrared: ISM; ISM: lines and bands; photon-dominated region (PDR); Errata, addenda C1 [Rosenberg, M. J. F.; Berne, O.; Tielens, A. G. G. M.] Leiden Univ, Sterrewacht Leiden, NL-2333 CA Leiden, Netherlands. [Rosenberg, M. J. F.] Int Space Univ, F-67400 Illkirch Graffenstaden, France. [Boersma, C.; Allamandola, L. J.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Rosenberg, MJF (reprint author), Leiden Univ, Sterrewacht Leiden, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. EM rosenberg@strw.leidenuniv.nl; Christiaan.Boersma@nasa.gov; Louis.J.Allamandola@nasa.gov RI Boersma, Christiaan/L-7696-2014 OI Boersma, Christiaan/0000-0002-4836-217X NR 1 TC 2 Z9 2 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2012 VL 537 AR C5 DI 10.1051/0004-6361/201016340e PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894HD UT WOS:000300416800157 ER PT J AU Saito, RK Hempel, M Minniti, D Lucas, PW Rejkuba, M Toledo, I Gonzalez, OA Alonso-Garcia, J Irwin, MJ Gonzalez-Solares, E Hodgkin, ST Lewis, JR Cross, N Ivanov, VD Kerins, E Emerson, JP Soto, M Amores, EB Gurovich, S Dekany, I Angeloni, R Beamin, JC Catelan, M Padilla, N Zoccali, M Pietrukowicz, P Bidin, CM Mauro, F Geisler, D Folkes, SL Sale, SE Borissova, J Kurtev, R Ahumada, AV Alonso, MV Adamson, A Arias, JI Bandyopadhyay, RM Barba, RH Barbuy, B Baume, GL Bedin, LR Bellini, A Benjamin, R Bica, E Bonatto, C Bronfman, L Carraro, G Chene, AN Claria, JJ Clarke, JRA Contreras, C Corvillon, A de Grijs, R Dias, B Drew, JE Farina, C Feinstein, C Fernandez-Lajus, E Gamen, RC Gieren, W Goldman, B Gonzalez-Fernandez, C Grand, RJJ Gunthardt, G Hambly, NC Hanson, MM Helminiak, KG Hoare, MG Huckvale, L Jordan, A Kinemuchi, K Longmore, A Lopez-Corredoira, M Maccarone, T Majaess, D Martin, EL Masetti, N Mennickent, RE Mirabel, IF Monaco, L Morelli, L Motta, V Palma, T Parisi, MC Parker, Q Penaloza, F Pietrzynski, G Pignata, G Popescu, B Read, MA Rojas, A Roman-Lopes, A Ruiz, MT Saviane, I Schreiber, MR Schroder, AC Sharma, S Smith, MD Sodre, L Stead, J Stephens, AW Tamura, M Tappert, C Thompson, MA Valenti, E Vanzi, L Walton, NA Weidmann, W Zijlstra, A AF Saito, R. K. Hempel, M. Minniti, D. Lucas, P. W. Rejkuba, M. Toledo, I. Gonzalez, O. A. Alonso-Garcia, J. Irwin, M. J. Gonzalez-Solares, E. Hodgkin, S. T. Lewis, J. R. Cross, N. Ivanov, V. D. Kerins, E. Emerson, J. P. Soto, M. Amores, E. B. Gurovich, S. Dekany, I. Angeloni, R. Beamin, J. C. Catelan, M. Padilla, N. Zoccali, M. Pietrukowicz, P. Bidin, C. Moni Mauro, F. Geisler, D. Folkes, S. L. Sale, S. E. Borissova, J. Kurtev, R. Ahumada, A. V. Alonso, M. V. Adamson, A. Arias, J. I. Bandyopadhyay, R. M. Barba, R. H. Barbuy, B. Baume, G. L. Bedin, L. R. Bellini, A. Benjamin, R. Bica, E. Bonatto, C. Bronfman, L. Carraro, G. Chene, A. N. Claria, J. J. Clarke, J. R. A. Contreras, C. Corvillon, A. de Grijs, R. Dias, B. Drew, J. E. Farina, C. Feinstein, C. Fernandez-Lajus, E. Gamen, R. C. Gieren, W. Goldman, B. Gonzalez-Fernandez, C. Grand, R. J. J. Gunthardt, G. Hambly, N. C. Hanson, M. M. Helminiak, K. G. Hoare, M. G. Huckvale, L. Jordan, A. Kinemuchi, K. Longmore, A. Lopez-Corredoira, M. Maccarone, T. Majaess, D. Martin, E. L. Masetti, N. Mennickent, R. E. Mirabel, I. F. Monaco, L. Morelli, L. Motta, V. Palma, T. Parisi, M. C. Parker, Q. Penaloza, F. Pietrzynski, G. Pignata, G. Popescu, B. Read, M. A. Rojas, A. Roman-Lopes, A. Ruiz, M. T. Saviane, I. Schreiber, M. R. Schroeder, A. C. Sharma, S. Smith, M. D. Sodre, L., Jr. Stead, J. Stephens, A. W. Tamura, M. Tappert, C. Thompson, M. A. Valenti, E. Vanzi, L. Walton, N. A. Weidmann, W. Zijlstra, A. TI VVV DR1: The first data release of the Milky Way bulge and southern plane from the near-infrared ESO public survey VISTA variables in the Via Lactea SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Galaxy: bulge; Galaxy: disk; Galaxy: stellar content; stars: abundances; infrared: stars; surveys ID GALACTIC BULGE; INTERSTELLAR EXTINCTION; ACS SURVEY; PHOTOMETRY; SYSTEM; 2MASS; CLUSTERS; DISTANCE; PROJECT; CAMERA AB Context. The ESO public survey VISTA variables in the Via Lactea (VVV) started in 2010. VVV targets 562 sq. deg in the Galactic bulge and an adjacent plane region and is expected to run for about five years. Aims. We describe the progress of the survey observations in the first observing season, the observing strategy, and quality of the data obtained. Methods. The observations are carried out on the 4-m VISTA telescope in the ZYJHK(s) filters. In addition to the multi-band imaging the variability monitoring campaign in the K-s filter has started. Data reduction is carried out using the pipeline at the Cambridge Astronomical Survey Unit. The photometric and astrometric calibration is performed via the numerous 2MASS sources observed in each pointing. Results. The first data release contains the aperture photometry and astrometric catalogues for 348 individual pointings in the ZYJHK(s) filters taken in the 2010 observing season. The typical image quality is similar to 0 ''.9-1 ''.0. The stringent photometric and image quality requirements of the survey are satisfied in 100% of the JHK(s) images in the disk area and 90% of the JHK(s) images in the bulge area. The completeness in the Z and Y images is 84% in the disk, and 40% in the bulge. The first season catalogues contain 1.28 x 10(8) stellar sources in the bulge and 1.68 x 10(8) in the disk area detected in at least one of the photometric bands. The combined, multi-band catalogues contain more than 1.63 x 10(8) stellar sources. About 10% of these are double detections because of overlapping adjacent pointings. These overlapping multiple detections are used to characterise the quality of the data. The images in the JHK(s) bands extend typically similar to 4 mag deeper than 2MASS. The magnitude limit and photometric quality depend strongly on crowding in the inner Galactic regions. The astrometry for K-s = 15-18 mag has rms similar to 35-175 mas. Conclusions. The VVV Survey data products offer a unique dataset to map the stellar populations in the Galactic bulge and the adjacent plane and provide an exciting new tool for the study of the structure, content, and star-formation history of our Galaxy, as well as for investigations of the newly discovered star clusters, star-forming regions in the disk, high proper motion stars, asteroids, planetary nebulae, and other interesting objects. C1 [Saito, R. K.; Hempel, M.; Minniti, D.; Alonso-Garcia, J.; Dekany, I.; Angeloni, R.; Beamin, J. C.; Catelan, M.; Padilla, N.; Zoccali, M.; Sale, S. E.; Corvillon, A.; Helminiak, K. G.; Jordan, A.; Rojas, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 4860, Chile. [Minniti, D.] Vatican Observ, I-00120 Vatican City, Vatican. [Minniti, D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Lucas, P. W.; Contreras, C.; Drew, J. E.; Thompson, M. A.] Univ Hertfordshire, Ctr Astrophys, Hatfield AL10 9AB, Herts, England. [Rejkuba, M.; Gonzalez, O. A.; Valenti, E.] European So Observ, D-85748 Garching, Germany. [Toledo, I.] Atacama Large Millimeter Array, Santiago, Chile. [Irwin, M. J.; Gonzalez-Solares, E.; Hodgkin, S. T.; Lewis, J. R.; Walton, N. A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Cross, N.; Hambly, N. C.; Read, M. A.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivanov, V. D.; Ahumada, A. V.; Carraro, G.; Monaco, L.; Saviane, I.] European So Observ, Santiago 19001, Chile. [Kerins, E.; Huckvale, L.; Zijlstra, A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Oxford, England. [Emerson, J. P.] Queen Mary Univ London, Sch Phys & Astron, Astron Unit, London E1 4NS, England. [Soto, M.; Arias, J. I.; Barba, R. H.; Roman-Lopes, A.] Univ La Serena, Dept Fis, La Serena 1200, Chile. [Amores, E. B.] Univ Lisbon, Fac Ciencia, P-1749016 Lisbon, Portugal. [Amores, E. B.] Lab Nacl Astrofis, BR-37504364 Itajuba, MG, Brazil. [Gurovich, S.; Alonso, M. V.] Consejo Nacl Invest Cient & Tecn, Inst Astron Teor & Expt, RA-5000 Cordoba, Argentina. [Padilla, N.; Vanzi, L.] Pontificia Univ Catolica Chile, Ctr Astro Ingn, Santiago 4860, Chile. [Zoccali, M.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Pietrukowicz, P.; Pietrzynski, G.] Univ Warsaw Observ, PL-400478 Warsaw, Poland. [Folkes, S. L.; Sale, S. E.; Borissova, J.; Kurtev, R.; Chene, A. N.; Clarke, J. R. A.; Motta, V.; Penaloza, F.; Schreiber, M. R.; Sharma, S.; Tappert, C.] Univ Valparaiso, Dept Fis & Astron, Fac Ciencias, Valparaiso 5030, Chile. [Adamson, A.] Gemini Observ, So Operat Ctr, La Serena, Chile. [Bandyopadhyay, R. M.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Barba, R. H.; Sharma, S.] ICATE CONICET, Inst Ciencias Astron Tierra & Espacio, San Juan, PR USA. [Barbuy, B.; Dias, B.; Sodre, L., Jr.] Univ Sao Paulo, IAG, BR-05508900 Sao Paulo, Brazil. [Baume, G. L.; Farina, C.; Feinstein, C.; Fernandez-Lajus, E.; Gamen, R. C.] Univ Nacl Plata, Fac Ciencias Astron & Geofis, La Plata, Argentina. [Bedin, L. R.] INAF Astron Observ Padova, I-35122 Padua, Italy. [Bellini, A.; Morelli, L.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Benjamin, R.] Univ Wisconsin, Dept Phys, Whitewater, WI 53190 USA. [Bica, E.; Bonatto, C.] Univ Fed Rio Grande do Sul, IF, BR-91501970 Porto Alegre, RS, Brazil. [Bronfman, L.; Ruiz, M. T.] Univ Chile, Dept Astron, Santiago, Chile. [de Grijs, R.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [de Grijs, R.] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 449701, Kyungki Do, South Korea. [Goldman, B.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Gonzalez-Fernandez, C.] Univ Alicante, Dept Fis, Alicante 03080, Spain. [Grand, R. J. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Hanson, M. M.; Popescu, B.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Hoare, M. G.; Stead, J.] Univ Leeds, Sch Phys Astron, Leeds LS2 9JT, W Yorkshire, England. [Kinemuchi, K.] NASA, Ames Res Center, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Longmore, A.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Lopez-Corredoira, M.] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Tenerife, Spain. [Lopez-Corredoira, M.] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain. [Maccarone, T.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Majaess, D.] St Marys Univ, Halifax, NS B3H 3C3, Canada. [Martin, E. L.] Ctr Astrobiol CSIC INTA, Madrid 28850, Spain. [Masetti, N.] Ist Astrofis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy. [Mirabel, I. F.] CEA Saclay, Serv Astrophys IRFU, F-91191 Gif Sur Yvette, France. [Mirabel, I. F.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Parker, Q.] Macquarie Univ, Dept Phys Astron, Sydney, NSW 2109, Australia. [Parker, Q.] Australian Astron Observ, Epping, NSW NSW1710, Australia. [Pignata, G.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Schroeder, A. C.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Schroeder, A. C.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa. Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263129, India. [Smith, M. D.] Univ Kent, Canterbury CT2 7NH, Kent, England. [Stephens, A. W.] Gemini Observ, No Operat Ctr, Hilo, HI 96720 USA. [Tamura, M.] Natl Astron Observ Japan, Div Opt & Infrared Astron, Mitaka, Tokyo 1818588, Japan. [Vanzi, L.] Pontificia Univ Catolica Chile, Dept Ingn Elect, Santiago, Chile. RP Saito, RK (reprint author), Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Av Vicuna Mackenna, Santiago 4860, Chile. EM rsaito@astro.puc.cl RI Saito, Roberto/L-6722-2016; 7, INCT/H-6207-2013; Sodre, Laerte/P-6045-2016; Bronfman, Leonardo/H-9544-2013; Astrofisica, Inct/H-9455-2013; Vanzi, Leonardo/D-1381-2014; Barba, Rodolfo/P-4649-2014; Gonzalez-Fernandez, Carlos/H-3569-2015; Alonso-Garcia, Javier/I-2723-2015; Gamen, Roberto/A-1728-2015; Helminiak, Krzysztof/N-6385-2015; Ruiz, Maria Teresa/I-5770-2016; OI Sodre, Laerte/0000-0002-3876-268X; Bronfman, Leonardo/0000-0002-9574-8454; Barba, Rodolfo/0000-0003-1086-1579; Gonzalez-Fernandez, Carlos/0000-0003-2612-0118; Alonso-Garcia, Javier/0000-0003-3496-3772; Helminiak, Krzysztof/0000-0002-7650-3603; Ruiz, Maria Teresa/0000-0002-6799-1537; Sale, Stuart/0000-0003-2155-0995; adamson, andrew/0000-0003-1120-5178; bedin, luigi/0000-0003-4080-6466; Rejkuba, Marina/0000-0002-6577-2787; de Grijs, Richard/0000-0002-7203-5996; Masetti, Nicola/0000-0001-9487-7740; Ivanov, Valentin/0000-0002-5963-1283; Toledo, Ignacio/0000-0003-1653-9468; Jordan, Andres/0000-0002-5389-3944; Drew, Janet/0000-0003-1192-7082 FU FONDAP Center for Astrophysics [15010003]; BASAL CATA Center for Astrophysics and Associated Technologies [PFB-06]; FONDECYT from CONICYT; Ministry for the Economy, Development, and Tourism [P07-021-F]; CONICYT [32080016, Al'32090002]; Proyecto FONDECYT [1090213, 1110393, 3110188, 3100029, 1110326]; FONDECYT [1080086]; Comitee Mixto ESO-Gobierno de Chile; National Natural Science Foundation of China [11073001]; US National Science Foundation [0607497, 1009550]; Millennium Center for Supernova Science [P06-045-F]; Programa Bicentenario de Ciencia y Tecnologa de CONICYT; Proyecto Anillo [ACT-86]; ESO-Government of Chile Mixed Committee; Gemini-CONICYT [32090014/2009]; FAPESP; CNPq; Fundacao para a Ciencia e Tecnologia (FCT) [SFRH/BPD/42239/2007]; Centro de Astrofisica de Valparaiso [DIUV23/2009] FX We gratefully acknowledge use of data from the ESO Public Survey programme ID 179.B-2002 taken with the VISTA telescope, data products from the Cambridge Astronomical Survey Unit, and funding from the FONDAP Center for Astrophysics 15010003, the BASAL CATA Center for Astrophysics and Associated Technologies PFB-06, the FONDECYT from CONICYT, and the Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cientifica Milenio through grant P07-021-F, awarded to The Milky Way Millennium Nucleus. R.K.S. and D.M. acknowledge financial support from CONICYT through Gemini Project No. 32080016. D.M. acknowledge support by Proyecto FONDECYT Regular No. 1090213. M.Z. and O.A.G. acknowledge support by Proyecto FONDECYT Regular No. 1110393. J.B. and F.P. are supported by FONDECYT Regular No. 1080086. J.R.A.C. is supported by CONICYT through Gemini Project No. Al'32090002. A.N.C. received support from Comitee Mixto ESO-Gobierno de Chile. M.S. acknowledges support by Proyecto FONDECYT Regular No. 3110188 and Comite Mixto ESO-Gobierno de Chile. Support for R.A. is provided by Proyecto FONDECYT Regular No. 3100029. R.d.G. acknowledges partial research support through grant 11073001 from the National Natural Science Foundation of China. M.M.H. is supported for this work by the US National Science Foundation under Grant Nos. 0607497 and 1009550. G.P. acknowledge support from the Millennium Center for Supernova Science through grant P06-045-F funded by Programa Bicentenario de Ciencia y Tecnologa de CONICYT. M.C., J.A.G. and I.D. acknowledge support by Proyecto FONDECYT Regular No. 1110326. M.C. is also supported in part by Proyecto Anillo ACT-86. S.L.F. acknowledges funding support from the ESO-Government of Chile Mixed Committee 2009 and from the Gemini-CONICYT grant No. 32090014/2009. B.B., B.D. and L.S.J. acknowledge support from FAPESP and CNPq. E.B.A. thanks Fundacao para a Ciencia e Tecnologia (FCT) under the grant SFRH/BPD/42239/2007. R.K. acknowledges support from the Centro de Astrofisica de Valparaiso and Proyecto DIUV23/2009. NR 49 TC 101 Z9 101 U1 3 U2 27 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 JAN PY 2012 VL 537 AR A107 DI 10.1051/0004-6361/201118407 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894HD UT WOS:000300416800107 ER PT J AU Schady, P Dwelly, T Page, MJ Kruhler, T Greiner, J Oates, SR De Pasquale, M Nardini, M Roming, PWA Rossi, A Still, M AF Schady, P. Dwelly, T. Page, M. J. Kruehler, T. Greiner, J. Oates, S. R. De Pasquale, M. Nardini, M. Roming, P. W. A. Rossi, A. Still, M. TI The dust extinction curves of gamma-ray burst host galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE dust, extinction; galaxies: ISM; gamma-ray burst: general; ultraviolet: ISM ID SPECTRAL IRRADIANCE CALIBRATION; SIMILAR-TO 2; HIGH-REDSHIFT; OPTICAL AFTERGLOW; ULTRAVIOLET EXTINCTION; RAPTOR OBSERVATIONS; COLUMN DENSITIES; GRB AFTERGLOWS; ALPHA SYSTEMS; LIGHT CURVES AB The composition and amount of interstellar dust within gamma-ray burst (GRB) host galaxies is of key importance when addressing selection effects in the GRB redshift distribution, and when studying the properties of their host galaxies. As well as the implications for GRB research, probing the dust within the high-z hosts of GRBs also contributes to our understanding of the conditions of the interstellar medium and star-formation in the distant Universe. Nevertheless, the physical properties of dust within GRB host galaxies continues to be a highly contended issue. In this paper we explore the mean extinction properties of dust within the host galaxies of a sample of 17 GRBs with total host galaxy visual extinction A(V) < 1 (< A(V)> = 0.4), covering a redshift range z = 0.7-3.1. We find the average host extinction curve to have an ultraviolet slope comparable to that of the LMC, but with little evidence of a 2175 angstrom dust extinction feature as observed along Milky Way and LMC sightlines. We cannot at present rule out the presence of a 2175 angstrom feature, and both the standard SMC and LMC extinction curves also provide good fits to our data. However, we can reject an extinction curve that has a UV slope as flat as the mean Milky Way extinction curve, whilst also having a 2175 angstrom feature as prominent as seen in the mean Milky Way extinction curve. This is in contrast to the clear detection of a 2175 angstrom bump and the flatter extinction curves of some more heavily extinguished GRBs (A(V) > 1), which may be indicative of there being a dependence between dust abundance and the wavelength dependence of dust extinction, as has been previously speculated. C1 [Schady, P.; Kruehler, T.; Greiner, J.; Nardini, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Schady, P.; Page, M. J.; Oates, S. R.; De Pasquale, M.] UCL Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Dwelly, T.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Kruehler, T.] Tech Univ Munich, D-85748 Garching, Germany. [Kruehler, T.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Nardini, M.] Univ Milano Bicocca, Dept Phys, I-20126 Milan, Italy. [Roming, P. W. A.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78238 USA. [Rossi, A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Still, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Schady, P (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. EM pschady@mpe.mpg.de RI Rossi, Andrea/N-4674-2015; OI Rossi, Andrea/0000-0002-8860-6538; Kruehler, Thomas/0000-0002-8682-2384 FU Deutsche Forschungsgemeinschaft (DFG) [SA 2001/2-1]; European Commission; Danish National Research Foundation; UKSA FX We thank the referee for the helpful comments that have improved this paper. P. S. acknowledges support through project SA 2001/2-1 of the DFG. T. K. acknowledges support from the Deutsche Forschungsgemeinschaft (DFG) cluster of excellence 'Origin and Structure of the Universe' as well as support from the European Commission under the Marie Curie Intra-European Fellowship Programme. The Dark Cosmology Centre is funded by the Danish National Research Foundation. S.R.O. and M.J.P. acknowledge the support of UKSA. This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), the UK Swift Science Data Centre at the University of Leicester and the Leicester Data base and Archive Service (LEDAS), provided by NASAs Goddard Space Flight Center and the Department of Physics and Astronomy, Leicester University, UK, respectively. NR 226 TC 36 Z9 37 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2012 VL 537 AR A15 DI 10.1051/0004-6361/201117414 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894HD UT WOS:000300416800015 ER PT J AU Gu, Y Liou, KN Jiang, JH Su, H Liu, X AF Gu, Y. Liou, K. N. Jiang, J. H. Su, H. Liu, X. TI Dust aerosol impact on North Africa climate: a GCM investigation of aerosol-cloud-radiation interactions using A-Train satellite data SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID GENERAL-CIRCULATION MODEL; MINERAL DUST; CIRRUS CLOUDS; ICE MICROPHYSICS; SAHEL CLIMATE; PARAMETERIZATION; TEMPERATURE; SCATTERING; SIMULATIONS; ABSORPTION AB The climatic effects of dust aerosols in North Africa have been investigated using the atmospheric general circulation model (AGCM) developed at the University of California, Los Angeles (UCLA). The model includes an efficient and physically based radiation parameterization scheme developed specifically for application to clouds and aerosols. Parameterization of the effective ice particle size in association with the aerosol first indirect effect based on ice cloud and aerosol data retrieved from A-Train satellite observations have been employed in climate model simulations. Offline simulations reveal that the direct solar, IR, and net forcings by dust aerosols at the top of the atmosphere (TOA) generally increase with increasing aerosol optical depth. When the dust semi-direct effect is included with the presence of ice clouds, positive IR radiative forcing is enhanced since ice clouds trap substantial IR radiation, while the positive solar forcing with dust aerosols alone has been changed to negative values due to the strong reflection of solar radiation by clouds, indicating that cloud forcing associated with aerosol semi-direct effect could exceed direct aerosol forcing. With the aerosol first indirect effect, the net cloud forcing is generally reduced in the case for an ice water path (IWP) larger than 20 g m(-2). The magnitude of the reduction increases with IWP. AGCM simulations show that the reduced ice crystal mean effective size due to the aerosol first indirect effect results in less OLR and net solar flux at TOA over the cloudy area of the North Africa region because ice clouds with smaller size trap more IR radiation and reflect more solar radiation. The precipitation in the same area, however, increases due to the aerosol indirect effect on ice clouds, corresponding to the enhanced convection as indicated by reduced OLR. Adding the aerosol direct effect into the model simulation reduces the precipitation in the normal rainfall band over North Africa, where precipitation is shifted to the south and the northeast produced by the absorption of sunlight and the subsequent heating of the air column by dust particles. As a result, rainfall is drawn further inland to the northeast. This study represents the first attempt to quantify the climate impact of the aerosol indirect effect using a GCM in connection with A-Train satellite data. The parameterization for the aerosol first indirect effect developed in this study can be readily employed for application to other GCMs. C1 [Gu, Y.; Liou, K. N.; Jiang, J. H.; Su, H.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. [Gu, Y.; Liou, K. N.; Jiang, J. H.; Su, H.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Jiang, J. H.; Su, H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Liu, X.] Pacific NW Natl Lab, Richland, WA 99352 USA. RP Gu, Y (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. EM gu@atmos.ucla.edu RI Liu, Xiaohong/E-9304-2011 OI Liu, Xiaohong/0000-0002-3994-5955 FU NSF [ATM-0924876, AGS-0946315]; DOE [DE-SC0006742, DE-AC06-76RLO 1830]; NASA ACMAP; NASA Aura Science Team; Jet Propulsion Laboratory, California Institute of Technology; NASA FX This research has been supported by NSF Grants ATM-0924876 and AGS-0946315, DOE Grant DE-SC0006742, NASA ACMAP program, NASA Aura Science Team, and the Pacific Northwest National Laboratory operated for DOE by Battelle Memorial Institute under contract DE-AC06-76RLO 1830. J. H. Jiang and H. Su acknowledge support by the Jet Propulsion Laboratory, California Institute of Technology, sponsored by NASA. NR 79 TC 11 Z9 11 U1 0 U2 18 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 4 BP 1667 EP 1679 DI 10.5194/acp-12-1667-2012 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 900GW UT WOS:000300875900002 ER PT J AU Gong, J Wu, DL Eckermann, SD AF Gong, J. Wu, D. L. Eckermann, S. D. TI Gravity wave variances and propagation derived from AIRS radiances SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID QUASI-BIENNIAL OSCILLATION; GENERAL-CIRCULATION; GLOBAL DISTRIBUTION; LOWER STRATOSPHERE; MOMENTUM FLUX; PARAMETERIZATION; CONVECTION; SATELLITE; MODELS; DRAG AB As the first gravity wave (GW) climatology study using nadir-viewing infrared sounders, 50 Atmospheric Infrared Sounder (AIRS) radiance channels are selected to estimate GW variances at pressure levels between 2-100 hPa. The GW variance for each scan in the cross-track direction is derived from radiance perturbations in the scan, independently of adjacent scans along the orbit. Since the scanning swaths are perpendicular to the satellite orbits, which are inclined meridionally at most latitudes, the zonal component of GW propagation can be inferred by differencing the variances derived between the westmost and the eastmost viewing angles. Consistent with previous GW studies using various satellite instruments, monthly mean AIRS variance shows large enhancements over meridionally oriented mountain ranges as well as some islands at winter hemisphere high latitudes. Enhanced wave activities are also found above tropical deep convective regions. GWs prefer to propagate westward above mountain ranges, and eastward above deep convection. AIRS 90 field-of-views (FOVs), ranging from +48 degrees to -48 degrees off nadir, can detect large-amplitude GWs with a phase velocity propagating preferentially at steep angles (e. g., those from orographic and convective sources). The annual cycle dominates the GW variances and the preferred propagation directions for all latitudes. Indication of a weak two-year variation in the tropics is found, which is presumably related to the Quasi-biennial oscillation (QBO). AIRS geometry makes its out-tracks capable of detecting GWs with vertical wavelengths substantially shorter than the thickness of instrument weighting functions. The novel discovery of AIRS capability of observing shallow inertia GWs will expand the potential of satellite GW remote sensing and provide further constraints on the GW drag parameterization schemes in the general circulation models (GCMs). C1 [Gong, J.; Wu, D. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Eckermann, S. D.] USN, Res Lab, Washington, DC 20375 USA. RP Gong, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jie.gong@jpl.nasa.gov RI Gong, Jie/H-2436-2011; Wu, Dong/D-5375-2012 FU NASA; Naval Research Laboratory FX This work is performed at Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. The authors acknowldge the supports from NASA Earth Sciences program and Naval Research Laboratory 6.1 research program. J. Gong is greatful to Moustafa Chahine, Kaoru Sato, Hye-Young Chun, and Stephen Licata for helpful discussions and comments. Two reviewers and editor's comments are highly appreciated. NR 48 TC 27 Z9 27 U1 1 U2 8 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 4 BP 1701 EP 1720 DI 10.5194/acp-12-1701-2012 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 900GW UT WOS:000300875900004 ER PT J AU Allen, DJ Pickering, KE Pinder, RW Henderson, BH Appel, KW Prados, A AF Allen, D. J. Pickering, K. E. Pinder, R. W. Henderson, B. H. Appel, K. W. Prados, A. TI Impact of lightning-NO on eastern United States photochemistry during the summer of 2006 as determined using the CMAQ model SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID OZONE MONITORING INSTRUMENT; AIR-QUALITY MODELS; TROPOSPHERIC NO2; RETRIEVAL ALGORITHM; CONVECTIVE RAINFALL; NATURAL EMISSIONS; DETECTION NETWORK; NITROGEN; VARIABILITY; METEOROLOGY AB A lightning-nitrogen oxide (NO) algorithm is implemented in the Community Multiscale Air Quality Model (CMAQ) and used to evaluate the impact of lightning-NO emissions (LNOx) on tropospheric photochemistry over the United States during the summer of 2006. For a 500 mole per flash lightning-NO source, the mean summertime tropospheric NO2 column agrees with satellite-retrieved columns to within -5 to + 13 %. Temporal fluctuations in the column are moderately well simulated; however, the addition of LNOx does not lead to a better simulation of day-to-day variability. The contribution of lightning-NO to the model column ranges from similar to 10% in the northern US to >45% in the south-central and southeastern US. Lightning-NO adds up to 20 ppbv to upper tropospheric model ozone and 1.5-4.5 ppbv to 8-h maximum surface layer ozone, although, on average, the contribution of LNOx to model surface ozone is 1-2 ppbv less on poor air quality days. LNOx increases wet deposition of oxidized nitrogen by 43% and total deposition of nitrogen by 10 %. This additional deposition reduces the mean magnitude of the CMAQ low-bias in nitrate wet deposition with respect to National Atmospheric Deposition monitors to near zero. Differences in urban/rural biases between model and satellite-retrieved NO2 columns were examined to identify possible problems in model chemistry and/or transport. CMAQ columns were too large over urban areas. Biases at other locations were minor after accounting for the impacts of lightning-NO emissions and the averaging kernel on model columns. In order to obtain an upper bound on the contribution of uncertainties in NOy chemistry to upper tropospheric NOx low biases, sensitivity calculations with updated chemistry were run for the time period of the Intercontinental Chemical Transport Experiment (INTEX-A) field campaign (summer 2004). After adjusting for possible interferences in NO2 measurements and averaging over the entire campaign, these updates reduced 7-9 km biases from 32 to 17% and 9-12 km biases from 57 to 46 %. While these changes lead to better agreement, a considerable unexplained NO2 low-bias remains in the uppermost troposphere. C1 [Allen, D. J.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Pickering, K. E.] NASA Goddard, Atmospher Chem & Dynam Lab, Greenbelt, MD USA. [Pinder, R. W.; Appel, K. W.] US EPA, Atmospher Modeling & Anal Div, Res Triangle Pk, NC 27711 USA. [Henderson, B. H.] Univ N Carolina, Chapel Hill, NC 27515 USA. [Prados, A.] Univ Maryland Baltimore Cty, Joint Ctr Earth Sci Technol JCET, Baltimore, MD 21228 USA. RP Allen, DJ (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. EM allen@atmos.umd.edu RI Pinder, Robert/F-8252-2011; Pickering, Kenneth/E-6274-2012; Allen, Dale/F-7168-2010; OI Pinder, Robert/0000-0001-6390-7126; Allen, Dale/0000-0003-3305-9669; Henderson, Barron/0000-0002-6755-3051 FU Earth Science Research Results project [ROSES07]; NASA FX This work was supported by a ROSES07 Decision Support through Earth Science Research Results project funded by the NASA Applied Sciences Air Quality Program. We thank Tom Pierce for his guidance on this project and his comments on the manuscript. We also thank Ronald Cohen and Eleanor Browne for helpful conversations regarding NOy measurement uncertainties. NR 76 TC 32 Z9 32 U1 4 U2 53 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 4 BP 1737 EP 1758 DI 10.5194/acp-12-1737-2012 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 900GW UT WOS:000300875900006 ER PT J AU Fast, JD Gustafson, WI Berg, LK Shaw, WJ Pekour, M Shrivastava, M Barnard, JC Ferrare, RA Hostetler, CA Hair, JA Erickson, M Jobson, BT Flowers, B Dubey, MK Springston, S Pierce, RB Dolislager, L Pederson, J Zaveri, RA AF Fast, J. D. Gustafson, W. I., Jr. Berg, L. K. Shaw, W. J. Pekour, M. Shrivastava, M. Barnard, J. C. Ferrare, R. A. Hostetler, C. A. Hair, J. A. Erickson, M. Jobson, B. T. Flowers, B. Dubey, M. K. Springston, S. Pierce, R. B. Dolislager, L. Pederson, J. Zaveri, R. A. TI Transport and mixing patterns over Central California during the carbonaceous aerosol and radiative effects study (CARES) SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID SAN-JOAQUIN VALLEY; LOW-LEVEL WINDS; AIR-QUALITY; AIRBORNE LIDAR; ARCTAS-CARB; OZONE; MODEL; QUANTIFICATION; TROPOSPHERE; CHEMISTRY AB We describe the synoptic and regional-scale meteorological conditions that affected the transport and mixing of trace gases and aerosols in the vicinity of Sacramento, California during June 2010 when the Carbonaceous Aerosol and Radiative Effects Study (CARES) was conducted. The meteorological measurements collected by various instruments deployed during the campaign and the performance of the chemistry version of the Weather Research and Forecasting model (WRF-Chem) are both discussed. WRF-Chem was run daily during the campaign to forecast the spatial and temporal variation of carbon monoxide emitted from 20 anthropogenic source regions in California to guide aircraft sampling. The model is shown to reproduce the overall circulations and boundary-layer characteristics in the region, although errors in the upslope wind speed and boundary-layer depth contribute to differences in the observed and simulated carbon monoxide. Thermally-driven upslope flows that transported pollutants from Sacramento over the foothills of the Sierra Nevada occurred every afternoon, except during three periods when the passage of mid-tropospheric troughs disrupted the regional-scale flow patterns. The meteorological conditions after the passage of the third trough were the most favorable for photochemistry and likely formation of secondary organic aerosols. Meteorological measurements and model forecasts indicate that the Sacramento pollutant plume was likely transported over a downwind site that collected trace gas and aerosol measurements during 23 time periods; however, direct transport occurred during only eight of these periods. The model also showed that emissions from the San Francisco Bay area transported by intrusions of marine air contributed a large fraction of the carbon monoxide in the vicinity of Sacramento, suggesting that this source likely affects local chemistry. Contributions from other sources of pollutants, such as those in the Sacramento Valley and San Joaquin Valley, were relatively low. Aerosol layering in the free troposphere was observed during the morning by an airborne Lidar. WRF-Chem forecasts showed that mountain venting processes contributed to aged pollutants aloft in the valley atmosphere that are then entrained into the growing boundary layer the subsequent day. C1 [Fast, J. D.; Gustafson, W. I., Jr.; Berg, L. K.; Shaw, W. J.; Pekour, M.; Shrivastava, M.; Barnard, J. C.; Zaveri, R. A.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Ferrare, R. A.; Hostetler, C. A.; Hair, J. A.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Erickson, M.; Jobson, B. T.] Washington State Univ, Pullman, WA 99164 USA. [Flowers, B.; Dubey, M. K.] Los Alamos Natl Lab, Los Alamos, NM USA. [Springston, S.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Pierce, R. B.] NOAA, Natl Environm Satellite Data & Informat Serv, Madison, WI USA. [Dolislager, L.; Pederson, J.] Calif Air Resources Board, Sacramento, CA USA. RP Fast, JD (reprint author), Pacific NW Natl Lab, Richland, WA 99352 USA. EM jerome.fast@pnl.gov RI Pierce, Robert Bradley/F-5609-2010; Dubey, Manvendra/E-3949-2010; Gustafson, William/A-7732-2008; Berg, Larry/A-7468-2016; OI Pierce, Robert Bradley/0000-0002-2767-1643; Dubey, Manvendra/0000-0002-3492-790X; Gustafson, William/0000-0001-9927-1393; Berg, Larry/0000-0002-3362-9492; Zaveri, Rahul/0000-0001-9874-8807; Jobson, Bertram/0000-0003-1812-9745 FU US DOE at Pacific Northwest National Laboratory (PNNL) [DE-AC06-76RLO 1830]; US Department of Energy, Office of Science, Office of Biological and Environmental Research (OBER), Climate and Environmental Sciences Division FX We thank the numerous scientists, pilots, and other staff that contributed to the data collection during CARES. Data were obtained from the Atmospheric Radiation Measurement (ARM) Program sponsored by the US Department of Energy, Office of Science, Office of Biological and Environmental Research (OBER), Climate and Environmental Sciences Division. We also thank the staff at Northside School in Cool and American River College, particularly Wendy Westsmith and Laduan Smedley, for the use of their facilities. Elaine Chapman provided valuable comments on the content of this paper. This research was supported by the US DOE's Atmospheric Science Research (ASR) Program under Contract DE-AC06-76RLO 1830 at Pacific Northwest National Laboratory (PNNL). PNNL is operated for the US DOE by Battelle Memorial Institute. NR 50 TC 31 Z9 31 U1 3 U2 44 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 4 BP 1759 EP 1783 DI 10.5194/acp-12-1759-2012 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 900GW UT WOS:000300875900007 ER PT J AU Wecht, KJ Jacob, DJ Wofsy, SC Kort, EA Worden, JR Kulawik, SS Henze, DK Kopacz, M Payne, VH AF Wecht, K. J. Jacob, D. J. Wofsy, S. C. Kort, E. A. Worden, J. R. Kulawik, S. S. Henze, D. K. Kopacz, M. Payne, V. H. TI Validation of TES methane with HIPPO aircraft observations: implications for inverse modeling of methane sources SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID TROPOSPHERIC EMISSION SPECTROMETER; ATMOSPHERIC METHANE; LOWER STRATOSPHERE; ERROR ANALYSIS; CH4; SENSITIVITY; VARIABILITY; RETRIEVALS; SCIAMACHY; ADJOINT AB We validate satellite methane observations from the Tropospheric Emission Spectrometer (TES) with 151 aircraft vertical profiles over the Pacific from the HIAPER Pole-to-Pole Observation (HIPPO) program. We find that a collocation window of +/- 750 km and +/- 24 h does not introduce significant error in comparing TES and aircraft profiles. We validate both the TES standard product (V004) and an experimental product with two pieces of information in the vertical (V005). We determine a V004 mean bias of 65.8 ppb and random instrument error of 43.3 ppb. For V005 we determine a mean bias of 42.3 ppb and random instrument error of 26.5 ppb in the upper troposphere, and mean biases (random instrument errors) in the lower troposphere of 28.8 (28.7) and 16.9 (28.9) ppb at high and low latitudes respectively. Even when V005 cannot retrieve two pieces of information it still performs better than V004. An observation system simulation experiment (OSSE) with the GEOS-Chem chemical transport model (CTM) and its adjoint shows that TES V004 has only limited value for constraining methane sources. Our successful validation of V005 encourages its production as a standard retrieval to replace V004. C1 [Wecht, K. J.; Jacob, D. J.; Wofsy, S. C.; Kort, E. A.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Worden, J. R.; Kulawik, S. S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Henze, D. K.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA. [Kopacz, M.] Princeton Univ, Woodrow Wilson Sch Publ & Int Affairs, Princeton, NJ 08544 USA. [Payne, V. H.] Atmospher Environm Res, Lexington, MA USA. RP Wecht, KJ (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. EM wecht@fas.harvard.edu RI Payne, Vivienne/D-9713-2012; Kort, Eric/F-9942-2012; Chem, GEOS/C-5595-2014 OI Kort, Eric/0000-0003-4940-7541; FU US National Science Foundation; NASA FX This work was supported by the US National Science Foundation under the HIPPO Program, by the NASA Atmospheric Composition Modeling and Analysis Program, and by a NASA Earth System Science Fellowship to KJW. NR 42 TC 38 Z9 38 U1 1 U2 23 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 4 BP 1823 EP 1832 DI 10.5194/acp-12-1823-2012 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 900GW UT WOS:000300875900010 ER PT J AU Wild, O Fiore, AM Shindell, DT Doherty, RM Collins, WJ Dentener, FJ Schultz, MG Gong, S MacKenzie, IA Zeng, G Hess, P Duncan, BN Bergmann, DJ Szopa, S Jonson, JE Keating, TJ Zuber, A AF Wild, O. Fiore, A. M. Shindell, D. T. Doherty, R. M. Collins, W. J. Dentener, F. J. Schultz, M. G. Gong, S. MacKenzie, I. A. Zeng, G. Hess, P. Duncan, B. N. Bergmann, D. J. Szopa, S. Jonson, J. E. Keating, T. J. Zuber, A. TI Modelling future changes in surface ozone: a parameterized approach SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID TROPOSPHERIC OZONE; CLIMATE-CHANGE; AIR-QUALITY; EMISSIONS; POLLUTION; GASES; STABILIZATION; TRANSPORT; AEROSOLS; PATHWAY AB This study describes a simple parameterization to estimate regionally averaged changes in surface ozone due to past or future changes in anthropogenic precursor emissions based on results from 14 global chemistry transport models. The method successfully reproduces the results of full simulations with these models. For a given emission scenario it provides the ensemble mean surface ozone change, a regional source attribution for each change, and an estimate of the associated uncertainty as represented by the variation between models. Using the Representative Concentration Pathway (RCP) emission scenarios as an example, we show how regional surface ozone is likely to respond to emission changes by 2050 and how changes in precursor emissions and atmospheric methane contribute to this. Surface ozone changes are substantially smaller than expected with the SRES A1B, A2 and B2 scenarios, with annual global mean reductions of as much as 2 ppb by 2050 vs. increases of 4-6 ppb under SRES, and this reflects the assumptions of more stringent precursor emission controls under the RCP scenarios. We find an average difference of around 5 ppb between the outlying RCP 2.6 and RCP 8.5 scenarios, about 75% of which can be attributed to differences in methane abundance. The study reveals the increasing importance of limiting atmospheric methane growth as emissions of other precursors are controlled, but highlights differences in modelled ozone responses to methane changes of as much as a factor of two, indicating that this remains a major uncertainty in current models. C1 [Wild, O.] Univ Lancaster, Lancaster Environm Ctr, Lancaster, England. [Fiore, A. M.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Shindell, D. T.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Shindell, D. T.] Columbia Univ, New York, NY USA. [Doherty, R. M.; MacKenzie, I. A.] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9YL, Midlothian, Scotland. [Collins, W. J.] Met Off Hadley Ctr, Exeter, Devon, England. [Dentener, F. J.] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21020 Ispra, Italy. [Schultz, M. G.] Forschungszentrum Julich, IEK 8, D-52425 Julich, Germany. [Gong, S.] Environm Canada, Sci & Technol Branch, Toronto, ON, Canada. [Zeng, G.] Natl Inst Water & Atmospher Res, Lauder, New Zealand. [Hess, P.] Cornell Univ, Dept Biol & Environm Engn, Ithaca, NY USA. [Duncan, B. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bergmann, D. J.] Lawrence Livermore Natl Lab, Atmospher Earth & Energy Div, Livermore, CA USA. [Szopa, S.] Lab Sci Climat & Environm, Gif Sur Yvette, France. [Jonson, J. E.] Norwegian Meteorol Inst, Oslo, Norway. [Keating, T. J.] US EPA, Off Policy Anal & Review, Washington, DC 20460 USA. [Zuber, A.] Commiss European Communities, Directorate Gen Environm, B-1049 Brussels, Belgium. RP Wild, O (reprint author), Univ Lancaster, Lancaster Environm Ctr, Lancaster, England. EM o.wild@lancaster.ac.uk RI Bergmann, Daniel/F-9801-2011; Wild, Oliver/A-4909-2009; Collins, William/A-5895-2010; Shindell, Drew/D-4636-2012; Duncan, Bryan/A-5962-2011; Szopa, Sophie/F-8984-2010; Schultz, Martin/I-9512-2012; mackenzie, ian/E-9320-2013; Hess, Peter/M-3145-2015 OI Bergmann, Daniel/0000-0003-4357-6301; Wild, Oliver/0000-0002-6227-7035; Collins, William/0000-0002-7419-0850; Szopa, Sophie/0000-0002-8641-1737; Schultz, Martin/0000-0003-3455-774X; Hess, Peter/0000-0003-2439-3796 NR 35 TC 48 Z9 48 U1 4 U2 43 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 4 BP 2037 EP 2054 DI 10.5194/acp-12-2037-2012 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 900GW UT WOS:000300875900023 ER PT J AU Parrington, M Palmer, PI Henze, DK Tarasick, DW Hyer, EJ Owen, RC Helmig, D Clerbaux, C Bowman, KW Deeter, MN Barratt, EM Coheur, PF Hurtmans, D Jiang, Z George, M Worden, JR AF Parrington, M. Palmer, P. I. Henze, D. K. Tarasick, D. W. Hyer, E. J. Owen, R. C. Helmig, D. Clerbaux, C. Bowman, K. W. Deeter, M. N. Barratt, E. M. Coheur, P. -F. Hurtmans, D. Jiang, Z. George, M. Worden, J. R. TI The influence of boreal biomass burning emissions on the distribution of tropospheric ozone over North America and the North Atlantic during 2010 SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID SURFACE EMISSIONS; IASI MEASUREMENTS; CARBON-MONOXIDE; ZONAL STRUCTURE; ERROR ANALYSIS; LIGHTNING NOX; TROPICAL O-3; GEOS-CHEM; SPECTROMETER; SATELLITE AB We have analysed the sensitivity of the tropospheric ozone distribution over North America and the North Atlantic to boreal biomass burning emissions during the summer of 2010 using the GEOS-Chem 3-D global tropospheric chemical transport model and observations from in situ and satellite instruments. We show that the model ozone distribution is consistent with observations from the Pico Mountain Observatory in the Azores, ozonesondes across Canada, and the Tropospheric Emission Spectrometer (TES) and Infrared Atmospheric Sounding Instrument (IASI) satellite instruments. Mean biases between the model and observed ozone mixing ratio in the free troposphere were less than 10 ppbv. We used the adjoint of GEOS-Chemto show the model ozone distribution in the free troposphere over Maritime Canada is largely sensitive to NOx emissions from biomass burning sources in Central Canada, lightning sources in the central US, and anthropogenic sources in the eastern US and southeastern Canada. We also used the adjoint of GEOS-Chem to evaluate the Fire Locating And Monitoring of Burning Emissions (FLAMBE) inventory through assimilation of CO observations from the Measurements Of Pollution In The Troposphere (MOPITT) satellite instrument. The CO inversion showed that, on average, the FLAMBE emissions needed to be reduced to 89% of their original values, with scaling factors ranging from 12% to 102 %, to fit the MOPITT observations in the boreal regions. Applying the CO scaling factors to all species emitted from boreal biomass burning sources led to a decrease of the model tropospheric distributions of CO, PAN, and NOx by as much as -20 ppbv, -50 pptv, and -20 pptv respectively. The modification of the biomass burning emission estimates reduced the model ozone distribution by approximately -3 ppbv (-8%) and on average improved the agreement of the model ozone distribution compared to the observations throughout the free troposphere, reducing the mean model bias from 5.5 to 4.0 ppbv for the Pico Mountain Observatory, 3.0 to 0.9 ppbv for ozonesondes, 2.0 to 0.9 ppbv for TES, and 2.8 to 1.4 ppbv for IASI. C1 [Parrington, M.; Palmer, P. I.; Barratt, E. M.] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland. [Henze, D. K.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA. [Tarasick, D. W.] Environm Canada, Air Qual Res Div, Downsview, ON, Canada. [Hyer, E. J.] USN, Res Lab, Marine Meteorol Div, Monterey, CA USA. [Owen, R. C.] Michigan Technol Univ, Dept Civil & Environm Engn, Houghton, MI 49931 USA. [Helmig, D.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Clerbaux, C.; George, M.] Univ Versailles St Quentin, Univ Paris 06, UPMC, CNRS INSU,LATMOS IPSL, Paris, France. [Bowman, K. W.; Worden, J. R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Deeter, M. N.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. [Coheur, P. -F.; Hurtmans, D.] Univ Libre Brussels, Serv Chim Quant & Photophys, Brussels, Belgium. [Jiang, Z.] Univ Toronto, Dept Phys, Toronto, ON, Canada. RP Parrington, M (reprint author), Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland. EM mark.parrington@ed.ac.uk RI clerbaux, cathy/I-5478-2013; Deeter, Merritt/O-6078-2016; Parrington, Mark/E-7148-2013; Chem, GEOS/C-5595-2014; Hyer, Edward/E-7734-2011; Palmer, Paul/F-7008-2010 OI Deeter, Merritt/0000-0002-3555-0518; Tarasick, David/0000-0001-9869-0692; Parrington, Mark/0000-0003-4313-6218; Hyer, Edward/0000-0001-8636-2026; FU Natural Environment Research Council [NE/F017391/1]; NASA [NNH07AF47I]; Nuffield Foundation; Leverhulme Philip Prize; US National Science Foundation [AGS1011968]; F.R.S.-FNRS; Belgian State Federal Office for Scientific, Technical and Cultural Affairs; European Space Agency (ESA); Actions de Recherche Concertee' (Communaute Francaise de Belgique) FX The BORTAS project is funded by the Natural Environment Research Council under grant NE/F017391/1. DKH is supported through the NASA New Investigator Program. EJH participation was funded by NASA IDS award #NNH07AF47I. PIP acknowledges funding for EMB from the Nuffield Foundation undergraduate bursary for summer 2010 and from Leverhulme Philip Prize for the summer of 2011. Measurements at the Pico Mountain Observatory were funded by the US National Science Foundation award #AGS1011968. PFC is Research Associate (Chercheur Qualifie) with F.R.S.-FNRS. The research in Belgium was funded by the F.R.S.-FNRS, the Belgian State Federal Office for Scientific, Technical and Cultural Affairs and the European Space Agency (ESA-Prodex arrangements). Financial support by the 'Actions de Recherche Concertee' (Communaute Francaise de Belgique) is also acknowledged. IASI has been developed and built under the responsibility of the Centre National des Etudes Spatiales (CNES, France). The IASI L1C data are distributed in near real time by Eumetsat through the Eumetcast dissemination system. The authors acknowledge the Ether French atmospheric database (http://ether.ipsl.jussieu.fr) for providing the IASI data. MOPITT CO and TES ozone data were obtained from the NASA Langley Research Center Atmospheric Science Data Center. NR 66 TC 41 Z9 42 U1 2 U2 16 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 4 BP 2077 EP 2098 DI 10.5194/acp-12-2077-2012 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 900GW UT WOS:000300875900025 ER PT J AU Reid, JS Xian, P Hyer, EJ Flatau, MK Ramirez, EM Turk, FJ Sampson, CR Zhang, C Fukada, EM Maloney, ED AF Reid, J. S. Xian, P. Hyer, E. J. Flatau, M. K. Ramirez, E. M. Turk, F. J. Sampson, C. R. Zhang, C. Fukada, E. M. Maloney, E. D. TI Multi-scale meteorological conceptual analysis of observed active fire hotspot activity and smoke optical depth in the Maritime Continent SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID MADDEN-JULIAN OSCILLATION; NINO-SOUTHERN-OSCILLATION; INDONESIAN FOREST-FIRES; TROPICAL INDIAN-OCEAN; EL-NINO; TEMPORAL RESOLUTION; FORECAST MODEL; KELVIN WAVES; HAZE EPISODE; DIPOLE MODE AB Much research and speculation exists about the meteorological and climatological impacts of biomass burning in the Maritime Continent (MC) of Indonesia and Malaysia, particularly during El Nino events. However, the MC hosts some of the world's most complicated meteorology, and we wish to understand how tropical phenomena at a range of scales influence observed burning activity. Using Moderate Resolution Imaging Spectroradiometer (MODIS) derived active fire hotspot patterns coupled with aerosol data assimilation products, satellite based precipitation, and meteorological indices, the meteorological context of observed fire prevalence and smoke optical depth in the MC are examined. Relationships of burning and smoke transport to such meteorological and climatic factors as the interannual El Nino-Southern Oscillation (ENSO), El Nino Modoki, Indian Ocean Dipole (IOD), the seasonal migration of the Intertropical Convergence Zone, the 30-90 day Madden Julian Oscillation (MJO), tropical waves, tropical cyclone activity, and diurnal convection were investigated. A conceptual model of how all of the differing meteorological scales affect fire activity is presented. Each island and its internal geography have different sensitivities to these factors which are likely relatable to precipitation patterns and land use practices. At the broadest scales as previously reported, we corroborate ENSO is indeed the largest factor. However, burning is also enhanced by periods of El Nino Modoki. Conversely, IOD influences are unclear. While interannual phenomena correlate to total seasonal burning, the MJO largely controls when visible burning occurs. High frequency phenomena which are poorly constrained in models such as diurnal convection and tropical cyclone activity also have an impact which cannot be ignored. Finally, we emphasize that these phenomena not only influence burning, but also the observability of burning, further complicating our ability to assign reasonable emissions. C1 [Reid, J. S.; Hyer, E. J.; Flatau, M. K.; Sampson, C. R.] USN, Marine Meteorol Div, Res Lab, Monterey, CA USA. [Ramirez, E. M.] Univ Utah, Dept Atmospher Sci, Salt Lake City, UT USA. [Turk, F. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Zhang, C.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Fukada, E. M.] Joint Typhoon Warning Ctr, Honolulu, HI USA. [Maloney, E. D.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RP Reid, JS (reprint author), USN, Marine Meteorol Div, Res Lab, Monterey, CA USA. EM jeffrey.reid@nrlmry.navy.mil RI Reid, Jeffrey/B-7633-2014; Hyer, Edward/E-7734-2011; Maloney, Eric/A-9327-2008 OI Reid, Jeffrey/0000-0002-5147-7955; Hyer, Edward/0000-0001-8636-2026; Maloney, Eric/0000-0002-2660-2611 FU NRL Base; NASA; Office of Naval Research [32] FX We are grateful to many of our 7SEAS partners for helpful discussions, and in particular Jukka Miettinen of the National University of Singapore Center for Remote Imaging. Sensing and Processing. We are also grateful to Song Yang, NRL, for helpful discussions on diurnal precipitation in the region. This paper was supported by the NRL Base Program, NASA Interdisciplinary Science Program, and the Office of Naval Research Code 32. NR 141 TC 40 Z9 40 U1 1 U2 23 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 4 BP 2117 EP 2147 DI 10.5194/acp-12-2117-2012 PG 31 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 900GW UT WOS:000300875900027 ER PT J AU Godfrey, LEH Bignall, H Tingay, S Harvey-Smith, L Kramer, M Burke-Spolaor, S Miller-Jones, JCA Johnston-Hollitt, M Ekers, R Gulyaev, S AF Godfrey, L. E. H. Bignall, H. Tingay, S. Harvey-Smith, L. Kramer, M. Burke-Spolaor, S. Miller-Jones, J. C. A. Johnston-Hollitt, M. Ekers, R. Gulyaev, S. TI Science at Very High Angular Resolution with the Square Kilometre Array SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE telescopes ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE BINARIES; X-RAY BINARIES; FAST RADIO TRANSIENTS; STRONG-FIELD TESTS; STAR-FORMATION; GRAVITATIONAL-WAVES; COSMIC MAGNETISM; GALAXY FORMATION; NEARBY GALAXIES AB Preliminary specifications for the Square Kilometre Array (SKA) call for 25% of the total collecting area of the dish array to be located at distances greater than 180 km from the core, with a maximum baseline of at least 3000 km. The array will provide angular resolution theta less than or similar to 40-2 mas at 0.5-10 GHz with image sensitivity reaching less than or similar to 50 nJy beam(-1) in an 8-hour integration with 500-MHz bandwidth. Given these specifications, the high-angular-resolution component of the SKA will be capable of detecting brightness temperatures less than or similar to 200 K with milliarcsecond-scale angular resolution. The aim of this article is to bring together in one place a discussion of the broad range of new and important high-angular-resolution science that will be enabled by the SKA, and in doing so, address the merits of long baselines as part of the SKA. We highlight the fact that high angular resolution requiring baselines greater than 1000 km provides a rich science case with projects from many areas of astrophysics, including important contributions to key SKA science. C1 [Godfrey, L. E. H.; Bignall, H.; Tingay, S.; Miller-Jones, J. C. A.; Ekers, R.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Harvey-Smith, L.; Burke-Spolaor, S.; Ekers, R.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 2121, Australia. [Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kramer, M.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Burke-Spolaor, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Gulyaev, S.] Auckland Univ Technol, Inst Radio Astron & Space Res, Auckland, New Zealand. RP Godfrey, LEH (reprint author), Curtin Univ Technol, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia. EM L.Godfrey@curtin.edu.au RI Johnston-Hollitt, Melanie/B-1803-2013; Godfrey, Leith/B-5283-2013; Tingay, Steven/B-5271-2013; Bignall, Hayley/B-2867-2013; Miller-Jones, James/B-2411-2013 OI Bignall, Hayley/0000-0001-6247-3071; Miller-Jones, James/0000-0003-3124-2814 NR 92 TC 8 Z9 8 U1 0 U2 3 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1323-3580 EI 1448-6083 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PY 2012 VL 29 IS 1 BP 42 EP 53 DI 10.1071/AS11050 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904XU UT WOS:000301233000005 ER PT J AU Zhang, H Sibeck, DG Zong, QG McFadden, JP Larson, D Glassmeier, KH Angelopoulos, V AF Zhang, H. Sibeck, D. G. Zong, Q. -G. McFadden, J. P. Larson, D. Glassmeier, K. -H. Angelopoulos, V. TI Global magnetospheric response to an interplanetary shock: THEMIS observations SO ANNALES GEOPHYSICAE LA English DT Article DE Interplanetary physics; Interplanetary shocks; Magnetospheric physics; Magnetospheric configuration and dynamics; Solar wind-magnetosphere interactions ID ION-CYCLOTRON WAVES; BOW SHOCK; PLASMASPHERIC PLUMES; PARTICLE INTERACTIONS; PLASMA INSTRUMENT; OMEGA-HE; MAGNETOPAUSE; PULSATIONS; GENERATION; DENSITY AB We investigate the global response of the geospace plasma environment to an interplanetary (IP) shock at similar to 02:24 UT on 28 May 2008 from multiple THEMIS spacecraft observations in the magnetosheath (THEMIS B and C), the mid-afternoon magnetosphere (THEMIS A), and the dusk magnetosphere (THEMIS D and E). The interaction of the transmitted IP shock with the magnetosphere has global effects. Consequently, it can affect geospace plasma significantly. After interacting with the bow shock, the IP shock transmitted a fast shock and a discontinuity which propagated through the magnetosheath toward the Earth at speeds of 301 km s(-1) and 137 km s(-1), respectively. THEMIS A observations indicate that the IP shock changed the properties of a plasmaspheric plume significantly. The plasmaspheric plume density increased rapidly from 10 to 100 cm(-3) in 4 min and the ion distribution changed from an isotropic to a strongly anisotropic distribution. Electromagnetic ion cyclotron (EMIC) waves observed by THEMIS A are most likely excited by the anisotropic ion distributions caused by the IP shock impact. THEMIS A, but not D or E, observed a plasmaspheric plume in the dayside magnetosphere. Multiple spacecraft observations indicate that the dawn-side edge of the plasmaspheric plume was located between THEMIS A and D (or E). C1 [Zhang, H.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zong, Q. -G.] Univ Massachusetts, Ctr Atmospher Res, Lowell, MA USA. [Zong, Q. -G.] Peking Univ, Inst Space Phys & Appl Technol, Beijing 100871, Peoples R China. [McFadden, J. P.; Larson, D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Glassmeier, K. -H.] TU Braunschweig, Inst Geopys & Extraterr Phys, Braunschweig, Germany. [Angelopoulos, V.] IGPP ESS UCLA, Los Angeles, CA 90095 USA. RP Zhang, H (reprint author), Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. EM hzhang@gi.alaska.edu RI Sibeck, David/D-4424-2012 FU Alaska NASA EPSCoR; German Ministerium fur Wirtschaft und Technologie; Deutsches Zentrum fur Luft- und Raumfahrt [50OC1001] FX This work is partly supported by the Alaska NASA EPSCoR Program. KHG was financially supported by the German Ministerium fur Wirtschaft und Technologie and the Deutsches Zentrum fur Luft- und Raumfahrt under grant 50OC1001. NR 51 TC 8 Z9 8 U1 0 U2 2 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 0992-7689 EI 1432-0576 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2012 VL 30 IS 2 BP 379 EP 387 DI 10.5194/angeo-30-379-2012 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 900HF UT WOS:000300876900009 ER PT J AU Abbasi, R Abdou, Y Abu-Zayyad, T Adams, J Aguilar, JA Ahlers, M Andeen, K Auffenberg, J Bai, X Baker, M Barwick, SW Bay, R Alba, JLB Beattie, K Beatty, JJ Bechet, S Becker, JK Becker, KH Benabderrahmane, ML BenZvi, S Berdermann, J Berghaus, P Berley, D Bernardini, E Bertrand, D Besson, DZ Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bose, D Boser, S Botner, O Braun, J Brown, AM Buitink, S Carson, M Chirkin, D Christy, B Clem, J Clevermann, F Cohen, S Colnard, C Cowen, DF D'Agostino, MV Danninger, M Daughhetee, J Davis, JC De Clercq, C Demirors, L Denger, T Depaepe, O Descamps, F Desiati, P de Vries-Uiterweerd, G DeYoung, T Diaz-Velez, JC Dierckxsens, M Dreyer, J Dumm, JP Ehrlich, R Eisch, J Ellsworth, RW Engdegard, O Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feusels, T Filimonov, K Finley, C Fischer-Wasels, T Foerster, MM Fox, BD Franckowiak, A Franke, R Gaisser, TK Gallagher, J Geisler, M Gerhardt, L Gladstone, L Glusenkamp, T Goldschmidt, A Goodman, JA Grant, D Griesel, T Gross, A Grullon, S Gurtner, M Ha, C Hallgren, A Halzen, F Han, K Hanson, K Heinen, D Helbing, K Herquet, P Hickford, S Hill, GC Hoffman, KD Homeier, A Hoshina, K Hubert, D Huelsnitz, W Hulss, JP Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobsen, J Japaridze, GS Johansson, H Joseph, JM Kampert, KH Kappes, A Karg, T Karle, A Kelley, JL Kenny, P Kiryluk, J Kislat, F Klein, SR Kohne, JH Kohnen, G Kolanoski, H Kopke, L Kopper, S Koskinen, DJ Kowalski, M Kowarik, T Krasberg, M Krings, T Kroll, G Kuehn, K Kuwabara, T Labare, M Lafebre, S Laihem, K Landsman, H Larson, MJ Lauer, R Lunemann, J Madsen, J Majumdar, P Marotta, A Maruyama, R Mase, K Matis, HS Meagher, K Merck, M Meszaros, P Meures, T Middell, E Milke, N Miller, J Montaruli, T Morse, R Movit, SM Nahnhauer, R Nam, JW Naumann, U Niessen, P Nygren, DR Odrowski, S Olivas, A Olivo, M O'Murchadha, A Ono, M Panknin, S Paul, L de los Heros, CP Petrovic, J Piegsa, A Pieloth, D Porrata, R Posselt, J Price, PB Prikockis, M Przybylski, GT Rawlins, K Redl, P Resconi, E Rhode, W Ribordy, M Rizzo, A Rodrigues, JP Roth, P Rothmaier, F Rott, C Ruhe, T Rutledge, D Ruzybayev, B Ryckbosch, D Sander, HG Santander, M Sarkar, S Schatto, K Schmidt, T Schonwald, A Schukraft, A Schultes, A Schulz, O Schunck, M Seckel, D Semburg, B Seo, SH Sestayo, Y Seunarine, S Silvestri, A Slipak, A Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stephens, G Stezelberger, T Stokstad, RG Stossl, A Stoyanov, S Strahler, EA Straszheim, T Stur, M Sullivan, GW Swillens, Q Taavola, H Taboada, I Tamburro, A Tepe, A Ter-Antonyan, S Tilav, S Toale, PA Toscano, S Tosi, D Turcan, D van Eijndhoven, N Vandenbroucke, J Van Overloop, A van Santen, J Vehring, M Voge, M Walck, C Waldenmaier, T Wallraff, M Walter, M Weaver, C Wendt, C Westerhoff, S Whitehorn, N Wiebe, K Wiebusch, CH Williams, DR Wischnewski, R Wissing, H Wolf, M Woschnagg, K Xu, C Xu, XW Yanez, JP Yodh, G Yoshida, S Zarzhitsk, P AF Abbasi, R. Abdou, Y. Abu-Zayyad, T. Adams, J. Aguilar, J. A. Ahlers, M. Andeen, K. Auffenberg, J. Bai, X. Baker, M. Barwick, S. W. Bay, R. Alba, J. L. Bazo Beattie, K. Beatty, J. J. Bechet, S. Becker, J. K. Becker, K. -H. Benabderrahmane, M. L. BenZvi, S. Berdermann, J. Berghaus, P. Berley, D. Bernardini, E. Bertrand, D. Besson, D. Z. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bose, D. Boeser, S. Botner, O. Braun, J. Brown, A. M. Buitink, S. Carson, M. Chirkin, D. Christy, B. Clem, J. Clevermann, F. Cohen, S. Colnard, C. Cowen, D. F. D'Agostino, M. V. Danninger, M. Daughhetee, J. Davis, J. C. De Clercq, C. Demiroers, L. Denger, T. Depaepe, O. Descamps, F. Desiati, P. de Vries-Uiterweerd, G. DeYoung, T. Diaz-Velez, J. C. Dierckxsens, M. Dreyer, J. Dumm, J. P. Ehrlich, R. Eisch, J. Ellsworth, R. W. Engdegard, O. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feusels, T. Filimonov, K. Finley, C. Fischer-Wasels, T. Foerster, M. M. Fox, B. D. Franckowiak, A. Franke, R. Gaisser, T. K. Gallagher, J. Geisler, M. Gerhardt, L. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Goodman, J. A. Grant, D. Griesel, T. Gross, A. Grullon, S. Gurtner, M. Ha, C. Hallgren, A. Halzen, F. Han, K. Hanson, K. Heinen, D. Helbing, K. Herquet, P. Hickford, S. Hill, G. C. Hoffman, K. D. Homeier, A. Hoshina, K. Hubert, D. Huelsnitz, W. Huelss, J. -P. Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jacobsen, J. Japaridze, G. S. Johansson, H. Joseph, J. M. Kampert, K. -H. Kappes, A. Karg, T. Karle, A. Kelley, J. L. Kenny, P. Kiryluk, J. Kislat, F. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koepke, L. Kopper, S. Koskinen, D. J. Kowalski, M. Kowarik, T. Krasberg, M. Krings, T. Kroll, G. Kuehn, K. Kuwabara, T. Labare, M. Lafebre, S. Laihem, K. Landsman, H. Larson, M. J. Lauer, R. Luenemann, J. Madsen, J. Majumdar, P. Marotta, A. Maruyama, R. Mase, K. Matis, H. S. Meagher, K. Merck, M. Meszaros, P. Meures, T. Middell, E. Milke, N. Miller, J. Montaruli, T. Morse, R. Movit, S. M. Nahnhauer, R. Nam, J. W. Naumann, U. Niessen, P. Nygren, D. R. Odrowski, S. Olivas, A. Olivo, M. O'Murchadha, A. Ono, M. Panknin, S. Paul, L. de los Heros, C. Perez Petrovic, J. Piegsa, A. Pieloth, D. Porrata, R. Posselt, J. Price, P. B. Prikockis, M. Przybylski, G. T. Rawlins, K. Redl, P. Resconi, E. Rhode, W. Ribordy, M. Rizzo, A. Rodrigues, J. P. Roth, P. Rothmaier, F. Rott, C. Ruhe, T. Rutledge, D. Ruzybayev, B. Ryckbosch, D. Sander, H. -G. Santander, M. Sarkar, S. Schatto, K. Schmidt, T. Schoenwald, A. Schukraft, A. Schultes, A. Schulz, O. Schunck, M. Seckel, D. Semburg, B. Seo, S. H. Sestayo, Y. Seunarine, S. Silvestri, A. Slipak, A. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stephens, G. Stezelberger, T. Stokstad, R. G. Stoessl, A. Stoyanov, S. Strahler, E. A. Straszheim, T. Stuer, M. Sullivan, G. W. Swillens, Q. Taavola, H. Taboada, I. Tamburro, A. Tepe, A. Ter-Antonyan, S. Tilav, S. Toale, P. A. Toscano, S. Tosi, D. Turcan, D. van Eijndhoven, N. Vandenbroucke, J. Van Overloop, A. van Santen, J. Vehring, M. Voge, M. Walck, C. Waldenmaier, T. Wallraff, M. Walter, M. Weaver, Ch Wendt, C. Westerhoff, S. Whitehorn, N. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wischnewski, R. Wissing, H. Wolf, M. Woschnagg, K. Xu, C. Xu, X. W. Yanez, J. P. Yodh, G. Yoshida, S. Zarzhitsk, P. TI Background studies for acoustic neutrino detection at the South Pole SO ASTROPARTICLE PHYSICS LA English DT Article DE Acoustic neutrino detection; Absolute noise level; Neutrino flux limit ID TELESCOPE; SIGNALS; WATER AB The detection of acoustic signals from ultra-high energy neutrino interactions is a promising method to measure the flux of cosmogenic neutrinos expected on Earth. The energy threshold for this process depends strongly on the absolute noise level in the target material. The South Pole Acoustic Test Setup (SPATS), deployed in the upper part of four boreholes of the IceCube Neutrino Observatory, has monitored the noise in Antarctic ice at the geographic South Pole for more than two years down to 500 m depth. The noise is very stable and Gaussian distributed. Lacking an in situ calibration up to now, laboratory measurements have been used to estimate the absolute noise level in the 10-50 kHz frequency range to be smaller than 20 mPa. Using a threshold trigger, sensors of the South Pole Acoustic Test Setup registered acoustic events in the IceCube detector volume and its vicinity. Acoustic signals from refreezing IceCube holes and from anthropogenic sources have been used to test the localization of acoustic events. An upper limit on the neutrino flux at energies E-v>10(11) GeV is derived from acoustic data taken over eight months. (C) 2011 Elsevier B.V. All rights reserved. C1 [Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Franke, R.; Han, K.; Kislat, F.; Lauer, R.; Majumdar, P.; Middell, E.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Tosi, D.; Walter, M.; Wischnewski, R.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany. [Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Geisler, M.; Gluesenkamp, T.; Heinen, D.; Huelss, J. -P.; Krings, T.; Laihem, K.; Meures, T.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Toale, P. A.; Williams, D. R.; Zarzhitsk, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Rawlins, K.] Univ Alaska, Dept Phys & Astron, Anchorage, AK 99508 USA. [Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. 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H.; Walck, C.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Lafebre, S.; Larson, M. J.; Prikockis, M.; Rutledge, D.; Slipak, A.; Stephens, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; de los Heros, C. Perez; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Auffenberg, J.; Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Kopper, S.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Montaruli, T.] Univ Bari, I-70126 Bari, Italy. [Montaruli, T.] Sezione Ist Nazl Fis Nucl, Dipartimento Fis, I-70126 Bari, Italy. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Berdermann, J (reprint author), DESY, D-15735 Zeuthen, Germany. EM jens.berdermann@desy.de; rolf.nahnhauer@desy.de RI Taavola, Henric/B-4497-2011; Hallgren, Allan/A-8963-2013; Botner, Olga/A-9110-2013; Tjus, Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014; Koskinen, David/G-3236-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011; Wiebusch, Christopher/G-6490-2012; Kowalski, Marek/G-5546-2012; Tamburro, Alessio/A-5703-2013 OI Schukraft, Anne/0000-0002-9112-5479; Perez de los Heros, Carlos/0000-0002-2084-5866; Taavola, Henric/0000-0002-2604-2810; Buitink, Stijn/0000-0002-6177-497X; Carson, Michael/0000-0003-0400-7819; Hubert, Daan/0000-0002-4365-865X; Benabderrahmane, Mohamed Lotfi/0000-0003-4410-5886; Auffenberg, Jan/0000-0002-1185-9094; Koskinen, David/0000-0002-0514-5917; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Ter-Antonyan, Samvel/0000-0002-5788-1369; Wiebusch, Christopher/0000-0002-6418-3008; FU US National Science Foundation-Office of Polar Programs; US National Science Foundation-Physics Division; University of Wisconsin Alumni Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin - Madison; Open Science Grid (OSG) grid infrastructure; US Department of Energy; National Energy Research Scientific Computing Center; Louisiana Optical Network Initiative (LONI) grid computing resources; National Science and Engineering Research Council of Canada; Swedish Research Council; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Research Department of Plasmas; Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO; Flanders Institute; Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, NewZealand; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland; EU; Capes Foundation, Ministry of Education of Brazil FX We acknowledge the support from the following agencies: US National Science Foundation-Office of Polar Programs, US National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin - Madison, the Open Science Grid (OSG) grid infrastructure; US Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; National Science and Engineering Research Council of Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, NewZealand; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; A. Gross acknowledges support by the EU Marie Curie OIF Program; J.P. Rodrigues acknowledges support by the Capes Foundation, Ministry of Education of Brazil. NR 25 TC 9 Z9 9 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 J9 ASTROPART PHYS JI Astropart Phys. PD JAN PY 2012 VL 35 IS 6 BP 312 EP 324 DI 10.1016/j.astropartphys.2011.09.004 PG 13 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 898RZ UT WOS:000300760800004 ER PT J AU Ackermann, M Ajello, M Allafort, A Atwood, WB Axelsson, M Baldini, L Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Berenji, B Bloom, ED Bonamente, E Borgland, AW Bouvier, A Bregeon, J Brez, A Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cecchi, C Charles, E Chekhtman, A Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Cutini, S de Palma, F Dermer, CD Digel, SW Silva, EDE Drell, PS Drlica-Wagner, A Dubois, R Enoto, T Falletti, L Favuzzi, C Fegan, SJ Focke, WB Fortin, P Fukazawa, Y Funk, S Fusco, P Gargano, F Gehrels, N Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Hadasch, D Hayashida, M Hays, E Hughes, RE Johannesson, G Johnson, AS Johnson, TJ Kamae, T Katagiri, H Kataoka, J Knodlseder, J Kuss, M Lande, J Latronico, L Lee, SH Longo, F Loparco, F Lovellette, MN Lubrano, P Madejski, GM Mazziotta, MN McEnery, JE Michelson, PF Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nakamori, T Naumann-Godo, M Nolan, PL Norris, JP Nuss, E Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Ozaki, M Paneque, D Panetta, JH Parent, D Pesce-Rollins, M Pierbattista, M Piron, F Raino, S Rando, R Razzano, M Reimer, A Reimer, O Reposeur, T Ritz, S Rochester, LS Sgro, C Siskind, EJ Smith, PD Spandre, G Spinelli, P Suson, DJ Takahashi, H Tanaka, T Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tosti, G Troja, E Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vilchez, N Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Yang, Z Zimmer, S AF Ackermann, M. Ajello, M. Allafort, A. Atwood, W. B. Axelsson, M. Baldini, L. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Berenji, B. Bloom, E. D. Bonamente, E. Borgland, A. W. Bouvier, A. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cecchi, C. Charles, E. Chekhtman, A. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Cutini, S. de Palma, F. Dermer, C. D. Digel, S. W. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Dubois, R. Enoto, T. Falletti, L. Favuzzi, C. Fegan, S. J. Focke, W. B. Fortin, P. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gehrels, N. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Hadasch, D. Hayashida, M. Hays, E. Hughes, R. E. Johannesson, G. Johnson, A. S. Johnson, T. J. Kamae, T. Katagiri, H. Kataoka, J. Knoedlseder, J. Kuss, M. Lande, J. Latronico, L. Lee, S. -H. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Madejski, G. M. Mazziotta, M. N. McEnery, J. E. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Naumann-Godo, M. Nolan, P. L. Norris, J. P. Nuss, E. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Panetta, J. H. Parent, D. Pesce-Rollins, M. Pierbattista, M. Piron, F. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Reposeur, T. Ritz, S. Rochester, L. S. Sgro, C. Siskind, E. J. Smith, P. D. Spandre, G. Spinelli, P. Suson, D. J. Takahashi, H. Tanaka, T. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tosti, G. Troja, E. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vilchez, N. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Yang, Z. Zimmer, S. TI In-flight measurement of the absolute energy scale of the Fermi Large Area Telescope SO ASTROPARTICLE PHYSICS LA English DT Article DE Cosmic-rays; Geomagnetic cutoff; Absolute energy scale; Fermi Large Area Telescope ID MISSION AB The Large Area Telescope (LAT) on-board the Fermi Gamma-ray Space Telescope is a pair-conversion telescope designed to survey the gamma-ray sky from 20 MeV to several hundreds of GeV. In this energy band there are no astronomical sources with sufficiently well known and sharp spectral features to allow an absolute calibration of the LAT energy scale. However, the geomagnetic cutoff in the cosmic ray electron-plus-positron (CRE) spectrum in low Earth orbit does provide such a spectral feature. The energy and spectral shape of this cutoff can be calculated with the aid of a numerical code tracing charged particles in the Earth's magnetic field. By comparing the cutoff value with that measured by the LAT in different geomagnetic positions, we have obtained several calibration points between similar to 6 and similar to 13 GeV with an estimated uncertainty of similar to 2%. An energy calibration with such high accuracy reduces the systematic uncertainty in LAT measurements of, for example, the spectral cutoff in the emission from gamma ray pulsars. (C) 2011 Elsevier B.V. All rights reserved. C1 [Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Enoto, T.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Reimer, A.; Reimer, O.; Rochester, L. S.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab,Dept Phys, Stanford, CA 94305 USA. [Atwood, W. B.; Bouvier, A.; Ritz, S.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Bouvier, A.; Ritz, S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Axelsson, M.; Vianello, G.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Axelsson, M.; Yang, Z.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Axelsson, M.] AlbaNova, Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bar, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Fortin, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.] CSIC, IEEE, Inst Ciencies Espai, Barcelona 08193, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.; Tibaldo, L.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, CEA,IRFU,CNRS,Lab AIM, F-91191 Gif Sur Yvette, France. [Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA. [Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Cohen-Tanugi, J.; Falletti, L.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France. [Cutini, S.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Fukazawa, Y.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Hughes, R. E.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Johnson, T. J.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Katagiri, H.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan. [Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.; Vilchez, N.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knoedlseder, J.; Vilchez, N.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Lee, S. -H.] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Moiseev, A. A.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Parent, D.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Reimer, A.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Zimmer, S.] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden. [Troja, E.] NASA, Postdoctoral Program, Greenbelt, MD 20771 USA. RP Pesce-Rollins, M (reprint author), Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. EM melissa.pesce.rollins@pi.infn.it RI Thompson, David/D-2939-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Funk, Stefan/B-7629-2015; Loparco, Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Orlando, E/R-5594-2016; OI Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Giroletti, Marcello/0000-0002-8657-8852; Cutini, Sara/0000-0002-1271-2924; Baldini, Luca/0000-0002-9785-7726; Loparco, Francesco/0000-0002-1173-5673; Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018 FU National Aeronautics and Space Administration; Department of Energy in the USA; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K.A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the USA, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K.A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden.; Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. NR 18 TC 16 Z9 16 U1 0 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 J9 ASTROPART PHYS JI Astropart Phys. PD JAN PY 2012 VL 35 IS 6 BP 346 EP 353 DI 10.1016/j.astropartphys.2011.10.007 PG 8 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 898RZ UT WOS:000300760800007 ER PT J AU Naraoka, H Mita, H Hamase, K Mita, M Yabuta, H Saito, K Fukushima, K Kitajima, F Sandford, SA Nakamura, T Noguchi, T Okazaki, R Nagao, K Ebihara, M Yurimoto, H Tsuchiyama, A Abe, M Shirai, K Ueno, M Yada, T Ishibashi, Y Okada, T Fujimura, A Mukai, T Yoshikawa, M Kawaguchi, J AF Naraoka, H. Mita, H. Hamase, K. Mita, M. Yabuta, H. Saito, K. Fukushima, K. Kitajima, F. Sandford, S. A. Nakamura, T. Noguchi, T. Okazaki, R. Nagao, K. Ebihara, M. Yurimoto, H. Tsuchiyama, A. Abe, M. Shirai, K. Ueno, M. Yada, T. Ishibashi, Y. Okada, T. Fujimura, A. Mukai, T. Yoshikawa, M. Kawaguchi, J. TI Preliminary organic compound analysis of microparticles returned from Asteroid 25143 Itokawa by the Hayabusa mission SO GEOCHEMICAL JOURNAL LA English DT Article DE Hayabusa spacecraft; Itokawa; microparticles; amino acid analysis; ToF-SIMS analysis ID EXTRATERRESTRIAL AMINO-ACIDS; DUST PARTICLES; METEORITES; CHONDRITES; SPACECRAFT; ISOVALINE; STARDUST; SAMPLES; FINES AB Microparticles recovered from the Asteroid 25143 Itokawa surface by the Hayabusa mission have been examined for the occurrence of soluble organic compounds. After five individual particles (similar to 50 to 100 mu m in diameter) were rinsed with organic solvents on a diamond plate, two extracts were hydrolyzed with hydrochloric acid for amino acid analysis (AAA), and three extracts were combined for time of flight-secondary ion mass spectrometry (ToF-SIMS) to look for other organic compounds, including polycyclic aromatic hydrocarbons. The organic compounds detected by both methods have the same concentrations as those in blank levels, indicating that indigenous organic compounds are not found in this study. Based on the sensitivities of AAA and ToF-SIMS with the reference sample analyses, the concentrations of indigenous organics in the samples are below part-per-million (ppm), if present. C1 [Naraoka, H.; Kitajima, F.; Okazaki, R.] Kyushu Univ, Dept Earth & Planetary Sci, Fukuoka 8128581, Japan. [Mita, H.] Fukuoka Inst Technol, Dept Life Environm & Mat Sci, Fukuoka 8110295, Japan. [Hamase, K.] Kyushu Univ, Grad Sch Pharmaceut Sci, Fukuoka 8128582, Japan. [Mita, M.] Shiseido Co Ltd, Frontier Sci Div, Minato Ku, Tokyo 1050021, Japan. [Yabuta, H.; Tsuchiyama, A.] Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Saito, K.; Fukushima, K.] Nagoya Univ, Grad Sch Bioagr Sci, Nagoya, Aichi 4648601, Japan. [Sandford, S. A.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Nakamura, T.] Tohoku Univ, Dept Earth & Planetary Mat Sci, Sendai, Miyagi 9808578, Japan. [Noguchi, T.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan. [Nagao, K.] Univ Tokyo, Geochem Res Ctr, Bunkyo Ku, Tokyo 1130033, Japan. [Ebihara, M.] Tokyo Metropolitan Univ, Dept Chem, Hachioji, Tokyo 1920397, Japan. [Yurimoto, H.] Hokkaido Univ, Dept Earth & Planetary Sci, Sapporo, Hokkaido 0600810, Japan. [Abe, M.; Shirai, K.; Ueno, M.; Yada, T.; Ishibashi, Y.; Okada, T.; Fujimura, A.; Mukai, T.; Yoshikawa, M.; Kawaguchi, J.] Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. RP Naraoka, H (reprint author), Kyushu Univ, Dept Earth & Planetary Sci, Fukuoka 8128581, Japan. EM naraoka@geo.kyushu-u.ac.jp RI Yabuta, Hikaru/M-9041-2014 OI Yabuta, Hikaru/0000-0002-4625-5362 FU Japan Society for the Promotion of Science [22340166]; Consortium Fukuoka FX We are grateful to Profs. D. P. Glavin, S. Pizzarello and G. D. Cody for helpful comments to revise the manuscript. This study was partially supported by Grant-in-Aid for Scientific Research (B) no 22340166 from Japan Society for the Promotion of Science and Research Fund form Consortium Fukuoka to HM and KH. NR 24 TC 13 Z9 15 U1 2 U2 17 PU GEOCHEMICAL SOC JAPAN PI TOKYO PA 358-5 YAMABUKI-CHO, SHINJUKU-KU, TOKYO, 162-0801, JAPAN SN 0016-7002 EI 1880-5973 J9 GEOCHEM J JI Geochem. J. PY 2012 VL 46 IS 1 BP 61 EP 72 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 904NX UT WOS:000301206300006 ER PT S AU Petrachenko, WT Niell, AE Corey, BE Behrend, D Schuh, H Wresnik, J AF Petrachenko, W. T. Niell, A. E. Corey, B. E. Behrend, D. Schuh, H. Wresnik, J. BE Kenyon, SC Pacino, MC Marti, UJ TI VLBI2010: Next Generation VLBI System for Geodesy and Astrometry SO GEODESY FOR PLANET EARTH: PROCEEDINGS OF THE 2009 IAG SYMPOSIUM SE International Association of Geodesy Symposia LA English DT Proceedings Paper CT Scientific Assembly of the International-Association-of-Geodesy (IAG) - Geodesy for Planet Earth CY AUG 31-SEP 04, 2009 CL Buenos Aires, ARGENTINA SP Int Assoc Geodesy (IAG) AB The International VLBI Service for Geodesy and Astrometry (IVS) is well on the way to fully defining a next generation VLBI system, called VLBI2010. The goals of the new system are to achieve 1-mm position accuracy over a 24-h observing session and to carry out continuous observations, with initial results to be delivered within 24 h after taking the data. These goals require a completely new technical and conceptual design of VLBI measurements. Based on extensive simulation studies, strategies have been developed by the IVS to significantly improve its product accuracy through the use of a network of small (similar to 12-m) fast-slewing antennas, a new method for generating high precision delay measurements, and improved methods for handling biases related to system electronics, deformations of the antenna structures, and radio source structure. To test many of the proposed strategies, NASA is sponsoring a proof-of-concept development effort using IVS antennas near Washington, DC, and Boston, MA. Furthermore, as of Feb. 2009, the construction of ten new VLBI2010 sites has already been funded, which will improve the geographical distribution of geodetic VLBI sites and provide an important step towards a global VLBI2010 network. C1 [Petrachenko, W. T.] Nat Resources Canada, Geodet Survey Div, CCRS, 615 Booth St, Ottawa, ON K1A 0E9, Canada. [Niell, A. E.; Corey, B. E.] MIT, Haystack Observ, Westford, MA 01886 USA. [Behrend, D.] NVI Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Schuh, H.; Wresnik, J.] Vienna Univ Technol, Inst Geodesy & Geophys, A-1040 Vienna, Austria. RP Petrachenko, WT (reprint author), Nat Resources Canada, Geodet Survey Div, CCRS, 615 Booth St, Ottawa, ON K1A 0E9, Canada. EM bill.petrachenko@nrc.gc.ca RI Symposia, IAG/K-2857-2012 NR 12 TC 7 Z9 7 U1 0 U2 3 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0939-9585 BN 978-3-642-20338-1; 978-3-642-20337-4 J9 IAG SYMP PY 2012 VL 136 BP 999 EP 1005 DI 10.1007/978-3-642-20338-1_125 PG 7 WC Geosciences, Multidisciplinary; Remote Sensing SC Geology; Remote Sensing GA BYU53 UT WOS:000300433100125 ER PT S AU Willis, P Bar-Sever, YE Bock, O AF Willis, P. Bar-Sever, Y. E. Bock, O. BE Kenyon, SC Pacino, MC Marti, UJ TI Estimating Horizontal Tropospheric Gradients in DORIS Data Processing: Preliminary Results SO GEODESY FOR PLANET EARTH: PROCEEDINGS OF THE 2009 IAG SYMPOSIUM SE International Association of Geodesy Symposia LA English DT Proceedings Paper CT Scientific Assembly of the International-Association-of-Geodesy (IAG) - Geodesy for Planet Earth CY AUG 31-SEP 04, 2009 CL Buenos Aires, ARGENTINA SP Int Assoc Geodesy (IAG) ID TIME-SERIES; PATH DELAY; GPS DATA; MISSIONS; NETWORK; MODEL AB Estimating horizontal tropospheric gradients is a common practice in VLBI and GPS data analyses. We investigate here the possibility to do the same for DORIS. We reprocessed all 2007 DORIS data for all satellites, using exactly the same strategy as the latest ignwd08 solution (Willis et al., Adv Space Res 45(12): 1470-1480, 2010) but adding two new parameters per day to account for any asymmetry of the tropospheric delays. When averaged over the full year the DORIS north gradient estimates show a significant correlation with GPS estimates at 33 co-located sites. The east gradient is loosely determined with DORIS due to the north-south orientation of the satellites passes in 2007. Typical values are below 1 mm and North component shows a latitude dependency, negative values in the Northern hemisphere and positive values in the Southern hemisphere. The stacking of DORIS station weekly coordinates provides a more realistic value for a factor of unit weight when done using gradient estimation. Station coordinates also indicate a small improvement in internal consistency when compared to a 1-year position and velocity solution without estimating gradients. The DORIS-derived tropospheric gradients may still absorb other types of un-modeled errors, but estimation of such parameters should be investigated in more detail before reprocessing the entire DORIS data set in view of the next ITRF realization, following ITRF2008. C1 [Willis, P.] Direct Tech, Inst Geog Natl, 2 Ave Pasteur, F-94165 St Mande, France. [Willis, P.] PRES Sorbonne Paris, UFR STEP, Inst Phys Globe Paris, F-75013 Paris, France. [Bar-Sever, Y. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, O.] LAREG, Inst Geog Natl, F-77455 Marne La Vallee, France. RP Willis, P (reprint author), Direct Tech, Inst Geog Natl, 2 Ave Pasteur, F-94165 St Mande, France. EM willis@ipgp.fr RI Willis, Pascal/A-8046-2008; Symposia, IAG/K-2857-2012 OI Willis, Pascal/0000-0002-3257-0679; NR 29 TC 10 Z9 10 U1 0 U2 6 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0939-9585 BN 978-3-642-20338-1; 978-3-642-20337-4 J9 IAG SYMP PY 2012 VL 136 BP 1013 EP 1019 DI 10.1007/978-3-642-20338-1_127 PG 7 WC Geosciences, Multidisciplinary; Remote Sensing SC Geology; Remote Sensing GA BYU53 UT WOS:000300433100127 ER PT J AU Schmidt, GA Jungclaus, JH Ammann, CM Bard, E Braconnot, P Crowley, TJ Delaygue, G Joos, F Krivova, NA Muscheler, R Otto-Bliesner, BL Pongratz, J Shindell, DT Solanki, SK Steinhilber, F Vieira, LEA AF Schmidt, G. A. Jungclaus, J. H. Ammann, C. M. Bard, E. Braconnot, P. Crowley, T. J. Delaygue, G. Joos, F. Krivova, N. A. Muscheler, R. Otto-Bliesner, B. L. Pongratz, J. Shindell, D. T. Solanki, S. K. Steinhilber, F. Vieira, L. E. A. TI Climate forcing reconstructions for use in PMIP simulations of the Last Millennium (v1.1) SO GEOSCIENTIFIC MODEL DEVELOPMENT LA English DT Article ID SOLAR IRRADIANCE; SUNSPOT CYCLE; SHAPE AB We update the forcings for the PMIP3 experiments for the Last Millennium to include new assessments of historical land use changes and discuss new suggestions for calibrating solar activity proxies to total solar irradiance. C1 [Schmidt, G. A.; Shindell, D. T.] Columbia Univ, NASA Goddard Inst Space Studies, New York, NY 10027 USA. [Schmidt, G. A.; Shindell, D. T.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Jungclaus, J. H.] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Ammann, C. M.; Otto-Bliesner, B. L.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Bard, E.] Univ Aix Marseille 3, CNRS, IRD, Coll France,CEREGE, F-13545 Aix En Provence 04, France. [Braconnot, P.] Lab Sci Climat & Environm, Gif Sur Yvette, France. [Crowley, T. J.] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland. [Delaygue, G.] Univ Grenoble 1, CNRS, LGGE, F-38402 St Martin Dheres, France. [Joos, F.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Joos, F.] Univ Bern, Oeschger Ctr Climate Change Res, CH-3012 Bern, Switzerland. [Krivova, N. A.; Solanki, S. K.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Muscheler, R.] Lund Univ, Dept Earth & Ecosyst Sci, S-22362 Lund, Sweden. [Pongratz, J.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Solanki, S. K.] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi, South Korea. [Steinhilber, F.] EAWAG, Swiss Fed Inst Aquat Sci & Technol, CH-8600 Dubendorf, Switzerland. [Vieira, L. E. A.] Lab Phys & Chim Environm & Espace, F-45071 Orleans 2, France. [Vieira, L. E. A.] Univ Orleans, F-45071 Orleans 2, France. RP Schmidt, GA (reprint author), Columbia Univ, NASA Goddard Inst Space Studies, New York, NY 10027 USA. EM gavin.a.schmidt@nasa.gov RI Vieira, Luis Eduardo/A-5548-2008; Schmidt, Gavin/D-4427-2012; Solanki, Sami/E-2487-2013; Shindell, Drew/D-4636-2012; Bard, Edouard/G-7717-2014; OI Vieira, Luis Eduardo/0000-0002-9376-475X; Schmidt, Gavin/0000-0002-2258-0486; Solanki, Sami/0000-0002-3418-8449; Joos, Fortunat/0000-0002-9483-6030 NR 38 TC 84 Z9 86 U1 2 U2 42 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1991-959X J9 GEOSCI MODEL DEV JI Geosci. Model Dev. PY 2012 VL 5 IS 1 BP 185 EP 191 DI 10.5194/gmd-5-185-2012 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 900HT UT WOS:000300878300011 ER PT J AU Li, B Toll, D Zhan, X Cosgrove, B AF Li, B. Toll, D. Zhan, X. Cosgrove, B. TI Improving estimated soil moisture fields through assimilation of AMSR-E soil moisture retrievals with an ensemble Kalman filter and a mass conservation constraint SO HYDROLOGY AND EARTH SYSTEM SCIENCES LA English DT Article ID LAND DATA ASSIMILATION; SURFACE MODEL; SYSTEM NLDAS; INFORMATION-SYSTEM; ALTIMETER DATA; TEMPERATURE; PREDICTION; FRAMEWORK; EQUATION; PRODUCTS AB Model simulated soil moisture fields are often biased due to errors in input parameters and deficiencies in model physics. Satellite derived soil moisture estimates, if retrieved appropriately, represent the spatial mean of near surface soil moisture in a footprint area, and can be used to reduce bias of model estimates (at locations near the surface) through data assimilation techniques. While assimilating the retrievals can reduce bias, it can also destroy the mass balance enforced by the model governing equation because water is removed from or added to the soil by the assimilation algorithm. In addition, studies have shown that assimilation of surface observations can adversely impact soil moisture estimates in the lower soil layers due to imperfect model physics, even though the bias near the surface is decreased. In this study, an ensemble Kalman filter (EnKF) with a mass conservation updating scheme was developed to assimilate Advanced Microwave Scanning Radiometer (AMSR-E) soil moisture retrievals, as they are without any scaling or preprocessing, to improve the estimated soil moisture fields by the Noah land surface model. Assimilation results using the conventional and the mass conservation updating scheme in the Little Washita watershed of Oklahoma showed that, while both updating schemes reduced the bias in the shallow root zone, the mass conservation scheme provided better estimates in the deeper profile. The mass conservation scheme also yielded physically consistent estimates of fluxes and maintained the water budget. Impacts of model physics on the assimilation results are discussed. C1 [Li, B.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Li, B.; Toll, D.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Zhan, X.] NOAA NESDIS Ctr Satellite Applicat & Res, Camp Springs, MD USA. [Cosgrove, B.] NOAA NWS Off Hydrol Dev, Silver Spring, MD USA. RP Li, B (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM bailing.li@nasa.gov RI Zhan, Xiwu/F-5487-2010 FU NOAA; NASA FX The work was supported by the NOAA Climate Prediction Program for America and NASA Terrestrial Hydrology Program. We thank the Department of Energy, the Department of Agriculture and US Geological Survey for making ground based measurements available in the public domain and the two anonymous reviewers for their comments and suggestions which helped improving the quality of this paper. NR 45 TC 21 Z9 21 U1 1 U2 15 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1027-5606 EI 1607-7938 J9 HYDROL EARTH SYST SC JI Hydrol. Earth Syst. Sci. PY 2012 VL 16 IS 1 BP 105 EP 119 DI 10.5194/hess-16-105-2012 PG 15 WC Geosciences, Multidisciplinary; Water Resources SC Geology; Water Resources GA 891QY UT WOS:000300232900008 ER PT J AU Stoklosa, AM Perchonok, MH Little, KM Nivens, DE Mauer, LJ AF Stoklosa, Adam M. Perchonok, Michele H. Little, Kenneth M. Nivens, David E. Mauer, Lisa J. TI EFFECTS OF LOW DOSE GAMMA-RADIATION ON SELECT WHEAT PROPERTIES SO INTERNATIONAL JOURNAL OF FOOD PROPERTIES LA English DT Article DE Apogee; Perigee; NASA; Space food; Radiation; Wheat ID IRRADIATION; PROTEINS; QUALITY; ACIDS AB The effects of space-travel-relevant radiation doses (gamma radiation) on structure, function, and antioxidant properties of select wheat cultivars (Triticum aestivum L) were investigated. Following radiation treatment, proteins were analyzed using SDS-PAGE, mixograph, and atomic force microscopy methods. Starch granule damage and pasting curve functionality were evaluated; lipid oxidation was determined using a thiobarbituric acid reactive substances method; and antioxidant capacity was measured using 2,2-diphenyl-1-picrythydrazyl analyses. Increasing radiation exposure resulted in significant differences between wheat cultivars. Therefore, low-dose gamma-radiation affects wheat, and differences exist between cultivars, so careful consideration is needed when selecting wheat for use in elevated radiation conditions. The Apogee cultivar is likely a better NASA candidate crop than Perigee; however, Yecora Rojo, Pars hall, and/or Yavaros 79 cultivars may be more stable to radiation and provide better food functionality traits. Ultimately, wheat should be protected from radiation exposure during space travel, if possible, to maintain quality. C1 [Stoklosa, Adam M.; Little, Kenneth M.; Nivens, David E.; Mauer, Lisa J.] Purdue Univ, Dept Food Sci, W Lafayette, IN 47907 USA. [Perchonok, Michele H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Mauer, LJ (reprint author), Purdue Univ, Dept Food Sci, 745 Agr Mall Dr, W Lafayette, IN 47907 USA. EM mauer@purdue.edu FU NASA [NAG5-12686] FX This research was partially funded by NASA grant NAG5-12686. The authors would like to acknowledge Dr. Cary Mitchell and Dr. Gioia Massa for their assistance in cultivating the wheat crops in the greenhouse at Purdue University. They also wish to thank Dr. Bruce Bugbee for providing wheat berries needed for production of Apogee and Perigee biomass Dr. Bruce Hamaker for use of the cereal lab facilities and equipment. NR 34 TC 0 Z9 0 U1 3 U2 9 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1094-2912 J9 INT J FOOD PROP JI Int. J. Food Prop. PD JAN-APR PY 2012 VL 15 IS 1-2 BP 109 EP 121 DI 10.1080/10942911003754668 PG 13 WC Food Science & Technology SC Food Science & Technology GA 901ZC UT WOS:000301007400011 ER PT J AU Heymsfield, E Fasanella, EL Hardy, RC Boitnott, RL AF Heymsfield, Ernest Fasanella, Edwin L. Hardy, Robin C. Boitnott, Richard L. TI Assessment of Soil Modeling Capability for Orion Contingency Land Landing SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE Crashworthiness testing; Swing test; Vertical drop test; Orion; Soil modeling ID AIRCRAFT AB Twenty-one swing tests were conducted at the NASA Langley Landing and Impact Research (LandIR) Facility in 2006 to evaluate Orion boilerplate ground landings as a function of impact velocity and pitch. In this article, experimental results from two capsule swing tests and three vertical drop tests are compared with numerical results. The numerical results were derived by using the nonlinear dynamic finite-element code LS-DYNA. The swing tests were conducted at 0 degrees and -15 degrees pitch, impacting a level soil mat at a 17.68 m/s (58 fps) horizontal velocity and 1.52 m/s (5 fps) vertical impact velocity. Three vertical drop tests were conducted with the boilerplate capsule at 0 degrees pitch. Each test was conducted to measure the impact on a level soil mat with varying impact velocities: 3.66 m/s, 7.31 m/s, and 10.97 m/s (12, 24, and 36 fps). Results of the study show the potential of using numerical modeling for vertical drop test and swing test simulations. Discrepancies between the numerical and experimental simulations primarily stem from the nonuniformity and complexity of soil behavior. DOI: 10.1061/(ASCE)AS.1943-5525.0000089. (C) 2012 American Society of Civil Engineers. C1 [Heymsfield, Ernest] Univ Arkansas, Dept Civil Engn, Fayetteville, AR 72701 USA. [Fasanella, Edwin L.] Natl Inst Aerosp, Hampton, VA 23681 USA. [Hardy, Robin C.; Boitnott, Richard L.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Heymsfield, E (reprint author), Univ Arkansas, Dept Civil Engn, Fayetteville, AR 72701 USA. EM ernie@uark.edu; Edwin.L.Fasanella@nasa.gov; robin.c.hardy@nasa.gov; richard.l.boitnott@nasa.gov NR 11 TC 2 Z9 2 U1 1 U2 5 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JAN PY 2012 VL 25 IS 1 BP 125 EP 131 DI 10.1061/(ASCE)AS.1943-5525.0000089 PG 7 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 894OS UT WOS:000300436900015 ER PT J AU Anyamba, A Linthicum, KJ Small, JL Collins, KM Tucker, CJ Pak, EW Britch, SC Eastman, JR Pinzon, JE Russell, KL AF Anyamba, Assaf Linthicum, Kenneth J. Small, Jennifer L. Collins, Kathrine M. Tucker, Compton J. Pak, Edwin W. Britch, Seth C. Eastman, James Ronald Pinzon, Jorge E. Russell, Kevin L. TI Climate Teleconnections and Recent Patterns of Human and Animal Disease Outbreaks SO PLOS NEGLECTED TROPICAL DISEASES LA English DT Article ID RIFT-VALLEY FEVER; HANTAVIRUS PULMONARY SYNDROME; EQUATORIAL INDIAN-OCEAN; SOUTH-EAST-ASIA; CHIKUNGUNYA VIRUS; AEDES-AEGYPTI; EL-NINO; UNITED-STATES; TEMPERATURE; DIPTERA AB Background: Recent clusters of outbreaks of mosquito-borne diseases (Rift Valley fever and chikungunya) in Africa and parts of the Indian Ocean islands illustrate how interannual climate variability influences the changing risk patterns of disease outbreaks. Although Rift Valley fever outbreaks have been known to follow periods of above-normal rainfall, the timing of the outbreak events has largely been unknown. Similarly, there is inadequate knowledge on climate drivers of chikungunya outbreaks. We analyze a variety of climate and satellite-derived vegetation measurements to explain the coupling between patterns of climate variability and disease outbreaks of Rift Valley fever and chikungunya. Methods and Findings: We derived a teleconnections map by correlating long-term monthly global precipitation data with the NINO3.4 sea surface temperature (SST) anomaly index. This map identifies regional hot-spots where rainfall variability may have an influence on the ecology of vector borne disease. Among the regions are Eastern and Southern Africa where outbreaks of chikungunya and Rift Valley fever occurred 2004-2009. Chikungunya and Rift Valley fever case locations were mapped to corresponding climate data anomalies to understand associations between specific anomaly patterns in ecological and climate variables and disease outbreak patterns through space and time. From these maps we explored associations among Rift Valley fever disease occurrence locations and cumulative rainfall and vegetation index anomalies. We illustrated the time lag between the driving climate conditions and the timing of the first case of Rift Valley fever. Results showed that reported outbreaks of Rift Valley fever occurred after,3-4 months of sustained above-normal rainfall and associated green-up in vegetation, conditions ideal for Rift Valley fever mosquito vectors. For chikungunya we explored associations among surface air temperature, precipitation anomalies, and chikungunya outbreak locations. We found that chikungunya outbreaks occurred under conditions of anomalously high temperatures and drought over Eastern Africa. However, in Southeast Asia, chikungunya outbreaks were negatively correlated (p < 0.05) with drought conditions, but positively correlated with warmer-than-normal temperatures and rainfall. Conclusions/Significance: Extremes in climate conditions forced by the El Nino/Southern Oscillation (ENSO) lead to severe droughts or floods, ideal ecological conditions for disease vectors to emerge, and may result in epizootics and epidemics of Rift Valley fever and chikungunya. However, the immune status of livestock (Rift Valley fever) and human (chikungunya) populations is a factor that is largely unknown but very likely plays a role in the spatial-temporal patterns of these disease outbreaks. As the frequency and severity of extremes in climate increase, the potential for globalization of vectors and disease is likely to accelerate. Understanding the underlying patterns of global and regional climate variability and their impacts on ecological drivers of vector-borne diseases is critical in long-range planning of appropriate disease and disease-vector response, control, and mitigation strategies. C1 [Anyamba, Assaf; Small, Jennifer L.; Collins, Kathrine M.; Tucker, Compton J.; Pak, Edwin W.; Pinzon, Jorge E.] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD USA. [Linthicum, Kenneth J.; Britch, Seth C.] USDA ARS, Ctr Med Agr & Vet Entomol, Gainesville, FL USA. [Eastman, James Ronald] Clark Univ, Clark Labs, Worcester, MA 01610 USA. [Russell, Kevin L.] Armed Forces Hlth Surveillance Ctr, Div GEIS Operat, Silver Spring, MD USA. RP Anyamba, A (reprint author), NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD USA. EM assaf.anyamba@nasa.gov RI Valle, Ruben/A-7512-2013 FU Department of Defense - Armed Forces Health Surveillance Center; Division of GEIS Operations; United States Department of Agriculture - Agricultural Research Service; Google Foundation; Betty-Moore Foundation; National Aeronautics and Space Administration [NNH08CD31C/ROSES 2007] FX This research is supported in part by funding from the Department of Defense - Armed Forces Health Surveillance Center, Division of GEIS Operations, the United States Department of Agriculture - Agricultural Research Service, Google and Betty-Moore Foundations and the National Aeronautics and Space Administration Grant # NNH08CD31C/ROSES 2007. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 60 TC 27 Z9 29 U1 6 U2 53 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1935-2727 J9 PLOS NEGLECT TROP D JI Plos Neglect. Trop. Dis. PD JAN PY 2012 VL 6 IS 1 AR e1465 DI 10.1371/journal.pntd.0001465 PG 14 WC Infectious Diseases; Parasitology; Tropical Medicine SC Infectious Diseases; Parasitology; Tropical Medicine GA 894GW UT WOS:000300416100016 PM 22292093 ER PT J AU Joshi, MM Haberle, RM AF Joshi, Manoj M. Haberle, Robert M. TI Suppression of the Water Ice and Snow Albedo Feedback on Planets Orbiting Red Dwarf Stars and the Subsequent Widening of the Habitable Zone SO ASTROBIOLOGY LA English DT Article DE M stars; Habitable zone; Climate; Albedo; Habitability ID CLIMATE; EARTH; MODEL; ATMOSPHERES; RADIATION AB M stars comprise 80% of main sequence stars, so their planetary systems provide the best chance for finding habitable planets, that is, those with surface liquid water. We have modeled the broadband albedo or reflectivity of water ice and snow for simulated planetary surfaces orbiting two observed red dwarf stars (or M stars), using spectrally resolved data of Earth's cryosphere. The gradual reduction of the albedos of snow and ice at wavelengths greater than 1 mu m, combined with M stars emitting a significant fraction of their radiation at these same longer wavelengths, means that the albedos of ice and snow on planets orbiting M stars are much lower than their values on Earth. Our results imply that the ice/snow albedo climate feedback is significantly weaker for planets orbiting M stars than for planets orbiting G-type stars such as the Sun. In addition, planets with significant ice and snow cover will have significantly higher surface temperatures for a given stellar flux if the spectral variation of cryospheric albedo is considered, which in turn implies that the outer edge of the habitable zone around M stars may be 10-30% farther away from the parent star than previously thought. C1 [Joshi, Manoj M.] Univ Reading, Dept Meteorol, NCAS Climate, Reading RG6 6BB, Berks, England. [Haberle, Robert M.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP Joshi, MM (reprint author), Univ Reading, Dept Meteorol, NCAS Climate, POB 243, Reading RG6 6BB, Berks, England. EM m.m.joshi@reading.ac.uk RI Joshi, Manoj/C-1795-2008 OI Joshi, Manoj/0000-0002-2948-2811 FU UK National Centres of Atmospheric Science (NCAS) Climate FX M.J. is supported by the UK National Centres of Atmospheric Science (NCAS) Climate. The authors would like to thank Jonathan Fortney for the M-star spectral data as well as Laurance Doyle for his helpful comments. We acknowledge the extremely useful comments of Stephen Warren and the other reviewers of the submitted manuscript. NR 23 TC 27 Z9 28 U1 0 U2 19 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 JAN PY 2012 VL 12 IS 1 BP 3 EP 8 DI 10.1089/ast.2011.0668 PG 6 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 885JY UT WOS:000299776500002 PM 22181553 ER PT J AU Flury, T Wu, DL Read, WG AF Flury, T. Wu, D. L. Read, W. G. TI Correlation among cirrus ice content, water vapor and temperature in the TTL as observed by CALIPSO and Aura/MLS SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID TROPICAL TROPOPAUSE LAYER; DEEP CONVECTIVE CLOUDS; TRANSPORT; MODEL AB Water vapor in the tropical tropopause layer (TTL) has a local radiative cooling effect. As a source for ice in cirrus clouds, however, it can also indirectly produce infrared heating. Using NASA A-Train satellite measurements of CALIPSO and Aura/MLS we calculated the correlation of water vapor, ice water content and temperature in the TTL. We find that temperature strongly controls water vapor (correlation r = 0.94) and cirrus clouds at 100 hPa (r = -0.91). Moreover we observe that the cirrus seasonal cycle is highly (r = -0.9) anticorrelated with the water vapor variation in the TTL, showing higher cloud occurrence during December-January-February. We further investigate the anticorrelation on a regional scale and find that the strong anticorrelation occurs generally in the ITCZ (Intertropical Convergence Zone). The seasonal cycle of the cirrus ice water content is also highly anticorrelated to water vapor (r = -0.91) and our results support the hypothesis that the total water at 100 hPa is roughly constant. Temperature acts as a main regulator for balancing the partition between water vapor and cirrus clouds. Thus, to a large extent, the depleting water vapor in the TTL during DJF is a manifestation of cirrus formation. C1 [Flury, T.; Wu, D. L.; Read, W. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Wu, D. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Flury, T (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM thomas.flury@jpl.nasa.gov FU Swiss National Science Foundation [PBBEP2_133505]; National Aeronautics and Space Administration (NASA) at the Jet Propulsion Laboratory (JPL); NASA FX The work of TF has been supported by the Swiss National Science Foundation under grant PBBEP2_133505 and the National Aeronautics and Space Administration (NASA) at the Jet Propulsion Laboratory (JPL). The research by DLW and WGR was performed at JPL, California Institute of Technology under contract with NASA. Copyright 2011 California Institute of Technology. Government sponsorship acknowledged. Copyright 2011. All rights reserved. NR 28 TC 10 Z9 10 U1 0 U2 8 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 2 BP 683 EP 691 DI 10.5194/acp-12-683-2012 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 892YL UT WOS:000300321500005 ER PT J AU Xie, F Wu, DL Ao, CO Mannucci, AJ Kursinski, ER AF Xie, F. Wu, D. L. Ao, C. O. Mannucci, A. J. Kursinski, E. R. TI Advances and limitations of atmospheric boundary layer observations with GPS occultation over southeast Pacific Ocean SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID GLOBAL POSITIONING SYSTEM; RADIO OCCULTATION; VOCALS-REX; LOWER TROPOSPHERE; STRATIFORM CLOUDS; LARGE-SCALE; STRATOCUMULUS; ASSIMILATION; SUPERREFRACTION; REFRACTIVITY AB The typical atmospheric boundary layer (ABL) over the southeast (SE) Pacific Ocean is featured with a strong temperature inversion and a sharp moisture gradient across the ABL top. The strong moisture and temperature gradients result in a sharp refractivity gradient that can be precisely detected by the Global Positioning System (GPS) radio occultation (RO) measurements. In this paper, the Constellation Observing System for Meteorology, Ionosphere & Climate (COSMIC) GPS RO soundings, radiosondes and the high-resolution ECMWF analysis over the SE Pacific are analyzed. COSMIC RO is able to detect a wide range of ABL height variations (1-2 km) as observed from the radiosondes. However, the ECMWF analysis systematically underestimates the ABL heights. The sharp refractivity gradient at the ABL top frequently exceeds the critical refraction (e. g., -157 N-unit km(-1)) and becomes the so-called ducting condition, which results in a systematic RO refractivity bias (or called N-bias) inside the ABL. Simulation study based on radiosonde profiles reveals the magnitudes of the N-biases are vertical resolution dependent. The N-bias is also the primary cause of the systematically smaller refractivity gradient (rarely exceeding -110 N-unit km(-1)) at the ABL top from RO measurement. However, the N-bias seems not affect the ABL height detection. Instead, the very large RO bending angle and the sharp refractivity gradient due to ducting allow reliable detection of the ABL height from GPS RO. The seasonal mean climatology of ABL heights derived from a nine-month composite of COSMIC RO soundings over the SE Pacific reveals significant differences from the ECMWF analysis. Both show an increase of ABL height from the shallow stratocumulus near the coast to a much higher trade wind inversion further off the coast. However, COSMIC RO shows an overall deeper ABL and reveals different locations of the minimum and maximum ABL heights as compared to the ECMWF analysis. At low latitudes, despite the decreasing number of COSMIC RO soundings and the lower percentage of soundings that penetrate into the lowest 500-m above the mean-sea-level, there are small sampling errors in the mean ABL height climatology. The difference of ABL height climatology between COSMIC RO and ECMWF analysis over SE Pacific is significant and requires further studies. C1 [Xie, F.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn JIFRESSE, Los Angeles, CA 90024 USA. [Xie, F.; Wu, D. L.; Ao, C. O.; Mannucci, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Kursinski, E. R.] Univ Arizona, Dept Atmospher Sci, Tucson, AZ USA. RP Xie, F (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn JIFRESSE, Los Angeles, CA 90024 USA. EM fxie@jifresse.ucla.edu RI XIE, FEIQIN/J-4569-2013; Wu, Dong/D-5375-2012 FU UCLA; NOAA JCSDA; Jet Propulsion Laboratory (JPL), California Institute of Technology; National Science Foundation FX This work was supported by an appointment to JIFRESSE at UCLA. F. Xie and E. R. Kursinski are partly supported by NOAA JCSDA. D. L. Wu, C. O. Ao and A. J. Mannucci are supported by the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with NASA. The COSMIC RO soundings were provided by JPL. The high-resolution ECMWF analysis data were acquired from ECMWF. The VOCALS radiosondes were provided by NCAR/EOL under sponsorship of the National Science Foundation. The rawinsondes from stratus cruises around 20 degrees S were provided by deSzoeke at Oregon State University. We thank S. Healy, R. Wood and J. Teixeira for the intriguing discussions. We thank Byron Iijima, Marc Pestana for assistance with the COSMIC retrievals and Evan Fishbein for help with ECMWF data. We also thank Rene Garreaud (editor) and the two reviewers for valuable comments. NR 61 TC 23 Z9 24 U1 0 U2 13 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 2 BP 903 EP 918 DI 10.5194/acp-12-903-2012 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 892YL UT WOS:000300321500020 ER PT J AU Wise, ME Baustian, KJ Koop, T Freedman, MA Jensen, EJ Tolbert, MA AF Wise, M. E. Baustian, K. J. Koop, T. Freedman, M. A. Jensen, E. J. Tolbert, M. A. TI Depositional ice nucleation onto crystalline hydrated NaCl particles: a new mechanism for ice formation in the troposphere SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID PHASE-TRANSITIONS; AEROSOL-PARTICLES; AMMONIUM-SULFATE; LOW-TEMPERATURES; SODIUM-CHLORIDE; WATER-VAPOR; SEA-SALT; DELIQUESCENCE; DEPENDENCE; MODEL AB Sea-salt aerosol (SSA) particles are ubiquitous in the marine boundary layer and over coastal areas. Therefore SSA have ability to directly and indirectly affect the Earth's radiation balance. The influence SSA have on climate is related to their water uptake and ice nucleation characteristics. In this study, optical microscopy coupled with Raman spectroscopy was used to detect the formation of a crystalline NaCl hydrate that could form under atmospheric conditions. NaCl(s) particles (similar to 1 to 10 mu m in diameter) deliquesced at 75.7 +/- 2.5% RH which agrees well with values previously established in the literature. NaCl(aq) particles effloresced to a mixture of hydrated and non-hydrated particles at temperatures between 236 and 252 K. The aqueous particles effloresced into the non-hydrated form at temperatures warmer than 252 K. At temperatures colder than 236 K all particles effloresced into the hydrated form. The deliquescence relative humidities (DRH) of hydrated NaCl(s) particles ranged from 76.6 to 93.2% RH. Based on the measured DRH and efflorescence relative humidities (ERH), we estimate crystalline NaCl particles could be in the hydrated form 40-80% of the time in the troposphere. Additionally, the ice nucleating abilities of NaCl(s) and hydrated NaCl(s) were determined at temperatures ranging from 221 to 238 K. Here, depositional ice nucleation is defined as the onset of ice nucleation and represents the conditions at which the first particle on the substrate nucleated ice. Thus the values reported here represent the lower limit of depositional ice nucleation. NaCl(s) particles depositionally nucleated ice at an average S-ice value of 1.11 +/- 0.07. Hydrated NaCl(s) particles depositionally nucleated ice at an average S-ice value of 1.02 +/- 0.04. When a mixture of hydrated and anhydrous NaCl(s) particles was present in the same sample, ice preferentially nucleated on the hydrated particles 100% of the time. While both types of particles are efficient ice nuclei, hydrated NaCl(s) particles are better ice nuclei than NaCl(s) particles. C1 [Wise, M. E.; Tolbert, M. A.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA. [Wise, M. E.; Baustian, K. J.; Tolbert, M. A.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Baustian, K. J.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Koop, T.] Univ Bielefeld, Fac Chem, D-33615 Bielefeld, Germany. [Freedman, M. A.] Penn State Univ, Dept Chem, University Pk, PA 16802 USA. [Jensen, E. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Tolbert, MA (reprint author), Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA. EM mawise@cu-portland.edu; tolbert@colorado.edu RI Koop, Thomas/B-7861-2008; Freedman, Miriam/A-4571-2013 OI Koop, Thomas/0000-0002-7571-3684; Freedman, Miriam/0000-0003-4374-6518 FU National Science Foundation [NSF-ATM 0650023, AGS1048536]; NASA (NESSF) [NN08AU77H]; CIRES at the University of Colorado at Boulder; European Commission [505390-GOCE-CT-2004] FX The authors gratefully acknowledge the National Science Foundation for supporting this work (NSF-ATM 0650023 and AGS1048536). K. Baustian received additional support from NASA (NESSF fellowship NN08AU77H) and by CIRES at the University of Colorado at Boulder. T. K. acknowledges funding from European Commission (505390-GOCE-CT-2004). NR 42 TC 37 Z9 38 U1 3 U2 59 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 2 BP 1121 EP 1134 DI 10.5194/acp-12-1121-2012 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 892YL UT WOS:000300321500033 ER PT J AU Apel, EC Olson, JR Crawford, JH Hornbrook, RS Hills, AJ Cantrell, CA Emmons, LK Knapp, DJ Hall, S Mauldin, RL Weinheimer, AJ Fried, A Blake, DR Crounse, JD St Clair, JM Wennberg, PO Diskin, GS Fuelberg, HE Wisthaler, A Mikoviny, T Brune, W Riemer, DD AF Apel, E. C. Olson, J. R. Crawford, J. H. Hornbrook, R. S. Hills, A. J. Cantrell, C. A. Emmons, L. K. Knapp, D. J. Hall, S. Mauldin, R. L., III Weinheimer, A. J. Fried, A. Blake, D. R. Crounse, J. D. St Clair, J. M. Wennberg, P. O. Diskin, G. S. Fuelberg, H. E. Wisthaler, A. Mikoviny, T. Brune, W. Riemer, D. D. TI Impact of the deep convection of isoprene and other reactive trace species on radicals and ozone in the upper troposphere SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID VOLATILE ORGANIC-COMPOUNDS; IONIZATION MASS-SPECTROMETRY; TROPICAL UPPER TROPOSPHERE; METHYL VINYL KETONE; LOWER STRATOSPHERE; PEM-TROPICS; IN-SITU; PTR-MS; CHEMICAL EVOLUTION; NORTH-ATLANTIC AB Observations of a comprehensive suite of inorganic and organic trace gases, including non-methane hydrocarbons (NMHCs), halogenated organics and oxygenated volatile organic compounds (OVOCs), obtained from the NASA DC-8 over Canada during the ARCTAS aircraft campaign in July 2008 illustrate that convection is important for redistributing both long-and short-lived species throughout the troposphere. Convective outflow events were identified by the elevated mixing ratios of organic species in the upper troposphere relative to background conditions. Several dramatic events were observed in which isoprene and its oxidation products were detected at hundreds of pptv at altitudes higher than 8 km. Two events are studied in detail using detailed experimental data and the NASA Langley Research Center (LaRC) box model. One event had no lightning NOx (NO + NO2) associated with it and the other had substantial lightning NOx (LNOx > 1 ppbv). When convective storms transport isoprene from the boundary layer to the upper troposphere and no LNOx is present, OH is reduced due to scavenging by isoprene, which serves to slow the chemistry, resulting in longer lifetimes for species that react with OH. Ozone and PAN production is minimal in this case. In the case where isoprene is convected and LNOx is present, there is a large effect on the expected ensuing chemistry: isoprene exerts a dominant impact on HOx and nitrogen-containing species; the relative contribution from other species to HOx, such as peroxides, is insignificant. The isoprene reacts quickly, resulting in primary and secondary products, including formaldehyde and methyl glyoxal. The model predicts enhanced production of alkyl nitrates (ANs) and peroxyacyl nitrate compounds (PANs). PANs persist because of the cold temperatures of the upper troposphere resulting in a large change in the NOx mixing ratios which, in turn, has a large impact on the HOx chemistry. Ozone production is substantial during the first few hours following the convection to the UT, resulting in a net gain of approximately 10 ppbv compared to the modeled scenario in which LNOx is present but no isoprene is present aloft. C1 [Apel, E. C.; Hornbrook, R. S.; Hills, A. J.; Cantrell, C. A.; Emmons, L. K.; Knapp, D. J.; Hall, S.; Mauldin, R. L., III; Weinheimer, A. J.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. [Fried, A.] Natl Ctr Atmospher Res, Earth Observing Lab, Boulder, CO 80307 USA. [Olson, J. R.; Crawford, J. H.; Diskin, G. S.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Blake, D. R.] Univ Calif Irvine, Sch Phys Sci, Irvine, CA USA. [Crounse, J. D.; St Clair, J. M.; Wennberg, P. O.] CALTECH, Pasadena, CA 91125 USA. [Fuelberg, H. E.] Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA. [Wisthaler, A.; Mikoviny, T.] Univ Innsbruck, Inst Ionenphys & Angew Phys, A-6020 Innsbruck, Austria. [Brune, W.] Penn State Univ, State Coll, PA USA. [Riemer, D. D.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Fried, A.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. RP Apel, EC (reprint author), Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. EM apel@ucar.edu RI Crounse, John/E-4622-2011; Crawford, James/L-6632-2013; Crounse, John/C-3700-2014; Emmons, Louisa/R-8922-2016; OI Crawford, James/0000-0002-6982-0934; Crounse, John/0000-0001-5443-729X; Emmons, Louisa/0000-0003-2325-6212; Hornbrook, Rebecca/0000-0002-6304-6554 FU NASA [X08AD33G]; Austrian Research Promotion Agency (FFG-ALR); Tiroler Zukunftstiftung; National Science Foundation FX The authors thank the crew and support team for the NASA DC-8 aircraft, and Mary Barth, Frank Flocke and John Orlando for helpful comments and discussion. The authors gratefully acknowledge the financial support of NASA (Grant No. X08AD33G). PTR-MS measurements were supported by the Austrian Research Promotion Agency (FFG-ALR) and the Tiroler Zukunftstiftung, and were carried out with the help/support of M. Graus, A. Hansel and T. D. Maerk. The National Center for Atmospheric Research is sponsored by the National Science Foundation. Any opinions, findings and conclusions or recommendations expressed in the publication are those of the authors and do not necessarily reflect the views of the National Science Foundation. NR 75 TC 9 Z9 9 U1 7 U2 58 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 2 BP 1135 EP 1150 DI 10.5194/acp-12-1135-2012 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 892YL UT WOS:000300321500034 ER PT J AU Cazorla, M Brune, WH Ren, X Lefer, B AF Cazorla, M. Brune, W. H. Ren, X. Lefer, B. TI Direct measurement of ozone production rates in Houston in 2009 and comparison with two estimation methods SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID LASER-INDUCED FLUORESCENCE; RO2 RADICALS; MECHANISM; HO2; UNCERTAINTY; CALIBRATION; CHEMISTRY; MASS; OH AB Net ozone production rates, P(O-3), were measured directly using the Penn State Measurement of Ozone Production Sensor (MOPS) during the Study of Houston Atmospheric Radical Precursors (SHARP, 2009). Measured P(O-3) peaked in the late morning, with values between 15 ppbv h(-1) and 100 ppbv h(-1), although values of 4080 ppbv h(-1) were typical for higher ozone days. These measurements were compared against ozone production rates calculated using measurements of hydroperoxyl (HO2), hydroxyl (OH), and nitric oxide (NO) radicals, called "calculated P(O-3)". The same comparison was done using modeled radicals obtained from a box model with the RACM2 mechanism, called " modeled P(O-3)". Measured and calculated P(O-3) had similar peak values but the calculated P(O-3) tended to peak earlier in the morning when NO values were higher. Measured and modeled P(O-3) had a similar dependence on NO, but the modeled P(O-3) was only half the measured P(O-3). The modeled P(O-3) is less than the calculated P(O3()) because the modeled HO2 is less than the measured HO2. While statistical analyses are not conclusive regarding the comparison between MOPS measurements and the two estimation methods, the calculated P(O-3) with measured HO2 produces peak values similar to the measured P(O3()) when ozone is high. Although the MOPS is new and more testing is required to verify its observations, the measurements in the SHARP field campaign show the potential of this new technique for contributing to the understanding of ozone-producing chemistry and to the monitoring of ozone's response to future air quality regulatory actions. C1 [Cazorla, M.; Brune, W. H.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Ren, X.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Coral Gables, FL 33124 USA. [Lefer, B.] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX USA. RP Cazorla, M (reprint author), NASA, Atmospher Chem & Dynam Lab, Goddard Space Flight Ctr, Greenbelt, MD USA. EM cazorla.chem@gmail.com RI Ren, Xinrong/E-7838-2015; OI Ren, Xinrong/0000-0001-9974-1666; Cazorla, Maria/0000-0001-5295-2968 FU NSF [ATM-0209972]; College of Earth and Mineral Sciences at the Pennsylvania State University; MOPS FX The authors thank the College of Earth and Mineral Sciences at the Pennsylvania State University for the Miller Faculty Fellowship, which provided graduate student support for M. C. and funds for the fabrication of MOPS. NSF grant ATM-0209972 supported the initial development of MOPS. We also thank J. Flynn, W. Luke, B. Rappengluck, T. Jobson, and others for providing measurements of NOx and VOCs used in the modeling. NR 41 TC 12 Z9 12 U1 4 U2 21 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 2 BP 1203 EP 1212 DI 10.5194/acp-12-1203-2012 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 892YL UT WOS:000300321500038 ER PT J AU Stiller, GP Kiefer, M Eckert, E von Clarmann, T Kellmann, S Garcia-Comas, M Funke, B Leblanc, T Fetzer, E Froidevaux, L Gomez, M Hall, E Hurst, D Jordan, A Kampfer, N Lambert, A McDermid, IS McGee, T Miloshevich, L Nedoluha, G Read, W Schneider, M Schwartz, M Straub, C Toon, G Twigg, LW Walker, K Whiteman, DN AF Stiller, G. P. Kiefer, M. Eckert, E. von Clarmann, T. Kellmann, S. Garcia-Comas, M. Funke, B. Leblanc, T. Fetzer, E. Froidevaux, L. Gomez, M. Hall, E. Hurst, D. Jordan, A. Kaempfer, N. Lambert, A. McDermid, I. S. McGee, T. Miloshevich, L. Nedoluha, G. Read, W. Schneider, M. Schwartz, M. Straub, C. Toon, G. Twigg, L. W. Walker, K. Whiteman, D. N. TI Validation of MIPAS IMK/IAA temperature, water vapor, and ozone profiles with MOHAVE-2009 campaign measurements SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID LIMB EMISSION-SPECTRA; ATMOSPHERIC SOUNDING MIPAS; MICHELSON INTERFEROMETER; RADIATIVE-TRANSFER; LOWER STRATOSPHERE; UPPER TROPOSPHERE; BOARD ENVISAT; RAMAN LIDAR; RETRIEVAL; MIPAS/ENVISAT AB MIPAS observations of temperature, water vapor, and ozone in October 2009 as derived with the scientific level-2 processor run by Karlsruhe Institute of Technology (KIT), Institute for Meteorology and Climate Research (IMK) and CSIC, Instituto de Astrofisica de Andalucia (IAA) and retrieved from version 4.67 level-1b data have been compared to co-located field campaign observations obtained during the MOHAVE-2009 campaign at the Table Mountain Facility near Pasadena, California in October 2009. The MIPAS measurements were validated regarding any potential biases of the profiles, and with respect to their precision estimates. The MOHAVE-2009 measurement campaign provided measurements of atmospheric profiles of temperature, water vapor/relative humidity, and ozone from the ground to the mesosphere by a suite of instruments including radiosondes, ozonesondes, frost point hygrometers, lidars, microwave radiometers and Fourier transform infrared (FTIR) spectrometers. For MIPAS temperatures (version V4O_T_204), no significant bias was detected in the middle stratosphere; between 22 km and the tropopause MIPAS temperatures were found to be biased low by up to 2 K, while below the tropopause, they were found to be too high by the same amount. These findings confirm earlier comparisons of MIPAS temperatures to ECMWF data which revealed similar differences. Above 12 km up to 45 km, MIPAS water vapor (version V4O_H2O_203) is well within 10% of the data of all correlative instruments. The well-known dry bias of MIPAS water vapor above 50 km due to neglect of non-LTE effects in the current retrievals has been confirmed. Some instruments indicate that MIPAS water vapor might be biased high by 20 to 40% around 10 km (or 5 km below the tropopause), but a consistent picture from all comparisons could not be derived. MIPAS ozone (version V4O_O3_202) has a high bias of up to +0.9 ppmv around 37 km which is due to a non-identified continuum like radiance contribution. No further significant biases have been detected. Cross-comparison to co-located observations of other satellite instruments (Aura/MLS, ACE-FTS, AIRS) is provided as well. C1 [Stiller, G. P.; Kiefer, M.; Eckert, E.; von Clarmann, T.; Kellmann, S.; Schneider, M.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, Karlsruhe, Germany. [Garcia-Comas, M.; Funke, B.] CSIC, Inst Astrofis Andalucia, Granada, Spain. [Leblanc, T.; McDermid, I. S.] CALTECH, Jet Prop Lab, Wrightwood, CA USA. [Fetzer, E.; Froidevaux, L.; Lambert, A.; Read, W.; Schwartz, M.; Toon, G.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Hall, E.; Hurst, D.; Jordan, A.] NOAA, Earth Syst Res Lab, Global Monitoring Div, Boulder, CO USA. [Hall, E.; Hurst, D.; Jordan, A.] Univ Colorado, CIRES, Boulder, CO 80309 USA. [Kaempfer, N.; Straub, C.] Univ Bern, Inst Appl Phys, CH-3012 Bern, Switzerland. [McGee, T.; Whiteman, D. N.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Miloshevich, L.] Milo Sci LLC, Lafayette, CO USA. [Gomez, M.; Nedoluha, G.] USN, Res Lab, Washington, DC 20375 USA. [Twigg, L. W.] Sci Syst & Applicat Inc, Lanham, MD USA. [Walker, K.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A1, Canada. RP Stiller, GP (reprint author), Karlsruhe Inst Technol, Inst Meteorol & Climate Res, Karlsruhe, Germany. EM gabriele.stiller@kit.edu RI Stiller, Gabriele/A-7340-2013; von Clarmann, Thomas/A-7287-2013; Kiefer, Michael/A-7254-2013; Schneider, Matthias/B-1441-2013; McGee, Thomas/G-4951-2013; Garcia-Comas, Maya/E-4050-2014; Funke, Bernd/C-2162-2008; Hurst, Dale/D-1554-2016; Schwartz, Michael/F-5172-2016 OI Stiller, Gabriele/0000-0003-2883-6873; von Clarmann, Thomas/0000-0003-2219-3379; Garcia-Comas, Maya/0000-0003-2323-4486; Funke, Bernd/0000-0003-0462-4702; Hurst, Dale/0000-0002-6315-2322; Schwartz, Michael/0000-0001-6169-5094 FU NASA; German Federal Ministry of Education and Research [50EE0901]; Naval Research Laboratory; ESA; Canadian Space Agency (CSA); Natural Sciences and Engineering Research Council of Canada (NSERC) FX The MOHAVE-2009 campaign was partly funded by the NASA Upper Atmosphere Research Program. The work by KIT was partly funded by the German Federal Ministry of Education and Research under contract no. 50EE0901. G. E. Nedoluha and R. M. Gomez were funded by NASA under the Upper Atmosphere Research Program and by the Naval Research Laboratory. M. Garcia-Comas was supported by the CHOCOLATE project by ESA within the framework of the Changing Earth Science Network Initiative. AIRS and MLS data were obtained through the Goddard Earth Sciences Data and Information Services Center (http://daac.gsfc.nasa.gov/). The Atmospheric Chemistry Experiment (ACE), also known as SCISAT, is a Canadian-led mission mainly supported by the Canadian Space Agency (CSA) and the Natural Sciences and Engineering Research Council of Canada (NSERC). The authors acknowledge ESA for providing MIPAS L1b data. GS and TvC would like to thank F. Hase, KIT, for helpful discussions. The authors are grateful to two anonymous reviewers who helped to improve the manuscript with constructive and supportive comments. NR 59 TC 32 Z9 32 U1 0 U2 10 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 EI 1867-8548 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2012 VL 5 IS 2 BP 289 EP 320 DI 10.5194/amt-5-289-2012 PG 32 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 900HD UT WOS:000300876700003 ER PT J AU Smirnov, A Sayer, AM Holben, BN Hsu, NC Sakerin, SM Macke, A Nelson, NB Courcoux, Y Smyth, TJ Croot, P Quinn, PK Sciare, J Gulev, SK Piketh, S Losno, R Kinne, S Radionov, VF AF Smirnov, A. Sayer, A. M. Holben, B. N. Hsu, N. C. Sakerin, S. M. Macke, A. Nelson, N. B. Courcoux, Y. Smyth, T. J. Croot, P. Quinn, P. K. Sciare, J. Gulev, S. K. Piketh, S. Losno, R. Kinne, S. Radionov, V. F. TI Effect of wind speed on aerosol optical depth over remote oceans, based on data from the Maritime Aerosol Network SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID SEA-SALT AEROSOL; SATELLITE RETRIEVALS; MARINE AEROSOL; NORTH-ATLANTIC; IN-SITU; SURFACE; MODEL; AERONET; VARIABILITY; THICKNESS AB The Maritime Aerosol Network (MAN) has been collecting data over the oceans since November 2006. The MAN archive provides a valuable resource for aerosol studies in maritime environments. In the current paper we investigate correlations between ship-borne aerosol optical depth (AOD) and near-surface wind speed, either measured (on-board or from satellite) or modeled (NCEP). According to our analysis, wind speed influences columnar aerosol optical depth, although the slope of the linear regression between AOD and wind speed is not steep (similar to 0.004-0.005), even for strong winds over 10m s(-1). The relationships show significant scatter (correlation coefficients typically in the range 0.3-0.5); the majority of this scatter can be explained by the uncertainty on the input data. The various wind speed sources considered yield similar patterns. Results are in good agreement with the majority of previously published relationships between surface wind speed and ship-based or satellite-based AOD measurements. The basic relationships are similar for all the wind speed sources considered; however, the gradient of the relationship varies by around a factor of two depending on the wind data used. C1 [Smirnov, A.] Sigma Space Corp, Lanham, MD USA. [Smirnov, A.; Sayer, A. M.; Holben, B. N.; Hsu, N. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sayer, A. M.] GESTAR, Columbia, MD USA. [Sakerin, S. M.] Russian Acad Sci, Inst Atmospher Opt, Tomsk, Russia. [Macke, A.] Leibniz Inst Tropospher Res, Leipzig, Germany. [Nelson, N. B.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. [Courcoux, Y.] Univ Reunion, St Denis, Reunion. [Smyth, T. J.] Plymouth Marine Lab, Plymouth, Devon, England. [Croot, P.] Leibniz Inst Marine Sci, D-24105 Kiel, Germany. [Quinn, P. K.] NOAA PMEL, Seattle, WA USA. [Sciare, J.] Lab Sci Climat & Environm, Gif Sur Yvette, France. [Gulev, S. K.] PP Shirshov Oceanol Inst, Moscow, Russia. [Piketh, S.] Univ Witwatersrand, Johannesburg, South Africa. [Losno, R.] Univ Paris 07, Creteil, France. [Losno, R.] Univ Paris 12, Creteil, France. [Kinne, S.] Univ Hamburg, Inst Meteorol, D-2000 Hamburg, Germany. [Radionov, V. F.] Arctic & Antarctic Res Inst, St Petersburg 199226, Russia. RP Smirnov, A (reprint author), Sigma Space Corp, Lanham, MD USA. EM alexander.smirnov-1@nasa.gov RI Smyth, Tim/D-2008-2012; Smirnov, Alexander/C-2121-2009; Sayer, Andrew/H-2314-2012; Hsu, N. Christina/H-3420-2013; Nelson, Norman/B-7343-2014; Croot, Peter/C-8460-2009; Gulev, Sergey/A-4994-2014; Quinn, Patricia/R-1493-2016 OI Smirnov, Alexander/0000-0002-8208-1304; Sayer, Andrew/0000-0001-9149-1789; Nelson, Norman/0000-0003-1767-7598; Croot, Peter/0000-0003-1396-0601; Quinn, Patricia/0000-0003-0337-4895 FU NASA; AMSR-E Science Team FX The authors thank Hal Maring (NASA Headquarters) for his support of AERONET. The authors thank Kirk Knobelspiesse (Columbia University and NASA GISS) and anonymous reviewer for constructive comments. Measurements onboard R/V Marion-Dufresne were supported by the French Polar Institute (IPEV). NCEP Reanalysis data provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from their Web site at http://www.esrl.noaa.gov/psd/. AMSR-E data are produced by Remote Sensing Systems and sponsored by the NASA Earth Science MEaSUREs DISCOVER Project and the AMSR-E Science Team. Data are available at www.remss.com. Gert Konig-Langlo from Alfred Wegener Institute for Polar and Marine Research (Bremerhaven, Germany) is acknowledged for providing the meteorological data from R/V Polarstern. British Oceanographic Data Centre is acknowledged for providing AMT19 and 20 meteorological data (the data were supplied to BODC by Chris Barnard, Gareth Knights and Jon Seddon). NR 44 TC 11 Z9 13 U1 1 U2 15 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2012 VL 5 IS 2 BP 377 EP 388 DI 10.5194/amt-5-377-2012 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 900HD UT WOS:000300876700008 ER PT J AU Varnai, T Marshak, A AF Varnai, T. Marshak, A. TI Analysis of co-located MODIS and CALIPSO observations near clouds SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID AEROSOL; ALGORITHM; AIR AB This paper aims at helping synergistic studies in combining data from different satellites for gaining new insights into two critical yet poorly understood aspects of anthropogenic climate change, aerosol-cloud interactions and aerosol radiative effects. In particular, the paper examines the way cloud information from the MODIS (MODerate resolution Imaging Spectroradiometer) imager can refine our perceptions based on CALIOP (Cloud-Aerosol Lidar with Orthogonal Polarization) lidar measurements about the systematic aerosol changes that occur near clouds. The statistical analysis of a yearlong dataset of co-located global maritime observations from the Aqua and CALIPSO (Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation) satellites reveals that MODIS's multispectral imaging ability can greatly help the interpretation of CALIOP observations. The results show that imagers on Aqua and CALIPSO yield very similar pictures, and that the discrepancies - due mainly to wind drift and differences in view angle - do not significantly hinder aerosol measurements near clouds. By detecting clouds outside the CALIOP track, MODIS reveals that clouds are usually closer to clear areas than CALIOP data alone would suggest. The paper finds statistical relationships between the distances to clouds in MODIS and CALIOP data, and proposes a rescaling approach to statistically account for the impact of clouds outside the CALIOP track even when MODIS cannot reliably detect low clouds, for example at night or over sea ice. Finally, the results show that the typical distance to clouds depends on both cloud coverage and cloud type, and accordingly varies with location and season. In maritime areas perceived cloud free, the global median distance to clouds below 3 km altitude is in the 4-5 km range. C1 [Varnai, T.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Marshak, A.] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD USA. RP Varnai, T (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. EM tamas.varnai@nasa.gov RI Marshak, Alexander/D-5671-2012 FU NASA; NASA CALIPSO FX We gratefully acknowledge support for this research by the NASA Radiation Sciences Program managed by Hal Maring and by the NASA CALIPSO project supervised by Charles Trepte as the technical officer. NR 25 TC 11 Z9 11 U1 1 U2 9 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2012 VL 5 IS 2 BP 389 EP 396 DI 10.5194/amt-5-389-2012 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 900HD UT WOS:000300876700009 ER PT J AU Worden, J Kulawik, S Frankenberg, C Payne, V Bowman, K Cady-Peirara, K Wecht, K Lee, JE Noone, D AF Worden, J. Kulawik, S. Frankenberg, C. Payne, V. Bowman, K. Cady-Peirara, K. Wecht, K. Lee, J. -E. Noone, D. TI Profiles of CH4, HDO, H2O, and N2O with improved lower tropospheric vertical resolution from Aura TES radiances SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID EMISSION SPECTROMETER; MICHELSON INTERFEROMETER; TROPICAL TROPOPAUSE; METHANE EMISSIONS; NADIR RETRIEVALS; HDO/H2O RATIOS; WATER-VAPOR; SATELLITE; CO2; SPACE AB Thermal infrared (IR) radiances measured near 8 microns contain information about the vertical distribution of water vapor (H2O), the water isotopologue HDO, and methane (CH4), key gases in the water and carbon cycles. Previous versions (Version 4 or less) of the TES profile retrieval algorithm used a "spectral-window" approach to minimize uncertainty from interfering species at the expense of reduced vertical resolution and sensitivity. In this manuscript we document changes to the vertical resolution and uncertainties of the TES version 5 retrieval algorithm. In this version (Version 5), joint estimates of H2O, HDO, CH4 and nitrous oxide (N2O) are made using radiances from almost the entire spectral region between 1100 cm(-1) and 1330 cm(-1). The TES retrieval constraints are also modified in order to better use this information. The new H2O estimates show improved vertical resolution in the lower troposphere and boundary layer, while the new HDO/H2O estimates can now profile the HDO/H2O ratio between 925 hPa and 450 hPa in the tropics and during summertime at high latitudes. The new retrievals are now sensitive to methane in the free troposphere between 800 and 150 mb with peak sensitivity near 500 hPa; whereas in previous versions the sensitivity peaked at 200 hPa. However, the upper troposphere methane concentrations are biased high relative to the lower troposphere by approximately 4% on average. This bias is likely related to temperature, calibration, and/or methane spectroscopy errors. This bias can be mitigated by normalizing the CH4 estimate by the ratio of the N2O estimate relative to the N2O prior, under the assumption that the same systematic error affects both the N2O and CH4 estimates. We demonstrate that applying this ratio theoretically reduces the CH4 estimate for non-retrieved parameters that jointly affect both the N2O and CH4 estimates. The relative upper troposphere to lower troposphere bias is approximately 2.8% after this bias correction. Quality flags based upon the vertical variability of the methane and N2O estimates can be used to reduce this bias further. While these new CH4, HDO/H2O, and H2O estimates are consistent with previous TES retrievals in the altitude regions where the sensitivities overlap, future comparisons with independent profile measurement will be required to characterize the biases of these new retrievals and determine if the calculated uncertainties using the new constraints are consistent with actual uncertainties. C1 [Worden, J.; Kulawik, S.; Frankenberg, C.; Bowman, K.; Lee, J. -E.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Payne, V.; Cady-Peirara, K.] Atmospher & Environm Res Inc, Lexington, MA USA. [Wecht, K.] Harvard Univ, Dept Earth & Planetary Sci Front Harvard, Cambridge, MA 02138 USA. [Noone, D.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Noone, D.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. RP Worden, J (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM john.worden@jpl.nasa.gov RI Frankenberg, Christian/A-2944-2013; Payne, Vivienne/D-9713-2012; Lee, Jung-Eun/F-8981-2012 OI Frankenberg, Christian/0000-0002-0546-5857; FU National Aeronautics and Space Administration FX Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The NASA ROSES Aura Science Team NNH07ZDA001N-AST 07-AST07-0069 contributed to the support of the analysis. NR 53 TC 57 Z9 59 U1 2 U2 19 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2012 VL 5 IS 2 BP 397 EP 411 DI 10.5194/amt-5-397-2012 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 900HD UT WOS:000300876700010 ER PT J AU Piters, AJM Boersma, KF Kroon, M Hains, JC Van Roozendael, M Wittrock, F Abuhassan, N Adams, C Akrami, M Allaart, MAF Apituley, A Beirle, S Bergwerff, JB Berkhout, AJC Brunner, D Cede, A Chong, J Clemer, K Fayt, C Friess, U Gast, LFL Gil-Ojeda, M Goutail, F Graves, R Griesfeller, A Grossmann, K Hemerijckx, G Hendrick, F Henzing, B Herman, J Hermans, C Hoexum, M van der Hoff, GR Irie, H Johnston, PV Kanaya, Y Kim, YJ Baltink, HK Kreher, K de Leeuw, G Leigh, R Merlaud, A Moerman, MM Monks, PS Mount, GH Navarro-Comas, M Oetjen, H Pazmino, A Perez-Camacho, M Peters, E du Piesanie, A Pinardi, G Puentedura, O Richter, A Roscoe, HK Schonhardt, A Schwarzenbach, B Shaiganfar, R Sluis, W Spinei, E Stolk, AP Strong, K Swart, DPJ Takashima, H Vlemmix, T Vrekoussis, M Wagner, T Whyte, C Wilson, KM Yela, M Yilmaz, S Zieger, P Zhou, Y AF Piters, A. J. M. Boersma, K. F. Kroon, M. Hains, J. C. Van Roozendael, M. Wittrock, F. Abuhassan, N. Adams, C. Akrami, M. Allaart, M. A. F. Apituley, A. Beirle, S. Bergwerff, J. B. Berkhout, A. J. C. Brunner, D. Cede, A. Chong, J. Clemer, K. Fayt, C. Friess, U. Gast, L. F. L. Gil-Ojeda, M. Goutail, F. Graves, R. Griesfeller, A. Grossmann, K. Hemerijckx, G. Hendrick, F. Henzing, B. Herman, J. Hermans, C. Hoexum, M. van der Hoff, G. R. Irie, H. Johnston, P. V. Kanaya, Y. Kim, Y. J. Baltink, H. Klein Kreher, K. de Leeuw, G. Leigh, R. Merlaud, A. Moerman, M. M. Monks, P. S. Mount, G. H. Navarro-Comas, M. Oetjen, H. Pazmino, A. Perez-Camacho, M. Peters, E. du Piesanie, A. Pinardi, G. Puentedura, O. Richter, A. Roscoe, H. K. Schoenhardt, A. Schwarzenbach, B. Shaiganfar, R. Sluis, W. Spinei, E. Stolk, A. P. Strong, K. Swart, D. P. J. Takashima, H. Vlemmix, T. Vrekoussis, M. Wagner, T. Whyte, C. Wilson, K. M. Yela, M. Yilmaz, S. Zieger, P. Zhou, Y. TI The Cabauw Intercomparison campaign for Nitrogen Dioxide measuring Instruments (CINDI): design, execution, and early results SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID MAX-DOAS MEASUREMENTS; ZENITH-SKY UV; SLANT COLUMN MEASUREMENTS; IN-SITU; VISIBLE SPECTROMETERS; AEROSOL EXTINCTION; TROPOSPHERIC NO2; POLAR CIRCLE; RETRIEVAL; VALIDATION AB From June to July 2009 more than thirty different in-situ and remote sensing instruments from all over the world participated in the Cabauw Intercomparison campaign for Nitrogen Dioxide measuring Instruments (CINDI). The campaign took place at KNMI's Cabauw Experimental Site for Atmospheric Research (CESAR) in the Netherlands. Its main objectives were to determine the accuracy of state-of-the-art ground-based measurement techniques for the detection of atmospheric nitrogen dioxide (both in-situ and remote sensing), and to investigate their usability in satellite data validation. The expected outcomes are recommendations regarding the operation and calibration of such instruments, retrieval settings, and observation strategies for the use in ground-based networks for air quality monitoring and satellite data validation. Twenty-four optical spectrometers participated in the campaign, of which twenty-one had the capability to scan different elevation angles consecutively, the so-called Multi-axis DOAS systems, thereby collecting vertical profile information, in particular for nitrogen dioxide and aerosol. Various in-situ samplers and lidar instruments simultaneously characterized the variability of atmospheric trace gases and the physical properties of aerosol particles. A large data set of continuous measurements of these atmospheric constituents has been collected under various meteorological conditions and air pollution levels. Together with the permanent measurement capability at the CESAR site characterizing the meteorological state of the atmosphere, the CINDI campaign provided a comprehensive observational data set of atmospheric constituents in a highly polluted region of the world during summertime. First detailed comparisons performed with the CINDI data show that slant column measurements of NO2, O-4 and HCHO with MAX-DOAS agree within 5 to 15 %, vertical profiles of NO2 derived from several independent instruments agree within 25% of one another, and MAX-DOAS aerosol optical thickness agrees within 20-30% with AERONET data. For the in-situ NO2 instrument using a molybdenum converter, a bias was found as large as 5 ppbv during day time, when compared to the other in-situ instruments using photolytic converters. C1 [Piters, A. J. M.; Boersma, K. F.; Kroon, M.; Allaart, M. A. F.; Apituley, A.; Baltink, H. Klein; du Piesanie, A.; Sluis, W.; Vlemmix, T.; Wilson, K. M.] Royal Netherlands Meteorol Inst KNMI, De Bilt, Netherlands. [Boersma, K. F.] TUE, Eindhoven, Netherlands. [Hains, J. C.] MDE, Baltimore, MD USA. [Van Roozendael, M.; Clemer, K.; Fayt, C.; Hemerijckx, G.; Hendrick, F.; Hermans, C.; Merlaud, A.; Pinardi, G.] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium. [Wittrock, F.; Peters, E.; Richter, A.; Schoenhardt, A.; Vrekoussis, M.] Univ Bremen, Inst Environm Phys IUP, D-28359 Bremen, Germany. [Abuhassan, N.] MSU, Baltimore, MD USA. [Abuhassan, N.; Cede, A.; Herman, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Adams, C.; Akrami, M.; Strong, K.; Whyte, C.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Gil-Ojeda, M.; Navarro-Comas, M.; Perez-Camacho, M.; Puentedura, O.; Yela, M.] Natl Inst Aerosp Technol INTA, Madrid, Spain. [Apituley, A.; Bergwerff, J. B.; Berkhout, A. J. C.; Gast, L. F. L.; Hoexum, M.; van der Hoff, G. R.; Stolk, A. P.; Swart, D. P. J.; Wilson, K. M.] Natl Inst Publ Hlth & Environm RIVM, Bilthoven, Netherlands. [Brunner, D.; Schwarzenbach, B.; Zhou, Y.] Swiss Fed Labs Mat Sci & Technol EMPA, Dubendorff, Switzerland. [Cede, A.; Herman, J.] UMBC, Catonsville, MD USA. [Chong, J.; Kim, Y. J.] Gwangju Inst Sci & Technol, Gwangiu, South Korea. [Friess, U.; Grossmann, K.; Yilmaz, S.] Heidelberg Univ, Inst Environm Phys, Heidelberg, Germany. [Goutail, F.; Griesfeller, A.; Pazmino, A.] Lab Atmospheres Milieux Observat Spatiales LATMOS, Guyancourt, France. [Graves, R.; Leigh, R.; Monks, P. S.] Univ Leicester, Dept Chem, Leicester LE1 7RH, Leics, England. [Henzing, B.; de Leeuw, G.; Moerman, M. M.] Netherlands Org Appl Sci Res TNO, Utrecht, Netherlands. [Irie, H.; Kanaya, Y.; Takashima, H.] JAMSTEC, Res Inst Global Change, Yokohama, Kanagawa, Japan. [Johnston, P. V.; Kreher, K.] Natl Inst Water & Atmospher Res NIWA, Lauder, New Zealand. [de Leeuw, G.] FMI, Helsinki, Finland. [Mount, G. H.; Spinei, E.] WSU, Lab Atmospher Res, Pullman, WA USA. [Oetjen, H.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England. [Roscoe, H. K.] BAS, Cambridge, England. [Beirle, S.; Shaiganfar, R.; Wagner, T.] MPIC, Mainz, Germany. [Zieger, P.] PSI, Lab Atmospher Chem, Villigen, Switzerland. [Vrekoussis, M.] Acad Athens, Res Ctr Atmospher Phys & Climatol, Athens, Greece. [de Leeuw, G.] Univ Helsinki, Dept Phys, Helsinki, Finland. RP Piters, AJM (reprint author), Royal Netherlands Meteorol Inst KNMI, De Bilt, Netherlands. EM piters@knmi.nl RI Puentedura, Olga/J-6884-2014; Kanaya, Yugo/C-7446-2012; Zieger, Paul/C-3408-2011; Strong, Kimberly/D-2563-2012; Brunner, Dominik/A-1255-2009; Boersma, Klaas/H-4559-2012; Wittrock, Folkard/B-6959-2008; Richter, Andreas/C-4971-2008; Navarro-Comas, Monica/J-6297-2014; Oetjen, Hilke/H-3708-2016; Monks, Paul/H-6468-2016; Yela, Margarita/J-7346-2016; Vrekoussis, Mihalis/G-9424-2012 OI Herman, Jay/0000-0002-9146-1632; Puentedura, Olga/0000-0002-4286-1867; Zieger, Paul/0000-0001-7000-6879; Brunner, Dominik/0000-0002-4007-6902; Boersma, Klaas/0000-0002-4591-7635; Wittrock, Folkard/0000-0002-3024-0211; Richter, Andreas/0000-0003-3339-212X; Navarro-Comas, Monica/0000-0002-6347-8955; Oetjen, Hilke/0000-0002-3542-1337; Monks, Paul/0000-0001-9984-4390; Yela, Margarita/0000-0003-3775-3156; Vrekoussis, Mihalis/0000-0001-8292-8352 NR 50 TC 26 Z9 26 U1 1 U2 25 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2012 VL 5 IS 2 BP 457 EP 485 DI 10.5194/amt-5-457-2012 PG 29 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 900HD UT WOS:000300876700014 ER PT J AU Colgan, W Rajaram, H Anderson, RS Steffen, K Zwally, HJ Phillips, T Abdalati, W AF Colgan, William Rajaram, Harihar Anderson, Robert S. Steffen, Konrad Zwally, H. Jay Phillips, Thomas Abdalati, Waleed TI The annual glaciohydrology cycle in the ablation zone of the Greenland ice sheet: Part 2. Observed and modeled ice flow SO JOURNAL OF GLACIOLOGY LA English DT Article ID SUBGLACIAL WATER-PRESSURE; JAKOBSHAVN ISBRAE; OUTLET GLACIER; SURFACE MELT; BASAL MOTION; SPEED-UP; ACCELERATION; TEMPERATURE; DYNAMICS; VELOCITY AB Ice velocities observed in 2005/06 at three GPS stations along the Sermeq Avannarleq flowline, West Greenland, are used to characterize an observed annual velocity cycle. We attempt to reproduce this annual ice velocity cycle using a 1-D ice-flow model with longitudinal stresses coupled to a 1-D hydrology model that governs an empirical basal sliding rule. Seasonal basal sliding velocity is parameterized as a perturbation of prescribed winter sliding velocity that is proportional to the rate of change of glacier water storage. The coupled model reproduces the broad features of the annual basal sliding cycle observed along this flowline, namely a summer speed-up event followed by a fall slowdown event. We also evaluate the hypothesis that the observed annual velocity cycle is due to the annual calving cycle at the terminus. We demonstrate that the ice acceleration due to a catastrophic calving event takes an order of magnitude longer to reach CU/ETH ('Swiss') Camp (46 km upstream of the terminus) than is observed. The seasonal acceleration observed at Swiss Camp is therefore unlikely to be the result of velocity perturbations propagated upstream via longitudinal coupling. Instead we interpret this velocity cycle to reflect the local history of glacier water balance. C1 [Colgan, William; Steffen, Konrad; Phillips, Thomas; Abdalati, Waleed] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Colgan, William; Steffen, Konrad; Abdalati, Waleed] Univ Colorado, Dept Geog, Boulder, CO 80309 USA. [Rajaram, Harihar] Univ Colorado, Dept Civil Environm & Architectural Engn, Boulder, CO 80309 USA. [Anderson, Robert S.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Anderson, Robert S.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Zwally, H. Jay] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Abdalati, Waleed] NASA, Washington, DC 20546 USA. RP Colgan, W (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. EM william.colgan@colorado.edu RI Colgan, William/H-1570-2014; Steffen, Konrad/C-6027-2013 OI Colgan, William/0000-0001-6334-1660; Steffen, Konrad/0000-0001-8658-1026 FU NASA [NNX08AT85G, NNX07AF15G]; US National Science Foundation (NSF) [DDRI 0926911]; Natural Sciences and Engineering Research Council (NSERC) of Canada; Cooperative Institute for Research in Environmental Sciences (CIRES); NSF [EAR 0922126] FX This work was supported by NASA Cryospheric Science Program grants NNX08AT85G and NNX07AF15G to K.S. and US National Science Foundation (NSF) DDRI 0926911 to W.C. W.C. thanks the Natural Sciences and Engineering Research Council (NSERC) of Canada for support through a Post-Graduate Scholarship, and the Cooperative Institute for Research in Environmental Sciences (CIRES) for support through a Graduate Research Fellowship. R.S.A. acknowledges support through NSF grant EAR 0922126. We thank Gwenn Flowers and an anonymous reviewer for thorough insights on the manuscript. Helen Fricker was our scientific editor. NR 56 TC 16 Z9 16 U1 1 U2 17 PU INT GLACIOL SOC PI CAMBRIDGE PA LENSFIELD RD, CAMBRIDGE CB2 1ER, ENGLAND SN 0022-1430 EI 1727-5652 J9 J GLACIOL JI J. Glaciol. PY 2012 VL 58 IS 207 BP 51 EP 64 DI 10.3189/2012JoG11J081 PG 14 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 898QV UT WOS:000300757800005 ER PT J AU Palamara, L Manderson, J Kohut, J Oliver, MJ Gray, S Goff, J AF Palamara, Laura Manderson, John Kohut, Josh Oliver, Matthew J. Gray, Steven Goff, John TI Improving habitat models by incorporating pelagic measurements from coastal ocean observatories SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Habitat characteristics; Pelagic; Remote sensing; Spatial fisheries management; Canonical correspondence analysis; CCA; Mid-Atlantic Bight ID MID-ATLANTIC BIGHT; MARINE ECOSYSTEM; VARIABILITY; BEHAVIOR; NETWORK; RADAR AB As in all temperate coastal seas, habitats in the Mid-Atlantic Bight are spatially and temporally dynamic. Understanding how species respond to the dynamics of their environment is important for developing effective management strategies. In this study, we used canonical correspondence analysis (CCA) to determine habitat variables most important in explaining variation in fish and invertebrate communities sampled with bottom trawls. We also quantified the relative explanatory power of seabed habitat features, pelagic features measured in situ and pelagic features measured remotely, all of which can be used to explain species variability. Pelagic habitat features, most notably surface and bottom temperature and stratification, explained 76% of the community variation observed, compared with 40.9% explained by seabed features, mainly depth. Remotely sensed pelagic characteristics explained 46.9% of the variation that was accounted for and were redundant for features measured in situ; this suggests that remotely sensed features are representative of features measured in situ including certain subsurface features. Cross-shelf and seasonal variation in environmental variables were the major predictors of species distributions and accounted for 71.3% of the total explained community variation. We described the seasonal dynamics of important habitat gradients and the responses of species with different habitat requirements and geographic range distributions to those gradients. We argue that consideration of dynamic pelagic features in addition to slowly changing features is important. Dynamic approaches are necessary for effective management and ocean observing systems can be used to develop dynamic space-based management strategies. C1 [Palamara, Laura; Kohut, Josh] Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08901 USA. [Manderson, John] NOAA, Natl Marine Fisheries Serv, NE Fisheries Sci Ctr, Ecosyst Proc Div,James J Howard Marine Sci Lab, Highlands, NJ 07732 USA. [Oliver, Matthew J.] Univ Delaware, Coll Earth Ocean & Environm, Lewes, DE 19958 USA. [Gray, Steven] Univ Hawaii, Dept Nat Resources & Environm Management, Honolulu, HI 96822 USA. [Goff, John] Univ Texas Austin, Inst Geophys, Jackson Sch Geosci, Austin, TX 78758 USA. RP Palamara, L (reprint author), Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08901 USA. EM palamara@marine.rutgers.edu FU NOAA Fisheries and the Environment [FATE NA08NMF450626]; NASA Biodiversity [NNG06GH75G1/3]; NASA [NNH07ZDA001N]; US IOOS [MARACOOS NA07NOS4730221, MARACOOS NA10NOS4730014, MARACOOS NA11NOS0120038]; Delaware Sea Grant [NA10OAR4170084] FX The authors thank the following agencies for support during this project: NOAA Fisheries and the Environment (FATE NA08NMF450626) for primary support, as well as NASA Biodiversity (NNG06GH75G1/3), NASA New Investigator Program (NNH07ZDA001N), US IOOS Program (MARACOOS NA07NOS4730221, MARACOOS NA10NOS4730014 and MARACOOS NA11NOS0120038) and Delaware Sea Grant (NA10OAR4170084). RU COOL, usSEABED, National Geophysical Data Center and M. Taylor, B. Phelan and S. Lucey at NOAA-NEFSC provided data used in the analysis. We also thank H. Fuchs, J. Manning and anonymous reviewers for their comments and advice. NR 49 TC 8 Z9 9 U1 1 U2 23 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2012 VL 447 BP 15 EP 30 DI 10.3354/meps09496 PG 16 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 897OG UT WOS:000300660600002 ER PT J AU Bodkin, JL Ballachey, BE Coletti, HA Esslinger, GG Kloecker, KA Rice, SD Reed, JA Monson, DH AF Bodkin, James L. Ballachey, Brenda E. Coletti, Heather A. Esslinger, George G. Kloecker, Kimberly A. Rice, Stanley D. Reed, John A. Monson, Daniel H. TI Long-term effects of the 'Exxon Valdez' oil spill: sea otter foraging in the intertidal as a pathway of exposure to lingering oil SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Sea otter; 'Exxon Valdez'; Oil spill; Enhydra lutris; Time-depth recorder; TDR ID PRINCE-WILLIAM-SOUND; CRUDE-OIL; PROTOTHACA-STAMINEA; HARLEQUIN DUCKS; FOOD LIMITATION; ENHYDRA-LUTRIS; ALASKA; HYDROCARBONS; RECOVERY; MORTALITY AB The protracted recovery of some bird and mammal populations in western Prince William Sound (WPWS), Alaska, and the persistence of spilled 'Exxon Valdez' oil in intertidal sediments, suggests a pathway of exposure to consumers that occupy nearshore habitats. To evaluate the hypothesis that sea otter (Enhydra lutris) foraging allows access to lingering oil, we contrast spatial relations between foraging behavior and documented oil distribution. We recovered archival time-depth recorders implanted in 19 sea otters in WPWS, where lingering oil and delayed ecosystem recovery are well documented. Sea otter foraging dives ranged from +2.7 to -92 m below sea level (MLLW), with intertidal accounting for 5 to 38% of all foraging. On average, female sea otters made 16 050 intertidal dives per year and 18% of these dives were at depths above the +0.80 m tidal elevation. Males made 4100 intertidal dives per year and 26% of intertidal foraging took place at depths above the +0.80 m tidal elevation. Estimated annual oil encounter rates ranged from 2 to 24 times yr(-1) for females, and 2 to 4 times yr(-1) for males. Exposure rates increased in spring when intertidal foraging doubled and females were with small pups. In summer 2008, we found sea otter foraging pits on 13.5 of 24.8 km of intertidal shoreline surveyed. Most pits (82%) were within 0.5 m of the zero tidal elevation and 15% were above 0.5 m, the level above which most (65%) lingering oil remains. In August 2008, we detected oil above background concentrations in 18 of 41 (44%) pits excavated by sea otters on beaches with prior evidence of oiling, with total PAH concentrations up to 56 000 ng g(-1) dry weight. Our estimates of intertidal foraging, the widespread presence of foraging pits in the intertidal, and the presence of oil in and near sea otter foraging pits documents a pathway of exposure from lingering intertidal oil to sea otters foraging in WPWS. C1 [Bodkin, James L.; Ballachey, Brenda E.; Esslinger, George G.; Kloecker, Kimberly A.; Reed, John A.; Monson, Daniel H.] US Geol Survey, Alaska Sci Ctr, Anchorage, AK 99508 USA. [Rice, Stanley D.] Natl Marine Fisheries Serv, Auke Bay Lab, Juneau, AK 99801 USA. RP Bodkin, JL (reprint author), US Geol Survey, Alaska Sci Ctr, 4210 Univ Dr, Anchorage, AK 99508 USA. EM jbodkin@usgs.gov RI Monson, Daniel/N-4469-2013; OI Monson, Daniel/0000-0002-4593-5673; Kloecker, Kimberly/0000-0002-2461-968X FU US Geological Survey; Alaska Science Center; Exxon Valdez Oil Spill Trustee Council FX This work was supported by the US Geological Survey, Alaska Science Center and the Exxon Valdez Oil Spill Trustee Council; however, the findings and conclusions do not necessarily reflect the views or position of the Trustee Council. Any use of trade names is for descriptive purposes only and does not represent endorsement by the US government. We gratefully acknowledge the assistance of J. deLaBruere, B. Hatfield, P. Kearney, M. Kenner and B. Uher-Koch for their significant contributions to sea otter captures and field data collection, to M. Murray and P. Snyder for veterinary procedures, and to J. Coffey for TDR data calibration. We appreciate the thoughtful reviews of this work by L. Bowen, D. Esler, K. Oakley, and 3 anonymous colleagues. NR 67 TC 21 Z9 22 U1 7 U2 93 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2012 VL 447 BP 273 EP 287 DI 10.3354/meps09523 PG 15 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 897OG UT WOS:000300660600019 ER PT J AU Mohapatra, BR La Duc, MT AF Mohapatra, Bidyut R. La Duc, Myron T. TI Evaluation of fluorescence in situ hybridization to detect encapsulated Bacillus pumilus SAFR-032 spores released from poly(methylmethacrylate) SO MICROBIOLOGY AND IMMUNOLOGY LA English DT Article DE Bacillus pumilus; bioburden; fluorescence in situ hybridization (FISH); spore ID SPACECRAFT ASSEMBLY FACILITY; VIABLE SPORES; RESISTANCE; CELLS; MICROORGANISMS; IDENTIFICATION; MICROBIOLOGY; ENVIRONMENTS; ENDOSPORES; VIABILITY AB Bacillus pumilus SAFR-032 spores originally isolated from the Jet Propulsion Laboratory spacecraft assembly facility clean room are extremely resistant to UV radiation, H2O2, desiccation, chemical disinfection and starvation compared to spores of other Bacillus species. The resistance of B. pumilus SAFR-032 spores to standard industrial clean room sterilization practices is not only a major concern for medical, pharmaceutical and food industries, but also a threat to the extraterrestrial environment during search for life via spacecraft. The objective of the present study was to investigate the potential of Alexa-FISH (fluorescence in situ hybridization with Alexa Fluor (R) 488 labeled oligonucleotide) method as a molecular diagnostic tool for enumeration of multiple sterilant-resistant B. pumilus SAFR-032 spores artificially encapsulated in, and released via organic solvent from, a model polymeric material: poly(methylmethacrylate) (Lucite, Plexiglas). Plexiglas is used extensively in various aerospace applications and in medical, pharmaceutical and food industries. Alexa-FISH signals were not detected from spores via standard methods for vegetative bacterial cells. Optimization of a spore permeabilization protocol capitalizing on the synergistic action of proteinase-K, lysozyme, mutanolysin and Triton X-100 facilitated efficient spore detection by Alexa-FISH microscopy. Neither of the Alexa-probes tested gave rise to considerable levels of Lucite- or solvent-associated background autofluorescence, demonstrating the immense potential of Alexa-FISH for rapid quantification of encapsulated B. pumilus SAFR-032 spores released from poly(methylmethacrylate). C1 [Mohapatra, Bidyut R.; La Duc, Myron T.] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA. RP Mohapatra, BR (reprint author), Univ S Alabama, Dauphin Isl Sea Lab, 101 Bienville Blvd, Dauphin Isl, AL 36528 USA. EM bmohapatra@disl.org FU NRA ROSES FX The authors thank Drs K. Venkateswaran, C. Stam and M. Cooper for valuable advice and consultation, and Dr C. Conley for helpful insight and discussion. 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. This research was funded by a 2007 NRA ROSES grant. NR 37 TC 7 Z9 7 U1 3 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0385-5600 J9 MICROBIOL IMMUNOL JI Microbiol. Immunol. PD JAN PY 2012 VL 56 IS 1 BP 40 EP 47 DI 10.1111/j.1348-0421.2011.00404.x PG 8 WC Immunology; Microbiology SC Immunology; Microbiology GA 895NZ UT WOS:000300504400005 PM 22145981 ER PT J AU Choi, S Wang, Y Salawitch, RJ Canty, T Joiner, J Zeng, T Kurosu, TP Chance, K Richter, A Huey, LG Liao, J Neuman, JA Nowak, JB Dibb, JE Weinheimer, AJ Diskin, G Ryerson, TB da Silva, A Curry, J Kinnison, D Tilmes, S Levelt, PF AF Choi, S. Wang, Y. Salawitch, R. J. Canty, T. Joiner, J. Zeng, T. Kurosu, T. P. Chance, K. Richter, A. Huey, L. G. Liao, J. Neuman, J. A. Nowak, J. B. Dibb, J. E. Weinheimer, A. J. Diskin, G. Ryerson, T. B. da Silva, A. Curry, J. Kinnison, D. Tilmes, S. Levelt, P. F. TI Analysis of satellite-derived Arctic tropospheric BrO columns in conjunction with aircraft measurements during ARCTAS and ARCPAC SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID OZONE DEPLETION EVENTS; STRATOSPHERIC BROMINE MONOXIDE; RADIATIVE-TRANSFER MODEL; SUNRISE EXPERIMENT 1992; BOUNDARY-LAYER; SEA-ICE; POLAR SUNRISE; GLOBAL OBSERVATIONS; MONITORING EXPERIMENT; LIMB MEASUREMENTS AB We derive tropospheric column BrO during the ARCTAS and ARCPAC field campaigns in spring 2008 using retrievals of total column BrO from the satellite UV nadir sensors OMI and GOME-2 using a radiative transfer model and stratospheric column BrO from a photochemical simulation. We conduct a comprehensive comparison of satellite-derived tropospheric BrO column to aircraft in-situ observations of BrO and related species. The aircraft profiles reveal that tropospheric BrO, when present during April 2008, was distributed over a broad range of altitudes rather than being confined to the planetary boundary layer (PBL). Perturbations to the total column resulting from tropospheric BrO are the same magnitude as perturbations due to longitudinal variations in the stratospheric component, so proper accounting of the stratospheric signal is essential for accurate determination of satellite-derived tropospheric BrO. We find reasonably good agreement between satellite-derived tropospheric BrO and columns found using aircraft in-situ BrO profiles, particularly when satellite radiances were obtained over bright surfaces (albedo >0.7), for solar zenith angle <80 degrees and clear sky conditions. The rapid activation of BrO due to surface processes (the bromine explosion) is apparent in both the OMI and GOME-2 based tropospheric columns. The wide orbital swath of OMI allows examination of the evolution of tropospheric BrO on about hourly time intervals near the pole. Low surface pressure, strong wind, and high PBL height are associated with an observed BrO activation event, supporting the notion of bromine activation by high winds over snow. C1 [Choi, S.; Wang, Y.; Zeng, T.; Huey, L. G.; Liao, J.; Curry, J.] Georgia Inst Technol, Atlanta, GA 30332 USA. [Salawitch, R. J.; Canty, T.] Univ Maryland, College Pk, MD 20742 USA. [Joiner, J.; da Silva, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kurosu, T. P.; Chance, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Richter, A.] Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. [Neuman, J. A.; Nowak, J. B.] Univ Colorado, CIRES, Boulder, CO 80309 USA. [Neuman, J. A.; Nowak, J. B.; Ryerson, T. B.] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Dibb, J. E.] Univ New Hampshire, Durham, NH 03824 USA. [Weinheimer, A. J.; Kinnison, D.; Tilmes, S.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Diskin, G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Levelt, P. F.] Royal Netherlands Meteorol Inst KNMI, De Bilt, Netherlands. [Levelt, P. F.] Univ Technol Eindhoven, Eindhoven, Netherlands. RP Choi, S (reprint author), Georgia Inst Technol, Atlanta, GA 30332 USA. RI Wang, Yuhang/B-5578-2014; Nowak, John/B-1085-2008; Canty, Timothy/F-2631-2010; da Silva, Arlindo/D-6301-2012; Joiner, Joanna/D-6264-2012; Salawitch, Ross/B-4605-2009; Liao, Jin/H-4865-2013; Neuman, Andy/A-1393-2009; Manager, CSD Publications/B-2789-2015; Ryerson, Tom/C-9611-2009; Richter, Andreas/C-4971-2008 OI Chance, Kelly/0000-0002-7339-7577; Nowak, John/0000-0002-5697-9807; Canty, Timothy/0000-0003-0618-056X; da Silva, Arlindo/0000-0002-3381-4030; Salawitch, Ross/0000-0001-8597-5832; Neuman, Andy/0000-0002-3986-1727; Richter, Andreas/0000-0003-3339-212X FU National Aeronautics and Space Administration (NASA); National Oceanic and Atmospheric Administration (NOAA); Smithsonian Institution FX This work was supported by the National Aeronautics and Space Administration (NASA) IPY, ARCTAS, and Aura science team programs, National Oceanic and Atmospheric Administration (NOAA) ARCPAC program, GEST GSSP program, and Smithsonian Institution. The authors are grateful to the NASA GMAO reanalysis processing teams as well as the GOME-2, OMI, and MODIS data processing teams for providing data sets. The authors also appreciate numerous helpful discussions with George Mount. We also thank Nicolas Theys for sharing his calculations of stratospheric column BrO and for many helpful email exchanges. Finally, the authors express special thanks to the two anonymous referees and editor Jan W. Bottenheim for valuable comments that improved this paper. NR 98 TC 25 Z9 25 U1 2 U2 23 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 3 BP 1255 EP 1285 DI 10.5194/acp-12-1255-2012 PG 31 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 897ND UT WOS:000300656500004 ER PT J AU Liao, J Huey, LG Scheuer, E Dibb, JE Stickel, RE Tanner, DJ Neuman, JA Nowak, JB Choi, S Wang, Y Salawitch, RJ Canty, T Chance, K Kurosu, T Suleiman, R Weinheimer, AJ Shetter, RE Fried, A Brune, W Anderson, B Zhang, X Chen, G Crawford, J Hecobian, A Ingall, ED AF Liao, J. Huey, L. G. Scheuer, E. Dibb, J. E. Stickel, R. E. Tanner, D. J. Neuman, J. A. Nowak, J. B. Choi, S. Wang, Y. Salawitch, R. J. Canty, T. Chance, K. Kurosu, T. Suleiman, R. Weinheimer, A. J. Shetter, R. E. Fried, A. Brune, W. Anderson, B. Zhang, X. Chen, G. Crawford, J. Hecobian, A. Ingall, E. D. TI Characterization of soluble bromide measurements and a case study of BrO observations during ARCTAS SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID IONIZATION MASS-SPECTROMETRY; SURFACE OZONE DEPLETION; SUNRISE EXPERIMENT 1992; POLAR SUNRISE; BOUNDARY-LAYER; AIR; TROPOSPHERE; AEROSOL; SUMMIT; MODEL AB A focus of the Arctic Research of the Composition of the Troposphere from Aircraft and Satellites (ARCTAS) mission was examination of bromine photochemistry in the spring time high latitude troposphere based on aircraft and satellite measurements of bromine oxide (BrO) and related species. The NASA DC-8 aircraft utilized a chemical ionization mass spectrometer (CIMS) to measure BrO and a mist chamber (MC) to measure soluble bromide. We have determined that the MC detection efficiency to molecular bromine (Br-2), hypobromous acid (HOBr), bromine oxide (BrO), and hydrogen bromide (HBr) as soluble bromide (Br-) was 0.9 +/- 0.1, 1.06 + 0.30/-0.35, 0.4 +/- 0.1, and 0.95 +/- 0.1, respectively. These efficiency factors were used to estimate soluble bromide levels along the DC-8 flight track of 17 April 2008 from photochemical calculations constrained to in situ BrO measured by CIMS. During this flight, the highest levels of soluble bromide and BrO were observed and atmospheric conditions were ideal for the spaceborne observation of BrO. The good agreement (R-2 = 0.76; slope = 0.95; intercept = -3.4 pmol mol(-1)) between modeled and observed soluble bromide, when BrO was above detection limit (>2 pmol mol(-1)) under unpolluted conditions (NO <10 pmol mol(-1)), indicates that the CIMS BrO measurements were consistent with the MC soluble bromide and that a well characterized MC can be used to derive mixing ratios of some reactive bromine compounds. Tropospheric BrO vertical column densities (BrOVCD) derived from CIMS BrO observations compare well with BrOTROPVCD from OMI on 17 April 2008. C1 [Liao, J.; Huey, L. G.; Dibb, J. E.; Stickel, R. E.; Tanner, D. J.; Choi, S.; Wang, Y.; Zhang, X.; Hecobian, A.; Ingall, E. D.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Scheuer, E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Neuman, J. A.; Nowak, J. B.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Neuman, J. A.; Nowak, J. B.] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Salawitch, R. J.; Canty, T.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Salawitch, R. J.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. [Salawitch, R. J.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Chance, K.; Kurosu, T.; Suleiman, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Weinheimer, A. J.; Shetter, R. E.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. [Fried, A.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Brune, W.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Anderson, B.; Chen, G.; Crawford, J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Huey, LG (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. EM greg.huey@eas.gatech.edu RI Wang, Yuhang/B-5578-2014; Neuman, Andy/A-1393-2009; Ingall, Ellery/A-5447-2008; Manager, CSD Publications/B-2789-2015; Nowak, John/B-1085-2008; Zhang, Xiaolu/F-9190-2011; Canty, Timothy/F-2631-2010; Salawitch, Ross/B-4605-2009; Hecobian, Arsineh/A-9743-2012; Liao, Jin/H-4865-2013; Crawford, James/L-6632-2013 OI Chance, Kelly/0000-0002-7339-7577; Neuman, Andy/0000-0002-3986-1727; Ingall, Ellery/0000-0003-1954-0317; Nowak, John/0000-0002-5697-9807; Canty, Timothy/0000-0003-0618-056X; Salawitch, Ross/0000-0001-8597-5832; Hecobian, Arsineh/0000-0001-9511-4868; Crawford, James/0000-0002-6982-0934 FU NASA [NNX08AR67G]; NASA Aura Science; ACMAP; ARCTAS FX This work was funded by the NASA Tropospheric Program - Contract NNX08AR67G, NASA Aura Science, ACMAP, and ARCTAS. NR 46 TC 16 Z9 16 U1 4 U2 25 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 3 BP 1327 EP 1338 DI 10.5194/acp-12-1327-2012 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 897ND UT WOS:000300656500007 ER PT J AU Gautam, R Hsu, NC Tsay, SC Lau, KM Holben, B Bell, S Smirnov, A Li, C Hansell, R Ji, Q Payra, S Aryal, D Kayastha, R Kim, KM AF Gautam, R. Hsu, N. C. Tsay, S. C. Lau, K. M. Holben, B. Bell, S. Smirnov, A. Li, C. Hansell, R. Ji, Q. Payra, S. Aryal, D. Kayastha, R. Kim, K. M. TI Accumulation of aerosols over the Indo-Gangetic plains and southern slopes of the Himalayas: distribution, properties and radiative effects during the 2009 pre-monsoon season (vol 11, pg 12841, 2011) SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Correction C1 [Gautam, R.] Univ Space Res Assoc, GESTAR, Columbia, MD 21044 USA. [Gautam, R.; Hsu, N. C.; Tsay, S. C.; Lau, K. M.; Holben, B.; Bell, S.; Smirnov, A.; Li, C.; Hansell, R.; Ji, Q.; Kim, K. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bell, S.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Smirnov, A.] Sigma Space Corp, Lanham, MD 20706 USA. [Li, C.; Hansell, R.; Ji, Q.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Payra, S.] Birla Inst Technol Mesra, Extens Ctr Jaipur, Jaipur, Rajasthan, India. [Aryal, D.] Tribhuwan Univ, Kathmandu, Nepal. [Kayastha, R.] Kathmandu Univ, Dhulikhel, Nepal. [Kim, K. M.] Morgan State Univ, GESTAR, Baltimore, MD 21251 USA. RP Gautam, R (reprint author), Univ Space Res Assoc, GESTAR, Columbia, MD 21044 USA. EM ritesh.gautam@nasa.gov RI Lau, William /E-1510-2012; Gautam, Ritesh/E-9776-2010; Tsay, Si-Chee/J-1147-2014; Hansell, Richard/J-2065-2014 OI Lau, William /0000-0002-3587-3691; Gautam, Ritesh/0000-0002-2177-9346; NR 1 TC 0 Z9 0 U1 0 U2 4 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 3 BP 1525 EP 1525 DI 10.5194/acp-12-1525-2012 PG 1 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 897ND UT WOS:000300656500019 ER PT J AU Casey, SPF Fetzer, EJ Kahn, BH AF Casey, S. P. F. Fetzer, E. J. Kahn, B. H. TI Revised identification of tropical oceanic cumulus congestus as viewed by CloudSat SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID TRIMODAL CHARACTERISTICS; CONVECTION; WAVES; RADAR; MJO AB Congestus cloud convective features are examined in one year of tropical oceanic cloud observations from the CloudSat/CALIPSO instruments. Two types of convective clouds (cumulus and deep convective, based on classification profiles from radar), and associated differences in radar reflectivity and radar/lidar cloud-top height are considered. Congestus convective features are defined as contiguous convective clouds with heights between 3 and 9 km. Three criteria were used in previous studies to identify congestus: (1) CloudSat and CALIPSO cloud-top heights less than 1 km apart; (2) CloudSat 0 dBZ echo-top height less than 1 km from CloudSat cloud-top height, and (3) CloudSat 10 dBZ echo-top height less than 2 km from CloudSat cloud-top height. A majority of congestus convective features satisfy the second and third requirements. However, over 40% of convective features identified had no associated CALIPSO cloud-top height, predominantly due to the extinguishment of the lidar beam above the CloudSat-reported convective cloud. For the remaining cells, approximately 56% of these satisfy all three requirements; when considering the lidar beam-extinction issue, only 31% of congestus convective features are identified using these criteria. This implies that while previous methods used to identify congestus clouds may be accurate in finding vigorous convection (such as transient congestus rising toward the tropopause), these criteria may miss almost 70% of the total observed congestus convective features, suggesting a more general approach should be used to describe congestus and its surrounding environment. C1 [Casey, S. P. F.; Fetzer, E. J.; Kahn, B. H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Casey, SPF (reprint author), Joint Ctr Satellite Data Assimilat, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM sean.casey@noaa.gov FU National Aeronautics and Space Administration; Government sponsorship FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. It was supported by the NASA Making Earth Science Data Records for Use in Research Environments (MEaSUREs) project. (C) 2011 California Institute of Technology. Government sponsorship acknowledged. NR 18 TC 11 Z9 11 U1 0 U2 9 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 3 BP 1587 EP 1595 DI 10.5194/acp-12-1587-2012 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 897ND UT WOS:000300656500023 ER PT J AU Casey, KA Kaab, A Benn, DI AF Casey, K. A. Kaab, A. Benn, D. I. TI Geochemical characterization of supraglacial debris via in situ and optical remote sensing methods: a case study in Khumbu Himalaya, Nepal SO CRYOSPHERE LA English DT Article ID SPACEBORNE THERMAL EMISSION; REFLECTION RADIOMETER ASTER; SATELLITE RADAR INTERFEROMETRY; AIRBORNE IMAGING SPECTROMETER; MOUNT EVEREST; FEATURE TRACKING; LANDSAT DATA; SNOW ALGAE; GLACIER; ICE AB Surface glacier debris samples and field spectra were collected from the ablation zones of Nepal Himalaya Ngozumpa and Khumbu glaciers in November and December 2009. Geochemical and mineral compositions of supraglacial debris were determined by X-ray diffraction and X-ray fluorescence spectroscopy. This composition data was used as ground truth in evaluating field spectra and satellite supraglacial debris composition and mapping methods. Satellite remote sensing methods for characterizing glacial surface debris include visible to thermal infrared hyper- and multispectral reflectance and emission signature identification, semi-quantitative mineral abundance indicies and spectral image composites. Satellite derived supraglacial debris mineral maps displayed the predominance of layered silicates, hydroxyl-bearing and calcite minerals on Khumbu Himalayan glaciers. Supraglacial mineral maps compared with satellite thermal data revealed correlations between glacier surface composition and glacier surface temperature. Glacier velocity displacement fields and shortwave, thermal infrared false color composites indicated the magnitude of mass flux at glacier confluences. The supraglacial debris mapping methods presented in this study can be used on a broader scale to improve, supplement and potentially reduce errors associated with glacier debris radiative property, composition, areal extent and mass flux quantifications. C1 [Casey, K. A.; Kaab, A.] Univ Oslo, Dept Geosci, N-0316 Oslo, Norway. [Benn, D. I.] Univ St Andrews, Dept Geog, St Andrews, Fife, Scotland. [Benn, D. I.] Univ Ctr Svalbard UNIS, N-9171 Longyearbyen, Norway. RP Casey, KA (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. EM kimberly.a.casey@nasa.gov RI Casey, Kimberly/A-4478-2013 OI Casey, Kimberly/0000-0002-6115-7525 FU Department of Geosciences at the University of Oslo, Norway; European Space Agency [21088/07/I-EC] FX This work was funded by the Department of Geosciences at the University of Oslo, Norway and European Space Agency's GlobGlacier project (21088/07/I-EC). We thank A. MacArthur and C. MacLellan of the Natural Environment Research Council Field Spectroscopy Facility for assistance with the field spectrometer loan (585.1210 to DIB). We also thank University of Oslo Department of Geosciences personnel R. Xie, B. L. Berg as well as M. Debella-Gilo for assistance with XRD/XRF and velocity analysis, respectively. We are very grateful to T. Bolch and A. Racoviteanu and for detailed manuscript reviews. Special acknowledgement is due to N. S. Rai for field assistance and R. Thapa, S. Bajracharya at the International Centre for Integrated Mountain Development ICIMOD for logistic support in Kathmandu, Nepal. NR 90 TC 18 Z9 18 U1 2 U2 21 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1994-0416 J9 CRYOSPHERE JI Cryosphere PY 2012 VL 6 IS 1 BP 85 EP 100 DI 10.5194/tc-6-85-2012 PG 16 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 891OO UT WOS:000300226700006 ER PT J AU Zhou, YY Weng, QH Gurney, KR Shuai, YM Hu, XF AF Zhou, Yuyu Weng, Qihao Gurney, Kevin R. Shuai, Yanmin Hu, Xuefei TI Estimation of the relationship between remotely sensed anthropogenic heat discharge and building energy use SO ISPRS JOURNAL OF PHOTOGRAMMETRY AND REMOTE SENSING LA English DT Article DE Anthropogenic heat discharge; Building energy use; Multi-scale; Urban heat island; Urban remote sensing ID LANDSAT SURFACE REFLECTANCE; BALANCE ALGORITHM; URBAN CLIMATES; TEB SCHEME; ASTER; ALBEDO; EMISSIVITY; SIMULATION; SEPARATION; EMISSIONS AB This paper examined the relationship between remotely sensed anthropogenic heat discharge and energy use from residential and commercial buildings across multiple scales in the city of Indianapolis, Indiana, USA. The anthropogenic heat discharge was estimated with a remote sensing-based surface energy balance model, which was parameterized using land cover, land surface temperature, albedo, and meteorological data. The building energy use was estimated using a GIS-based building energy simulation model in conjunction with Department of Energy/Energy Information Administration survey data, the Assessor's parcel data, GIS floor areas data, and remote sensing-derived building height data. The spatial patterns of anthropogenic heat discharge and energy use from residential and commercial buildings were analyzed and compared. Quantitative relationships were evaluated across multiple scales from pixel aggregation to census block. The results indicate that anthropogenic heat discharge is consistent with building energy use in terms of the spatial pattern, and that building energy use accounts for a significant fraction of anthropogenic heat discharge. The research also implies that the relationship between anthropogenic heat discharge and building energy use is scale-dependent. The simultaneous estimation of anthropogenic heat discharge and building energy use via two independent methods improves the understanding of the surface energy balance in an urban landscape. The anthropogenic heat discharge derived from remote sensing and meteorological data may be able to serve as a spatial distribution proxy for spatially-resolved building energy use, and even for fossil-fuel CO2 emissions if additional factors are considered. (C) 2011 International Society for Photogrammetry and Remote Sensing, Inc. (ISPRS) Published by Elsevier B.V. All rights reserved. C1 [Zhou, Yuyu] Pacific NW Natl Lab, Joint Global Change Res Inst, College Pk, MD 20740 USA. [Weng, Qihao] Indiana State Univ, Dept Earth & Environm Syst, Ctr Urban & Environm Change, Terre Haute, IN 47809 USA. [Gurney, Kevin R.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. [Shuai, Yanmin] Earth Resources Technol Inc, Laurel, MD 20707 USA. [Shuai, Yanmin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hu, Xuefei] Emory Univ, Rollins Sch Publ Hlth, Atlanta, GA 30322 USA. RP Zhou, YY (reprint author), Pacific NW Natl Lab, Joint Global Change Res Inst, 5825 Univ Res Court,Suite 3500, College Pk, MD 20740 USA. EM zhouyuyu@gmail.com RI Shuai, Yanmin/G-1329-2012; OI Weng, Qihao/0000-0002-2498-0934 NR 39 TC 17 Z9 20 U1 3 U2 28 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0924-2716 EI 1872-8235 J9 ISPRS J PHOTOGRAMM JI ISPRS-J. Photogramm. Remote Sens. PD JAN PY 2012 VL 67 BP 65 EP 72 DI 10.1016/j.isprsjprs.2011.10.007 PG 8 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 898NU UT WOS:000300749900007 ER PT J AU Hanson, JM Beard, BB AF Hanson, John M. Beard, Bernard B. TI Applying Monte Carlo Simulation to Launch Vehicle Design and Requirements Verification SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA Guidance, Navigation, and Control Conference CY AUG 02-05, 2010 CL Toronto, CANADA SP Amer Inst Aeronaut & Astronaut (AIAA) AB This paper is focused on applying a Monte Carlo simulation to probabilistic launch vehicle design and requirements verification. The approaches developed in this paper can be applied to other complex design efforts as well. Typically, the verification must show that requirement "x" is met for at least "y%" of cases, with, say, 10% consumer risk or 90% confidence. Two aspects of making these runs will be explored in this paper. First, there are several types of uncertainties that should be handled in different ways, depending on when they become known (or not). The paper describes how to handle different types of uncertainties and how to develop vehicle models that can be used to examine their characteristics. This includes items that are not known exactly during the design phase, but will be known for each assembled vehicle; other items that become known before or on flight day; and items that remain unknown on flight day. Second, this paper explains a method (order statistics) for determining whether certain probabilistic requirements are met and enables the user to determine how many Monte Carlo samples are required. The methods also apply to determining the design values of parameters of interest in driving the vehicle design. C1 [Hanson, John M.] NASA, George C Marshall Space Flight Ctr, Flight Mech & Anal Div, Huntsville, AL 35812 USA. [Beard, Bernard B.] ARES Corp, Tennessee Valley Off, Huntsville, AL 35805 USA. RP Hanson, JM (reprint author), NASA, George C Marshall Space Flight Ctr, Flight Mech & Anal Div, MSFC EV40, Huntsville, AL 35812 USA. EM john.m.hanson@nasa.gov; bbeard@arescorporation.com NR 9 TC 6 Z9 9 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD JAN-FEB PY 2012 VL 49 IS 1 BP 136 EP 144 DI 10.2514/1.52910 PG 9 WC Engineering, Aerospace SC Engineering GA 891HA UT WOS:000300206600014 ER PT J AU Whitley, RJ Ocampo, CA Williams, J AF Whitley, Ryan J. Ocampo, Cesar A. Williams, Jacob TI Performance of an Autonomous Multi-Maneuver Algorithm for Lunar Trans-Earth Injection SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA Guidance, Navigation, and Control Conference CY AUG 02-05, 2010 CL Toronto, CANADA SP Amer Inst Aeronaut & Astronaut (AIAA) ID TRAJECTORY MODEL; MOON AB Using a fully analytic initial estimate, a self-starting algorithm that constructs a flyable multiburn maneuver sequence to transfer a spacecraft from a closed low-lunar parking orbit to a desired Earth-entry state is developed and implemented. The algorithm is built to support the need for a human spacecraft to abort anytime during the mission and return automatically from a variety of lunar mission scenarios. This study presents a large set of representative test cases for algorithm evaluation, including highly constrained Earth-entry interface states that return the spacecraft to a specific landing site. For all cases, an optimal finite-burn solution is obtained successfully in computation time suitable for real-time on-board operation. C1 [Whitley, Ryan J.] NASA, Johnson Space Ctr, Houston, TX 77068 USA. [Ocampo, Cesar A.] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA. [Williams, Jacob] ERC Inc, ESCG, Houston, TX 77058 USA. RP Whitley, RJ (reprint author), NASA, JSC, 2101 NASA Pkwy, Houston, TX 77058 USA. EM ryan.j.whitley@nasa.gov NR 18 TC 3 Z9 3 U1 0 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD JAN-FEB PY 2012 VL 49 IS 1 BP 165 EP 174 DI 10.2514/1.52710 PG 10 WC Engineering, Aerospace SC Engineering GA 891HA UT WOS:000300206600017 ER PT S AU Birnbaum, KM Erkmen, BI AF Birnbaum, Kevin M. Erkmen, Baris I. BE Li, G Jager, DS TI Efficient multiplexing and demultiplexing of orbital angular momentum beams SO NEXT-GENERATION OPTICAL COMMUNICATION: COMPONENTS, SUB-SYSTEMS, AND SYSTEMS SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Next-Generation Optical Communication - Components, Sub-Systems, and Systems CY JAN 24-26, 2012 CL San Francisco, CA SP SPIE DE spatial division multiplexing; orbital angular momentum ID PHOTONS; LIGHT AB In the near-field regime, the number of spatial modes that a free-space communication system can efficiently use is given by the product of the Fresnel numbers of the transmit and receive apertures. It can be advantageous to decompose the field into modes that have rotational symmetry or definite orbital angular momentum (OAM modes). A key challenge to using OAM modes as parallel channels in a practical communication system is efficient multiplexing of single-spatial-mode transmitters to the orthogonal OAM modes, and demultiplexing the combined beam into single-spatial-mode receiver arrays. Previous approaches have utilized modes of different OAM, but ignored the radial coordinate, leading to inefficient use of the Fresnel number. We identify a method, using lenses and holographic phase plates, to efficiently and reversibly convert concentric Laguerre-Gauss OAM beams into an array of separated Gaussian beams. C1 [Birnbaum, Kevin M.; Erkmen, Baris I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Birnbaum, KM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 19 TC 0 Z9 0 U1 0 U2 5 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-927-2 J9 PROC SPIE PY 2012 VL 8284 AR 828407 DI 10.1117/12.909567 PG 7 WC Engineering, Electrical & Electronic; Optics; Telecommunications SC Engineering; Optics; Telecommunications GA BYT69 UT WOS:000300186800005 ER PT J AU Clampin, M Flanagan, KA AF Clampin, Mark Flanagan, Kathryn A. TI Space Telescopes SO OPTICAL ENGINEERING LA English DT Editorial Material C1 [Clampin, Mark] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Flanagan, Kathryn A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Clampin, M (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 667,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM mark.clampin@nasa.gov; flanagan@stsci.edu RI Clampin, mark/D-2738-2012 NR 1 TC 0 Z9 1 U1 0 U2 0 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 J9 OPT ENG JI Opt. Eng. PD JAN PY 2012 VL 51 IS 1 AR 011001 DI 10.1117/1.OE.51.1.011001 PG 2 WC Optics SC Optics GA 896ZV UT WOS:000300611300003 ER PT J AU Feinberg, L Cohen, L Dean, B Hayden, W Howard, J Keski-Kuha, R AF Feinberg, Lee Cohen, Lester Dean, Bruce Hayden, William Howard, Joseph Keski-Kuha, Ritva TI Space telescope design considerations SO OPTICAL ENGINEERING LA English DT Article DE space telescope; James Webb Space Telescope; optical telescope element; Hubble Space Telescope ID OPTIMUM SIZE AB The design considerations for astronomical space telescopes cover many disciplines but can be simplified into two overarching constraints: the desire to maximize science while adhering to budgetary constraints. More than ever, understanding the cost implications up front will be critical to success. Science performance can be translated into a set of simple performance metrics that set the requirements for design options. Cost is typically estimated by considering mass, complexity, technology maturity, and heritage. With this in mind, we survey the many diverse design considerations for a space telescope and, where appropriate, relate them to these basic performance metrics. In so doing, we hope to provide a roadmap for future space telescope designers on how best to optimize the design to maximize science and minimize total cost. (C) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.OE.51.1.011006] C1 [Feinberg, Lee; Dean, Bruce; Hayden, William; Howard, Joseph; Keski-Kuha, Ritva] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cohen, Lester] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Feinberg, L (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM Lee.D.Feinberg@nasa.gov NR 19 TC 9 Z9 12 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 0091-3286 EI 1560-2303 J9 OPT ENG JI Opt. Eng. PD JAN PY 2012 VL 51 IS 1 AR 011006 DI 10.1117/1.OE.51.1.011006 PG 9 WC Optics SC Optics GA 896ZV UT WOS:000300611300008 ER PT J AU Lightsey, PA Atkinson, C Clampin, M Feinberg, LD AF Lightsey, Paul A. Atkinson, Charles Clampin, Mark Feinberg, Lee D. TI James Webb Space Telescope: large deployable cryogenic telescope in space SO OPTICAL ENGINEERING LA English DT Article DE James Webb Space Telescope; light-weight mirrors; wavefront sensing and control; contamination; micrometeoroids; stray light ID MIRROR DEMONSTRATOR SBMD; BERYLLIUM AB The James Webb Space Telescope (JWST) is an infrared space telescope designed to explore four major science themes: first light and reionization, the assembly of galaxies, the birth of stars and protoplanetary systems, and planetary systems and origins of life. JWST is a segmented architecture telescope with an aperture of 6.6 m. It will operate at cryogenic temperature (40 K), achieved via passive cooling, in an orbit about the Earth-Sun second Lagrange point (L2). Passive cooling is facilitated by means of a large sunshield that provides thermal isolation and protection from direct illumination from the Sun. The large size of the telescope and spacecraft systems require that they are stowed for launch in a configuration that fits the Ariane 5 fairing, and then deployed after launch. Routine wavefront sensing and control measurements are used to achieve phasing of the segmented primary mirror and initial alignment of the telescope. A suite of instruments will provide the capability to observe over a spectral range from 0.6- to 27-mu m wavelengths with imaging and spectroscopic configurations. An overview is presented of the architecture and selected optical design features of JWST are described. (C) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.OE.51.1.011003] C1 [Lightsey, Paul A.] Ball Aerosp & Technol Corp, Boulder, CO 80306 USA. [Atkinson, Charles] Northrop Grumman Aerosp Syst, Redondo Beach, CA 90278 USA. [Clampin, Mark; Feinberg, Lee D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lightsey, PA (reprint author), Ball Aerosp & Technol Corp, POB 1062, Boulder, CO 80306 USA. EM plightse@ball.com RI Clampin, mark/D-2738-2012 FU Ball Aerospace & Technologies Corp. (BATC) [NAS5-02200]; NGAS under the JWST; NASA Goddard Space Flight Center FX Work was supported in part by the Ball Aerospace & Technologies Corp. (BATC) subcontract with NGAS under the JWST contract NAS5-02200 with the NASA Goddard Space Flight Center. The JWST system is a collaborative effort involving the National Aeronautics and Space Administration, European Space Agency, Canadian Space Agency, the astronomy community, and numerous principal investigators. We acknowledge the support and contributions of the many engineers and scientists among the many organizations that make up the JWST community. We especially wish to recognize the beryllium mirror team consisting of individuals at Brush Wellman, Axsys Technologies, Tinsley, and Quantum Coating, Inc. who were instrumental in supporting the BATC development of the mirrors. We also wish to recognize the team at ATK Composite Optics who provided support to NGAS in the development of the composite design and fabrication of the telescope support structures, and the team from ITT Exelis who have led the development of the ground support equipment for the OTE integration and test, and have a leadership role in the observatory optical testing program. The success of the team has also been dependent on the support by NASA personnel and their cadre of consultants, including the OTE Product Integrity Team, a group of experts from industry and academia who have reviewed and advised as we moved forward. NR 28 TC 28 Z9 29 U1 3 U2 17 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 JAN PY 2012 VL 51 IS 1 AR 011003 DI 10.1117/1.OE.51.1.011003 PG 19 WC Optics SC Optics GA 896ZV UT WOS:000300611300005 ER PT J AU Lyon, RG Clampin, M AF Lyon, Richard G. Clampin, Mark TI Space telescope sensitivity and controls for exoplanet imaging SO OPTICAL ENGINEERING LA English DT Article DE telescope; coronagraphy; exoplanets; wavefront sensing; wavefront control ID OBSCURATIONAL COMPLETENESS; SPECKLE NOISE; DYNAMIC-RANGE; PLANET; CORONAGRAPH; LIGHT; STAR; MASK AB We address design considerations and outline requirements for space telescopes with capabilities for high contrast imaging of exoplanets. The approach taken is to identify the span of potentially detectable Earth-sized terrestrial planets in the habitable zone of the nearest stars within 30 parsecs and estimate their inner working angles, flux ratios, SNR, sensitivities, wavefront error requirements, and sensing and control times parametrically versus aperture size. We consider 1, 2, 4, 8, and 16-m diameter telescope apertures. The achievable science, range of telescope architectures, and the coronagraphic approach are all active areas of research and are all subject to change in a rapidly evolving field. Thus presented is a snapshot of our current understanding with the goal of limiting the choices to those that appear currently technically feasible. We describe the top-level metrics of inner working angle, contrast and photometric throughput and explore how they are related to the range of target stars. A critical point is that for each telescope architecture and coronagraphic choice, the telescope stability requirements have differing impacts on the design for open-versus closed-loop sensing and control. (C) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.OE.51.1.011002] C1 [Lyon, Richard G.; Clampin, Mark] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lyon, RG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Richard.G.Lyon@nasa.gov RI Clampin, mark/D-2738-2012 NR 36 TC 6 Z9 6 U1 0 U2 2 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 J9 OPT ENG JI Opt. Eng. PD JAN PY 2012 VL 51 IS 1 AR 011002 DI 10.1117/1.OE.51.1.011002 PG 15 WC Optics SC Optics GA 896ZV UT WOS:000300611300004 ER PT J AU McEnery, JE Michelson, PF Paciesas, WS Ritz, S AF McEnery, Julie E. Michelson, Peter F. Paciesas, William S. Ritz, Steven TI Fermi Gamma-Ray Space Telescope SO OPTICAL ENGINEERING LA English DT Article DE astronomy; gamma rays; silicon ID LARGE-AREA TELESCOPE; BLIND FREQUENCY SEARCHES; PULSARS; LAT; DETECTOR; CATALOG AB The Fermi Gamma-ray Space Telescope, launched in June 2008, is an observatory designed to survey the high-energy gamma-ray sky. The primary instrument, the Large Area Telescope (LAT), provides observations from 20 MeV to greater than 300 GeV. A second instrument, the Gamma-ray Burst Monitor (GBM), provides observations of transients from less than 10 keV to 40 MeV. We describe the design and performance of the instruments and their subsystems, the spacecraft and the ground system. (C) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.OE.51.1.011012] C1 [McEnery, Julie E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Michelson, Peter F.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Paciesas, William S.] Univ Alabama, Huntsville Ctr Space Plasma & Aeron Res CSPAR, Huntsville, AL 35899 USA. [Ritz, Steven] Univ Calif Santa Cruz, Inst Particle Phys, Santa Cruz, CA 95064 USA. RP McEnery, JE (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM julie.mcenery@nasa.gov FU National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique / Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High-Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; NASA in the U.S; BMWi/DLR in Germany FX We thank our colleagues-scientists, engineers, technicians, and staff-around the world who worked together on the design, construction and operation of the Fermi Observatory. The mission would not have happened without them. We also thank Bill Atwood, Dave Thompson, Judy Racusin, and Jack Leibee for their inputs to this paper. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High-Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. The Fermi GBM collaboration acknowledges support for GBM development, operations and data analysis from NASA in the U.S. and .BMWi/DLR in Germany NR 22 TC 5 Z9 5 U1 0 U2 0 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 JAN PY 2012 VL 51 IS 1 AR 011012 DI 10.1117/1.OE.51.1.011012 PG 9 WC Optics SC Optics GA 896ZV UT WOS:000300611300014 ER PT J AU Miller, DA Wilson, DW Dereniak, EL AF Miller, Darren A. Wilson, Daniel W. Dereniak, Eustace L. TI Novel design and alignment of wire-grid diffraction gratings on a visible focal plane array SO OPTICAL ENGINEERING LA English DT Article DE micro-optics; polarimetry; polarization; alignment; Stokes; diffraction; pattern recognition; FPA AB A pixelated, wire-grid diffraction grating is designed, fabricated, aligned, and mounted on an active focal plane array of a camera operating in the visible. The resulting design of the pixelated wire-grid polarizer array eschewed the need for fine translational alignments and drastically reduced cross-talk between pixels detecting differing polarization states. Using common optomechanical elements in conjunction with a novel correlation-based alignment metric, we are able to achieve repeatable angular alignments to better than 0.004 deg between the focal plane array and the pixelated wire-grid polarizer array, both featuring 6.45 mu m pixels. An on-chip, four-state, linear snapshot polarimeter is yielded in the detailed processes and raw image data from the instrument are presented. (C) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.OE.51.1.014001] C1 [Miller, Darren A.; Dereniak, Eustace L.] Univ Arizona, Coll Opt Sci, Tucson, AZ 85721 USA. [Wilson, Daniel W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Miller, DA (reprint author), Univ Arizona, Coll Opt Sci, POB 210094,1630 E Univ Blvd, Tucson, AZ 85721 USA. EM dmiller@optics.arizona.edu FU University of Arizona FX The authors would like to thank NASA's Jet Propulsion Laboratory for the use of their facilities at the Micro-Devices Laboratory and for their financial support through the Strategic University Research Partnership with the University of Arizona. NR 8 TC 3 Z9 3 U1 2 U2 12 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 J9 OPT ENG JI Opt. Eng. PD JAN PY 2012 VL 51 IS 1 AR 014001 DI 10.1117/1.OE.51.1.014001 PG 7 WC Optics SC Optics GA 896ZV UT WOS:000300611300033 ER PT J AU Postman, M Brown, T Sembach, K Giavalisco, M Traub, W Stapelfeldt, K Calzetti, D Oegerle, W Rich, RM Stahl, HP Tumlinson, J Mountain, M Soummer, R Hyde, T AF Postman, Marc Brown, Tom Sembach, Kenneth Giavalisco, Mauro Traub, Wesley Stapelfeldt, Karl Calzetti, Daniela Oegerle, William Rich, R. Michael Stahl, H. Phillip Tumlinson, Jason Mountain, Matt Soummer, Remi Hyde, Tupper TI Advanced Technology Large-Aperture Space Telescope: science drivers and technology developments SO OPTICAL ENGINEERING LA English DT Article DE Advanced Technology Large-Aperture Space Telescope; ultraviolet/optical space telescopes; astrophysics; astrobiology; technology development ID LAYER ADAPTIVE OPTICS; INTERGALACTIC MEDIUM; MILKY-WAY; GALAXIES; PERFORMANCE; IMPROVEMENT; SATELLITES; PLANETS; MIRRORS; GAS AB The Advanced Technology Large-Aperture Space Telescope (ATLAST) is a concept for an 8- to 16-m ultraviolet optical near infrared space observatory for launch in the 2025 to 2030 era. ATLAST will allow astronomers to answer fundamental questions at the forefront of modern astrophysics, including: Is there life elsewhere in the Galaxy? We present a range of science drivers and the resulting performance requirements for ATLAST (8- to 16-marcsec angular resolution, diffraction limited imaging at 0.5-mu m wavelength, minimum collecting area of 45 m(2), high sensitivity to light wavelengths from 0.1 to 2.4 mu m, high stability in wavefront sensing and control). We also discuss the priorities for technology development needed to enable the construction of ATLAST for a cost that is comparable to that of current generation observatory-class space missions. (C) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.OE.51.1.011007] C1 [Postman, Marc; Brown, Tom; Sembach, Kenneth; Tumlinson, Jason; Mountain, Matt; Soummer, Remi] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Giavalisco, Mauro; Calzetti, Daniela] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Traub, Wesley] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Stapelfeldt, Karl; Oegerle, William; Hyde, Tupper] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rich, R. Michael] Univ Calif Los Angeles, Div Astron, Los Angeles, CA 90095 USA. [Stahl, H. Phillip] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Postman, M (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM postman@stsci.edu RI Oegerle, William/C-9070-2012; Stapelfeldt, Karl/D-2721-2012; OI Postman, Marc/0000-0002-9365-7989 NR 48 TC 29 Z9 31 U1 3 U2 18 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 J9 OPT ENG JI Opt. Eng. PD JAN PY 2012 VL 51 IS 1 AR 011007 DI 10.1117/1.OE.51.1.011007 PG 11 WC Optics SC Optics GA 896ZV UT WOS:000300611300009 ER PT J AU Weisskopf, MC AF Weisskopf, Martin C. TI Chandra x-ray optics SO OPTICAL ENGINEERING LA English DT Article DE x-ray astronomy; x-ray optics AB Significant advances in science always occur when the state of the art in instrumentation improves dramatically. NASA's Chandra X-ray Observatory represents such an advance. Launched in July of 1999, Chandra is an observatory designed to study the x-ray emission from all categories of astronomical objects-from comets, planets, and normal stars to quasars, galaxies, and clusters of galaxies. At the heart of this observatory is the precision x-ray optic that has been vital for Chandra's outstanding success and that features an angular resolution improved by an order of magnitude compared to its forerunners. The Chandra mission is now entering its thirteenth year of operation, which, given that the observatory was designed for a minimum of three years of operation, testifies to its robust and carefully thought-out design. We review the design and construction of the remarkable telescope, present examples of its usage for astronomy and astrophysics, and speculate on its future. (C) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.OE.51.1.011013] C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Weisskopf, MC (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM martin.c.weisskopf@nasa.gov NR 9 TC 2 Z9 2 U1 0 U2 1 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 J9 OPT ENG JI Opt. Eng. PD JAN PY 2012 VL 51 IS 1 AR 011013 DI 10.1117/1.OE.51.1.011013 PG 7 WC Optics SC Optics GA 896ZV UT WOS:000300611300015 ER PT J AU Werner, M AF Werner, Michael TI The Spitzer Space Telescope SO OPTICAL ENGINEERING LA English DT Article DE cryogenic systems; infrared; space telescope; Spitzer; telescope focus; thermal control ID FOCUS SLEW; MISSION; SIRTF AB The Spitzer Space Telescope, which has operated very successfully since 2003 in its unique Earth-trailing solar orbit, is NASA's Great Observatory for infrared astronomy. We provide a quick overview of the optical characteristics of Spitzer and review the observatory design. The main emphasis is on two unique on-orbit activities used to optimize the scientific return from Spitzer: 1. an unusual approach to focusing the telescope that minimized the use of the cryogenic focus mechanism, and 2. a methodology for extending the cryogenic lifetime of Spitzer by actively controlling the telescope temperature. (C) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.OE.51.1.011008] C1 CALTECH, Jet Prop Lab, Pasadena, CA 91107 USA. RP Werner, M (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91107 USA. EM Michael.w.werner@jpl.nasa.gov FU NASA FX Portions of the research described here were carried out at the Jet Propulsion Laboratory, operated by the California Institute of Technology under contract to NASA (copyright 2011 California Institute of Technology). Government sponsorship is acknowledged. NR 17 TC 1 Z9 1 U1 3 U2 6 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 JAN PY 2012 VL 51 IS 1 AR 011008 DI 10.1117/1.OE.51.1.011008 PG 7 WC Optics SC Optics GA 896ZV UT WOS:000300611300010 ER PT B AU Globus, RK Caiozzo, V Acharya, M Fike, JR Limoli, C AF Globus, Ruth K. Caiozzo, Vincent Acharya, Munjal Fike, John R. Limoli, Charles BE Spitz, DR Dornfeld, KJ Krishnan, K Gius, D TI Redox Regulation of Stem Cell Compartments: The Convergence of Radiation-Induced Normal Tissue Damage and Oxidative Stress SO OXIDATIVE STRESS IN CANCER BIOLOGY AND THERAPY SE Oxidative Stress in Applied Basic Research and Clinical Practice LA English DT Article; Book Chapter ID NEURAL PRECURSOR CELLS; SKELETAL-MUSCLE FIBERS; CENTRAL-NERVOUS-SYSTEM; EXTRACELLULAR-SUPEROXIDE DISMUTASE; NORMAL HUMAN FIBROBLASTS; TRANSFORMATION IN-VITRO; FREE-RADICAL SCAVENGERS; TOTAL-BODY IRRADIATION; REACTIVE OXYGEN; IONIZING-RADIATION AB The redox environment impacts normal stem cell niches throughout the body. Hematopoietic, muscle, and neural stem cell compartments respond to changes in reactive oxygen (ROS) and nitrogen (RNS) species by triggering signaling networks that impact cellular proliferation, survival, and differentiation. Work from many labs including our own has found that irradiation can trigger acute and chronic increases in oxidative stress. Low dose and/or protracted dose rates can elicit radioadaptive changes that have beneficial effects on proliferation and survival while influencing the development lineage-specific cell fates. Higher doses and dose rates have been found to impede the regeneration of irradiated tissues, through the depletion and/or damage of endogenous stem cell pools, and by promoting the onset and persistence of secondary reactive processes involving oxidative stress and inflammatory cytokines. Increasing evidence suggests that these important stem cell pools are differentially protected from DNA damaging agents compared to their immediate progeny (i.e., precursor/progenitor cells) due to enhanced DNA repair, antioxidant status, and reduced cell cycle activity. Thus, many of the adverse effects of irradiation on normal tissue are the consequence of damage to the rapidly expanding pool of precursor cells derived from asymmetric cell division. Irradiation of the bone marrow impairs the health of bone by promoting osteoclastogenesis (osteoclast-mediated bone resorption) and inhibiting osteoblastogenesis (osteoblast-mediated bone formation), with the net effect of reducing bone mass and structural integrity. Irradiation of the skeletal musculature impairs myogenesis (formation of muscle tissue) by damaging satellite cells (i.e., muscle stem cells) and reducing proproliferative levels of nitric oxide. In the brain, irradiation depletes neural stem and precursor cells and leads to persistent increases in ROS/RNS and inflammatory cytokines that inhibit neurogenesis (formation of new neurons and glia) and adversely impact cognition. In each of these foregoing cases, interventions targeted to reduce specific reactive species can attenuate the adverse effects of radiation exposure and point to the importance of understanding the interplay between endogenous stem cell niches and the microenvironmental redox state. C1 [Acharya, Munjal; Limoli, Charles] Univ Calif Irvine, Dept Radiat Oncol, Irvine, CA 92697 USA. [Caiozzo, Vincent] Univ Calif Irvine, Dept Orthopaed Surg, Irvine, CA 92697 USA. [Globus, Ruth K.] NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA. [Fike, John R.] Univ Calif San Francisco, Dept Neurol Surg, Brain & Spinal Injury Ctr, San Francisco, CA 94110 USA. [Fike, John R.] Univ Calif San Francisco, Dept Radiat Oncol, Brain & Spinal Injury Ctr, San Francisco, CA 94110 USA. RP Limoli, C (reprint author), Univ Calif Irvine, Dept Radiat Oncol, Irvine, CA 92697 USA. NR 121 TC 3 Z9 3 U1 2 U2 10 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-1-61779-396-7 J9 OXID STRESS APPL BAS JI Oxid. Stress Appl. Basic Res. Clin. Pract. PY 2012 BP 169 EP 192 DI 10.1007/978-1-61779-397-4_9 D2 10.1007/978-1-61779-397-4 PG 24 WC Medicine, General & Internal SC General & Internal Medicine GA BYQ04 UT WOS:000299709300010 ER PT J AU Nixon, CA Lorenz, RD AF Nixon, Conor A. Lorenz, Ralph D. TI Titan through time: Formation, evolution and fate Preface SO PLANETARY AND SPACE SCIENCE LA English DT Editorial Material C1 [Nixon, Conor A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Nixon, Conor A.] NASA, Goddard Space Flight Ctr, Planetary Syst Branch, Greenbelt, MD 20771 USA. [Lorenz, Ralph D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Nixon, CA (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM conor.a.nixon@nasa.gov RI Nixon, Conor/A-8531-2009; Lorenz, Ralph/B-8759-2016 OI Nixon, Conor/0000-0001-9540-9121; Lorenz, Ralph/0000-0001-8528-4644 NR 0 TC 0 Z9 0 U1 0 U2 2 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 JAN PY 2012 VL 60 IS 1 BP 1 EP 2 DI 10.1016/j.pss.2011.12.012 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895GC UT WOS:000300483200001 ER PT J AU Buratti, BJ Sotin, C Lawrence, K Brown, RH Le Mouelic, S Soderblom, JM Barnes, J Clark, RN Baines, KH Nicholson, PD AF Buratti, B. J. Sotin, C. Lawrence, K. Brown, R. H. Le Mouelic, S. Soderblom, J. M. Barnes, J. Clark, R. N. Baines, K. H. Nicholson, P. D. TI A newly discovered impact crater in Titan's Senkyo: Cassini VIMS observations and comparison with other impact features SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Titan Through Time-A Workshop on Titans Formation, Evolution and Fate CY APR 06-08, 2010 CL MD DE Titan; Surfaces; Craters ID LANDING SITE; SURFACE; RADAR AB Senkyo is an equatorial plain on Titan filled with dunes and surrounded by hummocky plateaus. During the Titan targeted flyby T61 on August 25, 2009, the Cassini Visual and Infrared Mapping Spectrometer (VIMS) onboard the Cassini spacecraft observed a circular feature, centered at 5.4 degrees N and 341 degrees W, that superimposes the dune fields and a bright plateau. This circular feature, which has been named Paxsi by the International Astronomical Union, is 120 +/- 10 km in diameter (measured from the outer edge of the crater rim) and exhibits a central bright area that can be interpreted as the central peak or pit of an impact crater. Although there are only a handful of certain impact craters on Titan, there are two other craters that are of similar size to this newly discovered feature and that have been studied by VIMS: Sinlap (Le Mouelic et al., 2008) and Selk (Soderblom et al., 2010). Sinlap is associated with a large downwind, fan-like feature that may have been formed from an impact plume that rapidly expanded and deposited icy particles onto the surface. Although much of the surrounding region is covered with dunes, the plume region is devoid of dunes. The formation process of Selk also appears to have removed (or covered up) dunes from parts of the adjacent dune-filled terrain. The circular feature on Senkyo is quite different: there is no evidence of an ejecta blanket and the crater itself appears to be infilled with dune material. The rim of the crater appears to be eroded by fluvial processes; at one point the rim is breached. The rim is unusually narrow, which may be due to mass wasting on its inside and subsequent infill by dunes. Based on these observations, we interpret this newly discovered feature to be a more eroded crater than both Sinlap and Selk. Paxsi may have formed during a period when Titan was warmer and more ductile than it is currently. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Buratti, B. J.; Sotin, C.; Lawrence, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brown, R. H.; Soderblom, J. M.] U AZ, Dept Planet Sci, Tucson, AZ 85721 USA. [Brown, R. H.; Soderblom, J. M.] U AZ, LPL, Tucson, AZ 85721 USA. [Le Mouelic, S.] Univ Nantes, CNRS, Lab Planetol & Geodynam, UMR 6112, F-44035 Nantes, France. [Barnes, J.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA. [Clark, R. N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA. [Baines, K. H.] SSEC Univ Wisconsin, Madison, WI 53706 USA. [Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Buratti, BJ (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-401, Pasadena, CA 91109 USA. EM bonnie.j.buratti@jpl.nasa.gov RI Barnes, Jason/B-1284-2009; OI Barnes, Jason/0000-0002-7755-3530; Soderblom, Jason/0000-0003-3715-6407 NR 22 TC 9 Z9 9 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD JAN PY 2012 VL 60 IS 1 BP 18 EP 25 DI 10.1016/j.pss.2011.05.004 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895GC UT WOS:000300483200004 ER PT J AU Langhans, MH Jaumann, R Stephan, K Brown, RH Buratti, BJ Clark, RN Baines, KH Nicholson, PD Lorenz, RD Soderblom, LA Soderblom, JM Sotin, C Barnes, JW Nelson, R AF Langhans, M. H. Jaumann, R. Stephan, K. Brown, R. H. Buratti, B. J. Clark, R. N. Baines, K. H. Nicholson, P. D. Lorenz, R. D. Soderblom, L. A. Soderblom, J. M. Sotin, C. Barnes, J. W. Nelson, R. TI Titan's fluvial valleys: Morphology, distribution, and spectral properties SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Titan Through Time-A Workshop on Titans Formation, Evolution and Fate CY APR 06-08, 2010 CL MD DE Titan; Valleys; Methane; Cassini; VIMS; RADAR ID CASSINI RADAR OBSERVATIONS; HUYGENS LANDING SITE; METHANE CYCLE; SURFACE; EROSION; VIMS; CHANNELS; DUNES; EARTH; LAKES AB Titan's fluvial channels have been investigated based on data obtained by the Synthetic Aperture Radar (SAR) instrument and the Visible and Infrared Mapping Spectrometer (VIMS) onboard the Cassini spacecraft. In this paper, a database of fluvial features is created based on radar-SAR data aiming to unveil the distribution and the morphologic and spectral characteristics of valleys on Titan on a global scale. It will also study the spatial relations between fluvial valleys and Titan's geologic units and spectral surface units which have become accessible thanks to Cassini-VIMS data. Several distinct morphologic types of fluvial valleys can be discerned by SAR-images. Dendritic valley networks appear to have much in common with terrestrial dendritic systems owing to a hierarchical and tree-shaped arrangement of the tributaries which is indicative of an origin from precipitation. Dry valleys constitute another class of valleys resembling terrestrial wadis, an indication of episodic and strong flow events. Other valley types, such as putative canyons, cannot be correlated with rainfall based on their morphology alone, since it cannot be ruled out that they may have originated from volcanic/tectonic action or groundwater sapping. Highly developed and complex fluvial networks with channel lengths of up to 1200 km and widths of up to 10 km are concentrated only at a few locations whereas single valleys are scattered over all latitudes. Fluvial valleys are frequently found in mountainous areas. Some terrains, such as equatorial dune fields and undifferentiated plains at mid-latitudes, are almost entirely free of valleys. Spectrally, fluvial terrains are often characterized by a high reflectance in each of Titan's atmospheric windows, as most of them are located on Titan's bright 'continents'. Nevertheless, valleys are spatially associated with a surface unit appearing blue due to its higher reflection at 1.3 mu m in a VIMS false color RGB composite with R: 1.59/1.27 mu m, G: 2.03/1.27 mu m, and B: 1.27/1.08 mu m: the channels either dissect pure bluish surface units or they are carved into terrain with a mixed spectral signature between bright and bluish surface materials. The global picture of fluvial flows clearly indicates a high diversity of parameters controlling fluvial erosion, such as climatic processes, as well as surface and bedrock types. Recent fluvial activity is very likely in the north polar region in contrast to more arid conditions at lower latitudes and at the south pole of Titan. This divergence is probably an indication of seasonal climatic asymmetries between the hemispheres. However, traces of previous fluvial activity are scattered over all latitudes of Titan, which is indicative of previous climatic conditions with at least episodic rainfall. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Langhans, M. H.; Jaumann, R.; Stephan, K.] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany. [Jaumann, R.] Free Univ Berlin, Inst Geosci Remote Sensing Earth & Planets, Dept Earth Sci, Berlin, Germany. [Brown, R. H.; Soderblom, J. M.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Buratti, B. J.; Baines, K. H.; Sotin, C.; Nelson, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Clark, R. N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA. [Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Lorenz, R. D.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Planetary Explorat Grp, Laurel, MD 20723 USA. [Soderblom, L. A.] US Geol Survey, Flagstaff, AZ 86001 USA. [Barnes, J. W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA. RP Langhans, MH (reprint author), German Aerosp Ctr, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany. EM mirjam.langhans@dlr.de RI Barnes, Jason/B-1284-2009; Lorenz, Ralph/B-8759-2016; OI Barnes, Jason/0000-0002-7755-3530; Lorenz, Ralph/0000-0001-8528-4644; Soderblom, Jason/0000-0003-3715-6407 NR 97 TC 31 Z9 31 U1 0 U2 23 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 JAN PY 2012 VL 60 IS 1 BP 34 EP 51 DI 10.1016/j.pss.2011.01.020 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895GC UT WOS:000300483200006 ER PT J AU Vixie, G Barnes, JW Bow, J Le Mouelic, S Rodriguez, S Brown, RH Cerroni, P Tosi, F Buratti, B Sotin, C Filacchione, G Capaccioni, F Coradini, A AF Vixie, Graham Barnes, Jason W. Bow, Jacob Le Mouelic, Stephane Rodriguez, Sebastien Brown, Robert H. Cerroni, Priscilla Tosi, Federico Buratti, Bonnie Sotin, Christophe Filacchione, Gianrico Capaccioni, Fabrizio Coradini, Angioletta TI Mapping Titan's surface features within the visible spectrum via Cassini VIMS SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Titan Through Time-A Workshop on Titans Formation, Evolution and Fate CY APR 06-08, 2010 CL MD DE Titan; Surface; Optical wavelength; Visible imaging; Cassini VIMS ID LANDING SITE; SPECTROPHOTOMETRY; SPECTROSCOPY; DIVERSITY; NEPTUNE; IMAGES; SATURN; URANUS AB Titan shows its surface through many methane windows in the 1-5 mu m region. Windows at shorter wavelengths also exist, polluted by scattering off of atmospheric haze that reduces the surface contrast. At visible wavelengths, the surface of Titan has been observed by Voyager 1, the Hubble Space Telescope, and ground-based telescopes. We present here global surface mapping of Titan using the visible wavelength channels from Cassini's Visual and Infrared Mapping Spectrometer (VIMS). We show global maps in each of the VIMS-V channels extending from 0.35 to 1.05 mu m. We find methane windows at 0.637, 0.681, 0.754, 0.827, 0.937, and 1.046 mu m and apply an RGB color scheme to the 0.754, 0.827 and 0.937 pm windows to search for surface albedo variations. Our results show that Titan appears gray at visible wavelengths; hence scattering albedo is a good approximation of the Bond albedo. Maps of this genre have already been made and published using the infrared channels of VIMS. Ours are the first global maps of Titan shortward of 0.938 mu m. We compare the older IR maps to the new VIMS-V maps to constrain surface composition. For instance Tui Regio and Hotei Regio, referred to as 5-mu m bright spots in previous papers, do not distinguish themselves at all visible wavelengths. The distinction between the dune areas and the bright albedo spots, however, such as the difference between Xanadu and Senkyo, is easily discernible. We employ an empirically derived algorithm to remove haze layers from Titan, revealing a better look at the surface contrast. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Vixie, Graham; Barnes, Jason W.; Bow, Jacob] Univ Idaho, Dept Phys, Moscow, ID 83844 USA. [Le Mouelic, Stephane] Univ Nantes, CNRS, Lab Planetol & Geodynam, UMR 6112, F-44300 Nantes, France. [Rodriguez, Sebastien] Univ Paris 07, CNRS, CEA Saclay, Lab AIM,DSM,IRFU,SAp, Gif Sur Yvette, France. [Brown, Robert H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Cerroni, Priscilla; Filacchione, Gianrico; Capaccioni, Fabrizio] Ist Astrofis Spaziale & Fis Cosm, Sez Roma, IT-00133 Rome, Italy. [Tosi, Federico; Coradini, Angioletta] Ist Fis Spazio Interplanetario, IT-00133 Rome, Italy. [Buratti, Bonnie; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Vixie, G (reprint author), Univ Idaho, Dept Phys, POB 440903, Moscow, ID 83844 USA. EM gvixie@vandals.uidaho.edu RI Barnes, Jason/B-1284-2009; Rodriguez, Sebastien/H-5902-2016; OI Barnes, Jason/0000-0002-7755-3530; Rodriguez, Sebastien/0000-0003-1219-0641; Cerroni, Priscilla/0000-0003-0239-2741; Capaccioni, Fabrizio/0000-0003-1631-4314; Filacchione, Gianrico/0000-0001-9567-0055; Tosi, Federico/0000-0003-4002-2434 NR 30 TC 6 Z9 6 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 JAN PY 2012 VL 60 IS 1 BP 52 EP 61 DI 10.1016/j.pss.2011.03.021 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895GC UT WOS:000300483200007 ER PT J AU Cottini, V Nixon, CA Jennings, DE de Kok, R Teanby, NA Irwin, PGJ Flasar, FM AF Cottini, V. Nixon, C. A. Jennings, D. E. de Kok, R. Teanby, N. A. Irwin, P. G. J. Flasar, F. M. TI Spatial and temporal variations in Titan's surface temperatures from Cassini CIRS observations SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Titan Through Time-A Workshop on Titans Formation, Evolution and Fate CY APR 06-08, 2010 CL MD DE Titan; Surface; Temperature; Infrared observations ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; THERMAL EMISSION; ATMOSPHERE; PAIRS; 300-K; SYSTEM; 50-K AB We report a wide-ranging study of Titan's surface temperatures by analysis of the Moon's outgoing radiance through a spectral window in the thermal infrared at 19 mu m (530 cm(-1)) characterized by lower atmospheric opacity. We begin by modeling Cassini Composite Infrared Spectrometer (CIRS) far infrared spectra collected in the period 2004-2010, using a radiative transfer forward model combined with a non-linear optimal estimation inversion method. At low-latitudes, we agree with the HASI near-surface temperature of about 94K at 10 degrees S (Fulchignoni et al., 2005). We find a systematic decrease from the equator toward the poles, hemispherically asymmetric, of similar to 1 K at 60 degrees south and similar to 3 K at 60 degrees north, in general agreement with a previous analysis of CIRS data (Jennings et al., 2009), and with Voyager results from the previous northern winter. Subdividing the available database, corresponding to about one Titan season, into 3 consecutive periods, small seasonal changes of up to 2 K at 60 degrees N became noticeable in the results. In addition, clear evidence of diurnal variations of the surface temperatures near the equator are observed for the first time: we find a trend of slowly increasing temperature from the morning to the early afternoon and a faster decrease during the night. The diurnal change is similar to 1.5 K, in agreement with model predictions for a surface with a thermal inertia between 300 and 600J m(-2) s(-1/2) K-1. These results provide important constraints on coupled surface-atmosphere models of Titan's meteorology and atmospheric dynamic. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Cottini, V.; Nixon, C. A.; Jennings, D. E.; Flasar, F. M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Cottini, V.; Nixon, C. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [de Kok, R.] SRON, NL-3584 CA Utrecht, Netherlands. [Teanby, N. A.; Irwin, P. G. J.] Univ Oxford, Oxford OX1 3PU, England. RP Cottini, V (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Planetary Syst Lab, Code 693,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM valeria.cottini@nasa.gov RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; Jennings, Donald/D-7978-2012; OI Nixon, Conor/0000-0001-9540-9121; Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X NR 29 TC 24 Z9 24 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD JAN PY 2012 VL 60 IS 1 BP 62 EP 71 DI 10.1016/j.pss.2011.03.015 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895GC UT WOS:000300483200008 ER PT J AU Le Mouelic, S Rannou, P Rodriguez, S Sotin, C Griffith, CA Le Corre, L Barnes, JW Brown, RH Baines, KH Buratti, BJ Clark, RN Nicholson, PD Tobie, G AF Le Mouelic, Stephane Rannou, Pascal Rodriguez, Sebastien Sotin, Christophe Griffith, Caitlin A. Le Corre, Lucille Barnes, Jason W. Brown, Robert H. Baines, Kevin H. Buratti, Bonnie J. Clark, Roger N. Nicholson, Philip D. Tobie, Gabriel TI Dissipation of Titan's north polar cloud at northern spring equinox SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Titan Through Time-A Workshop on Titans Formation, Evolution and Fate CY APR 06-08, 2010 CL MD DE Titan; Cloud; Meteorology; Cassini; VIMS ID METHANE ABSORPTION; 9500 CM(-1); ATMOSPHERE; DESCENT; WINDS; LAKES; HAZE AB Saturn's Moon Titan has a thick atmosphere with a meteorological cycle. We report on the evolution of the giant cloud system covering its north pole using observations acquired by the Visual and Infrared Mapping Spectrometer onboard the Cassini spacecraft. A radiative transfer model in spherical geometry shows that the clouds are found at an altitude between 30 and 65 km. We also show that the polar cloud system vanished progressively as Titan approached equinox in August 2009, revealing at optical wavelengths the underlying sea known as Kraken Mare. This decrease of activity suggests that the north-polar downwelling has begun to shut off. Such a scenario is compared with the Titan global circulation model of Rannou et al. (2006), which predicts a decrease of cloud coverage in northern latitudes at the same period of time. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Le Mouelic, Stephane; Sotin, Christophe; Le Corre, Lucille; Tobie, Gabriel] Univ Nantes, CNRS, Lab Planetol & Geodynam, UMR6112, F-44322 Nantes 3, France. [Rannou, Pascal] Univ Reims, GSMA, F-51100 Reims, France. [Rodriguez, Sebastien] CEA, Lab AIM, Gif Sur Yvette, France. [Sotin, Christophe; Baines, Kevin H.; Buratti, Bonnie J.] JPL, Pasadena, CA USA. [Griffith, Caitlin A.; Brown, Robert H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Griffith, Caitlin A.; Brown, Robert H.] Univ Arizona, Steward Observ, Tucson, AZ USA. [Barnes, Jason W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA. [Clark, Roger N.] USGS, Denver, CO USA. [Nicholson, Philip D.] Cornell Univ, Ithaca, NY 14853 USA. RP Le Mouelic, S (reprint author), Univ Nantes, CNRS, Lab Planetol & Geodynam, UMR6112, 2 Rue Houssiniere,BP92208, F-44322 Nantes 3, France. EM stephane.lemouelic@univ-nantes.fr RI Barnes, Jason/B-1284-2009; RANNOU, Pascal/I-9059-2012; Rodriguez, Sebastien/H-5902-2016; OI Barnes, Jason/0000-0002-7755-3530; Rodriguez, Sebastien/0000-0003-1219-0641; Le Corre, Lucille/0000-0003-0349-7932 NR 37 TC 15 Z9 15 U1 0 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD JAN PY 2012 VL 60 IS 1 BP 86 EP 92 DI 10.1016/j.pss.2011.04.006 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895GC UT WOS:000300483200010 ER PT J AU di Lauro, C Lattanzi, F Brown, LR Sung, K Vander Auwera, J Mantz, AW Smith, MAH AF di Lauro, Carlo Lattanzi, Franca Brown, Linda R. Sung, Keeyoon Vander Auwera, Jean Mantz, Arlan W. Smith, Mary Ann H. TI High resolution investigation of the 7 mu m region of the ethane spectrum SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Titan Through Time-A Workshop on Titans Formation, Evolution and Fate CY APR 06-08, 2010 CL MD DE Ethane; Theoretical Hamiltonian; Infrared; Line positions; Intensities; Molecular database ID MOLECULAR SPECTROSCOPIC DATABASE; HALF-WIDTH COEFFICIENTS; INFRARED-SPECTRUM; HOT TRANSITIONS; C2H6; BAND; SPLITTINGS; NU(4)+NU(12); (C2H6)-C-12; PARAMETERS AB Building upon previous studies, we re-investigated the ethane spectrum between 1330 and 1610 cm(-1) by combining unapodized spectra obtained at room temperature with a Bruker Fourier transform spectrometer (FTS) in Brussels and at 131 K with a Bruker FTS in Pasadena. The maximum optical path differences (MOPD) of the two datasets were 450 and 323.7 cm, corresponding to spectral resolutions of 0.0020 and 0.0028 cm(-1), respectively. Of the 15,000 lines observed, over 4592 transitions were assigned to the v(6) (at 1379 cm(-1)), vs (at 1472 cm(-1)), v(4) + v(12) (at 1481 cm(-1)) and 2v(4)+v(9) (at 1388 cm(-1)) bands, and another 1044 transitions were located for the v(4)+v(8) - v(4) hot band (at 1472 cm(-1)). Our new analysis included an improved implementation of the Hamiltonian calculation needed to interpret the complex spectral structures caused by numerous interactions affecting these four modes of vibration. From these results, we created the first line-by-line database containing the molecular parameters for over 20,000 (C2H6)-C-12 transitions at 7 mu m. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Brown, Linda R.; Sung, Keeyoon] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [di Lauro, Carlo; Lattanzi, Franca] Univ Naples Federico 2, I-80131 Naples, Italy. [Vander Auwera, Jean] Univ Libre Bruxelles, Serv Chim Quant & Photophys, B-1050 Brussels, Belgium. [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 26 TC 11 Z9 11 U1 0 U2 8 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 JAN PY 2012 VL 60 IS 1 BP 93 EP 101 DI 10.1016/j.pss.2011.01.008 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895GC UT WOS:000300483200011 ER PT J AU Bramall, NE Quinn, R Mattioda, A Bryson, K Chittenden, JD Cook, A Taylor, C Minelli, G Ehrenfreund, P Ricco, AJ Squires, D Santos, O Friedericks, C Landis, D Jones, NC Salama, F Allamandola, LJ Hoffmann, SV AF Bramall, Nathan E. Quinn, Richard Mattioda, Andrew Bryson, Kathryn Chittenden, Julie D. Cook, Amanda Taylor, Cindy Minelli, Giovanni Ehrenfreund, Pascale Ricco, Antonio J. Squires, David Santos, Orlando Friedericks, Charles Landis, David Jones, Nykola C. Salama, Farid Allamandola, Louis J. Hoffmann, Soren V. TI The development of the Space Environment Viability of Organics (SEVO) experiment aboard the Organism/Organic Exposure to Orbital Stresses (O/OREOS) satellite SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Organic; Biomarker; O/OREOS; SEVO; Astrobiology; CubeSat ID POLYCYCLIC AROMATIC-HYDROCARBONS; INTERSTELLAR ICE ANALOGS; INFRARED-SPECTROSCOPY; MOLECULES; ULTRAVIOLET; METEORITES; LIFE; UV; PHOTOCHEMISTRY; IRRADIATION AB The Space Environment Viability of Organics (SEVO) experiment is one of two scientific payloads aboard the triple-cube satellite Organism/ORganic Exposure to Orbital Stresses (O/OREOS). O/OREOS is the first technology demonstration mission of the NASA Astrobiology Small Payloads Program. The 1-kg, 1000-cm(3) SEVO cube is investigating the chemical evolution of organic materials in interstellar space and planetary environments by exposing organic molecules under controlled conditions directly to the low-Earth orbit (LEO) particle and electromagnetic radiation environment. O/OREOS was launched on November 19, 2010 into a 650-km, 72 degrees-inclination orbit and has a nominal operational lifetime of six months. Four classes of organic compounds, namely an amino acid, a quinone, a polycyclic aromatic hydrocarbon (PAH), and a metallo-porphyrin are being studied. Initial reaction conditions were established by hermetically sealing the thin-film organic samples in self-contained micro-environments. Chemical changes in the samples caused by direct exposure to LEO radiation and by interactions with the irradiated microenvironments are monitored in situ by ultraviolet/visible/near-infrared (UV/VIS/NIR) absorption spectroscopy using a novel compact fixed-grating CCD spectrometer with the Sun as its light source. The goals of the O/OREOS mission include: (1) demonstrating key small satellite technologies that can enable future low-cost astrobiology experiments, (2) deploying a miniature UV/VIS/NIR spectrometer suitable for in-situ astrobiology and other scientific investigations, (3) testing the capability to establish a variety of experimental reaction conditions to enable the study of astrobiological processes on small satellites, and (4) measuring the chemical evolution of organic molecules in LEO under conditions that can be extrapolated to interstellar and planetary environments. In this paper, the science and technology development of the SEVO instrument payload and its measurements are described. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Bramall, Nathan E.] Los Gatos Res, Mountain View, CA 94041 USA. [Quinn, Richard; Taylor, Cindy] SETI Inst, Mountain View, CA 94043 USA. [Chittenden, Julie D.; Cook, Amanda] NASA, Ames Res Ctr, NASA Postdoctoral Program, Moffett Field, CA 94035 USA. [Bryson, Kathryn] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Ehrenfreund, Pascale] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA. [Landis, David] Charles Stark Draper Lab Inc, Cambridge, MA 02139 USA. [Jones, Nykola C.; Hoffmann, Soren V.] Aarhus Univ, Inst Storage Ring Facil ISA, DK-8000 Aarhus C, Denmark. RP Bramall, NE (reprint author), Los Gatos Res, Mountain View, CA 94041 USA. EM nebramall@gmail.com RI Ricco, Antonio/A-5273-2010; Jones, Nykola/I-1751-2012; Bryson, Kathryn/I-6914-2012; Salama, Farid/A-8787-2009; OI Salama, Farid/0000-0002-6064-4401; Ricco, Antonio/0000-0002-2355-4984 FU NASA; Exobiology Program [09-EXOB09-1030]; NASA Astrobiology Institute (DDF) FX The authors would like to thank the NASA Astrobiology Small Payloads program for support, Emmett Quigley and Ryan Walker of the NASA Ames Airborne Instrument Development Lab for their work in producing the hardware necessary for the production of the sample cells, Robert Walker for outstanding technical support, the Exobiology Program for additional support (proposal number 09-EXOB09-1030), the NASA Astrobiology Institute (DDF program), and the NASA Postdoctoral Program (NPP) administered by Oak Ridge Associated Universities through a contract with NASA. We also thank the NASA Ames Small Spacecraft Payloads and Technologies Team for their many contributions to the design, development, integration, and test of the SEVO payload system. We also gratefully acknowledge financial support from NASA's Laboratory Astrophysics and Astrobiology Programs. NR 53 TC 6 Z9 6 U1 0 U2 11 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 JAN PY 2012 VL 60 IS 1 BP 121 EP 130 DI 10.1016/j.pss.2011.06.014 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895GC UT WOS:000300483200015 ER PT J AU Salamuniccar, G Loncaric, S Mazarico, E AF Salamuniccar, Goran Loncaric, Sven Mazarico, Erwan TI LU60645GT and MA132843GT catalogues of Lunar and Martian impact craters developed using a Crater Shape-based interpolation crater detection algorithm for topography data SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Moon; Mars; Surface; Cratering; Image processing ID EDGE-DETECTION; REGISTRATION; RECOGNITION AB For Mars, 57,633 craters from the manually assembled catalogues and 72,668 additional craters identified using several crater detection algorithms (CDAs) have been merged into the MA130301GT catalogue. By contrast, for the Moon the most complete previous catalogue contains only 74,923 craters. Two recent missions provided higher-quality digital elevation maps (DEMs): SELENE (in 1/16 degrees resolution) and Lunar Reconnaissance Orbiter (we used up to 1/512 degrees). This was the main motivation for work on the new Crater Shape-based interpolation module, which improves previous CDA as follows: (1) it decreases the number of false-detections for the required number of true detections; (2) it improves detection capabilities for very small craters; and (3) it provides more accurate automated measurements of craters' properties. The results are: (1) LU60645GT, which is currently the most complete (up to similar to D >= 8 km) catalogue of Lunar craters; and (2) MA132843GT catalogue of Martian craters complete up to similar to D >= 2 km, which is the extension of the previous MA130301GT catalogue. As previously achieved for Mars, LU60645GT provides all properties that were provided by the previous Lunar catalogues, plus: (1) correlation between morphological descriptors from used catalogues; (2) correlation between manually assigned attributes and automated measurements; (3) average errors and their standard deviations for manually and automatically assigned attributes such as position coordinates, diameter, depth/diameter ratio, etc; and (4) a review of positional accuracy of used datasets. Additionally, surface dating could potentially be improved with the exhaustiveness of this new catalogue. The accompanying results are: (1) the possibility of comparing a large number of Lunar and Martian craters, of e.g. depth/diameter ratio and 2D profiles; (2) utilisation of a method for re-projection of datasets and catalogues, which is very useful for craters that are very close to poles; and (3) the extension of the previous framework for evaluation of CDAs with datasets and ground-truth catalogue for the Moon. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Salamuniccar, Goran] AVL AST Doo, Zagreb 10020, Croatia. [Salamuniccar, Goran; Loncaric, Sven] Univ Zagreb, Fac Elect Engn & Comp, Zagreb 10000, Croatia. [Mazarico, Erwan] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Mazarico, Erwan] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Salamuniccar, G (reprint author), AVL AST Doo, Av Dubrovnik 10-2, Zagreb 10020, Croatia. EM gsc@ieee.org; sven.loncaric@fer.hr; erwan.m.mazarico@nasa.gov RI Mazarico, Erwan/N-6034-2014 OI Mazarico, Erwan/0000-0003-3456-427X NR 35 TC 15 Z9 17 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 JAN PY 2012 VL 60 IS 1 BP 236 EP 247 DI 10.1016/j.pss.2011.09.003 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895GC UT WOS:000300483200027 ER PT J AU Grun, E Sternovsky, Z Horanyi, M Hoxie, V Robertson, S Xi, J Auer, S Landgraf, M Postberg, F Price, MC Srama, R Starkey, NA Hillier, JK Franchi, IA Tsou, P Westphal, A Gainsforth, Z AF Gruen, E. Sternovsky, Z. Horanyi, M. Hoxie, V. Robertson, S. Xi, J. Auer, S. Landgraf, M. Postberg, F. Price, M. C. Srama, R. Starkey, N. A. Hillier, J. K. Franchi, I. A. Tsou, P. Westphal, A. Gainsforth, Z. TI Active Cosmic Dust Collector SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Interplanetary dust; Interstellar dust; Sample return; Dust collection; Trajectory analysis; Aerogel ID COMET 81P/WILD 2; STARDUST ALUMINUM FOILS; INTERSTELLAR DUST; INTERPLANETARY DUST; HYPERVELOCITY IMPACT; SOLAR-SYSTEM; SAMPLE RETURN; PARTICLE-SIZE; ANALYZER; CASSINI AB The Stardust mission returned two types of unprecedented extraterrestrial samples: the first samples of material from a known solar system body beyond the moon, the comet 81P/Wild2, and the first samples of contemporary interstellar dust. Both sets of samples were captured in aerogel and aluminum foil collectors and returned to Earth in January 2006. While the analysis of particles from comet Wild 2 yielded exciting new results, the search for and analysis of collected interstellar particles is more demanding and is ongoing. Novel dust instrumentation will tremendously improve future dust collection in interplanetary space: an Active Cosmic Dust Collector is a combination of an in-situ dust trajectory sensor (DTS) together with a dust collector consisting of aerogel and/or other collector materials, e.g. such as those used by the Stardust mission. Dust particles' trajectories are determined by the measurement of induced electrical signals when charged particles fly through a position sensitive electrode system. The recorded waveforms enable the reconstruction of the velocity vector with high precision. The DTS described here was subject to performance tests at the Heidelberg dust accelerator at the same time as the recording of impact signals from potential collector materials. The tests with dust particles in the speed range from 3 to 40 km/s demonstrate that trajectories can be measured with accuracies of similar to 1 degrees in direction and similar to 1% in speed. The sensitivity of the DTS electronics is of the order of 10(-16) C and thus the trajectory of cosmic dust particles as small as 0.4 mu m size can be measured. The impact position on the collector can be determined with better than 1 mm precision, which will ease immensely the task of locating sub-micron-sized particles on the collector. Statistically significant numbers of trajectories of interplanetary and interstellar dust particles can thus be collected in interplanetary space and their compositions correlated with their trajectories. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Gruen, E.; Sternovsky, Z.; Horanyi, M.; Hoxie, V.; Robertson, S.; Xi, J.] Univ Colorado, LASP, Boulder, CO 80303 USA. [Auer, S.] A&M Associates, Bayse, VA USA. [Landgraf, M.] ESA ESOC, Darmstadt, Germany. [Postberg, F.] Heidelberg Univ, D-6900 Heidelberg, Germany. [Price, M. C.] Univ Kent, CAPS, Canterbury, Kent, England. [Srama, R.] Univ Stuttgart, D-7000 Stuttgart, Germany. [Starkey, N. A.; Hillier, J. K.; Franchi, I. A.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. [Tsou, P.] JPL, Pasadena, CA USA. [Westphal, A.; Gainsforth, Z.] Univ Berkeley, Berkeley, CA USA. RP Grun, E (reprint author), Max Planck Inst Kernphys, Saupfercheckweg, D-69117 Heidelberg, Germany. EM eberhard.gruen@mpi-hd.mpg.de OI Horanyi, Mihaly/0000-0002-5920-9226 FU NASA; Office of Science, Office of Basic Energy Sciences, U.S. Department of Energy [DE-AC02- 05CH11231] FX The authors thank A.C. Levasseur-Regourd and an anonymous referee for their thoughtful comments that improved the manuscript significantly. The authors acknowledge the support from NASA's Heliophysics and Planetary Instrument Definition and Development programs. The operations of the Advanced Light Source and National Center for Electron Microscopy 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 77 TC 5 Z9 5 U1 2 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD JAN PY 2012 VL 60 IS 1 BP 261 EP 273 DI 10.1016/j.pss.2011.09.006 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895GC UT WOS:000300483200030 ER PT J AU Williams, KE McKay, CP Persson, F AF Williams, Kaj E. McKay, Christopher P. Persson, Fredrik TI The surface energy balance at the Huygens landing site and the moist surface conditions on Titan SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Titan; Surface; Liquid; Energy balance ID HYDROCARBON LAKES; ATMOSPHERE; TEMPERATURES; STABILITY; CONSTRAINTS; DYNAMICS; DRIZZLE; CLOUDS; OCEAN; RAIN AB The Huygens Probe provided a wealth of data concerning the atmosphere of Titan. It also provided tantalizing evidence of a small amount of surface liquid. We have developed a detailed surface energy balance for the Probe landing site. We find that the daily averaged non-radiative fluxes at the surface are 0.7 W m(-2), much larger than the global average value predicted by McKay et al. (1991) of 0.037 W m(-2). Considering the moist surface, the methane and ethane detected by the Probe from the surface is consistent with a ternary liquid of ethane, methane, and nitrogen present on the surface with mole fractions of methane, ethane, and nitrogen of 0.44, 0.34, and 0.22, respectively, and a total mass load of similar to 0.05 kg m(-2). If this liquid is included in the surface energy balance, only a small fraction of the non-radiative energy is due to latent heat release (similar to 10(-3) W m(-2)). If the amount of atmospheric ethane is less than 0.6 x 10(-5), the surface liquid is most likely evaporating over timescales of 5 Titan days, and the moist surface is probably a remnant of a recent precipitation event. If the surface liquid mass loading is increased to 0.5 kg m(-2), then the liquid lifetime increases to 56 Titan days. Our modeling results indicate a dew cycle is unlikely, given that even when the diurnal variation of liquid is in equilibrium, the diurnal mass variation is only 3% of the total liquid. If we assume a high atmospheric mixing ratio of ethane (> 0.6 x 10(-5)), the precipitation of liquid is large (38 cm/Titan year for an ethane mixing ratio of 2 x 10(-5)). Such a flux is many orders of magnitude in excess of the photochemical production rate of ethane. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Williams, Kaj E.; McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA. [Persson, Fredrik] Lulea Univ Technol, S-95187 Lulea, Sweden. RP Williams, KE (reprint author), NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Mail Stop 245-3, Moffett Field, CA 94035 USA. EM kaj.williams@gmail.com NR 39 TC 12 Z9 13 U1 2 U2 8 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 JAN PY 2012 VL 60 IS 1 BP 376 EP 385 DI 10.1016/j.pss.2011.11.005 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895GC UT WOS:000300483200043 ER PT J AU Manfredi, JAR AF Rodriguez Manfredi, Jose Antonio TI The exploration of Mars Past, present and future SO REVISTA DE OCCIDENTE LA Spanish DT Article C1 [Rodriguez Manfredi, Jose Antonio] Ctr Astrobiol INTA CSIC, Dept Instrumentac & Explorac Espacial, Madrid, Spain. [Rodriguez Manfredi, Jose Antonio] NASA, REMS, MSL, Washington, DC 20546 USA. RP Manfredi, JAR (reprint author), Ctr Astrobiol INTA CSIC, Dept Instrumentac & Explorac Espacial, Madrid, Spain. RI Rodriguez-Manfredi, Jose/L-8001-2014 OI Rodriguez-Manfredi, Jose/0000-0003-0461-9815 NR 0 TC 0 Z9 0 U1 0 U2 0 PU FUNDACION JOSE ORTEGA Y GASSET PI MADRID PA REVISTA DE OCCIDENTE FORTUNY 53, 28010 MADRID, SPAIN SN 0034-8635 J9 REV OCCIDENTE JI Rev. Occidente PD JAN PY 2012 IS 368 BP 7 EP 21 PG 15 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 895SF UT WOS:000300515900002 ER PT J AU Leblanc, T McDermid, IS Walsh, TD AF Leblanc, T. McDermid, I. S. Walsh, T. D. TI Ground-based water vapor raman lidar measurements up to the upper troposphere and lower stratosphere for long-term monitoring SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID TABLE MOUNTAIN FACILITY; HUMIDITY MEASUREMENTS; OZONE LIDAR; PERFORMANCE; VALIDATION; BACKSCATTER; CALIBRATION; ATMOSPHERE; SYSTEMS AB Recognizing the importance of water vapor in the upper troposphere and lower stratosphere (UTLS) and the scarcity of high-quality, long-term measurements, JPL began the development of a powerful Raman lidar in 2005 to try to meet these needs. This development was endorsed by the Network for the Detection of Atmospheric Composition Change (NDACC) and the validation program for the EOS-Aura satellite. In this paper we review the stages in the instrumental development, data acquisition and analysis, profile retrieval and calibration procedures of the lidar, as well as selected results from three validation campaigns: MOHAVE (Measurements of Humidity in the Atmosphere and Validation Experiments), MOHAVE-II, and MOHAVE 2009. In particular, one critical result from this latest campaign is the very good agreement (well below the reported uncertainties) observed between the lidar and the Cryogenic Frost-Point Hygrometer in the entire lidar range 3-20 km, with a mean bias not exceeding 2% (lidar dry) in the lower troposphere, and 3% (lidar moist) in the UTLS. Ultimately the lidar has demonstrated capability to measure water vapor profiles from similar to 1 km above the ground to the lower stratosphere with a precision of 10% or better near 13 km and below, and an estimated accuracy of 5 %. Since 2005, nearly 1000 profiles have been routinely measured, and since 2009, the profiles have typically reached 14 km for one-hour integration times and 1.5 km vertical resolution, and can reach 21 km for 6-h integration times using degraded vertical resolutions. These performance figures show that, with our present target of routinely running our lidar two hours per night, 4 nights per week, we can achieve measurements with a precision in the UTLS equivalent to that achieved if launching one CFH per month. C1 [Leblanc, T.; McDermid, I. S.; Walsh, T. D.] CALTECH, Table Mt Facil, Jet Prop Lab, Wrightwood, CA 92397 USA. RP Leblanc, T (reprint author), CALTECH, Table Mt Facil, Jet Prop Lab, Wrightwood, CA 92397 USA. EM leblanc@tmf.jpl.nasa.gov NR 32 TC 16 Z9 17 U1 2 U2 7 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2012 VL 5 IS 1 BP 17 EP 36 DI 10.5194/amt-5-17-2012 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 891RE UT WOS:000300233500002 ER PT J AU Burton, SP Ferrare, RA Hostetler, CA Hair, JW Rogers, RR Obland, MD Butler, CF Cook, AL Harper, DB Froyd, KD AF Burton, S. P. Ferrare, R. A. Hostetler, C. A. Hair, J. W. Rogers, R. R. Obland, M. D. Butler, C. F. Cook, A. L. Harper, D. B. Froyd, K. D. TI Aerosol classification using airborne High Spectral Resolution Lidar measurements - methodology and examples SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID TO-BACKSCATTER RATIO; SPACE TECHNOLOGY EXPERIMENT; ATMOSPHERIC BOUNDARY-LAYER; OPTICAL-PROPERTIES; SAHARAN DUST; RAMAN LIDAR; MULTIWAVELENGTH LIDAR; TROPOSPHERIC AEROSOL; ASIAN DUST; MICROPHYSICAL PROPERTIES AB The NASA Langley Research Center (LaRC) airborne High Spectral Resolution Lidar (HSRL) on the NASA B200 aircraft has acquired extensive datasets of aerosol extinction (532 nm), aerosol optical depth (AOD) (532 nm), backscatter (532 and 1064 nm), and depolarization (532 and 1064 nm) profiles during 18 field missions that have been conducted over North America since 2006. The lidar measurements of aerosol intensive parameters (lidar ratio, depolarization, backscatter color ratio, and spectral depolarization ratio) are shown to vary with location and aerosol type. A methodology based on observations of known aerosol types is used to qualitatively classify the extensive set of HSRL aerosol measurements into eight separate types. Several examples are presented showing how the aerosol intensive parameters vary with aerosol type and how these aerosols are classified according to this new methodology. The HSRL-based classification reveals vertical variability of aerosol types during the NASA ARCTAS field experiment conducted over Alaska and northwest Canada during 2008. In two examples derived from flights conducted during ARCTAS, the HSRL classification of biomass burning smoke is shown to be consistent with aerosol types derived from coincident airborne in situ measurements of particle size and composition. The HSRL retrievals of AOD and inferences of aerosol types are used to apportion AOD to aerosol type; results of this analysis are shown for several experiments. C1 [Burton, S. P.; Ferrare, R. A.; Hostetler, C. A.; Hair, J. W.; Rogers, R. R.; Obland, M. D.; Cook, A. L.; Harper, D. B.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Butler, C. F.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Froyd, K. D.] NOAA, Div Chem Sci, ESRL, Boulder, CO USA. RP Burton, SP (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM sharon.p.burton@nasa.gov RI Froyd, Karl/H-6607-2013; Manager, CSD Publications/B-2789-2015 FU NASA HQ Science Mission Directorate; NASA CALIPSO; US Department of Energy; Office of Science, Office of Biological and Environmental Research program [DE-AI02-05ER63985] FX Funding for this research came from the NASA HQ Science Mission Directorate Radiation Sciences Program; the NASA CALIPSO project; and the US Department of Energy's Atmospheric Science Program Atmospheric System Research, an Office of Science, Office of Biological and Environmental Research program, under Grant No. DE-AI02-05ER63985. The authors also acknowledge the NOAA Air Resources Laboratory (ARL) for the provision of the HYSPLIT transport and dispersion model and READY website (http://www.arl.noaa.gov/ready.php) used for some of the analysis described in this publication. The authors would also like to thank the NASA Langley B200 King Air flight crew for their outstanding work in support of HSRL measurements. NR 102 TC 102 Z9 107 U1 4 U2 46 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 EI 1867-8548 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2012 VL 5 IS 1 BP 73 EP 98 DI 10.5194/amt-5-73-2012 PG 26 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 891RE UT WOS:000300233500004 ER PT J AU O'Dell, CW Connor, B Bosch, H O'Brien, D Frankenberg, C Castano, R Christi, M Crisp, D Eldering, A Fisher, B Gunson, M McDuffie, J Miller, CE Natraj, V Oyafuso, F Polonsky, I Smyth, M Taylor, T Toon, GC Wennberg, PO Wunch, D AF O'Dell, C. W. Connor, B. Boesch, H. O'Brien, D. Frankenberg, C. Castano, R. Christi, M. Crisp, D. Eldering, A. Fisher, B. Gunson, M. McDuffie, J. Miller, C. E. Natraj, V. Oyafuso, F. Polonsky, I. Smyth, M. Taylor, T. Toon, G. C. Wennberg, P. O. Wunch, D. TI The ACOS CO2 retrieval algorithm - Part 1: Description and validation against synthetic observations SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID BULK SCATTERING PROPERTIES; GASES OBSERVING SATELLITE; ATMOSPHERIC CO2; CARBON-DIOXIDE; REFLECTED SUNLIGHT; ICE CLOUDS; COLUMN; SPACE; SCIAMACHY; CH4 AB This work describes the NASA Atmospheric CO2 Observations from Space (ACOS) X-CO2 retrieval algorithm, and its performance on highly realistic, simulated observations. These tests, restricted to observations over land, are used to evaluate retrieval errors in the face of realistic clouds and aerosols, polarized non-Lambertian surfaces, imperfect meteorology, and uncorrelated instrument noise. We find that post-retrieval filters are essential to eliminate the poorest retrievals, which arise primarily due to imperfect cloud screening. The remaining retrievals have RMS errors of approximately 1 ppm. Modeled instrument noise, based on the Greenhouse Gases Observing SATellite (GOSAT) in-flight performance, accounts for less than half the total error in these retrievals. A small fraction of unfiltered clouds, particularly thin cirrus, lead to a small positive bias of similar to 0.3 ppm. Overall, systematic errors due to imperfect characterization of clouds and aerosols dominate the error budget, while errors due to other simplifying assumptions, in particular those related to the prior meteorological fields, appear small. C1 [O'Dell, C. W.; O'Brien, D.; Christi, M.; Polonsky, I.; Taylor, T.] Colorado State Univ, Ft Collins, CO 80523 USA. [Connor, B.] BC Consulting Ltd, Alexandra, South Africa. [Boesch, H.] Univ Leicester, Leicester, Leics, England. [Frankenberg, C.; Castano, R.; Crisp, D.; Eldering, A.; Fisher, B.; Gunson, M.; McDuffie, J.; Miller, C. E.; Natraj, V.; Oyafuso, F.; Smyth, M.; Toon, G. C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Wennberg, P. O.; Wunch, D.] CALTECH, Pasadena, CA USA. RP O'Dell, CW (reprint author), Colorado State Univ, Ft Collins, CO 80523 USA. EM odell@cira.colostate.edu RI Boesch, Hartmut/G-6021-2012; Frankenberg, Christian/A-2944-2013 OI Frankenberg, Christian/0000-0002-0546-5857 FU National Aeronautics and Space Administration; NASA [1380533] FX The authors wish to thank two anonymous reviewers for their constructive suggestions and insightful comments. We would like to thank several colleagues for work they have done that has helped this project: Bashwar Sen for early algorithm management, Linda Brown for spectroscopy development, Rob Spurr for help with the radiative transfer, Lukas Mandrake for GOSAT data analysis, and Ross Salawitch for many useful discussions. A portion 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 Colorado State University contributions to this work were carried out under NASA contract 1380533. NR 72 TC 151 Z9 159 U1 6 U2 48 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2012 VL 5 IS 1 BP 99 EP 121 DI 10.5194/amt-5-99-2012 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 891RE UT WOS:000300233500005 ER PT J AU Kao, DL Wong, PC AF Kao, David L. Wong, Pak C. TI Special issue of selected papers from visualization and data analysis 2011 SO INFORMATION VISUALIZATION LA English DT Editorial Material C1 [Kao, David L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Wong, Pak C.] Pacific NW Natl Lab, Richland, WA 99352 USA. RP Kao, DL (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1473-8716 J9 INFORM VISUAL JI Inf. Vis. PD JAN PY 2012 VL 11 IS 1 SI SI BP 3 EP 4 DI 10.1177/1473871611431117 PG 2 WC Computer Science, Software Engineering SC Computer Science GA 892FI UT WOS:000300271700001 ER PT J AU Smith, SM Heer, M Wang, ZW Huntoon, CL Zwart, SR AF Smith, Scott M. Heer, Martina Wang, Zuwei Huntoon, Carolyn L. Zwart, Sara R. TI Long-Duration Space Flight and Bed Rest Effects on Testosterone and Other Steroids SO JOURNAL OF CLINICAL ENDOCRINOLOGY & METABOLISM LA English DT Article ID NUTRITIONAL-STATUS ASSESSMENT; ENERGY-EXPENDITURE; MALE RATS; SPACEFLIGHT; EXERCISE; MICROGRAVITY; ENDOCRINE; BALANCE; HUMANS; MUSCLE AB Context: Limited data suggest that testosterone is decreased during space flight, which could contribute to bone and muscle loss. Objective: The main objective was to assess testosterone and hormone status in long-and short-duration space flight and bed rest environments and to determine relationships with other physiological systems, including bone and muscle. Design: Blood and urine samples were collected before, during, and after long-duration space flight. Samples were also collected before and after 12-to 14-d missions and from participants in 30-to 90-d bed rest studies. Setting: Space flight studies were conducted on the International Space Station and before and after Space Shuttle missions. Bed rest studies were conducted in a clinical research center setting. Data from Skylab missions are also presented. Participants: All of the participants were male, and they included 15 long-duration and nine short-duration mission crew members and 30 bed rest subjects. Main Outcome Measures: Serum total, free, and bioavailable testosterone were measured along with serum and urinary cortisol, serum dehydroepiandrosterone, dehydroepiandrosterone sulfate, and SHBG. Results: Total, free, and bioavailable testosterone was not changed during long-duration space flight but were decreased (P < 0.01) on landing day after these flights and after short-duration space flight. There were no changes in other hormones measured. Testosterone concentrations dropped before and soon after bed rest, but bed rest itself had no effect on testosterone. Conclusions: There was no evidence for decrements in testosterone during long-duration space flight or bed rest. (J Clin Endocrinol Metab 97: 270-278, 2012) C1 [Smith, Scott M.; Huntoon, Carolyn L.] NASA, Lyndon B Johnson Space Ctr, Space Life Sci Directorate, Houston, TX 77058 USA. [Wang, Zuwei] Enterprise Advisory Serv Inc, Houston, TX 77058 USA. [Zwart, Sara R.] Univ Space Res Assoc, Houston, TX 77058 USA. [Heer, Martina] Univ Bonn, Dept Nutr & Food Sci, D-53117 Bonn, Germany. [Heer, Martina] Profil Inst Metab Res GmbH, D-41460 Neuss, Germany. RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Space Life Sci Directorate, Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA. EM scott.m.smith@nasa.gov FU National Aeronautics and Space Administration; Human Health and Countermeasures Element; International Space Station Medical Project; Flight Analogs Project; Nonexercise Physiological Countermeasures Project; National Center for Research Resources, National Institutes of Health [1UL1RR029876-01]; German Aerospace Center (Germany) [WB 0931] FX This work was funded by the National Aeronautics and Space Administration Human Research Program and specifically the Human Health and Countermeasures Element, the International Space Station Medical Project, the Flight Analogs Project, and the Nonexercise Physiological Countermeasures Project. Bed rest studies were conducted at the University of Texas Medical Branch in Galveston's Institute for Translational Sciences-Clinical Research Center and were supported in part by Grant 1UL1RR029876-01 from the National Center for Research Resources, National Institutes of Health. Support was also provided in part by Grant WB 0931 from the German Aerospace Center (Germany). NR 49 TC 20 Z9 20 U1 0 U2 9 PU ENDOCRINE SOC PI CHEVY CHASE PA 8401 CONNECTICUT AVE, SUITE 900, CHEVY CHASE, MD 20815-5817 USA SN 0021-972X J9 J CLIN ENDOCR METAB JI J. Clin. Endocrinol. Metab. PD JAN PY 2012 VL 97 IS 1 BP 270 EP 278 DI 10.1210/jc.2011-2233 PG 9 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 893YM UT WOS:000300393800060 PM 22049169 ER PT J AU Hwang, JS Han, HC Han, SC Kim, KO Kim, JH Kang, MH Kim, CH AF Hwang, Jong Sun Han, Hyun-Chul Han, Shin-Chan Kim, Kyong-O Kim, Jin-Ho Kang, Moo-Hee Kim, Chang Hwan TI Gravity and geoid model in South Korea and its vicinity by spherical cap harmonic analysis SO JOURNAL OF GEODYNAMICS LA English DT Article DE Gravity; Geoid; Geopotential theory; Asia ID SEA JAPAN SEA; ULLEUNG BASIN; EAST SEA; FIELD; CRUST AB Long wavelength gravity anomalies derived from satellite data have limitations of spatial resolution and accuracy. To complement these weak points, combined datasets merged with shipborne/land gravity data and satellite data are generally compiled using global spherical harmonic, rectangular harmonic, or spherical cap harmonic analysis etc. However, each method also has a different resolution and accuracy. In this study, gravity anomalies and geoid undulations of South Korea and its vicinity are calculated using the spherical cap harmonic method, and the results are compared with those of GGM02C and EGM2008. Absolute and relative geoid height differences between GPS/leveling data and the results of various other methods show that the method used in this study has the lowest RMS error (0.271 m vs 0.344-0.416 m) and standard deviation (0.236 m vs 0.309-0.362 m). This implies that the spherical cap harmonic method has better resolution and accuracy than the other methods. The short wavelength gravity anomalies derived from the spherical cap harmonic coefficients are used to estimate the sediment thickness of the Ulleung Basin, which is poorly known. The sediment thickness of the Ulleung Basin is about 5 km at the center of the basin, and about 12 km at the southern margin. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Hwang, Jong Sun; Han, Hyun-Chul; Kim, Kyong-O; Kim, Jin-Ho; Kang, Moo-Hee] Korea Inst Geosci & Mineral Resources, Petr & Marine Resources Res Div, Taejon 305350, South Korea. [Han, Shin-Chan] NASA, GEST UMBC Planetary Geodynam Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kim, Chang Hwan] Korea Ocean Res & Dev Inst, Dokdo Res Div, Ansan, South Korea. RP Hwang, JS (reprint author), Korea Inst Geosci & Mineral Resources, Petr & Marine Resources Res Div, Taejon 305350, South Korea. EM hwang1975@gmail.com RI Han, Shin-Chan/A-2022-2009 FU Korea Research Foundation; Korean Government [KRF-2006-C00077]; Ministry of Land, Transport and Maritime Affairs [MLTM-10-9106]; Korea Ocean Research and Development Institute [PE 98564] FX This work was partly supported by the Korea Research Foundation Grant funded by the Korean Government (KRF-2006-C00077), the Ministry of Land, Transport and Maritime Affairs (MLTM-10-9106), and Korea Ocean Research and Development Institute (East Sea Program; PE 98564). We thank staff scientists working for Korea Hydrographic and Oceanographic Administration (KHOA), Korea Institute of Geoscience & Mineral Resources (KIGAM), and Korea Ocean Research and Development Institute (KORDI) for providing the gravity data. We also appreciate the valuable comments made by anonymous reviewers, which helped us greatly improve the manuscript. NR 27 TC 0 Z9 0 U1 1 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0264-3707 J9 J GEODYN JI J. Geodyn. PD JAN PY 2012 VL 53 BP 27 EP 33 DI 10.1016/j.jog.2011.08.001 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 894XX UT WOS:000300461900004 ER PT J AU Cantrell, JH Yost, WT AF Cantrell, John H. Yost, William T. TI Determination of Peierls stress from acoustic harmonic generation SO PHILOSOPHICAL MAGAZINE LETTERS LA English DT Article DE Peierls stress; dislocation motion; acoustic harmonic generation; aluminum monocrystals ID WAVY SLIP METALS; DISLOCATION; PLASTICITY AB The interaction of acoustic waves with dislocations leads to aperiodic oscillations in the magnitude of the acoustic nonlinearity parameter beta as a function of the acoustic drive amplitude sigma(ampl). The magnitude and spacing of the oscillations depend on the value of the Peierls stress. A least-square curve fit of the beta(sigma(ampl)) equation to experimental data taken of 99.999% pure aluminum monocrystals oriented for wave propagation along the [1 0 0] crystal axis yields the value 6.2 x 10(4) Pa for the Peierls stress. The value is consistent with the smallest values reported in the literature for aluminum where for both theoretical and experimental studies the reported values range over three orders of magnitude. C1 [Cantrell, John H.; Yost, William T.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Cantrell, JH (reprint author), NASA, Langley Res Ctr, Mail Stop 231, Hampton, VA 23681 USA. EM john.h.cantrell@nasa.gov NR 14 TC 4 Z9 4 U1 0 U2 7 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0950-0839 J9 PHIL MAG LETT JI Philos. Mag. Lett. PY 2012 VL 92 IS 3 BP 128 EP 132 DI 10.1080/09500839.2011.637977 PG 5 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering; Physics, Applied; Physics, Condensed Matter SC Materials Science; Metallurgy & Metallurgical Engineering; Physics GA 894AE UT WOS:000300398400003 ER PT J AU Andersen, MPS Nielsen, OJ Hurley, MD Wallington, TJ AF Andersen, M. P. Sulbaek Nielsen, O. J. Hurley, M. D. Wallington, T. J. TI Atmospheric chemistry of t-CF3CH = CHCl: products and mechanisms of the gas-phase reactions with chlorine atoms and hydroxyl radicals SO PHYSICAL CHEMISTRY CHEMICAL PHYSICS LA English DT Article ID INITIATED OXIDATION; OH RADICALS; RATE CONSTANTS; CL ATOMS; SELF-REACTION; KINETICS; OZONE; ALDEHYDES; HYDROFLUOROCARBONS; DEGRADATION AB FTIR-smog chamber techniques were used to study the products and mechanisms of the Cl atom and OH radical initiated oxidation of trans-3,3,3-trifluoro-1-chloro-propene, t-CF3CH=CHCl, in 700 Torr of air or N-2/O-2 diluent at 296 +/- 2 K. The reactions of Cl atoms and OH radicals with t-CF3CH=CHCl occur via addition to the C=C double bond; chlorine atoms add 15 +/- 5% at the terminal carbon and 85 +/- 5% at the central carbon, OH radicals add approximately 40% at the terminal carbon and 60% at the central carbon. The major products in the Cl atom initiated oxidation of t-CF3CH=CHCl were CF3CHClCHO and CF3C(O)CHCl2, minor products were CF3CHO, HCOCl and CF3COCl. The yields of CF3C(O)CHCl2, CF3CHClCOCl and CF3COCl increased at the expense of CF3CHO, HCOCl and CF3CHClCHO as the O-2 partial pressure was increased over the range 10-700 Torr. Chemical activation plays a significant role in the fate of CF3CH(O)CHCl2 and CF3CClHCHClO radicals. In addition to reaction with O-2 to yield CF3COCl and HO2 the major competing fate of CF3CHClO is Cl elimination to give CF3CHO (not C-C bond scission as previously thought). As part of this study k(Cl + CF3C(O)CHCl2) = (2.3 +/- 0.3) x 10(-14) and k(Cl + CF3CHClCHO) = (7.5 +/- 2.0) x 10 (12) cm (3) molecule (1) s (1) were determined using relative rate techniques. Reaction with OH radicals is the major atmospheric sink for t-CF3CH=CHCl. Chlorine atom elimination giving the enol CF3CH=CHOH appears to be the sole atmospheric fate of the CF3CHCHClOH radicals. The yield of CF3COOH in the atmospheric oxidation of t-CF3CH=CHCl will be negligible (<2%). The results are discussed with respect to the atmospheric chemistry and environmental impact of t-CF3CH=CHCl. C1 [Andersen, M. P. Sulbaek] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nielsen, O. J.] Univ Copenhagen, Dept Chem, DK-2100 Copenhagen, Denmark. [Hurley, M. D.; Wallington, T. J.] Ford Motor Co, Syst Analyt & Environm Sci Dept, Dearborn, MI 48121 USA. RP Andersen, MPS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 183-901, Pasadena, CA 91109 USA. EM mpsa@jpl.nasa.gov RI Sulbaek Andersen, Mads/C-4708-2008; Nielsen, Ole/B-9988-2011 OI Sulbaek Andersen, Mads/0000-0002-7976-5852; Nielsen, Ole/0000-0002-0088-3937 FU Danish Natural Science Research Councilthe Villum Kann Rasmussen Foundation; EUROCHAMP2; National Aeronautics and Space Administration FX We thank R. Singh (Honeywell International Inc.) for providing the t-CF3CH=CHCl samples used in this study and S. P. Sander (JPL) for helpful discussions. We thank N. Prisle and F. F. Osterstrom (University of Copenhagen) for assistance in the experimental work. O.J.N. acknowledges financial support from the Danish Natural Science Research Councilthe Villum Kann Rasmussen Foundation and EUROCHAMP2. This work was performed partly at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. M.P.S.A. is supported by an appointment to the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. Copyright 2011. NR 33 TC 6 Z9 6 U1 1 U2 22 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1463-9076 J9 PHYS CHEM CHEM PHYS JI Phys. Chem. Chem. Phys. PY 2012 VL 14 IS 5 BP 1735 EP 1748 DI 10.1039/c1cp22925g PG 14 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 876MZ UT WOS:000299113000025 PM 22187719 ER PT S AU Jhabvala, M Choi, K AF Jhabvala, M. Choi, K. BE Razeghi, M Tournie, E Brown, GJ TI Evolution of QWIP focal plane development at the NASA/Goddard Space Flight Center SO QUANTUM SENSING AND NANOPHOTONIC DEVICES IX SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Quantum Sensing and Nanophotonic Devices IX CY JAN 22-26, 2012 CL San Francisco, CA SP SPIE DE QWIP detectors; quantum well detectors; infrared focal planes; IR detector arrays; GaAs detectors AB The development of GaAs quantum well infrared photodetectors (QWIPs) at NASA's Goddard Space Flight Center began in the late 1980s and has continued ever since. Initial developments produced single element detectors and shortly thereafter in 1990 a 128x 128 element array was developed in collaboration with AT&T Bell Labs and Rockwell Science Center. Since that time we have developed numerous generations of QWIP arrays most recently resulting in the multi-QWIP focal plane for the next NASA-US Geological Survey Landsat mission to be launched in December of 2012. This paper will describe the technological evolutionary process from concept to a space-flight qualified infrared detector system. Many developments have been accomplished in the ensuing two decades as well as numerous experiments, both ground-based and airborne en route to qualifying for a NASA space flight mission. Some of these experiments will also be described as well as our current development for the next generation of QWIP focal planes for potential earth observing missions. C1 [Jhabvala, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Jhabvala, M (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. NR 12 TC 2 Z9 2 U1 0 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-911-1 J9 PROC SPIE PY 2012 VL 8268 AR 82682P DI 10.1117/12.903680 PG 14 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA BYT71 UT WOS:000300191700070 ER PT S AU Soibel, A Nguyen, J Rafol, SB Liao, A Hoeglund, L Khoshakhlagh, A Keo, SA Mumolo, JM Liu, J Ting, DZY Gunapala, SD AF Soibel, Alexander Nguyen, Jean Rafol, Sir B. Liao, Anna Hoeglund, Linda Khoshakhlagh, Arezou Keo, Sam A. Mumolo, Jason M. Liu, John Ting, David Z-Y. Gunapala, Sarath D. BE Razeghi, M Tournie, E Brown, GJ TI High-performance LWIR superlattice detectors and FPA based on CBIRD design SO QUANTUM SENSING AND NANOPHOTONIC DEVICES IX SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Quantum Sensing and Nanophotonic Devices IX CY JAN 22-26, 2012 CL San Francisco, CA SP SPIE DE unipolar barrier; heterostructure; infrared; photodetector; superlattice AB We report our recent efforts on advancing of antimonide superlattice based infrared photodetectors and demonstration of focal plane arrays based on a complementary barrier infrared detector (CBIRD) design. By optimizing design and growth condition we succeeded to reduce the operational bias of CBIRD single pixel detector without increase of dark current or degradation of quantum efficiency. We demonstrated a 1024x1024 pixel long-wavelength infrared focal plane array utilizing CBIRD design. An 11.5 mu m cutoff focal plane without anti-reflection coating has yielded noise equivalent differential temperature of 53 mK at operating temperature of 80 K, with 300 K background and cold-stop. Imaging results from a recent 10 mu m cutoff focal plane array are also presented. These results advance state-of-the art of superlattice detectors and demonstrated advantages of CBIRD architecture for realization of FPA. C1 [Soibel, Alexander; Nguyen, Jean; Rafol, Sir B.; Liao, Anna; Hoeglund, Linda; Khoshakhlagh, Arezou; Keo, Sam A.; Mumolo, Jason M.; Liu, John; Ting, David Z-Y.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Soibel, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 16 TC 1 Z9 1 U1 0 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-911-1 J9 PROC SPIE PY 2012 VL 8268 AR 82680Y DI 10.1117/12.909614 PG 6 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA BYT71 UT WOS:000300191700025 ER PT J AU Ehrenfreund, P McKay, C Rummel, JD Foing, BH Neal, CR Masson-Zwaan, T Ansdell, M Peter, N Zarnecki, J Mackwell, S Perino, MA Billings, L Mankins, J Race, M AF Ehrenfreund, Pascale McKay, Chris Rummel, John D. Foing, Bernard H. Neal, Clive R. Masson-Zwaan, Tanja Ansdell, Megan Peter, Nicolas Zarnecki, John Mackwell, Steve Perino, Maria Antionetta Billings, Linda Mankins, John Race, Margaret TI Toward a global space exploration program: A stepping stone approach SO ADVANCES IN SPACE RESEARCH LA English DT Review DE Space exploration; Planetary protection; International cooperation ID GAMMA-RAY SPECTROMETER; LUNAR PROSPECTOR; MERIDIANI-PLANUM; INTERNATIONAL-CONFERENCE; CLEMENTINE MISSION; MAGNETIC-FIELDS; SMART-1 MISSION; LASER ALTIMETRY; BURNS FORMATION; LCROSS IMPACT AB In response to the growing importance of space exploration in future planning, the Committee on Space Research (COSPAR) Panel on Exploration (PEX) was chartered to provide independent scientific advice to support the development of exploration programs and to safeguard the potential scientific assets of solar system objects. In this report, PEX elaborates a stepwise approach to achieve a new level of space cooperation that can help develop world-wide capabilities in space science and exploration and support a transition that will lead to a global space exploration program. The proposed stepping stones are intended to transcend cross-cultural barriers, leading to the development of technical interfaces and shared legal frameworks and fostering coordination and cooperation on a broad front. Input for this report was drawn from expertise provided by COSPAR Associates within the international community and via the contacts they maintain in various scientific entities. The report provides a summary and synthesis of science roadmaps and recommendations for planetary exploration produced by many national and international working groups, aiming to encourage and exploit synergies among similar programs. While science and technology represent the core and, often, the drivers for space exploration, several other disciplines and their stakeholders (Earth science, space law, and others) should be more robustly interlinked and involved than they have been to date. The report argues that a shared vision is crucial to this linkage, and to providing a direction that enables new countries and stakeholders to join and engage in the overall space exploration effort. Building a basic space technology capacity within a wider range of countries, ensuring new actors in space act responsibly, and increasing public awareness and engagement are concrete steps that can provide a broader interest in space exploration, worldwide, and build a solid basis for program sustainability. By engaging developing countries and emerging space nations in an international space exploration program, it will be possible to create a critical bottom-up support structure to support program continuity in the development and execution of future global space exploration frameworks. With a focus on stepping stones, COSPAR can support a global space exploration program that stimulates scientists in current and emerging spacefaring nations, and that will invite those in developing countries to participate-pursuing research aimed at answering outstanding questions about the origins and evolution of our solar system and life on Earth (and possibly elsewhere). COSPAR, in cooperation with national and international science foundations and space-related organizations, will advocate this stepping stone approach to enhance future cooperative space exploration efforts. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Ehrenfreund, Pascale; Ansdell, Megan] George Washington Univ, Elliott Sch Int Affairs, Inst Space Policy, Washington, DC 20052 USA. [McKay, Chris] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. [Rummel, John D.] E Carolina Univ, Inst Coastal Sci & Policy, Greenville, NC 27858 USA. [Foing, Bernard H.] European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands. [Neal, Clive R.] Univ Notre Dame, Dept Civil Eng & Geol Sci, Notre Dame, IN 46556 USA. [Masson-Zwaan, Tanja] Leiden Univ, Int Inst Air & Space Law, NL-2311 ES Leiden, Netherlands. [Peter, Nicolas] European Space Agcy, F-75015 Paris, France. [Zarnecki, John] Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. [Mackwell, Steve] USRA Lunar & Planetary Inst, Houston, TX 77058 USA. [Perino, Maria Antionetta] Thales Alenia Spazio, I-10146 Turin, Italy. [Billings, Linda] George Washington Univ, Sch Media & Publ Affairs, Washington, DC 20052 USA. [Mankins, John] Artemis Innovat Management Solut LLC, Santa Maria, CA 93456 USA. [Race, Margaret] SETI Inst, Mountain View, CA 94043 USA. RP Ehrenfreund, P (reprint author), George Washington Univ, Elliott Sch Int Affairs, Inst Space Policy, Washington, DC 20052 USA. EM pehren@gwu.edu RI Mackwell, Stephen/H-2772-2013 NR 214 TC 17 Z9 18 U1 4 U2 21 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 JAN 1 PY 2012 VL 49 IS 1 BP 2 EP 48 DI 10.1016/j.asr.2011.09.014 PG 47 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 887YY UT WOS:000299972200002 ER PT J AU Gurgiolo, C Goldstein, ML Vinas, AF Fazakerley, AN AF Gurgiolo, C. Goldstein, M. L. Vinas, A. F. Fazakerley, A. N. TI Direct observations of the formation of the solar wind halo from the strahl SO ANNALES GEOPHYSICAE LA English DT Article DE Interplanetary physics; Solar wind plasma; Sources of the solar wind; Space plasma physics; Wave-particle interactions ID ELECTRON-DISTRIBUTION FUNCTIONS; HELIOS PLASMA-EXPERIMENT; SUPRATHERMAL ELECTRONS; WAVES; DISTRIBUTIONS; CORONA AB Observations of a continual erosion of the strahl and build up of the halo with distance from the sun suggests that, at least in part, the halo may be formed as a result of scattering of the strahl. This hypothesis is supported in this paper by observation of intense scattering of strahl electrons, which gives rise to a proto-halo electron population. This population eventually merges into, or becomes the halo. The fact that observations of intense scattering of the strahl are not common implies that the formation of the halo may not be a continuous process, but one that occurs, in part, in bursts in regions where the conditions responsible for the scattering are optimum. C1 [Gurgiolo, C.] Bitterroot Basic Res, Hamilton, MT 59840 USA. [Goldstein, M. L.; Vinas, A. F.] NASA, Geospace Sci Lab, Code 673, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fazakerley, A. N.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Gurgiolo, C (reprint author), Bitterroot Basic Res, Hamilton, MT 59840 USA. EM chris@gurgiolo.com RI Goldstein, Melvyn/B-1724-2008 FU NASA [NNX10AC90G] FX The authors would like to acknowledge the work and role the Cluster Active Archive (CAA) and thank the EFW, WHISPER and FGM teams for providing the data used in this study. We would also like to acknowledge the PEACE team at MSSL who worked on and are constantly improving the instrument calibration. CG would like to acknowledge support from NASA Grant NNX10AC90G. NR 31 TC 9 Z9 9 U1 0 U2 2 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 0992-7689 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2012 VL 30 IS 1 BP 163 EP 175 DI 10.5194/angeo-30-163-2012 PG 13 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 891PW UT WOS:000300230100016 ER PT J AU Huang, K Zhuang, G Lin, Y Fu, JS Wang, Q Liu, T Zhang, R Jiang, Y Deng, C Fu, Q Hsu, NC Cao, B AF Huang, K. Zhuang, G. Lin, Y. Fu, J. S. Wang, Q. Liu, T. Zhang, R. Jiang, Y. Deng, C. Fu, Q. Hsu, N. C. Cao, B. TI Typical types and formation mechanisms of haze in an Eastern Asia megacity, Shanghai SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID YANGTZE-RIVER DELTA; AEROSOL OPTICAL-PROPERTIES; TRACE GAS EMISSIONS; AIR-POLLUTION; CARBON-MONOXIDE; CHEMICAL-COMPOSITION; SOURCE APPORTIONMENT; ATMOSPHERIC AEROSOL; LIDAR OBSERVATIONS; TROPOSPHERIC NO2 AB An intensive aerosol and gases campaign was performed at Shanghai in the Yangtze River Delta region over Eastern China from late March to early June 2009. This study provided a complementary picture of typical haze types and the formation mechanisms in megacities over China by using a synergy of ground-based monitoring, satellite and lidar observations. During the whole study period, several extreme low visibility periods were observed with distinct characteristics, and three typical haze types were identified, i.e. secondary inorganic pollution, dust, and biomass burning. Sulfate, nitrate and ammonium accounted for a major part of PM2.5 mass during the secondary inorganic pollution, and the good correlation between SO2/NOx/CO and PM2.5 indicated that coal burning and vehicle emission were the major sources. Large-scale regions with high AOD (aerosol optical depths) and low Angstrom exponent were detected by remote-sensing observation during the dust pollution episode, and this episode corresponded to coarse particles rich in mineral components such as Al and Ca contributing 76.8% to TSP. The relatively low Ca/Al ratio of 0.75 along with the air mass backward trajectory analysis suggested the dust source was from Gobi Desert. Typical tracers for biomass burning from satellite observation (column CO and HCHO) and from ground measurement (CO, particulate K+, OC, and EC) were greatly enhanced during the biomass burning pollution episode. The exclusive linear correlation between CO and PM2.5 corroborated that organic aerosol dominated aerosol chemistry during biomass burning, and the high concentration and enrichment degree of arsenic (As) could be also partly derived from biomass burning. Aerosol optical profile observed by lidar demonstrated that aerosol was mainly constrained below the boundary layer and comprised of spheric aerosol (depolarization ratio <5%) during the secondary inorganic and biomass burning episodes, while thick dust layer distributed at altitudes from near surface to 1.4 km (average depolarization ratio = 0.122 +/- 0.023) with dust accounting for 44-55% of the total aerosol extinction coefficient during the dust episode. This study portrayed a good picture of the typical haze types and proposed that identification of the complicated emission sources is important for the air quality improvement in megacities in China. C1 [Huang, K.; Zhuang, G.; Lin, Y.; Wang, Q.; Liu, T.; Zhang, R.; Jiang, Y.; Deng, C.; Cao, B.] Fudan Univ, Dept Environm Sci & Engn, Ctr Atmospher Chem Study, Shanghai 200433, Peoples R China. [Huang, K.; Fu, J. S.] Univ Tennessee, Dept Civil & Environm Engn, Knoxville, TN 37996 USA. [Fu, Q.] Shanghai Environm Monitoring Ctr, Shanghai 200030, Peoples R China. [Hsu, N. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zhuang, G (reprint author), Fudan Univ, Dept Environm Sci & Engn, Ctr Atmospher Chem Study, Shanghai 200433, Peoples R China. EM gzhuang@fudan.edu.cn RI Huang, Kan/E-4824-2011; Hsu, N. Christina/H-3420-2013; Xiongfei, Zhao/G-7690-2015 FU MOST, China [2010DFA92230]; National Natural Science Foundation of China [41128005, 20877020, 20977017]; Shanghai environmental protection science developing funding [2010-003, 2011-55] FX Many thanks to the MODIS, OMI and AIRS data processing team members. We thank Sugimoto Nobuo and Shimizu Atsushi of National Institute for Environmental Studies, Japan, for the lidar setup and data inversion. This work was supported by the great international collaboration project of MOST, China (2010DFA92230), National Natural Science Foundation of China (Grant Nos. 41128005 (fund for collaboration with oversea scholars), 20877020, 20977017), and Shanghai environmental protection science developing funding (No. 2010-003, 2011-55). NR 110 TC 71 Z9 88 U1 17 U2 190 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 1 BP 105 EP 124 DI 10.5194/acp-12-105-2012 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 892XZ UT WOS:000300320200004 ER PT J AU Dupont, R Pierce, B Worden, J Hair, J Fenn, M Hamer, P Natarajan, M Schaack, T Lenzen, A Apel, E Dibb, J Diskin, G Huey, G Weinheimer, A Kondo, Y Knapp, D AF Dupont, R. Pierce, B. Worden, J. Hair, J. Fenn, M. Hamer, P. Natarajan, M. Schaack, T. Lenzen, A. Apel, E. Dibb, J. Diskin, G. Huey, G. Weinheimer, A. Kondo, Y. Knapp, D. TI Attribution and evolution of ozone from Asian wild fires using satellite and aircraft measurements during the ARCTAS campaign SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID TROPOSPHERIC EMISSION SPECTROMETER; BIOMASS BURNING EMISSIONS; LONG-RANGE TRANSPORT; AEROSOL OPTICAL-THICKNESS; BOREAL FOREST-FIRES; CARBON-MONOXIDE; INTERANNUAL VARIABILITY; POLLUTION TRANSPORT; FIELD EXPERIMENT; ZONAL STRUCTURE AB We use ozone and carbon monoxide measurements from the Tropospheric Emission Spectrometer (TES), model estimates of Ozone, CO, and ozone pre-cursors from the Real-time Air Quality Modeling System (RAQMS), and data from the NASA DC8 aircraft to characterize the source and dynamical evolution of ozone and CO in Asian wildfire plumes during the spring ARCTAS campaign 2008. On the 19 April, NASA DC8 O-3 and aerosol Differential Absorption Lidar (DIAL) observed two biomass burning plumes originating from North-Western Asia (Kazakhstan) and South-Eastern Asia (Thailand) that advected eastward over the Pacific reaching North America in 10 to 12 days. Using both TES observations and RAQMS chemical analyses, we track the wildfire plumes from their source to the ARCTAS DC8 platform. In addition to photochemical production due to ozone pre-cursors, we find that exchange between the stratosphere and the troposphere is a major factor influencing O-3 concentrations for both plumes. For example, the Kazakhstan and Siberian plumes at 55 degrees North is a region of significant springtime stratospheric/tropospheric exchange. Stratospheric air influences the Thailand plume after it is lofted to high altitudes via the Himalayas. Using comparisons of the model to the aircraft and satellite measurements, we estimate that the Kazakhstan plume is responsible for increases of O-3 and CO mixing ratios by approximately 6.4 ppbv and 38 ppbv in the lower troposphere (height of 2 to 6 km), and the Thailand plume is responsible for increases of O-3 and CO mixing ratios of approximately 11 ppbv and 71 ppbv in the upper troposphere (height of 8 to 12 km) respectively. However, there are significant sources of uncertainty in these estimates that point to the need for future improvements in both model and satellite observations. For example, it is challenging to characterize the fraction of air parcels from the stratosphere versus those from the fire because of the low sensitivity of the TES CO estimates used to mark stratospheric air versus air parcels affected by the smoke plume. Model transport uncertainties, such as too much dispersion, results in a broad plume structure from the Kazakhstan fires that is approximately 2 km lower than the plume observed by aircraft. Consequently, the model and TES data do not capture the photochemical production of ozone in the Kazakhstan plume that is apparent in the aircraft in situ data. However, ozone and CO distributions from TES and RAQMS model estimates of the Thailand plume are within the uncertainties of the TES data. Therefore, the RAQMS model is better able to characterize the emissions from this fire, the mixing of ozone from the stratosphere to the plume, and the photochemical production and transport of ozone and ozone pre-cursors as the plume moves across the Pacific. C1 [Dupont, R.; Worden, J.; Hamer, P.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Pierce, B.] NOAA NESDIS STAR, Madison, WI USA. [Hair, J.; Natarajan, M.; Diskin, G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Fenn, M.] Sci Syst & Applicat Inc, Hampton, VA USA. [Schaack, T.; Lenzen, A.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA. [Apel, E.; Weinheimer, A.; Knapp, D.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Dibb, J.] Univ New Hampshire EOS, Durham, NH USA. [Huey, G.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Kondo, Y.] Univ Tokyo, Adv Sci & Technol Res Ctr, Tokyo, Japan. RP Dupont, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA. EM richard.dupont@live.fr RI Kondo, Yutaka/D-1459-2012; Pierce, Robert Bradley/F-5609-2010 OI Pierce, Robert Bradley/0000-0002-2767-1643 FU NASA [NAG: NNX08AD29G] FX HCN measurements were obtained from the Caltech Chemical Ionization Mass Spectrometer and were made available by P. O. Wennberg, J. C. Crounse and A. Kurten. Support for Caltech from NASA (NAG: NNX08AD29G) is gratefully acknowledged. NR 104 TC 13 Z9 13 U1 1 U2 27 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 1 BP 169 EP 188 DI 10.5194/acp-12-169-2012 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 892XZ UT WOS:000300320200008 ER PT J AU Stevens, RG Pierce, JR Brock, CA Reed, MK Crawford, JH Holloway, JS Ryerson, TB Huey, LG Nowak, JB AF Stevens, R. G. Pierce, J. R. Brock, C. A. Reed, M. K. Crawford, J. H. Holloway, J. S. Ryerson, T. B. Huey, L. G. Nowak, J. B. TI Nucleation and growth of sulfate aerosol in coal-fired power plant plumes: sensitivity to background aerosol and meteorology SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID CLOUD CONDENSATION NUCLEI; SULFURIC-ACID; ATMOSPHERIC NUCLEATION; ULTRAFINE PARTICLES; CCN CONCENTRATIONS; UNITED-STATES; MEXICO-CITY; MODEL; UNCERTAINTIES; MICROPHYSICS AB New-particle formation in the plumes of coal-fired power plants and other anthropogenic sulfur sources may be an important source of particles in the atmosphere. It remains unclear, however, how best to reproduce this formation in global and regional aerosol models with grid-box lengths that are 10s of kilometers and larger. The predictive power of these models is thus limited by the resultant uncertainties in aerosol size distributions. In this paper, we focus on sub-grid sulfate aerosol processes within coal-fired power plant plumes: the sub-grid oxidation of SO2 with condensation of H2SO4 onto newly-formed and pre-existing particles. We have developed a modeling framework with aerosol microphysics in the System for Atmospheric Modelling (SAM), a Large-Eddy Simulation/Cloud-Resolving Model (LES/CRM). The model is evaluated against aircraft observations of new-particle formation in two different power-plant plumes and reproduces the major features of the observations. We show how the downwind plume aerosols can be greatly modified by both meteorological and background aerosol conditions. In general, new-particle formation and growth is greatly reduced during polluted conditions due to the large pre-existing aerosol surface area for H2SO4 condensation and particle coagulation. The new-particle formation and growth rates are also a strong function of the amount of sunlight and NOx since both control OH concentrations. The results of this study highlight the importance for improved sub-grid particle formation schemes in regional and global aerosol models. C1 [Stevens, R. G.; Pierce, J. R.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Brock, C. A.; Holloway, J. S.; Ryerson, T. B.; Nowak, J. B.] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Reed, M. K.] Tennessee Technol Univ, Cookeville, TN 38505 USA. [Crawford, J. H.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Huey, L. G.] Georgia Inst Technol, Dept Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Nowak, J. B.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. RP Stevens, RG (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. EM robin.stevens@dal.ca RI Nowak, John/B-1085-2008; Holloway, John/F-9911-2012; Brock, Charles/G-3406-2011; Pierce, Jeffrey/E-4681-2013; Ryerson, Tom/C-9611-2009; Crawford, James/L-6632-2013; Stevens, Robin/D-1341-2014; Manager, CSD Publications/B-2789-2015 OI Nowak, John/0000-0002-5697-9807; Holloway, John/0000-0002-4585-9594; Brock, Charles/0000-0002-4033-4668; Pierce, Jeffrey/0000-0002-4241-838X; Crawford, James/0000-0002-6982-0934; Stevens, Robin/0000-0002-8737-6988; FU Electric Power Research Institute (EPRI) FX This research was funded by the Electric Power Research Institute (EPRI). We would like to thank Marat Khairoutdinov of the School of Marine and Atmospheric Sciences, Stony Brook University, for access to and help with the System for Atmospheric Modeling. NCEP Reanalysis data provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from their Web site at http://www.esrl.noaa.gov/psd/. NR 59 TC 31 Z9 31 U1 2 U2 45 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 1 BP 189 EP 206 DI 10.5194/acp-12-189-2012 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 892XZ UT WOS:000300320200009 ER PT J AU Li, KF Tian, B Waliser, DE Schwartz, MJ Neu, JL Worden, JR Yung, YL AF Li, K. -F. Tian, B. Waliser, D. E. Schwartz, M. J. Neu, J. L. Worden, J. R. Yung, Y. L. TI Vertical structure of MJO-related subtropical ozone variations from MLS, TES, and SHADOZ data SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID MADDEN-JULIAN OSCILLATION; TROPOSPHERIC EMISSION SPECTROMETER; MONITORING INSTRUMENT; INTERIM REANALYSIS; AURA SATELLITE; RETRIEVALS; VALIDATION; OBJECTIVES; ENVISAT; SYSTEM AB Tian et al. (2007) found that the MJO-related total column ozone (O-3) anomalies of 10DU (peak-to-trough) are mainly evident over the subtropics and dynamically driven by the vertical movement of the subtropical tropopause layer. It was then hypothesized that the subtropical total column O-3 anomalies are primarily associated with the O-3 variability in the stratosphere rather the troposphere. In this paper, we investigate the vertical structure of MJO-related subtropical O-3 variations using the vertical O-3 profiles from the Aura Microwave Limb Sounder (MLS) and Tropospheric Emission Spectrometer (TES), as well as in-situ measurements by the Southern Hemisphere Additional Ozonesondes (SHADOZ) project. Our analysis indicates that the subtropical O-3 anomalies maximize approximately in the lower stratosphere (60-100 hPa). Furthermore, the spatial-temporal patterns of the subtropical O-3 anomalies in the lower stratosphere are very similar to that of the total column. In particular, they are both dynamically driven by the vertical movement of subtropical tropopause. The subtropical partial O-3 column anomalies between 30-200 hPa accounts for more than 50% of the total O-3 column anomalies. TES measurements show that at most 27% of the total O-3 column anomalies are contributed by the tropospheric components. This indicates that the subtropical total column O-3 anomalies are mostly from the O-3 anomalies in the lower stratosphere, which supports the hypothesis of Tian et al. (2007). The strong connection between the intraseasonal subtropical stratospheric O-3 variations and the MJO implies that the stratospheric O-3 variations may be predictable with similar lead times over the subtropics. Future work could involve a similar study or an O-3 budget analysis using a sophisticated chemical transport model in the near-equatorial regions where the observed MJO signals of total column O-3 are weak. C1 [Li, K. -F.; Yung, Y. L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Tian, B.; Waliser, D. E.; Schwartz, M. J.; Neu, J. L.; Worden, J. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Li, KF (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM kfl@gps.caltech.edu RI Tian, Baijun/A-1141-2007; Schwartz, Michael/F-5172-2016 OI Tian, Baijun/0000-0001-9369-2373; Schwartz, Michael/0000-0001-6169-5094 FU National Science Foundation (NSF) [ATM-0840787, ATM-0840755]; National Aeronautics and Space Administration FX This research was supported in part by the National Science Foundation (NSF) grant ATM-0840787 to California Institute of Technology (Caltech) and ATM-0840755 to University of California, Los Angeles. Part of this research was carried out at Jet Propulsion Laboratory, Caltech, under a contract with National Aeronautics and Space Administration. ERA-Interim data were obtained from the ECMWF Data Server (http://data.ecmwf.int/data/). The RMM index was obtained from the Bureau of Meteorology website (http://www.bom.gov.au/climate/mjo/). The SHADOZ data were obtained from SHADOZ data server (http://croc.gsfc.nasa.gov/shadoz/). NR 45 TC 9 Z9 10 U1 1 U2 17 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2012 VL 12 IS 1 BP 425 EP 436 DI 10.5194/acp-12-425-2012 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 892XZ UT WOS:000300320200023 ER PT J AU He, F Zhang, XX Chen, B Fok, MC AF He Fei Zhang Xiao-Xin Chen Bo Fok Mei-Ching TI Inversion of the Earth's plasmaspheric density distribution from EUV images with genetic algorithm SO CHINESE JOURNAL OF GEOPHYSICS-CHINESE EDITION LA Chinese DT Article DE Earth's plasmasphere; Density distribution; Genetic algorithm; Inversion ID ULTRAVIOLET-SCANNER; INTERPLANETARY GAS; RADIATION; TELESCOPE; MISSION; NIGHT; SKY AB The principles for inversion of plasmaspheric He+ density from the extreme ultraviolet images of the Earth's plasmasphere with one-dimensional genetic algorithm are introduced. The three-dimensional problem is transformed to one-dimensional case through flux tube approximation and dipole magnetic field approximation. With the weight matrix, the extreme ultraviolet intensity integration equation is discretized into linear equation systems, then the one-dimensional real-coded genetic algorithm is used to calculate the equatorial plane plasmaspheric He+ density, and finally the three-dimensional density is obtained by magnetic field line tracing. The density and intensity simulated by the dynamic global core plasma model are used as the primary input parameters, and the corresponding density distribution is determined through genetic iterations. The results show that the relative density error is less than 8% and the relative intensity error tends to be zero, which proves that our algorithm is effective and feasible. Investigations in this work will provide basis for the inversion of the moon-based EUV images in the Second Phase of Chinese Lunar Exploration Program. C1 [He Fei; Chen Bo] Chinese Acad Sci, Changchun Inst Opt Fine Mech & Phys, Changchun 130033, Peoples R China. [Zhang Xiao-Xin] China Meteorol Adm, Natl Ctr Space Weather, Beijing 100081, Peoples R China. [Fok Mei-Ching] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP He, F (reprint author), Chinese Acad Sci, Changchun Inst Opt Fine Mech & Phys, Changchun 130033, Peoples R China. EM hef@ciomp.ac.cn; xxzhang@cma.gov.cn RI he, fei/B-9277-2012; Fok, Mei-Ching/D-1626-2012 NR 25 TC 1 Z9 1 U1 1 U2 6 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 0001-5733 J9 CHINESE J GEOPHYS-CH JI Chinese J. Geophys.-Chinese Ed. PD JAN PY 2012 VL 55 IS 1 BP 29 EP 35 DI 10.6038/j.issn.0001-5733.2012.01.003 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 890FA UT WOS:000300129300003 ER PT J AU Rousseaux, CSG Lowe, R Feng, M Waite, AM Thompson, PA AF Rousseaux, Cecile S. G. Lowe, Ryan Feng, Ming Waite, Anya M. Thompson, Peter A. TI The role of the Leeuwin Current and mixed layer depth on the autumn phytoplankton bloom off Ningaloo Reef, Western Australia SO CONTINENTAL SHELF RESEARCH LA English DT Article DE Phytoplankton; Mixed layer depth; Leeuwin Current; Eastern Indian Ocean; Ningaloo Reef; ENSO ID SOFT CORALS; INTERANNUAL VARIABILITY; PRODUCTION REGIMES; NUTRIENT DYNAMICS; NORTH-ATLANTIC; OCEAN; GROWTH; COAST; CHLOROPHYLL; RESPIRATION AB On a seasonal cycle, the phytoplankton biomass off the North West Cape region of Australia surrounding Ningaloo Reef increased during the austral autumn and peaked in winter. In this study, historical field data sets, satellite-derived ocean color observations and output from a data-assimilating numerical ocean model are used to investigate physical mechanisms that influence the seasonal variability in phytoplankton biomass off this coast. The mixed layer depth (MLD) off Ningaloo deepened to similar to 100 m in autumn, partly due to the acceleration of the Leeuwin Current, which induced an increase in nutrient concentrations and is the key mechanism responsible for the seasonal enhancement in chlorophyll a concentrations observed in the waters off Ningaloo Reef. By comparing the MLDs and the critical depth it is suggested that while average irradiance throughout the MLD was low, this had less impact on net growth than grazing. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Rousseaux, Cecile S. G.; Lowe, Ryan; Waite, Anya M.] Univ Western Australia, Oceans Inst, Crawley, WA 6009, Australia. [Rousseaux, Cecile S. G.; Waite, Anya M.] Univ Western Australia, Sch Environm Syst Engn, Crawley, WA 6009, Australia. [Lowe, Ryan] Univ Western Australia, Sch Earth & Environm, Crawley, WA 6009, Australia. [Feng, Ming] CSIRO Marine & Atmospher Res, Floreat, WA, Australia. [Thompson, Peter A.] CSIRO Marine & Atmospher Res, Hobart, Tas, Australia. RP Rousseaux, CSG (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA. EM cecile.s.rousseaux@nasa.gov RI Rousseaux, Cecile/E-8811-2012; Feng, Ming/F-5411-2010; Lowe, Ryan/A-5032-2012; Thompson, Peter/A-2361-2012; Waite, Anya/A-5492-2015 OI Rousseaux, Cecile/0000-0002-3022-2988; Feng, Ming/0000-0002-2855-7092; Lowe, Ryan/0000-0002-7080-8406; Thompson, Peter/0000-0002-9504-5433; Waite, Anya/0000-0003-2965-0296 FU CSIRO; Western Australian Marine Science Institute; Australian Research Council [DP0770094] FX Funding was provided by a CSIRO Wealth from Oceans grant, the Western Australian Marine Science Institute (Node 1 and 3) to CSGR and an Australian Research Council Discovery Grant # DP0770094 to RJL. We acknowledge the CSIRO Marine and Atmospheric Research for providing the nutrient, salinity and temperature data set. NR 57 TC 12 Z9 13 U1 0 U2 22 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0278-4343 EI 1873-6955 J9 CONT SHELF RES JI Cont. Shelf Res. PD JAN 1 PY 2012 VL 32 BP 22 EP 35 DI 10.1016/j.csr.2011.10.010 PG 14 WC Oceanography SC Oceanography GA 888DF UT WOS:000299983300002 ER PT J AU Herrmann, M Najjar, RG Neeley, AR Vila-Costa, M Dacey, JWH DiTullio, GR Kieber, DJ Kiene, RP Matrai, PA Simo, R Vernet, M AF Herrmann, Maria Najjar, Raymond G. Neeley, Aimee R. Vila-Costa, Maria Dacey, John W. H. DiTullio, Giacomo R. Kieber, David J. Kiene, Ronald P. Matrai, Patricia A. Simo, Rafel Vernet, Maria TI Diagnostic modeling of dimethylsulfide production in coastal water west of the Antarctic Peninsula SO CONTINENTAL SHELF RESEARCH LA English DT Article DE Dimethylsulfide; DMS; Dimethylsulfoniopropionate; DMSP; Antarctic Peninsula; Palmer Station ID DIMETHYLATED SULFUR-COMPOUNDS; DIMETHYLSULFONIOPROPIONATE DMSP; ATMOSPHERIC SULFUR; CONTINENTAL-SHELF; SOUTHERN-OCEAN; SARGASSO SEA; MARINE-ALGAE; ROSS SEA; SULFIDE; PHYTOPLANKTON AB The rate of gross biological dimethylsulfide (DMS) production at two coastal sites west of the Antarctic Peninsula, off Anvers Island, near Palmer Station, was estimated using a diagnostic approach that combined field measurements from 1 January 2006 through 1 March 2006 and a one-dimensional physical model of ocean mixing. The average DMS production rate in the upper water column (0-60 m) was estimated to be 3.1 +/- 0.6 nM d(-1) at station B (closer to shore) and 2.7 +/- 0.6 nM d(-1) at station E (further from shore). The estimated DMS replacement time was on the order of 1 d at both stations. DMS production was greater in the mixed layer than it was below the mixed layer. The average DMS production normalized to chlorophyll was 0.5 +/- 0.1 (nM d(-1))/(mg m(-3)) at station B and 0.7 +/- 0.2 (nM d(-1))/(mg m(-3)) at station E. When the diagnosed production rates were normalized to the observed concentrations of total dimethylsulfoniopropionate (DMSPt, the biogenic precursor of DMS), we found a remarkable similarity between our estimates at stations B and E (0.06 +/- 0.02 and 0.04 +/- 0.01 (nM DMS d(-1))/(nM DMSP), respectively) and the results obtained in a previous study from a contrasting biogeochemical environment in the North Atlantic subtropical gyre (0.047 +/- 0.006 and 0.087 +/- 0.014 (nM DMS d(-1))/(nM DMSP) in a cyclonic and anticyclonic eddy, respectively). We propose that gross biological DMS production normalized to DMSPt might be relatively independent of the biogeochemical environment, and place our average estimate at 0.06 +/- 0.01 (nM DMS d(-1))/(nM DMSPt). The significance of this finding is that it can provide a means to use DMSPt measurements to extrapolate gross biological DMS production, which is extremely difficult to measure experimentally under realistic in situ conditions. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Herrmann, Maria; Najjar, Raymond G.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Neeley, Aimee R.] NASA, Goddard Space Flight Ctr, Ocean Ecol Branch, Washington, DC USA. [Vila-Costa, Maria] Ctr Estudis Avancats Blanes CSIC, Grp Limnol, Dept Continental Ecol, Blanes, Catalunya, Spain. [Dacey, John W. H.] Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA. [DiTullio, Giacomo R.] Univ Charleston, Grice Marine Lab, Charleston, SC 29412 USA. [Kieber, David J.] SUNY Syracuse, Dept Chem, Coll Environm Sci & Forestry, Syracuse, NY USA. [Kiene, Ronald P.] Univ S Alabama, Dauphin Isl Sea Lab, Dauphin Isl, AL 36528 USA. [Matrai, Patricia A.] Bigelow Lab Ocean Sci, W Boothbay Harbor, ME 04575 USA. [Simo, Rafel] CSIC, Inst Ciencies Mar, E-08003 Barcelona, Spain. [Vernet, Maria] Univ Calif San Diego, Integrat Oceanog Div, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Herrmann, M (reprint author), Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA. EM mxh367@psu.edu; najjar@meteo.psu.edu; phytogirl79@comcast.net; mariavila@ceab.csic.es; jdacey@whoi.edu; ditullioj@cofc.edu; djkieber@esf.edu; rkiene@disl.org; pmatrai@bigelow.org; rsimo@icm.csic.es; mvernet@ucsd.edu RI Vila-Costa, Maria/L-4833-2014 OI Vila-Costa, Maria/0000-0003-1730-8418 FU National Science Foundation (NSF) Office of Polar Programs (OPP) [OPP-0083078]; NSF [OPP-0537827, OPP-0338147, OPP-0230028] FX We are grateful to the GOTM-developer team: Hans Burchard, Karsten Bolding, Lars Umlauf, and Hannes Rennau. We also deeply appreciate the logistical collaboration and support of the Palmer Station LTER and the resident teams at the time of the field campaign, with special thanks to K. McElroy and G.R. Westby. This research was supported by the National Science Foundation (NSF) Office of Polar Programs (OPP) under Grant OPP-0083078 to P.A. Matrai. Data from the Palmer LTER data archive were supported by NSF Grant OPP-0217282. Meteorological data were supported by NSF Grants OPP-0537827, OPP-0338147, and OPP-0230028. Surface solar radiation data were provided by the NSF UV Monitoring Network, operated by Biospherical Instruments Inc. under a contract from the NSF OPP via Raytheon Polar Services Company. NR 61 TC 6 Z9 6 U1 2 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0278-4343 J9 CONT SHELF RES JI Cont. Shelf Res. PD JAN 1 PY 2012 VL 32 BP 96 EP 109 DI 10.1016/j.csr.2011.10.017 PG 14 WC Oceanography SC Oceanography GA 888DF UT WOS:000299983300008 ER PT J AU Wang, ML Hada, M Huff, J Pluth, JM Anderson, J O'Neill, P Cucinotta, FA AF Wang, Minli Hada, Megumi Huff, Janice Pluth, Janice M. Anderson, Jennifer O'Neill, Peter Cucinotta, Francis A. TI Heavy Ions Can Enhance TGF beta Mediated Epithelial to Mesenchymal Transition SO JOURNAL OF RADIATION RESEARCH LA English DT Article DE Space radiation; Heavy ions; HZE nuclei; EMT; TGF beta ID GROWTH-FACTOR-BETA; SIGNALING PATHWAYS; CARCINOMA-CELLS; MAMMARY-GLAND; ACTIVATION; IRRADIATION; PROGRESSION; INHIBITION; EXPRESSION; TGF-BETA-1 AB TGF beta is a key modulator of the Epithelial Mesenchymal Transition (EMT), a process important in cancer progression and metastasis, which leads to the suppression of epithelial genes and expression of mesenchymal proteins. Ionizing radiation was found to specifically induce expression of the TGF-beta 1 isoform, which can modulate late post-radiation changes and increase the risk of tumor development and metastasis. Interactions between TGF beta induced EMT and DNA damage responses have not been fully elucidated, particularly at low doses and following different radiation quality exposures. Further characterization of the relationship between radiation quality, EMT and cancer development is warranted. We investigated whether space radiation induced TGF beta dependent EMT, using hTERT immortalized human esophageal epithelial cells (EPC2-hTERT) and non-transformed mink lung epithelial cells (Mv1Lu). We have observed morphologic and molecular alterations in EPC2 and Mv1Lu cells consistent with EMT after pre-treatment with TGF beta 1. This effect could be efficiently inhibited in both cell lines by the use of a TGF beta RI inhibitor. High-energy silicon or iron nuclei were each able to cause a mild induction of EMT, with the inclusion of TGF beta 1 inducing a greatly enhanced EMT phenotype even when cells were irradiated with doses as low as 0.1 Gy. A further enhancement of EMT was achieved at a higher dose of 2 Gy. TGF beta RI inhibitor was able to reverse the EMT induced by the combination of TGF beta 1 and radiation. These studies indicate that heavy ions, even at a low dose, may trigger the process of TGF beta 1-induced EMT, and suggest further studies are needed to determine whether the chronic exposures received in space may potentiate this process in astronauts, leading to an increased risk of cancer. C1 [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Wang, Minli; Hada, Megumi; Huff, Janice] USRA, Div Life Sci, Houston, TX 77058 USA. [Pluth, Janice M.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Anderson, Jennifer; O'Neill, Peter] Univ Oxford, Gray Inst Radiat Oncol & Biol, Oxford OX3 7DQ, England. RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM francis.a.cucinotta@nasa.gov FU DoE; NASA; Medical and Accelerator Departments at BNL FX This research is supported by DoE Low Dose Program and NASA Space Radiation Program. We are indebted to Medical and Accelerator Departments at BNL for support at NSRL. NR 27 TC 6 Z9 7 U1 0 U2 3 PU JAPAN RADIATION RESEARCH SOC PI CHIBA PA C/O NAT INST RADIOLOGICAL SCI 9-1 ANAGAWA-4-CHOME INAGE-KU, CHIBA, 263, JAPAN SN 0449-3060 J9 J RADIAT RES JI J. Radiat. Res. PD JAN PY 2012 VL 53 IS 1 BP 51 EP 57 DI 10.1269/jrr.11121 PG 7 WC Biology; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Radiology, Nuclear Medicine & Medical Imaging GA 890IV UT WOS:000300139200007 PM 22302045 ER PT J AU Steinfadt, JDR Bildsten, L Kaplan, DL Fulton, BJ Howell, SB Marsh, TR Ofek, EO Shporer, A AF Steinfadt, Justin D. R. Bildsten, Lars Kaplan, David L. Fulton, Benjamin J. Howell, Steve B. Marsh, T. R. Ofek, Eran O. Shporer, Avi TI A Search for Pulsations in Helium White Dwarfs SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID ZZ-CETI STARS; DIGITAL-SKY-SURVEY; COMMON-ENVELOPE BINARIES; HORIZONTAL-BRANCH STARS; MAIN-SEQUENCE BINARIES; ADIABATIC MASS-LOSS; RED GIANT BRANCH; INSTABILITY STRIP; ASTEROSEISMOLOGICAL CONSTRAINTS; PHOTOMETRIC-OBSERVATIONS AB The recent plethora of sky surveys, especially the Sloan Digital Sky Survey, have discovered many low-mass (M < 0.45 M-circle dot) white dwarfs that should have cores made of nearly pure helium. These WDs come in two varieties: those with masses 0.2 < M < 0.45 M-circle dot and H envelopes so thin that they rapidly cool and those with M < 0: 2 M. (often called extremely low mass [ELM] WDs) that have thick enough H envelopes to sustain 10(9) yr of H burning. In both cases, these WDs evolve through the ZZ Ceti instability strip, T-eff approximate to 9000-12; 000 K, where g-mode pulsations always occur in carbon/oxygen WDs. This expectation, plus theoretical work on the contrasts between C/O and He-core WDs, motivated our search for pulsations in 12 well-characterized helium WDs. We report here on our failure to find any pulsators among our sample. Though we have varying amplitude limits, it appears likely that the theoretical expectations regarding the onset of pulsations in these objects require closer consideration. We close by encouraging additional observations as new He WD samples become available, and we speculate on where theoretical work may be needed. C1 [Steinfadt, Justin D. R.; Bildsten, Lars; Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bildsten, Lars] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Kaplan, David L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53211 USA. [Fulton, Benjamin J.; Shporer, Avi] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA USA. [Marsh, T. R.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Ofek, Eran O.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Steinfadt, JDR (reprint author), Univ Calif Santa Barbara, Dept Phys, Broida Hall, Santa Barbara, CA 93106 USA. EM jdrsteinfadt@gmail.com; bildsten@kitp.ucsb.edu; kaplan@uwm.edu; bjfulton@lcogt.net; ashporer@lcogt.net FU National Science Foundation [PHY 05-51164, AST 07-07633, AST 11-09174]; NASA through Space Telescope Science Institute [01207.01-A, HST-GO-11581.01-A]; NASA [NAS 5-26555, NAS5-26555] FX We thank both referees for comments that improved our article. This work was supported by the National Science Foundation under grants PHY 05-51164, AST 07-07633, and AST 11-09174. D. L. K. was partially supported by NASA through Hubble Fellowship Grant 01207.01-A awarded by the Space Telescope Science Institute, which is operated by AURA, Inc., for NASA, under contract NAS 5-26555. This article uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope. Support for Program number HST-GO-11581.01-A was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. NR 82 TC 13 Z9 13 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JAN PY 2012 VL 124 IS 911 BP 1 EP 13 DI 10.1086/663865 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 888ZF UT WOS:000300042600001 ER PT J AU Woillez, J Akeson, R Colavita, M Eisner, J Millan-Gabet, R Monnier, J Pott, JU Ragland, S Wizinowich, P Abajian, M Appleby, E Berkey, B Cooper, A Felizardo, C Herstein, J Hrynevych, M Medeiros, D Morrison, D Panteleeva, T Smith, B Summers, K Tsubota, K Tyau, C Wetherell, E AF Woillez, J. Akeson, R. Colavita, M. Eisner, J. Millan-Gabet, R. Monnier, J. Pott, J. -U. Ragland, S. Wizinowich, P. Abajian, M. Appleby, E. Berkey, B. Cooper, A. Felizardo, C. Herstein, J. Hrynevych, M. Medeiros, D. Morrison, D. Panteleeva, T. Smith, B. Summers, K. Tsubota, K. Tyau, C. Wetherell, E. TI Self-Phase-Referenced Spectro-Interferometry on the Keck Interferometer SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID II-TELESCOPE; TAURI; VLTI; INSTRUMENT; ASTROMETRY; FINITO; PRIMA; AMBER; MODE; DISK AB As part of the astrometric and phase-referenced astronomy (ASTRA) project, three new science modes are being developed for the Keck Interferometer that extend the science capabilities of this instrument to include higher spectral resolution, fainter magnitudes, and astrometry. We report on the successful implementation of the first of these science modes, the self-phase-referencing mode, which provides a K-band (lambda = 2.2 mu m) spectral resolution of R similar to 1000 on targets as faint as 7.8 mag with spatial resolution as fine as lambda/B = 5 mas in the K band, with the 85 m interferometer baseline. This level of spectral resolution would not have been possible without a phase-referencing implementation extending the integration time limit imposed by atmospheric turbulence. For narrow spectral features, we demonstrate a precision of +/- 0: 01 on the differential V-2(lambda), and +/- 1.7 mrad on the differential phase Phi(lambda), equivalent to a differential astrometry precision of +/- 1.45 mu as. This new Keck Interferometer instrument is typically used to study the geometry and location of narrow spectral features at high angular resolution, referenced to a continuum. By simultaneously providing spectral and spatial information, the geometry of velocity fields (e. g., rotating disks, inflows, outflows, etc.) larger than 150 km s(-1) can also be explored. C1 [Woillez, J.; Ragland, S.; Wizinowich, P.; Appleby, E.; Berkey, B.; Cooper, A.; Hrynevych, M.; Medeiros, D.; Morrison, D.; Panteleeva, T.; Smith, B.; Summers, K.; Tsubota, K.; Tyau, C.; Wetherell, E.] WM Keck Observ, Kamuela, HI 96743 USA. [Akeson, R.; Millan-Gabet, R.; Abajian, M.; Felizardo, C.; Herstein, J.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Colavita, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Eisner, J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Monnier, J.] Univ Michigan, Ann Arbor, MI 48109 USA. [Pott, J. -U.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Woillez, J (reprint author), WM Keck Observ, 65-1120 Mamalahoa Highway, Kamuela, HI 96743 USA. FU W. M. Keck Foundation; National Science Foundation [AST-0619965]; National Aeronautics and Space Administration FX The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The Keck Interferometer is funded by the National Aeronautics and Space Administration. The ASTRA project was funded by the Major Research Instrumentation program of the National Science Foundation (grant AST-0619965). This work has made use of services produced by the NASA Exoplanet Science Institute at the California Institute of Technology. NR 37 TC 12 Z9 12 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JAN PY 2012 VL 124 IS 911 BP 51 EP 61 DI 10.1086/664075 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 888ZF UT WOS:000300042600006 ER PT J AU Ofek, EO Laher, R Law, N Surace, J Levitan, D Sesar, B Horesh, A Poznanski, D van Eyken, JC Kulkarni, SR Nugent, P Zolkower, J Walters, R Sullivan, M Agueros, M Bildsten, L Bloom, J Cenko, SB Gal-Yam, A Grillmair, C Helou, G Kasliwal, MM Quimby, R AF Ofek, E. O. Laher, R. Law, N. Surace, J. Levitan, D. Sesar, B. Horesh, A. Poznanski, D. van Eyken, J. C. Kulkarni, S. R. Nugent, P. Zolkower, J. Walters, R. Sullivan, M. Agueeros, M. Bildsten, L. Bloom, J. Cenko, S. B. Gal-Yam, A. Grillmair, C. Helou, G. Kasliwal, M. M. Quimby, R. TI The Palomar Transient Factory Photometric Calibration SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID DIGITAL SKY SURVEY; RESOLVED CCD PHOTOMETRY; STARS; ENSEMBLE; MAGNITUDES; EXTINCTION; CATALOG; OBJECTS; SYSTEM AB The Palomar Transient Factory (PTF) provides multiple epoch imaging for a large fraction of the celestial sphere. Here, we describe the photometric calibration of the PTF data products that allows the PTF magnitudes to be related to other magnitude systems. The calibration process utilizes Sloan Digital Sky Survey (SDSS) r similar to 16 mag point-source objects as photometric standards. During photometric conditions, this allows us to solve for the extinction coefficients and color terms and to estimate the camera illumination correction. This also enables the calibration of fields that are outside the SDSS footprint. We test the precision and repeatability of the PTF photometric calibration. Given that PTF is observing in a single filter each night, we define a PTF calibrated magnitude system for the R band and g band. We show that, in this system, approximate to 59% (47%) of the photometrically calibrated PTF R-band (g-band) data achieve a photometric precision of 0.02-0.04 mag and have color terms and extinction coefficients that are close to their average values. Given the objects' color, the PTF magnitude system can be converted to other systems. Moreover, a night-by-night comparison of the calibrated magnitudes of individual stars observed on multiple nights shows that they are consistent to a level of approximate to 0.02 mag. Most of the data that were taken under nonphotometric conditions can be calibrated relative to other epochs of the same sky footprint obtained during photometric conditions. We provide a concise guide describing how to use the PTF photometric-calibration data products, as well as the transformations between the PTF magnitude system and the SDSS and Johnson-Cousins systems. C1 [Ofek, E. O.; Levitan, D.; Sesar, B.; Horesh, A.; Kulkarni, S. R.; Kasliwal, M. M.; Quimby, R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Ofek, E. O.; Gal-Yam, A.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Laher, R.; Surace, J.; Grillmair, C.; Helou, G.] CALTECH, Jet Prop Lab, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Law, N.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Poznanski, D.; Nugent, P.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Poznanski, D.; Bloom, J.; Cenko, S. B.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [van Eyken, J. C.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Zolkower, J.; Walters, R.] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. [Sullivan, M.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Agueeros, M.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Bildsten, L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bildsten, L.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. RP Ofek, EO (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RI Agueros, Marcel/K-7998-2014; Horesh, Assaf/O-9873-2016; OI Agueros, Marcel/0000-0001-7077-3664; Horesh, Assaf/0000-0002-5936-1156; Sullivan, Mark/0000-0001-9053-4820 FU Einstein fellowship; NSF [AST-0507734, AST-0908886]; Gary and Cynthia Bengier; Richard and Rhoda Goldman Fund; NASA [NNX10AI21G, GO-7100028]; TABASGO Foundation FX We thank Andrew Pickles and an anonymous referee for useful comments on the article. This article 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. E. O. O. is supported by an Einstein fellowship and NASA grants. S. R. K. and his group are partially supported by the NSF grant AST-0507734. S. B. C. acknowledges generous financial assistance from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, NASA/Swift grants NNX10AI21G and GO-7100028, the TABASGO Foundation, and NSF grant AST-0908886. NR 30 TC 75 Z9 75 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JAN PY 2012 VL 124 IS 911 BP 62 EP 73 DI 10.1086/664065 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 888ZF UT WOS:000300042600007 ER PT J AU Rinella, DJ Wipfli, MS Stricker, CA Heintz, RA Rinella, MJ AF Rinella, Daniel J. Wipfli, Mark S. Stricker, Craig A. Heintz, Ron A. Rinella, Matthew J. TI Pacific salmon (Oncorhynchus spp.) runs and consumer fitness: growth and energy storage in stream-dwelling salmonids increase with salmon spawner density SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES LA English DT Article ID JUVENILE COHO SALMON; STABLE-ISOTOPE RATIOS; FRESH-WATER; FOOD WEBS; SOCKEYE-SALMON; SOUTHEASTERN ALASKA; RESIDENT SALMONIDS; MARINE SUBSIDIES; NUCLEIC-ACIDS; KISUTCH AB We examined how marine-derived nutrients (MDN), in the form of spawning Pacific salmon, influenced the nutritional status and delta N-15 of stream-dwelling fishes. We sampled juvenile coho salmon (Oncorhynchus kisutch) and Dolly Varden (Salvelinus malma) during spring and fall from 11 south-central Alaskan streams that ranged widely in spawning salmon biomass (0.1-4.7 kg.m(-2)). Growth rate (as indexed by RNA-DNA ratios), energy density, and delta N-15 enrichment in spring-sampled fishes increased with spawner biomass, indicating the persistence of spawner effects more than 6 months after salmon spawning. Point estimates suggest that spawner effects on nutrition were substantially greater for coho salmon than Dolly Varden (268% and 175% greater for growth and energy, respectively), indicating that both species benefitted physiologically, but that juvenile coho salmon accrued more benefits than Dolly Varden. Although the data were less conclusive for fall-than spring-sampled fish, they do suggest spawner effects were also generally positive during fall, soon after salmon spawned. In a follow-up analysis where growth rate and energy density were modeled as a function of delta N-15 enrichment, results suggested that both increased with MDN assimilation, especially in juvenile coho salmon. Our results support the importance of salmon runs to the nutritional ecology of stream-dwelling fishes. C1 [Rinella, Daniel J.] Univ Alaska Anchorage, Alaska Nat Heritage Program, Environm & Nat Resources Inst, Anchorage, AK 99508 USA. [Rinella, Daniel J.] Univ Alaska Fairbanks, Dept Biol & Wildlife, Alaska Cooperat Fish & Wildlife Res Unit, Fairbanks, AK 99775 USA. [Wipfli, Mark S.] Univ Alaska Fairbanks, Inst Arctic Biol, Alaska Cooperat Fish & Wildlife Res Unit, US Geol Survey, Fairbanks, AK 99775 USA. [Stricker, Craig A.] US Geol Survey, Ft Collins Sci Ctr, Denver Fed Ctr, Denver, CO 80225 USA. [Heintz, Ron A.] Auke Bay Labs, Natl Marine Fisheries Serv, Juneau, AK 99801 USA. [Rinella, Matthew J.] ARS, USDA, Miles City, MT 59301 USA. RP Rinella, DJ (reprint author), Univ Alaska Anchorage, Alaska Nat Heritage Program, Environm & Nat Resources Inst, 3211 Providence Dr,Beatrice McDonald Hall, Anchorage, AK 99508 USA. EM rinella@uaa.alaska.edu FU Exxon Valdez Oil Spill Trustees Council; University of Alaska Anchorage's Environment and Natural Resources Institute FX Thanks go to the Gulf Ecosystem Monitoring program (Exxon Valdez Oil Spill Trustees Council) for funding this project. Coowe Walker, Steve Baird, and Megan Murphy with the Kachemak Bay Research Reserve gave invaluable help in the field. Thanks also go to Ted Otis, David Westerman, Mike Booz, and Jeff Breakfield for help with Alaska Department of Fish and Game spawner counts and to Cayce Gulbransen for performing the isotope analyses. Advice from Hal Geiger and two anonymous reviewers greatly improved the manuscript. The US Forest Service Forest Health and the Kachemak Bay Research Reserve provided laboratory and bunkhouse space in Cooper Landing and Homer, respectively. Finally, thanks are extended to the University of Alaska Anchorage's Environment and Natural Resources Institute for supplemental funding during analysis and writing. The use of trade, product, or firm names in this publication is for descriptive purposes only and does not imply endorsement by the US Government. NR 64 TC 13 Z9 13 U1 0 U2 32 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0706-652X EI 1205-7533 J9 CAN J FISH AQUAT SCI JI Can. J. Fish. Aquat. Sci. PD JAN PY 2012 VL 69 IS 1 BP 73 EP 84 DI 10.1139/F2011-133 PG 12 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 885PE UT WOS:000299790400006 ER PT J AU Becker, M Meyssignac, B Letetrel, C Llovel, W Cazenave, A Delcroix, T AF Becker, M. Meyssignac, B. Letetrel, C. Llovel, W. Cazenave, A. Delcroix, T. TI Sea level variations at tropical Pacific islands since 1950 SO GLOBAL AND PLANETARY CHANGE LA English DT Article DE sea level rise; sea level variability; tide gauge; satellite altimetry; ENSO; Pacific Islands ID COORDINATE TIME-SERIES; EL-NINO; SATELLITE ALTIMETRY; GLOBAL OCEAN; TIDE GAUGES; CIRCULATION MODEL; RISE; VARIABILITY; IMPACT; GPS AB The western tropical Pacific is usually considered as one of the most vulnerable regions of the world under present-day and future global warming. It is often reported that some islands of the region already suffer significant sea level rise. To clarify the latter concern, in the present study we estimate sea level rise and variability since 1950 in the western tropical Pacific region (20 degrees S-15 degrees N; 120 degrees E-135 degrees W). We estimate the total rate of sea level change at selected individual islands, as a result of climate variability and change, plus vertical ground motion where available. For that purpose, we reconstruct a global sea level field from 1950 to 2009, combining long (over 1950-2009) good quality tide gauge records with 50-year-long (1958-2007) gridded sea surface heights from the Ocean General Circulation Model DRAKKAR. The results confirm that El Nino-Southern Oscillation (ENSO) events have a strong modulating effect on the interannual sea level variability of the western tropical Pacific, with lower/higher-than-average sea level during El Nino/La Nina events, of the order of +/- 20-30 cm. Besides this sub-decadal ENSO signature, sea level of the studied region also shows low-frequency (multi decadal) variability which superimposes to, thus in some areas amplifies current global mean sea level rise due to ocean warming and land ice loss. We use GPS precise positioning records whenever possible to estimate the vertical ground motion component that is locally superimposed to the climate-related sea level components. Superposition of global mean sea level rise, low-frequency regional variability and vertical ground motion shows that some islands of the region suffered significant 'total' sea level rise (i.e., that felt by the population) during the past 60 years. This is especially the case for the Funafuti Island (Tuvalu) where the "total" rate of rise is found to be about 3 times larger than the global mean sea level rise over 1950-2009. (C) 2011 Elsevier B.V. All rights reserved. C1 [Becker, M.; Meyssignac, B.; Cazenave, A.; Delcroix, T.] UMR5566 CNES CNRS UPS IRD, LEGOS, Toulouse, France. [Letetrel, C.] UMR6250 CNRS Univ La Rochelle, LIENSs, La Rochelle, France. [Llovel, W.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Becker, M (reprint author), 18 Av E Belin, F-31400 Toulouse, France. EM melanie.becker@legos.obs-mip.fr RI BECKER, Melanie/B-3658-2012; Meyssignac, Benoit/O-1910-2015; LLOVEL, William/G-6930-2016; Delcroix, Thierry/I-6103-2016 OI BECKER, Melanie/0000-0002-0263-5558; Delcroix, Thierry/0000-0002-8850-4865 FU ANR CNRS [ANR-09-CEP-001-01]; NASA FX We would like to thank two anonymous reviewers for very helpful comments that led to significant improvement of the manuscript. We also thank G. Woppelmann (LIENSs, CNRS) and F. Perosanz (DTP, CNES) for kindly helping us for the GPS section. The altimeter products were produced by SSALTO/DUACS and distributed by AVISO with support from CNES. M. Becker and C. Letetrel are supported by an ANR CNRS grant number ANR-09-CEP-001-01 (CECILE project). W. Llovel is supported by a NASA Postdoctorate fellowship. The SONEL data assembly center is also acknowledged for providing a comprehensive access to GPS data at tide gauges, and assistance for the latest ULR solution. NR 76 TC 81 Z9 83 U1 6 U2 69 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-8181 EI 1872-6364 J9 GLOBAL PLANET CHANGE JI Glob. Planet. Change PD JAN PY 2012 VL 80-81 BP 85 EP 98 DI 10.1016/j.gloplacha.2011.09.004 PG 14 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 883BC UT WOS:000299606600007 ER PT J AU Lissauer, JJ Barnes, JW Chambers, JE AF Lissauer, Jack J. Barnes, Jason W. Chambers, John E. TI Obliquity variations of a moonless Earth SO ICARUS LA English DT Article DE Astrobiology; Earth; Extrasolar planets; Rotational dynamics ID LONG-TERM EVOLUTION; INSOLATION QUANTITIES; SOLAR-SYSTEM; SPIN; ACCRETION; PLANETS; MARS AB We numerically explore the obliquity (axial tilt) variations of a hypothetical moonless Earth. Previous work has shown that the Earth's Moon stabilizes Earth's obliquity such that it remains within a narrow range, between 22.1 degrees and 24.5 degrees. Without lunar influence, a frequency map analysis by Laskar et al. (Laskar, J., Joutel, F., Robutel, P. [1993]. Nature 361, 615-617) showed that the obliquity could vary between 0 degrees and 85 degrees. This has left an impression in the astrobiology community that a big moon is necessary to maintain a habitable climate on an Earth-like planet. Using a modified version of the orbital integrator mercury, we calculate the obliquity evolution for moonless Earths with various initial conditions for up to 4 Gyr. We find that while obliquity varies significantly more than that of the actual Earth over 100,000 year timescales, the obliquity remains within a constrained range, typically 20-25 degrees in extent, for timescales of hundreds of millions of years. None of our Solar System integrations in which planetary orbits behave in a typical manner show obliquity accessing more than 65% of the full range allowed by frequency-map analysis. The obliquities of moonless Earths that rotate in the retrograde direction are more stable than those of prograde rotators. The total obliquity range explored for moonless Earths with rotation periods less than 12 h is much less than that for slower-rotating moonless Earths. A large moon thus does not seem to be needed to stabilize the obliquity of an Earth-like planet on timescales relevant to the development of advanced life. (C) 2011 Elsevier Inc. All rights reserved. C1 [Barnes, Jason W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA. [Lissauer, Jack J.; Barnes, Jason W.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Chambers, John E.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. RP Barnes, JW (reprint author), Univ Idaho, Dept Phys, Campus Box 440903, Moscow, ID 83844 USA. EM jack.j.lissauer@nasa.gov; jwbarnes@uidaho.edu RI Barnes, Jason/B-1284-2009 OI Barnes, Jason/0000-0002-7755-3530 FU NASA [RTOP 344-30-50-01] FX The initial portions of this work were funded by NASA's Exobiology program. Support for the completion of this study was provided by the NASA Origins of Solar Systems Program (J.E.C.) and by NASA's Planetary Geology and Geophysics Program through RTOP 344-30-50-01 (J.J.L.). J.W.B. acknowledges the support of the NASA Postdoctoral Program, administered for NASA by Oak Ridge Associated Universities, and the NASA Exobiology program. The authors thank Tony Dobrovolskis and Elisa Quintana for careful reviews and useful manuscript comments. NR 22 TC 21 Z9 21 U1 2 U2 26 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JAN PY 2012 VL 217 IS 1 BP 77 EP 87 DI 10.1016/j.icarus.2011.10.013 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 876TP UT WOS:000299130900007 ER PT J AU Le Gall, A Hayes, AG Ewing, R Janssen, MA Radebaugh, J Savage, C Encrenaz, P AF Le Gall, A. Hayes, A. G. Ewing, R. Janssen, M. A. Radebaugh, J. Savage, C. Encrenaz, P. CA Cassini Radar Team TI Latitudinal and altitudinal controls of Titan's dune field morphometry SO ICARUS LA English DT Article DE Titan; Radar observations; Radio observations; Geological processes ID CASSINI RADAR; SURFACE; DESERT; WINDS AB Dune fields dominate similar to 13% of Titan's surface and represent an important sink of carbon in the methane cycle. Herein, we discuss correlations in dune morphometry with altitude and latitude. These correlations, which have important implications in terms of geological processes and climate on Titan, are investigated through the microwave electromagnetic signatures of dune fields using Cassini radar and radiometry observations. The backscatter and emissivity from Titan's dune terrains are primarily controlled by the amount of interdune area within the radar footprint and are also expected to vary with the degree of the interdunal sand cover. Using SAR-derived topography, we find that Titan's main June fields (Shangri-La, Fensal, Belet and Aztlan) tend to occupy the lowest elevation areas in Equatorial regions occurring at mean elevations between similar to-400 and similar to 0 m (relative to the geoid). In elevated,June terrains, we show a definite trend towards a smaller dune to interdune ratio and possibly a thinner sand cover in the interdune areas. A similar correlation is observed with latitude, suggesting that the quantity of windblown sand in the dune fields tends to decrease as one moves farther north. The altitudinal trend among Titan's sand seas is consistent with the idea that sediment source zones most probably occur in lowlands, which would reduce the sand supply toward elevated regions. The latitudinal preference could result from a gradual increase in dampness with latitude due to the asymmetric seasonal forcing associated with Titan's current orbital configuration unless it is indicative of a latitudinal preference in the sand source distribution or wind transport capacity. (C) 2011 Elsevier Inc. All rights reserved. C1 [Le Gall, A.] Observ Spatiales LATMOS UVSQ, Atmospheres Lab, Paris, France. [Le Gall, A.; Janssen, M. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hayes, A. G.; Ewing, R.] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. [Radebaugh, J.; Savage, C.] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. RP Le Gall, A (reprint author), Observ Spatiales LATMOS UVSQ, Atmospheres Lab, Paris, France. EM alice.legall@latmos.ipsl.fr RI Hayes, Alexander/P-2024-2014 OI Hayes, Alexander/0000-0001-6397-2630 FU Cassini/Huygens mission; NASA; European Space Agency (ESA); Italian Space Agency (ASI) FX This work was supported by the Cassini/Huygens mission, which is a joint endeavor of NASA, the European Space Agency (ESA), and the Italian Space Agency (ASI) and is managed by JPL/Caltech under a contract with NASA. A. Le Gall is supported by the NASA Postdoctoral Program, administrated by Oak Ridge Associated Universities (ORAU). The authors are grateful to Don Jennings for sharing his CIRS measurements of the latitudinal ground temperature distribution. They also wish to thank Oded Aharonson for providing essential facilities for this work and Lori Fenton for her thoughtful comments that greatly help improving this Manuscript. NR 46 TC 17 Z9 17 U1 2 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD JAN PY 2012 VL 217 IS 1 BP 231 EP 242 DI 10.1016/j.icarus.2011.10.024 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 876TP UT WOS:000299130900019 ER PT J AU Stubbs, TJ Wang, YL AF Stubbs, Timothy J. Wang, Yongli TI Illumination conditions at the Asteroid 4 Vesta: Implications for the presence of water ice SO ICARUS LA English DT Article DE Asteroid Vesta; Asteroids, Surfaces; Ices; Solar radiation; Thermal histories ID CERES AB The mean illumination conditions and surface temperatures over one orbital period are calculated for the Asteroid 4 Vesta using a coarse digital elevation model produced from Hubble Space Telescope images. Even with the anticipated effects of finer-scale topography taken into account, it is unlikely that any significant permanently shadowed regions currently exist on Vesta due to its large axial tilt (approximate to 27 degrees). However, under present day conditions, it is predicted that about half of Vesta's surface has an average temperature of less than 145 K, which, based on previous thermal modeling of main belt asteroids, suggests that water ice could survive in the top few meters of the vestal regolith on billion-year timescales. (C) 2011 Elsevier Inc. All rights reserved. C1 [Stubbs, Timothy J.; Wang, Yongli] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stubbs, Timothy J.] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA. [Wang, Yongli] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA. [Stubbs, Timothy J.; Wang, Yongli] NASA, Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA 94035 USA. RP Stubbs, TJ (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 695, Greenbelt, MD 20771 USA. EM Timothy.J.Stubbs@NASA.gov; Yongli.Wang@NASA.gov RI Stubbs, Timothy/I-5139-2013 OI Stubbs, Timothy/0000-0002-5524-645X FU NASA [NNX08AM76G, NNX09AG78A] FX The development of the illumination code, and its application to Vesta, were funded by NASA Grants NNX08AM76G and NNX09AG78A, respectively. The NASA Planetary Data System (PDS) facilitated access to the 4 Vesta DEM used in this investigation. NR 16 TC 5 Z9 5 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD JAN PY 2012 VL 217 IS 1 BP 272 EP 276 DI 10.1016/j.icarus.2011.11.007 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 876TP UT WOS:000299130900022 ER PT J AU El Maarry, MR Dohm, JM Marzo, GA Fergason, R Goetz, W Heggy, E Pack, A Markiewicz, WJ AF El Maarry, M. Ramy Dohm, James M. Marzo, Giuseppe A. Fergason, Robin Goetz, Walter Heggy, Essam Pack, Andreas Markiewicz, Wojciech J. TI Searching for evidence of hydrothermal activity at Apollinaris Mons, Mars SO ICARUS LA English DT Article DE Mars, Surface; Volcanism; Geological processes ID LAYERED EJECTA CRATERS; MARTIAN IMPACT CRATERS; EASTERN HELLAS REGION; SLOPE STREAKS; NEW-ZEALAND; TECTONIC ACTIVITY; RAY SPECTROMETER; FLUVIAL VALLEYS; RAMPART CRATERS; NORTHERN PLAINS AB A multidisciplinary approach involving various remote sensing instruments is used to investigate Apollinaris Mons, a prominent volcano on Mars, as well as the surrounding plains for signs of prolonged hydrologic and volcanic, and possibly hydrothermal activity. The main findings include (1) evidence from laser altimetry indicating the large thickness (1.5-2 km at some locations) of the fan deposits draping the southern flank contrary to previous estimates, coupled with possible layering which point to a significant emplacement phase at Apollinaris Mons, (2) corroboration of Robinson et al. (Robinson, M.S., Mouginis-Mark, P.J., Zimbelman, J.R., Wu, S.S.C., Ablin, K.K., Howington-Kraus, A.E. [1993]. Icarus 104, 301-323) hypothesis regarding the formation of incised valleys on the western flanks by density current erosion which would indicate magma-water interaction or, alternatively, volatile-rich magmas early in the volcano's history, (3) mounds of diverse geometric shapes, many of which display summit depressions and occur among faults and fractures, possibly marking venting, (4) strong indicators on the flanks of the volcano for lahar events, and possibly, a caldera lake, (5) ubiquitous presence of impact craters displaying fluidized ejecta in both shield-forming (flank and caldera) materials and materials that surround the volcano that are indicative of water-rich target materials at the time of impact, (6) long-term complex association in time among shield-forming materials and Medusae Fossae Formation. The findings point to a site of extensive volcanic and hydrologic activity with possibly a period of magma-water interaction and hydrothermal activity. Finally, we propose that the mound structures around Apollinaris should be prime targets for further in situ exploration and search for possible exobiological signatures. (C) 2011 Elsevier Inc. All rights reserved. C1 [El Maarry, M. Ramy; Goetz, Walter; Markiewicz, Wojciech J.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [El Maarry, M. Ramy; Pack, Andreas] Univ Gottingen, Geowissensch Zentrum, D-37077 Gottingen, Germany. [Dohm, James M.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Marzo, Giuseppe A.] CR Casaccia, ENEA, I-00123 Rome, Italy. [Fergason, Robin] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Heggy, Essam] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP El Maarry, MR (reprint author), Univ Bern, Inst Phys, Sidler Str 5, CH-3012 Bern, Switzerland. EM mohamed.elmaarry@space.unibe.ch RI Heggy, Essam/E-8250-2013; Dohm, James/A-3831-2014; Marzo, Giuseppe/A-9765-2015; OI Heggy, Essam/0000-0001-7476-2735; EL-MAARRY, MOHAMED RAMY/0000-0002-8262-0320 FU MPG-IMPRS; NASA FX M.R. El Maarry was supported by an MPG-IMPRS Grant. James M. Dohm was funded through NASA's Mars Data Analysis Program. The first author would like to thank Johan Verkamp for his clarifications on the nature and evolution of volcanic lakes on Earth, and Roberto Bugiolacchi for his valuable comments. We would also like to thank two anonymous reviewers for their critical comments and suggestions that greatly improved this paper. NR 161 TC 5 Z9 5 U1 3 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 JAN PY 2012 VL 217 IS 1 BP 297 EP 314 DI 10.1016/j.icarus.2011.10.022 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 876TP UT WOS:000299130900024 ER PT J AU Cloutis, EA Hudon, P Hiroi, T Gaffey, MJ AF Cloutis, E. A. Hudon, P. Hiroi, T. Gaffey, M. J. TI Spectral reflectance properties of carbonaceous chondrites: 3. CR chondrites SO ICARUS LA English DT Article DE Asteroids; Meteorites; Mineralogy; Spectroscopy ID AQUEOUS ALTERATION; THERMAL METAMORPHISM; REFRACTORY INCLUSIONS; ISOTOPIC COMPOSITIONS; METEORITE SPECTRA; ANOMALOUS PHASES; SILICATE GRAINS; CM CHONDRITES; II CHONDRULES; IRON-OXIDES AB Powdered samples of a suite of 14 CR and CR-like chondrites, ranging from petrologic grade 1 to 3, were spectrally characterized over the 0.3-2.5 mu m interval as part of a larger study of carbonaceous chondrite reflectance spectra. Spectral analysis was complicated by absorption bands due to Fe oxyhydroxides near 0.9 mu m, resulting from terrestrial weathering. This absorption feature masks expected absorption bands due to constituent silicates in this region. In spite of this interference, most of the CR spectra Exhibit absorption bands attributable to silicates, in particular an absorption feature due to Fe2+-bearing phyllosilicates near 1.1 mu m. Mafic silicate absorption bands are weak to nonexistent due to a number of factors, including low Fe content, low degree of silicate crystallinity in some cases, and presence of fine-grained, finely dispersed opaques. With increasing aqueous alteration, phyllosilicate: mafic silicate ratios increase, resulting in more resolvable phyllosilicate absorption bands in the 1.1 mu m region. the most phyllosilicate-rich CR chondrite, GRO 95577 (CR1), an additional possible phyllosilicate absorption band is seen at 2.38 mu m. In contrast to CM spectra, CR spectra generally do not exhibit an absorption band in the 0.65-0.7 mu m region, which is attributable to Fe3+-Fe2+ charge transfers, suggesting that CR phyllosilicates are not as Fe3+-rich as CM phyllosilicates. CR2 and CR3 spectra are uniformly red-sloped, likely due to the presence of abundant Fe-Ni metal. Absolute reflectance seems to decrease with increasing degree of aqueous alteration, perhaps due to the formation of fine-grained opaques from pre-existing metal. Overall, CR spectra are characterized by widely varying reflectance (4-21% maximum reflectance), weak silicate absorption bands in the 0.9-1.3 mu m region, overall red slopes, and the lack of an Fe3+-Fe2+ charge transfer absorption band in the 0.65-0.7 mu m region. (C) 2011 Elsevier Inc. All rights reserved. C1 [Cloutis, E. A.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada. [Hudon, P.] NASA Johnson Space Ctr, Astromat Res & Explorat Sci Off, Houston, TX 77058 USA. [Hiroi, T.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Gaffey, M. J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. RP Cloutis, EA (reprint author), Univ Winnipeg, Dept Geog, 515 Portage Ave, Winnipeg, MB R3B 2E9, Canada. EM e.cloutis@uwinnipeg.ca; pierre.hudon@mcgill.ca; takahiro_hiroi@brown.edu; gaffey@space.edu FU NASA [NNG06GJ31G] FX We wish to thank the invaluable and generous assistance provided by many individuals which made this study possible. We particularly thank Dr. Jeffrey Post of the Smithsonian Institution National Museum of Natural History and Dr. Linda Reinen of Pomona College for providing a number of the mineral samples used in this study, Mr. Neil Ball and Dr. Frank Hawthorne of the University of Manitoba for acquisition of XRD data for the mineral samples, and Dr. Stanley Mertzman for XRF analysis of the mineral samples. The establishment and operation of the Planetary Spectrophotometer Facility (PSF) at the University of Winnipeg was made possible through the assistance of the Canada Foundation for Innovation, the Manitoba Research Innovations Fund, the Canadian Space Agency, the Natural Sciences and Engineering Research Council of Canada (NSERC), and the University of Winnipeg. The RELAB facility at Brown University is a multi-user facility operated with support from NASA Planetary Geology and Geophysics grant NNG06GJ31G, whose support is gratefully acknowledged. We also wish to thank the National Science Foundation, the NASA Meteorite Working Group, and the Japanese National Institute of Polar Research for their efforts in collecting, classifying and distributing Antarctic meteorites to the scientific community. We thank Josep Trigo-Rodriguez and an anonymous reviewer for their many useful suggestions on revising and improving the manuscript. NR 112 TC 23 Z9 23 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 J9 ICARUS JI Icarus PD JAN PY 2012 VL 217 IS 1 BP 389 EP 407 DI 10.1016/j.icarus.2011.11.004 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 876TP UT WOS:000299130900030 ER PT J AU Catauro, PM Perchonok, MH AF Catauro, Patricia M. Perchonok, Michele H. TI Assessment of the Long-Term Stability of Retort Pouch Foods to Support Extended Duration Spaceflight SO JOURNAL OF FOOD SCIENCE LA English DT Article DE NASA food system; retort pouch; shelf life; thermal processing ID SHELF-LIFE; STORAGE; PRODUCTS; QUALITY; EGGS AB To determine the suitability of retort processed foods to support long-duration spaceflight, a series of 36-mo accelerated shelf life studies were performed on 13 representative retort pouch products. Combined sensory evaluations, physical properties assessments, and nutritional analyses were employed to determine shelf life endpoints for these foods, which were either observed during the analysis or extrapolated via mathematical projection. Data obtained through analysis of these 13 products were later used to estimate the shelf life values of all retort-processed spaceflight foods. In general, the major determinants of shelf life appear to be the development of off-flavor and off-color in products over time. These changes were assumed to be the result of Maillard and oxidation reactions, which can be initiated or accelerated as a result of the retort process and product formulation. Meat products and other vegetable entrees are projected to maintain their quality the longest, between 2 and 8 y, without refrigeration. Fruit and dessert products (1.5 to 5 y), dairy products (2.5 to 3.25 y), and starches, vegetable, and soup products (1 to 4 y) follow. Aside from considerable losses in B and C vitamin content, nutritional value of most products was maintained throughout shelf life. Fortification of storage-labile vitamins was proposed as a countermeasure to ensure long-term nutritive value of these products. The use of nonthermal sterilization technologies was also recommended, as a means to improve initial quality of these products and extend their shelf life for use in long-duration missions. Data obtained also emphasize the importance of low temperature storage in maintaining product quality. C1 [Perchonok, Michele H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Catauro, Patricia M.] Lockheed Martin Informat Syst & Global Solut, Houston, TX 77058 USA. RP Perchonok, MH (reprint author), NASA, Lyndon B Johnson Space Ctr, Mailcode SF3,2101 NASA Pkwy, Houston, TX 77058 USA. EM michele.h.perchonok@nasa.gov FU Space Food Systems Laboratory (SFSL) team FX This multiyear research effort has been accomplished only through the support of many contributing NASA and contractor teams. We would like to express our appreciation for the direction of the NASA Human Research Program (HRP), the support of the Space Food Systems Laboratory (SFSL) team, the participation of the Johnson Space Center (JSC) Sensory Evaluation Center panelists, and the contributions of the HRP Advanced Food Technology (AFT) researchers who directed this study. NR 30 TC 4 Z9 4 U1 4 U2 21 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1147 J9 J FOOD SCI JI J. Food Sci. PD JAN PY 2012 VL 77 IS 1 BP S29 EP S39 DI 10.1111/j.1750-3841.2011.02445.x PG 11 WC Food Science & Technology SC Food Science & Technology GA 878KX UT WOS:000299257000041 PM 22260129 ER PT J AU Daryabeigi, K Knutson, JR Cunnington, GR AF Daryabeigi, Kamran Knutson, Jeffrey R. Cunnington, George R. TI Reducing Thermal Contact Resistance for Rigid-Insulation Thermal Measurements SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER LA English DT Article; Proceedings Paper CT 49th AIAA Aerospace Sciences Meeting/New Horizons Forum and Aerospace Exposition CY JAN 03-07, 2011 CL Orlando, FL SP AIAA ID RADIATIVE HEAT-TRANSFER; FIBROUS INSULATIONS C1 [Daryabeigi, Kamran] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA. [Cunnington, George R.] Cunnington & Associates, Palo Alto, CA 94303 USA. [Knutson, Jeffrey R.] NASA, Langley Res Ctr, Syst Integrat & Test Branch, Hampton, VA 23681 USA. RP Daryabeigi, K (reprint author), NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Mail Stop 190, Hampton, VA 23681 USA. NR 17 TC 1 Z9 1 U1 0 U2 2 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0887-8722 J9 J THERMOPHYS HEAT TR JI J. Thermophys. Heat Transf. PD JAN-MAR PY 2012 VL 26 IS 1 BP 172 EP 175 DI 10.2514/1.T3788 PG 4 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA 885FS UT WOS:000299764500018 ER PT J AU Han, JW Meyyappan, M AF Han, Jin-Woo Meyyappan, M. TI Determination of crystal orientation of silicon via shape-controlled vapor-solid growth of copper nanoparticles SO JOURNAL OF VACUUM SCIENCE & TECHNOLOGY B LA English DT Article ID DEPENDENCE; LAYERS; GOLD; TEM AB Crystal lattice orientations of substrates are inspected via morphology of copper particles generated by a vapor-solid growth process. The high thermal energy enables diffusion of copper ions into the crystal substrate, and then the copper ions on the substrate are preferentially gathered, forming single-crystalline metal particles. The shapes of the particles are bounded by the facets to minimize the surface energy. Thus, polyhedral particles are truncated and bounded by {100}, {110}, and {111} facets, which results in equilateral square and triangle shapes on (100) and (111) plane substrates, respectively. The directions of the sides of the square and triangle shapes indicate < 100 > and < 110 > directions, respectively. (C) 2012 American Vacuum Society. [DOI: 10.1116/1.3672007] C1 [Han, Jin-Woo; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Han, JW (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. EM jin-woo.han@nasa.gov NR 15 TC 0 Z9 0 U1 0 U2 7 PU A V S AMER INST PHYSICS PI MELVILLE PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA SN 1071-1023 J9 J VAC SCI TECHNOL B JI J. Vac. Sci. Technol. B PD JAN PY 2012 VL 30 IS 1 AR 010604 DI 10.1116/1.3672007 PG 4 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Physics, Applied SC Engineering; Science & Technology - Other Topics; Physics GA 880ES UT WOS:000299388200004 ER PT J AU Smith, AJ Wang, L Oliver, SJ Auld, R Bock, J Brisbin, D Burgarella, D Chanial, P Chapin, E Clements, DL Conversi, L Cooray, A Dowell, CD Eales, S Farrah, D Franceschini, A Glenn, J Griffin, M Ivison, RJ Mortier, AMJ Page, MJ Papageorgiou, A Pearson, CP Perez-Fournon, I Pohlen, M Rawlings, JI Raymond, G Rodighiero, G Roseboom, IG Rowan-Robinson, M Savage, R Scott, D Seymour, N Symeonidis, M Tugwell, KE Vaccari, M Valtchanov, I Vigroux, L Ward, R Wright, G Zemcov, M AF Smith, A. J. Wang, L. Oliver, S. J. Auld, R. Bock, J. Brisbin, D. Burgarella, D. Chanial, P. Chapin, E. Clements, D. L. Conversi, L. Cooray, A. Dowell, C. D. Eales, S. Farrah, D. Franceschini, A. Glenn, J. Griffin, M. Ivison, R. J. Mortier, A. M. J. Page, M. J. Papageorgiou, A. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Rawlings, J. I. Raymond, G. Rodighiero, G. Roseboom, I. G. Rowan-Robinson, M. Savage, R. Scott, Douglas Seymour, N. Symeonidis, M. Tugwell, K. E. Vaccari, M. Valtchanov, I. Vigroux, L. Ward, R. Wright, G. Zemcov, M. TI HerMES: point source catalogues from deep Herschel-SPIRE observations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; catalogues; galaxies: photometry; submillimetre: galaxies ID SOURCE EXTRACTION; NUMBER COUNTS; MU-M; INSTRUMENT AB We describe the generation of single-band point source catalogues from submillimetre Herschel-SPIRE observations taken as part of the Science Demonstration Phase of the Herschel Multi-tiered Extragalactic Survey (HerMES). Flux densities are found by means of peak finding and the fitting of a Gaussian point-response function. With highly confused images, careful checks must be made on the completeness and flux-density accuracy of the detected sources. This is done by injecting artificial sources into the images and analysing the resulting catalogues. Measured flux densities at which 50 per cent of injected sources result in good detections at (250, 350 and 500) mu m range from (11.6, 13.2 and 13.1) to (25.7, 27.1 and 35.8) mJy, depending on the depth of the observation (where a good detection is taken to be one with positional offset less than one full-width half-maximum of the point-response function, and with the measured flux density within a factor of 2 of the flux density of the injected source). This paper acts as a reference for the 2010 July HerMES public data release. C1 [Smith, A. J.; Wang, L.; Oliver, S. J.; Farrah, D.; Roseboom, I. G.; Savage, R.; Ward, R.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Auld, R.; Eales, S.; Griffin, M.; Papageorgiou, A.; Pohlen, M.; Raymond, G.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Bock, J.; Cooray, A.; Dowell, C. D.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Dowell, C. D.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brisbin, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Burgarella, D.] Univ Aix Marseille, CNRS, Lab Astrophys Marseille, OAMP, F-13388 Marseille 13, France. [Chanial, P.] Univ Paris Diderot, Lab AIM Paris Saclay, CE Saclay, CEA,DSM,Irfu,CNRS, F-91191 Gif Sur Yvette, France. [Chapin, E.; Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Clements, D. L.; Mortier, A. M. J.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Conversi, L.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Franceschini, A.; Rodighiero, G.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA. [Ivison, R. J.; Wright, G.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.; Roseboom, I. G.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Pearson, C. P.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Perez-Fournon, I.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Savage, R.] Univ Warwick, Warwick Syst Biol Ctr, Coventry CV4 7AL, W Midlands, England. [Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Vigroux, L.] UPMC Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Page, M. J.; Rawlings, J. I.; Seymour, N.; Symeonidis, M.; Tugwell, K. E.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Smith, AJ (reprint author), Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. EM A.J.Smith@Sussex.ac.uk RI Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; OI Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Scott, Douglas/0000-0002-6878-9840; Seymour, Nicholas/0000-0003-3506-5536; Rodighiero, Giulia/0000-0002-9415-2296 FU Science and Technology Facilities Council [ST/F002858/1, ST/I000976/1] FX We acknowledge support from the Science and Technology Facilities Council (grant numbers ST/F002858/1 and ST/I000976/1. NR 17 TC 52 Z9 52 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2012 VL 419 IS 1 BP 377 EP 389 DI 10.1111/j.1365-2966.2011.19709.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 865HZ UT WOS:000298303300048 ER PT J AU Ukwatta, TN Dhuga, KS Stamatikos, M Dermer, CD Sakamoto, T Sonbas, E Parke, WC Maximon, LC Linnemann, JT Bhat, PN Eskandarian, A Gehrels, N Abeysekara, AU Tollefson, K Norris, JP AF Ukwatta, T. N. Dhuga, K. S. Stamatikos, M. Dermer, C. D. Sakamoto, T. Sonbas, E. Parke, W. C. Maximon, L. C. Linnemann, J. T. Bhat, P. N. Eskandarian, A. Gehrels, N. Abeysekara, A. U. Tollefson, K. Norris, J. P. TI The lag-luminosity relation in the GRB source frame: an investigation with Swift BAT bursts SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-ray burst: general ID GAMMA-RAY BURST; SPECTRAL LAGS; PEAK LUMINOSITY; RESOLUTION SPECTROSCOPY; HOST GALAXY; ENERGY; PULSES; ENVIRONMENT; CONNECTION; EVOLUTION AB Spectral lag, which is defined as the difference in time of arrival of high- and low-energy photons, is a common feature in gamma-ray bursts (GRBs). Previous investigations have shown a correlation between this lag and the isotropic peak luminosity for long duration bursts. However, most of the previous investigations used lags extracted in the observer frame only. In this work (based on a sample of 43 Swift long GRBs with known redshifts), we present an analysis of the lagluminosity relation in the GRB source frame. Our analysis indicates a higher degree of correlation -0.82 +/- 0.05 (chance probability of similar to 5.5 x 10(-5)) between the spectral lag and the isotropic peak luminosity, L-iso, with a best-fitting power-law index of -1.2 +/- 0.2, such that L-iso proportional to lag(-1.2). In addition, there is an anticorrelation between the source-frame spectral lag and the source-frame peak energy of the burst spectrum, E-pk(1 + z). C1 [Ukwatta, T. N.; Linnemann, J. T.; Abeysekara, A. U.; Tollefson, K.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Ukwatta, T. N.; Stamatikos, M.; Sakamoto, T.; Sonbas, E.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dhuga, K. S.; Parke, W. C.; Maximon, L. C.; Eskandarian, A.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Stamatikos, M.] Ohio State Univ, Dept Phys, CCAPP, Columbus, OH 43210 USA. [Dermer, C. D.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Sakamoto, T.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Sonbas, E.] Univ Adiyaman, Dept Phys, TR-02040 Adiyaman, Turkey. [Sonbas, E.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Bhat, P. N.] Univ Alabama, Ctr Space Plasma & Aeronom Res, Huntsville, AL 35805 USA. [Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. RP Ukwatta, TN (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM tilan.ukwatta@gmail.com RI Gehrels, Neil/D-2971-2012 FU NSF [1002432]; Office of Naval Research; Fermi Guest Investigator grants; GRB Temporal Analysis Consortium (GTAC) FX We thank the anonymous referee for comments that significantly improved the paper. The NSF grant 1002432 provided partial support for the work of TNU and is gratefully acknowledged. The work of CDD is supported by the Office of Naval Research and Fermi Guest Investigator grants. We acknowledge that this work has been performed via th eauspices of the GRB Temporal Analysis Consortium (GTAC), which represents a comprehensive effort dedicated towards the systematic study of spectral variation in Gamma-ray Bursts. NR 78 TC 19 Z9 19 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2012 VL 419 IS 1 BP 614 EP 623 DI 10.1111/j.1365-2966.2011.19723.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 865HZ UT WOS:000298303300065 ER PT J AU Harker, GJA Pritchard, JR Burns, JO Bowman, JD AF Harker, Geraint J. A. Pritchard, Jonathan R. Burns, Jack O. Bowman, Judd D. TI An MCMC approach to extracting the global 21-cm signal during the cosmic dawn from sky-averaged radio observations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; cosmology: theory; diffuse radiation; radio lines: general ID BRIGHTNESS TEMPERATURE; DECAMETER WAVELENGTHS; INTERGALACTIC MEDIUM; REIONIZATION EPOCH; HIGH-REDSHIFT; BLACK-HOLES; LY-ALPHA; HYDROGEN; UNIVERSE; PROSPECTS AB Efforts are being made to observe the 21-cm signal from the cosmic dawn using sky-averaged observations with individual radio dipoles. In this paper, we develop a model of the observations accounting for the 21-cm signal, foregrounds and several major instrumental effects. Given this model, we apply Markov Chain Monte Carlo techniques to demonstrate the ability of these instruments to separate the 21-cm signal from foregrounds and quantify their ability to constrain properties of the first galaxies. For concreteness, we investigate observations between 40 and 120 MHz with the proposed Dark Ages Radio Explorer mission in lunar orbit, showing its potential for science return. C1 [Harker, Geraint J. A.; Burns, Jack O.] Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Harker, Geraint J. A.; Burns, Jack O.] NASA Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA 94035 USA. [Pritchard, Jonathan R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowman, Judd D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Harker, GJA (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Campus Box 391, Boulder, CO 80309 USA. EM geraint.harker@colorado.edu RI Harker, Geraint/C-4885-2012; OI Harker, Geraint/0000-0002-7894-4082; Pritchard, Jonathan/0000-0003-4127-5353 FU NASA Lunar Science Institute [NNA09DB30A] FX We thank Stuart Bale for providing an estimate of the noise caused by exospheric dust impacts on the antenna and the spacecraft. We also acknowledge the work of the DARE team in designing the mission, including Joseph Lazio, Rich Bradley, Chris Carilli, Steve Furlanetto, Avi Loeb, Larry Webster, Jill Bauman and Ian O'Dwyer. The authors are members of the LUNAR consortium (http://lunar.colorado.edu), headquartered at the University of Colorado, which is funded by the NASA Lunar Science Institute (via Cooperative Agreement NNA09DB30A) to investigate concepts for astrophysical observatories on the Moon. NR 47 TC 23 Z9 23 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2012 VL 419 IS 2 BP 1070 EP 1084 DI 10.1111/j.1365-2966.2011.19766.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867VG UT WOS:000298482300013 ER PT J AU Petrov, L AF Petrov, Leonid TI The EVN Galactic Plane Survey - EGaPS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: interferometers; catalogues; surveys; astrometry ID VLBA CALIBRATOR SURVEY; CELESTIAL REFERENCE FRAME; EXTRAGALACTIC RADIO-SOURCES; BASE-LINE INTERFEROMETRY; ALL-SKY SURVEY; BESSEL SURVEY; ASTROMETRY; CANDIDATE; POSITIONS; ALIGNMENT AB I present a catalogue of the positions and correlated flux densities of 109 compact extragalactic radio sources in the Galactic plane determined from an analysis of a 48-h Very Long Baseline Interferometry (VLBI) experiment at 22 GHz with the European VLBI Network. The median position uncertainty is 9 mas. The correlated flux densities of the detected sources are in the range of 20300 mJy. In addition to the target sources, nine water masers have been detected, of which two are new. I derived the positions of the masers with an accuracy of 30200 mas and determined the velocities of the maser components and their correlated flux densities. The catalogue and the supporting material are available at http://astrogeo.org/egaps. C1 ADNET Syst Inc, NASA GSFC, Greenbelt, MD 20771 USA. RP Petrov, L (reprint author), ADNET Syst Inc, NASA GSFC, Code 610-2, Greenbelt, MD 20771 USA. EM Leonid.Petrov@lpetrov.net FU MERRA atmospheric re-analysis project; national research councils; University of California, Los Angeles; Jet Propulsion Laboratory/California Institute of Technology; NASA FX I made use of the data base CATS of the Special Astrophysical Observatory. I used in our work the data set MAI6NPANA provided by the NASA/Global Modelling and Assimilation Office (GMAO) in the framework of the MERRA atmospheric re-analysis project. The European VLBI Network is a joint facility of European, Chinese, South African, Russian and other radio-astronomy institutes funded by their national research councils. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by NASA. NR 39 TC 5 Z9 5 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2012 VL 419 IS 2 BP 1097 EP 1106 DI 10.1111/j.1365-2966.2011.19765.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867VG UT WOS:000298482300015 ER PT J AU Roediger, E ZuHone, JA AF Roediger, E. ZuHone, J. A. TI Fast simulations of gas sloshing and cold front formation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: clusters: general; galaxies: clusters: individual: A2029; X-rays: galaxies: clusters ID GALAXY CLUSTERS; CHANDRA OBSERVATION; INTERGALACTIC MEDIUM; CENTAURUS CLUSTER; PERSEUS CLUSTER; 2A 0335+096; XMM-NEWTON; CORE; TEMPERATURE; BUBBLES AB We present a simplified and fast method for simulating minor mergers between galaxy clusters. Instead of following the evolution of the dark matter haloes directly by the N-body method, we employ a rigid potential approximation for both clusters. The simulations are run in the rest frame of the more massive cluster and account for the resulting inertial accelerations in an optimized way. We test the reliability of this method for studies of minor merger induced gas sloshing by performing a one-to-one comparison between our simulations and hydro+N-body ones. We find that the rigid potential approximation reproduces the sloshing-related features well except for two artefacts: the temperature just outside the cold fronts is slightly overpredicted, and the outward motion of the cold fronts is delayed by typically 200 Myr. We discuss reasons for both artefacts. C1 [Roediger, E.] Univ Bremen, D-28725 Bremen, Germany. [ZuHone, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Roediger, E (reprint author), Univ Bremen, POB 750 561, D-28725 Bremen, Germany. EM e.roediger@jacobs-university.de FU DFG (German Research Foundation); John-Neumann Institut at the Forschungszentrum Julich [NIC 3711, 4368]; NASA; DOE ASC/Alliances FX ER is supported by the Priority Programme 'Witnesses of Cosmic History' of the DFG (German Research Foundation) and the supercomputing grants NIC 3711 and 4368 at the John-Neumann Institut at the Forschungszentrum Julich. JAZ is supported under the NASA postdoctoral program. We thank Marcus Bruggen for helpful discussions, and the referee Max Ruffert for his clarifying comments. The results presented were produced using the FLASH code, a product of the DOE ASC/Alliances-funded Center for Astrophysical Thermonuclear Flashes at the University of Chicago. NR 29 TC 15 Z9 15 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2012 VL 419 IS 2 BP 1338 EP 1349 DI 10.1111/j.1365-2966.2011.19794.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867VG UT WOS:000298482300035 ER PT J AU Grunhut, JH Rivinius, T Wade, GA Townsend, RHD Marcolino, WLF Bohlender, DA Szeifert, T Petit, V Matthews, JM Rowe, JF Moffat, AFJ Kallinger, T Kuschnig, R Guenther, DB Rucinski, SM Sasselov, D Weiss, WW AF Grunhut, J. H. Rivinius, Th. Wade, G. A. Townsend, R. H. D. Marcolino, W. L. F. Bohlender, D. A. Szeifert, Th. Petit, V. Matthews, J. M. Rowe, J. F. Moffat, A. F. J. Kallinger, T. Kuschnig, R. Guenther, D. B. Rucinski, S. M. Sasselov, D. Weiss, W. W. CA MiMeS Collaboration TI HR 5907: Discovery of the most rapidly rotating magnetic early B-type star by the MiMeS Collaboration SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; techniques: polarimetric; stars: circumstellar matter; stars: individual HR 5907; stars: magnetic field; stars: rotation ID HELIUM-STRONG STARS; DRIVEN STELLAR WINDS; CONTROLLED CIRCUMSTELLAR MATTER; DYNAMICAL SIMULATIONS; MASS-LOSS; ORI-E; LINE; FIELD; EMISSION; EXTINCTION AB We report the discovery and analysis of a very strong magnetic field in the rapidly rotating early B-type star HR 5907, based on observations obtained as part of the Magnetism in Massive Stars (MiMeS) project. We infer a rotation period of 0.508 276+0.000 015-0.000 012 d from photometric and Ha EW measurements, making this the shortest period, non-degenerate, magnetic massive star known to date. From the comparison of IUE UV and optical spectroscopy with LTE bruce/kylie models we find a solid-angle integrated, uniform black-body temperature of 17 000 +/- 1000 K, a projected rotational velocity of 290 +/- 10 km s-1, an equatorial radius of 3.1 +/- 0.2 R circle dot, a stellar mass of 5.5 +/- 0.5 M circle dot, and an inclination angle of the rotation axis to our line-of-sight of 70 +/- 10 degrees. Our measurements of the longitudinal magnetic field, which vary between -500 and -2000 G, phase coherently with the rotation period and imply a surface dipole field strength of similar to 15.7 kG. On the other hand, from fits to mean Least-Squares Deconvolved Stokes V line profiles we infer a dipole field strength of similar to 10.4 kG. This disagreement may result from a magnetic configuration more complex than our model, and/or from the non-uniform helium surface abundance distribution. In either case we obtain a magnetic obliquity nearly aligned with the rotation axis (beta=7-1+2 degrees). Our optical spectroscopy also shows weak variability in carbon, silicon and nitrogen lines. The emission variability in hydrogen Balmer and Paschen lines indicates the presence of a dense, highly structured magnetosphere, interpreted as a centrifugally supported, magnetically confined circumstellar disc. C1 [Grunhut, J. H.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada. [Grunhut, J. H.; Wade, G. A.] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada. [Rivinius, Th.; Szeifert, Th.] ESO European Org Astron Res So Hemisphere, Santiago 19, Chile. [Townsend, R. H. D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Marcolino, W. L. F.] Univ Fed Rio de Janeiro, Observatorio Valongo Ladeira Pedro Antonio, BR-20080 Rio De Janeiro, Brazil. [Bohlender, D. A.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Petit, V.] W Chester Univ, Dept Geol & Astron, W Chester, PA 19383 USA. [Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Rowe, J. F.; Kallinger, T.; Kuschnig, R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Kallinger, T.; Kuschnig, R.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Guenther, D. B.; Weiss, W. W.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada. [Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Grunhut, JH (reprint author), Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada. EM Jason.Grunhut@rmc.ca RI 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; Marcolino, Wagner/M-7428-2014; OI Kallinger, Thomas/0000-0003-3627-2561 FU Natural Sciences and Engineering Research Council of Canada (NSERC); NSF [AST-0904607, AST-0908688]; CFHT; TBL; ESO FX JHG acknowledges financial support in the form of an Alexander Graham Bell Canada Graduate Scholarship from the Natural Sciences and Engineering Research Council of Canada (NSERC). GAW, JMM, AFJM, DBG and SMR acknowledge support from NSERC. RHDT acknowledges support from NSF grants AST-0904607 and AST-0908688. The authors thank Dr Stefano Bagnulo for his guidance in the reduction of FORS data, Dr John Landstreet for helpful discussion and Phil Landry for assistance in the period analysis. The 'Magnetism in Massive Stars' (MiMeS) project is supported by the CFHT, TBL and ESO (through the allocation of telescope time). We thank the CFHT/QSO and ESO operations staff for their efficiency at collecting data for this challenging target. NR 51 TC 23 Z9 23 U1 0 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2012 VL 419 IS 2 BP 1610 EP 1627 DI 10.1111/j.1365-2966.2011.19824.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867VG UT WOS:000298482300060 ER PT J AU Bendo, GJ Boselli, A Dariush, A Pohlen, M Roussel, H Sauvage, M Smith, MWL Wilson, CD Baes, M Cooray, A Clements, DL Cortese, L Foyle, K Galametz, M Gomez, HL Lebouteiller, V Lu, N Madden, SC Mentuch, E O'Halloran, B Page, MJ Remy, A Schulz, B Spinoglio, L AF Bendo, G. J. Boselli, A. Dariush, A. Pohlen, M. Roussel, H. Sauvage, M. Smith, M. W. L. Wilson, C. D. Baes, M. Cooray, A. Clements, D. L. Cortese, L. Foyle, K. Galametz, M. Gomez, H. L. Lebouteiller, V. Lu, N. Madden, S. C. Mentuch, E. O'Halloran, B. Page, M. J. Remy, A. Schulz, B. Spinoglio, L. TI Investigations of dust heating in M81, M83 and NGC 2403 with the Herschel Space Observatory SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: individual: M81; galaxies: individual: M83; galaxies: individual: NGC 2403; galaxies: ISM; galaxies: spiral; infrared: galaxies ID FAR-INFRARED LUMINOSITY; 160 MU-M; MULTIBAND IMAGING PHOTOMETER; FORMATION RATE INDICATORS; NEARBY GALAXIES SURVEY; STAR-FORMING GALAXIES; H-II REGIONS; SPIRAL GALAXIES; MOLECULAR GAS; M33 HERM33ES AB We use Spitzer Space Telescope and Herschel Space Observatory far-infrared data along with ground-based optical and near-infrared data to understand how dust heating in the nearby face-on spiral galaxies M81, M83 and NGC 2403 is affected by the starlight from all stars and by the radiation from star-forming regions. We find that 70/160 m surface brightness ratios tend to be more strongly influenced by star-forming regions. However, the 250/350 m and 350/500 m surface brightness ratios are more strongly affected by the light from the total stellar populations, suggesting that the dust emission at >250 m originates predominantly from a component that is colder than the dust seen at <160 m and that is relatively unaffected by star formation activity. We conclude by discussing the implications of this for modelling the spectral energy distributions of both nearby and more distant galaxies and for using far-infrared dust emission to trace star formation. C1 [Bendo, G. J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys,UK ALMA Reg Ctr Node, Manchester M13 9PL, Lancs, England. [Bendo, G. J.; Dariush, A.; Clements, D. L.; O'Halloran, B.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Boselli, A.] CNRS, UMR6110, Lab Astrophys Marseille, F-13388 Marseille, France. [Dariush, A.; Pohlen, M.; Smith, M. W. L.; Gomez, H. L.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Dariush, A.] Inst Res Fundamental Sci IPM, Sch Astron, Tehran, Iran. [Roussel, H.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Sauvage, M.; Lebouteiller, V.; Madden, S. C.; Remy, A.] Univ Paris Diderot, CEA, IRFU, Serv Astrophys,Lab AIM, F-91191 Gif Sur Yvette, France. [Wilson, C. D.; Foyle, K.; Mentuch, E.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Baes, M.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Cortese, L.] European So Observ, D-85748 Garching, Germany. [Galametz, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Lu, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lu, N.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Schulz, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Spinoglio, L.] INAF, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. RP Bendo, GJ (reprint author), Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys,UK ALMA Reg Ctr Node, Oxford Rd, Manchester M13 9PL, Lancs, England. EM george.bendo@manchester.ac.uk RI Baes, Maarten/I-6985-2013; OI Baes, Maarten/0000-0002-3930-2757; Lebouteiller, Vianney/0000-0002-7716-6223; Spinoglio, Luigi/0000-0001-8840-1551; Cortese, Luca/0000-0002-7422-9823 FU STFC; Canadian Space Agency; Natural Sciences and Engineering Research Council of Canada; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA); National Aeronautics and Space Administration FX GJB thanks Simone Bianchi and the reviewer for helpful comments on this paper. GJB was funded by the STFC. The research of CDW and KF is supported by grants to CDW from the Canadian Space Agency and the Natural Sciences and Engineering Research Council of Canada. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA (USA). HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. This research has made use of the NED which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 96 TC 85 Z9 85 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2012 VL 419 IS 3 BP 1833 EP 1859 DI 10.1111/j.1365-2966.2011.19735.x PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872XI UT WOS:000298844300002 ER PT J AU Miglio, A Brogaard, K Stello, D Chaplin, WJ D'Antona, F Montalban, J Basu, S Bressan, A Grundahl, F Pinsonneault, M Serenelli, AM Elsworth, Y Hekker, S Kallinger, T Mosser, B Ventura, P Bonanno, A Noels, A Aguirre, VS Szabo, R Li, J McCauliff, S Middour, CK Kjeldsen, H AF Miglio, A. Brogaard, K. Stello, D. Chaplin, W. J. D'Antona, F. Montalban, J. Basu, S. Bressan, A. Grundahl, F. Pinsonneault, M. Serenelli, A. M. Elsworth, Y. Hekker, S. Kallinger, T. Mosser, B. Ventura, P. Bonanno, A. Noels, A. Aguirre, V. Silva Szabo, R. Li, J. McCauliff, S. Middour, C. K. Kjeldsen, H. TI Asteroseismology of old open clusters with Kepler: direct estimate of the integrated red giant branch mass-loss in NGC 6791 and 6819 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE asteroseismology; stars: late-type; stars: mass-loss; open clusters and associations: individual: NGC 6791; open clusters and associations: individual: NGC 6819 ID COLOR-MAGNITUDE DIAGRAMS; DWARF COOLING SEQUENCE; SOLAR-LIKE OSCILLATIONS; GLOBULAR-CLUSTERS; DUST PRODUCTION; WHITE-DWARFS; MAIN-SEQUENCE; STELLAR EVOLUTION; SPACE-TELESCOPE; EVOLVED STARS AB Mass-loss of red giant branch (RGB) stars is still poorly determined, despite its crucial role in the chemical enrichment of galaxies. Thanks to the recent detection of solar-like oscillations in GK giants in open clusters with Kepler, we can now directly determine stellar masses for a statistically significant sample of stars in the old open clusters NGC 6791 and 6819. The aim of this work is to constrain the integrated RGB mass-loss by comparing the average mass of stars in the red clump (RC) with that of stars in the low-luminosity portion of the RGB [i.e. stars with L less than or similar to L(RC)]. Stellar masses were determined by combining the available seismic parameters v(max) and Delta v with additional photometric constraints and with independent distance estimates. We measured the masses of 40 stars on the RGB and 19 in the RC of the old metal-rich cluster NGC 6791. We find that the difference between the average mass of RGB and RC stars is small, but significant [Delta(M) over bar = 0.009 +/- 0.03 (random) +/- 0.04 (systematic)M-circle dot]. Interestingly, such a small Delta(M) over bar does not support scenarios of an extreme mass-loss for this metal-rich cluster. If we describe the mass-loss rate with Reimers prescription, a first comparison with isochrones suggests that the observed Delta(M) over bar is compatible with a mass-loss efficiency parameter in the range 0.1 less than or similar to eta less than or similar to 0.3. Less stringent constraints on the RGB mass-loss rate are set by the analysis of the similar to 2 Gyr old NGC 6819, largely due to the lower mass-loss expected for this cluster, and to the lack of an independent and accurate distance determination. In the near future, additional constraints from frequencies of individual pulsation modes and spectroscopic effective temperatures will allow further stringent tests of the Delta v and v(max) scaling relations, which provide a novel, and potentially very accurate, means of determining stellar radii and masses. C1 [Miglio, A.; Chaplin, W. J.; Elsworth, Y.; Hekker, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Brogaard, K.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Stello, D.] Univ Sydney, Sch Phys, SIfA, Sydney, NSW 2006, Australia. [D'Antona, F.; Ventura, P.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. [Montalban, J.; Noels, A.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Basu, S.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Bressan, A.] SISSA, I-34136 Trieste, Italy. [Bressan, A.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Grundahl, F.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Pinsonneault, M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Serenelli, A. M.] Fac Ciencies, CSIC IEEC, Inst Space Sci, Bellaterra 08193, Spain. [Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Kallinger, T.] Univ British Colombia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Mosser, B.] Univ Paris 07, Univ Paris 06, CNRS, Observ Paris,LESIA, F-92195 Meudon, France. [Bonanno, A.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Aguirre, V. Silva] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Szabo, R.] Hungarian Acad Sci, Konkoly Observ Budapest, H-1121 Budapest, Hungary. [Li, J.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [McCauliff, S.; Middour, C. K.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. RP Miglio, A (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. EM miglioa@bison.ph.bham.ac.uk RI Basu, Sarbani/B-8015-2014; OI Basu, Sarbani/0000-0002-6163-3472; D'Antona, Francesca/0000-0003-4697-0945; Ventura, Paolo/0000-0002-5026-6400; Kallinger, Thomas/0000-0003-3627-2561; Bonanno, Alfio/0000-0003-3175-9776; Brogaard, Karsten/0000-0003-2001-0276; Szabo, Robert/0000-0002-3258-1909; Serenelli, Aldo/0000-0001-6359-2769 FU NASA's Science Mission Directorate; School of Physics and Astronomy, University of Birmingham; Carlsberg Foundation; Australian Research Council; UK STFC; European Union [PIRG-GA-2009-247732]; MICINN [AYA08-1839/ESP]; ESF EUROCORES (MICINN) [EUI2009-04170]; SGR of the Generalitat de Catalunya; Netherlands Organization for Scientific Research (NWO); Hungarian OTKA [K83790, MB08C 81013]; Janos Bolyai Research Scholarship; European Community [269194]; Hungarian Academy of Sciences FX The authors acknowledge the Kepler Science Team and all those who have contributed to making the Kepler mission possible. Funding for the Kepler Discovery mission is provided by NASA's Science Mission Directorate. AM acknowledges the support of the School of Physics and Astronomy, University of Birmingham. KB acknowledges financial support from the Carlsberg Foundation. DS acknowledges support from the Australian Research Council. WJC and YE acknowledge support from the UK STFC. AMS is supported by the European Union International Reintegration Grant PIRG-GA-2009-247732, the MICINN grant AYA08-1839/ESP, by the ESF EUROCORES Programme EuroGENESIS (MICINN grant EUI2009-04170), by SGR grants of the Generalitat de Catalunya and by the EU-FEDER funds. SH acknowledges financial support from the Netherlands Organization for Scientific Research (NWO). This project has been supported by the 'Lendulet' program of the Hungarian Academy of Sciences and the Hungarian OTKA grants K83790 and MB08C 81013. RS thanks the support of the Janos Bolyai Research Scholarship. The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 269194. NR 87 TC 122 Z9 122 U1 0 U2 7 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2012 VL 419 IS 3 BP 2077 EP 2088 DI 10.1111/j.1365-2966.2011.19859.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872XI UT WOS:000298844300018 ER PT J AU Berge, J Price, S Amara, A Rhodes, J AF Berge, Joel Price, Sedona Amara, Adam Rhodes, Jason TI On point spread function modelling: towards optimal interpolation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; methods: data analysis; methods: statistical ID COSMIC SHEAR; WEAK; SYSTEMATICS; SOFTWARE AB Point spread function (PSF) modelling is a central part of any astronomy data analysis relying on measuring the shapes of objects. It is especially crucial for weak gravitational lensing, in order to beat down systematics and allow one to reach the full potential of weak lensing in measuring dark energy. A PSF modelling pipeline is made of two main steps: the first one is to assess its shape on stars, and the second is to interpolate it at any desired position (usually galaxies). We focus on the second part, and compare different interpolation schemes, including polynomial interpolation, radial basis functions, Delaunay triangulation and Kriging. For that purpose, we develop simulations of PSF fields, in which stars are built from a set of basis functions defined from a principal components analysis of a real ground-based image. We find that Kriging gives the most reliable interpolation, significantly better than the traditionally used polynomial interpolation. We also note that although a Kriging interpolation on individual images is enough to control systematics at the level necessary for current weak lensing surveys, more elaborate techniques will have to be developed to reach future ambitious surveys requirements. C1 [Berge, Joel; Amara, Adam] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Berge, Joel; Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Berge, Joel; Price, Sedona; Rhodes, Jason] CALTECH, Pasadena, CA 91125 USA. RP Berge, J (reprint author), ETH, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. EM jberge@phys.ethz.ch OI Price, Sedona/0000-0002-0108-4176 FU HST [AR-11747]; Caltech Summer Undergraduate Research Fellowship (SURF); Jet Propulsion Laboratory, California Institute of Technology under NASA FX We want to thank Barney Rowe and Alexandre Refregier for useful discussions. We thank Satoshi Miyazaki for providing us with Subaru weak lensing images. We also thank Richard Massey for his comments on the manuscript, as well as the anonymous referee for their useful comments. JB acknowledges support from HST grant AR-11747. SP acknowledges support from the Caltech Summer Undergraduate Research Fellowship (SURF) programme, through the Elachi endowment and internal JPL research funding. Part of this work was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 25 TC 15 Z9 15 U1 0 U2 4 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2012 VL 419 IS 3 BP 2356 EP 2368 DI 10.1111/j.1365-2966.2011.19888.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872XI UT WOS:000298844300040 ER PT J AU Rowlands, K Dunne, L Maddox, S Bourne, N Gomez, HL Kaviraj, S Bamford, SP Brough, S Charlot, S da Cunha, E Driver, SP Eales, SA Hopkins, AM Kelvin, L Nichol, RC Sansom, AE Sharp, R Smith, DJB Temi, P van der Werf, P Baes, M Cava, A Cooray, A Croom, SM Dariush, A De Zotti, G Dye, S Fritz, J Hopwood, R Ibar, E Ivison, RJ Liske, J Loveday, J Madore, B Norberg, P Popescu, CC Rigby, EE Robotham, A Rodighiero, G Seibert, M Tuffs, RJ AF Rowlands, K. Dunne, L. Maddox, S. Bourne, N. Gomez, H. L. Kaviraj, S. Bamford, S. P. Brough, S. Charlot, S. da Cunha, E. Driver, S. P. Eales, S. A. Hopkins, A. M. Kelvin, L. Nichol, R. C. Sansom, A. E. Sharp, R. Smith, D. J. B. Temi, P. van der Werf, P. Baes, M. Cava, A. Cooray, A. Croom, S. M. Dariush, A. De Zotti, G. Dye, S. Fritz, J. Hopwood, R. Ibar, E. Ivison, R. J. Liske, J. Loveday, J. Madore, B. Norberg, P. Popescu, C. C. Rigby, E. E. Robotham, A. Rodighiero, G. Seibert, M. Tuffs, R. J. TI Herschel-ATLAS/GAMA: dusty early-type galaxies and passive spirals SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE dust; extinction; galaxies: elliptical and lenticular; cD; galaxies: evolution; infrared: galaxies; submillimetre: galaxies ID DIGITAL-SKY-SURVEY; RECENT STAR-FORMATION; MASS ASSEMBLY GAMA; SCIENCE DEMONSTRATION PHASE; NEARBY ELLIPTIC GALAXIES; ACTIVE GALACTIC NUCLEI; LOW-REDSHIFT GALAXIES; X-RAY-EMISSION; RED-SEQUENCE; STELLAR MASS AB We present the dust properties and star formation histories of local submillimetre-selected galaxies, classified by optical morphology. Most of the galaxies are late types and very few are early types. The early-type galaxies (ETGs) that are detected contain as much dust as typical spirals, and form a unique sample that has been blindly selected at submillimetre wavelengths. Additionally, we investigate the properties of the most passive, dusty spirals. We morphologically classify 1087 galaxies detected in the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS) Science Demonstration Phase data. Comparing to a control sample of optically selected galaxies, we find 5.5 per cent of luminous ETGs are detected in H-ATLAS. The H-ATLAS ETGs contain a significant mass of cold dust: the mean dust mass is 5.5 x 10(7)M(circle dot), with individual galaxies ranging from 9 x 10(5) to 4 x 10(8)M(circle dot). This is comparable to that of spiral galaxies in our sample, and is an order of magnitude more dust than that found for the control early-types, which have a median dust mass inferred from stacking of (0.8-4.0) x 10(6)M(circle dot) for a cold dust temperature of 25-15 K. The early-types detected in H-ATLAS tend to have bluer NUV - r colours, higher specific star formation rates and younger stellar populations than early-types which are optically selected, and may be transitioning from the blue cloud to the red sequence. We also find that H-ATLAS and control early-types inhabit similar low-density environments. We investigate whether the observed dust in H-ATLAS early-types is from evolved stars, or has been acquired from external sources through interactions and mergers. We conclude that the dust in H-ATLAS and control ETGs cannot be solely from stellar sources, and a large contribution from dust formed in the interstellar medium or external sources is required. Alternatively, dust destruction may not be as efficient as predicted. We also explore the properties of the most passive spiral galaxies in our sample with specific star formation rate (SSFR) < 10(-11) yr(-1). We find these passive spirals have lower dust-to-stellar mass ratios, higher stellar masses and older stellar population ages than normal spirals. The passive spirals inhabit low-density environments similar to those of the normal spiral galaxies in our sample. This shows that the processes which turn spirals passive do not occur solely in the intermediate-density environments of group and cluster outskirts. C1 [Rowlands, K.; Dunne, L.; Maddox, S.; Bourne, N.; Bamford, S. P.; Smith, D. J. B.; Dye, S.; Rigby, E. E.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Gomez, H. L.; Eales, S. A.; Dye, S.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Kaviraj, S.; Dariush, A.; Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. [Brough, S.; Hopkins, A. M.] Australian Astron Observ, Epping, NSW 1710, Australia. [Charlot, S.] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. [da Cunha, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Driver, S. P.; Kelvin, L.; Robotham, A.] Univ Western Australia, Int Ctr Radio Astron ICRAR, Crawley, WA 6009, Australia. [Driver, S. P.; Kelvin, L.] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Nichol, R. C.] ICG, Portsmouth PO1 3FX, Hants, England. [Sansom, A. E.; Popescu, C. C.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Sharp, R.] Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Smith, D. J. B.] Univ Hertfordshire, Ctr Astrophys, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. [Temi, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [van der Werf, P.] Leiden Univ, NL-2300 RA Leiden, Netherlands. [Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Croom, S. M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [De Zotti, G.; Rodighiero, G.] Univ Padua, Dept Astron, INAF, Vicolo Osservatorio, I-35122 Padua, Italy. [De Zotti, G.] SISSA, I-34136 Trieste, Italy. [Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.; Norberg, P.; Rigby, E. E.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Liske, J.] European So Observ, D-85748 Garching, Germany. [Loveday, J.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Madore, B.; Seibert, M.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Tuffs, R. J.] Max Planck Inst Nucl Phys MPIK, D-69117 Heidelberg, Germany. RP Rowlands, K (reprint author), Univ Nottingham, Sch Phys & Astron, Univ Pk Campus, Nottingham NG7 2RD, England. EM ppxkr@nottingham.ac.uk RI Baes, Maarten/I-6985-2013; Robotham, Aaron/H-5733-2014; Driver, Simon/H-9115-2014; Ivison, R./G-4450-2011; Bamford, Steven/E-8702-2010; Cava, Antonio/C-5274-2017; OI Dye, Simon/0000-0002-1318-8343; Smith, Daniel/0000-0001-9708-253X; Rodighiero, Giulia/0000-0002-9415-2296; da Cunha, Elisabete/0000-0001-9759-4797; Liske, Jochen/0000-0001-7542-2927; Maddox, Stephen/0000-0001-5549-195X; Baes, Maarten/0000-0002-3930-2757; Robotham, Aaron/0000-0003-0429-3579; Driver, Simon/0000-0001-9491-7327; Ivison, R./0000-0001-5118-1313; Bamford, Steven/0000-0001-7821-7195; Cava, Antonio/0000-0002-4821-1275; De Zotti, Gianfranco/0000-0003-2868-2595 FU STFC (UK); ARC (Australia); AAO; ASI/INAF [I/009/10/0] FX GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the SDSS and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KIDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing UV-to-radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO and the participating institutions. The GAMA website is http://www.gama-survey.org/. The Italian group acknowledges partial financial support from ASI/INAF agreement n. I/009/10/0. NR 145 TC 56 Z9 57 U1 1 U2 9 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2012 VL 419 IS 3 BP 2545 EP 2578 DI 10.1111/j.1365-2966.2011.19905.x PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872XI UT WOS:000298844300055 ER PT J AU Romano, P Mangano, V Ducci, L Esposito, P Evans, PA Vercellone, S Kennea, JA Burrows, DN Gehrels, N AF Romano, P. Mangano, V. Ducci, L. Esposito, P. Evans, P. A. Vercellone, S. Kennea, J. A. Burrows, D. N. Gehrels, N. TI Swift/X-ray Telescope monitoring of the candidate supergiant fast X-ray transient IGR J16418-4532 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE X-rays: binaries; X-rays: individual: IGR J16418-4532 ID XMM-NEWTON; MULTIWAVELENGTH OBSERVATIONS; INTEGRAL OBSERVATIONS; COMPANION STAR; BINARY-SYSTEMS; XTE J1739-302; NEUTRON-STAR; O-STARS; MASS; WINDS AB We report on the Swift monitoring of the candidate supergiant fast X-ray transient (SFXT) IGR J16418-4532, for which both orbital and spin periods are known (similar to 3.7 d and similar to 1250 s, respectively). Our observations, for a total of similar to 43 ks, span over three orbital periods and represent the most intense and complete sampling of the light curve of this source with a sensitive X-ray instrument. With this unique set of observations, we can address the nature of this transient. By applying the clumpy wind model for blue supergiants to the observed X-ray light curve, and assuming a circular orbit, the X-ray emission from this source can be explained in terms of the accretion from a spherically symmetric clumpy wind, composed of clumps with different masses, ranging from similar to 5 x 10(16) to 10(21) g. Our data suggest, based on the X-ray behaviour, that this is an intermediate SFXT. C1 [Romano, P.; Mangano, V.; Vercellone, S.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-90146 Palermo, Italy. [Ducci, L.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Esposito, P.] Osserv Astrofis Catania, INAF, I-09012 Capoterra, Italy. [Evans, P. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Kennea, J. A.; Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Romano, P (reprint author), INAF, Ist Astrofis Spaziale & Fis Cosm, Via U La Malfa 153, I-90146 Palermo, Italy. EM romano@ifc.inaf.it RI Gehrels, Neil/D-2971-2012; OI Vercellone, Stefano/0000-0003-1163-1396; Esposito, Paolo/0000-0003-4849-5092 FU SFXT; ASI-INAF [I/009/10/0]; PSU by NASA [NAS5-00136]; Autonomous Region of Sardinia [L.R. 7/2007] FX We thank the Swift team duty scientists and science planners. We also thank the remainder of the Swift XRT and BAT teams, S. Barthelmy and J.A. Nousek, in particular, for their invaluable help and support of the SFXT project as a whole. We thank A. Cucchiara for helpful discussions. We acknowledge financial contribution from the agreement ASI-INAF I/009/10/0. This work was supported at PSU by NASA contract NAS5-00136. PE acknowledges financial support from the Autonomous Region of Sardinia through a research grant under the programme PO Sardegna FSE 2007-2013, L.R. 7/2007 'Promoting scientific research and innovation technology in Sardinia'. We also thank the anonymous referee for swift comments that helped improve the paper. NR 53 TC 13 Z9 13 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2012 VL 419 IS 3 BP 2695 EP 2702 DI 10.1111/j.1365-2966.2011.19916.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872XI UT WOS:000298844300065 ER PT J AU Ramirez, JM Tombesi, F AF Ramirez, J. M. Tombesi, F. TI On the X-ray low- and high-velocity outflows in active galactic nuclei SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; galaxies: active; X-rays: galaxies ID ACCRETION DISC OUTFLOWS; ULTRA-FAST OUTFLOWS; SHELL ABSORPTION-LINES; BLACK-HOLE; APM 08279+5255; WARM ABSORBERS; QUASAR; WINDS; SPECTRA; RADIATION AB An exploration of the relationship between bolometric luminosity and outflow velocity for two classes of X-ray outflows in a large sample of active galactic nuclei has been performed. We find that line radiation pressure could be one physical mechanism that might accelerate the gas we observe in warm absorber, v similar to 1001000 km s(-1), and on comparable but less stringent grounds the ultrafast outflows, v similar to 0.030.3c. If comparable with the escape velocity of the system, the first is naturally located at distances of the dusty torus, approximate to 1 pc, and the second at subparsec scales, approximate to 0.01 pc, in accordance with large set of observational evidence existing in the literature. The presentation of this relationship might give us key clues for our understanding of the different physical mechanisms acting in the centre of galaxies, the feedback process and its impact on the evolution of the host galaxy. C1 [Ramirez, J. M.] Leibniz Inst Astrophys Potsdam, D-14482 Potsdam, Germany. [Tombesi, F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Tombesi, F.] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Tombesi, F.] NASA, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ramirez, JM (reprint author), Leibniz Inst Astrophys Potsdam, Sternwarte 16, D-14482 Potsdam, Germany. EM jramirez@aip.de FU NASA through the ADAP/LTSA; National Aeronautics and Space Administration; ESA FX JMR would like to thank T. Kallman for a reading of the manuscript. JMR also wants to thank the useful and constructive comments from the referee which helped to improve several aspects of the work. FT provided the data based on observations obtained with the XMM-Newton satellite, an ESA funded mission with contributions by ESA member states and USA. FT acknowledges support from NASA through the ADAP/LTSA programme. 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. NR 50 TC 3 Z9 4 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2012 VL 419 IS 1 BP L64 EP L68 DI 10.1111/j.1745-3933.2011.01180.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 865HZ UT WOS:000298303300014 ER PT J AU Davami, K Mortazavi, B Ghassemi, HM Yassar, RS Lee, JS Remond, Y Meyyappan, M AF Davami, Keivan Mortazavi, Bohayra Ghassemi, Hessam M. Yassar, Reza S. Lee, Jeong-Soo Remond, Yves Meyyappan, M. TI A computational and experimental investigation of the mechanical properties of single ZnTe nanowires SO NANOSCALE LA English DT Article ID CARBON NANOTUBE ROPES; MOLECULAR-DYNAMICS; ZNO NANOWIRES; ELASTIC PROPERTIES; STRENGTH; MICROSCOPY; CONSTANTS AB One-dimensional nanostructures such as ZnTe, CdTe, Bi2Te3 and others have attracted much attention in recent years for their potential in thermoelectric devices among other applications. A better understanding of their mechanical properties is important for the design of devices. A combined experimental and computational approach has been used here to investigate the size effects on the Young's modulus of ZnTe nanowires (NWs). The mechanical properties of individual ZnTe nanowires in a wide diameter range (50-230 nm) were experimentally measured inside a high resolution transmission electron microscope using an atomic force microscope probe with the ability to record in situ continuous force-displacement curves. The in situ observations showed that ZnTe NWs are flexible nanostructures with the ability to withstand relatively high buckling forces without becoming fractured. The Young's modulus is found to be independent of nanowire diameter in the investigated range, in contrast to reported results for ZnO NWs and carbon nanotubes where the modulus increases with a decrease in diameter. Molecular dynamics simulations performed for nanowires with diameters less than 20 nm show limited size dependence for diameters smaller than 5 nm. The surface atoms present lower Young's modulus according to the simulations and the limited size dependency of the cylindrical ZnTe NWs is attributed to the short range covalent interactions. C1 [Davami, Keivan; Lee, Jeong-Soo; Meyyappan, M.] Pohang Univ Sci & Technol POSTECH, Dept IT Convergence Engn, Pohang, South Korea. [Mortazavi, Bohayra] Ctr Rech Publ Henri Tudor, Dept Adv Mat & Struct, L-4002 Esch Sur Alzette, Luxembourg. [Mortazavi, Bohayra; Remond, Yves] Univ Strasbourg, CNRS, Inst Mecan Fluides & Solides, F-67000 Strasbourg, France. [Ghassemi, Hessam M.; Yassar, Reza S.] Michigan Technol Univ, Dept Mech Engn Engn Mech, Houghton, MI 49931 USA. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lee, JS (reprint author), Pohang Univ Sci & Technol POSTECH, Dept IT Convergence Engn, Pohang, South Korea. EM ljs6951@postech.ac.kr; m.meyyappan@nasa.gov RI Remond, Yves/G-8954-2011 OI Remond, Yves/0000-0003-3312-8361 FU World Class University through the National Research Foundation of Korea; Ministry of Education, Science and Technology [R31-2008-000-10100-0]; NSF-DMR [0820884]; NSF-CMMI [0926819] FX This work was supported by the World Class University program through the National Research Foundation of Korea funded by the Ministry of Education, Science and Technology under Project R31-2008-000-10100-0. RSY would like to acknowledge the funding support through the NSF-DMR Grant 0820884 and NSF-CMMI Grant 0926819. NR 34 TC 7 Z9 8 U1 3 U2 46 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 2040-3364 EI 2040-3372 J9 NANOSCALE JI Nanoscale PY 2012 VL 4 IS 3 BP 897 EP 903 DI 10.1039/c2nr11593j PG 7 WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 878YE UT WOS:000299292600031 PM 22173853 ER PT J AU Benavides, JA Huchard, E Pettorelli, N King, AJ Brown, ME Archer, CE Appleton, CC Raymond, M Cowlishaw, G AF Benavides, Julio A. Huchard, Elise Pettorelli, Nathalie King, Andrew J. Brown, Molly E. Archer, Colleen E. Appleton, Chris C. Raymond, Michel Cowlishaw, Guy TI From parasite encounter to infection: Multiple-scale drivers of parasite richness in a wild social primate population SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE home range use; gut parasites; physical condition; baboon; sociality ID SEXUAL SIZE DIMORPHISM; SPECIES RICHNESS; GASTROINTESTINAL PARASITES; BODY CONDITION; SMALL MAMMALS; SOUTH-AFRICA; ECOLOGY; DIVERSITY; DISEASES; MHC AB Host parasite diversity plays a fundamental role in ecological and evolutionary processes, yet the factors that drive it are still poorly understood. A variety of processes, operating across a range of spatial scales, are likely to influence both the probability of parasite encounter and subsequent infection. Here, we explored eight possible determinants of parasite richness, comprising rainfall and temperature at the population level, ranging behavior and home range productivity at the group level, and age, sex, body condition, and social rank at the individual level. We used a unique dataset describing gastrointestinal parasites in a terrestrial subtropical vertebrate (chacma baboons, Papio ursinus), comprising 662 fecal samples from 86 individuals representing all age-sex classes across two groups over two dry seasons in a desert population. Three mixed models were used to identify the most important factor at each of the three spatial scales (population, group, individual); these were then standardized and combined in a single, global, mixed model. Individual age had the strongest influence on parasite richness, in a convex relationship. Parasite richness was also higher in females and animals in poor condition, albeit at a lower order of magnitude than age. Finally, with a further halving of effect size, parasite richness was positively correlated to day range and temperature. These findings indicate that a range of factors influence host parasite richness through both encounter and infection probabilities but that individual-level processes may be more important than those at the group or population level. Am J Phys Anthropol 147: 52-63, 2012. (C) 2011 Wiley-Liss,Inc. C1 [Benavides, Julio A.; Raymond, Michel] Univ Montpellier 2, CNRS, Inst Sci Evolut, F-34095 Montpellier 5, France. [Benavides, Julio A.; Pettorelli, Nathalie; King, Andrew J.; Cowlishaw, Guy] Zool Soc London, Inst Zool, London NW1 4RY, England. [Huchard, Elise] German Primate Ctr, Dept Behav Ecol & Sociobiol, D-37077 Gottingen, Germany. [Huchard, Elise] Univ Gottingen, Courant Res Ctr Evolut Social Behav, Gottingen, Germany. [King, Andrew J.] Univ London, Struct & Mot Lab, Royal Vet Coll, Hatfield AL9 7DY, Herts, England. [Brown, Molly E.] NASA, SSAI, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Archer, Colleen E.; Appleton, Chris C.] Univ KwaZulu Natal, Sch Biol & Conservat Sci, Durban, South Africa. RP Benavides, JA (reprint author), Univ Montpellier 2, CNRS, Inst Sci Evolut, Pl Eugene Bataillon,CC 065, F-34095 Montpellier 5, France. EM benavidesjulio@yahoo.fr RI Huchard, Elise/G-9072-2011; Brown, Molly/M-5146-2013; Raymond, Michel/C-9049-2015; Brown, Molly/E-2724-2010; OI Huchard, Elise/0000-0002-6944-449X; Brown, Molly/0000-0001-7384-3314; Brown, Molly/0000-0001-7384-3314; Raymond, Michel/0000-0002-1714-6984 FU CONICYT (Chilean Government); Deutsches Forschungsgemeinschaft [HU 1820/1-1]; Natural Environment Research Council (NERC) (UK); Ministere de l'Education et de la Recherche (France) FX Grant sponsors: CONICYT Scholarship (Chilean Government); Deutsches Forschungsgemeinschaft Research Grant; Grant number: HU 1820/1-1; Natural Environment Research Council (NERC) (UK) Project Grant; Advanced Fellowship; NERC Studentship; Ministere de l'Education et de la Recherche (France) Studentship. NR 87 TC 10 Z9 11 U1 2 U2 38 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD JAN PY 2012 VL 147 IS 1 BP 52 EP 63 DI 10.1002/ajpa.21627 PG 12 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 862JL UT WOS:000298086900007 PM 21989507 ER PT J AU Konopka, D Johnson, MA Errico, M Bahrami, P Hays, CC AF Konopka, Daniel Johnson, Michael A. Errico, Michael Bahrami, Poyan Hays, Charles C. TI Oxidation and Oxygen Reduction on Polycrystalline Platinum in Aqueous Tetramethylguanidine Alkaline Electrolyte SO ELECTROCHEMICAL AND SOLID STATE LETTERS LA English DT Article ID ANION-EXCHANGE MEMBRANE; FUEL-CELLS; GUANIDINES; STATE AB Aqueous, 0.1M 1,1,3,3-tetramethylguanidine was shown to be an active alkaline liquid electrolyte (without metal cations) using a polycrystalline platinum electrode. Cyclic voltammetry reveals that the electrolyte supports -OH conductivity, showing many platinum redox features observed in traditional electrolytes. Gradual reaction with H2O decreases ionic conductivity over several months. Oxygen reduction curves in TMG lack a distinct transition from kinetic to diffusion-limiting behavior due to organic adsorbates. Results ultimately show that tetramethylguanidine could be developed as an alternative to NaOH/KOH for enhancing ionic conductivity of alkaline anion exchange membranes of similar composition. (C) 2011 The Electrochemical Society. [DOI: 10.1149/2.009203esl] All rights reserved. C1 [Konopka, Daniel; Johnson, Michael A.; Errico, Michael; Bahrami, Poyan; Hays, Charles C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Konopka, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM konopka@caltech.edu FU Department of Energy [DE-PS36-08GO98101]; National Aeronautics and Space Administration FX The research described in this presentation was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We would like to thank our collaborators in the group of Dr. Yu Seung Kim at Los Alamos National Laboratory, and acknowledge the support of the Department of Energy (DE-PS36-08GO98101). NR 18 TC 3 Z9 3 U1 1 U2 23 PU ELECTROCHEMICAL SOC INC PI PENNINGTON PA 65 SOUTH MAIN STREET, PENNINGTON, NJ 08534 USA SN 1099-0062 J9 ELECTROCHEM SOLID ST JI Electrochem. Solid State Lett. PY 2012 VL 15 IS 3 BP B17 EP B19 DI 10.1149/2.009203esl PG 3 WC Electrochemistry; Materials Science, Multidisciplinary SC Electrochemistry; Materials Science GA 876QT UT WOS:000299123400004 ER PT J AU Marancik, KE Richardson, DE Lyczkowski-Shultz, J Cowen, RK Konieczna, M AF Marancik, Katrin E. Richardson, David E. Lyczkowski-Shultz, Joanne Cowen, Robert K. Konieczna, Malgorzata TI Spatial and temporal distribution of grouper larvae (Serranidae: Epinephelinae: Epinephelini) in the Gulf of Mexico and Straits of Florida SO FISHERY BULLETIN LA English DT Article ID GAG MYCTEROPERCA-MICROLEPIS; US-VIRGIN-ISLANDS; EASTERN GULF; NASSAU GROUPER; SPAWNING AGGREGATIONS; PROTECTED AREAS; NORTH-CAROLINA; LIFE-HISTORY; RED GROUPER; PROTOGYNOUS GROUPER AB Little is known about the seasonality and distribution of grouper larvae (Serranidae: Epinephelini) in the Gulf of Mexico and Atlantic Ocean off the coast of the southeast United States. Grouper larvae were collected from a transect across the Straits of Florida in 2003 and 2004 and during the Southeast Area Monitoring and Assessment Program spring and fall surveys from 1982 through 2005. Analysis of these larval data provided information on location and timing of spawning, larval distribution patterns, and interannual occurrence for a group of species not easily studied as adults. Our analyses indicated that shelf-edge habitat is important for spawning of many species of grouper-some species for which data were not previously available. Spawning for some species may occur year-round, but two peak seasons are evident: late winter and late summer through early fall. Interannual variability in the use of three important subregions by species or groups of species was partially explained by environmental factors (surface temperature, surface salinity, and water depth). A shift in species dominance over the last three decades from spring-spawned species (most of the commercial species) to fall-spawned species also was documented. The results of these analyses expand our understanding of the basic distribution and spawning patterns of northwest Atlantic grouper species and indicate a need for further examination of the changing population structure of individual species and species dominance in the region. C1 [Marancik, Katrin E.; Richardson, David E.] NOAA, Narragansett Lab, NE Fisheries Sci Ctr, Natl Marine Fisheries Serv, Narragansett, RI 02882 USA. [Marancik, Katrin E.; Lyczkowski-Shultz, Joanne] NOAA, Mississippi Lab, SE Fisheries Sci Ctr, Natl Marine Fisheries Serv, Pascagoula, MS 39567 USA. [Marancik, Katrin E.] IAP World Serv Inc, Pascagoula, MS 39567 USA. [Cowen, Robert K.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Konieczna, Malgorzata] Plankton Sorting & Identificat Ctr, Sea Fisheries Inst, PL-71550 Szczecin, Poland. RP Marancik, KE (reprint author), NOAA, Narragansett Lab, NE Fisheries Sci Ctr, Natl Marine Fisheries Serv, 28 Tarzwell Dr, Narragansett, RI 02882 USA. EM Katey.marancik@noaa.gov FU OAR Cooperative Institute Program Office; Northern Gulf Institute, a NOAA Cooperative Institute; National Science Foundation [OCE-0136132]; Gulf States Marine Fisheries Commission [Billfish-2005-017] FX We would like to thank the following people for their significant contributions to this research: L. Bulloc, J. Llopiz, C. Guigand, A. Exum, J. VanWye, K. Shulzitski, K. Williams, The SEAMAP Plankton Team, and the staff at the Sea Fisheries Institute, Plankton Sorting and Identification Center. This research would not have been possible without the resourcefulness and skilled assistance of the crews of the NOAA research vessels Chapman, Oregon II and Gordon Gunter and the dedication of biologists and volunteers who participated in SEAMAP plankton surveys sampling. N. Bachelor and J. Hare provided statistical expertise. This project was funded through the OAR Cooperative Institute Program Office and is part of the research program of the Northern Gulf Institute, a NOAA Cooperative Institute. Funding for the Florida Straits sampling was provided by grants from the National Science Foundation (OCE-0136132) and the Gulf States Marine Fisheries Commission (Billfish-2005-017). NR 64 TC 6 Z9 7 U1 0 U2 21 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 J9 FISH B-NOAA JI Fish. Bull. PD JAN PY 2012 VL 110 IS 1 BP 1 EP 20 PG 20 WC Fisheries SC Fisheries GA 880KO UT WOS:000299406200001 ER PT J AU Rodgveller, CJ Lunsford, CR Fujioka, JT AF Rodgveller, Cara J. Lunsford, Chris R. Fujioka, Jeffrey T. TI Effects of maternal age and size on embryonic energy reserves, developmental timing, and fecundity in quillback rockfish (Sebastes maliger) SO FISHERY BULLETIN LA English DT Article ID YELLOWTAIL ROCKFISH; LARVAL SURVIVAL; FISH; RECRUITMENT; POPULATIONS; MANAGEMENT; MELANOPS; GROWTH AB Maternal effects on the quality of progeny can have direct impacts on population productivity. Rockfish are viviparous and the oil globule size of larvae at parturition has been shown to have direct effects on time until starvation and growth rate. We sampled embryos and preparturition larvae opportunistically from 89 gravid quillback rockfish (Sebastes maliger) in Southeast Alaska. Because the developmental stage and sampling period were correlated with oil globule size, they were treated as covariates in an analysis of maternal age, length, and weight effects on oil globule size. Maternal factors were related to developmental timing for almost all sampling periods, indicating that older, longer, and heavier females develop embryos earlier than younger, shorter, or lighter ones. Oil globule diameter and maternal length and weight were statistically linked, but the relationships may not be biologically significant. Weight-specific fecundity did not increase with maternal size or age, suggesting that reproductive output does not increase more quickly as fish age and grow. Age or size truncation of a rockfish population, in which timing of parturition is related to age and size, could result in a shorter parturition season. This shortening of the parturition season could make the population vulnerable to fluctuating environmental conditions. C1 [Rodgveller, Cara J.; Lunsford, Chris R.; Fujioka, Jeffrey T.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Alaska Biol Lab, Juneau, AK 99801 USA. RP Rodgveller, CJ (reprint author), NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Alaska Biol Lab, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA. EM cara.rodgveller@noaa.gov NR 28 TC 4 Z9 4 U1 1 U2 16 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 J9 FISH B-NOAA JI Fish. Bull. PD JAN PY 2012 VL 110 IS 1 BP 36 EP 45 PG 10 WC Fisheries SC Fisheries GA 880KO UT WOS:000299406200003 ER PT J AU Angelov, P Yager, R AF Angelov, Plamen Yager, Ronald TI A new type of simplified fuzzy rule-based system SO INTERNATIONAL JOURNAL OF GENERAL SYSTEMS LA English DT Article DE fuzzy rule-based systems; Mamdani and Takagi-Sugeno fuzzy systems; recursive least square estimation; data density and distribution; clustering ID INFERENCE SYSTEM; DATA STREAMS; IDENTIFICATION; PREDICTION; NETWORK; MODELS AB Over the last quarter of a century, two types of fuzzy rule-based (FRB) systems dominated, namely Mamdani and Takagi-Sugeno type. They use the same type of scalar fuzzy sets defined per input variable in their antecedent part which are aggregated at the inference stage by t-norms or co-norms representing logical AND/OR operations. In this paper, we propose a significantly simplified alternative to define the antecedent part of FRB systems by data Clouds and density distribution. This new type of FRB systems goes further in the conceptual and computational simplification while preserving the best features (flexibility, modularity, and human intelligibility) of its predecessors. The proposed concept offers alternative non-parametric form of the rules antecedents, which fully reflects the real data distribution and does not require any explicit aggregation operations and scalar membership functions to be imposed. Instead, it derives the fuzzy membership of a particular data sample to a Cloud by the data density distribution of the data associated with that Cloud. Contrast this to the clustering which is parametric data space decomposition/partitioning where the fuzzy membership to a cluster is measured by the distance to the cluster centre/prototype ignoring all the data that form that cluster or approximating their distribution. The proposed new approach takes into account fully and exactly the spatial distribution and similarity of all the real data by proposing an innovative and much simplified form of the antecedent part. In this paper, we provide several numerical examples aiming to illustrate the concept. C1 [Angelov, Plamen] Univ Lancaster, Sch Comp & Commun, Infolab21, Lancaster LA1 4WA, England. [Yager, Ronald] Iona Coll, Inst Machine Intelligence, New Rochelle, NY 10801 USA. [Yager, Ronald] New York Acad Sci, New York, NY USA. [Yager, Ronald] Natl Sci Fdn, Arlington, VA 22230 USA. [Yager, Ronald] NASA, Stanford, CA USA. [Yager, Ronald] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Yager, Ronald] King Saud Univ, Riyadh, Saudi Arabia. [Yager, Ronald] Aalborg Univ, Aalborg, Denmark. RP Angelov, P (reprint author), Univ Lancaster, Sch Comp & Commun, Infolab21, Lancaster LA1 4WA, England. EM p.angelov@lancaster.ac.uk NR 33 TC 30 Z9 31 U1 1 U2 6 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0308-1079 J9 INT J GEN SYST JI Int. J. Gen. Syst. PY 2012 VL 41 IS 2 BP 163 EP 185 DI 10.1080/03081079.2011.634807 PG 23 WC Computer Science, Theory & Methods; Ergonomics SC Computer Science; Engineering GA 879FA UT WOS:000299313900006 ER PT J AU Leckey, CAC Hinders, MK AF Leckey, Cara A. C. Hinders, Mark K. TI Viscous effects in the acoustic manipulation of algae for biofuel production SO JOURNAL OF APPLIED PHYCOLOGY LA English DT Article DE Biofuels; Microalgae; Acoustic manipulation; Acoustic force; Algae biofuels; Micromanipulation; Acoustic sorting ID ULTRASONIC STANDING-WAVE; DIVIDED-FLOW-FIELDS; SUSPENDED PARTICLES; RADIATION PRESSURE; SEPARATION; SPHERE; FLUID; MICROALGAE; BIODIESEL; DEVICE AB Microalgae are emerging as a promising source for environmentally friendly biofuels. Acoustic manipulation of algal cells using standing waves is a relatively new method for dewatering and/or sorting algae harvests. Recent work in the field has shown that acoustic dewatering methods may be more efficient and economical than traditional methods. Optimization of acoustic algal cell manipulation requires a knowledge of the acoustic radiation force upon the cells. Previous work in the field does not account for viscosity of the algal cells or surrounding fluid. We have implemented inviscid and viscous acoustic force models for standing waves incident upon algal cells in salt and freshwater. The results presented in this paper show that significant viscous effects can occur at certain frequencies and/or cell sizes and may need to be taken into account in the development of efficient experimental techniques. C1 [Leckey, Cara A. C.] NASA Langley Res Ctr, Hampton, VA 23681 USA. [Hinders, Mark K.] Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23187 USA. RP Leckey, CAC (reprint author), NASA Langley Res Ctr, MS 231,3B E Taylor St, Hampton, VA 23681 USA. EM cara.ac.leckey@nasa.gov FU Virginia Space Grant Consortium FX The authors thank Tom Crockett for assistance using the Sciclone computing cluster and the Virginia Space Grant Consortium for partial funding. NR 45 TC 3 Z9 3 U1 1 U2 17 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0921-8971 J9 J APPL PHYCOL JI J. Appl. Phycol. PD JAN PY 2012 VL 24 IS 1 BP 145 EP 156 DI 10.1007/s10811-011-9662-7 PG 12 WC Biotechnology & Applied Microbiology; Marine & Freshwater Biology SC Biotechnology & Applied Microbiology; Marine & Freshwater Biology GA 876QI UT WOS:000299122200016 ER PT J AU Muller, HSP Cernicharo, J Agundez, M Decin, L Encrenaz, P Pearson, JC Teyssier, D Waters, LBFM AF Mueller, Holger S. P. Cernicharo, Jose Agundez, M. Decin, L. Encrenaz, P. Pearson, J. C. Teyssier, D. Waters, L. B. F. M. TI Spectroscopic parameters for silacyclopropynylidene, SiC2, from extensive astronomical observations toward CW Leo (IRC+10216) with the Herschel satellite SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE Rotational spectroscopy; Interstellar molecule; Silicon compound; Centrifugal distortion ID SILICON DICARBIDE SIC2; JET-COOLED SIC2; LINE SURVEY; MOLECULAR-SPECTROSCOPY; ROTATIONAL SPECTRUM; COLOGNE DATABASE; EXCITED-STATE; IDENTIFICATION; (SIC2)-SI-30; RESOLUTION AB A molecular line survey has been carried out toward the carbon-rich asymptotic giant branch star CW Leo employing the HIFI instrument on board of the Herschel satellite. Numerous features from 480 GHz to beyond 1100 GHz could be assigned unambiguously to the fairly floppy SiC2 molecule. However, predictions from laboratory data exhibited large deviations from the observed frequencies even after some lower frequency data from this survey were incorporated into a fit. Therefore, we present a combined fit of all available laboratory data together with data from radio-astronomical observations. (C) 2011 Elsevier Inc. All rights reserved. C1 [Mueller, Holger S. P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Cernicharo, Jose; Agundez, M.] CSIC, Dept Astrofis, Ctr Astrobiol, INTA, Madrid 28850, Spain. [Agundez, M.] Observ Paris, LUTH, F-92190 Meudon, France. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Decin, L.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Decin, L.; Waters, L. B. F. M.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Teyssier, D.] ESA, European Space Astron Ctr, Madrid, Spain. [Waters, L. B. F. M.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. RP Muller, HSP (reprint author), Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. EM hspm@ph1.uni-koeln.de RI Agundez, Marcelino/I-5369-2012; OI Agundez, Marcelino/0000-0003-3248-3564; Mueller, Holger/0000-0002-0183-8927 FU Bundesministerium fur Bildung und Forschung (BMBF); Spanish MICINN [AYA2009-07304, CSD-2009-00038] FX H.S.P.M. is very grateful to the Bundesministerium fur Bildung und Forschung (BMBF) for financial support aimed at maintaining the Cologne Database for Molecular Spectroscopy, CDMS. This support has been administered by the Deutsches Zentrum fur Luft-und Raumfahrt (DLR). J.C. thanks the Spanish MICINN for funding support under Grants AYA2009-07304 and CSD-2009-00038. NR 37 TC 9 Z9 9 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD JAN PY 2012 VL 271 IS 1 BP 50 EP 55 DI 10.1016/j.jms.2011.11.006 PG 6 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 881DZ UT WOS:000299462000009 ER PT J AU Chen, YJ Hemmati, H Ortiz, GG AF Chen, Yijiang Hemmati, Hamid Ortiz, Gerry G. TI Feasibility of infrared Earth tracking for deep-space optical communications SO OPTICS LETTERS LA English DT Article AB Infrared (IR) Earth thermal tracking is a viable option for optical communications to distant planet and outer-planetary missions. However, blurring due to finite receiver aperture size distorts IR Earth images in the presence of Earth's nonuniform thermal emission and limits its applicability. We demonstrate a deconvolution algorithm that can overcome this limitation and reduce the error from blurring to a negligible level. The algorithm is applied successfully to Earth thermal images taken by the Mars Odyssey spacecraft. With the solution to this critical issue, IR Earth tracking is established as a viable means for distant planet and outer-planetary optical communications. (C) 2011 Optical Society of America C1 [Chen, Yijiang; Hemmati, Hamid; Ortiz, Gerry G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chen, YJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM yijiang.chen@jpl.nasa.gov FU NASA FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 6 TC 1 Z9 2 U1 4 U2 8 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 J9 OPT LETT JI Opt. Lett. PD JAN 1 PY 2012 VL 37 IS 1 BP 73 EP 75 PG 3 WC Optics SC Optics GA 877HB UT WOS:000299167100023 PM 22212795 ER PT J AU Fisher, RR AF Fisher, R. R. TI THE SOLAR DYNAMICS OBSERVATORY Preface SO SOLAR PHYSICS LA English DT Editorial Material C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. RP Fisher, RR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. EM richard.r.fisher@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JAN PY 2012 VL 275 IS 1-2 BP 1 EP 2 DI 10.1007/s11207-011-9914-3 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YT UT WOS:000299294600001 ER PT J AU Pesnell, WD Thompson, BJ Chamberlin, PC AF Pesnell, W. Dean Thompson, B. J. Chamberlin, P. C. TI The Solar Dynamics Observatory (SDO) SO SOLAR PHYSICS LA English DT Article DE SDO; Solar cycle; Helioseismology; Coronal; Space weather AB The Solar Dynamics Observatory (SDO) was launched on 11 February 2010 at 15: 23 UT from Kennedy Space Center aboard an Atlas V 401 (AV-021) launch vehicle. A series of apogee-motor firings lifted SDO from an initial geosynchronous transfer orbit into a circular geosynchronous orbit inclined by 28 about the longitude of the SDO-dedicated ground station in New Mexico. SDO began returning science data on 1 May 2010. SDO is the first space-weather mission in NASA's Living With a Star (LWS) Program. SDO's main goal is to understand, driving toward a predictive capability, those solar variations that influence life on Earth and humanity's technological systems. The SDO science investigations will determine how the Sun's magnetic field is generated and structured, how this stored magnetic energy is released into the heliosphere and geospace as the solar wind, energetic particles, and variations in the solar irradiance. Insights gained from SDO investigations will also lead to an increased understanding of the role that solar variability plays in changes in Earth's atmospheric chemistry and climate. The SDO mission includes three scientific investigations (the Atmospheric Imaging Assembly (AIA), Extreme Ultraviolet Variability Experiment (EVE), and Helioseismic and Magnetic Imager (HMI)), a spacecraft bus, and a dedicated ground station to handle the telemetry. The Goddard Space Flight Center built and will operate the spacecraft during its planned five-year mission life; this includes: commanding the spacecraft, receiving the science data, and forwarding that data to the science teams. The science investigations teams at Stanford University, Lockheed Martin Solar Astrophysics Laboratory (LMSAL), and University of Colorado Laboratory for Atmospheric and Space Physics (LASP) will process, analyze, distribute, and archive the science data. We will describe the building of SDO and the science that it will provide to NASA. C1 [Pesnell, W. Dean; Thompson, B. J.; Chamberlin, P. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. RP Pesnell, WD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. EM william.d.pesnell@nasa.gov; barbara.j.thompson@nasa.gov; phillip.c.chamberlin@nasa.gov RI Chamberlin, Phillip/C-9531-2012; Pesnell, William/D-1062-2012; Thompson, Barbara/C-9429-2012 OI Chamberlin, Phillip/0000-0003-4372-7405; Pesnell, William/0000-0002-8306-2500; FU NASA's Solar Dynamics Observatory (SDO) FX This work was supported by NASA's Solar Dynamics Observatory (SDO). NR 11 TC 582 Z9 589 U1 8 U2 41 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JAN PY 2012 VL 275 IS 1-2 BP 3 EP 15 DI 10.1007/s11207-011-9841-3 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YT UT WOS:000299294600002 ER PT J AU Martens, PCH Attrill, GDR Davey, AR Engell, A Farid, S Grigis, PC Kasper, J Korreck, K Saar, SH Savcheva, A Su, Y Testa, P Wills-Davey, M Bernasconi, PN Raouafi, NE Delouille, VA Hochedez, JF Cirtain, JW DeForest, CE Angryk, RA De Moortel, I Wiegelmann, T Georgoulis, MK McAteer, RTJ Timmons, RP AF Martens, P. C. H. Attrill, G. D. R. Davey, A. R. Engell, A. Farid, S. Grigis, P. C. Kasper, J. Korreck, K. Saar, S. H. Savcheva, A. Su, Y. Testa, P. Wills-Davey, M. Bernasconi, P. N. Raouafi, N. -E. Delouille, V. A. Hochedez, J. F. Cirtain, J. W. DeForest, C. E. Angryk, R. A. De Moortel, I. Wiegelmann, T. Georgoulis, M. K. McAteer, R. T. J. Timmons, R. P. TI Computer Vision for the Solar Dynamics Observatory (SDO) SO SOLAR PHYSICS LA English DT Article DE Instrumentation and data management; Solar Dynamics Observatory ID CORONAL MASS EJECTIONS; HINODE XRT OBSERVATIONS; MAGNETIC-FIELDS; WAVELET ANALYSIS; FLUX ROPES; NUMERICAL SIMULATIONS; VECTOR MAGNETOGRAMS; AUTOMATIC DETECTION; FILAMENT DETECTION; CONE MODEL AB In Fall 2008 NASA selected a large international consortium to produce a comprehensive automated feature-recognition system for the Solar Dynamics Observatory (SDO). The SDO data that we consider are all of the Atmospheric Imaging Assembly (AIA) images plus surface magnetic-field images from the Helioseismic and Magnetic Imager (HMI). We produce robust, very efficient, professionally coded software modules that can keep up with the SDO data stream and detect, trace, and analyze numerous phenomena, including flares, sigmoids, filaments, coronal dimmings, polarity inversion lines, sunspots, Xray bright points, active regions, coronal holes, EIT waves, coronal mass ejections (CMEs), coronal oscillations, and jets. We also track the emergence and evolution of magnetic elements down to the smallest detectable features and will provide at least four full-disk, nonlinear, force-free magnetic field extrapolations per day. The detection of CMEs and filaments is accomplished with Solar and Heliospheric Observatory (SOHO)/Large Angle and Spectrometric Coronagraph (LASCO) and ground-based H alpha data, respectively. A completely new software element is a trainable feature-detection module based on a generalized image-classification algorithm. Such a trainable module can be used to find features that have not yet been discovered (as, for example, sigmoids were in the pre-Yohkoh era). Our codes will produce entries in the Heliophysics Events Knowledgebase (HEK) as well as produce complete catalogs for results that are too numerous for inclusion in the HEK, such as the X-ray bright-point metadata. This will permit users to locate data on individual events as well as carry out statistical studies on large numbers of events, using the interface provided by the Virtual Solar Observatory. The operations concept for our computer vision system is that the data will be analyzed in near real time as soon as they arrive at the SDO Joint Science Operations Center and have undergone basic processing. This will allow the system to produce timely space-weather alerts and to guide the selection and production of quicklook images and movies, in addition to its prime mission of enabling solar science. We briefly describe the complex and unique data-processing pipeline, consisting of the hardware and control software required to handle the SDO data stream and accommodate the computer-vision modules, which has been set up at the Lockheed-Martin Space Astrophysics Laboratory (LMSAL), with an identical copy at the Smithsonian Astrophysical Observatory (SAO). C1 [Martens, P. C. H.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Martens, P. C. H.; Attrill, G. D. R.; Davey, A. R.; Engell, A.; Farid, S.; Grigis, P. C.; Kasper, J.; Korreck, K.; Saar, S. H.; Savcheva, A.; Su, Y.; Testa, P.; Wills-Davey, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Savcheva, A.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Bernasconi, P. N.; Raouafi, N. -E.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Delouille, V. A.; Hochedez, J. F.] SIDC Royal Observ Belgium, B-1180 Brussels, Belgium. [Cirtain, J. W.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [DeForest, C. E.] SW Res Inst, Boulder, CO 80302 USA. [Angryk, R. A.] Montana State Univ, Dept Comp Sci, Bozeman, MT 59717 USA. [De Moortel, I.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. [Wiegelmann, T.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Georgoulis, M. K.] Acad Athens, Res Ctr Astron & Appl Math, Athens 11527, Greece. [McAteer, R. T. J.] Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland. [McAteer, R. T. J.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Timmons, R. P.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA. RP Martens, PCH (reprint author), Montana State Univ, Dept Phys, 247 EPS, Bozeman, MT 59717 USA. EM martens@physics.montana.edu RI Angryk, Rafal/F-5696-2012; Kasper, Justin/D-1152-2010; Bernasconi, Pietro/H-2224-2016; Raouafi, Nour/C-2286-2016 OI Kasper, Justin/0000-0002-7077-930X; Bernasconi, Pietro/0000-0002-0787-8954; Raouafi, Nour/0000-0003-2409-3742 FU NASA [NNX09AB03G]; Applied Physics Laboratory of Johns Hopkins University; Lockheed Martin Solar and Astrophysics Laboratory; NASA Marshall Space Flight Center FX This research and development project is supported by NASA Grant NNX09AB03G to the Smithsonian Astrophysical Observatory with subcontracts to the Southwest Research Institute, Montana State University, the Applied Physics Laboratory of Johns Hopkins University, and the Lockheed Martin Solar and Astrophysics Laboratory, and with the participation of the NASA Marshall Space Flight Center. This project would be impossible without the major contributions from our European collaborators. The institutions involved are the Royal Observatory of Belgium, the Academy of Athens, Trinity College Dublin, the University of St Andrews, and the Max-Planck-Institut fur Sonnensystemforschung. NR 105 TC 49 Z9 49 U1 1 U2 17 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 JAN PY 2012 VL 275 IS 1-2 BP 79 EP 113 DI 10.1007/s11207-010-9697-y PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YT UT WOS:000299294600006 ER PT J AU Woods, TN Eparvier, FG Hock, R Jones, AR Woodraska, D Judge, D Didkovsky, L Lean, J Mariska, J Warren, H McMullin, D Chamberlin, P Berthiaume, G Bailey, S Fuller-Rowell, T Sojka, J Tobiska, WK Viereck, R AF Woods, T. N. Eparvier, F. G. Hock, R. Jones, A. R. Woodraska, D. Judge, D. Didkovsky, L. Lean, J. Mariska, J. Warren, H. McMullin, D. Chamberlin, P. Berthiaume, G. Bailey, S. Fuller-Rowell, T. Sojka, J. Tobiska, W. K. Viereck, R. TI Extreme Ultraviolet Variability Experiment (EVE) on the Solar Dynamics Observatory (SDO): Overview of Science Objectives, Instrument Design, Data Products, and Model Developments SO SOLAR PHYSICS LA English DT Article DE EVE; SDO; Solar EUV irradiance; Space weather research ID EUV IRRADIANCE VARIABILITY; OPEN MAGNETIC-FLUX; SPACE WEATHER; FAR-SIDE; ATOMIC DATABASE; EMISSION-LINES; EXPERIMENT SEE; SUN; WAVELENGTHS; OPERATIONS AB The highly variable solar extreme ultraviolet (EUV) radiation is the major energy input to the Earth's upper atmosphere, strongly impacting the geospace environment, affecting satellite operations, communications, and navigation. The Extreme ultraviolet Variability Experiment (EVE) onboard the NASA Solar Dynamics Observatory (SDO) will measure the solar EUV irradiance from 0.1 to 105 nm with unprecedented spectral resolution (0.1 nm), temporal cadence (ten seconds), and accuracy (20%). EVE includes several irradiance instruments: The Multiple EUV Grating Spectrographs (MEGS)-A is a grazing-incidence spectrograph that measures the solar EUV irradiance in the 5 to 37 nm range with 0.1-nm resolution, and the MEGS-B is a normal-incidence, dual-pass spectrograph that measures the solar EUV irradiance in the 35 to 105 nm range with 0.1-nm resolution. To provide MEGS in-flight calibration, the EUV SpectroPhotometer (ESP) measures the solar EUV irradiance in broadbands between 0.1 and 39 nm, and a MEGS-Photometer measures the Sun's bright hydrogen emission at 121.6 nm. The EVE data products include a near real-time space-weather product (Level 0C), which provides the solar EUV irradiance in specific bands and also spectra in 0.1-nm intervals with a cadence of one minute and with a time delay of less than 15 minutes. The EVE higher-level products are Level 2 with the solar EUV irradiance at higher time cadence (0.25 seconds for photometers and ten seconds for spectrographs) and Level 3 with averages of the solar irradiance over a day and over each one-hour period. The EVE team also plans to advance existing models of solar EUV irradiance and to operationally use the EVE measurements in models of Earth's ionosphere and thermosphere. Improved understanding of the evolution of solar flares and extending the various models to incorporate solar flare events are high priorities for the EVE team. C1 [Woods, T. N.; Eparvier, F. G.; Hock, R.; Jones, A. R.; Woodraska, D.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Judge, D.; Didkovsky, L.] Univ So Calif, Ctr Space Sci, Los Angeles, CA 90089 USA. [Lean, J.; Mariska, J.; Warren, H.] USN, Res Lab, Washington, DC 20375 USA. [McMullin, D.] Space Syst Res Corp, Alexandria, VA 22314 USA. [Chamberlin, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Berthiaume, G.] MIT, Lincoln Lab, Lexington, MA 02420 USA. [Bailey, S.] Virginia Tech, Dept Elect & Comp Engn, Blacksburg, VA 24061 USA. [Fuller-Rowell, T.] Univ Colorado, CIRES, Boulder, CO 80305 USA. [Fuller-Rowell, T.; Viereck, R.] NOAA, Space Weather Predict Ctr, Boulder, CO 80305 USA. [Sojka, J.] Utah State Univ, Ctr Atmospher & Space Sci, Logan, UT 84322 USA. [Tobiska, W. K.] Space Environm Technol, Pacific Palisades, CA 90272 USA. RP Woods, TN (reprint author), Univ Colorado, Atmospher & Space Phys Lab, 1234 Innovat Dr, Boulder, CO 80303 USA. EM tom.woods@lasp.colorado.edu RI Chamberlin, Phillip/C-9531-2012; OI Chamberlin, Phillip/0000-0003-4372-7405; Lean, Judith/0000-0002-0087-9639 FU NASA [NAS5-02140] FX This research is supported by NASA contract NAS5-02140 to the University of Colorado. The authors gratefully acknowledge the many people who have contributed to the success of this new instrument throughout concept, design, fabrication, and testing. Special thanks to Vanessa George for her support in preparing this manuscript. NR 67 TC 150 Z9 150 U1 3 U2 23 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 JAN PY 2012 VL 275 IS 1-2 BP 115 EP 143 DI 10.1007/s11207-009-9487-6 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YT UT WOS:000299294600007 ER PT J AU Hock, RA Chamberlin, PC Woods, TN Crotser, D Eparvier, FG Woodraska, DL Woods, EC AF Hock, R. A. Chamberlin, P. C. Woods, T. N. Crotser, D. Eparvier, F. G. Woodraska, D. L. Woods, E. C. TI Extreme Ultraviolet Variability Experiment (EVE) Multiple EUV Grating Spectrographs (MEGS): Radiometric Calibrations and Results SO SOLAR PHYSICS LA English DT Article DE SDO; EVE; Solar EUV irradiance; Calibration; Synchrotron ID PHOTOMETER SYSTEM XPS; IRRADIANCE; DESIGN AB The NASA Solar Dynamics Observatory (SDO), scheduled for launch in early 2010, incorporates a suite of instruments including the Extreme Ultraviolet Variability Experiment (EVE). EVE has multiple instruments including the Multiple Extreme ultraviolet Grating Spectrographs (MEGS) A, B, and P instruments, the Solar Aspect Monitor (SAM), and the Extreme ultraviolet SpectroPhotometer (ESP). The radiometric calibration of EVE, necessary to convert the instrument counts to physical units, was performed at the National Institute of Standards and Technology (NIST) Synchrotron Ultraviolet Radiation Facility (SURF III) located in Gaithersburg, Maryland. This paper presents the results and derived accuracy of this radiometric calibration for the MEGS A, B, P, and SAM instruments, while the calibration of the ESP instrument is addressed by Didkovsky et al. (Solar Phys., 2010, doi:10.1007/s11207-009-9485-8). In addition, solar measurements that were taken on 14 April 2008, during the NASA 36.240 sounding-rocket flight, are shown for the prototype EVE instruments. C1 [Hock, R. A.; Woods, T. N.; Crotser, D.; Eparvier, F. G.; Woodraska, D. L.] Lab Atmospher & Space Phys, Boulder, CO 80303 USA. [Chamberlin, P. C.] NASA, Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Woods, E. C.] Rhodes Coll, Memphis, TN 38112 USA. RP Hock, RA (reprint author), Lab Atmospher & Space Phys, 1234 Innovat Dr, Boulder, CO 80303 USA. EM rachel.hock@lasp.colorado.edu RI Chamberlin, Phillip/C-9531-2012 OI Chamberlin, Phillip/0000-0003-4372-7405 FU NASA [NAS5-02140] FX The authors would like to express their appreciation to Mitch Furst and the staff at NIST SURF III for all of their help throughout this calibration process, and special thanks go to Mitch Furst for reviewing this paper. We would also like to thank the many dedicated LASP scientists and engineers who designed and built EVE, and the many who also spent many weeks at the NIST calibration facility to obtain these calibration results. We also express special thanks to Vanessa George at LASP for supporting the preparation of this manuscript. We thank the referee for their helpful comments and suggestions. The solar irradiance results from 14 April 2008 can be obtained from the LASP Interactive Solar Irradiance Datacenter (LISIRD, http://lasp.colorado.edu/lisird). The EIT image is from the SOHO/EIT Consortium; SOHO is a joint ESA and NASA program. This research is supported by NASA contract NAS5-02140. NR 20 TC 22 Z9 22 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JAN PY 2012 VL 275 IS 1-2 BP 145 EP 178 DI 10.1007/s11207-010-9520-9 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YT UT WOS:000299294600008 ER PT J AU Scherrer, PH Schou, J Bush, RI Kosovichev, AG Bogart, RS Hoeksema, JT Liu, Y Duvall, TL Zhao, J Title, AM Schrijver, CJ Tarbell, TD Tomczyk, S AF Scherrer, P. H. Schou, J. Bush, R. I. Kosovichev, A. G. Bogart, R. S. Hoeksema, J. T. Liu, Y. Duvall, T. L., Jr. Zhao, J. Title, A. M. Schrijver, C. J. Tarbell, T. D. Tomczyk, S. TI The Helioseismic and Magnetic Imager (HMI) Investigation for the Solar Dynamics Observatory (SDO) SO SOLAR PHYSICS LA English DT Article DE Solar Dynamics Observatory; Helioseismology; Instrumentation and data management; Magnetic fields, photosphere ID TIME-DISTANCE HELIOSEISMOLOGY; MICHELSON DOPPLER IMAGER; FIELD; SUN; RECONSTRUCTION; AMBIGUITY; EMERGENCE; SUNSPOT; TESTS AB The Helioseismic and Magnetic Imager (HMI) instrument and investigation as a part of the NASA Solar Dynamics Observatory (SDO) is designed to study convection-zone dynamics and the solar dynamo, the origin and evolution of sunspots, active regions, and complexes of activity, the sources and drivers of solar magnetic activity and disturbances, links between the internal processes and dynamics of the corona and heliosphere, and precursors of solar disturbances for space-weather forecasts. A brief overview of the instrument, investigation objectives, and standard data products is presented. C1 [Scherrer, P. H.; Schou, J.; Bush, R. I.; Kosovichev, A. G.; Bogart, R. S.; Hoeksema, J. T.; Liu, Y.; Zhao, J.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Duvall, T. L., Jr.] NASA, Astron & Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Title, A. M.; Schrijver, C. J.; Tarbell, T. D.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Tomczyk, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80301 USA. RP Scherrer, PH (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. EM pscherrer@solar.stanford.edu RI Duvall, Thomas/C-9998-2012; Zhao, Junwei/A-1177-2007 FU NASA [NAS5-02139, NNG05GM85G, NNG06GE40G, NNX07AP61G, NNX09AB10G, NNX09AG81G, NNX10AC55G] FX The HMI project is supported by NASA contract NAS5-02139. Efforts to develop science analysis code for the pipeline have been supported by NASA grants NNG05GM85G, NNG06GE40G, NNX07AP61G, NNX09AB10G, NNX09AG81G, and NNX10AC55G. We wish to thank Elizabeth Citrin the NASA SDO Program Manager, Barbara Thompson and Dean Pesnell the SDO project scientists, Madhulika Guhathakurta the NASA LWS program scientist, Arthur Poland, George Withbroe, and Richard Fisher at NASA Headquarters for both formative and continuing support. NR 49 TC 471 Z9 474 U1 5 U2 18 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 JAN PY 2012 VL 275 IS 1-2 BP 207 EP 227 DI 10.1007/s11207-011-9834-2 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YT UT WOS:000299294600010 ER PT J AU Schou, J Scherrer, PH Bush, RI Wachter, R Couvidat, S Rabello-Soares, MC Bogart, RS Hoeksema, JT Liu, Y Duvall, TL Akin, DJ Allard, BA Miles, JW Rairden, R Shine, RA Tarbell, TD Title, AM Wolfson, CJ Elmore, DF Norton, AA Tomczyk, S AF Schou, J. Scherrer, P. H. Bush, R. I. Wachter, R. Couvidat, S. Rabello-Soares, M. C. Bogart, R. S. Hoeksema, J. T. Liu, Y. Duvall, T. L., Jr. Akin, D. J. Allard, B. A. Miles, J. W. Rairden, R. Shine, R. A. Tarbell, T. D. Title, A. M. Wolfson, C. J. Elmore, D. F. Norton, A. A. Tomczyk, S. TI Design and Ground Calibration of the Helioseismic and Magnetic Imager (HMI) Instrument on the Solar Dynamics Observatory (SDO) SO SOLAR PHYSICS LA English DT Article DE Solar Dynamics Observatory; Helioseismology, observations; Instrumentation and data management; Magnetic fields, photosphere AB The Helioseismic and Magnetic Imager (HMI) investigation (Solar Phys. doi:10.1007/s11207-011-9834-2, 2011) will study the solar interior using helioseismic techniques as well as the magnetic field near the solar surface. The HMI instrument is part of the Solar Dynamics Observatory (SDO) that was launched on 11 February 2010. The instrument is designed to measure the Doppler shift, intensity, and vector magnetic field at the solar photosphere using the 6173 angstrom Fe I absorption line. The instrument consists of a front-window filter, a telescope, a set of waveplates for polarimetry, an image-stabilization system, a blocking filter, a five-stage Lyot filter with one tunable element, two wide-field tunable Michelson interferometers, a pair of 4096(2) pixel cameras with independent shutters, and associated electronics. Each camera takes a full-disk image roughly every 3.75 seconds giving an overall cadence of 45 seconds for the Doppler, intensity, and line-of-sight magnetic-field measurements and a slower cadence for the full vector magnetic field. This article describes the design of the HMI instrument and provides an overview of the pre-launch calibration efforts. Overviews of the investigation, details of the calibrations, data handling, and the science analysis are provided in accompanying articles. C1 [Schou, J.; Scherrer, P. H.; Bush, R. I.; Wachter, R.; Couvidat, S.; Rabello-Soares, M. C.; Bogart, R. S.; Hoeksema, J. T.; Liu, Y.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. [Akin, D. J.; Allard, B. A.; Miles, J. W.; Rairden, R.; Shine, R. A.; Tarbell, T. D.; Title, A. M.; Wolfson, C. J.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Miles, J. W.] NASA, USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Elmore, D. F.; Norton, A. A.; Tomczyk, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80301 USA. RP Schou, J (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. EM schou@sun.stanford.edu RI Duvall, Thomas/C-9998-2012; Rabello Soares, Maria Cristina/C-3207-2013; OI Rabello Soares, Maria Cristina/0000-0003-0172-3713 FU NASA [NAS5-02139] FX A large number of people in the Stanford Solar Physics group provided invaluable help during the design and test of the instrument, including: Jim Aloise, Art Amezcua, John Beck, Keh-Cheng Chu, Carl Cimilluca, Romeo Durscher, Sarah Gregory, Tim Larson, Kim Ross, Jeneen Sommers, and Hao Thai. We would also like to thank Robert Byer, Carsten Langrock, Joe Schaar, and Karel Urbanek at Stanford's Ginzton Laboratory for help with designing and assembling the tunable solid-state laser. At LMSAL a large number of engineers and other personnel helped with design and test, including Ron Baraze, Jerry Drake, Dexter Duncan, Jay Dusenbury, Chris Edwards, Barbara Fischer, Glen Gradwohl, Gary Heyman, Noah Katz, Dwana Kacensky, Dave Kirkpatrick, Gary Kushner, Russ Lindgren, Gary Linford, Dnyanesh Mathur, Edward McFeaters, Keith Mitchell, Rose Navarro, Tom Nichols, Roger Rehse, J.-P. Riley, Larry Springer, Bob Stern, Louie Tavarez, Edgar Thomas, Darrel Torgerson, Ross Yamamoto, Carl Yanari, and Kent Zickhur. We also thank Tom Anderson, Lisa Bartusek, Michael Bay, Liz Citrin, Peter Gonzales, Juli Lander, Eliane Larduinat, Wendy Morgenstern, Dean Pesnell, Chad Salo, Mike Scott, and Barbara Thompson at GSFC, Juan Manuel Borrero, Greg Card, Rebecca Centeno, Tony Darnell, and Bruce Lites at HAO, KD Leka at NWRA/CORA, Matthew Clapp, Sarah Dunkin, and Nick Waltham at RAL, Gary Auker and Rob Wilson at E2V, John Hunter, Ian Miller, and Jeff Wimperis at LightMachinery, and Gerard Gleeson at ASO. Finally we would like to thank Jack Harvey for useful comments and advice. This work was supported by NASA contract NAS5-02139 to Stanford University. The HMI data used are courtesy of NASA/SDO and the HMI science team. NR 9 TC 521 Z9 529 U1 5 U2 24 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JAN PY 2012 VL 275 IS 1-2 BP 229 EP 259 DI 10.1007/s11207-011-9842-2 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YT UT WOS:000299294600011 ER PT J AU Wachter, R Schou, J Rabello-Soares, MC Miles, JW Duvall, TL Bush, RI AF Wachter, R. Schou, J. Rabello-Soares, M. C. Miles, J. W. Duvall, T. L., Jr. Bush, R. I. TI Image Quality of the Helioseismic and Magnetic Imager (HMI) Onboard the Solar Dynamics Observatory (SDO) SO SOLAR PHYSICS LA English DT Article DE Helioseismology, observations; Instrumental effects; Solar Dynamics Observatory AB We describe the imaging quality of the Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO) as measured during the ground calibration of the instrument. We describe the calibration techniques and report our results for the final configuration of HMI. We present the distortion, modulation transfer function, stray light, image shifts introduced by moving parts of the instrument, best focus, field curvature, and the relative alignment of the two cameras. We investigate the gain and linearity of the cameras, and present the measured flat field. C1 [Wachter, R.; Schou, J.; Rabello-Soares, M. C.; Bush, R. I.] Stanford Univ, Stanford, CA 94305 USA. [Miles, J. W.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA. [Miles, J. W.] NASA, SOFIA USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Duvall, T. L., Jr.] NASA, Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wachter, R (reprint author), Stanford Univ, Stanford, CA 94305 USA. EM richard@sun.stanford.edu RI Duvall, Thomas/C-9998-2012; Rabello Soares, Maria Cristina/C-3207-2013; OI Rabello Soares, Maria Cristina/0000-0003-0172-3713 FU NASA [NAS5-02139]; LMATC; GSFC; ASO FX This work has been supported by the NASA grant NAS5-02139 (HMI). Many people were involved in the calibration efforts for the instrument. We thank staff members at LMATC, GSFC, and ASO for their support. In particular, we thank Dave Kirkpatrick, Darrel Torgerson, Bob Stern, and Brett Allard. We also thank Phil Scherrer, Ted Tarbell, and Alan Title for their input. NR 11 TC 30 Z9 30 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JAN PY 2012 VL 275 IS 1-2 BP 261 EP 284 DI 10.1007/s11207-011-9709-6 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YT UT WOS:000299294600012 ER PT J AU Couvidat, S Schou, J Shine, RA Bush, RI Miles, JW Scherrer, PH Rairden, RL AF Couvidat, Sebastien Schou, Jesper Shine, Richard A. Bush, Rock I. Miles, John W. Scherrer, Philip H. Rairden, Richard L. TI Wavelength Dependence of the Helioseismic and Magnetic Imager (HMI) Instrument onboard the Solar Dynamics Observatory (SDO) SO SOLAR PHYSICS LA English DT Article DE Sun: helioseismology; Instrument: SDO/HMI ID BIREFRINGENT FILTERS; LINE ASYMMETRIES; IMPROVEMENTS; SHIFTS AB The Helioseismic and Magnetic Imager (HMI) instrument will produce Doppler-velocity and vector-magnetic-field maps of the solar surface, whose accuracy is dependent on a thorough knowledge of the transmission profiles of the components of the HMI optical-filter system. Here we present a series of wavelength-dependence calibration tests, performed on the instrument from 2005 onwards, to obtain these profiles. We obtained the transmittances as a function of wavelength for the tunable and non-tunable filter elements, as well as the variation of these transmittances with temperature and the angle of incidence of rays of light. We also established the presence of fringe patterns produced by interferences inside the blocking filter and the front window, as well as a change in transmitted intensity with the tuning position. This thorough characterization of the HMI-filter system confirmed the very high quality of the instrument, and showed that its properties are well within the required specifications to produce superior data with high spatial and temporal resolution. C1 [Couvidat, Sebastien; Schou, Jesper; Shine, Richard A.; Scherrer, Philip H.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Shine, Richard A.; Rairden, Richard L.] Lockheed Martin Solar & Astrophys Lab, Org ADBS, Palo Alto, CA 94304 USA. [Miles, John W.] NASA, USRA SOFIA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Couvidat, S (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, 491 S Serv Rd, Stanford, CA 94305 USA. EM couvidat@stanford.edu FU NASA [NAS5-02139] FX This work was supported by NASA Grant NAS5-02139 (HMI). We thank the HMI team members for their hard work, A. Title for providing us with notes regarding Jones calculus applied to the Lyot elements, and R. K. Ulrich for providing us with profiles of the solar Fe I line at 6173 angstrom. The HMI project is grateful to Karel Urbanek, Carsten Langrock, Joe Schaar and Robert Byer at Stanford University's Ginzton Laboratory for designing and building the tunable solid-state laser. We also thank Todd Hoeksema, Brett Allard, and countless others at LMSAL for their help with the taking of the calibration data. Finally, we acknowledge the comments of the anonymous referee for improving the quality of this article. NR 12 TC 25 Z9 25 U1 1 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 JAN PY 2012 VL 275 IS 1-2 BP 285 EP 325 DI 10.1007/s11207-011-9723-8 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YT UT WOS:000299294600013 ER PT J AU Couvidat, S Zhao, J Birch, AC Kosovichev, AG Duvall, TL Parchevsky, K Scherrer, PH AF Couvidat, S. Zhao, J. Birch, A. C. Kosovichev, A. G. Duvall, T. L., Jr. Parchevsky, K. Scherrer, P. H. TI Implementation and Comparison of Acoustic Travel-Time Measurement Procedures for the Solar Dynamics Observatory/Helioseismic and Magnetic Imager Time-Distance Helioseismology Pipeline SO SOLAR PHYSICS LA English DT Article DE Sun: helioseismology; Sun: time-distance analysis; HMI ID SOUND-SPEED; FLOWS; SENSITIVITY; TOMOGRAPHY; INVERSION; SUNSPOT AB The Helioseismic and Magnetic Imager (HMI) instrument onboard the Solar Dynamics Observatory (SDO) satellite is designed to produce high-resolution Doppler-velocity maps of oscillations at the solar surface with high temporal cadence. To take advantage of these high-quality oscillation data, a time - distance helioseismology pipeline (Zhao et al., Solar Phys. submitted, 2010) has been implemented at the Joint Science Operations Center (JSOC) at Stanford University. The aim of this pipeline is to generate maps of acoustic travel times from oscillations on the solar surface, and to infer subsurface 3D flow velocities and sound-speed perturbations. The wave travel times are measured from cross-covariances of the observed solar oscillation signals. For implementation into the pipeline we have investigated three different travel-time definitions developed in time - distance helioseismology: a Gabor-wavelet fitting (Kosovichev and Duvall, SCORE'96: Solar Convection and Oscillations and Their Relationship, ASSL, Dordrecht, 241, 1997), a minimization relative to a reference cross-covariance function (Gizon and Birch, Astrophys. J. 571, 966, 2002), and a linearized version of the minimization method (Gizon and Birch, Astrophys. J. 614, 472, 2004). Using Doppler-velocity data from the Michelson Doppler Imager (MDI) instrument onboard SOHO, we tested and compared these definitions for the mean and difference travel-time perturbations measured from reciprocal signals. Although all three procedures return similar travel times in a quiet-Sun region, the method of Gizon and Birch (Astrophys. J. 614, 472, 2004) gives travel times that are significantly different from the others in a magnetic (active) region. Thus, for the pipeline implementation we chose the procedures of Kosovichev and Duvall (SCORE'96: Solar Convection and Oscillations and Their Relationship, ASSL, Dordrecht, 241, 1997) and Gizon and Birch (Astrophys. J. 571, 966, 2002). We investigated the relationships among these three travel-time definitions, their sensitivities to fitting parameters, and estimated the random errors that they produce. C1 [Couvidat, S.; Zhao, J.; Kosovichev, A. G.; Parchevsky, K.; Scherrer, P. H.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Birch, A. C.] NW Res Associates, CoRA Div, Boulder, CO 80301 USA. [Duvall, T. L., Jr.] NASA, Solar Phys Lab, GSFC, Greenbelt, MD 20771 USA. RP Couvidat, S (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, 491 S Serv Rd, Stanford, CA 94305 USA. EM couvidat@stanford.edu RI Zhao, Junwei/A-1177-2007; Duvall, Thomas/C-9998-2012 FU NASA [NAS5-02139] FX This work was supported by NASA grant NAS5-02139 (HMI). The authors thank Laurent Gizon for suggesting a way of using the Gizon and Birch (2002, 2004) definitions in an active region, and for providing us with a MDI data cube of the quiet Sun. NR 25 TC 13 Z9 13 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JAN PY 2012 VL 275 IS 1-2 BP 357 EP 374 DI 10.1007/s11207-010-9652-y PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YT UT WOS:000299294600015 ER PT J AU Zhao, J Couvidat, S Bogart, RS Parchevsky, KV Birch, AC Duvall, TL Beck, JG Kosovichev, AG Scherrer, PH AF Zhao, J. Couvidat, S. Bogart, R. S. Parchevsky, K. V. Birch, A. C. Duvall, T. L., Jr. Beck, J. G. Kosovichev, A. G. Scherrer, P. H. TI Time-Distance Helioseismology Data-Analysis Pipeline for Helioseismic and Magnetic Imager Onboard Solar Dynamics Observatory (SDO/HMI) and Its Initial Results SO SOLAR PHYSICS LA English DT Article DE Sun: helioseismology; Sun: oscillations; Sun: SDO ID MICHELSON DOPPLER IMAGER; EMERGING ACTIVE-REGION; TRAVEL-TIMES; 3-DIMENSIONAL INVERSION; REALISTIC SIMULATIONS; LOCAL HELIOSEISMOLOGY; ACOUSTIC SHOWERGLASS; SENSITIVITY KERNELS; MERIDIONAL FLOWS; SOUND-SPEED AB The Helioseismic and Magnetic Imager onboard the Solar Dynamics Observatory (SDO/HMI) provides continuous full-disk observations of solar oscillations. We develop a data-analysis pipeline based on the time-distance helioseismology method to measure acoustic travel times using HMI Doppler-shift observations, and infer solar interior properties by inverting these measurements. The pipeline is used for routine production of near-real-time full-disk maps of subsurface wave-speed perturbations and horizontal flow velocities for depths ranging from 0 to 20 Mm, every eight hours. In addition, Carrington synoptic maps for the subsurface properties are made from these full-disk maps. The pipeline can also be used for selected target areas and time periods. We explain details of the pipeline organization and procedures, including processing of the HMI Doppler observations, measurements of the travel times, inversions, and constructions of the full-disk and synoptic maps. Some initial results from the pipeline, including full-disk flow maps, sunspot subsurface flow fields, and the interior rotation and meridional flow speeds, are presented. C1 [Zhao, J.; Couvidat, S.; Bogart, R. S.; Parchevsky, K. V.; Beck, J. G.; Kosovichev, A. G.; Scherrer, P. H.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Birch, A. C.] NW Res Associates, CoRA Div, Boulder, CO 80301 USA. [Duvall, T. L., Jr.] NASA, Astron & Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zhao, J (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. EM junwei@sun.stanford.edu RI Duvall, Thomas/C-9998-2012; Zhao, Junwei/A-1177-2007 NR 55 TC 25 Z9 25 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 JAN PY 2012 VL 275 IS 1-2 BP 375 EP 390 DI 10.1007/s11207-011-9757-y PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YT UT WOS:000299294600016 ER PT J AU Drobnes, E Littleton, A Pesnell, WD Beck, K Buhr, S Durscher, R Hill, S McCaffrey, M McKenzie, DE Myers, D Scherrer, D Wawro, M Wolt, A AF Drobnes, E. Littleton, A. Pesnell, W. D. Beck, K. Buhr, S. Durscher, R. Hill, S. McCaffrey, M. McKenzie, D. E. Myers, D. Scherrer, D. Wawro, M. Wolt, A. TI The Solar Dynamics Observatory (SDO) Education and Outreach (E/PO) Program: Changing Perceptions One Program at a Time SO SOLAR PHYSICS LA English DT Article DE Solar dynamics observatory; Education and public outreach AB We outline the context and overall philosophy for the combined Solar Dynamics Observatory (SDO) Education and Public Outreach (E/PO) program, present a brief overview of all SDO E/PO programs along with more detailed highlights of a few key programs, followed by a review of our results to date, conclude a summary of the successes, failures, and lessons learned, which future missions can use as a guide, while incorporating their own content to enhance the public's knowledge and appreciation of science and technology as well as its benefit to society. C1 [Drobnes, E.; Littleton, A.; Myers, D.; Wawro, M.; Wolt, A.] ADNET Syst Inc, Greenbelt, MD 20771 USA. [Pesnell, W. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Buhr, S.; McCaffrey, M.] CIRES, Boulder, CO 80309 USA. [Beck, K.] Stanford Univ, Haas Ctr Publ Serv, Stanford, CA 94305 USA. [Hill, S.] RS Informat Syst, Lexington Pk, MD 20653 USA. [McKenzie, D. E.] Montana State Univ, Bozeman, MT 59717 USA. RP Drobnes, E (reprint author), ADNET Syst Inc, Greenbelt, MD 20771 USA. EM emilie.drobnes@nasa.gov RI Pesnell, William/D-1062-2012 OI Pesnell, William/0000-0002-8306-2500 FU Solar Dynamics Observatory; NASA [NNH08CD27C-ROSES, NNH09ZDA001N-EPOESS] FX This work was supported, in part, by the Solar Dynamics Observatory Project and NASA Grants NNH08CD27C-ROSES and NNH09ZDA001N-EPOESS. NR 15 TC 0 Z9 0 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JAN PY 2012 VL 275 IS 1-2 BP 391 EP 406 DI 10.1007/s11207-011-9917-0 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YT UT WOS:000299294600017 ER PT J AU Hannan, KM Driggers, WB Hanisko, DS Jones, LM Canning, AB AF Hannan, Kristin M. Driggers, William B., III Hanisko, David S. Jones, Lisa M. Canning, Amanda B. TI DISTRIBUTION OF THE NURSE SHARK, GINGLYMOSTOMA CIRRATUM, IN THE NORTHERN GULF OF MEXICO SO BULLETIN OF MARINE SCIENCE LA English DT Article ID EAST-COAST AB The distribution of nurse sharks, Ginglymostoma cirratum (Bonaterre, 1778), in the northern Gulf of Mexico was examined using fisheries-independent bottom longline data collected from 1995 to 2009. Results indicate that nurse sharks are most abundant in the eastern Gulf of Mexico and their occurrence is relatively rare west of the Mississippi River Delta. While the eastern Gulf of Mexico had significantly different abiotic characteristics than the central and western regions, it is hypothesized that nurse shark distribution in the Gulf of Mexico is most associated with hard bottom substrate. Most nurse sharks were captured in groups of two or more individuals, indicating this species frequently aggregates. Nurse sharks in the region likely aggregate in response to prey availability, rather than for predator avoidance or mating purposes. C1 [Hannan, Kristin M.; Driggers, William B., III; Hanisko, David S.; Jones, Lisa M.; Canning, Amanda B.] Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA. RP Hannan, KM (reprint author), Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39567 USA. EM kristin.hannan@noaa.gov NR 19 TC 1 Z9 2 U1 3 U2 9 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD JAN PY 2012 VL 88 IS 1 BP 73 EP 80 DI 10.5343/bms.2011.1033 PG 8 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 879TR UT WOS:000299355600007 ER PT J AU Stoner, AW Davis, MH Booker, CJ AF Stoner, Allan W. Davis, Martha H. Booker, Catherine J. TI NEGATIVE CONSEQUENCES OF ALLEE EFFECT ARE COMPOUNDED BY FISHING PRESSURE: COMPARISON OF QUEEN CONCH REPRODUCTION IN FISHING GROUNDS AND A MARINE PROTECTED AREA SO BULLETIN OF MARINE SCIENCE LA English DT Article ID COD GADUS-MORHUA; STROMBUS-GIGAS; POPULATION RECOVERY; TEMPORAL VARIATION; LARVAL PRODUCTION; MATURITY; STOCK; SIZE; AGE; SUSTAINABILITY AB Relationships between density of mature adults and mating frequency in queen conch (Strombus gigas Linnaeus, 1758) were observed at three sites in the central Bahamas including one no-take marine reserve (Exuma Gays Land and Sea Park) and two historically important fishing grounds (Berry Islands and Andros Island). No mating was observed in arty one count with density < 47 adults ha(-1), consistent with an earlier study suggesting a mate-finding Allee effect in queen conch. The unfished site had larger and older conch, and mating at that site increased rapidly with adult density, reaching an asymptote at 12%-14% of the population mating at highest density levels. Logistic modeling showed that a 90% probability of mating occurred at 100 adults ha(-1). Mating frequencies increased more slowly with density on the fishing grounds; asymptotic mating frequencies were 6.3% in the Berry Islands and just 2.3% at Andros Island. In contrast to the marine reserve, 90% probability of mating required 350 and 570 adults ha(-1) at Andros Island and the Berry Islands, respectively. Higher densities required for successful mating in the fished areas were associated with numerical dominance by small, thick-shelled adults. The small phenotype in adults appears to result from selectivity imposed by fishing pressure, and those adults had low mating frequencies, compounding the density effect on reproduction. Because releases of hatchery-reared queen conch have not been successful, preserving the integrity of spawner density and population structure will be critical for conch conservation. C1 [Stoner, Allan W.] NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. [Davis, Martha H.] Community Conch, Littleton, CO 80121 USA. [Booker, Catherine J.] Community Conch, Savannah, GA 31405 USA. RP Stoner, AW (reprint author), NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2030 S Marine Sci Dr, Newport, OR 97365 USA. EM Al.Stoner@noaa.gov FU NOAA (US Department of Commerce); Bahamas Department of Marine Resources (DMR); Bahamas National Trust; Nature Conservancy's Northern Caribbean Office; Community Conch FX This study was supported with funds and logistical assistance from the National Undersea Research Program of NOAA (US Department of Commerce), The Bahamas Department of Marine Resources (DMR), The Bahamas National Trust, The Nature Conservancy's Northern Caribbean Office, and Community Conch. DMR provided assistance from L Anderson and J Dillet, and a small boat for surveys in the Berry Islands and Andros Island. Exuma Gays diving was directed by M Ray-Culp, assisted by E Bartels, T Hall, L Hambrick, R Jones, C Kuiken, and N Mehta. H Bethel, A Davis, L Davis, and K Finalyson, A McLean, T Thompson, and A Vellacott assisted with diving in the Berry Islands and Andros Island. M Vandenrydt was critical as boat captain, chief engineer, and diver for the project in the Berry Islands and Andros Island. We are also grateful to a long list of community members and fishers at each of the sites who provided help with travel, logistics, and guidance on queen conch distribution. We thank RA Glazer who participated in extensive discussion on the subject of density-dependent reproduction and three anonymous reviewers who provided thoughtful criticism. NR 50 TC 17 Z9 17 U1 1 U2 38 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD JAN PY 2012 VL 88 IS 1 BP 89 EP 104 DI 10.5343/bms.2011.1044 PG 16 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 879TR UT WOS:000299355600009 ER PT J AU Zhou, SJ Qiu, J Hawick, K AF Zhou, Shujia Qiu, Judy Hawick, Kenneth TI Guest Editor's Introduction: Special Section on Challenges and Solutions in Multicore and Many-Core Computing SO CONCURRENCY AND COMPUTATION-PRACTICE & EXPERIENCE LA English DT Editorial Material C1 [Zhou, Shujia] NASA, Washington, DC 20546 USA. [Qiu, Judy] Indiana Univ, Bloomington, IN 47405 USA. [Hawick, Kenneth] Massey Univ, Palmerston North, New Zealand. RP Zhou, SJ (reprint author), NASA, Washington, DC 20546 USA. EM xqiu@indiana.edu RI Hawick, Ken/E-1609-2013 OI Hawick, Ken/0000-0002-2447-3940 NR 9 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1532-0626 J9 CONCURR COMP-PRACT E JI Concurr. Comput.-Pract. Exp. PD JAN PY 2012 VL 24 IS 1 SI SI BP 1 EP 2 DI 10.1002/cpe.1861 PG 2 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA 869GA UT WOS:000298584200001 ER PT J AU Zhou, SJ Cruz, C Duffy, D Tucker, R Purcell, M AF Zhou, Shujia Cruz, Carlos Duffy, Daniel Tucker, Robert Purcell, Mark TI Accelerating climate and weather simulations through hybrid computing SO CONCURRENCY AND COMPUTATION-PRACTICE & EXPERIENCE LA English DT Article DE acceleration; climate; weather; hybrid computing AB Unconventional multi- and many-core processors (e.g. IBM (R) Cell B.E. TM and NVIDIA (R) GPU) have emerged as effective accelerators in trial climate and weather simulations. Yet these climate and weather models typically run on parallel computers with conventional processors (e.g. Intel (R), AMD (R), and IBM) using Message Passing Interface. To address challenges involved in efficiently and easily connecting accelerators to parallel computers, we investigated using IBM's Dynamic Application Virtualization TM (IBM DAV) software in a prototype hybrid computing system with representative climate and weather model components. The hybrid system comprises two Intel blades and two IBM QS22 Cell B.E. blades, connected with both InfiniBand (R) (IB) and 1-Gigabit Ethernet. The system significantly accelerates a solar radiation model component by offloading compute-intensive calculations to the Cell blades. Systematic tests show that IBM DAV can seamlessly offload compute-intensive calculations from Intel blades to Cell B.E. blades in a scalable, load-balanced manner. However, noticeable communication overhead was observed, mainly due to IP over the IB protocol. Full utilization of IB Sockets Direct Protocol and the lower latency production version of IBM DAV will reduce this overhead. Copyright (C) 2011 John Wiley & Sons, Ltd. C1 [Zhou, Shujia; Cruz, Carlos; Duffy, Daniel] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tucker, Robert; Purcell, Mark] DSL, Damastown, Dublin, Ireland. RP Zhou, SJ (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM shujia.zhou@nasa.gov NR 12 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1532-0626 J9 CONCURR COMP-PRACT E JI Concurr. Comput.-Pract. Exp. PD JAN PY 2012 VL 24 IS 1 SI SI BP 54 EP 61 DI 10.1002/cpe.1729 PG 8 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA 869GA UT WOS:000298584200006 ER PT J AU Weis, JS Candelmo, A AF Weis, Judith S. Candelmo, Allison TI Pollutants and fish predator/prey behavior: A review of laboratory and field approaches SO CURRENT ZOOLOGY LA English DT Article DE Predator; Feeding; Prey; Pollution; Activity; Trophic ID MUMMICHOGS FUNDULUS-HETEROCLITUS; MINNOWS PIMEPHALES-PROMELAS; THE-YEAR BLUEFISH; TROUT ONCORHYNCHUS-MYKISS; PREY CAPTURE ABILITY; ZEBRAFISH DANIO-RERIO; FATHEAD MINNOWS; POMATOMUS-SALTATRIX; FEEDING-BEHAVIOR; RAINBOW-TROUT AB Fish behavior can be altered by contaminants. There is an extensive literature on laboratory behavioral assays, with many chemicals impairing feeding or predator avoidance. However, there is not extensive work on fishes that live in contaminated environments. Therefore, we then review our recent research on feeding and trophic relations of populations from contaminated estuaries compared with relatively unpolluted sites. The mummichog Fundulus heteroclitus, is a non-migratory fish; those from more contaminated areas are poor predators and slower to capture active prey (grass shrimp, Palaemonetes pugio). In the field, they consume much detritus and sediment, which is not nutritious. They are less active than fish from cleaner sites and more vulnerable to predation. They have altered thyroid glands and neurotransmitter levels, which may underlie altered behaviors. Fish from the reference site kept in tanks with sediment and food from the polluted site showed bioaccumulation and reduced prey capture after two months, although fish from the polluted site did not show significant improvement when maintained in a clean environment. Poor nutrition and predator avoidance may be responsible for their being smaller and having a shorter life span than reference fish. Bluefish Pomatomus saltatrix, are a marine species in which the young-of-the-year spend their first summer in estuaries. We found bioaccumulation of contaminants and reduced activity, schooling, and feeding in young-of-the-year bluefish from a relatively unpolluted site that were fed prey fish from a contaminated site. They also had altered thyroid glands and neurotransmitter levels. Many field-caught specimens had empty stomachs, which is rare in this species. In the fall, when they migrate back out to the ocean, they are smaller, slower, and more likely to starve or to be eaten than those that spent their summer in cleaner estuaries [Current Zoology 58 (1): 9-20, 2012]. C1 [Weis, Judith S.] Rutgers State Univ, Dept Biol Sci, Newark, NJ 07102 USA. [Candelmo, Allison] NOAA, Natl Marine Fisheries Serv, James Howard Lab, Highlands, NJ 07732 USA. RP Weis, JS (reprint author), Rutgers State Univ, Dept Biol Sci, Newark, NJ 07102 USA. EM jweis@andromeda.rutgers.edu FU NJ Sea Grant Program; NOAA; Rutgers University Marine Field Station (RUMFS); Meadowlands Environmental Research Institute (MERI) FX We appreciate the assistance of numerous undergraduate students and of the staff at the James Howard NOAA Laboratory at Sandy Hook New Jersey. We are grateful for the help of Dr. Peddrick Weis with thyroid histology. This research received funding from the NJ Sea Grant Program, the NOAA CMER Program, The Rutgers University Marine Field Station (RUMFS), and the Meadowlands Environmental Research Institute (MERI). NR 78 TC 21 Z9 22 U1 4 U2 38 PU CURRENT ZOOLOGY PI BEIJING PA CHINESE ACAD SCIENCES, INST ZOOLOGY, BEICHEN XILU, CHAOYANG DISTRICT, BEIJING, 100101, PEOPLES R CHINA SN 1674-5507 J9 CURR ZOOL JI Curr. Zool. PY 2012 VL 58 IS 1 BP 9 EP 20 PG 12 WC Zoology SC Zoology GA 877TA UT WOS:000299204400003 ER PT J AU Hackney, KJ Ploutz-Snyder, LL AF Hackney, K. J. Ploutz-Snyder, L. L. TI Unilateral lower limb suspension: integrative physiological knowledge from the past 20 years (1991-2011) SO EUROPEAN JOURNAL OF APPLIED PHYSIOLOGY LA English DT Review DE Disuse; Inactivity; Space flight analogs; Unweighting ID HUMAN SKELETAL-MUSCLE; HUMAN QUADRICEPS MUSCLE; DOWN BED REST; RESISTANCE EXERCISE; SIMULATED MICROGRAVITY; PROTEIN-SYNTHESIS; VISCOELASTIC PROPERTIES; TENDINOUS ADAPTATIONS; VASCULAR OCCLUSION; ACTION-POTENTIALS AB In 1991, Hans Berg and colleagues published the first research investigation using unilateral lower limb suspension (ULLS) as a human model to study the influence of unloading on skeletal muscle. ULLS requires a participant to perform all activities with axillary crutches while wearing one thick-soled shoe. The elevated shoe eliminates ground contact with the adjacent foot, thereby unloading the lower limb. Today, ULLS is a well-known ground-based analog for microgravity. The present review will synthesize the physiological findings from investigations using ULLS to study the deleterious effects of unloading. Compromised human performance and the neuromuscular, musculoskeletal and circulatory mechanisms leading to altered function will be a major emphasis of the work. Results from prolonged bed rest will also be included in order for general comparisons to be made between analogs. Finally, the efficacy of exercise to mitigate the negative consequences of unloading is presented. C1 [Hackney, K. J.; Ploutz-Snyder, L. L.] Syracuse Univ, Dept Exercise Sci, Syracuse, NY 13244 USA. [Hackney, K. J.; Ploutz-Snyder, L. L.] NASA, Johnson Space Ctr Exercise Physiol, Houston, TX USA. [Hackney, K. J.; Ploutz-Snyder, L. L.] NASA, Countermeasures Project, Houston, TX USA. [Ploutz-Snyder, L. L.] Univ Space Res Assoc, Houston, TX USA. RP Hackney, KJ (reprint author), Syracuse Univ, Dept Exercise Sci, Womens Bldg,Room 201, Syracuse, NY 13244 USA. EM kjhackne@syr.edu FU National Aeronautics and Space Administration [NNX08AW71H] FX We would like to thank Dr. Gregory Adams, University of California Irvine for reviewing the manuscript. We thank both the dedicated researchers and ULLS study participants for their commitment to scientific discovery. This work was partially supported by the National Aeronautics and Space Administration Graduate Student Research Program Training Grant (NNX08AW71H). NR 109 TC 22 Z9 22 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1439-6319 J9 EUR J APPL PHYSIOL JI Eur. J. Appl. Physiol. PD JAN PY 2012 VL 112 IS 1 BP 9 EP 22 DI 10.1007/s00421-011-1971-7 PG 14 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA 875AU UT WOS:000299002500002 PM 21533809 ER PT J AU Afsar, MZ AF Afsar, M. Z. TI Insight into the two-source structure of the jet noise spectrum using a generalized shell model of turbulence SO EUROPEAN JOURNAL OF MECHANICS B-FLUIDS LA English DT Article DE Jet noise; Turbulence; Shell models ID ISOTROPIC TURBULENCE; ANISOTROPIC TURBULENCE; SUPERSONIC JETS; GRID TURBULENCE; MIXING NOISE; ORDER; AEROACOUSTICS; NUMBER; FLOWS; HOT AB There is a large body of experimental evidence which shows that the jet noise spectrum is composed of two sources. Our aim here is to prove, mathematically, that the two-source paradigm can be derived using a minimum number of self-consistent approximations based on our current knowledge of jet turbulence in cold flows. The starting point of the paper is Goldstein's (2003) [20] exact re-arrangement of the Navier-Stokes equations, which shows that turbulence enters the acoustic spectrum formula through the Reynolds stress auto-covariance tensor. We extend the shell model of turbulence using a more general symmetry approximation that amounts to assuming that the Reynolds stress auto-covariance is, firstly, axi-symmetric, and secondly is equivalent to the same tensor only after it has been averaged (point-wise) over the azimuthal separation. As a consequence of these two assumptions, the space-time Fourier transform of the Reynolds stress auto-covariance (which we refer to as the spectral tensor) depends on the transverse wave vector only through the square of its magnitude and, moreover, is also an axi-symmetric tensor. This defines the generalized shell model (or GSM) and we apply it to the jet noise problem. The final result shows that the acoustic spectrum can be written as the sum of two groups of terms, one of which corresponds to the peak jet noise in the weakly non-parallel flow limit. Published by Elsevier Masson SAS. C1 [Afsar, M. Z.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Afsar, MZ (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA. EM mohammed.afsar@cantab.net FU Department of Applied Mathematics and Theoretical Physics, Cambridge, UK; Center for Turbulence Research at Stanford University, USA; NASA FX M.Z.A acknowledges the financial support of the David Crighton Fellowship from the Department of Applied Mathematics and Theoretical Physics, Cambridge, UK (2008); the Post-doctoral Fellowship from the Center for Turbulence Research at Stanford University, USA (2009) and the NASA Post-doctoral Program Fellowship (2010). He is grateful to Dr. S.J. Leib for pointing out the relations in Appendix B and would also like to thank the anonymous referee for making helpful suggestions to improve the paper. NR 71 TC 3 Z9 3 U1 0 U2 0 PU GAUTHIER-VILLARS/EDITIONS ELSEVIER PI PARIS PA 23 RUE LINOIS, 75015 PARIS, FRANCE SN 0997-7546 J9 EUR J MECH B-FLUID JI Eur. J. Mech. B-Fluids PD JAN-FEB PY 2012 VL 31 BP 129 EP 139 DI 10.1016/j.euromechflu.2011.06.002 PG 11 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 877PL UT WOS:000299194300010 ER PT J AU Galin, N Worby, A Markus, T Leuschen, C Gogineni, P AF Galin, Natalia Worby, Anthony Markus, Thorsten Leuschen, Carl Gogineni, Prasad TI Validation of Airborne FMCW Radar Measurements of Snow Thickness Over Sea Ice in Antarctica SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Airborne; Antarctica; frequency modulated continuous wave (FMCW); sea ice; snow ID DIELECTRIC-PROPERTIES; SIGNATURES; MODEL AB Antarctic sea ice and its snow cover are integral components of the global climate system, yet many aspects of their vertical dimensions are poorly understood, making their representation in global climate models poor. Remote sensing is the key to monitoring the dynamic nature of sea ice and its snow cover. Reliable and accurate snow thickness data are currently a highly sought after data product. Remotely sensed snow thickness measurements can provide an indication of precipitation levels, predicted to increase with effects of climate change in the polar regions. Airborne techniques provide a means for regional-scale estimation of snow depth and distribution. Accurate regional-scale snow thickness data will also facilitate an increase in the accuracy of sea ice thickness retrieval from satellite altimeter freeboard estimates. The airborne data sets are easier to validate with in situ measurements and are better suited to validating satellite algorithms when compared with in situ techniques. This is primarily due to two factors: better chance of getting coincident in situ and airborne data sets and the tractability of comparison between an in situ data set and the airborne data set averaged over the footprint of the antennas. A 2-8-GHz frequency modulated continuous wave (FMCW) radar loaned by the Center for Remote Sensing of Ice Sheets to the Australian Antarctic Division is used to measure snow thickness over sea ice in East Antarctica. Provided with the radar design parameters, the expected performance parameters of the radar are summarized. The necessary conditions for unambiguous identification of the air/snow and snow/ice layers for the radar are presented. Roughnesses of the snow and ice surfaces are found to be dominant determinants in the effectiveness of layer identification for this radar. Finally, this paper presents the first in situ validated snow thickness estimates over sea ice in Antarctica derived from an FMCW radar on a helicopterborne platform. C1 [Galin, Natalia] UCL, Ctr Polar Observat & Modelling, London WC1E 6BT, England. [Worby, Anthony] Australian Antarctic Div, Kingston, Tas 7050, Australia. [Markus, Thorsten] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. [Leuschen, Carl; Gogineni, Prasad] Univ Kansas, Lawrence, KS 66045 USA. RP Galin, N (reprint author), UCL, Ctr Polar Observat & Modelling, Mortimer St, London WC1E 6BT, England. EM n.galin@ucl.ac.uk; A.Worby@utas.edu.au; thorsten.markus@nasa.gov; leuschen@eecs.ku.edu; gogineni@cresis.ku.edu RI Markus, Thorsten/D-5365-2012 NR 36 TC 12 Z9 12 U1 0 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JAN PY 2012 VL 50 IS 1 BP 3 EP 12 DI 10.1109/TGRS.2011.2159121 PG 10 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 872BS UT WOS:000298782000001 ER PT J AU Amarin, RA Jones, WL El-Nimri, SF Johnson, JW Ruf, CS Miller, TL Uhlhorn, E AF Amarin, Ruba A. Jones, W. Linwood El-Nimri, Salem Fawwaz Johnson, James W. Ruf, Christopher S. Miller, Timothy L. Uhlhorn, Eric TI Hurricane Wind Speed Measurements in Rainy Conditions Using the Airborne Hurricane Imaging Radiometer (HIRAD) SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Hurricane imaging; hurricane imaging radiometer (HIRAD); hurricanes wind speed retrievals; synthetic aperture radiometry ID MICROWAVE RADIOMETER; OCEAN AB This paper describes a realistic computer simulation of airborne hurricane surveillance using the recently developed microwave remote sensor, the hurricane imaging radiometer (HIRAD). An end-to-end simulation is described of HIRAD wind speed and rain rate measurements during two hurricanes while flying on a high-altitude aircraft. This simulation addresses the particular challenge which is accurate hurricane wind speed measurements in the presence of intense rain rates. The objective of this research is to develop baseline retrieval algorithms and provide a wind speed measurement accuracy assessment for future hurricane flights including the NASA GRIP hurricane field program that was conducted in summer of 2010. Examples of retrieved hurricane wind speed and rain rate images are presented, and comparisons of the retrieved parameters with two different numerical hurricane models data are made. Special emphasis is provided on the wind speed measurement error, and statistical results are presented over a broad range of wind and rain conditions over the full measurement swath (earth incidence angle). C1 [Amarin, Ruba A.; Jones, W. Linwood; El-Nimri, Salem Fawwaz; Johnson, James W.] Univ Cent Florida, Orlando, FL 32816 USA. [Ruf, Christopher S.] Univ Michigan, Ann Arbor, MI 48109 USA. [Miller, Timothy L.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Uhlhorn, Eric] NOAA, AOML, Hurricane Res Div, Miami, FL 33149 USA. RP Amarin, RA (reprint author), Univ Cent Florida, Orlando, FL 32816 USA. EM ramarin@mail.ucf.edu; ljones@ucf.edu; selnimri@knights.ucf.edu; jwjohnson.8443@gmail.com; cruf@umich.edu; tim.miller@nasa.gov; eric.uhlhorn@noaa.gov RI Ruf, Christopher/I-9463-2012; Uhlhorn, Eric/B-1336-2014 OI Uhlhorn, Eric/0000-0002-4759-5342 FU NASA Marshall Space Flight Center; Von Braun Center for Science and Innovation; Von Braun Center for Science and Innovation, Huntsville, AL FX This work was supported by the HIRAD Project of the NASA Marshall Space Flight Center under a contract with the Von Braun Center for Science and Innovation.; This work was sponsored under Grants from the Von Braun Center for Science and Innovation, Huntsville, AL. NR 13 TC 7 Z9 7 U1 1 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JAN PY 2012 VL 50 IS 1 BP 180 EP 192 DI 10.1109/TGRS.2011.2161637 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 872BS UT WOS:000298782000015 ER PT J AU Taylor, TE O'Dell, CW O'Brien, DM Kikuchi, N Yokota, T Nakajima, TY Ishida, H Crisp, D Nakajima, T AF Taylor, Thomas E. O'Dell, Christopher W. O'Brien, Denis M. Kikuchi, Nobuyuki Yokota, Tatsuya Nakajima, Takashi Y. Ishida, Haruma Crisp, Dave Nakajima, Teruyuki TI Comparison of Cloud-Screening Methods Applied to GOSAT Near-Infrared Spectra SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Atmospheric measurements; clouds; remote sensing ID RADIATIVE-TRANSFER MODEL; THIN CIRRUS CLOUDS; PART I; SCATTERING ATMOSPHERE; MODIS; PERFORMANCE; TERRA; BAND; CO2; SPECTROMETER AB Several existing and proposed satellite remote sensing instruments are designed to derive concentrations of trace gases, such as carbon dioxide (CO2) and methane (CH4), from measured spectra of reflected sunlight in absorption bands of the gases. Generally, these analyses require that the scenes be free of cloud and aerosol, necessitating robust screening algorithms. In this work, two cloud-screening algorithms are compared. One applies threshold tests, similar to those used by the MODerate resolution Imaging Spectrometer (MODIS), to visible and infrared reflectances measured by the Cloud and Aerosol Imager aboard the Greenhouse gases Observing SATellite (GOSAT). The second is a fast retrieval algorithm that operates on high-resolution spectra in the oxygen A-band measured by the Fourier Transform Spectrometer on GOSAT. Near-simultaneous cloud observations from the MODIS Aqua satellite are used for comparison. Results are expressed in terms of agreement and disagreement in the identification of clear and cloudy scenes for land and non-sun glint viewing over water. The accuracy, defined to be the fraction of scenes that are classified the same, is approximately 80% for both algorithms over land when comparing with MODIS. The accuracy rises to approximately 90% over ocean. Persistent difficulties with identifying cirrus clouds are shown to yield a large fraction of the disagreement with MODIS. C1 [Taylor, Thomas E.; O'Dell, Christopher W.; O'Brien, Denis M.] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. [Kikuchi, Nobuyuki; Yokota, Tatsuya] Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan. [Nakajima, Takashi Y.] Tokai Univ, Res & Informat Ctr, Tokyo 1510063, Japan. [Ishida, Haruma] Yamaguchi Univ, Dept Mech Engn, Ube, Yamaguchi 7558611, Japan. [Crisp, Dave] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nakajima, Teruyuki] Univ Tokyo, Ctr Climate Syst Res, Tokyo 1130033, Japan. RP Taylor, TE (reprint author), Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. RI Nakajima, Takashi/C-2747-2009; Nakajima, Teruyuki/H-2370-2013 OI Nakajima, Teruyuki/0000-0002-9042-504X FU Jet Propulsion Laboratory [1380533] FX The work of T. Taylor, C. O'Dell, and D. O'Brien were supported by the Jet Propulsion Laboratory under Contract 1380533. NR 41 TC 20 Z9 21 U1 1 U2 27 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JAN PY 2012 VL 50 IS 1 BP 295 EP 309 DI 10.1109/TGRS.2011.2160270 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 872BS UT WOS:000298782000024 ER PT J AU Meister, G Franz, BA Kwiatkowska, EJ McClain, CR AF Meister, Gerhard Franz, Bryan A. Kwiatkowska, Ewa J. McClain, Charles R. TI Corrections to the Calibration of MODIS Aqua Ocean Color Bands Derived From SeaWiFS Data SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Calibration; image sensors; remote sensing ID RESOLUTION IMAGING SPECTRORADIOMETER; AEROSOL OPTICAL-THICKNESS; POLARIZATION-SENSITIVITY; TERRA; WATER; PHYTOPLANKTON; RETRIEVAL; SENSORS AB The National Aeronautics and Space Administration ocean color products of Sea-viewing Wide Field-of-view Sensor (SeaWiFS) and Moderate Resolution Imaging Spectroradiometer (MODIS) Aqua have been reprocessed in 2009. This paper describes the changes to the calibration approach for MODIS Aqua. Due to a significant downward trend in the operational MODIS Aqua water-leaving radiances at 412 nm, the previous calibration approach was no longer sufficient. The new approach uses SeaWiFS water-leaving radiances to adjust the temporal trends of the radiometric calibration of MODIS Aqua bands at 412 and 443 nm. The adjustments to the temporal trends at the beginning of the scan are minor but are significant around nadir and at the end of scan (up to 5% at 412 nm and up to 1% for 443 nm). The remaining five bands (488 to 678 nm) are adjusted with regard to their scan-angle dependence only; no temporal correction is necessary. There is no indication that the sensor polarization sensitivity needs to be modified for MODIS Aqua. C1 [Meister, Gerhard; Franz, Bryan A.; Kwiatkowska, Ewa J.; McClain, Charles R.] NASA, Goddard Space Flight Ctr, Ocean Ecol Branch Code 614 2, Greenbelt, MD 20771 USA. RP Meister, G (reprint author), NASA, Goddard Space Flight Ctr, Ocean Ecol Branch Code 614 2, Code 661, Greenbelt, MD 20771 USA. EM Gerhard.Meister@nasa.gov RI Meister, Gerhard/F-7159-2012; Franz, Bryan/D-6284-2012 OI Franz, Bryan/0000-0003-0293-2082 NR 29 TC 32 Z9 32 U1 2 U2 9 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 JAN PY 2012 VL 50 IS 1 BP 310 EP 319 DI 10.1109/TGRS.2011.2160552 PG 10 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 872BS UT WOS:000298782000025 ER PT J AU Adler, RF Gu, GJ Huffman, GJ AF Adler, Robert F. Gu, Guojun Huffman, George J. TI Estimating Climatological Bias Errors for the Global Precipitation Climatology Project (GPCP) SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID GAUGE OBSERVATIONS; TRMM; PRODUCTS; RETRIEVALS AB A procedure is described to estimate bias errors for mean precipitation by using multiple estimates from different algorithms, satellite sources, and merged products. The Global Precipitation Climatology Project (GPCP) monthly product is used as a base precipitation estimate, with other input products included when they are within +/- 50% of the GPCP estimates on a zonal-mean basis (ocean and land separately). The standard deviation a of the included products is then taken to be the estimated systematic, or bias, error. The results allow one to examine monthly climatologies and the annual climatology, producing maps of estimated bias errors, zonal-mean errors, and estimated errors over large areas such as ocean and land for both the tropics and the globe. For ocean areas, where there is the largest question as to absolute magnitude of precipitation, the analysis shows spatial variations in the estimated bias errors, indicating areas where one should have more or less confidence in the mean precipitation estimates. In the tropics, relative bias error estimates (sigma/mu, where mu is the mean precipitation) over the eastern Pacific Ocean are as large as 20%, as compared with 10%-15% in the western Pacific part of the ITCZ. An examination of latitudinal differences over ocean clearly shows an increase in estimated bias error at higher latitudes, reaching up to 50%. Over land, the error estimates also locate regions of potential problems in the tropics and larger cold-season errors at high latitudes that are due to snow. An empirical technique to area average the gridded errors (sigma) is described that allows one to make error estimates for arbitrary areas and for the tropics and the globe (land and ocean separately, and combined). Over the tropics this calculation leads to a relative error estimate for tropical land and ocean combined of 7%, which is considered to be an upper bound because of the lack of sign-of-the-error canceling when integrating over different areas with a different number of input products. For the globe the calculated relative error estimate from this study is about 9%, which is also probably a slight overestimate. These tropical and global estimated bias errors provide one estimate of the current state of knowledge of the planet's mean precipitation. C1 [Adler, Robert F.; Gu, Guojun] Univ Maryland, ESSIC, College Pk, MD 20740 USA. [Gu, Guojun; Huffman, George J.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Huffman, George J.] Sci Syst & Applicat Inc, Greenbelt, MD USA. RP Adler, RF (reprint author), Univ Maryland, ESSIC, Ste 4001,5825 Univ Res Ct, College Pk, MD 20740 USA. EM radler@umd.edu RI Huffman, George/F-4494-2014 OI Huffman, George/0000-0003-3858-8308 FU NASA FX This research is supported under the NASA Energy and Water-Cycle Study (NEWS) program. NR 24 TC 46 Z9 46 U1 0 U2 27 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD JAN PY 2012 VL 51 IS 1 BP 84 EP 99 DI 10.1175/JAMC-D-11-052.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 880HE UT WOS:000299395100007 ER PT J AU Cullather, RI Bosilovich, MG AF Cullather, Richard I. Bosilovich, Michael G. TI The Energy Budget of the Polar Atmosphere in MERRA SO JOURNAL OF CLIMATE LA English DT Article ID IN-SITU; DATA ASSIMILATION; RADIATION BUDGET; EAST ANTARCTICA; ANNUAL CYCLE; HEAT-BUDGET; SURFACE; BALANCE; OCEAN; VARIABILITY AB Components of the atmospheric energy budget from the Modern-Era Retrospective Analysis for Research and Applications (MERRA) are evaluated in polar regions for the period 1979-2005 and compared with previous estimates, in situ observations, and contemporary reanalyses. Closure of the budget is reflected by the analysis increments term, which indicates an energy surplus of 11 W m(-2) over the North Polar cap (70 degrees-90 degrees N) and 22 W m(-2) over the South Polar cap (70 degrees-90 degrees S). Total atmospheric energy convergence from MERRA compares favorably with previous studies for northern high latitudes but exceeds the available previous estimate for the South Polar cap by 46%. Discrepancies with the Southern Hemisphere energy transport are largest in autumn and may be related to differences in topography with earlier reanalyses. For the Arctic; differences between MERRA and other sources in top of atmosphere (TOA) and surface radiative fluxes are largest in May. These differences are concurrent with the largest discrepancies between MERRA parameterized and observed surface albedo. For May, in situ observations of the upwelling shortwave flux in the Arctic are 80 W m(-2) larger than MERRA, while the MERRA downwelling longwave flux is underestimated by 12 W m(-2) throughout the year. Over grounded ice sheets, the annual mean net surface energy flux in MERRA is erroneously nonzero. Contemporary reanalyses from the Climate Forecast Center (CFSR) and the Interim Re-Analyses of the European Centre for Medium-Range Weather Forecasts (ERA-I) are found to have better surface parameterizations; however, these reanalyses also disagree with observed surface and TOA energy fluxes. Discrepancies among available reanalyses underscore the challenge of reproducing credible estimates of the atmospheric energy budget in polar regions. C1 [Cullather, Richard I.; Bosilovich, Michael G.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Cullather, Richard I.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Cullather, RI (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, GSFC Code 610-1,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM richard.cullather@nasa.gov RI Bosilovich, Michael/F-8175-2012 FU NASA; NASA Energy and Water Cycle Study (NEWS) FX Data from the Surface Heat Budget of the Arctic Ocean experiment (SHEBA) were obtained from the University of Washington Department of Atmospheric Sciences, Seattle, Washington. Reference Antarctic Data for Environmental Research (READER) is a project of the Scientific Committee on Antarctic Research (SCAR) and were obtained from British Antarctic Survey (BAS), Cambridge, United Kingdom. Arctic station values from the Integrated Surface Database (ISD) and the Integrated Rawinsonde Global Rawinsonde Archive (IGRA) were obtained from the National Climate Data Center, Asheville, North Carolina. The ERA-I was obtained from the Data Support Section at the National Center for Atmospheric Research. The CFSR was obtained from the National Climate Data Center. This study was funded by grants from the NASA Modeling Analysis and Prediction Program (MAP) and the NASA Energy and Water Cycle Study (NEWS) to the second author. NR 56 TC 31 Z9 32 U1 1 U2 15 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD JAN PY 2012 VL 25 IS 1 BP 5 EP 24 DI 10.1175/2011JCLI4138.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 876TG UT WOS:000299130000002 ER PT J AU Braun, SA Sippel, JA Nolan, DS AF Braun, Scott A. Sippel, Jason A. Nolan, David S. TI The Impact of Dry Midlevel Air on Hurricane Intensity in Idealized Simulations with No Mean Flow SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID PLANETARY BOUNDARY-LAYER; TROPICAL CYCLONE FORMATION; WAVE CRITICAL LAYER; OBSERVATIONAL ANALYSIS; EASTERLY WAVES; PART I; CYCLOGENESIS; MODEL; ATLANTIC; PARAMETERIZATION AB This study examines the potential negative influences of dry midlevel air on the development of tropical cyclones (specifically, its role in enhancing cold downdraft activity and suppressing storm development). The Weather Research and Forecasting model is used to construct two sets of idealized simulations of hurricane development in environments with different configurations of dry air. The first set of simulations begins with dry air located north of the vortex center by distances ranging from 0 to 270 km, whereas the second set of simulations begins with dry air completely surrounding the vortex, but with moist envelopes in the vortex core ranging in size from 0 to 150 km in radius. No impact of the dry air is seen for dry layers located more than 270 km north of the initial vortex center (similar to 3 times the initial radius of maximum wind). When the dry air is initially closer to the vortex center, it suppresses convective development where it entrains into the storm circulation, leading to increasingly asymmetric convection and slower storm development. The presence of dry air throughout the domain, including the vortex center, substantially slows storm development. However, the presence of a moist envelope around the vortex center eliminates the deleterious impact on storm intensity. Instead, storm size is significantly reduced. The simulations suggest that dry air slows intensification only when it is located very close to the vortex core at early times. When it does slow storm development, it does so primarily by inducing outward-moving convective asymmetries that temporarily shift latent heating radially outward away from the high-vorticity inner core. C1 [Braun, Scott A.; Sippel, Jason A.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Nolan, David S.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. RP Braun, SA (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Mail Code 612, Greenbelt, MD 20771 USA. EM scott.a.braun@nasa.gov FU NASA Headquarters; NASA; NSF [ATM-0851021] FX This work was supported by Dr. Ramesh Kakar at NASA Headquarters with funds from the NASA Hurricane Science Research Program. J. A. Sippel contributed to this study while under the NASA Postdoctoral Program and while working for the Goddard Earth Sciences and Technology Center. D. S. Nolan was supported by NSF Grant ATM-0851021. The simulations were conducted on NASA Center for Computational Sciences facilities. We wish to thank the three anonymous reviewers for their very helpful comments that greatly helped to improve the manuscript. NR 49 TC 18 Z9 18 U1 1 U2 14 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD JAN PY 2012 VL 69 IS 1 BP 236 EP 257 DI 10.1175/JAS-D-10-05007.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 876TF UT WOS:000299129900015 ER PT J AU Fridlind, AM van Diedenhoven, B Ackerman, AS Avramov, A Mrowiec, A Morrison, H Zuidema, P Shupe, MD AF Fridlind, Ann M. van Diedenhoven, Bastiaan Ackerman, Andrew S. Avramov, Alexander Mrowiec, Agnieszka Morrison, Hugh Zuidema, Paquita Shupe, Matthew D. TI A FIRE-ACE/SHEBA Case Study of Mixed-Phase Arctic Boundary Layer Clouds: Entrainment Rate Limitations on Rapid Primary Ice Nucleation Processes SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID GENERAL HYDRODYNAMIC THEORY; BULK MICROPHYSICS SCHEME; LARGE-EDDY SIMULATIONS; SURFACE-ENERGY BUDGET; CONDENSATION NUCLEI; AEROSOL-PARTICLES; STRATIFORM CLOUDS; RADIATION BUDGET; VAPOR-DEPOSITION; FALL SPEEDS AB Observations of long-lived mixed-phase Arctic boundary layer clouds on 7 May 1998 during the First International Satellite Cloud Climatology Project (ISCCP) Regional Experiment (FIRE)-Arctic Cloud Experiment (ACE)/Surface Heat Budget of the Arctic Ocean (SHEBA) campaign provide a unique opportunity to test understanding of cloud ice formation. Under the microphysically simple conditions observed (apparently negligible ice aggregation, sublimation, and multiplication), the only expected source of new ice crystals is activation of heterogeneous ice nuclei (IN) and the only sink is sedimentation. Large-eddy simulations with size-resolved microphysics are initialized with IN number concentration N-IN measured above cloud top, but details of IN activation behavior are unknown. If activated rapidly (in deposition, condensation, or immersion modes), as commonly assumed, IN are depleted from the well-mixed boundary layer within minutes. Quasi-equilibrium ice number concentration N-i is then limited to a small fraction of overlying N-IN that is determined by the cloud-top entrainment rate w(e) divided by the number-weighted ice fall speed at the surface upsilon(f). Because w(c) < 1 cm s(-1) and upsilon f > 10 cm s(-1), N-i/N-IN << 1. Such conditions may be common for this cloud type, which has implications for modeling IN diagnostically, interpreting measurements, and quantifying sensitivity to increasing N-IN (when w(e)/upsilon(f) < 1, entrainment rate limitations serve to buffer cloud system response). To reproduce observed ice crystal size distributions and cloud radar reflectivities with rapidly consumed IN in this case, the measured above-cloud N-IN must be multiplied by approximately 30. However, results are sensitive to assumed ice crystal properties not constrained by measurements. In addition, simulations do not reproduce the pronounced mesoscale heterogeneity in radar reflectivity that is observed. C1 [Fridlind, Ann M.; Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [van Diedenhoven, Bastiaan; Avramov, Alexander; Mrowiec, Agnieszka] Columbia Univ, New York, NY USA. [Morrison, Hugh] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Zuidema, Paquita] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Shupe, Matthew D.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Shupe, Matthew D.] NOAA, ESRL, PSD, Boulder, CO USA. RP Fridlind, AM (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM ann.fridlind@nasa.gov RI Ackerman, Andrew/D-4433-2012; Fridlind, Ann/E-1495-2012; van Diedenhoven, Bastiaan/A-2002-2013; Zuidema, Paquita/C-9659-2013; Shupe, Matthew/F-8754-2011; OI Ackerman, Andrew/0000-0003-0254-6253; Zuidema, Paquita/0000-0003-4719-372X; Shupe, Matthew/0000-0002-0973-9982; van Diedenhoven, Bastiaan/0000-0001-5622-8619 FU Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; DOE Office of Science, Office of Biological and Environmental Research [DE-AI02-06ER64173, DE-AI02-08ER64547]; NASA; NASA Advanced Supercomputing Division; National Science Foundation; NOAA's Environmental Technology Laboratory; Naval Postgraduate School FX 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 DE-AC02-05CH11231. Fridlind and Ackerman were supported by the DOE Office of Science, Office of Biological and Environmental Research, through Interagency Agreements DE-AI02-06ER64173 and DE-AI02-08ER64547, the NASA Radiation Sciences Program, and the NASA Advanced Supercomputing Division. We thank the SHEBA Atmospheric Surface Flux Group, Ed Andreas, Chris Fairall, Peter Guest, and Ola Persson for collecting and processing the tower data. The National Science Foundation supported their research with grants to the U.S. Army Cold Regions Research and Engineering Laboratory, NOAA's Environmental Technology Laboratory, and the Naval Postgraduate School. NCEP reanalysis data provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, from their website at http://www.esrl.noaa.gov/psd/. NR 108 TC 25 Z9 25 U1 2 U2 29 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD JAN PY 2012 VL 69 IS 1 BP 365 EP 389 DI 10.1175/JAS-D-11-052.1 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 876TF UT WOS:000299129900022 ER PT J AU Fischer, DG van Dijk, T Visser, TD Wolf, E AF Fischer, David G. van Dijk, Thomas Visser, Taco D. Wolf, Emil TI Coherence effects in Mie scattering SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA A-OPTICS IMAGE SCIENCE AND VISION LA English DT Article ID THEOREM; FIELDS; LIGHT AB The scattering of a partially coherent beam by a deterministic, spherical scatterer is studied. In particular, the Mie scattering by a Gaussian Schell-model beam is analyzed. Expressions are derived for (a) the extinguished power, (b) the radiant intensity of the scattered field, and (c) the encircled energy in the far field. It is found that the radiant intensity and the encircled energy in the far field depend on the degree of coherence of the incident beam, whereas the extinguished power does not. (C) 2011 Optical Society of America C1 [Fischer, David G.] NASA, Res & Technol Directorate, Glenn Res Ctr, Cleveland, OH 44135 USA. [van Dijk, Thomas; Visser, Taco D.] Free Univ Amsterdam, Dept Phys & Astron, Amsterdam, Netherlands. [Visser, Taco D.] Delft Univ Technol, Dept Elect Engn, Delft, Netherlands. [Wolf, Emil] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Wolf, Emil] Univ Rochester, Inst Opt, Rochester, NY 14627 USA. RP Fischer, DG (reprint author), NASA, Res & Technol Directorate, Glenn Res Ctr, Cleveland, OH 44135 USA. EM dgfischer@nasa.gov FU United States Air Force Office of Scientific Research (USAFOSR) [FA9550-08-1-0417]; Netherlands Foundation for Fundamental Research of Matter (FOM) FX The research of E. W. is supported by the United States Air Force Office of Scientific Research (USAFOSR) under grant FA9550-08-1-0417. T. D. V. acknowledges support from The Netherlands Foundation for Fundamental Research of Matter (FOM). NR 19 TC 15 Z9 15 U1 3 U2 9 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1084-7529 J9 J OPT SOC AM A JI J. Opt. Soc. Am. A-Opt. Image Sci. Vis. PD JAN PY 2012 VL 29 IS 1 BP 78 EP 84 PG 7 WC Optics SC Optics GA 877GR UT WOS:000299166000008 PM 22218353 ER PT J AU Pakkanen, MS Petric, AD Olsen, LH Stepancic, A Schlegel, TT Falk, T Rasmussen, CE Starc, V AF Pakkanen, M. Spiljak Petric, A. Domanjko Olsen, L. H. Stepancic, A. Schlegel, T. T. Falk, T. Rasmussen, C. E. Starc, V. TI Advanced Electrocardiographic Parameters Change with Severity of Mitral Regurgitation in Cavalier King Charles Spaniels in Sinus Rhythm SO JOURNAL OF VETERINARY INTERNAL MEDICINE LA English DT Article DE Advanced ECG; Cardiac disease; Dog; Screening ID QT INTERVAL VARIABILITY; HEART-RATE-VARIABILITY; CORONARY-ARTERY-DISEASE; VENTRICULAR REPOLARIZATION; DOGS; CARDIOMYOPATHY; MORPHOLOGY; ACCURACY; INDEX; ECG AB Background: Multiple advanced resting ECG (A-ECG) techniques have improved the diagnostic or prognostic value of ECG in detecting human cardiac diseases even before onset of clinical signs or changes in conventional ECG. Objective: To determine which A-ECG parameters, derived from 12-lead A-ECG recordings, change with severity of mitral regurgitation (MR) caused by myxomatous mitral valve disease (MMVD) in Cavalier King Charles Spaniels (CKCSs) in sinus rhythm. Animals: Seventy-six privately owned CKCSs. Methods: Dogs were prospectively divided into 5 groups according to the degree of MR (estimated by color Doppler mapping as the percentage of the left atrial area affected by the MR jet) and presence of clinical signs. High fidelity approximately 5-minute 12-lead ECG recordings were evaluated using custom software to calculate multiple conventional and A-ECG parameters. Results: Nineteen of 76 ECG parameters were significantly different (P < .05) across the 5 dog groups. A 4-parameter model that incorporated results from 1 parameter of heart rate variability, 2 parameters of QT variability, and 1 parameter of QRS amplitude was identified that explained 82.4% of the variance with a correlation coefficient (R) of 0.60 (P < .01). When age or murmur grade was included in the statistical model the prediction value further increased the R to 0.74 and 0.85 (P < .01), respectively. Conclusion: In CKCSs with sinus rhythm, 4 selected A-ECG parameters further improve prediction of MR jet severity beyond age and murmur grade, although the predictive increment in this study probably is not sufficient to warrant utilization in clinical veterinary practice. C1 [Pakkanen, M. Spiljak; Starc, V.] Univ Ljubljana, Fac Med, Inst Physiol, SI-1000 Ljubljana, Slovenia. [Petric, A. Domanjko] Univ Ljubljana, Clin Surg & Small Anim Med, Fac Vet, SI-1000 Ljubljana, Slovenia. [Olsen, L. H.] Univ Copenhagen, Dept Vet Dis Biol, Fac Life Sci, Frederiksberg, Denmark. [Falk, T.; Rasmussen, C. E.] Univ Copenhagen, Dept Anim & Vet Sci, Fac Life Sci, Frederiksberg, Denmark. [Stepancic, A.] Met & Chem Ind Cinkarna Celje Inc, Qual Control Dept, Celje, Slovenia. [Schlegel, T. T.] NASA Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX USA. Univ Copenhagen, Dept Basic Anim & Vet Sci, Fac Life Sci, Frederiksberg, Denmark. Small Anim Hosp Din Veterinar, Helsingborg, Sweden. RP Starc, V (reprint author), Univ Ljubljana, Fac Med, Inst Physiol, Zaloska 4, SI-1000 Ljubljana, Slovenia. EM vito.starc@mf.uni-lj.si FU Slovenian Research Agency [P3-0019]; Slovene Human Resources Development and Scholarship Fund FX Research was supported by the Slovenian Research Agency (P3-0019) and the Slovene Human Resources Development and Scholarship Fund. NR 35 TC 1 Z9 1 U1 1 U2 4 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0891-6640 J9 J VET INTERN MED JI J. Vet. Intern. Med. PD JAN-FEB PY 2012 VL 26 IS 1 BP 93 EP 100 DI 10.1111/j.1939-1676.2011.00845.x PG 8 WC Veterinary Sciences SC Veterinary Sciences GA 874KU UT WOS:000298956800012 PM 22168834 ER PT J AU Mittlefehldt, DW Beck, AW Lee, CTA Mcsween, HY Buchanan, PC AF Mittlefehldt, David W. Beck, Andrew W. Lee, Cin-Ty A. Mcsween, Harry Y., Jr. Buchanan, Paul C. TI Compositional constraints on the genesis of diogenites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID EUCRITE PARENT BODY; ORTHO-PYROXENE; BASALTIC ACHONDRITES; OLIVINE DIOGENITES; ANTARCTIC EUCRITES; ELEMENT CHEMISTRY; ASTEROID VESTA; CORE FORMATION; IMPACT MELT; GEOCHEMISTRY AB We have done bulk rock compositional analyses (INAA, ICP-MS) and petrologic study of a suite of diogenite meteorites. Most contain orthopyroxenes with mg#s of 70.679.0. Meteorite Hills (MET) 00425 is magnesian (mg# of 83.9). Lewis Cliff (LEW) 88011 contains orthopyroxene grains of varying mg# (76.368.6). Queen Alexandra Range (QUE) 93009 (orthopyroxene mg# 70.6) contains coarse-grained noritic clasts (plagioclase An84.788.3), and is rich in incompatible trace elements. It has Eu/Eu* < 1, indicating that cumulate norites do not dominate its trace element inventory. Queen Alexandra Range 93009 may be transitional between diogenites and magnesian cumulate eucrites. Lewis Cliff 88679, a dimict breccia of harzburgite and orthopyroxenite, has anomalously low concentrations of highly incompatible elements (e.g., Nb, La, Ta, U) compared to other diogenites, but is similar to them in less highly incompatible elements (e.g., Y, Zr, Yb, Hf). It is unlikely that this characteristic reflects a low proportion of a trapped melt component. The highly incompatible elements were likely mobilized after impact mixing of the two parent lithologies. Graves Nunataks 98108 shows an extreme range in Eu/Eu* attributable to the heterogeneous distribution of plagioclase; one sample has the lowest Eu/Eu* among diogenites. We find no compelling evidence to support the hypothesis that diogenite parent magmas were contaminated by partial melts of the eucritic crust. We posit that subsolidus equilibration between orthopyroxene and minor/trace phases (including phosphates) resulted in preferential redistribution of Eu2+ relative to Eu3+ and other rare earth elements, and results in anomalously low Eu/Eu* in samples leached in acids that dissolve phosphates. C1 [Mittlefehldt, David W.] NASA, Mail Code KR, Astromat Res Off, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Beck, Andrew W.; Mcsween, Harry Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Beck, Andrew W.; Mcsween, Harry Y., Jr.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. [Lee, Cin-Ty A.] Rice Univ, Dept Earth Sci, Houston, TX 77005 USA. [Buchanan, Paul C.] Kilgore Coll, Kilgore, TX 75662 USA. RP Mittlefehldt, DW (reprint author), NASA, Mail Code KR, Astromat Res Off, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM david.w.mittlefehldt@nasa.gov RI Lee, Cin-Ty/A-5469-2008; Beck, Andrew/J-7215-2015 OI Beck, Andrew/0000-0003-4455-2299 FU National Science Foundation; Meteorite Working Group, NASA JSC; National Museum of Natural History (Smithsonian Institution); NASA [NNG06GG36G] FX We thank the National Science Foundation for funding the ANSMET collecting teams that brought back the Antarctic samples studied here, and the Meteorite Working Group, NASA JSC, and the National Museum of Natural History (Smithsonian Institution) for allocation of the samples. We thank K. J. Domanik and the late M. J. Drake of the University of Arizona for providing the sample of Bilanga studied here. This work was funded through the NASA Cosmochemistry Program to D. W. M. and Cosmochemistry grant NNG06GG36G to H. Y. M. We thank MAPS AE R. Korotev and referees J.-A. Barrat and "anonymous'' for thorough reviews and editorial handling that greatly improved the quality of this article. NR 75 TC 28 Z9 29 U1 2 U2 17 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JAN PY 2012 VL 47 IS 1 BP 72 EP 98 DI 10.1111/j.1945-5100.2011.01314.x PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 871NC UT WOS:000298743900005 ER PT J AU LaBelle, R Rochblatt, D AF LaBelle, R. Rochblatt, D. TI Ka-band high-rate telemetry system upgrade for the NASA deep space network SO ACTA ASTRONAUTICA LA English DT Article DE Telemetry tracking & command system; Deep space communication equipment; James Webb Space Telescope; Beam waveguide antenna; Cryogenic low-noise amplifier AB The NASA Deep Space Network (DSN) has a new requirement to support high-data-rate Category A (Cat A) missions (within 2 million kilometers of the Earth) with simultaneous S-band uplink, S-band downlink and Ka-band downlink. The S-band links are required for traditional telemetry, tracking & command (TT&C) support to the spacecraft, while the Ka-band link is intended for high-data-rate science returns. The new Ka-band system combines the use of proven DSN cryogenic designs, for low system temperature, and high-data-rate capability using commercial telemetry receivers. The initial Cat A support is required for the James Webb Space Telescope (JWST) in 2014 and possibly other missions. The upgrade has been implemented into 3 different 34-meter Beam Waveguide (BWG) antennas in the DSN, one at each of the complexes in Canberra (Australia), Goldstone (California) and Madrid (Spain). System test data are presented to show that the requirements were met and the DSN is ready for Cat A Ka-band operational support. (C) 2011 Elsevier Ltd. All rights reserved. C1 [LaBelle, R.; Rochblatt, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP LaBelle, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM remi.labelle@jpl.nasa.gov NR 6 TC 1 Z9 1 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JAN-FEB PY 2012 VL 70 BP 58 EP 68 DI 10.1016/j.actaastro.2011.07.023 PG 11 WC Engineering, Aerospace SC Engineering GA 869UC UT WOS:000298622700007 ER PT J AU Baars, WJ Tinney, CE Ruf, JH Brown, AM McDaniels, DM AF Baars, Woutijn J. Tinney, Charles E. Ruf, Joseph H. Brown, Andrew M. McDaniels, David M. TI Wall Pressure Unsteadiness and Side Loads in Overexpanded Rocket Nozzles SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA/ASME/SAE/ASEE 46th Joint Propulsion Conference and Exhibit CY JUL 25-29, 2010 CL Nashville, TN SP AIAA, ASME, SAE, ASEE ID RESTRICTED SHOCK SEPARATION; COMPRESSION RAMP INTERACTION; FLOWS AB Surveys of both the static and dynamic wall pressure signatures on the interior surface of a subscale, cold-flow, and thrust-optimized parabolic nozzle are conducted during fixed nozzle pressure ratios corresponding to free shock separation and restricted shock separation states. The motive is to develop a better understanding for the sources of off-axis loads during the transient startup of overexpanded rocket nozzles. During free shock separation state, pressure spectra reveal frequency content resembling shock wave turbulent boundary-layer interaction. Presumably, when the internal flow is in restricted shock separation state, separation bubbles are trapped by shocks and expansion waves; interactions between the separated flow regions and the waves produce asymmetric pressure distributions. An analysis of the azimuthal modes reveals how the breathing mode encompasses most of the resolved energy and that the side load inducing mode is coherent with the response moment measured by strain gauges mounted upstream of the nozzle on a flexible tube. Finally, the unsteady pressure is locally more energetic during restricted shock separation, albeit direct measurements of the response moments indicate higher side load activity when in free shock separation state. It is postulated that these discrepancies are attributed to cancellation effects between annular separation bubbles. C1 [Baars, Woutijn J.; Tinney, Charles E.] Univ Texas Austin, Austin, TX 78712 USA. [Ruf, Joseph H.; McDaniels, David M.] NASA, Marshall Space Flight Ctr, Fluid Dynam Branch ER42, Huntsville, AL 35812 USA. [Brown, Andrew M.] NASA, Marshall Space Flight Ctr, Propuls Struct & Dynam Anal Branch ER41, Huntsville, AL 35812 USA. RP Baars, WJ (reprint author), Univ Texas Austin, Austin, TX 78712 USA. RI Baars, Woutijn/F-6600-2016 OI Baars, Woutijn/0000-0003-1526-3084 NR 28 TC 12 Z9 12 U1 0 U2 15 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD JAN PY 2012 VL 50 IS 1 BP 61 EP 73 DI 10.2514/1.J051075 PG 13 WC Engineering, Aerospace SC Engineering GA 872TD UT WOS:000298831600005 ER PT J AU Huberty, JM Konishi, H Heck, PR Fournelle, JH Valley, JW Xu, HF AF Huberty, Jason M. Konishi, Hiromi Heck, Philipp R. Fournelle, John H. Valley, John W. Xu, Huifang TI Silician magnetite from the Dales Gorge Member of the Brockman Iron Formation, Hamersley Group, Western Australia SO AMERICAN MINERALOGIST LA English DT Article DE Magnetite; silician magnetite; banded iron formation; Dales Gorge; Hamersley; biosignature ID SEDIMENTOLOGICAL EVIDENCE; IRON(III) HYDROXIDE; GEOCHEMISTRY; METAMORPHISM; SI; POLYMERIZATION; DEPOSITION; REDUCTION; CHEMISTRY; GENESIS AB We report silician magnetite from banded iron formation (BIF) in the Dales Gorge Member of the Brockman Iron Formation, Hamersley Group, Western Australia. Magnetite mesobands typically consisting of individual similar to 100 mu m microlaminae are revealed to be composed of silician magnetite overgrowths on magnetite. Silician magnetite overgrowths contain from 1 to 3 wt% SiO(2), whereas (low-Si) magnetite domains contain less than 1 wt% SiO(2). Silicon solid solution is present in the magnetite crystal lattice as determined by in situ micro-X-ray diffraction and high-resolution transmission electron microscopy. Three textures are distinguished in magnetite mesobands: (1) magnetite sub-microlaminae with silician magnetite overgrowths, (2) recrystallized magnetite fragments with silician magnetite overgrowths, and (3) a complex intergrowth of magnetite and silician magnetite. All three textures are found in magnetite mesobands from the BIF4-5 and BIF12-16 macrobands of the Dales Gorge type-section drill core DDH-47A from Wittenoom, Western Australia. Magnetite domains contain numerous submicrometer-to-micrometer inclusions of quartz, carbonate, stilpnomelane, and apatite, whereas silician magnetite overgrowths are devoid of mineral inclusions. The presence of mineral inclusions in magnetite indicates the BIF oxide precipitate was not chemically pure iron oxyhydroxide/oxide. Magnetite domains display textures formed during soft sediment deformation that are the earliest and best preserved relict sedimentary structures in this BIF. Silician magnetite is the dominant iron oxide in the Dales Gorge BIF and is present in many other sub-greenschist facies BIFs worldwide. We suggest the former presence of organic matter creates reducing conditions necessary to stabilize silician magnetite. Thus, silician magnetite is a potential biosignature in BIFs. C1 [Huberty, Jason M.; Konishi, Hiromi; Heck, Philipp R.; Fournelle, John H.; Valley, John W.; Xu, Huifang] Univ Wisconsin, NASA Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA. RP Huberty, JM (reprint author), Univ Wisconsin, NASA Astrobiol Inst, Dept Geosci, 1215 W Dayton St, Madison, WI 53706 USA. EM jason@geology.wisc.edu RI Heck, Philipp/C-6092-2012; Valley, John/B-3466-2011 OI Valley, John/0000-0003-3530-2722 FU NASA Astrobiology Institute [N07-5489]; NSF-EAR [0509639, 0838058, 0619368]; DOE [93ER 14389, 09ER 16050] FX We thank Alec Trendall and Richard Morris for conversations during the 5th International Archean Symposium. Richard Morris helped authenticate our samples. We thank Cornelius (Kase) Klein, Clark Johnson, and the UW-Madison Geology Museum for providing the drill core samples used in this study. We thank Brian Hess for sample preparation and Phil Brown and Chloe Bonamici for helpful conversations. Reviews by Phillip Fralick and Nicolaus Dauphas substantially improved this paper. This study was funded by the NASA Astrobiology Institute (N07-5489), NSF-EAR (0509639, 0838058, 0619368), and DOE (93ER 14389, 09ER 16050). NR 51 TC 13 Z9 13 U1 1 U2 9 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD JAN PY 2012 VL 97 IS 1 BP 26 EP 37 DI 10.2138/am.2012.3864 PG 12 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 873OT UT WOS:000298893400003 ER PT J AU Horch, EP Bahi, LAP Gaulin, JR Howell, SB Sherry, WH Galle, RB van Altena, WF AF Horch, Elliott P. Bahi, Lizzie Anne P. Gaulin, Joseph R. Howell, Steve B. Sherry, William H. Baena Galle, Roberto van Altena, William F. TI SPECKLE OBSERVATIONS OF BINARY STARS WITH THE WIYN* TELESCOPE. VII. MEASURES DURING 2008-2009 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: visual; techniques: high angular resolution; techniques: interferometric; techniques: photometric ID PEAK 4-M TELESCOPE; GENEVA-COPENHAGEN SURVEY; INTERFEROMETRIC MEASUREMENTS; KITT-PEAK; CD-ROM; DIFFERENTIAL PHOTOMETRY; HIPPARCOS BINARIES; SOLAR NEIGHBORHOOD; DIFFRACTION LIMIT; BRIGHT STARS AB Five hundred thirty-one speckle measures of binary stars are reported. These data were taken mainly during the period 2008 June through 2009 October at the WIYN 3.5 m Telescope at Kitt Peak and represent the last data set of single-filter speckle observations taken in the WIYN speckle program prior to the use of the current two-channel speckle camera. The astrometric and photometric precision of these observations is consistent with previous papers in this series: we obtain a typical linear measurement uncertainty of approximately 2.5 mas, and the magnitude differences reported have typical uncertainties in the range of 0.1-0.14 mag. In combination with measures already in the literature, the data presented here permit the revision of the orbit of A 1634AB (= HIP 76041) and the first determination of visual orbital elements for HDS 1895 (= HIP 65982). C1 [Horch, Elliott P.; Bahi, Lizzie Anne P.; Gaulin, Joseph R.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Howell, Steve B.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Baena Galle, Roberto] Observ Fabra, Reial Acad Ciencies & Arts Barcelona, E-08002 Barcelona, Spain. [van Altena, William F.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. EM horche2@southernct.edu; bahil1@owls.southernct.edu; jgaulin.jg@gmail.com; steve.b.howell@nasa.gov; wsherry@noao.edu; rbaena@am.ub.es; william.vanaltena@yale.edu FU NSF [AST-0908125] FX It is a pleasure to thank all of the outstanding staff at WIYN for their continued assistance and support at the telescope, especially Bill Binkert, Karen Butler, Charles Corson, Jenny Power, Krissy Reetz, Dave Summers, and George Will. This work was funded by NSF Grant AST-0908125. It made use of the Washington Double Star Catalog maintained at the U.S. Naval Observatory and the SIMBAD database, operated at CDS, Strasbourg, France. NR 52 TC 14 Z9 16 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2012 VL 143 IS 1 AR 10 DI 10.1088/0004-6256/143/1/10 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 865OY UT WOS:000298321400010 ER PT J AU Lake, SE Wright, EL Petty, S Assef, RJ Jarrett, TH Stanford, SA Stern, D Tsai, CW AF Lake, S. E. Wright, E. L. Petty, S. Assef, R. J. Jarrett, T. H. Stanford, S. A. Stern, D. Tsai, C. -W. TI OPTICAL SPECTROSCOPIC SURVEY OF HIGH-LATITUDE WISE-SELECTED SOURCES SO ASTRONOMICAL JOURNAL LA English DT Article DE catalogs; galaxies: general; Galaxy: stellar content; surveys ID SPECTRAL ENERGY-DISTRIBUTIONS; ACTIVE GALACTIC NUCLEI; EVOLUTION SURVEY; DATA RELEASE; 1ST DATA; RESOLUTION; GALAXY AB We report on the results of an optical spectroscopic survey at high Galactic latitude (vertical bar b vertical bar >= 30 degrees) of a sample of WISE-selected targets, grouped by WISE W1 (lambda(eff) = 3.4 mu m) flux, which we use to characterize the sources WISE detected. We observed 762 targets in 10 disjoint fields centered on ultraluminous infrared galaxy candidates using DEIMOS on Keck II. We find 0.30 +/- 0.02 galaxies arcmin(-2) with a median redshift of z = 0.33 +/- 0.01 for the sample with W1 >= 120 mu Jy. The foreground stellar densities in our survey range from 0.23 +/- 0.07 arcmin(-2) to 1.1 +/- 0.1 arcmin (2) for the same sample. We obtained spectra that produced science grade redshifts for >= 90% of our targets for sources with W1 flux >= 120 mu Jy that also had an i-band flux greater than or similar to 18 mu Jy. We used this for targeting very preliminary data reductions available to the team in 2010 August. Our results therefore present a conservative estimate of what is possible to achieve using WISE's Preliminary Data Release for the study of field galaxies. C1 [Lake, S. E.; Wright, E. L.; Petty, S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Assef, R. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jarrett, T. H.; Tsai, C. -W.] CALTECH, Infrared Proc & Anal Ctr IPAC, Pasadena, CA 91125 USA. [Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. RP Lake, SE (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. EM lake@physics.ucla.edu FU National Aeronautics and Space Administration; National Science Foundation [AST-0071048]; Alfred P. Sloan Foundation; U.S. Department of Energy FX This publication makes use of data products from 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 WISE Web site is http://wise.ssl.berkeley.edu/.; The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from the NSF grant AST-0071048.; 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. The SDSS-III Web site is http://www.sdss3.org/. NR 23 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2012 VL 143 IS 1 AR 7 DI 10.1088/0004-6256/143/1/7 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 865OY UT WOS:000298321400007 ER PT J AU Abbasi, R Abdou, Y Abu-Zayyad, T Adams, J Aguilar, JA Ahlers, M Andeen, K Auffenberg, J Bai, X Baker, M Barwick, SW Bay, R Alba, JLB Beattie, K Beatty, JJ Bechet, S Becker, JK Becker, KH Benabderrahmane, ML BenZvi, S Berdermann, J Berghaus, P Berley, D Bernardini, E Bertrand, D Besson, DZ Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bose, D Boser, S Botner, O Braun, J Brown, AM Buitink, S Carson, M Chirkin, D Christy, B Clem, J Clevermann, F Cohen, S Colnard, C Cowen, DF D'Agostino, MV Danninger, M Daughhetee, J Davis, JC De Clercq, C Demirors, L Denger, T Depaepe, O Descamps, F Desiati, P de Vries-Uiterweerd, G DeYoung, T Diaz-Velez, JC Dierckxsens, M Dreyer, J Dumm, JP Ehrlich, R Eisch, J Ellsworth, RW Engdegrd, O Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feusels, T Filimonov, K Finley, C Fischer-Wasels, T Foerster, MM Fox, BD Franckowiak, A Franke, R Gaisser, TK Gallagher, J Geisler, M Gerhardt, L Gladstone, L Glusenkamp, T Goldschmidt, A Goodman, JA Grant, D Griesel, T Gross, A Grullon, S Gurtner, M Ha, C Hallgren, A Halzen, F Han, K Hanson, K Heinen, D Helbing, K Herquet, P Hickford, S Hill, GC Hoffman, KD Homeier, A Hoshina, K Hubert, D Huelsnitz, W Hulss, JP Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobsen, J Japaridze, GS Johansson, H Joseph, JM Kampert, KH Kappes, A Karg, T Karle, A Kelley, JL Kenny, P Kiryluk, J Kislat, F Klein, SR Kohne, JH Kohnen, G Kolanoski, H Kopke, L Kopper, S Koskinen, DJ Kowalski, M Kowarik, T Krasberg, M Krings, T Kroll, G Kuehn, K Kurahashi, N Kuwabara, T Labare, M Lafebre, S Laihem, K Landsman, H Larson, MJ Lauer, R Lunemann, J Madsen, J Majumdar, P Marotta, A Maruyama, R Mase, K Matis, HS Meagher, K Merck, M Meszaros, P Meures, T Middell, E Milke, N Miller, J Montaruli, T Morse, R Movit, SM Nahnhauer, R Nam, JW Naumann, U Niessen, P Nygren, DR Odrowski, S Olivas, A Olivo, M O'Murchadha, A Ono, M Panknin, S Paul, L de los Heros, CP Petrovic, J Piegsa, A Pieloth, D Porrata, R Posselt, J Price, PB Prikockis, M Przybylski, GT Rawlins, K Redl, P Resconi, E Rhode, W Ribordy, M Rizzo, A Rodrigues, JP Roth, P Rothmaier, F Rott, C Ruhe, T Rutledge, D Ruzybayev, B Ryckbosch, D Sander, HG Santander, M Sarkar, S Schatto, K Schmidt, T Schonwald, A Schukraft, A Schultes, A Schulz, O Schunck, M Seckel, D Semburg, B Seo, SH Sestayo, Y Seunarine, S Silvestri, A Slipak, A Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stephens, G Stezelberger, T Stokstad, RG Stossl, A Stoyanov, S Strahler, EA Straszheim, T Stur, M Sullivan, GW Swillens, Q Taavola, H Taboada, I Tamburro, A Tepe, A Ter-Antonyan, S Tilav, S Toale, PA Toscano, S Tosi, D Turcan, D van Eijndhoven, N Vandenbroucke, J Van Overloop, A van Santen, J Vehring, M Voge, M Walck, C Waldenmaier, T Wallraff, M Walter, M Weaver, C Wendt, C Westerhoff, S Whitehorn, N Wiebe, K Wiebusch, CH Williams, DR Wischnewski, R Wissing, H Wolf, M Woschnagg, K Xu, C Xu, XW Yodh, G Yoshida, S Zarzhitsky, P AF Abbasi, R. Abdou, Y. Abu-Zayyad, T. Adams, J. Aguilar, J. A. Ahlers, M. Andeen, K. Auffenberg, J. Bai, X. Baker, M. Barwick, S. W. Bay, R. Alba, J. L. Bazo Beattie, K. Beatty, J. J. Bechet, S. Becker, J. K. Becker, K. -H. Benabderrahmane, M. L. BenZvi, S. Berdermann, J. Berghaus, P. Berley, D. Bernardini, E. Bertrand, D. Besson, D. Z. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bose, D. Boeser, S. Botner, O. Braun, J. Brown, A. M. Buitink, S. Carson, M. Chirkin, D. Christy, B. Clem, J. Clevermann, F. Cohen, S. Colnard, C. Cowen, D. F. D'Agostino, M. V. Danninger, M. Daughhetee, J. Davis, J. C. De Clercq, C. Demiroers, L. Denger, T. Depaepe, O. Descamps, F. Desiati, P. de Vries-Uiterweerd, G. DeYoung, T. Diaz-Velez, J. C. Dierckxsens, M. Dreyer, J. Dumm, J. P. Ehrlich, R. Eisch, J. Ellsworth, R. W. Engdegrd, O. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feusels, T. Filimonov, K. Finley, C. Fischer-Wasels, T. Foerster, M. M. Fox, B. D. Franckowiak, A. Franke, R. Gaisser, T. K. Gallagher, J. Geisler, M. Gerhardt, L. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Goodman, J. A. Grant, D. Griesel, T. Gross, A. Grullon, S. Gurtner, M. Ha, C. Hallgren, A. Halzen, F. Han, K. Hanson, K. Heinen, D. Helbing, K. Herquet, P. Hickford, S. Hill, G. C. Hoffman, K. D. Homeier, A. Hoshina, K. Hubert, D. Huelsnitz, W. Huelss, J. -P. Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jacobsen, J. Japaridze, G. S. Johansson, H. Joseph, J. M. Kampert, K. -H. Kappes, A. Karg, T. Karle, A. Kelley, J. L. Kenny, P. Kiryluk, J. Kislat, F. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koepke, L. Kopper, S. Koskinen, D. J. Kowalski, M. Kowarik, T. Krasberg, M. Krings, T. Kroll, G. Kuehn, K. Kurahashi, N. Kuwabara, T. Labare, M. Lafebre, S. Laihem, K. Landsman, H. Larson, M. J. Lauer, R. Luenemann, J. Madsen, J. Majumdar, P. Marotta, A. Maruyama, R. Mase, K. Matis, H. S. Meagher, K. Merck, M. Meszaros, P. Meures, T. Middell, E. Milke, N. Miller, J. Montaruli, T. Morse, R. Movit, S. M. Nahnhauer, R. Nam, J. W. Naumann, U. Niessen, P. Nygren, D. R. Odrowski, S. Olivas, A. Olivo, M. O'Murchadha, A. Ono, M. Panknin, S. Paul, L. de los Heros, C. Perez Petrovic, J. Piegsa, A. Pieloth, D. Porrata, R. Posselt, J. Price, P. B. Prikockis, M. Przybylski, G. T. Rawlins, K. Redl, P. Resconi, E. Rhode, W. Ribordy, M. Rizzo, A. Rodrigues, J. P. Roth, P. Rothmaier, F. Rott, C. Ruhe, T. Rutledge, D. Ruzybayev, B. Ryckbosch, D. Sander, H. -G. Santander, M. Sarkar, S. Schatto, K. Schmidt, T. Schoenwald, A. Schukraft, A. Schultes, A. Schulz, O. Schunck, M. Seckel, D. Semburg, B. Seo, S. H. Sestayo, Y. Seunarine, S. Silvestri, A. Slipak, A. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stephens, G. Stezelberger, T. Stokstad, R. G. Stoessl, A. Stoyanov, S. Strahler, E. A. Straszheim, T. Stuer, M. Sullivan, G. W. Swillens, Q. Taavola, H. Taboada, I. Tamburro, A. Tepe, A. Ter-Antonyan, S. Tilav, S. Toale, P. A. Toscano, S. Tosi, D. Turcan, D. van Eijndhoven, N. Vandenbroucke, J. Van Overloop, A. van Santen, J. Vehring, M. Voge, M. Walck, C. Waldenmaier, T. Wallraff, M. Walter, M. Weaver, Ch. Wendt, C. Westerhoff, S. Whitehorn, N. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wischnewski, R. Wissing, H. Wolf, M. Woschnagg, K. Xu, C. Xu, X. W. Yodh, G. Yoshida, S. Zarzhitsky, P. CA IceCube Collaboration TI TIME-DEPENDENT SEARCHES FOR POINT SOURCES OF NEUTRINOS WITH THE 40-STRING AND 22-STRING CONFIGURATIONS OF ICECUBE SO ASTROPHYSICAL JOURNAL LA English DT Article DE astroparticle physics; cosmic rays; neutrinos ID GAMMA-RAY BURSTS; TEV BLAZAR 1ES-1959+650; HIGH-ENERGY NEUTRINOS; LARGE-AREA TELESCOPE; MULTIWAVELENGTH OBSERVATIONS; COSMIC-RAYS; AGILE DETECTION; MUON NEUTRINOS; SGR 0501+4516; MARKARIAN 421 AB This paper presents four searches for flaring sources of neutrinos using the IceCube neutrino telescope. For the first time, a search is performed over the entire parameter space of energy, direction, and time with sensitivity to neutrino flares lasting between 20 mu s and a year duration from astrophysical sources. Searches that integrate over time are less sensitive to flares because they are affected by a larger background of atmospheric neutrinos and muons that can be reduced by the use of additional timing information. Flaring sources considered here, such as active galactic nuclei, soft gamma-ray repeaters, and gamma-ray bursts, are promising candidate neutrino emitters. Two searches are "untriggered" in the sense that they look for any possible flare in the entire sky and from a predefined catalog of sources from which photon flares have been recorded. The other two searches are triggered by multi-wavelength information on flares from blazars and from a soft gamma-ray repeater. One triggered search uses lightcurves from Fermi-LAT which provides continuous monitoring. A second triggered search uses information where the flux states have been measured only for short periods of time near the flares. The untriggered searches use data taken by 40 strings of IceCube between 2008 April 5 and 2009 May 20. The triggered searches also use data taken by the 22-string configuration of IceCube operating between 2007 May 31 and 2008 April 5. The results from all four searches are compatible with a fluctuation of the background. C1 [Aguilar, J. A.; Braun, J.; Chirkin, D.; Diaz-Velez, J. C.; Eisch, J.; Fedynitch, A.; Halzen, F.; Hill, G. C.; Jacobsen, J.; Karle, A.; Kelley, J. L.; Landsman, H.; O'Murchadha, A.; van Santen, J.; Weaver, Ch.; Wendt, C.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium. [Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Adams, J.; Brown, A. M.; Gross, A.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch, New Zealand. [Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Auffenberg, J.; Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Kopper, S.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Gesamthsch Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Franke, R.; Han, K.; Kislat, F.; Lauer, R.; Majumdar, P.; Middell, E.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Tosi, D.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany. [Beattie, K.; Buitink, S.; Gerhardt, L.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Petrovic, J.; Swillens, Q.] Univ Libre Brussels, Fac Sci, B-1050 Brussels, Belgium. [Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany. [Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Roth, P.; Schmidt, T.; Straszheim, T.; Sullivan, G. W.; Turcan, D.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Geisler, M.; Gluesenkamp, T.; Heinen, D.; Huelss, J. -P.; Krings, T.; Laihem, K.; Meures, T.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Bose, D.; De Clercq, C.; Depaepe, O.; Hubert, D.; Labare, M.; Rizzo, A.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Boeser, S.; Denger, T.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Stuer, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Botner, O.; Engdegrd, O.; Hallgren, A.; Miller, J.; de los Heros, C. Perez; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Clevermann, F.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany. [Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany. [Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Lafebre, S.; Larson, M. J.; Meszaros, P.; Prikockis, M.; Rutledge, D.; Slipak, A.; Stephens, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Grant, D.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Ishihara, A.; Mase, K.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Univ Berlin, Inst Phys, D-12489 Berlin, Germany. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Toale, P. A.; Williams, D. R.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Montaruli, T.] Univ Bari, I-70126 Bari, Italy. [Montaruli, T.] Sezione Ist Nazl Fis Nucl, Dipartimento Fis, I-70126 Bari, Italy. RP Abbasi, R (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. RI Taavola, Henric/B-4497-2011; Wiebusch, Christopher/G-6490-2012; Kowalski, Marek/G-5546-2012; Tamburro, Alessio/A-5703-2013; Hallgren, Allan/A-8963-2013; Botner, Olga/A-9110-2013; Tjus, Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014; Koskinen, David/G-3236-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011; Maruyama, Reina/A-1064-2013 OI Schukraft, Anne/0000-0002-9112-5479; Perez de los Heros, Carlos/0000-0002-2084-5866; Taavola, Henric/0000-0002-2604-2810; Buitink, Stijn/0000-0002-6177-497X; Carson, Michael/0000-0003-0400-7819; Hubert, Daan/0000-0002-4365-865X; Benabderrahmane, Mohamed Lotfi/0000-0003-4410-5886; Wiebusch, Christopher/0000-0002-6418-3008; Auffenberg, Jan/0000-0002-1185-9094; Koskinen, David/0000-0002-0514-5917; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Ter-Antonyan, Samvel/0000-0002-5788-1369; Maruyama, Reina/0000-0003-2794-512X FU U.S. National Science Foundation-Office of Polar Programs; U.S. National Science Foundation-Physics Division; University of Wisconsin Alumni Research Foundation; Grid Laboratory Of Wisconsin (GLOW), University of Wisconsin-Madison; Open Science Grid (OSG); U.S. Department of Energy; National Energy Research Scientific Computing Center; Louisiana Optical Network Initiative (LONI); National Science and Engineering Research Council of Canada; Swedish Research Council; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute; Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland; EU; Capes Foundation, Ministry of Education of Brazil FX We acknowledge the support from the following agencies: U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; National Science and Engineering Research Council of Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; A. Gross acknowledges support by the EU Marie Curie OIF Program; J. P. Rodrigues acknowledges support by the Capes Foundation, Ministry of Education of Brazil. NR 75 TC 21 Z9 22 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2012 VL 744 IS 1 AR 1 DI 10.1088/0004-637X/744/1/1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866TY UT WOS:000298408300001 ER PT J AU Ajello, M Allafort, A Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bloom, ED Bonamente, E Borgland, AW Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cecchi, C Charles, E Chekhtman, A Ciprini, S Claus, R Cohen-Tanugi, J Cutini, S de Angelis, A de Palma, F Dermer, CD Silva, EDE Drell, PS Drlica-Wagner, A Dubois, R Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Frailis, M Fukazawa, Y Fukui, Y Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Grove, JE Guiriec, S Hadasch, D Hanabata, Y Harding, AK Hayashi, K Hays, E Itoh, R Johannesson, G Johnson, AS Kamae, T Katagiri, H Kataoka, J Knodlseder, J Kubo, H Kuss, M Lande, J Latronico, L Lee, SH Lionetto, AM Longo, F Loparco, F Lovellette, MN Lubrano, P Mazziotta, MN Mehault, J Michelson, PF Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nakamori, T Naumann-Godo, M Nishino, S Nolan, PL Norris, JP Nuss, E Ohno, M Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Paneque, D Parent, D Pelassa, V Pesce-Rollins, M Pierbattista, M Piron, F Porter, TA Raino, S Rando, R Reimer, A Reimer, O Reposeur, T Roth, M Sadrozinski, HFW Sgro, C Siskind, EJ Smith, PD Spandre, G Spinelli, P Suson, DJ Tajima, H Takahashi, H Tanaka, T Thayer, JG Thayer, JB Tibaldo, L Tibolla, O Torres, DF Tosti, G Tramacere, A Troja, E Uchiyama, Y Uehara, T Usher, TL Vandenbroucke, J Van Etten, A Vasileiou, V Vianello, G Vilchez, N Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Yamamoto, H Yamazaki, R Yang, Z Yasuda, H Ziegler, M Zimmer, S AF Ajello, M. Allafort, A. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cecchi, C. Charles, E. Chekhtman, A. Ciprini, S. Claus, R. Cohen-Tanugi, J. Cutini, S. de Angelis, A. de Palma, F. Dermer, C. D. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Dubois, R. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Frailis, M. Fukazawa, Y. Fukui, Y. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grove, J. E. Guiriec, S. Hadasch, D. Hanabata, Y. Harding, A. K. Hayashi, K. Hays, E. Itoh, R. Johannesson, G. Johnson, A. S. Kamae, T. Katagiri, H. Kataoka, J. Knoedlseder, J. Kubo, H. Kuss, M. Lande, J. Latronico, L. Lee, S. -H. Lionetto, A. M. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Mazziotta, M. N. Mehault, J. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Naumann-Godo, M. Nishino, S. Nolan, P. L. Norris, J. P. Nuss, E. Ohno, M. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Paneque, D. Parent, D. Pelassa, V. Pesce-Rollins, M. Pierbattista, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Reimer, A. Reimer, O. Reposeur, T. Roth, M. Sadrozinski, H. F. -W. Sgro, C. Siskind, E. J. Smith, P. D. Spandre, G. Spinelli, P. Suson, D. J. Tajima, H. Takahashi, H. Tanaka, T. Thayer, J. G. Thayer, J. B. Tibaldo, L. Tibolla, O. Torres, D. F. Tosti, G. Tramacere, A. Troja, E. Uchiyama, Y. Uehara, T. Usher, T. L. Vandenbroucke, J. Van Etten, A. Vasileiou, V. Vianello, G. Vilchez, N. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Yamamoto, H. Yamazaki, R. Yang, Z. Yasuda, H. Ziegler, M. Zimmer, S. TI FERMI LARGE AREA TELESCOPE OBSERVATIONS OF THE SUPERNOVA REMNANT G8.7-0.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; gamma rays: ISM; ISM: individual objects (G8.7-0.1, HESS J1804-216); ISM: supernova remnants ID GAMMA-RAY EMISSION; PULSAR WIND NEBULA; GALACTIC COSMIC-RAYS; MOLECULAR CLOUDS; HIGH-ENERGY; INNER GALAXY; HESS J1804-216; X-RAY; DISCOVERY; CATALOG AB We present a detailed analysis of the GeV gamma-ray emission toward the supernova remnant (SNR) G8.7-0.1 with the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope. An investigation of the relationship between G8.7-0.1 and the TeV unidentified source HESS J1804-216 provides us with an important clue on diffusion process of cosmic rays if particle acceleration operates in the SNR. The GeV gamma-ray emission is extended with most of the emission in positional coincidence with the SNR G8.7-0.1 and a lesser part located outside the western boundary of G8.7-0.1. The region of the gamma-ray emission overlaps spatially connected molecular clouds, implying a physical connection for the gamma-ray structure. The total gamma-ray spectrum measured with LAT from 200 MeV-100 GeV can be described by a broken power-law function with a break of 2.4 +/- 0.6 (stat) +/- 1.2 (sys) GeV, and photon indices of 2.10 +/- 0.06 (stat) +/- 0.10 (sys) below the break and 2.70 +/- 0.12 (stat) +/- 0.14 (sys) above the break. Given the spatial association among the gamma rays, the radio emission of G8.7-0.1, and the molecular clouds, the decay of pi(0)s produced by particles accelerated in the SNR and hitting the molecular clouds naturally explains the GeV gamma-ray spectrum. We also find that the GeV morphology is not well represented by the TeV emission from HESS J1804-216 and that the spectrum in the GeV band is not consistent with the extrapolation of the TeV gamma-ray spectrum. The spectral index of the TeV emission is consistent with the particle spectral index predicted by a theory that assumes energy-dependent diffusion of particles accelerated in an SNR. We discuss the possibility that the TeV spectrum originates from the interaction of particles accelerated in G8.7-0.1 with molecular clouds, and we constrain the diffusion coefficient of the particles. C1 [Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Van Etten, A.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA. [Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chekhtman, A.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Van Etten, A.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Naumann-Godo, M.; Pierbattista, M.; Tibaldo, L.] Univ Paris Diderot, Lab AIM, CEA IRFU, CNRS,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Allafort, A.; Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA. [Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France. [Cutini, S.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [de Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ferrara, E. C.; Harding, A. K.; Hays, E.; Moiseev, A. A.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Frailis, M.] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy. [Fukazawa, Y.; Hanabata, Y.; Hayashi, K.; Itoh, R.; Mizuno, T.; Nishino, S.; Uehara, T.; Yasuda, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Fukui, Y.; Yamamoto, H.] Nagoya Univ, Dept Phys & Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.; Pelassa, V.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Katagiri, H.] Ibaraki Univ, Coll Sci, Bunkyo Ku, Mito, Ibaraki 3108512, Japan. [Kataoka, J.; Nakamori, T.] Waseda Univ Tokyo, Res Inst Sci & Engn, Tokyo 1698555, Japan. [Knoedlseder, J.; Vilchez, N.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knoedlseder, J.; Vilchez, N.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France. [Kubo, H.] Kyoto Univ, Dept Phys, Grad Sch Sci, Kyoto 606, Japan. [Lee, S. -H.] Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 6068502, Japan. [Lionetto, A. M.; Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Lionetto, A. M.; Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Moiseev, A. A.] Ctr Res & Explorat Space Sci & Technol CRESST, Greenbelt, MD 20771 USA. [Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. [Ohno, M.; Okumura, A.] JAXA, Inst Space & Astronaut Sci, Kanagawa 2525210, Japan. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Parent, D.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reposeur, T.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France. [Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Torres, D. F.] ICREA, Barcelona, Spain. [Tramacere, A.; Vianello, G.] CIFS, I-10133 Turin, Italy. [Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. [Yamazaki, R.] Aoyama Gakuin Univ, Dept Math & Phys, Sagamihara, Kanagawa 2525258, Japan. [Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Yang, Z.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. RP Ajello, M (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA. EM hanabata@hep01.hepl.hiroshima-u.ac.jp; katagiri@mx.ibaraki.ac.jp RI Harding, Alice/D-3160-2012; Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; OI Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Giordano, Francesco/0000-0002-8651-2394; giommi, paolo/0000-0002-2265-5003; De Angelis, Alessandro/0000-0002-3288-2517; Frailis, Marco/0000-0002-7400-2135; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; Giroletti, Marcello/0000-0002-8657-8852; Berenji, Bijan/0000-0002-4551-772X; Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726 FU International Doctorate on Astroparticle Physics (IDAPP) program; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX Partially supported by the International Doctorate on Astroparticle Physics (IDAPP) program.; Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. NR 54 TC 26 Z9 26 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2012 VL 744 IS 1 AR 80 DI 10.1088/0004-637X/744/1/80 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866TY UT WOS:000298408300080 ER PT J AU Barrows, RS Stern, D Madsen, K Harrison, F Assef, RJ Comerford, JM Cushing, MC Fassnacht, CD Gonzalez, AH Griffith, R Hickox, R Kirkpatrick, JD Lagattuta, DJ AF Barrows, R. Scott Stern, Daniel Madsen, Kristin Harrison, Fiona Assef, Roberto J. Comerford, Julia M. Cushing, Michael C. Fassnacht, Christopher D. Gonzalez, Anthony H. Griffith, Roger Hickox, Ryan Kirkpatrick, J. Davy Lagattuta, David J. TI A CANDIDATE DUAL ACTIVE GALACTIC NUCLEUS AT z=1.175 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (CXOXBJ142607.6+353351); galaxies: nuclei; quasars: emission lines ID NARROW-LINE REGION; BLACK-HOLE BINARIES; DIGITAL-SKY-SURVEY; DOUBLE-PEAKED EMITTER; QUASAR SDSS J092712.65+294344.0; REDSHIFT RADIO GALAXIES; WIDE-FIELD SURVEY; X-RAY SOURCE; EMISSION-LINES; BOOTES-FIELD AB The X-ray source CXOXBJ142607.6+353351 (CXOJ1426+35), which was identified in a 172 ks Chandra image in the Bootes field, shows double-peaked rest-frame optical/UV emission lines, separated by 0.''69 (5.5 kpc) in the spatial dimension and by 690 km s(-1) in the velocity dimension. The high excitation lines and emission line ratios indicate both systems are ionized by an active galactic nucleus (AGN) continuum, and the double-peaked profile resembles that of candidate dual AGNs. At a redshift of z = 1.175, this source is the highest redshift candidate dual AGN yet identified. However, many sources have similar emission line profiles for which other interpretations are favored. We have analyzed the substantial archival data available in this field as well as acquired near-infrared (NIR) adaptive optics (AO) imaging and NIR slit spectroscopy. The X-ray spectrum is hard, implying a column density of several 10(23) cm(-2). Though heavily obscured, the source is also one of the brightest in the field, with an absorption-corrected 2-10 keV luminosity of similar to 10(45) erg s(-1). Outflows driven by an accretion disk may produce the double-peaked lines if the central engine accretes near the Eddington limit. However, we may be seeing the narrow line regions of two AGNs following a galactic merger. While the AO image reveals only a single source, a second AGN would easily be obscured by the significant extinction inferred from the X-ray data. Understanding the physical processes producing the complex emission line profiles seen in CXOJ1426+35 and related sources is important for interpreting the growing population of dual AGN candidates. C1 [Barrows, R. Scott] Univ Arkansas, Arkansas Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA. [Stern, Daniel; Assef, Roberto J.; Cushing, Michael C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Madsen, Kristin; Harrison, Fiona] CALTECH, Pasadena, CA 91125 USA. [Comerford, Julia M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Fassnacht, Christopher D.; Lagattuta, David J.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Griffith, Roger; Kirkpatrick, J. Davy] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Hickox, Ryan] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Barrows, RS (reprint author), Univ Arkansas, Arkansas Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA. EM rbarrows@uark.edu OI Madsen, Kristin/0000-0003-1252-4891 FU National Science Foundation [AST-0708490]; Strategic University Research Partnership Program; National Aeronautics and Space Administration; W. M. Keck Foundation; Smithsonian Astrophysical Observatory [SV4-74018, A31] FX The authors thank an anonymous referee for helpful comments that greatly improved the quality of the paper. The authors gratefully acknowledge discussions on similar dual AGN candidates with close collaborators, especially Claud Lacy, Daniel Kennefick, Julia Kennefick, and Joel Berrier. R.S.B. is also grateful to D.S. for funding an extended visit to JPL in Summer 2010. A.H.G. acknowledges support from the National Science Foundation under grant AST-0708490. This research was partially carried out at the Jet Propulsion Laboratory/California Institute of Technology and was sponsored by the Strategic University Research Partnership Program and the National Aeronautics and Space Administration. This work is based in part on observations 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. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This work is based in part on observations obtained with Chandra, under contract SV4-74018, A31 with the Smithsonian Astrophysical Observatory which operates the CXO for NASA. This work makes use of image data from the NOAO Deep Wide-Field Survey (NDWFS) as distributed by the NOAO Science Archive. NOAO is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under a cooperative agreement with the National Science Foundation. This paper would not have been possible without the efforts of the Spitzer, Chandra, and Keck support staff. NR 125 TC 21 Z9 21 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2012 VL 744 IS 1 AR 7 DI 10.1088/0004-637X/744/1/7 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866TY UT WOS:000298408300007 ER PT J AU Braun, DC Birch, AC Rempel, M Duvall, TL AF Braun, D. C. Birch, A. C. Rempel, M. Duvall, T. L., Jr. TI HELIOSEISMOLOGY OF A REALISTIC MAGNETOCONVECTIVE SUNSPOT SIMULATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: helioseismology; Sun: interior ID TIME-DISTANCE HELIOSEISMOLOGY; FOCUSED SEISMIC HOLOGRAPHY; INCLINED MAGNETIC-FIELDS; ACOUSTIC-WAVE-FIELD; LOCAL HELIOSEISMOLOGY; SOUND-SPEED; NUMERICAL SIMULATIONS; SUBSURFACE STRUCTURE; SOLAR CONVECTION; DOPPLER IMAGER AB We compare helioseismic travel-time shifts measured from a realistic magnetoconvective sunspot simulation using both helioseismic holography and time-distance helioseismology, and measured from real sunspots observed with the Helioseismic and Magnetic Imager instrument on board the Solar Dynamics Observatory and the Michelson Doppler Imager instrument on board the Solar and Heliospheric Observatory. We find remarkable similarities in the travel-time shifts measured between the methodologies applied and between the simulated and real sunspots. Forward modeling of the travel-time shifts using either Born or ray approximation kernels and the sound-speed perturbations present in the simulation indicates major disagreements with the measured travel-time shifts. These findings do not substantially change with the application of a correction for the reduction of wave amplitudes in the simulated and real sunspots. Overall, our findings demonstrate the need for new methods for inferring the subsurface structure of sunspots through helioseismic inversions. C1 [Braun, D. C.; Birch, A. C.] NW Res Associates, Boulder, CO 80301 USA. [Rempel, M.] Natl Ctr Atmospher Res, HAO Div, Boulder, CO 80301 USA. [Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. RP Braun, DC (reprint author), NW Res Associates, 3380 Mitchell Lane, Boulder, CO 80301 USA. EM dbraun@cora.nwra.com; aaronb@cora.nwra.com; renpel@ucar.edu; Thomas.L.Duvall@nasa.gov RI Duvall, Thomas/C-9998-2012 FU NASA SDO Science Center [NNH09CE41C, NNH09AK021, SCEX22011D]; NASA [NNG07EI51C]; NASA; National Science Foundation FX This work is supported by the NASA SDO Science Center program through contract NNH09CE41C awarded to NWRA, grant NNH09AK021 awarded to NCAR, and grant SCEX22011D awarded to NASA GSFC. Additional support is provided by the NASA Heliophysics GI program through contract NNG07EI51C awarded to NWRA and a subcontract through the NASA sponsored HMI project at Stanford University awarded to NWRA. The National Center for Atmospheric Research is sponsored by the National Science Foundation. SOHO is a project of international cooperation between ESA and NASA. SDO data are provided courtesy of NASA/SDO and the AIA, EVE, and HMI science teams. The authors acknowledge the Texas Advanced Computing Center (TACC) at The University of Texas at Austin for providing HPC resources that have contributed to the research results reported within this paper. We thank the referee for useful comments which helped to improve the manuscript. NR 65 TC 14 Z9 14 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2012 VL 744 IS 1 AR 77 DI 10.1088/0004-637X/744/1/77 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866TY UT WOS:000298408300077 ER PT J AU Burlaga, LF Ness, NF AF Burlaga, L. F. Ness, N. F. TI MAGNETIC FIELD STRENGTH FLUCTUATIONS IN THE HELIOSHEATH: VOYAGER 1 OBSERVATIONS DURING 2009 SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun: heliosphere ID SOLAR-WIND; MULTIFRACTAL STRUCTURE; STATISTICAL-MECHANICS; VELOCITY FLUCTUATION; RECURRENT STREAMS; TURBULENCE; AU; FRACTALS; MODEL; HOLES AB We analyze the "microscale fluctuations" of the magnetic field strength B on a scale of several hours observed by Voyager1 (V1) in the heliosheath during 2009. The microscale fluctuations of B range from coherent to stochastic structures. The amplitude of microscale fluctuations of B during 1 day is measured by the standard deviation (SD) of 48 s averages of B. The distribution of the daily values of SD is lognormal. SD(t) from day of year (DOY) 1 to 331, 2009, is very intermittent. SD(t) has a 1/f or "pink noise" spectrum on scales from 1 to 100 days, and it has a broad multifractal spectrum f(alpha) with 0.57 <= alpha <= 1.39. The time series of increments SD(t + tau) - SD(t) has a pink noise spectrum with alpha' = 0.88 +/- 0.14 on scales from 1 to 100 days. The increments have a Tsallis (q-Gaussian) distribution on scales from 1 to 165 days, with an average q = 1.75 +/- 0.12. The skewness S and kurtosis K have Gaussian and lognormal distributions, respectively. The largest spikes in K(t) and S(t) are often associated with a change in B across a data gap and with identifiable physical structures. The "turbulence" observed by V1 during 2009 was weakly compressible on average but still very intermittent, highly variable, and highly compressible at times. The turbulence observed just behind the termination shock by Voyager 2 was twice as strong. These observations place strong constraints on any model of "turbulence" in the heliosheath. C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Code 673, Greenbelt, MD 20771 USA. EM lburlagahsp@verizon.net; nfnudel@yahoo.com FU [NNX10AU53G] FX The data in this paper are from the magnetic field experiment on Voyager 1. N. F. Ness was partially supported by grant NNX10AU53G to the Catholic University of America. McClanahan and S. Kramer carried out the processing of the data. The "0-offset tables" were computed by D. Berdichevsky. NR 51 TC 12 Z9 12 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2012 VL 744 IS 1 AR 51 DI 10.1088/0004-637X/744/1/51 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866TY UT WOS:000298408300051 ER PT J AU Foley, RJ Challis, PJ Filippenko, AV Ganeshalingam, M Landsman, W Li, W Marion, GH Silverman, JM Beaton, RL Bennert, VN Cenko, SB Childress, M Guhathakurta, P Jiang, L Kalirai, JS Kirshner, RP Stockton, A Tollerud, EJ Vinko, J Wheeler, JC Woo, JH AF Foley, Ryan J. Challis, P. J. Filippenko, A. V. Ganeshalingam, M. Landsman, W. Li, W. Marion, G. H. Silverman, J. M. Beaton, R. L. Bennert, V. N. Cenko, S. B. Childress, M. Guhathakurta, P. Jiang, L. Kalirai, J. S. Kirshner, R. P. Stockton, A. Tollerud, E. J. Vinko, J. Wheeler, J. C. Woo, J. -H. TI VERY EARLY ULTRAVIOLET AND OPTICAL OBSERVATIONS OF THE TYPE Ia SUPERNOVA 2009ig SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (SN 2009g) ID HUBBLE-SPACE-TELESCOPE; HOBBY-EBERLY TELESCOPE; LIGHT CURVES; LEGACY SURVEY; DARK ENERGY; RISE TIMES; IMPROVED DISTANCES; STANDARD STARS; K-CORRECTIONS; SWIFT UVOT AB Supernova (SN) 2009ig was discovered 17 hr after explosion by the Lick Observatory Supernova Search, promptly classified as a normal Type Ia SN (SN Ia), peaked at V = 13.5 mag, and was equatorial, making it one of the foremost SNe for intensive study in the last decade. Here, we present ultraviolet (UV) and optical observations of SN 2009ig, starting about 1 day after explosion until around maximum brightness. Our data include excellent UV and optical light curves, 25 premaximum optical spectra, and 8 UV spectra, including the earliest UV spectrum ever obtained of an SN Ia. SN 2009ig is a relatively normal SN Ia, but does display high-velocity ejecta-the ejecta velocity measured in our earliest spectra (v approximate to -23,000 km s(-1) for Si ii.6355) is the highest yet measured in an SN Ia. The spectral evolution is very dramatic at times earlier than 12 days before maximum brightness, but slows after that time. The early-time data provide a precise measurement of 17.13 +/- 0.07 days for the SN rise time. The optical color curves and early-time spectra are significantly different from template light curves and spectra used for light-curve fitting and K-corrections, indicating that the template light curves and spectra do not properly represent all SNe Ia at very early times. In the age of wide-angle sky surveys, SNe like SN 2009ig that are nearby, bright, well positioned, and promptly discovered will still be rare. As shown with SN 2009ig, detailed studies of single events can provide significantly more information for testing systematic uncertainties related to SN Ia distance estimates and constraining progenitor and explosion models than large samples of more distant SNe. C1 [Foley, Ryan J.; Challis, P. J.; Marion, G. H.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Filippenko, A. V.; Ganeshalingam, M.; Li, W.; Silverman, J. M.; Cenko, S. B.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Landsman, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Beaton, R. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Bennert, V. N.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Childress, M.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Childress, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Guhathakurta, P.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Jiang, L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Kalirai, J. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Stockton, A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Tollerud, E. J.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA. [Vinko, J.] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Vinko, J.; Wheeler, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Woo, J. -H.] Seoul Natl Univ, Astron Program, Dept Phys & Astron, Seoul 151742, South Korea. RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rfoley@cfa.harvard.edu RI Woo, Jong-Hak/A-2790-2014; OI Tollerud, Erik/0000-0002-9599-310X; Beaton, Rachael/0000-0002-1691-8217 FU NSF [AST-0907903, AST-0908886, AST-0707769]; NASA [NNX09AG54G, NNX10AF52G]; Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund; TABASGO Foundation; Hungarian OTKA [K76816]; Texas Advanced Research Project grant [ARP-0094]; W. M. Keck Foundation; Sun Microsystems, Inc.; Hewlett-Packard Company; AutoScope Corporation; Lick Observatory; University of California; Sylvia & Jim Katzman Foundation; [GI-5080130] FX R.J.F. is supported by a Clay Fellowship. We thank the anonymous referee for informed comments and suggestions. We thank D. Kasen for useful discussions. We are grateful to the staffs at the Lick, Keck, HET, and MMT Observatories for their dedicated services. J. Bullock, J. Caldwell, M. Kandrashoff, A. Morton, P. Nugent, S. Odewahn, D. Poznanski, S. Rostopchin, H.-Y. Shih, F. Vilas, and G. Williams helped obtain some of the data presented here; we also thank J. Lee and D. Tytler for attempting to obtain data. Swift spectroscopic observations were performed under program GI-5080130; we are very grateful to N. Gehrels and the Swift team for executing the program quickly. Supernova research at Harvard is supported by NSF grant AST-0907903. A.V.F.'s supernova group at U. C. Berkeley is supported by NASA/Swift grants NNX09AG54G and NNX10AF52G, NSF grant AST-0908886, Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, and the TABASGO Foundation. J. V. received support from Hungarian OTKA Grant K76816, NSF Grant AST-0707769, and Texas Advanced Research Project grant ARP-0094.; 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. The Hobby-Eberly Telescope (HET) is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universitat Munchen, and Georg-August-Universitat Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. We acknowledge the use of public data from the Swift data archive. KAIT was constructed and supported by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 87 TC 66 Z9 67 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2012 VL 744 IS 1 AR 38 DI 10.1088/0004-637X/744/1/38 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866TY UT WOS:000298408300038 ER PT J AU Gopalswamy, N Nitta, N Akiyama, S Makela, P Yashiro, S AF Gopalswamy, Nat Nitta, Nariaki Akiyama, Sachiko Maekela, Pertti Yashiro, Seiji TI CORONAL MAGNETIC FIELD MEASUREMENT FROM EUV IMAGES MADE BY THE SOLAR DYNAMICS OBSERVATORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; shock waves; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: radio radiation ID INTERPLANETARY SPACE; STANDOFF DISTANCE; SHOCK-WAVES; BOW SHOCK; NEAR-SUN; STRENGTH; SDO/AIA; MODEL AB By measuring the geometrical properties of the coronal mass ejection (CME) flux rope and the leading shock observed on 2010 June 13 by the Solar Dynamics Observatory (SDO) mission's Atmospheric Imaging Assembly we determine the Alfven speed and the magnetic field strength in the inner corona at a heliocentric distance of similar to 1.4 Rs. The basic measurements are the shock standoff distance (Delta R) ahead of the CME flux rope, the radius of curvature of the flux rope (R-c), and the shock speed. We first derive the Alfvenic Mach number (M) using the relationship, Delta R/R-c = 0.81[(gamma - 1) M-2 + 2]/[(gamma + 1)(M-2 - 1)], where gamma is the only parameter that needed to be assumed. For gamma = 4/3, the Mach number declined from 3.7 to 1.5 indicating shock weakening within the field of view of the imager. The shock formation coincided with the appearance of a type II radio burst at a frequency of similar to 300 MHz (harmonic component), providing an independent confirmation of the shock. The shock compression ratio derived from the radio dynamic spectrum was found to be consistent with that derived from the theory of fast-mode MHD shocks. From the measured shock speed and the derived Mach number, we found the Alfven speed to increase from similar to 140 km s(-1) to 460 km s(-1) over the distance range 1.2-1.5 Rs. By deriving the upstream plasma density from the emission frequency of the associated type II radio burst, we determined the coronal magnetic field to be in the range 1.3-1.5 G. The derived magnetic field values are consistent with other estimates in a similar distance range. This work demonstrates that the EUV imagers, in the presence of radio dynamic spectra, can be used as coronal magnetometers. C1 [Gopalswamy, Nat; Akiyama, Sachiko; Maekela, Pertti; Yashiro, Seiji] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nitta, Nariaki] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Akiyama, Sachiko; Maekela, Pertti; Yashiro, Seiji] Catholic Univ Amer, Washington, DC 20064 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Gopalswamy, Nat/D-3659-2012; OI Gopalswamy, Nat/0000-0001-5894-9954 FU NASA FX Work supported by NASA's LWS program. NR 28 TC 44 Z9 44 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 JAN 1 PY 2012 VL 744 IS 1 AR 72 DI 10.1088/0004-637X/744/1/72 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866TY UT WOS:000298408300072 ER PT J AU Green, JC Froning, CS Osterman, S Ebbets, D Heap, SH Leitherer, C Linsky, JL Savage, BD Sembach, K Shull, JM Siegmund, OHW Snow, TP Spencer, J Stern, SA Stocke, J Welsh, B Beland, S Burgh, EB Danforth, C France, K Keeney, B McPhate, J Penton, SV Andrews, J Brownsberger, K Morse, J Wilkinson, E AF Green, James C. Froning, Cynthia S. Osterman, Steve Ebbets, Dennis Heap, Sara H. Leitherer, Claus Linsky, Jeffrey L. Savage, Blair D. Sembach, Kenneth Shull, J. Michael Siegmund, Oswald H. W. Snow, Theodore P. Spencer, John Stern, S. Alan Stocke, John Welsh, Barry Beland, Stephane Burgh, Eric B. Danforth, Charles France, Kevin Keeney, Brian McPhate, Jason Penton, Steven V. Andrews, John Brownsberger, Kenneth Morse, Jon Wilkinson, Erik TI THE COSMIC ORIGINS SPECTROGRAPH SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: spectrographs; ultraviolet: general ID LY-ALPHA FOREST; ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; FLUORESCENT H-2 EMISSION; HOT INTERGALACTIC MEDIUM; HUBBLE-SPACE-TELESCOPE; STAR-FORMING GALAXIES; HIGH-VELOCITY CLOUD; LOW-REDSHIFT; T-TAURI; HST/COS OBSERVATIONS AB The Cosmic Origins Spectrograph (COS) is a moderate-resolution spectrograph with unprecedented sensitivity that was installed into the Hubble Space Telescope (HST) in 2009 May, during HST Servicing Mission 4 (STS-125). We present the design philosophy and summarize the key characteristics of the instrument that will be of interest to potential observers. For faint targets, with flux F(lambda) approximate to 1.0 x 10(-14) erg cm(-2) s(-1) angstrom(-1), COS can achieve comparable signal to noise (when compared to Space Telescope Imaging Spectrograph echelle modes) in 1%-2% of the observing time. This has led to a significant increase in the total data volume and data quality available to the community. For example, in the first 20 months of science operation (2009 September-2011 June) the cumulative redshift pathlength of extragalactic sight lines sampled by COS is nine times than sampled at moderate resolution in 19 previous years of Hubble observations. COS programs have observed 214 distinct lines of sight suitable for study of the intergalactic medium as of 2011 June. COS has measured, for the first time with high reliability, broad Ly alpha absorbers and Ne VIII in the intergalactic medium, and observed the He II reionization epoch along multiple sightlines. COS has detected the first CO emission and absorption in the UV spectra of low-mass circumstellar disks at the epoch of giant planet formation, and detected multiple ionization states of metals in extra-solar planetary atmospheres. In the coming years, COS will continue its census of intergalactic gas, probe galactic and cosmic structure, and explore physics in our solar system and Galaxy. C1 [Green, James C.; Shull, J. Michael; Snow, Theodore P.; Stocke, John] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Green, James C.; Froning, Cynthia S.; Osterman, Steve; Shull, J. Michael; Snow, Theodore P.; Stocke, John; Beland, Stephane; Burgh, Eric B.; Danforth, Charles; France, Kevin; Keeney, Brian; Penton, Steven V.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Ebbets, Dennis; Brownsberger, Kenneth] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA. [Heap, Sara H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Leitherer, Claus; Sembach, Kenneth] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Linsky, Jeffrey L.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Linsky, Jeffrey L.] NIST, Boulder, CO 80309 USA. [Savage, Blair D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Siegmund, Oswald H. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Spencer, John; Stern, S. Alan; Andrews, John; Wilkinson, Erik] SW Res Inst, Boulder, CO 80302 USA. [Welsh, Barry; McPhate, Jason] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Morse, Jon] NASA Headquarters, Washington, DC 20546 USA. RP Green, JC (reprint author), Univ Colorado, Dept Astrophys & Planetary Sci, 391-UCB, Boulder, CO 80309 USA. FU NASA [NAS5-98043, NAG5-12279, NNX08AC14G] FX The authors thank the entire team at Goddard Space Flight Center, Ball Aerospace, JY Horiba, and the Space Telescope Science Institute for making the Cosmic Origins Spectrograph a reality. Literally hundreds of people contributed to its success. We especially thank Hsiao Smith, Jean Flammand, Francis Bonnemason, and Francis Cepollina for their years of service to the program. We also thank Gregory Herczeg for providing the AA Tau data. This work was supported by NASA programs NAS5-98043, NAG5-12279, and NNX08AC14G. NR 84 TC 158 Z9 158 U1 2 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2012 VL 744 IS 1 AR 60 DI 10.1088/0004-637X/744/1/60 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866TY UT WOS:000298408300060 ER PT J AU Guillemot, L Johnson, TJ Venter, C Kerr, M Pancrazi, B Livingstone, M Janssen, GH Jaroenjittichai, P Kramer, M Cognard, I Stappers, BW Harding, AK Camilo, F Espinoza, CM Freire, PCC Gargano, F Grove, JE Johnston, S Michelson, PF Noutsos, A Parent, D Ransom, SM Ray, PS Shannon, R Smith, DA Theureau, G Thorsett, SE Webb, N AF Guillemot, L. Johnson, T. J. Venter, C. Kerr, M. Pancrazi, B. Livingstone, M. Janssen, G. H. Jaroenjittichai, P. Kramer, M. Cognard, I. Stappers, B. W. Harding, A. K. Camilo, F. Espinoza, C. M. Freire, P. C. C. Gargano, F. Grove, J. E. Johnston, S. Michelson, P. F. Noutsos, A. Parent, D. Ransom, S. M. Ray, P. S. Shannon, R. Smith, D. A. Theureau, G. Thorsett, S. E. Webb, N. TI PULSED GAMMA RAYS FROM THE ORIGINAL MILLISECOND AND BLACK WIDOW PULSARS: A CASE FOR CAUSTIC RADIO EMISSION? SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: general; pulsars: general; pulsars: individual (PSR B1937+21, PSR B1957+20); radiation mechanisms: non-thermal ID LARGE-AREA TELESCOPE; BLIND FREQUENCY SEARCHES; HIGH-ENERGY EMISSION; FERMI LAT; PSR B1957+20; LIGHT CURVES; MONTE-CARLO; TIMING OBSERVATIONS; SPACE-TELESCOPE; POLARIZATION AB We report the detection of pulsed gamma-ray emission from the fast millisecond pulsars (MSPs) B1937+21 (also known as J1939+2134) and B1957+20 (J1959+2048) using 18 months of survey data recorded by the Fermi Large Area Telescope and timing solutions based on radio observations conducted at the Westerbork and Nancay radio telescopes. In addition, we analyzed archival Rossi X-ray Timing Explorer and XMM-Newton X-ray data for the two MSPs, confirming the X-ray emission properties of PSR B1937+21 and finding evidence (similar to 4 sigma) for pulsed emission from PSR B1957+20 for the first time. In both cases the gamma-ray emission profile is characterized by two peaks separated by half a rotation and are in close alignment with components observed in radio and X-rays. These two pulsars join PSRs J0034-0534 and J2214+3000 to form an emerging class of gamma-ray MSPs with phase-aligned peaks in different energy bands. The modeling of the radio and gamma-ray emission profiles suggests co-located emission regions in the outer magnetosphere. C1 [Guillemot, L.; Kramer, M.; Freire, P. C. C.; Noutsos, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Johnson, T. J.; Harding, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Johnson, T. J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Johnson, T. J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Johnson, T. J.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Venter, C.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Kerr, M.; Michelson, P. F.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Kerr, M.; Michelson, P. F.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Pancrazi, B.; Webb, N.] CNRS, IRAP, F-31028 Toulouse 4, France. [Pancrazi, B.; Webb, N.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France. [Livingstone, M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Janssen, G. H.; Jaroenjittichai, P.; Kramer, M.; Stappers, B. W.; Espinoza, C. M.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Cognard, I.; Theureau, G.] CNRS, LPCE, UMR 6115, Lab Phys & Chim Environm, F-45071 Orleans 02, France. [Cognard, I.; Theureau, G.] Observ Paris, CNRS, INSU, Stn Radioastron Nancay, F-18330 Nancay, France. [Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Gargano, F.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Grove, J. E.; Ray, P. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Johnston, S.; Shannon, R.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Parent, D.] George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA. [Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Smith, D. A.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Thorsett, S. E.] Willamette Univ, Dept Phys, Salem, OR 97031 USA. RP Guillemot, L (reprint author), Max Planck Inst Radioastron, D-53121 Bonn, Germany. EM guillemo@mpifr-bonn.mpg.de; tyrel.j.johnson@gmail.com; Christo.Venter@nwu.ac.za; kerrm@stanford.edu RI Harding, Alice/D-3160-2012; Venter, Christo/E-6884-2011; Gargano, Fabio/O-8934-2015; OI Venter, Christo/0000-0002-2666-4812; Gargano, Fabio/0000-0002-5055-6395; Thorsett, Stephen/0000-0002-2025-9613; Shannon, Ryan/0000-0002-7285-6348; Ransom, Scott/0000-0001-5799-9714; Ray, Paul/0000-0002-5297-5278 FU National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council and the Swedish National Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden.; Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. NR 73 TC 41 Z9 41 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2012 VL 744 IS 1 AR 33 DI 10.1088/0004-637X/744/1/33 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866TY UT WOS:000298408300033 ER PT J AU Hajian, A Viero, MP Addison, G Aguirre, P Appel, JW Battaglia, N Bock, JJ Bond, JR Das, S Devlin, MJ Dicker, SR Dunkley, J Dunner, R Essinger-Hileman, T Hughes, JP Fowler, JW Halpern, M Hasselfield, M Hilton, M Hincks, AD Hlozek, R Irwin, KD Klein, J Kosowsky, A Lin, YT Marriage, TA Marsden, D Marsden, G Menanteau, F Moncelsi, L Moodley, K Netterfield, CB Niemack, MD Nolta, MR Page, LA Parker, L Patanchon, G Scott, D Sehgal, N Sievers, J Spergel, DN Staggs, ST Swetz, DS Switzer, ER Thornton, R Wollack, E AF Hajian, Amir Viero, Marco P. Addison, Graeme Aguirre, Paula Appel, John William Battaglia, Nick Bock, James J. Bond, J. Richard Das, Sudeep Devlin, Mark J. Dicker, Simon R. Dunkley, Joanna Duenner, Rolando Essinger-Hileman, Thomas Hughes, John P. Fowler, Joseph W. Halpern, Mark Hasselfield, Matthew Hilton, Matt Hincks, Adam D. Hlozek, Renee Irwin, Kent D. Klein, Jeff Kosowsky, Arthur Lin, Yen-Ting Marriage, Tobias A. Marsden, Danica Marsden, Gaelen Menanteau, Felipe Moncelsi, Lorenzo Moodley, Kavilan Netterfield, Calvin B. Niemack, Michael D. Nolta, Michael R. Page, Lyman A. Parker, Lucas Patanchon, Guillaume Scott, Douglas Sehgal, Neelima Sievers, Jon Spergel, David N. Staggs, Suzanne T. Swetz, Daniel S. Switzer, Eric R. Thornton, Robert Wollack, Ed TI CORRELATIONS IN THE (SUB) MILLIMETER BACKGROUND FROM ACT x BLAST SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: evolution; infrared: galaxies; large-scale structure of universe; submillimeter: galaxies ID ATACAMA COSMOLOGY TELESCOPE; SOUTH-POLE TELESCOPE; APERTURE SUBMILLIMETER TELESCOPE; ANGULAR POWER SPECTRA; STAR-FORMING GALAXIES; DEEP FIELD-SOUTH; NUMBER COUNTS; STATISTICAL PROPERTIES; SOURCE CATALOGS; ARRAY CAMERA AB We present measurements of the auto- and cross-frequency correlation power spectra of the cosmic (sub) millimeter background at 250, 350, and 500 mu m (1200, 860, and 600 GHz) from observations made with the Balloonborne Large Aperture Submillimeter Telescope (BLAST); and at 1380 and 2030 mu m (218 and 148 GHz) from observations made with the Atacama Cosmology Telescope (ACT). The overlapping observations cover 8.6 deg(2) in an area relatively free of Galactic dust near the south ecliptic pole. The ACT bands are sensitive to radiation from the cosmic microwave background, to the Sunyaev-Zel'dovich effect from galaxy clusters, and to emission by radio and dusty star-forming galaxies (DSFGs), while the dominant contribution to the BLAST bands is from DSFGs. We confirm and extend the BLAST analysis of clustering with an independent pipeline and also detect correlations between the ACT and BLAST maps at over 25 sigma significance, which we interpret as a detection of the DSFGs in the ACT maps. In addition to a Poisson component in the cross-frequency power spectra, we detect a clustered signal at 4 sigma, and using a model for the DSFG evolution and number counts, we successfully fit all of our spectra with a linear clustering model and a bias that depends only on redshift and not on scale. Finally, the data are compared to, and generally agree with, phenomenological models for the DSFG population. This study demonstrates the constraining power of the cross-frequency correlation technique to constrain models for the DSFGs. Similar analyses with more data will impose tight constraints on future models. C1 [Hajian, Amir; Battaglia, Nick; Bond, J. Richard; Nolta, Michael R.; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Hajian, Amir; Das, Sudeep; Dunkley, Joanna; Marriage, Tobias A.; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Hajian, Amir; Appel, John William; Das, Sudeep; Dunkley, Joanna; Duenner, Rolando; Essinger-Hileman, Thomas; Fowler, Joseph W.; Hincks, Adam D.; Niemack, Michael D.; Page, Lyman A.; Parker, Lucas; Staggs, Suzanne T.; Switzer, Eric R.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Viero, Marco P.; Bock, James J.] CALTECH, Pasadena, CA 91125 USA. [Viero, Marco P.; Netterfield, Calvin B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Addison, Graeme; Dunkley, Joanna; Hlozek, Renee] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Aguirre, Paula] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Bock, James J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA. [Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Devlin, Mark J.; Dicker, Simon R.; Klein, Jeff; Marsden, Danica; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Fowler, Joseph W.; Irwin, Kent D.; Niemack, Michael D.; Swetz, Daniel S.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Halpern, Mark; Marsden, Danica; Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Hasselfield, Matthew; Patanchon, Guillaume] Univ Paris Diderot, Lab APC, F-75205 Paris, France. [Hilton, Matt; Moodley, Kavilan] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Sci, ZA-4041 Durban, South Africa. [Hilton, Matt] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan. [Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Moncelsi, Lorenzo] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Sehgal, Neelima] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Switzer, Eric R.] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Thornton, Robert] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA. [Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hajian, A (reprint author), Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. RI Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Hilton, Matthew James/N-5860-2013; Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU NASA [NAG5-12785, NAG5-13301, NNGO-6GI11G, NNX08AH30G]; NSF Office of Polar Programs; Canadian Space Agency; Natural Sciences and Engineering Research Council (NSERC) of Canada; UK Science and Technology Facilities Council (STFC); Canadian Institute for Advanced Research; U.S. National Science Foundation [AST- 0408698, PHY-0355328, AST- 0707731, PIRE-0507768]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation; Compute Canada; Government of Ontario; Ontario Research Fund-Research Excellence; University of Toronto; RCUK Fellowship; NSF [AST-0546035, AST-0606975]; NSF Physics Frontier Center [PHY-0114422]; Berkeley Center for Cosmological Physics FX BLAST was made possible through the support of NASA through grant Nos. NAG5-12785, NAG5-13301, and NNGO-6GI11G, the NSF Office of Polar Programs, the Canadian Space Agency, the Natural Sciences and Engineering Research Council (NSERC) of Canada, and the UK Science and Technology Facilities Council (STFC). C.B.N. acknowledges support from the Canadian Institute for Advanced Research.; ACT was supported by the U.S. National Science Foundation through awards AST- 0408698 for the ACT project, and PHY-0355328, AST- 0707731, and PIRE-0507768. Funding was also provided by Princeton University and the University of Pennsylvania. Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund-Research Excellence; and the University of Toronto. J.D. acknowledges support from an RCUK Fellowship. S. D., A. H., and T. M. were supported through NASA grant NNX08AH30G. A. K. was partially supported through NSF AST-0546035 and AST-0606975 for work on ACT. E. S. acknowledges support by NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics. S. D. acknowledges support from the Berkeley Center for Cosmological Physics. We thank CONICYT for overseeing the Chajnantor Science Preserve, enabling instruments like ACT to operate in Chile; and we thank AstroNorte for operating our scientific base station. Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) package. NR 72 TC 18 Z9 18 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 JAN 1 PY 2012 VL 744 IS 1 AR 40 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866TY UT WOS:000298408300040 ER PT J AU Hornbeck, JB Grady, CA Perrin, MD Wisniewski, JP Tofflemire, BM Brown, A Holtzman, JA Arraki, K Hamaguchi, K Woodgate, B Petre, R Daly, B Grogin, NA Bonfield, DG Williger, GM Lauroesch, JT AF Hornbeck, J. B. Grady, C. A. Perrin, M. D. Wisniewski, J. P. Tofflemire, B. M. Brown, A. Holtzman, J. A. Arraki, K. Hamaguchi, K. Woodgate, B. Petre, R. Daly, B. Grogin, N. A. Bonfield, D. G. Williger, G. M. Lauroesch, J. T. TI PDS 144: THE FIRST CONFIRMED Herbig Ae-Herbig Ae WIDE BINARY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Herbig-Haro objects; ISM: jets and outflows; protoplanetary disks; stars: individual (IRAS 15462-2551, TYC 6782-878-1); stars: variables: T Tauri, Herbig Ae/Be ID T-TAURI STARS; INTERMEDIATE-MASS STARS; YOUNG BINARIES; OB ASSOCIATION; AE/BE STARS; SCORPIUS; MULTIPLICITY; HD-163296; OUTFLOWS; CATALOG AB PDS 144 is a pair of Herbig Ae stars that are separated by 5.'' 35 on the sky. It has previously been shown to have an A2Ve Herbig Ae star viewed at 83 degrees inclination as its northern member and an A5Ve Herbig Ae star as its southern member. Direct imagery revealed a disk occulting PDS 144 N-the first edge-on disk observed around a Herbig Ae star. The lack of an obvious disk in direct imagery suggested PDS 144 S might be viewed face-on or not physically associated with PDS 144 N. Multi-epoch Hubble Space Telescope imagery of PDS 144 with a 5 year baseline demonstrates PDS 144 N & S are comoving and have a common proper motion with TYC 6782-878-1. TYC 6782-878-1 has previously been identified as a member of Upper Sco sub-association A at d = 145 +/- 2 pc with an age of 5-10 Myr. Ground-based imagery reveals jets and a string of Herbig-Haro knots extending 13' (possibly further) which are aligned to within 7 degrees +/- 6 degrees on the sky. By combining proper motion data and the absence of a dark mid-plane with radial velocity data, we measure the inclination of PDS 144 S to be i = 73 degrees +/- 7 degrees. The radial velocity of the jets from PDS 144 N & S indicates they, and therefore their disks, are misaligned by 25 degrees +/- 9 degrees. This degree of misalignment is similar to that seen in T Tauri wide binaries. C1 [Hornbeck, J. B.; Williger, G. M.; Lauroesch, J. T.] Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. [Grady, C. A.] Eureka Sci, Oakland, CA 96402 USA. [Grady, C. A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Perrin, M. D.; Grogin, N. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Wisniewski, J. P.; Tofflemire, B. M.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Tofflemire, B. M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Brown, A.] Univ Colorado, CASA, Boulder, CO 80309 USA. [Holtzman, J. A.; Arraki, K.] New Mexico State Univ, Dept Astron, Dept 4500, Las Cruces, NM 88003 USA. [Hamaguchi, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Hamaguchi, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Hamaguchi, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Daly, B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Bonfield, D. G.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Williger, G. M.] Univ Nice, UMR 6525, Lab Fizeau, F-06108 Nice 2, France. RP Hornbeck, JB (reprint author), Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. RI Woodgate, Bruce/D-2970-2012 FU NASA [NAS 5-26555]; NSF [AST 08-02230, AST-0702933]; Kentucky Science and Engineering Foundation [KSEF-148-502-08-241]; Kentucky Science and Technology Corporation; NASA Kentucky Space Grant Consortium [3049024102-11-175]; NASA; [HST-GO-11155]; [HST-GO-12016]; [11200435] FX This work, in part, 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 programs HST-GO-11155, HST-GO-12016, Chandra program 11200435, and NASA RTOP 399131.02.02.02.32 to Goddard Space Flight Center. The first epoch ACS data used in this study were obtained under HST GO 10603 (PI: Deborah Padgett). Data used in this study were also obtained at the Lick Observatory Shane 3 m telescope and the Apache Point Observatory 3.5 m. The Apache Point observations were made under a grant of Director's Discretionary Time. J. P. W. is supported by NSF Astronomy and Astrophysics Postdoctoral Fellowship, AST 08-02230. M. D. P. was supported in part by an NSF Astronomy and Astrophysics Postdoctoral Fellowship, AST-0702933. This researchwas supported in part by a grant from the Kentucky Science and Engineering Foundation as per Grant Agreement KSEF-148-502-08-241 with the Kentucky Science and Technology Corporation and NASA Kentucky Space Grant Consortium Award 3049024102-11-175. D. G. B. was partly supported by a NASA Postdoctoral Program Fellowship administered by Oak Ridge Associated Universities. K. A. acknowledges her NSF Graduate Research Fellowhip. NR 36 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2012 VL 744 IS 1 AR 54 DI 10.1088/0004-637X/744/1/54 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866TY UT WOS:000298408300054 ER PT J AU Plume, R Bergin, EA Phillips, TG Lis, DC Wang, S Crockett, NR Caux, E Comito, C Goldsmith, PF Schilke, P AF Plume, R. Bergin, E. A. Phillips, T. G. Lis, D. C. Wang, S. Crockett, N. R. Caux, E. Comito, C. Goldsmith, P. F. Schilke, P. TI A DIRECT MEASUREMENT OF THE TOTAL GAS COLUMN DENSITY IN ORION KL SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: individual objects (Orion KL); ISM: molecules ID MOLECULAR CLOUD CORES; STAR-FORMATION; (CO)-O-18/(CO)-O-17 RATIO; COLOGNE DATABASE; SPECTRAL SURVEYS; LINE SURVEY; SUBMILLIMETER; SPECTROSCOPY; ABUNDANCES; MILLIMETER AB The large number of high-J lines of C(18)O available via the Herschel Space Observatory provide an unprecedented ability to model the total CO column density in hot cores. Using the emission from all the observed lines (up to J = 15-14), we sum the column densities in each individual level to obtain the total column after correcting for the population in the unobserved states. With additional knowledge of source size, V(LSR), and line width, and both local thermodynamic equilibrium (LTE) and non-LTE modeling, we have determined the total C18O column densities in the Extended Ridge, Outflow/Plateau, Compact Ridge, and Hot Core components of Orion KL to be 1.4 x 10(16) cm(-2), 3.5 x 10(16) cm(-2), 2.2 x 10(16) cm(-2), and 6.2 x 10(16) cm(-2), respectively. We also find that the C(18)O/C(17)O abundance ratio varies from 1.7 in the Outflow/Plateau, 2.3 in the Extended Ridge, 3.0 in the Hot Core, and to 4.1 in the Compact Ridge. This is in agreement with models in which regions with higher ultraviolet radiation fields selectively dissociate C(17)O, although care must be taken when interpreting these numbers due to the size of the uncertainties in the C(18)O/C(17)O abundance ratio. C1 [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Plume, R.] Univ Calgary, Inst Space Imaging Sci, Calgary, AB T2N 1N4, Canada. [Bergin, E. A.; Wang, S.; Crockett, N. R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Phillips, T. G.; Lis, D. C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Caux, E.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Caux, E.] CNRS, IRAP, F-31028 Toulouse 4, France. [Comito, C.; Schilke, P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Goldsmith, P. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Schilke, P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Plume, R (reprint author), Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. EM plume@ras.ucalgary.ca RI Goldsmith, Paul/H-3159-2016 FU National Sciences and Engineering Research Council of Canada (NSERC); National Science Foundation [AST-0838261]; NASA FX 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: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; The Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronmico Nacional (IGN), Centro de Astrobiologa (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. Support for this work was provided, in part, by a National Sciences and Engineering Research Council of Canada (NSERC) grant to R. Plume, by the National Science Foundation grant AST-0838261 to the Caltech Submillimeter Observatory, and by NASA through an award issued by JPL/Caltech. NR 25 TC 16 Z9 16 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2012 VL 744 IS 1 AR 28 DI 10.1088/0004-637X/744/1/28 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866TY UT WOS:000298408300028 ER PT J AU Venter, C Johnson, TJ Harding, AK AF Venter, C. Johnson, T. J. Harding, A. K. TI MODELING PHASE-ALIGNED GAMMA-RAY AND RADIO MILLISECOND PULSAR LIGHT CURVES SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; gamma rays: stars; pulsars: individual (PSR J0034-0534, PSR J1939+2134, PSR J1959+2-48); radiation mechanisms: non-thermal ID LARGE-AREA TELESCOPE; HIGH-ENERGY EMISSION; RAPIDLY SPINNING PULSARS; XMM-NEWTON OBSERVATIONS; X-RAY; MONTE-CARLO; SLOT GAPS; PARTICLE-ACCELERATION; OPTICAL OBSERVATIONS; OUTER MAGNETOSPHERE C1 [Venter, C.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Johnson, T. J.; Harding, A. K.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Johnson, T. J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. RP Venter, C (reprint author), North West Univ, Ctr Space Res, Potchefstroom Campus, ZA-2520 Potchefstroom, South Africa. RI Harding, Alice/D-3160-2012; Venter, Christo/E-6884-2011 OI Venter, Christo/0000-0002-2666-4812 FU South African National Research Foundation; NASA; Fermi Guest Investigator Program; NASA DPR [S-15633-Y] FX C. V. is supported by the South African National Research Foundation. A. K. H. acknowledges support from the NASA Astrophysics Theory Program. C. V., T.J.J., and A. K. H. acknowledge support from the Fermi Guest Investigator Program as well as fruitful discussions with Dick Manchester and Matthew Kerr. Portions of this work were performed by T.J.J. while he was a postdoc at the Naval Research Laboratory, sponsored by NASA DPR S-15633-Y. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States; the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy; the Ministry of Education, Culture, Sports, Science, and Technology (MEXT), High Energy Accelerator Research Organization (KEK), and Japan Aerospace Exploration Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. NR 92 TC 33 Z9 33 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2012 VL 744 IS 1 AR 34 DI 10.1088/0004-637X/744/1/34 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866TY UT WOS:000298408300034 ER PT J AU Waldmann, IP Tinetti, G Drossart, P Swain, MR Deroo, P Griffith, CA AF Waldmann, I. P. Tinetti, G. Drossart, P. Swain, M. R. Deroo, P. Griffith, C. A. TI GROUND-BASED NEAR-INFRARED EMISSION SPECTROSCOPY OF HD 189733B SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; planets and satellites: atmospheres; planets and satellites: individual (HD 189733b); techniques: spectroscopic ID EXTRASOLAR PLANET; TRANSMISSION SPECTRUM; DAYSIDE SPECTRUM; PRIMARY TRANSIT; LINE LIST; MU-M; ATMOSPHERE; METHANE; WATER; JUPITER AB We investigate the K- and L-band dayside emission of the hot-Jupiter HD 189733b with three nights of secondary eclipse data obtained with the SpeX instrument on the NASA Infrared Telescope Facility. The observations for each of these three nights use equivalent instrument settings and the data from one of the nights have previously been reported by Swain et al. We describe an improved data analysis method that, in conjunction with themulti-night data set, allows increased spectral resolution (R similar to 175) leading to high-confidence identification of spectral features. We confirm the previously reported strong emission at similar to 3.3 mu m and, by assuming a 5% vibrational temperature excess for methane, we show that non-LTE emission from the methane nu(3) branch is a physically plausible source of this emission. We consider two possible energy sources that could power non-LTE emission and additional modeling is needed to obtain a detailed understanding of the physics of the emission mechanism. The validity of the data analysis method and the presence of strong 3.3 mu m emission are independently confirmed by simultaneous, long-slit, L-band spectroscopy of HD 189733b and a comparison star. C1 [Waldmann, I. P.; Tinetti, G.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Drossart, P.] Univ Paris Diderot, Univ Paris 06, LESIA, Observ Paris,CNRS, F-92195 Meudon, France. [Swain, M. R.; Deroo, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Griffith, C. A.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. RP Waldmann, IP (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM ingo@star.ucl.ac.uk OI Tinetti, Giovanna/0000-0001-6058-6654 FU STFC FX I. P. W. is supported by an STFC studentship. We thank the IRTF, which is operated by the University of Hawaii under Cooperative Agreement no NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. NR 42 TC 42 Z9 42 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2012 VL 744 IS 1 AR 35 DI 10.1088/0004-637X/744/1/35 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866TY UT WOS:000298408300035 ER PT J AU Campbell, JR Welton, EJ Krotkov, NA Yang, K Stewart, SA Fromm, MD AF Campbell, James R. Welton, Ellsworth J. Krotkov, Nickolay A. Yang, Kai Stewart, Sebastian A. Fromm, Michael D. TI Likely seeding of cirrus clouds by stratospheric Kasatochi volcanic aerosol particles near a mid-latitude tropopause fold SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Aerosol indirect effect; Volcanic aerosol; Cloud seeding; Cirrus clouds; UTLS processes; Lidar ID MOUNT-PINATUBO ERUPTION; POLARIZATION LIDAR; TROPOSPHERE; RADIATION; EXCHANGE; CLIMATE; DEBRIS; WATER; ICE AB Following the explosive 7-8 August 2008 Mt. Kasatochi volcanic eruption in southwestern Alaska, a segment of the dispersing stratospheric aerosol layer was profiled beginning 16 August in continuous ground-based lidar measurements over the Mid-Atlantic coast of the eastern United States. On 17-18 August, the layer was displaced downward into the upper troposphere through turbulent mixing near a tropopause fold. Cirrus clouds and ice crystal fallstreaks were subsequently observed, having formed within the entrained layer. The likely seeding of these clouds by Kasatochi aerosol particles is discussed. Cloud formation is hypothesized as resulting from either preferential homogenous freezing of relatively large sulfate-based solution droplets deliquesced after mixing into the moist upper troposphere or through heterogeneous droplet activation by volcanic ash. Satellite-borne spectrometer measurements illustrate the evolution of elevated Kasatochi SO2 mass concentrations regionally and the spatial extent of the cirrus cloud band induced by likely particle seeding. Satellite-borne polarization lidar observations confirm ice crystal presence within the clouds. Geostationary satellite-based water vapor channel imagery depicts strong regional subsidence, symptomatic of tropopause folding, along a deepening trough in the sub-tropical westerlies. Regional radiosonde profiling confirms both the position of the fold and depth of upper-tropospheric subsidence. These data represent the first unambiguous observations of likely cloud seeding by stratospheric volcanic aerosol particles after mixing back into the upper troposphere. Published by Elsevier Ltd. C1 [Campbell, James R.] USN, Res Lab, Monterey, CA 93943 USA. [Stewart, Sebastian A.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. [Fromm, Michael D.] USN, Res Lab, Washington, DC 20375 USA. [Yang, Kai] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. RP Campbell, JR (reprint author), USN, Res Lab, 7 Grace Hopper Ave,Stop 2, Monterey, CA 93943 USA. EM james.campbell@nrlmry.navy.mil RI Welton, Ellsworth/A-8362-2012; Campbell, James/C-4884-2012; Krotkov, Nickolay/E-1541-2012 OI Campbell, James/0000-0003-0251-4550; Krotkov, Nickolay/0000-0001-6170-6750 FU NASA Shared Services Center on behalf of the Micropulse Lidar Network [NNX10AE14G]; NASA [NNH07AG44I, NNG06GI00G] FX This work was supported by Grant NNX10AE14G issued by NASA Shared Services Center on behalf of the Micropulse Lidar Network project, and NASA Grant NNH07AG44I as part of the CALIPSO Science Team. Author N. K. acknowledges NASA Grant NNG06GI00G. The authors gratefully acknowledge the University of Wyoming Department of Atmospheric Sciences for access to visualization tools for their radiosonde archive, the Department of Earth, Atmospheric and Planetary Sciences at the Massachusetts Institute of Technology for access to their online GEMPAK data plotting software, and the NASA Langley Research Center Atmospheric Sciences Data Center for the CALIOP data used in this research. Special thanks are due to Cynthia Karengin at U.S. Naval Research Laboratory (NRL) Monterey for help constructing each of the figures, and Robert Holz at the University of Wisconsin Madison for restoring and generating the GOES water vapor imagery. Edward Hyer, Thomas Lee and Elizabeth Reid at NRL Monterey assisted with editing. Finally, we are grateful for the very helpful comments received by two anonymous colleagues during peer review. NR 56 TC 5 Z9 5 U1 1 U2 17 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD JAN PY 2012 VL 46 BP 441 EP 448 DI 10.1016/j.atmosenv.2011.09.027 PG 8 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 871UM UT WOS:000298763200047 ER PT J AU Mickley, LJ Leibensperger, EM Jacob, DJ Rind, D AF Mickley, L. J. Leibensperger, E. M. Jacob, D. J. Rind, D. TI Regional warming from aerosol removal over the United States: Results from a transient 2010-2050 climate simulation SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Regional climate change; Pollution; Short-lived species; Air quality; Particulate matter ID DIURNAL TEMPERATURE-RANGE; BLACK CARBON AEROSOLS; TROPOSPHERIC OZONE; SOLAR-RADIATION; SOIL-MOISTURE; EMISSIONS; IMPACTS; MODEL; POLLUTION; SURFACE AB We use a general circulation model (NASA Goddard Institute for Space Studies GCM 3) to investigate the regional climate response to removal of aerosols over the United States. We perform a pair of transient 2010-2050 climate simulations following a scenario of increasing greenhouse gas concentrations, with and without aerosols over the United States and with present-day aerosols elsewhere. We find that removing U.S. aerosol significantly enhances the warming from greenhouse gases in a spatial pattern that strongly correlates with that of the aerosol. Warming is nearly negligible outside the United States, but annual mean surface temperatures increase by 0.4-0.6 K in the eastern United States. Temperatures during summer heat waves in the Northeast rise by as much as 1-2 K due to aerosol removal, driven in part by positive feedbacks involving soil moisture and low cloud cover. Reducing U.S. aerosol sources to achieve air quality objectives could thus have significant unintended regional warming consequences. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Mickley, L. J.; Leibensperger, E. M.; Jacob, D. J.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Leibensperger, E. M.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [Rind, D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Mickley, LJ (reprint author), Harvard Univ, Sch Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02138 USA. EM mickley@fas.harvard.edu RI Mickley, Loretta/D-2021-2012 OI Mickley, Loretta/0000-0002-7859-3470 FU Electric Power Research Institute (EPRI); EPA FX This work was funded by the Electric Power Research Institute (EPRI) and by an EPA Science to Achieve Results (STAR) Graduate Research Fellowship to Eric Leibensperger. The EPA has not officially endorsed this publication and the views expressed herein may not reflect those of the EPA. We also thank two anonymous reviewers. NR 73 TC 21 Z9 21 U1 0 U2 12 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 JAN PY 2012 VL 46 BP 545 EP 553 DI 10.1016/j.atmosenv.2011.07.030 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 871UM UT WOS:000298763200057 ER PT J AU Kerstman, EL Scheuring, RA Barnes, MG DeKorse, TB Saile, LG AF Kerstman, Eric L. Scheuring, Richard A. Barnes, Matt G. DeKorse, Tyson B. Saile, Lynn G. TI Space Adaptation Back Pain: A Retrospective Study SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE crewmembers; NASA; zero gravity environment; spine; spinal lengthening; lumbar ID HEAD-DOWN TILT; US ASTRONAUTS; BED REST; MICROGRAVITY; SHUTTLE AB Introduction: Back pain is frequently reported by astronauts during the early phase of spaceflight as they adapt to microgravity. The epidemiology of space adaptation back pain has not been well defined. This study aims to develop a case definition of space adaptation back pain, determine its incidence, and assess the effectiveness of available treatments. Methods: Medical records from the Mercury, Apollo, Apollo-Soyuz Test Project (ASTP), Skylab, Mir, International Space Station (ISS), and Shuttle programs were reviewed. All episodes of in-flight back pain that met the criteria for space adaptation back pain were recorded. Pain characteristics, including intensity, location, and duration of the pain, were noted. The effectiveness of specific treatments was also recorded. Results: The incidence of space adaptation back pain among astronauts was determined to be 52% (382/728). Most of the affected astronauts reported mild pain (86%). Moderate pain was reported by 11 % of the affected astronauts and severe pain was reported by 3% of the affected astronauts. The most effective treatments were fetal positioning (91%) and the use of analgesic medications and exercise (primarily treadmill and cycle ergometer), which were both 85% effective. Discussion: This retrospective study examines the epidemiology of space adaptation back pain. Space adaptation back pain is usually mild and self-limited. However, there is a risk of functional impairment and mission impact in cases of moderate or severe pain that do not respond to currently available treatments. Therefore, the development of preventive measures and more effective treatments should be pursued. C1 [Kerstman, Eric L.] Wyle Integrated Sci & Engn, Houston, TX 77058 USA. Univ Texas Med Branch, Galveston, TX USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Dewitt Army Community Hosp Wyle, Houston, TX USA. MSU Wyle, Houston, TX USA. RP Kerstman, EL (reprint author), Wyle Integrated Sci & Engn, 1290 Hercules, Houston, TX 77058 USA. EM ekerstman@wylehou.com NR 16 TC 6 Z9 7 U1 2 U2 8 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD JAN PY 2012 VL 83 IS 1 BP 2 EP 7 DI 10.3357/ASEM.2876.2012 PG 6 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 867GG UT WOS:000298442300002 PM 22272509 ER PT J AU Singh, H Giardina, TD Petersen, LA Smith, MW Paul, LW Dismukes, K Bhagwath, G Thomas, EJ AF Singh, Hardeep Giardina, Traber Davis Petersen, Laura A. Smith, Michael W. Paul, Lindsey Wilson Dismukes, Key Bhagwath, Gayathri Thomas, Eric J. TI Exploring situational awareness in diagnostic errors in primary care SO BMJ QUALITY & SAFETY LA English DT Article ID PATIENT SAFETY; MALPRACTICE CLAIMS; DECISION-MAKING; MISSED OPPORTUNITIES; CANCER DIAGNOSIS; DYNAMIC-SYSTEMS; ADVERSE EVENTS; MEDICINE; STRATEGIES; COGNITION AB Objective: Diagnostic errors in primary care are harmful but poorly studied. To facilitate the understanding of diagnostic errors in real-world primary care settings that use electronic health records (EHRs), this study explored the use of the situational awareness (SA) framework from aviation human factors research. Methods: A mixed-methods study was conducted involving reviews of EHR data followed by semi-structured interviews of selected providers from two institutions in the USA. The study population included 380 consecutive patients with colorectal and lung cancers diagnosed between February 2008 and January 2009. Using a pre-tested data collection instrument, trained physicians identified diagnostic errors, defined as lack of timely action on one or more established indications for diagnostic work-up for lung and colorectal cancers. Twenty-six providers involved in cases with and without errors were interviewed. Interviews probed for providers' lack of SA and how this may have influenced the diagnostic process. Results: Of 254 cases meeting inclusion criteria, errors were found in 30 of 92 (32.6%) lung cancer cases and 56 of 167 (33.5%) colorectal cancer cases. Analysis of interviews related to error cases revealed evidence of lack of one of four levels of SA applicable to primary care practice: information perception, information comprehension, forecasting future events, and choosing appropriate action based on the first three levels. In cases without error, application of the SA framework provided insight into processes involved in attention management. Conclusions: A framework of SA can help analyse and understand diagnostic errors in primary care settings that use EHRs. C1 [Singh, Hardeep; Giardina, Traber Davis; Petersen, Laura A.; Smith, Michael W.] Baylor Coll Med, Houston VA HSR&D Ctr Excellence, Michael E DeBakey Vet Affairs Med Ctr, Houston, TX 77030 USA. [Singh, Hardeep; Giardina, Traber Davis; Petersen, Laura A.; Smith, Michael W.] Baylor Coll Med, Dept Med, Sect Hlth Serv Res, Houston, TX 77030 USA. [Paul, Lindsey Wilson] Univ Texas Austin, Sch Social Work, Austin, TX 78712 USA. [Dismukes, Key] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bhagwath, Gayathri] Univ Texas Galveston, Med Branch, Dept Internal Med, Div Hematol Oncol, Galveston, TX 77550 USA. [Thomas, Eric J.] Univ Texas Houston, Sch Med, Dept Med, Div Gen Med, Houston, TX 77030 USA. [Thomas, Eric J.] Univ Texas Houston, Sch Med, Mem Hermann Ctr Healthcare Qual, Houston, TX USA. RP Singh, H (reprint author), Med Ctr 152, 2002 Holcombe Blvd, Houston, TX 77030 USA. EM hardeeps@bcm.edu OI Davis Giardina, Traber/0000-0002-9184-6524 FU NIH [K23CA125585]; Houston VA HSR&D Center of Excellence [HFP90-020] FX This study was supported by an NIH K23 career development award (K23CA125585) to Dr Singh, and in part by the Houston VA HSR&D Center of Excellence (HFP90-020). These sources had no role in the design and conduct of the study; collection, management, analysis, and interpretation of the data; and preparation, review, or approval of the manuscript. NR 77 TC 19 Z9 20 U1 4 U2 14 PU BMJ PUBLISHING GROUP PI LONDON PA BRITISH MED ASSOC HOUSE, TAVISTOCK SQUARE, LONDON WC1H 9JR, ENGLAND SN 2044-5415 J9 BMJ QUAL SAF JI BMJ Qual. Saf. PD JAN PY 2012 VL 21 IS 1 BP 30 EP 38 DI 10.1136/bmjqs-2011-000310 PG 9 WC Health Care Sciences & Services; Health Policy & Services SC Health Care Sciences & Services GA 862ZZ UT WOS:000298133900005 PM 21890757 ER PT J AU Davis, RE Denery, DG Kendrick, DA Mehra, RK AF Davis, Ronald E. Denery, Dallas G. Kendrick, David A. Mehra, Raman K. TI Introduction to the Works of Rodney C. Wingrove: Engineering Approaches to Macroeconomic Modeling SO COMPUTATIONAL ECONOMICS LA English DT Article DE Macroeconomic models; Stochastic dynamic control models; Parameter estimation; System identification; Business cycles; Money supply regulation; Simulation of policy alternatives ID STABILIZATION; UNCERTAINTY; POLICY; RULES AB A continuous-time control model was formulated and fitted to macroeconomic data by an expert control engineer who worked at NASA-AMES in the 1980s, Rodney C. Wingrove. Two articles were prepared and made available to the aerospace industry at that time, however the authors feel that wider distribution of his study posthumously is warranted at this time. This introduction to the two Wingrove articles that follow provides background information on the technologies Wingrove was working with, as well as subsequent developments in both macroeconomic and engineering modeling and analysis technology. Our purpose is to stimulate further research along the same lines which can potentially lead to structural and/or policy rule improvements that can prevent the extremely turbulent abberations that have been seen in recent years, and promote steady growth with low inflation and low unemployment in a sustainable way. Of particular concern is the exploding national debt problem. C1 [Davis, Ronald E.] San Jose State Univ, San Jose, CA 95192 USA. [Denery, Dallas G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kendrick, David A.] Univ Texas Austin, Austin, TX 78712 USA. [Mehra, Raman K.] Sci Syst Co Inc, Woburn, MA USA. RP Davis, RE (reprint author), San Jose State Univ, San Jose, CA 95192 USA. EM ronald.davis@sjsu.edu; kendrick@austin.utexas.edu; Raman.Mehra@ssci.com NR 35 TC 0 Z9 0 U1 3 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0927-7099 J9 COMPUT ECON JI Comput. Econ. PD JAN PY 2012 VL 39 IS 1 BP 71 EP 76 DI 10.1007/s10614-011-9298-3 PG 6 WC Economics; Management; Mathematics, Interdisciplinary Applications SC Business & Economics; Mathematics GA 863VH UT WOS:000298195900005 ER PT J AU Wingrove, RC Davis, RE AF Wingrove, Rodney C. Davis, Ronald E. TI Classical Linear-Control Analysis Applied to Business-Cycle Dynamics and Stability SO COMPUTATIONAL ECONOMICS LA English DT Article DE Linear-control analysis; Dynamic macroeconomic systems; Business-cycle dynamics; Stabilization policies ID RATIONAL-EXPECTATIONS; MONEY; POLICIES AB Classical linear-control analysis provides a framework for studying dynamic systems involving random disturbances. This framework is used to develop a set of equations that, in historical perspective, combine traditional concepts about the dynamics of economic systems and about the effects of random economic disturbances. This set of equations provides relationships among well-known ideas in general macroeconomics and provides a means to interrelate and examine ideas about stabilization policies. In this study, linear-control analysis is applied as an aid in understanding the fluctuations of business cycles in the past, and to examine monetary policies that might improve stabilization. The analysis shows how different policies change the frequency and damping of the economic system dynamics, and how they modify the amplitude of the fluctuations that are caused by random disturbances. Examples are used to show how policy feedbacks and policy lags can be incorporated, and how different monetary strategies for stabilization can be analytically compared. Representative numerical results are used to illustrate the main points. C1 [Davis, Ronald E.] San Jose State Univ, San Jose, CA 95192 USA. [Wingrove, Rodney C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Davis, RE (reprint author), San Jose State Univ, San Jose, CA 95192 USA. EM Ronald.Davis@sjsu.edu NR 30 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0927-7099 J9 COMPUT ECON JI Comput. Econ. PD JAN PY 2012 VL 39 IS 1 BP 77 EP 98 DI 10.1007/s10614-011-9299-2 PG 22 WC Economics; Management; Mathematics, Interdisciplinary Applications SC Business & Economics; Mathematics GA 863VH UT WOS:000298195900006 ER PT J AU Wingrove, RC Davis, RE AF Wingrove, Rodney C. Davis, Ronald E. TI Manual-Control Analysis Applied to the Money Supply Control Task SO COMPUTATIONAL ECONOMICS LA English DT Article ID POLICIES; MODELS AB The recent procedure implemented by the Federal Reserve Board to control the money supply is formulated in the form of a tracking model as used in the study of manual-control tasks. Using this model, an analysis is made to determine the effect of monetary control on the fluctuations in economic output. The results indicate that monetary control can reduce the amplitude of fluctuations at frequencies near the region of historic business cycles. However, with significant time lags in the control loop, monetary control tends to increase the amplitude of the fluctuations at the higher frequencies. The study outlines how the investigator or student can use the tools developed in the field of manual-control analysis to study the nature of economic fluctuations and to examine different strategies for stabilization. C1 [Davis, Ronald E.] San Jose State Univ, San Jose, CA 95192 USA. [Wingrove, Rodney C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Davis, RE (reprint author), San Jose State Univ, San Jose, CA 95192 USA. EM Ronald.Davis@sjsu.edu NR 22 TC 0 Z9 0 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0927-7099 J9 COMPUT ECON JI Comput. Econ. PD JAN PY 2012 VL 39 IS 1 BP 99 EP 111 DI 10.1007/s10614-011-9301-z PG 13 WC Economics; Management; Mathematics, Interdisciplinary Applications SC Business & Economics; Mathematics GA 863VH UT WOS:000298195900007 ER PT J AU Feng, M Huang, CQ Channan, S Vermote, EF Masek, JG Townshend, JR AF Feng, Min Huang, Chengquan Channan, Saurabh Vermote, Eric F. Masek, Jeffrey G. Townshend, John R. TI Quality assessment of Landsat surface reflectance products using MODIS data SO COMPUTERS & GEOSCIENCES LA English DT Article DE Surface reflectance; Landsat; MODIS; Object-oriented programming; Quality assessment ID ATMOSPHERIC CORRECTION; ALBEDO PRODUCTS; SATELLITE DATA; TM DATA; VALIDATION; CLASSIFICATION; SCIENCE; MISSION; RECORD; 6S AB Surface reflectance adjusted for atmospheric effects is a primary input for land cover change detection and for developing many higher level surface geophysical parameters. With the development of automated atmospheric correction algorithms, it is now feasible to produce large quantities of surface reflectance products using Landsat images. Validation of these products requires in situ measurements, which either do not exist or are difficult to obtain for most Landsat images. The surface reflectance products derived using data acquired by the Moderate Resolution Imaging Spectroradiometer (MOD'S), however, have been validated more comprehensively. Because the MODIS on the Terra platform and the Landsat 7 are only half an hour apart following the same orbit, and each of the 6 Landsat spectral bands overlaps with a MODIS band, good agreements between MODIS and Landsat surface reflectance values can be considered indicators of the reliability of the Landsat products, while disagreements may suggest potential quality problems that need to be further investigated. Here we develop a system called Landsat-MODIS Consistency Checking System (LMCCS). This system automatically matches Landsat data with MODIS observations acquired on the same date over the same locations and uses them to calculate a set of agreement metrics. To maximize its portability, Java and open-source libraries were used in developing this system, and object-oriented programming (OOP) principles were followed to make it more flexible for future expansion. As a highly automated system designed to run as a stand-alone package or as a component of other Landsat data processing systems, this system can be used to assess the quality of essentially every Landsat surface reflectance image where spatially and temporally matching MODIS data are available. The effectiveness of this system was demonstrated using it to assess preliminary surface reflectance products derived using the Global Land Survey (GLS) Landsat images for the 2000 epoch. As surface reflectance likely will be a standard product for future Landsat missions, the approach developed in this study can be adapted as an operational quality assessment system for those missions. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Feng, Min] Chinese Acad Sci, State Key Lab Resources & Environm Informat Syst, Inst Geog Sci & Nat Resources Res, Beijing 100101, Peoples R China. [Feng, Min; Huang, Chengquan; Channan, Saurabh; Townshend, John R.] Univ Maryland, Dept Geog, Global Land Cover Facil, College Pk, MD 20742 USA. [Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. RP Feng, M (reprint author), Chinese Acad Sci, State Key Lab Resources & Environm Informat Syst, Inst Geog Sci & Nat Resources Res, Beijing 100101, Peoples R China. EM feng.tank@gmail.com RI Masek, Jeffrey/D-7673-2012; Vermote, Eric/K-3733-2012; OI Huang, Chengquan/0000-0003-0055-9798 FU NASA [NNH06ZDA001N-MEASURES]; Land Cover and Land Use Change [NNH07ZDA001N-LCLUC]; Earth System Science Research Using Data and Products from Terra, Aqua, and Acrimsat Satellites [NNH06ZDA001N-EOS] FX Funding support for this study was provided by the following NASA programs: making Earth System Data Records for Use in Research Environments (NNH06ZDA001N-MEASURES), Land Cover and Land Use Change (NNH07ZDA001N-LCLUC), and Earth System Science Research Using Data and Products from Terra, Aqua, and Acrimsat Satellites (NNH06ZDA001N-EOS). The MODIS daily products used in this study were obtained through Greg Ederer and Robert Wolfe. The GLS datasets were sent to GLCF by Rachel Headley. Joseph O. Sexton, Raghuram Narasimhan, and other colleagues and collaborators of the Global Forest Cover Change (GFCC) Project provided valuable inputs for improving this manuscript and the method described here. We also thank Prof. Jiulin Sun for his support on this work. NR 43 TC 35 Z9 38 U1 2 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0098-3004 EI 1873-7803 J9 COMPUT GEOSCI-UK JI Comput. Geosci. PD JAN PY 2012 VL 38 IS 1 BP 9 EP 22 DI 10.1016/j.cageo.2011.04.011 PG 14 WC Computer Science, Interdisciplinary Applications; Geosciences, Multidisciplinary SC Computer Science; Geology GA 868LF UT WOS:000298524100002 ER PT J AU Foustoukos, DI Stern, JC AF Foustoukos, Dionysis I. Stern, Jennifer C. TI Oxidation pathways for formic acid under low temperature hydrothermal conditions: Implications for the chemical and isotopic evolution of organics on Mars SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID GAS-PHASE REACTIONS; MOLAL THERMODYNAMIC PROPERTIES; OH RADICAL REACTIONS; MARTIAN DUST DEVILS; HYDROGEN-PEROXIDE; SUPERCRITICAL WATER; THERMAL-DECOMPOSITION; ELEVATED-TEMPERATURES; OXIDANT ENHANCEMENT; HYDROXYL RADICALS AB In order to evaluate the oxidation effect of dissolved hydrogen peroxide and the catalytic role of iron oxides on the kinetics of formic acid decarboxylation, a series of flow-through hydrothermal experiments was conducted at temperatures ranging from 80 to 150 degrees C and pressures of 172-241 bar. delta C-13 composition of residual HCOOH(aq) was also monitored to examine kinetic isotope effects associated with oxidation processes. Our results reveal that decomposition of H2O2(aq) in presence of magnetite follows pseudo first order kinetics, highly enhanced relative to the homogeneous H2O2(aq)-HCOOOH(aq)-H2O system, which possibly reflect synthesis of hydroxyl radicals ((OH)-O-center dot) through Fenton processes. The kinetic rate constants of HCOOH(aq) decarboxylation to CO2(aq) are also elevated relative to those previously measured in H2O2(aq) free experiments. However, reaction kinetics are slightly slower in the case of H2O2(aq) aqueous solutions coexisting with magnetite than in the absence of mineral phases. This behavior is attributed to the possible formation of Fe-bearing hydroxyl formate aqueous species that could serve as stable transition states leading to a decrease in the activation entropy of formic acid decomposition. delta C-13 values of residual formic acid in the homogeneous H2O2(aq)-HCOOH(aq)-H2O system are consistent with previous studies. However, magnetite-bearing experiments produce a negative shift in delta C-13 of residual formic acid, perhaps specific to (OH)-O-center dot-imposed oxidation of organic compounds. This would indicate that isotopic fractionations by this oxidation pathway are opposite to kinetic fractionation effects expected in biologically driven oxidation processes. This could have important implications for putative H2O2(aq)-bearing Martian subsurface environments and the evolution of organics at low-temperature hydrothermal conditions. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Foustoukos, Dionysis I.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Stern, Jennifer C.] NASA, Planetary Environm Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Foustoukos, DI (reprint author), Carnegie Inst Sci, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA. EM dfoustoukos@ciw.edu; jennifer.c.stern@nasa.gov RI Stern, Jennifer/E-3135-2012 OI Stern, Jennifer/0000-0002-0162-8807 FU NSF [OCE-0752221]; Carnegie Institution of Washington; NASA Astrobiology Institute Goddard Center for Astrobiology FX This research was conducted with support from the NSF OCE-0752221, the Carnegie Institution of Washington (DF) and the NASA Astrobiology Institute Goddard Center for Astrobiology (JCS). We acknowledge contributions by the W. M. Keck Foundation, the CIW-Canada and Shell towards supporting the hydrothermal lab at the Geophysical Lab. We would like to thank Dr. Daniel Hummer for assistance on the XRD analysis performed. Finally, we would like to thank the contributions and comments from the Associate Editor, Prof. J. Horita, two anonymous reviewers and Dr. P. Niles. NR 112 TC 4 Z9 4 U1 4 U2 37 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 JAN 1 PY 2012 VL 76 BP 14 EP 28 DI 10.1016/j.gca.2011.10.016 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 863FR UT WOS:000298148700002 ER PT J AU Bridges, NT Bourke, MC Geissler, PE Banks, ME Colon, C Diniega, S Golombek, MP Hansen, CJ Mattson, S McEwen, AS Mellon, MT Stantzos, N Thomson, BJ AF Bridges, Nathan T. Bourke, Mary C. Geissler, Paul E. Banks, Maria E. Colon, Cindy Diniega, Serina Golombek, Matthew P. Hansen, Candice J. Mattson, Sarah McEwen, Alfred S. Mellon, Michael T. Stantzos, Nicholas Thomson, Bradley J. TI Planet-wide sand motion on Mars SO GEOLOGY LA English DT Article ID GENERAL-CIRCULATION MODEL; DUNES; MOVEMENT; DEPOSITS; EROSION; VALLEY; ICE AB Prior to Mars Reconnaissance Orbiter data, images of Mars showed no direct evidence for dune and ripple motion. This was consistent with climate models and lander measurements indicating that winds of sufficient intensity to mobilize sand were rare in the low-density atmosphere. We show that many sand ripples and dunes across Mars exhibit movement of as much as a few meters per year, demonstrating that Martian sand migrates under current conditions in diverse areas of the planet. Most motion is probably driven by wind gusts that are not resolved in global circulation models. A past climate with a thicker atmosphere is only required to move large ripples that contain coarse grains. C1 [Bridges, Nathan T.; Thomson, Bradley J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Bourke, Mary C.; Hansen, Candice J.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Geissler, Paul E.; Stantzos, Nicholas] US Geol Survey, Flagstaff, AZ 86001 USA. [Banks, Maria E.] Smithsonian Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Colon, Cindy] Rutgers State Univ, Dept Earth & Environm Sci, Newark, NJ 07102 USA. [Diniega, Serina; Golombek, Matthew P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mattson, Sarah; McEwen, Alfred S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Mellon, Michael T.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Bridges, NT (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. RI Bourke, Mary/I-4387-2012; Mellon, Michael/C-3456-2016; Bridges, Nathan/D-6341-2016; OI Bourke, Mary/0000-0002-0424-0322; Thomson, Bradley/0000-0001-8635-8932 FU Mars Reconnaissance Orbiter/HiRISE (High Resolution Imaging Science Experiment); National Aeronautics and Space Administration FX We thank Devon Burr, Lori Fenton, and an anonymous reviewer for very helpful reviews. Support to Bridges and several coauthors was through Mars Reconnaissance Orbiter/HiRISE (High Resolution Imaging Science Experiment) funding provided by the National Aeronautics and Space Administration. NR 38 TC 48 Z9 49 U1 3 U2 31 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD JAN PY 2012 VL 40 IS 1 BP 31 EP 34 DI 10.1130/G32373.1 PG 4 WC Geology SC Geology GA 866VK UT WOS:000298414000008 ER PT J AU Ma, KL Liao, I Frazier, J Hauser, H Kostis, HN AF Ma, Kwan-Liu Liao, Isaac Frazier, Jennifer Hauser, Helwig Kostis, Helen-Nicole TI Scientific Storytelling Using Visualization SO IEEE COMPUTER GRAPHICS AND APPLICATIONS LA English DT Editorial Material C1 [Ma, Kwan-Liu; Liao, Isaac] Univ Calif Davis, Dept Comp Sci, Davis, CA 95616 USA. [Frazier, Jennifer] Univ Bergen, N-5020 Bergen, Norway. [Kostis, Helen-Nicole] NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA. RP Ma, KL (reprint author), Univ Calif Davis, Dept Comp Sci, Davis, CA 95616 USA. EM ma@cs.ucdavis.edu; ihliao@ucdavis.edu; jfrazier@exploratorium.edu; helwig.hauser@uib.no; helen-nicole.kostis@nasa.gov NR 8 TC 16 Z9 16 U1 1 U2 5 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 0272-1716 EI 1558-1756 J9 IEEE COMPUT GRAPH JI IEEE Comput. Graph. Appl. PD JAN-FEB PY 2012 VL 32 IS 1 BP 12 EP 19 PG 8 WC Computer Science, Software Engineering SC Computer Science GA 871UH UT WOS:000298762700004 PM 24808289 ER PT J AU Valdivia-Silva, JE Navarro-Gonzalez, R Fletcher, L Perez-Montano, S Condori-Apaza, R Ortega-Gutierrez, F Mckay, C AF Valdivia-Silva, Julio E. Navarro-Gonzalez, Rafael Fletcher, Lauren Perez-Montano, Saul Condori-Apaza, Renee Ortega-Gutierrez, Fernando Mckay, Christopher TI Climatological characteristics in the extreme hyper-arid region of Pampas de La Joya, Peru. Astrobiological approach in four years of observation: 2004-2008 SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Article DE hyper-arid soils; extreme environments; Atacama Desert; Pampas de La Joya; Mars analogues ID 1997-98 EL-NINO; ATACAMA DESERT; NORTHERN CHILE; LIFE; TEMPERATURE; SOILS; CORE; MARS; FOG AB This study reports the environmental conditions of temperature, moisture and radiation for four years (May 2004 to July 2008) in the area known as Pampas de La Joya in southern Peru, which recently has been considered as a new Mars analogue. The period of evaluation includes the El Nino Southern Oscillation (ENSO) during the months of September 2006 to March 2007, which, despite not having catastrophic effects like its predecessor on 1997-1998, showed an interesting increase in humidity. Our data describe the extreme conditions present in the region and their relationship with the presence of potential habitats that could allow for the survival of micro-organisms. The average environmental temperature was 18.9 degrees C, with a maximum of 35.9 degrees C and a minimum of -4.5 degrees C. The annual average incident solar radiation was 508 W m(-2), with high near 1060 W m(-2) at noon during the driest period between September and March. The average relative humidity (RH) was 29.5, 20.1 and 20.4% for air, soil and rock, respectively. The RH had higher values at night due to fog during the months of June and August, and during the early morning between December and March. During the months of ENSO event there were four episodes of precipitation (1.1, 1.5, 2.0 and 0.9 mm), of which three increased soil and rock moisture on an average more than 45% and persisted for over 15 days after precipitation, while the atmospheric environment had no significant variations. Finally, quartz rocks and evaporite minerals colonized with micro-organisms were found as the only micro-habitats, in this region, capable of supporting life in this extreme environment. Received 3 February 2011, accepted 11 September 2011, first published online 17 October 2011 C1 [Valdivia-Silva, Julio E.; Navarro-Gonzalez, Rafael] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Lab Quim Plasmas & Estudios Planetarios, Mexico City 04510, DF, Mexico. [Valdivia-Silva, Julio E.; Fletcher, Lauren; Mckay, Christopher] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Fletcher, Lauren] Univ Oxford, Oxford, England. [Perez-Montano, Saul] San Jose State Univ, Dept Chem, San Jose, CA 95192 USA. [Condori-Apaza, Renee] Univ Nacl San Agustin, Fac Ingn Quim, Arequipa, Peru. [Ortega-Gutierrez, Fernando] Univ Nacl Autonoma Mexico, Inst Geol, Mexico City 04510, DF, Mexico. RP Valdivia-Silva, JE (reprint author), Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Lab Quim Plasmas & Estudios Planetarios, Mexico City 04510, DF, Mexico. EM jvsilva@nucleares.unam.mx RI Gonzalez, Rafael/D-1748-2009; OI CONDORI APAZA, RENEE/0000-0002-1097-5026 FU Universidad Nacional Autonoma de Mexico (DGAPA) [IN 107107, IN109110]; Consejo Nacional de Ciencia y Tecnologia de Mexico (CONACyT) [45810-F, 98466, 121479]; NASA FX Funding for this research comes from Grants from the Universidad Nacional Autonoma de Mexico (DGAPA IN 107107, IN109110), Consejo Nacional de Ciencia y Tecnologia de Mexico (CONACyT 45810-F, 98466, 121479), NASA Posdoctoral Program and by the National Aeronautics and Space Administration Astrobiology Science and Technology for Exploring Planets Program. We thank Instituto Geofisico of the Universidad Nacional San Agustin, Arequipa-Peru and Mr Antonio Ballon for logistical support in the expeditions to the desert. NR 41 TC 4 Z9 4 U1 2 U2 17 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD JAN PY 2012 VL 11 IS 1 BP 25 EP 35 DI 10.1017/S1473550411000292 PG 11 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 862IC UT WOS:000298083100004 ER PT J AU Nettles, AT Jackson, JR Hodge, AJ AF Nettles, Alan Tate Jackson, Justin R. Hodge, Andrew J. TI Change in damage tolerance characteristics of sandwich structure with a Thermal Protection System (TPS) SO JOURNAL OF COMPOSITE MATERIALS LA English DT Article DE CAI; sandwich structure; damage tolerance; impact; launch vehicle ID PHENOMENOLOGICAL MODELS; HYBRID COMPOSITES; FAILURE ANALYSIS; IMPACT; COMPRESSION; POLYETHYLENE AB Most composite damage tolerance assessments are made on bare laminates where the impactor comes into direct contact with the outermost ply. However, structures such as those used on launch vehicles are often covered with a thermal protection system (TPS) during the majority of the life of the part. This TPS covering may change the impact characteristics of the laminate rendering damage tolerance testing on bare laminates irrelevant to the part. This study examines the composite interstage structure of the ARES I launch vehicle which is scheduled to be covered with a sprayable foam TPS after manufacture. Damage tolerance testing is performed on bare sandwich structure and sandwich structure covered with the TPS selected for use on the ARES I composite interstage. Instrumented impact, infrared thermography, visual, cross-sectional and compression after impact CAI data are compared. Results show that the TPS covering does change most of the impact characteristics of the sandwich structure. It was found that the TPS created a larger damage zone as detected by IRT, however the TPS covered specimens possessed a higher residual compression strength for a given impact energy and damage size. These results are attempted to be explained by the different damage morphology that occurs between the bare and TPS covered specimens. C1 [Nettles, Alan Tate; Jackson, Justin R.; Hodge, Andrew J.] NASA MSFC, Huntsville, AL 35812 USA. RP Nettles, AT (reprint author), NASA MSFC, Bldg 4610, Huntsville, AL 35812 USA. EM alan.t.nettles@nasa.gov FU National Aeronautics and Space Administration under Upper Stage Program Office at Marshall Space Flight Center [136905.08.05.12] FX This study was funded by the National Aeronautics and Space Administration under the auspices of the Upper Stage Program Office at Marshall Space Flight Center (136905.08.05.12). NR 17 TC 0 Z9 0 U1 1 U2 3 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0021-9983 J9 J COMPOS MATER JI J. Compos Mater. PD JAN PY 2012 VL 46 IS 2 BP 211 EP 226 DI 10.1177/0021998311410509 PG 16 WC Materials Science, Composites SC Materials Science GA 866BL UT WOS:000298354500008 ER PT J AU Campagnola, S Kawakatsu, Y AF Campagnola, Stefano Kawakatsu, Yasuhiro TI Three-Dimensional Resonant Hopping Strategies and the Jupiter Magnetospheric Orbiter SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID DESIGN; GRAPH C1 [Kawakatsu, Yasuhiro] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. RP Campagnola, S (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM stefano.campagnola@jpl.nasa.gov NR 15 TC 2 Z9 2 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD JAN-FEB PY 2012 VL 35 IS 1 BP 340 EP 344 DI 10.2514/1.53334 PG 5 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 876ZO UT WOS:000299146500032 ER PT J AU Raj, R Kim, J McQuillen, J AF Raj, Rishi Kim, Jungho McQuillen, John TI On the Scaling of Pool Boiling Heat Flux With Gravity and Heater Size SO JOURNAL OF HEAT TRANSFER-TRANSACTIONS OF THE ASME LA English DT Article DE pool boiling; scaling parameter; variable gravity; heater size; subcooling; dissolved gas ID REDUCED GRAVITY; DISSOLVED-GAS; MICROGRAVITY; CONVECTION AB A framework for scaling pool boiling heat flux is developed using data from various heater sizes over a range of gravity levels. Boiling is buoyancy dominated for large heaters and/or high gravity conditions and the heat flux is heater size independent. The power law coefficient for gravity is a function of wall temperature. As the heater size or gravity level is reduced, a sharp transition in the heat flux is observed at a threshold value of L-h/L-c = 2.1. Below this threshold value, boiling is surface tension dominated and the dependence on gravity is smaller. The gravity scaling parameter for the heat flux in the buoyancy dominated boiling regime developed in the previous work is updated to account for subcooling effect. Based on this scaling parameter and the transition criteria, a methodology for predicting heat flux in the surface tension dominated boiling regime, typically observed under low-gravity conditions, is developed. Given the heat flux at a reference gravity level and heater size, the current framework allows the prediction of heat flux at any other gravity level and/or heater size under similar experimental conditions. The prediction is validated using data at over a range of subcoolings (11 degrees C <= Delta T-sub <= 32.6 degrees C), heater sizes (2.1 mm <= L-h <= 7 mm), and dissolved gas concentrations (3 ppm <= c(g) <= 3500 ppm). The prediction errors are significantly smaller than those from correlations currently available in the literature. [DOI: 10.1115/1.4004370] C1 [Raj, Rishi; Kim, Jungho] Univ Maryland, Dept Mech Engn, College Pk, MD 20742 USA. [McQuillen, John] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Kim, J (reprint author), Univ Maryland, Dept Mech Engn, College Pk, MD 20742 USA. EM rraj@umd.edu; kimjh@umd.edu; John.B.McQuillen@nasa.gov RI Raj, Rishi/A-5215-2010 OI Raj, Rishi/0000-0002-9805-0609 FU NASA through the Advanced Capabilities Division in the Exploration Systems Mission Directorate at NASA Headquarters [NNX08AI60A] FX This work was supported by NASA Grant No. NNX08AI60A through the Advanced Capabilities Division in the Exploration Systems Mission Directorate at NASA Headquarters. The authors would like to thank the European Space Agency for accommodating our experiment on the 48th and 52nd ESA Parabolic Flight Campaign in April 2008 and May 2010. The preliminary version of the current work was presented in the ASME/JSME 2011 8th Thermal Engineering Joint Conference, Honolulu, HI (Paper No. AJTEC2011-44449). NR 33 TC 6 Z9 6 U1 3 U2 15 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0022-1481 EI 1528-8943 J9 J HEAT TRANS-T ASME JI J. Heat Transf.-Trans. ASME PD JAN PY 2012 VL 134 IS 1 AR 011502 DI 10.1115/1.4004370 PG 13 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA 860EQ UT WOS:000297932000005 ER PT J AU Mulenburg, G AF Mulenburg, Gerald TI The Art of Invention: The Creative Process of Discovery and Design SO JOURNAL OF PRODUCT INNOVATION MANAGEMENT LA English DT Book Review C1 [Mulenburg, Gerald] NASA, Washington, DC 20546 USA. NR 1 TC 0 Z9 0 U1 4 U2 8 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0737-6782 J9 J PROD INNOVAT MANAG JI J. Prod. Innov. Manage. PD JAN PY 2012 VL 29 IS 1 BP 158 EP 159 DI 10.1111/j.1540-5885.2011.00885.x PG 2 WC Business; Engineering, Industrial; Management SC Business & Economics; Engineering GA 861BQ UT WOS:000297994300014 ER PT J AU Brauer, CS Sung, K Pearson, JC Brown, LR Xu, LH AF Brauer, Carolyn S. Sung, Keeyoon Pearson, John C. Brown, Linda R. Xu, Li-Hong TI Empirical line intensities of methanol in the 300-500 cm(-1) region SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Methanol; Intensities; Far-infrared; Torsion; Dipole moment ID STAR-FORMING REGIONS; DIPOLE-MOMENT; MU-M; INTEGRATED-INTENSITIES; ABSORPTION FEATURES; INTERSTELLAR CLOUDS; MOLECULAR CLOUDS; HITRAN DATABASE; DIAGNOSTIC-TOOL; METHYL-ALCOHOL AB Given the expectations associated with modern observational facilities such as Herschel, ALMA and SOFIA, and the ubiquity of methanol in interstellar gas, precise knowledge of the methanol spectrum is critical. Abundant research has characterized the line positions and quantum assignments in the far infrared, but there is a dearth of line intensity information at most wavelengths. In this work, an empirical database of methanol line intensities from 300 to 500 cm(-1) has been compiled from far-infrared measurements recorded on the Bruker IFS 125 HR Fourier transform spectrometer located at the Jet Propulsion Laboratory. The sum of the integrated line intensities has been computed (Sigma(Int) = 1.13 x 10(-18) cm(-1)/(molecule cm(-2))) at 296 K for 1317 measured features. These have been combined with known assignments for 2v(12)-gs, v(12)-gs, 2v(12)-v(12) plus a few other bands with a small number of transitions in the spectral range of this study. Line intensities of 916 unblended features have been compared to available theoretical calculations of Mekhtiev et al., J. Mol. Spectrosc., 194, 171-178 (1999). These results support the analysis of astronomical observations taken from orbit by the Herschel HIFI instrument. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Brauer, Carolyn S.; Sung, Keeyoon; Pearson, John C.; Brown, Linda R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Xu, Li-Hong] Univ New Brunswick, Dept Phys, Ctr Laser Atom & Mol Sci CLAMS, St John, NB E2L 4L5, Canada. RP Pearson, JC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM John.C.Pearson@jpl.nasa.gov RI Xu, Li-Hong/J-5095-2015; Sung, Keeyoon/I-6533-2015 FU National Aeronautics and Space Administration; Natural Sciences and Engineering Research Council of Canada FX Portions of research described in this paper were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Support for this work was part of the NASA Heterodyne Instrument for Far Infrared on ground calibration campaign. LHX thanks the Natural Sciences and Engineering Research Council of Canada for financial support of this research. Copyright 2011 California Institute of Technology, all rights reserved. NR 64 TC 8 Z9 9 U1 2 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JAN PY 2012 VL 113 IS 2 BP 128 EP 139 DI 10.1016/j.jqsrt.2011.09.012 PG 12 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 873HH UT WOS:000298871200002 ER PT J AU Korkin, SV Lyapustin, AI Marshak, AL AF Korkin, Sergey V. Lyapustin, Alexei I. Marshak, Alexander L. TI On the accuracy of double scattering approximation for atmospheric polarization computations SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Vector radiative transfer; Secondary scattering; Arbitrary scattering law ID RADIATIVE-TRANSFER; ABSORBING MEDIA; ORDERS; MODEL AB Interpretation of multi-angle spectro-polarimetric data in remote sensing of atmospheric aerosols requires fast and accurate methods of solving the vector radiative transfer equation (VRTE). The single and double scattering approximations could provide an analytical framework for the inversion algorithms and are relatively fast; however accuracy assessments of these approximations for the aerosol atmospheres in the atmospheric window channels have been missing. This paper provides such analysis for a vertically homogeneous aerosol atmosphere with weak and strong asymmetry of scattering. In both cases, the double scattering approximation gives a high accuracy result (relative error similar to 0.2%) only for the low optical path similar to 10(-2). As the error rapidly grows with optical thickness, a full VRTE solution is required for the practical remote sensing analysis. It is shown that the scattering anisotropy is not important at low optical thicknesses neither for reflected nor for transmitted polarization components of radiation. Published by Elsevier Ltd. C1 [Korkin, Sergey V.; Lyapustin, Alexei I.; Marshak, Alexander L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Korkin, Sergey V.] Univ Space Res Assoc, Columbia, MD 21044 USA. RP Korkin, SV (reprint author), NASA, Goddard Space Flight Ctr, Code 618, Greenbelt, MD 20771 USA. EM sergey.v.korkin@nasa.gov RI Marshak, Alexander/D-5671-2012; Lyapustin, Alexei/H-9924-2014 OI Lyapustin, Alexei/0000-0003-1105-5739 NR 24 TC 1 Z9 1 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JAN PY 2012 VL 113 IS 2 BP 172 EP 181 DI 10.1016/j.jqsrt.2011.10.008 PG 10 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 873HH UT WOS:000298871200006 ER PT J AU Adamack, AT Stow, CA Mason, DM Rozas, LP Minello, TJ AF Adamack, Aaron T. Stow, Craig A. Mason, Doran M. Rozas, Lawrence P. Minello, Thomas J. TI Predicting the effects of freshwater diversions on juvenile brown shrimp growth and production: a Bayesian-based approach SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Farfantepenaeus aztecus; Restoration; Salt marsh; Freshwater diversion; Mississippi River; Louisiana ID GULF-OF-MEXICO; PENAEUS-AZTECUS IVES; FARFANTEPENAEUS-AZTECUS; NORTHERN GULF; MISSISSIPPI DELTA; BIOENERGETICS MODEL; OXYGEN-CONSUMPTION; SETIFERUS LINNAEUS; CHESAPEAKE BAY; WETLAND LOSS AB Freshwater diversions from the Mississippi River may help restore coastal wetlands in Louisiana, but their implementation will alter temperature and salinity regimes, potentially affecting juvenile shrimp growth and production. We developed a bioenergetics model for brown shrimp Farfantepenaeus aztecus to investigate water temperature and salinity effects on brown shrimp growth. The model used a Bayesian framework that provided estimates of parameter and model uncertainty. Temperature affected shrimp metabolism, whereas salinity modified food availability. Mortality was modeled using a size-dependent function. We examined the effects of diversion timing (February, March, April and May), length (2x 14, as well as 30 and 60 d), temperature change (+1, 0, -1, -5 and -10 degrees C), initial salinity (5, 15, 25), salinity during the diversion (2, 5, 10, 15, 20 and 25) and prey biomass response time (7, 14 and 28 d) on juvenile brown shrimp production. Diversions during February and March had little effect on shrimp, but 30 and 60 d diversions starting in April and May often had large, negative effects on production. April and May diversions that dropped water temperature by 5 degrees C or more could decrease juvenile brown shrimp production by 40 to 60% compared with the baseline, no diversion scenarios. Whether changes in salinity had a positive or negative effect on brown shrimp production depended on the initial salinity of the scenario. Longer diversions and slower prey response times extended the duration brown shrimp were exposed to either the positive or negative effects of diversions, and this magnified the overall (positive or negative) effect on shrimp production. Limiting diversions to February and March when brown shrimp populations are not abundant would minimize negative effects on shrimp production, though managers will be constrained by the needs of other species such as oysters, as well as ecosystem considerations. C1 [Adamack, Aaron T.] Univ Michigan, Cooperat Inst Limnol & Ecosyst Res, Ann Arbor, MI 48108 USA. [Stow, Craig A.; Mason, Doran M.] NOAA, Great Lakes Environm Res Lab, Ann Arbor, MI 48108 USA. [Rozas, Lawrence P.] Natl Marine Fisheries Serv, NOAA, SEFSC, Estuarine Habitats & Coastal Fisheries Ctr, Lafayette, LA 70506 USA. [Minello, Thomas J.] Natl Marine Fisheries Serv, NOAA, SEFSC, Galveston Lab, Galveston, TX 77551 USA. RP Adamack, AT (reprint author), Univ Canberra, Inst Appl Ecol, Canberra, ACT 2601, Australia. EM aaron.adamack@canberra.edu.au OI Mason, Doran/0000-0002-6017-4243; Stow, Craig/0000-0001-6171-7855; Adamack, Aaron/0000-0002-9746-5351 FU Northern Gulf Institute; Southeast Fisheries Science Center; Great Lakes Environmental Research Laboratory FX Personnel from the NOAA Fisheries Service, Southeast Fisheries Science Center, Fishery Ecology Branch assisted in conducting the field growth experiments and processing the growth data used to develop the model. We thank T. Kramer for the preparation of a much improved version of Fig. 3. We acknowledge funding of this research project from the Northern Gulf Institute, Southeast Fisheries Science Center and the Great Lakes Environmental Research Laboratory. The findings and conclusions in this report are those of the authors and do not necessarily represent the views of NOAA. This is contribution number 1600 of the NOAA Great Lakes Environmental Research Laboratory. NR 83 TC 7 Z9 8 U1 1 U2 16 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2012 VL 444 BP 155 EP 173 DI 10.3354/meps09431 PG 19 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 874PP UT WOS:000298970900012 ER PT J AU Zaretsky, EV AF Zaretsky, E. V. TI Rolling bearing steels - a technical and historical perspective SO MATERIALS SCIENCE AND TECHNOLOGY LA English DT Article DE Bearing steels; History; Metallurgy; 52100 ID ELEMENT FATIGUE LIVES; P-S-N; LIFE THEORIES; ROLLER PROFILE; CONTACT; PREDICTION AB Starting about 1920 it becomes easier to track the growth of bearing materials technology. Until 1955, with few exceptions, comparatively little progress was made in this area. AISI 52100 and some carburising grades (AISI 4320, AISI 9310) were adequate for most applications. The catalyst to quantum advances in high-performance rolling-element bearing steels was the advent of the aircraft gas turbine engine. With improved bearing manufacturing and steel processing together with lubrication technology, the potential improvements in bearing life can as much as 80 times that attainable in the late 1950s or as much as 400 times that attainable in 1940. This paper summarises the chemical, metallurgical and physical aspects of bearing steels and their effect on rolling bearing life and reliability: the single most important variable that has significantly increased bearing life and reliability is vacuum processing of bearing steel. Differences between through hardened, case carburised and corrosion resistant steels are discussed. The interrelation of alloy elements and carbides and their effect on bearing life are presented. An equation relating bearing life, steel hardness and temperature is given. Life factors for various steels are suggested and discussed. A relation between compressive residual stress and bearing life is presented. The effects of retained austenite and grain size are discussed. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Zaretsky, EV (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM ezaretsky@sbcglobal.net NR 66 TC 13 Z9 14 U1 3 U2 35 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0267-0836 J9 MATER SCI TECH-LOND JI Mater. Sci. Technol. PD JAN PY 2012 VL 28 IS 1 BP 58 EP 69 DI 10.1179/1743284711Y.0000000043 PG 12 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 866QK UT WOS:000298395900010 ER PT J AU Pappalardo, R AF Pappalardo, Robert TI RONALD GREELEY Planetary pioneer SO NATURE GEOSCIENCE LA English DT News Item C1 NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pappalardo, R (reprint author), NASA, Jet Prop Lab, M-S 321-560,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM robert.pappalardo@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 2 U2 2 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 J9 NAT GEOSCI JI Nat. Geosci. PD JAN PY 2012 VL 5 IS 1 BP 10 EP 10 PG 1 WC Geosciences, Multidisciplinary SC Geology GA 866WT UT WOS:000298417600008 ER PT J AU Fairweather, S Potter, C Crabtree, R Li, S AF Fairweather, Stacey Potter, Christopher Crabtree, Robert Li, Shuang TI A Comparison of Multispectral ASTER and Hyperspectral AVIRIS Multiple Endmember Spectral Mixture Analysis for Sagebrush and Herbaceous Cover in Yellowstone SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Review ID NATIONAL-PARK; IMAGING SPECTROMETER; MAPPING VEGETATION; SAGE-GROUSE; PLANT COVER; GRASSLAND; RANGELAND; EXCHANGE; SOIL; PRECIPITATION AB Remote sensing techniques can provide information on habitat quality, biodiversity, and cover change at the regional scales of sagebrush-steppe dominated systems and with the repeatability necessary for resource management. In this paper, we present the results of multiple endmember spectral mixture analysis applied to Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) and Airborne Visible/Infrared Imaging Spectrometer (AVIRIs) imagery, comparing affects of seasonality and spectral resolution on the discrimination of soil, grass/forb, and sagebrush abundance in Yellowstone National Park. Our results showed that AVIRIS, despite late season phenology, correlated well with herbaceous and sagebrush cover field measurements (R(2) = 0.77 and 0.75, respectively), utilizing high spectral resolution to separate soils from vegetation. However, ASTER-derived values during peak green correlated best with field measurements (0.75 and 0.78). These results demonstrated an effective method to monitor semi-arid regions with readily available imagery and highlight applications for future hyperspectral satellite missions. C1 [Fairweather, Stacey] Montana State Univ, Bozeman, MT 59715 USA. [Fairweather, Stacey; Crabtree, Robert] Yellowstone Ecol Res Ctr, Bozeman, MT 59718 USA. [Potter, Christopher; Li, Shuang] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Fairweather, S (reprint author), Montana State Univ, 2327 Univ Way,3rd Floor, Bozeman, MT 59715 USA. EM chris.potter@nasa.gov NR 56 TC 5 Z9 5 U1 3 U2 19 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA SN 0099-1112 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD JAN PY 2012 VL 78 IS 1 BP 23 EP 33 PG 11 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 873FX UT WOS:000298867600001 ER PT J AU Grant, PM AF Grant, Paul Michael TI Upbraiding the Utilities SO POWER LA English DT Editorial Material C1 [Grant, Paul Michael] EPRI Sci, Palo Alto, CA USA. RP Grant, PM (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM w2agz@w2agz.com NR 0 TC 0 Z9 0 U1 2 U2 2 PU TRADEFAIR GROUP PI HOUSTON PA 11000 RICHMOND, STE 500, HOUSTON, TX 77042 USA SN 0032-5929 J9 POWER JI Power PD JAN PY 2012 VL 156 IS 1 BP 72 EP 72 PG 1 WC Energy & Fuels SC Energy & Fuels GA 876WP UT WOS:000299138800018 ER PT J AU Jelinek, M Bean, AS Antcliff, R Whalen-Pedersen, E Cantwell, A AF Jelinek, Mariann Bean, Alden S. Antcliff, Richard Whalen-Pedersen, Erik Cantwell, April TI 21st-Century R&D New Rules and Roles for the R&D "Lab" of the Future SO RESEARCH-TECHNOLOGY MANAGEMENT LA English DT Article DE Research-on-Research; Lab of the Future; Future of R&D; R&D strategy ID INDUSTRIAL-RESEARCH AB In May 2007, Richard Antcliff challenged IRI members with a presentation asserting the notion that "three tsunamis" were about to break upon R&D managers, demanding urgent response. Technological exponentials, global demographic shifts, and the phenomenon of climate change all posed challenges that promised to transform R&D. How are R&D managers responding to the perfect storm created by those tsunamis? Survey results and interviews of managers at nearly 60 IRI-member companies revealed a range of responses. Open innovation, globally dispersed R&D operations, and an emphasis on collaboration suggest that the R&D lab of the future is far less likely to be "a lab" (especially a single, central corporate lab) than an intricate, dynamic innovation ecosystem. Not only R&D managers, but senior executives and government policy makers as well will have new roles to map in this model for twenty-first-century R&D. C1 [Jelinek, Mariann] Coll William & Mary, Mason Sch Business, Williamsburg, VA 23187 USA. [Jelinek, Mariann] Natl Sci Fdn, Innovat & Org Change Program, Arlington, VA 22230 USA. [Bean, Alden S.] N Carolina State Univ, CIMS, Raleigh, NC USA. [Bean, Alden S.] Lehigh Univ, Bethlehem, PA USA. [Bean, Alden S.] Univ Cincinnati, Cincinnati, OH 45221 USA. [Bean, Alden S.] SUNY Albany, Albany, NY 12222 USA. [Bean, Alden S.] Northwestern Univ, Evanston, IL 60208 USA. [Antcliff, Richard] NASA, Langley Res Ctr, Strateg Relationships Off, Washington, DC USA. [Cantwell, April] N Carolina State Univ, Execut Educ Program, Raleigh, NC USA. RP Jelinek, M (reprint author), Tech Univ Eindhoven Netherlands, Eindhoven, Netherlands. EM Mariann.Jelinek@Mason.wm.edu; abean27@cox.net; Richard.R.Antcliff@nasa.gov; epedersen@kraftfoods.com; acantwell@nc.rr.com RI Gomes, Leonardo/E-9980-2015 FU IRI; ROR committee; NASA; IBM; Center for Innovation Management Studies (CIMS) at North Carolina State University; National Science Foundation [0830340] FX The research reported here was sponsored by IRI and its ROR committee, NASA, IBM, and the Center for Innovation Management Studies (CIMS) at North Carolina State University; the work was funded by National Science Foundation grant #0830340. NR 21 TC 4 Z9 4 U1 4 U2 26 PU INDUSTRIAL RESEARCH INST, INC PI ARLINGTON PA 2200 CLARENDON BLVD, STE 1102, ARLINGTON, VA 22201 USA SN 0895-6308 J9 RES TECHNOL MANAGE JI Res.-Technol. Manage. PD JAN-FEB PY 2012 VL 55 IS 1 BP 16 EP 26 DI 10.5437/08956308X5501011 PG 11 WC Business; Engineering, Industrial; Management SC Business & Economics; Engineering GA 873RL UT WOS:000298900600007 ER PT J AU Antcliff, RR AF Antcliff, Richard R. TI 2012 R&D Trends Forecast Results from the Industrial Research Institute's Annual Survey SO RESEARCH-TECHNOLOGY MANAGEMENT LA English DT Article C1 [Antcliff, Richard R.] NASA, Langley Res Ctr, Washington, DC USA. RP Antcliff, RR (reprint author), NASA, Langley Res Ctr, Washington, DC USA. EM Richard.rantcliff@nasa.gov NR 1 TC 0 Z9 0 U1 0 U2 0 PU INDUSTRIAL RESEARCH INST, INC PI ARLINGTON PA 2200 CLARENDON BLVD, STE 1102, ARLINGTON, VA 22201 USA SN 0895-6308 J9 RES TECHNOL MANAGE JI Res.-Technol. Manage. PD JAN-FEB PY 2012 VL 55 IS 1 BP 27 EP 32 DI 10.5437/08956308X5501010 PG 6 WC Business; Engineering, Industrial; Management SC Business & Economics; Engineering GA 873RL UT WOS:000298900600008 ER PT J AU Hoyt, DP AF Hoyt, Diana P. TI The Social Organization: How to Use Social Media to Tap the Collective Genius of Your Customers and Employees SO RESEARCH-TECHNOLOGY MANAGEMENT LA English DT Book Review C1 [Hoyt, Diana P.] NASA, Off Chief Technologist, Washington, DC USA. RP Hoyt, DP (reprint author), NASA, Off Chief Technologist, Washington, DC USA. EM diana.hoyt@nasa.gov NR 1 TC 0 Z9 0 U1 0 U2 0 PU INDUSTRIAL RESEARCH INST, INC PI ARLINGTON PA 2200 CLARENDON BLVD, STE 1102, ARLINGTON, VA 22201 USA SN 0895-6308 J9 RES TECHNOL MANAGE JI Res.-Technol. Manage. PD JAN-FEB PY 2012 VL 55 IS 1 BP 65 EP 66 PG 2 WC Business; Engineering, Industrial; Management SC Business & Economics; Engineering GA 873RL UT WOS:000298900600015 ER PT J AU Abdul-Aziz, A Woike, MR Oza, NC Matthews, BL Iekki, JD AF Abdul-Aziz, Ali Woike, Mark R. Oza, Nikunj C. Matthews, Bryan L. Iekki, John D. TI Rotor health monitoring combining spin tests and data-driven anomaly detection methods SO STRUCTURAL HEALTH MONITORING-AN INTERNATIONAL JOURNAL LA English DT Article DE online health monitoring; IVHM; rotor disk; data-driven anomaly; crack detection; IMS; orca ID SUPPORT AB Health monitoring is highly dependent on sensor systems that are capable of performing in various engine environmental conditions and able to transmit a signal upon a predetermined crack length, while acting in a neutral form upon the overall performance of the engine system. Efforts are under way at NASA Glenn Research Center through support of the Intelligent Vehicle Health Management Project (IVHM) to develop and implement such sensor technology for a wide variety of applications. These efforts are focused on developing high temperature, wireless, low cost, and durable products. In an effort to address technical issues concerning health monitoring, this article considers data collected from an experimental study using high frequency capacitive sensor technology to capture blade tip clearance and tip timing measurements in a rotating turbine engine-like-disk to detect the disk faults and assess its structural integrity. The experimental results composed at a range of rotational speeds from tests conducted at the NASA Glenn Research Center's Rotordynamics Laboratory are evaluated and integrated into multiple data-driven anomaly detection techniques to identify faults and anomalies in the disk. In summary, this study presents a select evaluation of online health monitoring of a rotating disk using high caliber capacitive sensors and demonstrates the capability of the in-house spin system. C1 [Abdul-Aziz, Ali] Cleveland State Univ, NASA, Glenn Resident Associate, Cleveland, OH 44115 USA. [Woike, Mark R.; Iekki, John D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Oza, Nikunj C.; Matthews, Bryan L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Abdul-Aziz, A (reprint author), Cleveland State Univ, NASA, Glenn Resident Associate, Cleveland, OH 44115 USA. EM ali.abdul-aziz-1@nasa.gov NR 16 TC 5 Z9 5 U1 1 U2 13 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1475-9217 J9 STRUCT HEALTH MONIT JI Struct. Health Monit. PD JAN PY 2012 VL 11 IS 1 BP 3 EP 12 DI 10.1177/1475921710395811 PG 10 WC Engineering, Multidisciplinary; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 874VT UT WOS:000298986900001 ER PT J AU Chandra, V Yu, SU Kim, SH Yoon, YS Kim, DY Kwon, AH Meyyappan, M Kim, KS AF Chandra, Vimlesh Yu, Seong Uk Kim, Seon Ho Yoon, Yo Seob Kim, Dong Young Kwon, Ah Hyun Meyyappan, M. Kim, Kwang S. TI Highly selective CO2 capture on N-doped carbon produced by chemical activation of polypyrrole functionalized graphene sheets SO CHEMICAL COMMUNICATIONS LA English DT Article ID SOLID AMINE SORBENT; DIOXIDE CAPTURE; SURFACE-AREA; ADSORPTION; ADSORBENTS; NITROGEN; OXIDE; FORMALDEHYDE; PERFORMANCE; TRANSISTORS AB N-doped porous carbon produced via chemical activation of polypyrrole functionalized graphene sheets shows selective adsorption of CO2 (4.3 mmol g(-1)) over N-2 (0.27 mmol g(-1)) at 298 K. The potential for large scale production and facile regeneration makes this material useful for industrial applications. C1 [Chandra, Vimlesh; Yu, Seong Uk; Kim, Seon Ho; Yoon, Yo Seob; Kim, Dong Young; Kwon, Ah Hyun; Kim, Kwang S.] Pohang Univ Sci & Technol, Dept Chem, Ctr Superfunct Mat, Pohang 790784, South Korea. [Meyyappan, M.] NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA. [Meyyappan, M.] POSTECH, Div IT CE, Pohang 790784, South Korea. RP Kim, KS (reprint author), Pohang Univ Sci & Technol, Dept Chem, Ctr Superfunct Mat, Pohang 790784, South Korea. EM kim@postech.ac.kr RI Kim, Kwang/C-7538-2012; Yoon, Yoseob/D-5400-2013 OI Kim, Kwang/0000-0002-6929-5359; Yoon, Yoseob/0000-0002-8832-897X FU NRF [2010-0020414, WCU: R32-2008-000-10180-0] FX Funding from NRF (National Honor Scientist Program: 2010-0020414, WCU: R32-2008-000-10180-0) is acknowledged along with WCU-ITCE program. NR 47 TC 123 Z9 128 U1 19 U2 166 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1359-7345 J9 CHEM COMMUN JI Chem. Commun. PY 2012 VL 48 IS 5 BP 735 EP 737 DI 10.1039/c1cc15599g PG 3 WC Chemistry, Multidisciplinary SC Chemistry GA 861EF UT WOS:000298001300029 PM 22117227 ER PT J AU Troglio, G Le Moigne, J Benediktsson, JA Moser, G Serpico, SB AF Troglio, Giulia Le Moigne, Jacqueline Benediktsson, Jon Atli Moser, Gabriele Serpico, Sebastiano B. TI Automatic Extraction of Ellipsoidal Features for Planetary Image Registration SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Crater detection; feature extraction; Hough transform; watershed segmentation ID CRATER DETECTION ALGORITHMS; MARTIAN IMPACT CRATERS; RECOGNITION; MARS AB With the launch of several planetary missions in the last decade, a large amount of planetary images has been already acquired and much more will be available for analysis in the coming years. The image data need to be analyzed, preferably by automatic processing techniques because of the huge amount of data. Although many automatic feature extraction methods have been proposed and utilized for earth remote sensing images, these methods are not always applicable to planetary data that often present low contrast and uneven illumination characteristics. Here, we propose a new unsupervised method for the extraction of different features of elliptical and geometrically compact shapes, such as craters and rocks of compact shape (e.g., boulders), to be used for image registration purposes. This approach is based on the combination of several image processing techniques, including watershed segmentation and the generalized Hough transform. The method potentially has application for extraction of craters, rocks, and other geological features. C1 [Troglio, Giulia; Benediktsson, Jon Atli] Univ Iceland, Fac Elect & Comp Engn, IS-107 Reykjavik, Iceland. [Troglio, Giulia; Moser, Gabriele; Serpico, Sebastiano B.] Univ Genoa, Dept Biophys & Elect Engn, I-16145 Genoa, Italy. [Le Moigne, Jacqueline] NASA, Goddard Space Flight Ctr, Software Engn Div, Greenbelt, MD 20771 USA. RP Troglio, G (reprint author), Univ Iceland, Fac Elect & Comp Engn, IS-107 Reykjavik, Iceland. EM giulia.troglio@unige.it RI Benediktsson, Jon/F-2861-2010 OI Benediktsson, Jon/0000-0003-0621-9647 FU University of Iceland FX Manuscript received September 25, 2010; revised February 15, 2011 and June 21, 2011; accepted June 27, 2011. Date of publication August 30, 2011; date of current version December 23, 2011. This work was supported in part by the Research of Fund of the University of Iceland and started during G. Troglio's research visit to NASA's Goddard Space Flight Center, Greenbelt, MD, USA. NR 27 TC 13 Z9 14 U1 0 U2 17 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD JAN PY 2012 VL 9 IS 1 BP 95 EP 99 DI 10.1109/LGRS.2011.2161263 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 866KY UT WOS:000298380800020 ER PT J AU Doelling, DR Lukashin, C Minnis, P Scarino, B Morstad, D AF Doelling, David R. Lukashin, Constantine Minnis, Patrick Scarino, Benjamin Morstad, Daniel TI Spectral Reflectance Corrections for Satellite Intercalibrations Using SCIAMACHY Data SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Calibrations; satellites; SCanning Imaging Absorption spectroMeter for Atmospheric CartograpHY (SCIAMACHY); spectral response ID HIGH-RESOLUTION RADIOMETER; CALIBRATION; CHANNELS; MODIS AB High-resolution spectra measured by the ENVISAT SCanning Imaging Absorption spectroMeter for Atmospheric CartograpHY (SCIAMACHY) are used to develop spectral correction factors for satellite imager solar channels to improve the transfer of calibrations from one imager to another. SCIAMACHY spectra averaged for various scene types demonstrate the dependence of reflectance on imager spectral response functions. Pseudo imager radiances were computed separately over land and water from SCIAMACHY pixel spectra taken over two tropical domains. Spectral correction factors were computed from these pseudo imager radiance pairs. Intercalibrations performed using matched 12th Geostationary Operational Environmental Satellite and Terra MODerate-resolution Imaging Spectroradiometer (MODIS) visible (similar to 0.65 mu m) channel data over the same domains yielded ocean and land calibration gain and offset differences of 4.5% and 41%, respectively. Applying the spectral correction factors reduces the gain and offset differences to 0.1% and 3.8%, respectively, for free linear regression. Forcing the regression to use the known offset count reduces the land-ocean radiance differences to 0.3% or less. Similar difference reductions were found for matched MODIS and Meteosat-8 Spinning Enhanced Visible and Infrared Imager channel 2 (similar to 0.86 mu m). The results demonstrate that SCIAMACHY-based spectral corrections can be used to significantly improve the transfer of calibration between any pair of imagers measuring reflected solar radiances under similar viewing and illumination conditions. C1 [Doelling, David R.; Lukashin, Constantine; Minnis, Patrick] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Scarino, Benjamin; Morstad, Daniel] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. RP Doelling, DR (reprint author), NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. EM David.R.Doelling@nasa.gov; constantine.lukashin-1@nasa.gov; patrick.minnis-1@nasa.gov; benjiman.r.scarino@nasa.gov RI Richards, Amber/K-8203-2015; Minnis, Patrick/G-1902-2010 OI Minnis, Patrick/0000-0002-4733-6148 FU National Aeronautics and Space Administration Earth Science Mission Directorate; Clouds and the Earth's Radiant Energy System Project; Environmental Sciences Division of the Department of Energy [DE-AI0207ER64546]; National Oceanic and Atmospheric Administration [MOA IA1-1016] FX Manuscript received October 26, 2010; revised March 10, 2011 and June 6, 2011; accepted June 15, 2011. Date of publication August 30, 2011; date of current version December 23, 2011. This work was supported in part by the National Aeronautics and Space Administration Earth Science Mission Directorate through the Modeling, Analysis, and Prediction Program and the Clouds and the Earth's Radiant Energy System Project, by the Environmental Sciences Division of the Department of Energy through the Atmospheric Radiation Measurement Program Interagency Agreement under Contract DE-AI0207ER64546, and by the National Oceanic and Atmospheric Administration Climate Data Records Program through Grant MOA IA1-1016. NR 14 TC 28 Z9 29 U1 0 U2 8 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 JAN PY 2012 VL 9 IS 1 BP 119 EP 123 DI 10.1109/LGRS.2011.2161751 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 866KY UT WOS:000298380800025 ER PT J AU Orleanski, P Michalska, M Nowosielski, W Pearson, JC Ciechanowicz, M Klein, T Risacher, C Helmich, F Jacobs, H Jellema, W de Jonge, A Roelfsema, P Shipman, R di Giorgio, A Teyssier, D AF Orleanski, Piotr Michalska, Malgorzata Nowosielski, Witold Pearson, John C. Ciechanowicz, Mirek Klein, Thomas Risacher, Christophe Helmich, Frank Jacobs, Herman Jellema, Willem de Jonge, Albrecht Roelfsema, Peter Shipman, Russet di Giorgio, Anna Teyssier, David GP IEEE TI Controlling the THz Heterodyne - lesson learned from HIFI/Herschel Mission SO 2012 19th International Conference on Microwave Radar and Wireless Communications (MIKON), Vols 1 and 2 LA English DT Proceedings Paper CT 19th International Conference on Microwaves, Radar and Wireless Communications (MIKON) CY MAY 21-23, 2012 CL Warsaw, POLAND DE HIFI; HERSCHEL; biasing and protection of microwave components ID HIFI AB The Local Oscillator Subsystem (LOS/S) is a part of the HIFI (Heterodyne Instrument for the Far Infrared) project, an infrared heterodyne instrument for astronomical observations on the ESA HERSCHEL Space Observatory. Local Oscillator Subsystem uses the set of sensitive microwave components, essential for frequency multiplication from K/Ka Bands to 480/1910GHz. The paper presents the methods of biasing of the LOU independent microwave amplifiers and diodes. The special care at the design phase was given to different methods of protection against wrong biasing of such components. The results of the protection, implemented in ECU hardware and software, are discussed at the paper, based on the lessons learned from more than four years of pre-launch activities and almost three years of HIFI operations on the orbit. C1 [Orleanski, Piotr; Michalska, Malgorzata; Nowosielski, Witold] Polish Acad Sci, Space Res Ctr, Warsaw, Poland. [Pearson, John C.] Jet Prop Lab, Pasadena, CA USA. [Ciechanowicz, Mirek; Klein, Thomas; Risacher, Christophe] Max Planck Inst Radioastron, Bonn, Germany. [Helmich, Frank; Jacobs, Herman; Jellema, Willem; de Jonge, Albrecht; Roelfsema, Peter; Shipman, Russet] SRON Netherlands Inst Space Res Groningen Utrecht, Groningen, Netherlands. [di Giorgio, Anna] Ist Fis Spazio Interplanetario, Rome, Italy. [Teyssier, David] European Space Astron Ctr, Madrid, Spain. RP Orleanski, P (reprint author), Polish Acad Sci, Space Res Ctr, Warsaw, Poland. NR 9 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4577-1435-1 PY 2012 BP 426 EP 432 PG 7 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA BG8ZA UT WOS:000392845700084 ER PT S AU Chattopadhyay, G Reck, T Schlecht, E Lin, R Deal, W AF Chattopadhyay, Goutam Reck, Theodore Schlecht, Erich Lin, Robert Deal, William GP IEEE TI Cryogenic Amplifier Based Receivers at Submillimeter Wavelengths SO 2012 37TH INTERNATIONAL CONFERENCE ON INFRARED, MILLIMETER, AND TERAHERTZ WAVES (IRMMW-THZ) SE International Conference on Infrared Millimeter and Terahertz Waves LA English DT Proceedings Paper CT 37th International Conference on Infrared, Millimeter, and Terahertz Waves (IRMMW-THz) CY SEP 23-28, 2012 CL Univ Wollongong, Wollongong, AUSTRALIA SP IEEE, USN, Off Naval Res Sci & Technol, ETRI, UOW, Sch Engn Phys, Ctr Ultrahigh Bandwidth Devices Opt Syst, Victoria Suntech Adv Solar Facil, Swinburne, Ctr Micro Photon, Edinburgh Photon, Tydex, TRAS Inc, Inst Photon & Opt Sci, LakeShore, Australian Synchrotron, CSIRO, Univ Wollongong, Inst Superconducting & Elect Mat, Ctr Med Radiat Phys, Univ Sydney, IEEE Microwave Theory & Tech Soc HO Univ Wollongong AB The operating frequency of InP high electron mobility transistor (HEMT) based amplifiers has moved well in the submillimeter-wave frequencies over the last couple of years. Working amplifiers with usable gain in waveguide packages has been reported beyond 700 GHz. When cooled cryogenically, they have shown substantial improvement in their noise temperature. This has opened up the real possibility of cryogenic amplifier based heterodyne receivers at submillimeter wavelengths for ground-based, air-borne, and space-based instruments for astrophysics, planetary, and Earth science applications. This paper provides an overview of the science applications at submillimeter wavelengths that will benefit from this technology. It also describes the current state of the InP HEMT based cryogenic amplifier receivers at submillimeter wavelengths. C1 [Chattopadhyay, Goutam; Reck, Theodore; Schlecht, Erich; Lin, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Chattopadhyay, G (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2162-2027 BN 978-1-4673-1597-5 J9 INT CONF INFRA MILLI PY 2012 PG 2 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BJT74 UT WOS:000330301800121 ER PT S AU Lee, C Chattopadhyay, G Cooper, K Mehdi, I AF Lee, Choonsup Chattopadhyay, Goutam Cooper, Ken Mehdi, Imran GP IEEE TI Curvature Control of Silicon Microlens for THz Dielectric Antenna SO 2012 37TH INTERNATIONAL CONFERENCE ON INFRARED, MILLIMETER, AND TERAHERTZ WAVES (IRMMW-THZ) SE International Conference on Infrared Millimeter and Terahertz Waves LA English DT Proceedings Paper CT 37th International Conference on Infrared, Millimeter, and Terahertz Waves (IRMMW-THz) CY SEP 23-28, 2012 CL Univ Wollongong, Wollongong, AUSTRALIA SP IEEE, USN, Off Naval Res Sci & Technol, ETRI, UOW, Sch Engn Phys, Ctr Ultrahigh Bandwidth Devices Opt Syst, Victoria Suntech Adv Solar Facil, Swinburne, Ctr Micro Photon, Edinburgh Photon, Tydex, TRAS Inc, Inst Photon & Opt Sci, LakeShore, Australian Synchrotron, CSIRO, Univ Wollongong, Inst Superconducting & Elect Mat, Ctr Med Radiat Phys, Univ Sydney, IEEE Microwave Theory & Tech Soc HO Univ Wollongong AB We have controlled the curvature of silicon microlens by changing the amount of photoresist in order to microfabricate hemispherical silicon microlens which can improve the directivity and reduce substrate mode losses. C1 [Lee, Choonsup; Chattopadhyay, Goutam; Cooper, Ken; Mehdi, Imran] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. RP Lee, C (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. EM Choonsup.lee@jpl.nasa.gov NR 5 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2162-2027 BN 978-1-4673-1597-5 J9 INT CONF INFRA MILLI PY 2012 PG 2 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BJT74 UT WOS:000330301800067 ER PT S AU Arslanian, PJ Matin, P AF Arslanian, Peter John Matin, Payam GP ASEE TI AC 2012-3461: UNDERGRADUATE RESEARCH ON CONCEPTUAL DESIGN OF A WIND TUNNEL FOR INSTRUCTIONAL PURPOSES SO 2012 ASEE ANNUAL CONFERENCE SE ASEE Annual Conference & Exposition LA English DT Proceedings Paper CT ASEE Annual Conference CY JUN 10-13, 2012 CL San Antonio, TX SP ASEE ID CONTRACTIONS AB Senior students in the engineering programs are challenged to thoroughly apply their learned engineering knowledge and research skills toward design and implementation of a challenging senior design project. A wind tunnel is often used in mechanical or aerospace engineering programs as a laboratory instrument to gather experimental data for investigation of fluid flow behavior. The authors have conducted research to implement a comprehensive design of a small size inexpensive wind tunnel for instructional purposes {overall length: 1.8105m, maximum diameter (contraction nozzle): 0.375m, working section dimensions: 0.25m in length X 0.125m in diameter}. The objectives of this research project are to engage an undergraduate engineering student: 1) to design a well-structured wind tunnel model by means of fluid mechanics fundamentals and simulation software, and 2) to develop wind tunnel experiments such as flow visualization, lift and drag measurement around different geometries including NACA airfoils. The wind tunnel designed is an open-loop circuit contained of three basic sections: the contraction nozzle, the working or experiment section, and the diffuser nozzle. Fluid thrust is delivered by an axial fan attached to the end of the diffuser nozzle. The Student was able to obtain the geometric properties of the contraction nozzle and diffuser nozzle by fluid mechanics theories governing a constant pressure decrease, or increase respectively. The working section is a duct of constant area that maintains a uniform fluid velocity. The student built the solid models of the contraction nozzle, working section and diffuser nozzle for flow simulation. The performance of the wind tunnel designed has been verified through CFD-based simulation. The data collected from the simulation results indicate that a uniform laminar flow is maintained in the working section as desired. Different testing models such as sphere and infinite wing have been included in the simulation to characterize the performance of the wind tunnel during testing. The simulation results are promising. Extensive engineering knowledge acquired throughout the course of undergraduate study is applied by the student. Significant understanding of shearing forces developed in the boundary layer has been gained throughout this undergraduate research. C1 [Arslanian, Peter John] NASA, Comp Sci Corp, Washington, DC USA. [Matin, Payam] Univ Maryland Eastern Shore, Anne, MD 21853 USA. RP Arslanian, PJ (reprint author), NASA, Comp Sci Corp, Washington, DC USA. NR 13 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC ENGINEERING EDUCATION PI WASHINGTON PA 1818 N STREET, NW SUITE 600, WASHINGTON, DC 20036 USA SN 2153-5965 J9 ASEE ANNU CONF EXPO PY 2012 PG 21 WC Education & Educational Research; Education, Scientific Disciplines; Engineering, Multidisciplinary SC Education & Educational Research; Engineering GA BF1AU UT WOS:000380253704019 ER PT S AU Berland, LK Allen, DT Crawford, RH Farmer, C Guerra, L AF Berland, Leema Kuhn Allen, David T. Crawford, Richard H. Farmer, Cheryl Guerra, Lisa GP ASEE TI LEARNING SCIENCES GUIDED HIGH SCHOOL ENGINEERING CURRICULUM DEVELOPMENT SO 2012 ASEE ANNUAL CONFERENCE SE ASEE Annual Conference & Exposition LA English DT Proceedings Paper CT ASEE Annual Conference CY JUN 10-13, 2012 CL San Antonio, TX SP ASEE ID DESIGN; INQUIRY C1 [Berland, Leema Kuhn] Univ Texas Austin, Sci Educ, Austin, TX 78712 USA. [Allen, David T.] Univ Texas Austin, Chem Engn, Austin, TX 78712 USA. [Allen, David T.] Univ Texas Austin, Ctr Energy & Environm Resources, Austin, TX 78712 USA. [Crawford, Richard H.] Univ Texas Austin, Mech Engn, Austin, TX 78712 USA. [Farmer, Cheryl] UTeachEngineering, Austin, TX USA. [Guerra, Lisa] NASA Headquarters, Washington, DC USA. RP Berland, LK (reprint author), Univ Texas Austin, Sci Educ, Austin, TX 78712 USA. NR 21 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC ENGINEERING EDUCATION PI WASHINGTON PA 1818 N STREET, NW SUITE 600, WASHINGTON, DC 20036 USA SN 2153-5965 J9 ASEE ANNU CONF EXPO PY 2012 PG 10 WC Education & Educational Research; Education, Scientific Disciplines; Engineering, Multidisciplinary SC Education & Educational Research; Engineering GA BF1AT UT WOS:000380252705014 ER PT S AU Dansberry, BE AF Dansberry, Bryan E. GP ASEE TI EXAMINING OUTCOMES DATA FROM AN UNDERGRADUATE INTERNSHIP PROGRAM SO 2012 ASEE ANNUAL CONFERENCE SE ASEE Annual Conference & Exposition LA English DT Proceedings Paper CT ASEE Annual Conference CY JUN 10-13, 2012 CL San Antonio, TX SP ASEE AB In 2008 NASA's Undergraduate Student Research Program (USRP) implemented an end-to-end on-line database system to manage internship processes from application and selection through near-term evaluation and long-term retention outcomes. From 2008 through 2011 this database documented over 10,000 applicants and 1,415 STEM internship experiences. This paper presents initial findings from the analysis of this database, including information on cognitive and affective learning outcomes, post-graduation retention including career and academic choices, and employer return-on-investment metrics. C1 [Dansberry, Bryan E.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. RP Dansberry, BE (reprint author), NASA, Johnson Space Ctr, Houston, TX 77058 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC ENGINEERING EDUCATION PI WASHINGTON PA 1818 N STREET, NW SUITE 600, WASHINGTON, DC 20036 USA SN 2153-5965 J9 ASEE ANNU CONF EXPO PY 2012 PG 8 WC Education & Educational Research; Education, Scientific Disciplines; Engineering, Multidisciplinary SC Education & Educational Research; Engineering GA BF1AT UT WOS:000380252702039 ER PT S AU Farmer, C Allen, DT Berland, LK Crawford, RH Guerra, L AF Farmer, Cheryl Allen, David T. Berland, Leema Kuhn Crawford, Richard H. Guerra, Lisa GP ASEE TI AC 2012-3949: ENGINEER YOUR WORLD: AN INNOVATIVE APPROACH TO DEVELOPING A HIGH SCHOOL ENGINEERING DESIGN COURSE SO 2012 ASEE ANNUAL CONFERENCE SE ASEE Annual Conference & Exposition LA English DT Proceedings Paper CT ASEE Annual Conference CY JUN 10-13, 2012 CL San Antonio, TX SP ASEE ID INQUIRY AB As standards for K-12 engineering learning emerge with the development of the Next Generation Science Standards, the nation's school systems will likely struggle with the question of whether engineering should be employed as a tool for teaching science and mathematics content (i.e., embedded in science and mathematics courses) or treated as a unique discipline in which science and mathematics are employed as tools for solving design challenges (i.e., offered as a standalone course). Acting on the belief that the latter paradigm is a more appropriate depiction of engineering, the UTeachEngineering project at The University of Texas undertook to demonstrate how rigorous engineering content can be deployed in secondary classrooms by developing a year-long high school engineering course built on a foundation of solid research in the learning sciences, couched in the context of a rigorous engineering design process and scaffolded to build engineering skills and habits of mind. This paper explains why UTeachEngineering, a program initially designed to prepare pre-service and in-service educators to teach design- based engineering courses at the secondary level, shifted focus early in the project to developing, piloting, evaluating and refining such a course. It describes the target student population for the course, details the engineering development work required, describes the research-and practice-based principles upon which pedagogical decisions are based, and offers a view into the course content. Finally, it describes the piloting of the course in a small number of Texas high schools during the 2011-2012 academic year, discusses how feedback from this pilot is informing course revisions, and outlines plans for leveraging a partnership with NASA to expand implementation of the revised course and pilot a new teacher mentorship model in 2012-2013. C1 [Farmer, Cheryl] UTeachEngineering, Austin, TX USA. [Allen, David T.; Berland, Leema Kuhn; Crawford, Richard H.] Univ Texas Austin, Austin, TX USA. [Guerra, Lisa] NASA, Washington, DC USA. RP Farmer, C (reprint author), UTeachEngineering, Austin, TX USA. NR 20 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC ENGINEERING EDUCATION PI WASHINGTON PA 1818 N STREET, NW SUITE 600, WASHINGTON, DC 20036 USA SN 2153-5965 J9 ASEE ANNU CONF EXPO PY 2012 PG 20 WC Education & Educational Research; Education, Scientific Disciplines; Engineering, Multidisciplinary SC Education & Educational Research; Engineering GA BF1AT UT WOS:000380252701048 ER PT S AU Guerra, L Allen, DT Crawford, RH Farmer, C AF Guerra, Lisa Allen, David T. Crawford, Richard H. Farmer, Cheryl GP ASEE TI A UNIQUE APPROACH TO CHARACTERIZING THE ENGINEERING DESIGN PROCESS SO 2012 ASEE ANNUAL CONFERENCE SE ASEE Annual Conference & Exposition LA English DT Proceedings Paper CT ASEE Annual Conference CY JUN 10-13, 2012 CL San Antonio, TX SP ASEE C1 [Guerra, Lisa] NASA, Washington, DC 20546 USA. [Allen, David T.] Univ Texas Austin, Chem Engn, Austin, TX 78712 USA. [Allen, David T.] Univ Texas Austin, Ctr Energy & Environm Resources, Austin, TX 78712 USA. [Crawford, Richard H.] Univ Texas Austin, Mech Engn, Austin, TX 78712 USA. [Farmer, Cheryl] UTeachEngineering, Austin, TX USA. RP Guerra, L (reprint author), NASA, Washington, DC 20546 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC ENGINEERING EDUCATION PI WASHINGTON PA 1818 N STREET, NW SUITE 600, WASHINGTON, DC 20036 USA SN 2153-5965 J9 ASEE ANNU CONF EXPO PY 2012 PG 14 WC Education & Educational Research; Education, Scientific Disciplines; Engineering, Multidisciplinary SC Education & Educational Research; Engineering GA BF1AS UT WOS:000380250101073 ER PT S AU Klesh, AT Cutler, JW Atkins, EM AF Klesh, Andrew T. Cutler, James W. Atkins, Ella M. GP IEEE Comp Soc TI Cyber-Physical Challenges for Space Systems SO 2012 IEEE/ACM THIRD INTERNATIONAL CONFERENCE ON CYBER-PHYSICAL SYSTEMS (ICCPS 2012) SE ACM-IEEE International Conference on Cyber-Physical Systems LA English DT Proceedings Paper CT 3rd IEEE/ACM International Conference on Cyber-Physical Systems (ICCPS) CY APR 17-19, 2012 CL Beijing, PEOPLES R CHINA SP ACM, IEEE Comp Soc, IEEE DE space systems; robotics; communication; attitude control AB Modern space systems necessarily have a tight coupling between onboard cyber (processing, communication) and physical (sensing, actuation) elements to survive the harsh extraterrestrial environment and successfully complete ambitious missions. This article first summarizes space exploration missions and existing platforms that to-date have been developed by ad hoc, one-of-a-kind cyber-physical integration efforts. The primary goal of this paper is to present a series of cyber-physical systems (CPS) challenges that, if addressed in the emerging science of CPS, will greatly facilitate complex space systems development in the future. Areas of focus include spacecraft communications, driven by relative orbiting network node positions as well as bandwidth and power considerations, attitude control and orbit determination, and space robotics and science payload systems. A strong CPS challenge problem is introduced: scheduling the instructions executed on a small spacecraft processor such that the magnetic field introduced by this processor induces torques favorable for spacecraft pointing. C1 [Klesh, Andrew T.] CALTECH, Jet Prop Lab, Planetary Missions 312A, Oak Grove, CA USA. [Cutler, James W.; Atkins, Ella M.] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA. RP Klesh, AT (reprint author), CALTECH, Jet Prop Lab, Planetary Missions 312A, Oak Grove, CA USA. EM andrew.t.klesh@jpl.nasa.gov; jwcutler@umich.edu; ematkins@umich.edu NR 27 TC 1 Z9 1 U1 1 U2 2 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA SN 2375-8317 BN 978-0-7695-4695-7 J9 ACM IEEE INT CONF CY PY 2012 BP 45 EP 52 DI 10.1109/ICCPS.2012.13 PG 8 WC Computer Science, Information Systems; Computer Science, Software Engineering; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BG9NL UT WOS:000393451600005 ER PT S AU Kulkarni, CS Celaya, JR Biswas, G Goebel, K AF Kulkarni, Chetan S. Celaya, Jose R. Biswas, Gautam Goebel, Kai GP IEEE TI Prognostics of Power Electronics, methods and validation experiments SO 2012 IEEE AUTOTESTCON PROCEEDINGS SE IEEE Autotestcon LA English DT Proceedings Paper CT IEEE Autotestcon Conference CY SEP 10-13, 2012 CL Anaheim, CA SP Inst Elect & Elect Engineers, IEEE Instrumentat & Measurement Soc, AESS, Disneyland, IEEE Aerosp & Electr Syst Soc AB Failure of electronic devices is a concern for future electric aircrafts that will see an increase of electronics to drive and control safety-critical equipment throughout the aircraft. As a result, investigation of precursors to failure in electronics and prediction of remaining life of electronic components is of key importance. DC-DC power converters are power electronics systems employed typically as sourcing elements for avionics equipment. Current research efforts in prognostics for these power systems focuses on the identification of failure mechanisms and the development of accelerated aging methodologies and systems to accelerate the aging process of test devices, while continuously measuring key electrical and thermal parameters. Preliminary model-based prognostics algorithms have been developed making use of empirical degradation models and physics-inspired degradation model with focus on key components like electrolytic capacitors and power MOSFETs (metal-oxide-semiconductor-field-effect-transistor). This paper presents current results on the development of validation methods for prognostics algorithms of power electrolytic capacitors. Particularly, in the use of accelerated aging systems for algorithm validation. Validation of prognostics algorithms present difficulties in practice due to the lack of run-to-failure experiments in deployed systems. By using accelerated experiments, we circumvent this problem in order to define initial validation activities. C1 [Kulkarni, Chetan S.; Biswas, Gautam] Vanderbilt Univ, Inst Software Integrated Syst, Nashville, TN 37212 USA. [Celaya, Jose R.] NASA, Ames Res Ctr, SGT Inc, Moffett Field, CA 94035 USA. [Goebel, Kai] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kulkarni, CS (reprint author), Vanderbilt Univ, Inst Software Integrated Syst, Nashville, TN 37212 USA. EM chetan.kulkarni@vanderbilt.edu; jose.r.celaya@nasa.gov; gautam.biswas@vanderbilt.edu; kai.goebel@nasa.gov FU NASA Aviation Safety Program; SSAT FX This work was funded by the NASA Aviation Safety Program, SSAT project. NR 18 TC 1 Z9 1 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1088-7725 BN 978-1-4673-0699-7; 978-1-4673-0700-0 J9 IEEE AUTOTESTCON PY 2012 BP 194 EP 199 PG 6 WC Engineering, Electrical & Electronic SC Engineering GA BG9AS UT WOS:000392928300038 ER PT S AU Lansdowne, CA Gorringe, C McCartney, P AF Lansdowne, Chatwin A. Gorringe, Chris McCartney, Patrick GP IEEE TI Experimental Applications of Automatic Test Markup Language (ATML) SO 2012 IEEE AUTOTESTCON PROCEEDINGS SE IEEE Autotestcon LA English DT Proceedings Paper CT IEEE Autotestcon Conference CY SEP 10-13, 2012 CL Anaheim, CA SP Inst Elect & Elect Engineers, IEEE Instrumentat & Measurement Soc, AESS, Disneyland, IEEE Aerosp & Electr Syst Soc DE Software standards; Testing; Test equipment; Test facilities; Software management; Software reusability; Fault diagnosis; Sensor systems and applications; System-level Design AB The authors describe challenging use-cases for Automatic Test Markup Language (ATML), and evaluate solutions. The first case uses ATML Test Results to deliver active features to support test procedure development and test flow, and bridging mixed software development environments. The second case examines adding attributes to Systems Modelling Language (SysML) to create a linkage for deriving information from a model to fill in an ATML document set. Both cases are outside the original concept of operations for ATML but are typical for integrating large heterogeneous systems with modular contributions from multiple disciplines. C1 [Lansdowne, Chatwin A.] NASA, Houston, TX 77058 USA. [Gorringe, Chris] Cassidian Test Engn Serv Ltd, Houston, TX USA. [McCartney, Patrick] METECS, Houston, TX 77058 USA. RP Lansdowne, CA (reprint author), NASA, Houston, TX 77058 USA. EM chatwin.lansdowne@nasa.gov; chris.gorringe@eads-ts.com FU NASA CIO Information Technology Labs Study FX Manuscript received June 1, 2012. This work was performed in NASA Johnson Space Center's Avionics Systems Division, collaboratively with Cassidian. Funding was provided by a NASA CIO Information Technology Labs Study. NR 7 TC 0 Z9 1 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1088-7725 BN 978-1-4673-0699-7; 978-1-4673-0700-0 J9 IEEE AUTOTESTCON PY 2012 BP 318 EP 323 PG 6 WC Engineering, Electrical & Electronic SC Engineering GA BG9AS UT WOS:000392928300060 ER PT S AU Kulkarni, CS Celaya, JR Biswas, G Goebel, K AF Kulkarni, Chetan S. Celaya, Jose R. Biswas, Gautam Goebel, Kai GP IEEE TI Accelerated Aging Experiments for Capacitor Health Monitoring and Prognostics SO 2012 IEEE AUTOTESTCON PROCEEDINGS SE IEEE Autotestcon LA English DT Proceedings Paper CT IEEE Autotestcon Conference CY SEP 10-13, 2012 CL Anaheim, CA SP Inst Elect & Elect Engineers, IEEE Instrumentat & Measurement Soc, AESS, Disneyland, IEEE Aerosp & Electr Syst Soc AB This paper discusses experimental setups for health monitoring and prognostics of electrolytic capacitors under nominal operation and accelerated aging conditions. Electrolytic capacitors have higher failure rates than other components in electronic systems like power drives, power converters etc. Our current work focuses on developing first-principles-based degradation models for electrolytic capacitors under varying electrical and thermal stress conditions. Prognostics and health management for electronic systems aims to predict the onset of faults, study causes for system degradation, and accurately compute remaining useful life. Accelerated life test methods are often used in prognostics research as a way to model multiple causes and assess the effects of the degradation process through time. It also allows for the identification and study of different failure mechanisms and their relationships under different operating conditions. Experiments are designed for aging of the capacitors such that the degradation pattern induced by the aging can be monitored and analyzed. Experimental setups and data collection methods are presented to demonstrate this approach. C1 [Kulkarni, Chetan S.; Biswas, Gautam] Vanderbilt Univ, Inst Software Integrated Syst, 221 Kirkland Hall, Nashville, TN 37235 USA. [Celaya, Jose R.] SGT Inc, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Goebel, Kai] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kulkarni, CS (reprint author), Vanderbilt Univ, Inst Software Integrated Syst, 221 Kirkland Hall, Nashville, TN 37235 USA. EM chetan.kulkarni@vanderbilt.edu; jose.r.celaya@nasa.gov; gautam.biswas@vanderbilt.edu; kai.goebel@nasa.gov FU NASA Aviation Safety Program; SSAT project FX This work was funded by the NASA Aviation Safety Program, SSAT project. NR 12 TC 2 Z9 2 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1088-7725 BN 978-1-4673-0699-7; 978-1-4673-0700-0 J9 IEEE AUTOTESTCON PY 2012 BP 356 EP 361 PG 6 WC Engineering, Electrical & Electronic SC Engineering GA BG9AS UT WOS:000392928300067 ER PT S AU Chen, CW Piepmeier, JR Johnson, JT Ghaemi, H AF Chen, Curtis W. Piepmeier, Jeffrey R. Johnson, Joel T. Ghaemi, Hirad GP IEEE TI ASSESSMENT OF THE IMPACTS OF RADIO FREQUENCY INTERFERENCE ON SMAP RADAR AND RADIOMETER MEASUREMENTS SO 2012 IEEE INTERNATIONAL GEOSCIENCE AND REMOTE SENSING SYMPOSIUM (IGARSS) SE IEEE International Symposium on Geoscience and Remote Sensing IGARSS LA English DT Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS) CY JUL 22-27, 2012 CL Munich, GERMANY SP IEEE, IEEE Geosci & Remote Sensing Soc, DLR, ESA DE Soil moisture remote sensing; microwave radar; microwave radiometry; radio frequency interference ID MICROWAVE RADIOMETRY; ALGORITHMS; SALINITY; MISSION; SMOS AB The NASA Soil Moisture Active and Passive (SMAP) mission will measure soil moisture with a combination of L-band radar and radiometer measurements. We present an assessment of the expected impact of radio frequency interference (RFI) on SMAP performance, incorporating projections based on recent data collected by the Aquarius and SMOS missions. We discuss the impacts of RFI on the radar and radiometer separately given the differences in (1) RFI environment between the shared radar band and the protected radiometer band, (2) mitigation techniques available for the different measurements, and (3) existing data sources available that can inform predictions for SMAP. C1 [Chen, Curtis W.; Ghaemi, Hirad] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Piepmeier, Jeffrey R.] NASA, GSFC, Los Angeles, CA USA. [Johnson, Joel T.] Ohio State Univ, Columbus, OH 43210 USA. RP Chen, CW (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 16 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2153-6996 BN 978-1-4673-1159-5 J9 INT GEOSCI REMOTE SE PY 2012 BP 1 EP 4 DI 10.1109/IGARSS.2012.6351538 PG 4 WC Engineering, Electrical & Electronic; Geosciences, Multidisciplinary; Remote Sensing SC Engineering; Geology; Remote Sensing GA BDG99 UT WOS:000313189400001 ER PT S AU Reeves, JD Eveleigh, T Holzer, T Sarkani, S AF Reeves, John D. Eveleigh, Tim Holzer, Thomas Sarkani, Shahryar GP IEEE TI The Impact of Early Design Phase Risk Identification Biases on Space System Project Performance SO 2012 IEEE INTERNATIONAL SYSTEMS CONFERENCE (SYSCON) SE Annual IEEE Systems Conference LA English DT Proceedings Paper CT 6th IEEE International Systems Conference (SYS CON) CY MAR 19-22, 2012 CL Vancouver, CANADA SP IEEE, IEEE Syst Council, INCOSE, IEEE Vancouver Sect DE costs; project management; risk analysis; space vehicles; systems engineering and theory AB Risk identification during the early design phases of complex systems is commonly implemented but often fails to result in the identification of events and circumstances that truly challenge project performance. Inefficiencies in cost and schedule estimation are usually held accountable for cost and schedule overruns, but the true root cause is often the realization of programmatic risks. A deeper understanding of frequent risk identification trends and biases pervasive during space system design and development is needed, for it would lead to improved execution of existing identification processes and methods. C1 [Reeves, John D.] NASA, Space Miss Anal Branch, Langley Res Ctr, Hampton, VA 23681 USA. [Eveleigh, Tim; Holzer, Thomas; Sarkani, Shahryar] George Washington Univ, Dept Engn Management & Syst Engn, Washington, DC 20052 USA. RP Reeves, JD (reprint author), NASA, Space Miss Anal Branch, Langley Res Ctr, Hampton, VA 23681 USA. EM john.d.reeves@nasa.gov NR 17 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1944-7620 BN 978-1-4673-0749-9 J9 ANN IEEE SYST CONF PY 2012 BP 657 EP 664 PG 8 WC Engineering, Industrial; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BEK23 UT WOS:000317054300106 ER PT J AU McKenzie, C Parness, A AF McKenzie, Clifford Parness, Aaron BE Azad, AKM Cowan, NJ Tokhi, MO Virk, GS Eastman, RD TI DROP THE DURABLE RECONNAISSANCE AND OBSERVATION PLATFORM SO ADAPTIVE MOBILE ROBOTICS LA English DT Proceedings Paper CT 15th International Conference on Climbing and Walking Robots and the Support Technologies for Mobile Machines CY JUL 23-26, 2012 CL Baltimore, MD SP Assoc Advancement Med Instrumentat, Inst Mech Engineers, No Illinois Univ, Johns Hopkins Univ, CLAWAR Assoc, Loyola Univ, Univ Maryland, Natl Inst Stand & Technol AB The Durable Reconnaissance and Observation Platform (DROP) is a prototype robotic platform with the ability to climb concrete surfaces up to 85 degrees at a rate of 25cm/s, make rapid horizontal to vertical transitions, carry an audio/visual reconnaissance payload, and survive impacts from 3 meters. The platform uses a two-wheel, two-motor design that delivers high mobility with low complexity. DROP extends microspine climbing technology from a linear to rotary implementation, providing improved transition ability, increased speeds, and simpler body mechanics while maintaining microspines' ability to opportunistically grip rough surfaces. Various aspects of the prototype robot's design and performance are discussed, including the climbing mechanism, body design, and impact survival. C1 [McKenzie, Clifford] N Carolina State Univ, Dept Mech & Aerosp Engn, Raleigh, NC 27695 USA. [Parness, Aaron] CALTECH, Jet Prop Lab, Robot Platforms Grp, Pasadena, CA 91109 USA. RP McKenzie, C (reprint author), N Carolina State Univ, Dept Mech & Aerosp Engn, Raleigh, NC 27695 USA. NR 12 TC 0 Z9 0 U1 0 U2 0 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 978-981-4415-94-1 PY 2012 BP 623 EP 630 PG 8 WC Robotics SC Robotics GA BC4AM UT WOS:000352212900080 ER PT B AU Cowley, MS Margerum, S Harvill, L Rajulu, S AF Cowley, Matthew S. Margerum, Sarah Harvill, Lauren Rajulu, Sudhakar BE Duffy, VG TI Model for Predicting the Performance of Planetary Suit Hip Bearing Designs SO ADVANCES IN APPLIED HUMAN MODELING AND SIMULATION SE Advances in Human Factors and Ergonomics Series LA English DT Article; Book Chapter DE space suit; design; modeling; performance AB Designing a space suit is very complex and often requires difficult trade-offs between performance, cost, mass, and system complexity. During the development period of the suit numerous design iterations need to occur before the hardware meets human performance requirements. Using computer models early in the design phase of hardware development is advantageous, by allowing virtual prototyping to take place. A virtual design environment allows designers to think creatively, exhaust design possibilities, and study design impacts on suit and human performance. A model of the rigid components of the Mark III Technology Demonstrator Suit ( planetary-type space suit) and a human manikin were created and tested in a virtual environment. The performance of the Mark III hip bearing model was first developed and evaluated virtually by comparing the differences in mobility performance between the nominal bearing configurations and modified bearing configurations. Suited human performance was then simulated with the model and compared to actual suited human performance data using the same bearing configurations. The Mark III hip bearing model was able to visually represent complex bearing rotations and the theoretical volumetric ranges of motion in three dimensions. The model was also able to predict suited human hip flexion and abduction maximums to within 10% of the actual suited human subject data, except for one modified bearing condition in hip flexion that was off by 24%. Differences between the model predictions and the human subject performance data were attributed to the lack of joint moment limits in the model, human subject fitting issues, and the limited suit experience of some of the subjects. The results demonstrate that modeling space suit rigid segments is a feasible design tool for evaluating and optimizing suited human performance. C1 [Cowley, Matthew S.; Margerum, Sarah; Harvill, Lauren] Lockheed Martin, Houston, TX 77258 USA. [Rajulu, Sudhakar] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Cowley, MS (reprint author), Lockheed Martin, 1300 Hercules, Houston, TX 77258 USA. EM matthew.s.cowley@lmco.com; sudhakar.rajulu-1@nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-7032-7; 978-1-4398-7031-0 J9 ADV HUM FACT ERG SER JI ADV. HUMAN FACT. ERG. SER PY 2012 BP 317 EP 326 PG 10 WC Ergonomics SC Engineering GA BC2WC UT WOS:000351388700031 ER PT B AU England, S Benson, E Cowley, M Harvill, L Blackledge, C Perez, E Rajulu, S AF England, Scott Benson, Elizabeth Cowley, Matthew Harvill, Lauren Blackledge, Christopher Perez, Esau Rajulu, Sudhakar BE Duffy, VG TI Comparative Ergonomic Evaluation of Spacesuit and Space Vehicle Design SO ADVANCES IN APPLIED HUMAN MODELING AND SIMULATION SE Advances in Human Factors and Ergonomics Series LA English DT Article; Book Chapter DE Spacesuits; Anthropometry; Ergonomics; Biomechanics; Human System Integration; NASA; Motion Capture; Population Analysis AB With the advent of the latest human spaceflight objectives, a series of prototype architectures have been developed for a new launch and reentry spacesuit that would fit with the new mission goals. Four prototype suits were evaluated to compare their performance and enable selection of the preferred suit components and designs. A consolidated approach to testing was taken: concurrently collecting suit mobility data, seat-suit-vehicle interface clearances, and qualitative assessments of suit performance within the volume of a Multi-Purpose Crew Vehicle mockup. It was necessary to maintain high fidelity in a mockup and use advanced motion-capture technologies to achieve the objectives of the study. These seemingly mutually exclusive goals were accommodated with the construction of an optically transparent and fully adjustable frame mockup. The construction of the mockup was such that it could be dimensionally validated rapidly with the motion-capture system. This paper describes the method used to create a space vehicle mockup compatible with use of an optical motion-capture system, the consolidated approach for evaluating spacesuits in action, and a way to use the complex data set resulting from a limited number of test subjects to generate hardware requirements for an entire population. Kinematics, hardware clearance, anthropometry (suited and unsuited), and subjective feedback data were recorded on 15 unsuited and 5 suited subjects. The selection of unsuited subjects was chiefly based on their anthropometry in an attempt to find subjects who fell within predefined criteria for medium male, large male, and small female subjects. The suited subjects were selected as a subset of the unsuited medium male subjects and were tested in both unpressurized and pressurized conditions. The prototype spacesuits were each fabricated in a single size to accommodate an approximately average-sized male, so select findings from the suit testing were systematically extrapolated to the extremes of the population to anticipate likely problem areas. This extrapolation was achieved by first comparing suited subjects' performance with their unsuited performance, and then applying the results to the entire range of the population. The use of a transparent space vehicle mockup enabled the collection of large amounts of data during human-in-the-loop testing. Mobility data revealed that most of the tested spacesuits had sufficient ranges of motion for the selected tasks to be performed successfully. A suited subject's inability to perform a task most often stemmed from a combination of poor field of view in a seated position and poor dexterity of the pressurized gloves, or from suit/vehicle interface issues. Seat ingress and egress testing showed that problems with anthropometric accommodation did not exclusively occur with the largest or smallest subjects, but also with specific combinations of measurements that led to narrower seat ingress/egress clearance. C1 [England, Scott; Benson, Elizabeth; Blackledge, Christopher] MEI Technol Inc, Houston, TX 77058 USA. [Cowley, Matthew; Harvill, Lauren; Perez, Esau] Lockheed Martin, Houston, TX 77058 USA. [Rajulu, Sudhakar] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP England, S (reprint author), MEI Technol Inc, 2525 Bay Area Blvd Suite 300, Houston, TX 77058 USA. NR 1 TC 3 Z9 3 U1 0 U2 1 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-7032-7; 978-1-4398-7031-0 J9 ADV HUM FACT ERG SER JI ADV. HUMAN FACT. ERG. SER PY 2012 BP 374 EP 383 PG 10 WC Ergonomics SC Engineering GA BC2WC UT WOS:000351388700037 ER PT J AU Tibbs, CT Paladini, R Dickinson, C AF Tibbs, Christopher T. Paladini, Roberta Dickinson, Clive TI On the Limitations of the Anomalous Microwave Emission Emissivity SO ADVANCES IN ASTRONOMY LA English DT Article ID CENTIMETER-WAVE CONTINUUM; SPINNING DUST EMISSION; ANISOTROPY-PROBE; MOLECULAR CLOUD; RADIATION; GALAXY; MODEL; EVOLUTION; EXCESS; REGION AB Many studies of anomalous microwave emission (AME) have computed an AME emissivity to compare the strength of the AME detected in different regions. Such a value is usually defined as the ratio between the intensity of the AME at 1 cm and the thermal dust emission at 100 mu m. However, as studies of Galactic dust emission have shown, the intensity of the thermal dust emission at 100 mu m is strongly dependent on the dust temperature, which has severe implications for the AME emissivity defined in this way. In this work, we illustrate and quantify this effect and find that the AME emissivity decreases by a factor of 11.1 between dust temperatures of 20 and 30 K. We, therefore, conclude that computing the AME emissivity relative to the 100 mu m emission does not allow for accurate comparisons between the AME observed in different environments. With this in mind, we investigate the use of other tracers of the dust emission with which to compute the AME emissivity and we ultimately conclude that, despite the difficulty in deriving its value, the column density of the dust would be the most suitable quantity with which to compute the AME emissivity. C1 [Tibbs, Christopher T.] CALTECH, Spitzer Sci Ctr, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Paladini, Roberta] CALTECH, NASA, Herschel Sci Ctr, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Dickinson, Clive] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Tibbs, CT (reprint author), CALTECH, Spitzer Sci Ctr, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. EM ctibbs@ipac.caltech.edu FU SFTC Advanced Fellowship; EU Marie-Curie IRG Grant; NASA/ADP ROSES [09-ADP09-0059] FX The authors thank the referee for useful comments which helped improve the content of the paper. This work has been performed within the framework of a NASA/ADP ROSES-2009 Grant no. 09-ADP09-0059. C. Dickinson acknowledges the support from an SFTC Advanced Fellowship and an EU Marie-Curie IRG Grant under the FP7. NR 39 TC 3 Z9 3 U1 0 U2 0 PU HINDAWI PUBLISHING CORPORATION PI NEW YORK PA 410 PARK AVENUE, 15TH FLOOR, #287 PMB, NEW YORK, NY 10022 USA SN 1687-7969 EI 1687-7977 J9 ADV ASTRON JI Adv. Astron. PY 2012 AR 124931 DI 10.1155/2012/124931 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA V30RP UT WOS:000208833400001 ER PT B AU Way, MJ Scargle, JD Ali, KM Srivastava, AN AF Way, Michael J. Scargle, Jeffrey D. Ali, Kamal M. Srivastava, Ashok N. BE Way, MJ Scargle, JD Ali, KM Srivastava, AN TI Perspective SO ADVANCES IN MACHINE LEARNING AND DATA MINING FOR ASTRONOMY SE Chapman & Hall-CRC Data Mining and Knowledge Discovery Series LA English DT Editorial Material; Book Chapter C1 [Way, Michael J.] NASA Goddard Inst Space Studies, New York, NY 10025 USA. [Ali, Kamal M.] Stanford Univ, Stanford, CA 94305 USA. [Srivastava, Ashok N.] NASA Ames Res Ctr, Data Min & Syst Hlth Management, New York, NY USA. RP Way, MJ (reprint author), NASA Goddard Inst Space Studies, New York, NY 10025 USA. NR 13 TC 13 Z9 13 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-4174-7; 978-1-4398-4173-0 J9 CH CRC DATA MIN KNOW PY 2012 BP XIII EP XXIV PG 12 WC Computer Science, Information Systems; Computer Science, Theory & Methods SC Computer Science GA BC2TP UT WOS:000351309800002 ER PT B AU Scargle, JD AF Scargle, Jeffrey D. BE Way, MJ Scargle, JD Ali, KM Srivastava, AN TI Probability and Statistics in Astronomical Machine Learning and Data Mining SO ADVANCES IN MACHINE LEARNING AND DATA MINING FOR ASTRONOMY SE Chapman & Hall-CRC Data Mining and Knowledge Discovery Series LA English DT Article; Book Chapter C1 NASA Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP Scargle, JD (reprint author), NASA Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-4174-7; 978-1-4398-4173-0 J9 CH CRC DATA MIN KNOW PY 2012 BP 27 EP 36 PG 10 WC Computer Science, Information Systems; Computer Science, Theory & Methods SC Computer Science GA BC2TP UT WOS:000351309800005 ER PT B AU Jenkins, JM Smith, JC Tenenbaum, P Twicken, JD Van Cleve, J AF Jenkins, Jon M. Smith, Jeffrey C. Tenenbaum, Peter Twicken, Joseph D. Van Cleve, Jeffrey BE Way, MJ Scargle, JD Ali, KM Srivastava, AN TI Planet Detection The Kepler Mission SO ADVANCES IN MACHINE LEARNING AND DATA MINING FOR ASTRONOMY SE Chapman & Hall-CRC Data Mining and Knowledge Discovery Series LA English DT Article; Book Chapter ID TRANSITING PLANET; LOW-DENSITY; STAR; CANDIDATES; SCIENCE; VARIABILITY; PERFORMANCE; DISCOVERY; COMPANION; SYSTEM C1 [Jenkins, Jon M.; Smith, Jeffrey C.; Tenenbaum, Peter; Twicken, Joseph D.; Van Cleve, Jeffrey] SETI Inst, Mountain View, CA 94043 USA. [Jenkins, Jon M.; Smith, Jeffrey C.; Tenenbaum, Peter] NASA Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA USA. [Twicken, Joseph D.] NASA Ames Res Ctr, Programs & Projects Directorate, Moffett Field, CA USA. [Van Cleve, Jeffrey] NASA Ames Res Ctr, Sci Directorate, Moffett Field, CA USA. RP Jenkins, JM (reprint author), SETI Inst, Mountain View, CA 94043 USA. NR 47 TC 2 Z9 2 U1 1 U2 1 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-4174-7; 978-1-4398-4173-0 J9 CH CRC DATA MIN KNOW PY 2012 BP 355 EP 381 PG 27 WC Computer Science, Information Systems; Computer Science, Theory & Methods SC Computer Science GA BC2TP UT WOS:000351309800019 ER PT B AU Oza, N AF Oza, Nikunj BE Way, MJ Scargle, JD Ali, KM Srivastava, AN TI Classification SO ADVANCES IN MACHINE LEARNING AND DATA MINING FOR ASTRONOMY SE Chapman & Hall-CRC Data Mining and Knowledge Discovery Series LA English DT Article; Book Chapter C1 NASA Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. RP Oza, N (reprint author), NASA Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. NR 22 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-4174-7; 978-1-4398-4173-0 J9 CH CRC DATA MIN KNOW PY 2012 BP 505 EP 522 PG 18 WC Computer Science, Information Systems; Computer Science, Theory & Methods SC Computer Science GA BC2TP UT WOS:000351309800025 ER PT B AU Wagstaff, KL AF Wagstaff, Kiri L. BE Way, MJ Scargle, JD Ali, KM Srivastava, AN TI Data Clustering SO ADVANCES IN MACHINE LEARNING AND DATA MINING FOR ASTRONOMY SE Chapman & Hall-CRC Data Mining and Knowledge Discovery Series LA English DT Article; Book Chapter ID GAMMA-RAY BURSTS; K-MEANS C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Wagstaff, KL (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 55 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-4174-7; 978-1-4398-4173-0 J9 CH CRC DATA MIN KNOW PY 2012 BP 543 EP 561 PG 19 WC Computer Science, Information Systems; Computer Science, Theory & Methods SC Computer Science GA BC2TP UT WOS:000351309800027 ER PT B AU Das, K Bhaduri, K AF Das, Kamalika Bhaduri, Kanishka BE Way, MJ Scargle, JD Ali, KM Srivastava, AN TI Parallel and Distributed Data Mining for Astronomy Applications SO ADVANCES IN MACHINE LEARNING AND DATA MINING FOR ASTRONOMY SE Chapman & Hall-CRC Data Mining and Knowledge Discovery Series LA English DT Article; Book Chapter ID HETEROGENEOUS DATA; NETWORKS; ALGORITHMS; REGRESSION C1 [Das, Kamalika; Bhaduri, Kanishka] NASA Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. RP Das, K (reprint author), NASA Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. NR 77 TC 1 Z9 1 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-4174-7; 978-1-4398-4173-0 J9 CH CRC DATA MIN KNOW PY 2012 BP 595 EP 615 PG 21 WC Computer Science, Information Systems; Computer Science, Theory & Methods SC Computer Science GA BC2TP UT WOS:000351309800029 ER PT B AU Crespo, LG Munoz, CA Narkawicz, AJ Kenny, SP Giesy, DP AF Crespo, L. G. Munoz, C. A. Narkawicz, A. J. Kenny, S. P. Giesy, D. P. BE Berenguer, C Grall, A Soares, CG TI Uncertainty analysis via failure domain characterization: Polynomial requirement functions SO ADVANCES IN SAFETY, RELIABILITY AND RISK MANAGEMENT LA English DT Proceedings Paper CT European Safety And Reliability Conference (ESREL) CY SEP 18-22, 2011 CL FRANCE SP Univ Technologie Troyes, European Safety & Reliabil Assoc, Reg Champagne Ardenne, Ville Troyes, Ctr Natl Rech Sci, Electricite France, GIS 3SGS, Det Norske Veritas, Grand Troyes, GDR MACS CNRS, MAIF AB This paper proposes an uncertainty analysis framework based on the characterization of the uncertain parameter space. This characterization enables the identification of worst-case uncertainty combinations and the approximation of the failure and safe domains with a high level of accuracy. Because these approximations are comprised of subsets of readily computable probability, they enable the calculation of arbitrarily tight upper and lower bounds to the failure probability. A Bernstein expansion approach is used to size hyper-rectangular subsets while a sum of squares programming approach is used to size quasi-ellipsoidal subsets. These methods are applicable to requirement functions whose functional dependency on the uncertainty is a known polynomial. Some of the most prominent features of the methodology are the substantial desensitization of the calculations from the uncertainty model assumed (i.e., the probability distribution describing the uncertainty) as well as the accommodation for changes in such a model with a practically insignificant amount of computational effort. C1 [Crespo, L. G.] NIA, Hampton, VA 23666 USA. [Munoz, C. A.; Narkawicz, A. J.; Kenny, S. P.; Giesy, D. P.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. NR 13 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-0-203-13510-5; 978-0-415-68379-1 PY 2012 BP 1153 EP 1160 PG 8 WC Engineering, Industrial; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BG8LW UT WOS:000392426502021 ER PT B AU Crespo, LG Kenny, SP Giesy, DP AF Crespo, L. G. Kenny, S. P. Giesy, D. P. BE Berenguer, C Grall, A Soares, CG TI Uncertainty analysis via failure domain characterization: Unrestricted requirement functions SO ADVANCES IN SAFETY, RELIABILITY AND RISK MANAGEMENT LA English DT Proceedings Paper CT European Safety And Reliability Conference (ESREL) CY SEP 18-22, 2011 CL FRANCE SP Univ Technologie Troyes, European Safety & Reliabil Assoc, Reg Champagne Ardenne, Ville Troyes, Ctr Natl Rech Sci, Electricite France, GIS 3SGS, Det Norske Veritas, Grand Troyes, GDR MACS CNRS, MAIF ID DESIGN AB This paper proposes an uncertainty analysis framework based on the characterization of the uncertain parameter space. This characterization enables the identification of worst-case uncertainty combinations and the approximation of the failure and safe domains with a high level of accuracy. Because these approximations are comprised of subsets of readily computable probability, they enable the calculation of arbitrarily tight upper and lower bounds to the failure probability. The methods developed herein, which are based on nonlinear constrained optimization, are applicable to requirement functions whose functional dependency on the uncertainty is arbitrary and whose explicit form may even be unknown. Some of the most prominent features of the methodology are the substantial desensitization of the calculations from the assumed uncertainty model (i.e., the probability distribution describing the uncertainty) as well as the accommodation for changes in such a model with a practically insignificant amount of computational effort. C1 [Crespo, L. G.] NIA, Hampton, VA 23666 USA. [Kenny, S. P.; Giesy, D. P.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. NR 8 TC 1 Z9 1 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-0-203-13510-5; 978-0-415-68379-1 PY 2012 BP 2205 EP 2212 PG 8 WC Engineering, Industrial; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BG8LW UT WOS:000392426503028 ER PT S AU Ye, J Yanovsky, I Dong, B Gandlin, R Brandt, A Osher, S AF Ye, Jian Yanovsky, Igor Dong, Bin Gandlin, Rima Brandt, Achi Osher, Stanley BE Bebis, G Boyle, R Parvin, B Koracin, D Fowlkes, C Wang, S Choi, MH Mantler, S Schulze, J Acevedo, D Mueller, K Papka, M TI Multigrid Narrow Band Surface Reconstruction via Level Set Functions SO ADVANCES IN VISUAL COMPUTING, ISVC 2012, PT I SE Lecture Notes in Computer Science LA English DT Proceedings Paper CT 8th International Symposium on Visual Computing (ISVC) CY JUL 16-18, 2012 CL Rethymnon, GREECE SP BAE Syst, Intel, Ford, Hewlett Packard, Mitsubishi Elect Res Labs, Toyota, Gen Elect, UNR Comp Vis Lab, Desert Res Inst, Berkeley Lab, NASA DE Level set; multigrid method; point cloud; surface reconstruction ID SHAPE RECONSTRUCTION; EQUATIONS AB In this paper we propose a novel fast method for implicit surface reconstruction from unorganized point clouds. Our algorithm employs a multigrid solver on a narrow band of the level set function that represents the reconstructed surface, which greatly improves computational efficiency of surface reconstruction. The new model can accurately reconstruct surfaces from noisy unorganized point clouds that also have missing information. C1 [Ye, Jian; Brandt, Achi; Osher, Stanley] Univ Calif Los Angeles, Dept Math, Los Angeles, CA 90024 USA. [Yanovsky, Igor] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Yanovsky, Igor] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Dong, Bin] Univ Arizona, Dept Math, Tucson, AZ 85721 USA. [Gandlin, Rima] Carnegie Mellon Univ, Dept Math, Pittsburgh, PA 15213 USA. [Brandt, Achi] Weizmann Inst Sci, Dept Comp Sci & Appl Math, IL-76100 Rehovot, Israel. RP Ye, J (reprint author), Univ Calif Los Angeles, Dept Math, Los Angeles, CA 90024 USA. NR 19 TC 2 Z9 2 U1 0 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 978-3-642-33179-4 J9 LECT NOTES COMPUT SC PY 2012 VL 7431 BP 61 EP 70 PG 10 WC Computer Science, Artificial Intelligence; Computer Science, Information Systems; Computer Science, Theory & Methods; Mathematical & Computational Biology SC Computer Science; Mathematical & Computational Biology GA BD7LL UT WOS:000363266600007 ER PT S AU Tilton, JC Comer, DC Priebe, CE Sussman, D Chen, L AF Tilton, James C. Comer, Douglas C. Priebe, Carey E. Sussman, Daniel Chen, Li BE Shen, SS Lewis, PE TI Refinement of a Method for Identifying Probable Archaeological Sites from Remotely Sensed Data SO ALGORITHMS AND TECHNOLOGIES FOR MULTISPECTRAL, HYPERSPECTRAL, AND ULTRASPECTRAL IMAGERY XVIII SE Proceedings of SPIE LA English DT Proceedings Paper CT Annual Conference on Algorithms and Technologies for Multispectral, Hyperspectral, and Ultraspectral Imagery XVIII CY APR 23-27, 2012 CL Baltimore, MD SP SPIE DE Image processing; classification; feature extraction AB To facilitate locating archaeological sites before they are compromised or destroyed, we are developing approaches for generating maps of probable archaeological sites, through detecting subtle anomalies in vegetative cover, soil chemistry, and soil moisture by analyzing remotely sensed data from multiple sources. We previously reported some success in this effort with a statistical analysis of slope, radar, and Ikonos data (including tasseled cap and NDVI transforms) with Student's t-test. We report here on new developments in our work, performing an analysis of 8-band multispectral Worldview-2 data. The Worldview-2 analysis begins by computing medians and median absolute deviations for the pixels in various annuli around each site of interest on the 28 band difference ratios. We then use principle components analysis followed by linear discriminant analysis to train a classifier which assigns a posterior probability that a location is an archaeological site. We tested the procedure using leave-one-out cross validation with a second leave-one-out step to choose parameters on a 9,859x23,000 subset of the WorldView-2 data over the western portion of Ft. Irwin, CA, USA. We used 100 known non-sites and trained one classifier for lithic sites (n=33) and one classifier for habitation sites (n=16). We then analyzed convex combinations of scores from the Archaeological Predictive Model (APM) and our scores. We found that that the combined scores had a higher area under the ROC curve than either individual method, indicating that including WorldView-2 data in analysis improved the predictive power of the provided APM. C1 [Tilton, James C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tilton, JC (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 606-3, Greenbelt, MD 20771 USA. EM James.C.Tilton@nasa.gov RI Priebe, Carey E./A-3305-2010 NR 9 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-9068-1 J9 PROC SPIE PY 2012 VL 8390 AR 83901K DI 10.1117/12.918366 PG 11 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA BBD51 UT WOS:000306561700049 ER PT S AU Greer, F Lee, MC Nikzad, S Traub, W Beasley, M AF Greer, Frank Lee, Michael C. Nikzad, Shouleh Traub, Wesley Beasley, Matthew BE Elam, JW Londergan, A VanDerStraten, O Roozeboom, F DeGendt, S Bent, SF Delabie, A TI Enabling High Performance Mirrors for Astronomy with ALD SO ATOMIC LAYER DEPOSITION APPLICATIONS 8 SE ECS Transactions LA English DT Proceedings Paper CT Symposium on Atomic Layer Deposition Applications 8 held during the PRiME Joint Int Meeting of the Electrochemical-Soc and the Electrochemical-Soc-of-Japan CY OCT 07-12, 2012 CL Honolulu, HI SP Electrochem Soc, Electrochem Soc Japan, Japan Soc Appl Phys, Korean Electrochem Soc, Royal Australian Chem Inst, Electrochemistry Div, Chinese Soc Electrochemistry, Dielectr Sci & Technol Div, Elect & Photon Div AB The technology of Atomic Layer Deposition holds promise to enable new classes of instruments and space missions a future flagship mission that can address both ultraviolet (UV) astrophysics and optical exoplanet science with a shared telescope. The technology path to a shared telescope requires the development of a mirror coating with high reflectance from 100 nm to 1000 nm, and low polarization effects (i.e., s-p phase shifts that can vary with angle of incidence across a primary and secondary mirror) in the optical range. Currently, UV coatings have low reflectance, and optical coatings have poor polarization properties for high-contrast coronagraph applications. In this paper we to take a first step toward solving both problems simultaneously by using ALD, taking advantage of the fact that ALD can potentially produce mirror coatings with denser layers than conventional coatings (hence better reflectance and durability), and ALD can potentially produce coatings with new composite materials (hence better control of polarization). We report here the results of our initial experiments with mirror coatings using ALD. C1 [Greer, Frank; Lee, Michael C.; Nikzad, Shouleh; Traub, Wesley] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Beasley, Matthew] Univ Colorado, Boulder, CO 80303 USA. RP Greer, F (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration FX y The authors would like to thank Professor Steven George for helpful discussions regarding MgF2 ALD chemistry. 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 3 TC 0 Z9 0 U1 0 U2 1 PU ELECTROCHEMICAL SOC INC PI PENNINGTON PA 65 S MAIN ST, PENNINGTON, NJ 08534-2839 USA SN 1938-5862 BN 978-1-62332-012-6 J9 ECS TRANSACTIONS PY 2012 VL 50 IS 13 BP 141 EP 148 DI 10.1149/05013.0141ecst PG 8 WC Electrochemistry; Materials Science, Multidisciplinary SC Electrochemistry; Materials Science GA BA8EE UT WOS:000338022100015 ER PT S AU Nelson, E AF Nelson, Emily BE Dahlquist, E TI Alternative fuels and green aviation SO BIOMASS AS ENERGY SOURCE: RESOURCES, SYSTEMS AND APPLICATIONS SE Sustainable Energy Developments LA English DT Article; Book Chapter ID TEMPERATURE-DEPENDENT VISCOSITY; ALGAL OIL PRODUCTION; COLD-FLOW PROPERTIES; FATTY-ACID METHYL; BIODIESEL FUELS; DIESEL FUEL; JET FUEL; BIOFUELS PRODUCTION; MICROALGAL BIOMASS; THERMOPHYSICAL PROPERTIES C1 NASA, Bio Sci & Technol Branch, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Nelson, E (reprint author), NASA, Bio Sci & Technol Branch, Glenn Res Ctr, Cleveland, OH 44135 USA. EM emily.s.nelson@nasa.gov NR 189 TC 0 Z9 0 U1 1 U2 1 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA SN 2164-0645 BN 978-0-203-12025-5; 978-0-415-62087-1 J9 SUSTAIN ENERG DEV PY 2012 VL 3 BP 177 EP 228 PG 52 WC Biotechnology & Applied Microbiology; Energy & Fuels SC Biotechnology & Applied Microbiology; Energy & Fuels GA BC2LZ UT WOS:000351074900014 ER PT B AU Landis, GA AF Landis, G. A. BE VanSark, WGJHM Sayigh, A TI Solar Power Satellites SO COMPREHENSIVE RENEWABLE ENERGY, VOL 1: PHOTOVOLTAIC SOLAR ENERGY LA English DT Article; Book Chapter C1 NASA, Glenn Res Ctr, Cleveland, OH USA. RP Landis, GA (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. NR 19 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS BN 978-0-08-087873-7; 978-0-08-087872-0 PY 2012 BP 767 EP 774 DI 10.1016/B978-0-08-087872-0.00137-2 PG 8 WC Electrochemistry; Energy & Fuels SC Electrochemistry; Energy & Fuels GA BA3HQ UT WOS:000334268400037 ER PT J AU Burke, K AF Burke, K. BE Sayigh, A TI Current Perspective on Hydrogen and Fuel Cells SO COMPREHENSIVE RENEWABLE ENERGY, VOL 4: FUEL CELLS AND HYDROGEN TECHNOLOGY LA English DT Article; Book Chapter C1 NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Burke, K (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA. NR 48 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS BN 978-0-08-087873-7 PY 2012 BP 29 EP 63 DI 10.1016/B978-0-08-087872-0.00402-9 PG 35 WC Electrochemistry; Energy & Fuels SC Electrochemistry; Energy & Fuels GA BA3KV UT WOS:000334336700002 ER PT J AU Mertens, CJ Kress, BT Wiltberger, M Tobiska, WK Grajewski, B Xu, XJ AF Mertens, Christopher J. Kress, Brian T. Wiltberger, Michael Tobiska, W. Kent Grajewski, Barbara Xu, Xiaojing BE Nenoi, M TI Atmospheric Ionizing Radiation from Galactic and Solar Cosmic Rays SO CURRENT TOPICS IN IONIZING RADIATION RESEARCH LA English DT Article; Book Chapter ID DOSE CONVERSION COEFFICIENTS; ENERGETIC PARTICLE EVENT; FEMALE FLIGHT ATTENDANTS; CANCER INCIDENCE; COMMERCIAL AVIATION; AIRCRAFT ALTITUDES; GEOMAGNETIC CUTOFF; SPACE EXPLORATION; PUBLISHED DATA; CREW-MEMBERS C1 [Mertens, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Kress, Brian T.] Dartmouth Coll, Hanover, NH 03755 USA. [Wiltberger, Michael] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Tobiska, W. Kent] Space Environm Technol, Pacific Palisades, CA USA. [Grajewski, Barbara] NIOSH, Cincinnati, OH 45226 USA. [Xu, Xiaojing] Sci Syst & Applicat Inc, Lanham, MD USA. RP Mertens, CJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. NR 128 TC 10 Z9 10 U1 1 U2 1 PU INTECH EUROPE PI RIJEKA PA JANEZA TRDINE9, RIJEKA, 51000, CROATIA BN 978-953-51-0196-3 PY 2012 BP 683 EP 738 D2 10.5772/2027 PG 56 WC Biochemistry & Molecular Biology; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Biochemistry & Molecular Biology; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA BG2EG UT WOS:000387290700032 ER PT S AU Sakamoto, T AF Sakamoto, Takanori BE Roming, PWA Kawai, N Pian, E TI GRB Prompt X-ray Emission SO DEATH OF MASSIVE STARS: SUPERNOVAE AND GAMMA-RAY BURSTS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 279th Symposium of the International Astronomical Union CY MAR 12-16, 2012 CL Nikko, JAPAN SP Int Astronom Union, Minist Educ Culture Sport Sci & Technol Japan, Japan Soc Promot Sci, Univ Tokyo, Inst Phys & Math Universe, Tokyo Tech, SW Res Inst, Global COE Program Quantum Phys & Nanoscience, Grant Aid Prior Res Area Decipher Ancient Universe Gamma Ray Bursts, Astronom Soc Japan DE gamma rays: bursts ID LUMINOSITY RELATION; PEAK LUMINOSITY; COMPLETE SAMPLE; BURSTS; SUPERNOVA; HETE-2; SPECTRA; MISSION; LONG; LAGS AB I present the observational properties of the prompt emission of supernova associated GRBs (SN-GRBs) focusing on temporal and spectral characteristics. I compare the properties of SN-GRBs with typical long GRBs to see whether there is a distinct difference or not. Furthermore, I present our attempt to search for hard X-ray emission prior to the discovery date from optically identified type Ibc supernovae using Swift BAT survey data. C1 [Sakamoto, Takanori] NASA, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sakamoto, Takanori] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Sakamoto, Takanori] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sakamoto, T (reprint author), NASA, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Taka.Sakamoto@nasa.gov NR 28 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-1-107-01979-9 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2012 VL 279 BP 40 EP 45 DI 10.1017/S1743921312012665 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BG9KJ UT WOS:000393362200007 ER PT S AU Burrows, DN Park, S Helder, EA Dewey, D McCray, R Zhekov, SA Racusin, JL Dwek, E AF Burrows, David N. Park, Sangwook Helder, Eveline A. Dewey, Daniel McCray, Richard Zhekov, Svetozar A. Racusin, Judith L. Dwek, Eli BE Roming, PWA Kawai, N Pian, E TI N1987A: the X-ray remnant at age 25 years SO DEATH OF MASSIVE STARS: SUPERNOVAE AND GAMMA-RAY BURSTS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 279th Symposium of the International Astronomical Union CY MAR 12-16, 2012 CL Nikko, JAPAN SP Int Astronom Union, Minist Educ Culture Sport Sci & Technol Japan, Japan Soc Promot Sci, Univ Tokyo, Inst Phys & Math Universe, Tokyo Tech, SW Res Inst, Global COE Program Quantum Phys & Nanoscience, Grant Aid Prior Res Area Decipher Ancient Universe Gamma Ray Bursts, Astronom Soc Japan DE X-rays:individual(SN1987A); stars:supernovae:individual(SN1987A) ID SNR 1987A; SUPERNOVA 1987A; EVOLUTION AB SN1987A is the best-studied core-collapse supernova in the sky. We know what the progenitor was, what the circumstellar environment was, and what the explosion looked like over a broad electromagnetic bandpass and in neutrinos. For over a decade, the Chandra X-ray Observatory has been monitoring SN1987A on a regular basis, obtaining resolved images of the developing interaction with the circumstellar material, as well as high resolution grating spectroscopy of the X-ray emission. We highlight the latest results from this campaign and discuss the overall picture of the remnant's structure that emerges from these observations. C1 [Burrows, David N.; Helder, Eveline A.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Park, Sangwook] Univ Texas Arlington, Arlington, TX 76019 USA. [Dewey, Daniel] MIT, Kavli Inst, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [McCray, Richard] Univ Colorado, Boulder, CO 80309 USA. [Zhekov, Svetozar A.] Space Res & Technol Inst, Sofia, Bulgaria. [Racusin, Judith L.; Dwek, Eli] NASA, GSFC, Greenbelt, MD USA. RP Burrows, DN (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM burrows@astro.psu.edu NR 16 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-1-107-01979-9 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2012 VL 279 BP 71 EP 74 DI 10.1017/S1743921312012719 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BG9KJ UT WOS:000393362200012 ER PT S AU Thone, CC Postigo, AD Fryer, C Page, K Gorosabel, J Perley, D Aloy, M Kouveliotou, C AF Thone, C. C. de Ugarte Postigo, A. Fryer, C. Page, K. Gorosabel, J. Perley, D. Aloy, M. Kouveliotou, C. CA Christmas Burst Collaboration BE Roming, PWA Kawai, N Pian, E TI GRB 101225A-a new class of GRBs? SO DEATH OF MASSIVE STARS: SUPERNOVAE AND GAMMA-RAY BURSTS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 279th Symposium of the International Astronomical Union CY MAR 12-16, 2012 CL Nikko, JAPAN SP Int Astronom Union, Minist Educ Culture Sport Sci & Technol Japan, Japan Soc Promot Sci, Univ Tokyo, Inst Phys & Math Universe, Tokyo Tech, SW Res Inst, Global COE Program Quantum Phys & Nanoscience, Grant Aid Prior Res Area Decipher Ancient Universe Gamma Ray Bursts, Astronom Soc Japan DE gamma rays: bursts; supernovae: individual ID GAMMA-RAY BURST; SUPERNOVA; REDSHIFT AB The Christmas burst, GRB 101225A, was one of the most controversial bursts in the last few years. Its exceptionally long duration but bright X-ray emission showing a thermal component followed by a strange afterglow with a thermal SED lead to two different interpretations. We present here our model ascribing this strange event to a new type of GRB progenitor consisting of a neutron star and an evolved main-sequence star in a very faint galaxy at red shift 0.33 while Campana et al. (2011) proposed a Galactic origin. New observations at several wavelengths might resolve the question between the two models in the near future. C1 [Thone, C. C.; de Ugarte Postigo, A.; Gorosabel, J.] CSIC, IAA, Glorieta Astron S-N, E-18008 Granada, Spain. [de Ugarte Postigo, A.] Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Fryer, C.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Page, K.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Perley, D.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Aloy, M.] Univ Valencia, Dept Astron & Astrofis, E-46100 Burjassot, Spain. [Kouveliotou, C.] NASA, Sci & Technol Off, MSFC, Huntsville, AL 35812 USA. RP Thone, CC (reprint author), CSIC, IAA, Glorieta Astron S-N, E-18008 Granada, Spain. EM cthoene@iaa.es OI de Ugarte Postigo, Antonio/0000-0001-7717-5085; Thone, Christina/0000-0002-7978-7648 FU "Estallidos" of the Spanish MEC [AYA2010-21887-004-01]; FEDER; IAU to attend this conference FX CCT acknowledges support from "Estallidos" under program number AYA2010-21887-004-01 of the Spanish MEC and by FEDER and generous support from the IAU to attend this conference. NR 16 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-1-107-01979-9 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2012 VL 279 BP 91 EP 94 DI 10.1017/S1743921312012744 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BG9KJ UT WOS:000393362200015 ER PT S AU Lien, A Sakamoto, T Gehrels, N Palmer, D Graziani, C AF Lien, Amy Sakamoto, Takanori Gehrels, Neil Palmer, David Graziani, Carlo BE Roming, PWA Kawai, N Pian, E TI Trigger Simulations for GRB Detection with the Swift Burst Alert Telescope SO DEATH OF MASSIVE STARS: SUPERNOVAE AND GAMMA-RAY BURSTS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 279th Symposium of the International Astronomical Union CY MAR 12-16, 2012 CL Nikko, JAPAN SP Int Astronom Union, Minist Educ Culture Sport Sci & Technol Japan, Japan Soc Promot Sci, Univ Tokyo, Inst Phys & Math Universe, Tokyo Tech, SW Res Inst, Global COE Program Quantum Phys & Nanoscience, Grant Aid Prior Res Area Decipher Ancient Universe Gamma Ray Bursts, Astronom Soc Japan DE Gamma-ray Bursts ID GAMMA-RAY BURSTS AB Understanding the intrinsic cosmic long gamma-ray burst (GRB) rate is essential in many aspects of astrophysics and cosmology, such as revealing the connection between GRBs, supernovae (SNe), and stellar evolution. Swift, a multi-wavelength space telescope, is quickly expanding the GRB category by observing hundreds of GRBs and their redshifts. However, it remains difficult to determine the intrinsic GRB rate due to the complex trigger algorithm adopted by Swift. Current studies of the GRB rate usually approximate the Swift trigger algorithm by a single detection threshold. Nevertheless, unlike the previously flown GRB instruments, Swift has over 500 trigger criteria based on count rates and additional thresholds for localization. To investigate possible systematic biases and further explore the intrinsic GRB rate as a function of redshift and the GRB luminosity function, we adopt a Monte Carlo approach by simulating all trigger criteria used by Swift. A precise estimation of the intrinsic GRB rate is important to reveal the GRB origins and their relation to the black-hole forming SNe. Additionally, the GRB rate at high redshifts provides a strong probe of the star formation history in the early universe, which is hard to measure directly through other methods. C1 [Lien, Amy; Sakamoto, Takanori; Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Palmer, David] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Graziani, Carlo] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Lien, Amy] ORAU, Oak Ridge, TN USA. [Sakamoto, Takanori] UMBC, CRESST, Baltimore, MD USA. RP Lien, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM amy.y.lien@nasa.gov; takanori@milkyway.gsfc.nasa.gov; neil.gehrels@nasa.gov; palmer@lanl.gov; carlo@oddjob.uchicago.edu NR 6 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-1-107-01979-9 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2012 VL 279 BP 347 EP 348 DI 10.1017/S1743921312013282 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BG9KJ UT WOS:000393362200068 ER PT S AU Nishikawa, KI Zhang, B Choi, EJ Min, KW Niemiec, J Medvedev, M Hardee, P Mizuno, Y Nordlund, A Frederiksen, J Sol, H Pohl, M Hartmann, DH Fishman, GJ AF Nishikawa, K. -I. Zhang, B. Choi, E. J. Min, K. W. Niemiec, J. Medvedev, M. Hardee, P. Mizuno, Y. Nordlund, A. Frederiksen, J. Sol, H. Pohl, M. Hartmann, D. H. Fishman, G. J. BE Roming, PWA Kawai, N Pian, E TI Radiation from accelerated particles in shocks SO DEATH OF MASSIVE STARS: SUPERNOVAE AND GAMMA-RAY BURSTS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 279th Symposium of the International Astronomical Union CY MAR 12-16, 2012 CL Nikko, JAPAN SP Int Astronom Union, Minist Educ Culture Sport Sci & Technol Japan, Japan Soc Promot Sci, Univ Tokyo, Inst Phys & Math Universe, Tokyo Tech, SW Res Inst, Global COE Program Quantum Phys & Nanoscience, Grant Aid Prior Res Area Decipher Ancient Universe Gamma Ray Bursts, Astronom Soc Japan DE Relativistic jets; Weibel instability; magnetic field generation; particle acceleration; radiation ID EMISSION AB Recent PIC simulations of relativistic electron-positron (electron-ion) jets injected into a stationary medium show that particle acceleration occurs in the shocked regions. Simulations show that the Weibel instability is responsible for generating and amplifying highly nonuniform, small-scale magnetic fields and for particle acceleration. These magnetic fields contribute to the electron's transverse deflection behind the shock. The "jitter" radiation from deflected electrons in turbulent magnetic fields has properties different from synchrotron radiation calculated in a uniform magnetic field. This jitter radiation may be important for understanding the complex time evolution and/or spectral structure of gamma-ray bursts, relativistic jets in general, and supernova remnants. In order to calculate radiation from first principles and go beyond the standard synchrotron model, we have used PIC simulations. We present synthetic spectra to compare with the spectra obtained from Fermi observations. C1 [Nishikawa, K. -I.] Univ Alabama, Ctr Space Plasma & Aeron Res, 320 Sparkman Dr, Huntsville, AL 35805 USA. [Zhang, B.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. [Choi, E. J.; Min, K. W.] Korea Adv Inst Sci & Technol, Daejeon 305701, South Korea. [Niemiec, J.] PAN, Inst Nucl Phys, PL-31342 Krakow, Poland. [Medvedev, M.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Hardee, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Mizuno, Y.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Nordlund, A.; Frederiksen, J.] Niels Bohr Inst, DK-2100 Kbenhavn, Denmark. [Sol, H.] Observ Paris, LUTH, F-92195 Meudon, France. [Pohl, M.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Hartmann, D. H.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Fishman, G. J.] NASA, MSFC, Huntsville, AL 35805 USA. RP Nishikawa, KI (reprint author), Univ Alabama, Ctr Space Plasma & Aeron Res, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM ken-ichi.nishikawa-1@nasa.gov OI Mizuno, Yosuke/0000-0002-8131-6730 FU MNiSW [N N203 393034]; Foundation for Polish Science through the HOMING program; EEA Financial Mechanism; NSF; Danish Natural Science Research Council; National Science Foundation [PHY05-51164]; [NSF-AST-0506719]; [AST-0506666]; [AST-0908040]; [AST-0908010]; [NASA-NNG05GK73G]; [NNX07AJ88G]; [NNX08AG83G]; [NNX08AL39G]; [NNX09AD 16G] FX This work is supported by NSF-AST-0506719, AST-0506666, AST-0908040, AST-0908010, NASA-NNG05GK73G, NNX07AJ88G, NNX08AG83G, NNX08AL39G, and NNX09AD 16G. JN was supported by MNiSW research project N N203 393034, and The Foundation for Polish Science through the HOMING program, which is supported through the EEA Financial Mechanism. Simulations were performed at the Columbia facility at the NASA Advanced Supercomputing (NAS), and on the IBM p690 (Copper) at the National Center for Supercomputing Applications (NCSA) which is supported by the NSF. Part of this work was done while K.-I. N. was visiting the Niels Bohr Institute. Support from the Danish Natural Science Research Council is gratefully acknowledged. This report was finalized during the program "Particle Acceleration in Astrophysical Plasmas" at the Kavli Institute for Theoretical Physics which is supported by the National Science Foundation under Grant No. PHY05-51164. NR 4 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-1-107-01979-9 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2012 VL 279 BP 371 EP 372 DI 10.1017/S1743921312013403 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BG9KJ UT WOS:000393362200080 ER PT S AU Stockdale, CJ Ryder, SD Horesh, A Weiler, KW Panagia, N Van Dyk, SD Bauer, FE Immler, S Sramek, RA Pooley, D Marcaide, JM Kassim, N AF Stockdale, Christopher J. Ryder, S. D. Horesh, A. Weiler, K. W. Panagia, N. Van Dyk, S. D. Bauer, F. E. Immler, S. Sramek, R. A. Pooley, D. Marcaide, J. M. Kassim, N. BE Roming, PWA Kawai, N Pian, E TI Radio Insight into the Nature of Type IIb Progenitors SO DEATH OF MASSIVE STARS: SUPERNOVAE AND GAMMA-RAY BURSTS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 279th Symposium of the International Astronomical Union CY MAR 12-16, 2012 CL Nikko, JAPAN SP Int Astronom Union, Minist Educ Culture Sport Sci & Technol Japan, Japan Soc Promot Sci, Univ Tokyo, Inst Phys & Math Universe, Tokyo Tech, SW Res Inst, Global COE Program Quantum Phys & Nanoscience, Grant Aid Prior Res Area Decipher Ancient Universe Gamma Ray Bursts, Astronom Soc Japan AB We present the results of over two decades of radio observations of type IIb Supernovae with the Very Large Array and the Australia Telescope Compact Array. These radio studies illustrate the need for multi-wavelength follow-up to determine the progenitor scenario for type lib events. C1 [Stockdale, Christopher J.] Marquette Univ, Dept Phys, POB 1811, Milwaukee, WI 53201 USA. [Ryder, S. D.] Australian Astron Observ, Epping, NSW 1710, Australia. [Horesh, A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Weiler, K. W.] Computat Phys Inc, Springfield, VA 22151 USA. [Panagia, N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Van Dyk, S. D.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Immler, S.] NASA, Ctr Res & Explorat Space Sci & Technol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sramek, R. A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Pooley, D.] Sam Houston State Univ, Dept Phys, Huntsville, TX 77341 USA. [Marcaide, J. M.] Univ Valencia, Dept Astron, E-46100 Burjassot, Spain. [Kassim, N.] Naval Res Lab, Washington, DC 20375 USA. RP Stockdale, CJ (reprint author), Marquette Univ, Dept Phys, POB 1811, Milwaukee, WI 53201 USA. EM chris.stockdale@mu.edu OI Horesh, Assaf/0000-0002-5936-1156; Ryder, Stuart/0000-0003-4501-8100; Van Dyk, Schuyler/0000-0001-9038-9950 NR 18 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-1-107-01979-9 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2012 VL 279 BP 393 EP 394 DI 10.1017/S1743921312013506 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BG9KJ UT WOS:000393362200090 ER PT J AU Buzulukova, N Fok, MC Glocer, A AF Buzulukova, Natalia Fok, Mei-Ching Glocer, Alex BE Lazar, M TI Impact of Solar Wind on the Earth Magnetosphere: Recent Progress in the Modeling of Ring Current and Radiation Belts SO EXPLORING THE SOLAR WIND LA English DT Article; Book Chapter ID PITCH-ANGLE DIFFUSION; INNER MAGNETOSPHERE; RELATIVISTIC ELECTRONS; RESONANT INTERACTION; GEOMAGNETIC STORMS; SPACE WEATHER; KINETIC-MODEL; CONVECTION; SUBSTORM; FIELD C1 [Buzulukova, Natalia; Fok, Mei-Ching; Glocer, Alex] NASA, Goddard Space Flight Ctr, Washington, DC USA. [Buzulukova, Natalia] CRESST, Washington, DC USA. [Buzulukova, Natalia] Univ Maryland, College Pk, MD 20742 USA. RP Buzulukova, N (reprint author), NASA, Goddard Space Flight Ctr, Washington, DC USA. NR 97 TC 1 Z9 1 U1 1 U2 1 PU INTECH EUROPE PI RIJEKA PA JANEZA TRDINE9, RIJEKA, 51000, CROATIA BN 978-953-51-0339-4 PY 2012 BP 317 EP 336 D2 10.5772/2079 PG 20 WC Astronomy & Astrophysics; Physics, Fluids & Plasmas SC Astronomy & Astrophysics; Physics GA BC9KW UT WOS:000356532100015 ER PT B AU Mehta, RD Bell, JH Reda, DC Wilder, MC Zilliac, GG Driver, DM AF Mehta, R. D. Bell, J. H. Reda, D. C. Wilder, M. C. Zilliac, G. G. Driver, D. M. BE Smits, AJ Lim, TT TI PRESSURE AND SHEAR SENSITIVE COATINGS SO FLOW VISUALIZATION: TECHNIQUES AND EXAMPLES, 2ND EDITION LA English DT Article; Book Chapter ID THERMOCHROMIC LIQUID-CRYSTALS; PAINT; DISTRIBUTIONS; CALIBRATION; TRANSITION C1 [Mehta, R. D.; Bell, J. H.; Reda, D. C.; Wilder, M. C.; Zilliac, G. G.; Driver, D. M.] NASA, Expt Aerophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Mehta, RD (reprint author), NASA, Expt Aerophys Branch, Ames Res Ctr, Mail Stop 260-1, Moffett Field, CA 94035 USA. NR 29 TC 0 Z9 0 U1 0 U2 0 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 978-1-84816-792-6; 978-1-84816-791-9 PY 2012 BP 191 EP 225 D2 10.1142/p808 PG 35 WC Physics, Applied; Physics, Fluids & Plasmas SC Physics GA BA7HC UT WOS:000337526500009 ER PT J AU Roden, EE McBeth, JM Blothe, M Percak-Dennett, EM Fleming, EJ Holyoke, RR Luther, GW Emerson, D Schieber, J AF Roden, Eric E. McBeth, Joyce M. Bloethe, Marco Percak-Dennett, Elizabeth M. Fleming, Emily J. Holyoke, Rebecca R. Luther, George W., III Emerson, David Schieber, Juergen TI The microbial ferrous wheel in a neutral pH groundwater seep SO FRONTIERS IN MICROBIOLOGY LA English DT Article DE neutral pH; microbial; iron; cycling; microscale; 16S rRNA gene; barcode sequencing AB Evidence for microbial Fe redox cycling was documented in a circumneutral pH ground-water seep near Bloomington, Indiana. Geochemical and microbiological analyses were conducted at two sites, a semi-consolidated microbial mat and a floating puffball structure. In situ voltammetric microelectrode measurements revealed steep opposing gradients of O-2 and Fe(II) at both sites, similar to other groundwater seep and sedimentary environments known to support microbial Fe redox cycling. The puffball structure showed an abrupt increase in dissolved Fe(II) just at its surface (similar to 5 cm depth), suggesting an internal Fe(II) source coupled to active Fe(III) reduction. Most probable number enumerations detected microaerophilic Fe(II)-oxidizing bacteria (FeOB) and dissimilatory Fe(III)-reducing bacteria (FeRB) at densities of 10(2) to 10(5) cells mL(-1) in samples from both sites. In vitro Fe(III) reduction experiments revealed the potential for immediate reduction (no lag period) of native Fe(III) oxides. Conventional full-length 16S rRNA gene clone libraries were compared with high throughput barcode sequencing of the V1, V4, or V6 variable regions of 16S rRNA genes in order to evaluate the extent to which new sequencing approaches could provide enhanced insight into the composition of Fe redox cycling microbial community structure. The composition of the clone libraries suggested a lithotroph-dominated microbial community centered around taxa related to known FeOB (e.g., Gallionella, Sideroxydans, Aquabacterium). Sequences related to recognized FeRB (e.g., Rhodoferax, Aeromonas, Geobacter, Desulfovibrio) were also well-represented. Overall, sequences related to known FeOB and FeRB accounted for 88 and 59% of total clone sequences in the mat and puffball libraries, respectively. Taxa identified in the barcode libraries showed partial overlap with the clone libraries, but were not always consistent across different variable regions and sequencing platforms. However, the barcode libraries provided confirmation of key clone library results (e.g., the predominance of Betaproteobacteria) and an expanded view of lithotrophic microbial community composition. C1 [Roden, Eric E.; Bloethe, Marco; Percak-Dennett, Elizabeth M.] Univ Wisconsin, Dept Geosci, NASA, Astrobiol Inst, Madison, WI 53706 USA. [McBeth, Joyce M.; Fleming, Emily J.; Emerson, David] Bigelow Lab Ocean Sci, East Boothbay, ME USA. [Holyoke, Rebecca R.; Luther, George W., III] Univ Delaware, Coll Earth Ocean & Environm, Lewes, DE 19958 USA. [Bloethe, Marco] Geozentrum Hannover, Fed Inst Geosci & Nat Resources, Hannover, Germany. [Schieber, Juergen] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. RP Roden, EE (reprint author), Univ Wisconsin, Dept Geosci, 1215W Dayton St, Madison, WI 53706 USA. EM eroden@geology.wisc.edu RI Luther, III, George/A-6384-2008 OI Luther, III, George/0000-0002-0780-885X FU NASA Astrobiology Institute (University of California, Berkeley and University of Wisconsin Madison nodes); U.S. Department of Energy, Office of Biological and Environmental Research, Subsurface Biogeochemical Research Program through the SBR Scientific Focus Area at the Pacific Northwest National Laboratory; Office of Naval Research [N00014-08-1-0334]; National Science Foundation [IOS-0951077] FX We are indebted to Mitch Sogin and colleagues at MBL, and Noah Fierer and colleagues at the University of Colorado Boulder, for facilitating the barcode sequencing of our 16S rRNA gene samples. This work was supported by the NASA Astrobiology Institute (University of California, Berkeley and University of Wisconsin Madison nodes), and the U.S. Department of Energy, Office of Biological and Environmental Research, Subsurface Biogeochemical Research Program through the SBR Scientific Focus Area at the Pacific Northwest National Laboratory. Work in the Emerson laboratory at Bigelow was also supported by grants from the Office of Naval Research N00014-08-1-0334 and the National Science Foundation IOS-0951077. NR 100 TC 26 Z9 28 U1 5 U2 60 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1664-302X J9 FRONT MICROBIOL JI Front. Microbiol. PY 2012 VL 3 AR 172 DI 10.3389/fmicb.2012.00172 PG 18 WC Microbiology SC Microbiology GA V31DF UT WOS:000208863600222 PM 22783228 ER PT J AU Van Kranendonk, MJ Altermann, W Beard, BL Hoffman, PF Johnson, CM Kasting, JF Melezhik, VA Nutman, AP Papineau, D Pirajno, F AF Van Kranendonk, M. J. Altermann, Wladyslaw Beard, Brian L. Hoffman, Paul F. Johnson, Clark M. Kasting, James F. Melezhik, Victor A. Nutman, Allen P. Papineau, Dominic Pirajno, Franco BE Gradstein, FM Ogg, JG Schmitz, MD Ogg, GM TI A Chronostratigraphic Division of the Precambrian SO GEOLOGIC TIME SCALE 2012, VOLS 1 & 2 LA English DT Article; Book Chapter ID U-PB ZIRCON; SOUTHERN WEST GREENLAND; BANDED IRON-FORMATIONS; BILLION YEARS AGO; GREAT OXIDATION EVENT; ISUA SUPRACRUSTAL BELT; NEOPROTEROZOIC SNOWBALL EARTH; PROTEROZOIC OCEAN CHEMISTRY; MULTIPLE SULFUR ISOTOPES; LARGE IGNEOUS PROVINCE AB This chapter provides a review of events through Precambrian Earth history, with the aim of providing an up-to-date foundation on which to construct a chronostratigraphic revision of the Precambrian time scale. The guiding principles used to develop a revised Precambrian time scale follow Cloud's vision to "...seek trend-related events that have affected the entire Earth over relatively short intervals of time and left recognizable signatures in the rock sequences of the globe.", and apply Gould's historical principles of directionality and contingency. Analysis of the Precambrian geological record reveals a series of linked, causative events over time that can be used as a basis for a more naturalistic time scale that better reflects our knowledge of events in the history of our planet and can be used as a template for further research. A revised Precambrian time scale envisages three eons: 1) A Hadean Eon, which extends from the time of formation of the solar system (T-0 = 4567 Ma), to the age of Earth's oldest rock (4030 Ma Acasta Gneiss); 2) An Archean Eon, extending from the top of the Hadean Eon to the time of the fundamental transition from an early, hotter, reducing Earth to a more modern, cooler, oxidized Earth, at c. 2420 Ma; 3) A Proterozoic Eon, from the c. 2420 Ma Archean-Proterozoic boundary to the base of the Phanerozoic Eon (542 Ma). Each of the eons may be subdivided into a number of eras and periods that can each be marked by a chronostratigraphic Global Stratotype Section and Point (GSSP), excepting lower most chronometric divisions of the Hadean Eon and Paleoarchean Era. Suggestions are presented for the age, name, and GSSP locality of each division. [GRAPHICS] . C1 [Van Kranendonk, M. J.] Univ New S Wales, Sch Biol Earth & Environm Sci, Randwick, NSW 2052, Australia. [Altermann, Wladyslaw] Univ Pretoria, Dept Geol, ZA-0002 Pretoria, South Africa. [Beard, Brian L.] NASA, Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA. [Johnson, Clark M.] Univ Wisconsin Madison, Dept Geosci, Madison, WI 53706 USA. [Kasting, James F.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Melezhik, Victor A.] Geol Survey Norway, N-7491 Trondheim, Norway. [Nutman, Allen P.] Univ Wollongong, Sch Earth & Environm Sci, Wollongong, NSW 2522, Australia. [Papineau, Dominic] Boston Coll, Dept Earth & Environm Sci, Chestnut Hill, MA 02467 USA. [Pirajno, Franco] Geol Survey Western Australia, Perth, WA 6004, Australia. RP Van Kranendonk, MJ (reprint author), Univ New S Wales, Sch Biol Earth & Environm Sci, Randwick, NSW 2052, Australia. EM martin.vankranendonk@unsw.edu.au; wlady.altermann@up.ac.za; beardb@geology.wisc.edu; paulfhoffman@gmail.com; clarkj@geology.wisc.edu; kasting@essc.psu.edu; victor.melezhik@ngu.no; allen.nutman@gmail.com; dominic.papineau@bc.edu; franco.pirajno@dmp.wa.gov.au NR 966 TC 17 Z9 17 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS BN 978-0-44-459425-9 PY 2012 BP 299 EP 392 DI 10.1016/B978-0-444-59425-9.00016-0 PG 94 WC Geology SC Geology GA BE2BX UT WOS:000368986200017 ER PT B AU Fraichard, T Howard, TM AF Fraichard, Thierry Howard, Thomas M. BE Eskandarian, A TI Iterative Motion Planning and Safety Issue SO HANDBOOK OF INTELLIGENT VEHICLES, VOLS 1 AND 2 LA English DT Article; Book Chapter ID TRAJECTORY GENERATION; COLLISION-AVOIDANCE; MOVING OBSTACLES; MOBILE ROBOTS; NAVIGATION; ENVIRONMENTS; VEHICLE; TERRAIN; PATHS; VISION AB This chapter addresses safe mobile robot navigation in complex environments. The challenges in this class of navigation problems include nontrivial vehicle dynamics and terrain interaction, static and dynamic environments, and incomplete information. This complexity prompted the design of hierarchical solutions featuring a multilevel strategy where strategic behaviors are planned at a global scale and tactical or safety decisions are made at a local scale. While the task of the high level is generally to compute the sequence of waypoints or waystates to reach the goal, the local planner computes the actual trajectory that will be executed by the system. Due to computational resource limitations, finite sensing horizon, and temporal constraints of mobile robots, the local trajectory is only partially computed to provide a motion that makes progress toward the goal state. This chapter focuses on safely and efficiently computing the local trajectory in the context of mobile robot navigation. This chapter is divided into three sections: motion safety, iterative motion planning, and applications. Motion safety discusses the issues related to determining if a trajectory is safely traversable by a mobile robot. Iterative motion planning reviews developments in local motion planning search space design with a focus on potential field, sampling, and graph search techniques. The applications section surveys experiments and applications in autonomous mobile robot navigation in outdoor and urban environments. C1 [Fraichard, Thierry] CNRS LIG, INRIA Grenoble Rhone Alpes, Grenoble, France. [Fraichard, Thierry] Grenoble Univ, Grenoble, France. [Howard, Thomas M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Fraichard, T (reprint author), CNRS LIG, INRIA Grenoble Rhone Alpes, Grenoble, France. NR 88 TC 3 Z9 3 U1 0 U2 0 PU SPRINGER-VERLAG LONDON LTD PI GODALMING PA SWEETAPPLE HOUSE CATTESHALL RD FARNCOMBE, GODALMING GU7 1NH, SURREY, ENGLAND BN 978-0-85729-085-4; 978-0-85729-084-7 PY 2012 BP 1433 EP 1458 DI 10.1007/978-0-85729-085-4_55 D2 10.1007/978-0-85729-085-4 PG 26 WC Automation & Control Systems; Computer Science, Interdisciplinary Applications; Transportation Science & Technology SC Automation & Control Systems; Computer Science; Transportation GA BC0PD UT WOS:000349295700056 ER PT S AU Kalar, D Green, C AF Kalar, Donald Green, Collin GP Assoc Comp Machinery TI Understanding Situational Awareness in Multi-Unit Supervisory Control Through Data-Mining and Modeling with Real-Time Strategy Games SO HRI'12: PROCEEDINGS OF THE SEVENTH ANNUAL ACM/IEEE INTERNATIONAL CONFERENCE ON HUMAN-ROBOT INTERACTION SE ACMIEEE International Conference on Human-Robot Interaction LA English DT Proceedings Paper CT 7th ACM/IEEE International Conference on Human-Robot Interaction (HRI) CY MAR 05-08, 2012 CL Boston, MA SP Assoc Comp Machinery, IEEE, ACM SIGCHI, ACM SIGART, HFES, AAAI, IEEE Robot & Automat DE multi-agent HRI; Real-time strategy; meta-analysis AB As robots become increasingly capable and autonomous, the role of a human operator may be to supervise multiple robots and intervene to handle problems and provide strategic guidance. In such cases, the extent to which HRI tools support the human supervisor's situational awareness (SA) and ability to intervene in an appropriate and timely fashion will constrain the scale of operations (e.g., the number of robots; the complexity of tasks) that can reasonably be supervised by a single person. One approach to understanding how humans might acquire, maintain, and use situational awareness in multi-robot supervision tasks is to look at video games that require similar activities. We describe our initial efforts at analyzing and modeling data from Real-Time Strategy (RTS) games with the goal of answering basic questions about the nature of situational awareness and supervisory control of multiple semi-autonomous agents. C1 [Kalar, Donald] San Jose State Univ, Dept Psychol, San Jose, CA 95192 USA. [Green, Collin] NASA Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA USA. RP Kalar, D (reprint author), San Jose State Univ, Dept Psychol, San Jose, CA 95192 USA. EM donald.kalar@sjsu.edu; collin.b.green@nasa.gov NR 2 TC 0 Z9 0 U1 0 U2 0 PU ASSOC COMPUTING MACHINERY PI NEW YORK PA 1515 BROADWAY, NEW YORK, NY 10036-9998 USA SN 2167-2121 BN 978-1-4503-1063-5 J9 ACMIEEE INT CONF HUM PY 2012 BP 163 EP 164 PG 2 WC Engineering, Electrical & Electronic; Robotics SC Engineering; Robotics GA BG9JL UT WOS:000393315300043 ER PT B AU Middleton, EM Huemmrich, KF Cheng, YB Margolis, HA AF Middleton, Elizabeth M. Huemmrich, K. Fred Cheng, Yen-Ben Margolis, Hank A. BE Thenkabail, PS Lyon, JG Huete, A TI Spectral Bioindicators of Photosynthetic Efficiency and Vegetation Stress SO HYPERSPECTRAL REMOTE SENSING OF VEGETATION LA English DT Article; Book Chapter ID LIGHT-USE EFFICIENCY; PHOTOCHEMICAL REFLECTANCE INDEX; NET PRIMARY PRODUCTION; RADIATION-USE-EFFICIENCY; SPACEBORNE IMAGING SPECTROSCOPY; MODELING CANOPY PHOTOSYNTHESIS; THERMAL-ENERGY DISSIPATION; CARBON-DIOXIDE UPTAKE; LEAF-AREA INDEX; XANTHOPHYLL CYCLE C1 [Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Huemmrich, K. Fred] Univ Maryland Baltimore Cty, College Pk, MD USA. [Huemmrich, K. Fred] Joint Ctr Earth Syst Technol, Baltimore, MD USA. [Cheng, Yen-Ben] Earth Resources Technol Inc, Laurel, MD USA. [Margolis, Hank A.] Univ Laval, Fac Foresterie, Ctr Etud Foret Geog & Geomat, Laval, PQ, Canada. RP Middleton, EM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 148 TC 14 Z9 14 U1 1 U2 1 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-4538-7; 978-1-4398-4537-0 PY 2012 BP 265 EP 288 PG 24 WC Agronomy; Remote Sensing SC Agriculture; Remote Sensing GA BC7PO UT WOS:000355136500014 ER PT B AU Witt, G Hottman, SB AF Witt, Glen Hottman, Stephen B. BE Barnhart, RK Hottman, SB Marshall, DM Shappee, E TI Certificate of Authorization Process SO INTRODUCTION TO UNMANNED AIRCRAFT SYSTEMS LA English DT Article; Book Chapter C1 [Witt, Glen] New Mexico State Univ, Airspace Operat Tech Anal & Applicat Ctr, Las Cruces, NM 88003 USA. [Witt, Glen] US Air Force, Washington, DC USA. [Witt, Glen] Lakenheath Radar Air Traff Control Ctr, Lakenheath AFB, England. [Witt, Glen] Albuquerque ARTCC, FAA, Albuquerque, NM USA. [Witt, Glen] FAA, Washington, DC USA. [Witt, Glen] Fac Airspace & Procedures Off, Paris, France. [Witt, Glen] DESA, Belgrade, Serbia. [Witt, Glen] NASA, Environm Res Aircraft & Sensor Technol ERAST Prog, Washington, DC USA. [Hottman, Stephen B.] UAS, TAAC, New Delhi, India. [Hottman, Stephen B.] New Mexico State Univ, Phys Sci Lab, Res & Dev, Las Cruces, NM 88003 USA. [Hottman, Stephen B.] New Mexico State Univ, Phys Sci Lab, Las Cruces, NM 88003 USA. [Hottman, Stephen B.] NMSU, Las Cruces, NM USA. [Hottman, Stephen B.] DoD, Pentagon, AR USA. NR 20 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-3521-0; 978-1-4398-3520-3 PY 2012 BP 51 EP 68 PG 18 WC Transportation SC Transportation GA BC8SE UT WOS:000356056600005 ER PT B AU Srivastava, AN Han, JW AF Srivastava, Ashok N. Han, Jiawei BE Srivastava, AN Han, J TI Machine Learning and Knowledge Discovery for Engineering Systems Health Management SO MACHINE LEARNING AND KNOWLEDGE DISCOVERY FOR ENGINEERING SYSTEMS HEALTH MANAGEMENT SE Chapman & Hall-CRC Data Mining and Knowledge Discovery Series LA English DT Editorial Material; Book Chapter C1 [Srivastava, Ashok N.] NASA, System Wide Safety & Assurance Technol Project, Washington, DC 20546 USA. [Srivastava, Ashok N.] NASA, Integrated Vehicle Hlth Management Res Project, Washington, DC 20546 USA. [Srivastava, Ashok N.] NASA Ames Res Ctr, Intelligent Data Understanding Grp, Moffett Field, CA USA. [Han, Jiawei] Univ Illinois, Comp Sci, Chicago, IL 60680 USA. RP Srivastava, AN (reprint author), NASA, System Wide Safety & Assurance Technol Project, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-4179-2; 978-1-4398-4178-5 J9 CH CRC DATA MIN KNOW PY 2012 BP XXIII EP XXXI PG 9 WC Computer Science, Information Systems; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA BF6FO UT WOS:000383031900001 ER PT B AU Oza, N Das, S AF Oza, Nikunj Das, Santanu BE Srivastava, AN Han, J TI Anomaly Detection in a Fleet of Systems SO MACHINE LEARNING AND KNOWLEDGE DISCOVERY FOR ENGINEERING SYSTEMS HEALTH MANAGEMENT SE Chapman & Hall-CRC Data Mining and Knowledge Discovery Series LA English DT Article; Book Chapter ID NOVELTY DETECTION; DATA SETS; ALGORITHMS; CLASSIFICATION; MATRIX C1 [Oza, Nikunj; Das, Santanu] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. RP Oza, N (reprint author), NASA Ames Res Ctr, Moffett Field, CA 94035 USA. NR 42 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-4179-2; 978-1-4398-4178-5 J9 CH CRC DATA MIN KNOW PY 2012 BP 67 EP 113 PG 47 WC Computer Science, Information Systems; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA BF6FO UT WOS:000383031900004 ER PT B AU Goebel, K Saxena, A Saha, S Saha, B Celaya, J AF Goebel, Kai Saxena, Abhinav Saha, Sankalita Saha, Bhaskar Celaya, Jose BE Srivastava, AN Han, J TI Prognostic Performance Metrics SO MACHINE LEARNING AND KNOWLEDGE DISCOVERY FOR ENGINEERING SYSTEMS HEALTH MANAGEMENT SE Chapman & Hall-CRC Data Mining and Knowledge Discovery Series LA English DT Article; Book Chapter C1 [Goebel, Kai] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Saxena, Abhinav; Celaya, Jose] SGT Inc, Moffett Field, CA USA. [Saha, Sankalita; Saha, Bhaskar] MCT Inc, Moffett Field, CA USA. RP Goebel, K (reprint author), NASA Ames Res Ctr, Moffett Field, CA 94035 USA. NR 41 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-4179-2; 978-1-4398-4178-5 J9 CH CRC DATA MIN KNOW PY 2012 BP 147 EP 177 PG 31 WC Computer Science, Information Systems; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA BF6FO UT WOS:000383031900006 ER PT B AU Smelyanskiy, VN Luchinsky, DG Hafiychuk, VV Osipov, VV Kulikov, I Patterson-Hine, A AF Smelyanskiy, Vadim N. Luchinsky, Dmitry G. Hafiychuk, Vasyl V. Osipov, Viatcheslav V. Kulikov, Igor Patterson-Hine, Ann BE Srivastava, AN Han, J TI Physics-Based Methods of Failure Analysis and Diagnostics in Human Space Flight SO MACHINE LEARNING AND KNOWLEDGE DISCOVERY FOR ENGINEERING SYSTEMS HEALTH MANAGEMENT SE Chapman & Hall-CRC Data Mining and Knowledge Discovery Series LA English DT Article; Book Chapter ID CHAOTIC DYNAMICAL-SYSTEMS; TIME-SERIES; NONLINEAR DYNAMICS; MODELS; NOISE; LIKELIHOOD; COHERENCE; INFERENCE; DESIGN C1 [Smelyanskiy, Vadim N.; Patterson-Hine, Ann] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Luchinsky, Dmitry G.; Osipov, Viatcheslav V.] Mission Crit Technol Inc, NASA Ames Res Ctr, Moffett Field, CA USA. [Hafiychuk, Vasyl V.] SGT Inc, NASA Ames Res Ctr, Moffett Field, CA USA. [Kulikov, Igor] CALTECH, Pasadena, CA 91125 USA. RP Smelyanskiy, VN (reprint author), NASA Ames Res Ctr, Moffett Field, CA 94035 USA. NR 46 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-4179-2; 978-1-4398-4178-5 J9 CH CRC DATA MIN KNOW PY 2012 BP 245 EP 284 PG 40 WC Computer Science, Information Systems; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA BF6FO UT WOS:000383031900009 ER PT B AU Orchard, M Vachtsevanos, G Goebel, K AF Orchard, Marcos Vachtsevanos, George Goebel, Kai BE Srivastava, AN Han, J TI A Combined Model-Based and Data-Driven Prognostic Approach for Aircraft System Life Management SO MACHINE LEARNING AND KNOWLEDGE DISCOVERY FOR ENGINEERING SYSTEMS HEALTH MANAGEMENT SE Chapman & Hall-CRC Data Mining and Knowledge Discovery Series LA English DT Article; Book Chapter ID FAILURE PROGNOSIS C1 [Orchard, Marcos] Univ Chile, Santiago, Chile. [Vachtsevanos, George] Georgia Inst Technol, Atlanta, GA 30332 USA. [Goebel, Kai] NASA Ames Res Ctr, Moffett Field, CA USA. RP Orchard, M (reprint author), Univ Chile, Santiago, Chile. NR 24 TC 1 Z9 1 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-4179-2; 978-1-4398-4178-5 J9 CH CRC DATA MIN KNOW PY 2012 BP 363 EP 394 PG 32 WC Computer Science, Information Systems; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA BF6FO UT WOS:000383031900012 ER PT S AU McClain, C Meister, G AF McClain, Charles Meister, Gerhard BE McClain, C Meister, G TI Mission Requirements for Future Ocean-Colour Sensors Introduction SO MISSION REQUIREMENTS FOR FUTURE OCEAN-COLOUR SENSORS SE IOCCG Report LA English DT Editorial Material; Book Chapter ID RESOLUTION IMAGING SPECTRORADIOMETER; WATER-LEAVING RADIANCE; ORBIT SPECTRAL CHARACTERIZATION; REFLECTANCE-BASED CALIBRATION; AEROSOL OPTICAL-THICKNESS; ATMOSPHERIC CORRECTION; DIFFUSE-REFLECTANCE; SURFACE-ROUGHNESS; RADIOMETRIC CALIBRATION; VICARIOUS CALIBRATION C1 [McClain, Charles; Meister, Gerhard] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP McClain, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 124 TC 0 Z9 0 U1 0 U2 0 PU INT OCEAN COLOUR COORDINATING GROUP-IOCCG PI DARTMOUTH PA IOCCG PROJECT OFF, BEDFORD INST OCEANOGRAPHY, B240, PO BOX 1006, DARTMOUTH, NOVA SCOTIA B2Y 4A2, CANADA SN 1098-6030 BN 978-1-896246-64-2 J9 IOCCG REP PY 2012 IS 13 BP 1 EP + PG 10 WC Oceanography; Remote Sensing SC Oceanography; Remote Sensing GA BC5LN UT WOS:000353359500001 ER PT S AU McClain, C Meister, G AF McClain, Charles Meister, Gerhard BE McClain, C Meister, G TI Science Questions and Applications SO MISSION REQUIREMENTS FOR FUTURE OCEAN-COLOUR SENSORS SE IOCCG Report LA English DT Article; Book Chapter C1 [McClain, Charles; Meister, Gerhard] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP McClain, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU INT OCEAN COLOUR COORDINATING GROUP-IOCCG PI DARTMOUTH PA IOCCG PROJECT OFF, BEDFORD INST OCEANOGRAPHY, B240, PO BOX 1006, DARTMOUTH, NOVA SCOTIA B2Y 4A2, CANADA SN 1098-6030 BN 978-1-896246-64-2 J9 IOCCG REP PY 2012 IS 13 BP 5 EP 16 PG 12 WC Oceanography; Remote Sensing SC Oceanography; Remote Sensing GA BC5LN UT WOS:000353359500002 ER PT S AU McClain, C Meister, G AF McClain, Charles Meister, Gerhard BE McClain, C Meister, G TI Approaches and Data Product Requirements SO MISSION REQUIREMENTS FOR FUTURE OCEAN-COLOUR SENSORS SE IOCCG Report LA English DT Article; Book Chapter C1 [McClain, Charles; Meister, Gerhard] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP McClain, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU INT OCEAN COLOUR COORDINATING GROUP-IOCCG PI DARTMOUTH PA IOCCG PROJECT OFF, BEDFORD INST OCEANOGRAPHY, B240, PO BOX 1006, DARTMOUTH, NOVA SCOTIA B2Y 4A2, CANADA SN 1098-6030 BN 978-1-896246-64-2 J9 IOCCG REP PY 2012 IS 13 BP 17 EP 30 PG 14 WC Oceanography; Remote Sensing SC Oceanography; Remote Sensing GA BC5LN UT WOS:000353359500003 ER PT S AU McClain, C Meister, G AF McClain, Charles Meister, Gerhard BE McClain, C Meister, G TI Space Measurement and Mission Requirements SO MISSION REQUIREMENTS FOR FUTURE OCEAN-COLOUR SENSORS SE IOCCG Report LA English DT Article; Book Chapter C1 [McClain, Charles; Meister, Gerhard] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP McClain, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU INT OCEAN COLOUR COORDINATING GROUP-IOCCG PI DARTMOUTH PA IOCCG PROJECT OFF, BEDFORD INST OCEANOGRAPHY, B240, PO BOX 1006, DARTMOUTH, NOVA SCOTIA B2Y 4A2, CANADA SN 1098-6030 BN 978-1-896246-64-2 J9 IOCCG REP PY 2012 IS 13 BP 31 EP 78 PG 48 WC Oceanography; Remote Sensing SC Oceanography; Remote Sensing GA BC5LN UT WOS:000353359500004 ER PT S AU McClain, C Meister, G AF McClain, Charles Meister, Gerhard BE McClain, C Meister, G TI International Cooperation SO MISSION REQUIREMENTS FOR FUTURE OCEAN-COLOUR SENSORS SE IOCCG Report LA English DT Article; Book Chapter C1 [McClain, Charles; Meister, Gerhard] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP McClain, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU INT OCEAN COLOUR COORDINATING GROUP-IOCCG PI DARTMOUTH PA IOCCG PROJECT OFF, BEDFORD INST OCEANOGRAPHY, B240, PO BOX 1006, DARTMOUTH, NOVA SCOTIA B2Y 4A2, CANADA SN 1098-6030 BN 978-1-896246-64-2 J9 IOCCG REP PY 2012 IS 13 BP 79 EP 88 PG 10 WC Oceanography; Remote Sensing SC Oceanography; Remote Sensing GA BC5LN UT WOS:000353359500005 ER PT S AU McClain, C Meister, G AF McClain, Charles Meister, Gerhard BE McClain, C Meister, G TI Mission Requirements for Future Ocean-Colour Sensors Conclusions SO MISSION REQUIREMENTS FOR FUTURE OCEAN-COLOUR SENSORS SE IOCCG Report LA English DT Editorial Material; Book Chapter C1 [McClain, Charles; Meister, Gerhard] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP McClain, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU INT OCEAN COLOUR COORDINATING GROUP-IOCCG PI DARTMOUTH PA IOCCG PROJECT OFF, BEDFORD INST OCEANOGRAPHY, B240, PO BOX 1006, DARTMOUTH, NOVA SCOTIA B2Y 4A2, CANADA SN 1098-6030 BN 978-1-896246-64-2 J9 IOCCG REP PY 2012 IS 13 BP 89 EP 90 PG 2 WC Oceanography; Remote Sensing SC Oceanography; Remote Sensing GA BC5LN UT WOS:000353359500006 ER PT S AU McClain, C Meister, G AF McClain, Charles Meister, Gerhard BE McClain, C Meister, G TI Tabular Summaries of Previous, Current, and Future Ocean Colour Missions SO MISSION REQUIREMENTS FOR FUTURE OCEAN-COLOUR SENSORS SE IOCCG Report LA English DT Article; Book Chapter C1 [McClain, Charles; Meister, Gerhard] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP McClain, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU INT OCEAN COLOUR COORDINATING GROUP-IOCCG PI DARTMOUTH PA IOCCG PROJECT OFF, BEDFORD INST OCEANOGRAPHY, B240, PO BOX 1006, DARTMOUTH, NOVA SCOTIA B2Y 4A2, CANADA SN 1098-6030 BN 978-1-896246-64-2 J9 IOCCG REP PY 2012 IS 13 BP 91 EP 96 PG 6 WC Oceanography; Remote Sensing SC Oceanography; Remote Sensing GA BC5LN UT WOS:000353359500007 ER PT J AU Rankin-Gee, EK Lera, M Lingappa, U Bebout, B Marcu, O AF Rankin-Gee, E. K. Lera, M. Lingappa, U. Bebout, B. Marcu, O. TI Molecular and biochemical responses of Volvox carteri to oxidative stress SO MOLECULAR BIOLOGY OF THE CELL LA English DT Meeting Abstract C1 [Rankin-Gee, E. K.] Univ Calif Los Angeles, Los Angeles, CA USA. [Rankin-Gee, E. K.; Lera, M.; Lingappa, U.; Bebout, B.; Marcu, O.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rankin-Gee, E. K.; Lingappa, U.; Marcu, O.] SETI Inst, Carl Sagan Ctr, Mountain View, CA USA. [Lera, M.] Lockheed Martin, Moffett Field, CA USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER SOC CELL BIOLOGY PI BETHESDA PA 8120 WOODMONT AVE, STE 750, BETHESDA, MD 20814-2755 USA SN 1059-1524 EI 1939-4586 J9 MOL BIOL CELL JI Mol. Biol. Cell PY 2012 VL 23 MA 794 PG 1 WC Cell Biology SC Cell Biology GA V38MX UT WOS:000209348602426 ER PT B AU Grecu, M Olson, WS Shie, CL AF Grecu, Mircea Olson, William S. Shie, Chung-Lin BE Chang, NB Hong, Y TI Instantaneous Precipitation and Latent Heating Estimation over Land from Combined Spaceborne Radar and Microwave Radiometer Observations SO MULTISCALE HYDROLOGIC REMOTE SENSING: PERSPECTIVES AND APPLICATIONS LA English DT Article; Book Chapter ID PROFILING ALGORITHM; TRMM; RETRIEVAL; SATELLITE; SENSORS C1 [Grecu, Mircea] Morgan State Univ, Goddard Earth Sci Technol & Res Studies & Invest, Baltimore, MD 21239 USA. [Grecu, Mircea; Olson, William S.; Shie, Chung-Lin] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Olson, William S.; Shie, Chung-Lin] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP Grecu, M (reprint author), Morgan State Univ, Goddard Earth Sci Technol & Res Studies & Invest, Baltimore, MD 21239 USA. NR 23 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-7763-0; 978-1-4398-7745-6 PY 2012 BP 387 EP 398 D2 10.1201/b11279 PG 12 WC Remote Sensing; Water Resources SC Remote Sensing; Water Resources GA BC8ER UT WOS:000355569800017 ER PT J AU Nilsson, RH Tedersoo, L Abarenkov, K Ryberg, M Kristiansson, E Hartmann, M Schoch, CL Nylander, JAA Bergsten, J Porter, TM Jumpponen, A Vaishampayan, P Ovaskainen, O Hallenberg, N Bengtsson-Palme, J Eriksson, KM Larsson, KH Larsson, E Koljalg, U AF Nilsson, R. Henrik Tedersoo, Leho Abarenkov, Kessy Ryberg, Martin Kristiansson, Erik Hartmann, Martin Schoch, Conrad L. Nylander, Johan A. A. Bergsten, Johannes Porter, Teresita M. Jumpponen, Ari Vaishampayan, Parag Ovaskainen, Otso Hallenberg, Nils Bengtsson-Palme, Johan Eriksson, K. Martin Larsson, Karl-Henrik Larsson, Ellen Koljalg, Urmas TI Five simple guidelines for establishing basic authenticity and reliability of newly generated fungal ITS sequences SO MYCOKEYS LA English DT Article DE ITS; sequence reliability; sequence quality control; fungi; databases; barcoding AB Molecular data form an important research tool in most branches of mycology. A non-trivial proportion of the public fungal DNA sequences are, however, compromised in terms of quality and reliability, contributing noise and bias to sequence-borne inferences such as phylogenetic analysis, diversity assessment, and barcoding. In this paper we discuss various aspects and pitfalls of sequence quality assessment. Based on our observations, we provide a set of guidelines to assist in manual quality management of newly generated, near-full-length (Sanger-derived) fungal ITS sequences and to some extent also sequences of shorter read lengths, other genes or markers, and groups of organisms. The guidelines are intentionally non-technical and do not require substantial bioinformatics skills or significant computational power. Despite their simple nature, we feel they would have caught the vast majority of the severely compromised ITS sequences in the public corpus. Our guidelines are nevertheless not infallible, and common sense and intuition remain important elements in the pursuit of compromised sequence data. The guidelines focus on basic sequence authenticity and reliability of the newly generated sequences, and the user may want to consider additional resources and steps to accomplish the best possible quality control. A discussion on the technical resources for further sequence quality management is therefore provided in the supplementary material. C1 [Nilsson, R. Henrik; Hallenberg, Nils; Eriksson, K. Martin; Larsson, Ellen] Univ Gothenburg, Dept Biol & Environm Sci, S-40530 Gothenburg, Sweden. [Tedersoo, Leho; Abarenkov, Kessy; Koljalg, Urmas] Univ Tartu, Inst Ecol & Earth Sci, EE-50090 Tartu, Estonia. [Tedersoo, Leho; Koljalg, Urmas] Univ Tartu, Nat Hist Museum, EE-50090 Tartu, Estonia. [Ryberg, Martin] Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN 37996 USA. [Kristiansson, Erik] Chalmers, Dept Math Stat, S-41296 Gothenburg, Sweden. [Hartmann, Martin] Mol Ecol Agroscope Reckenholz Tanikon Res Stn ART, Zurich, Switzerland. [Hartmann, Martin] Swiss Fed Res Inst WSL, Forest Soils & Biogeochem, Birmensdorf, Switzerland. [Schoch, Conrad L.] Natl Lib Med, Natl Ctr Biotechnol Informat, NIH, Bethesda, MD 20892 USA. [Nylander, Johan A. A.] Swedish Museum Nat Hist, Dept Biodivers Informat, S-10405 Stockholm, Sweden. [Bergsten, Johannes] Swedish Museum Nat Hist, Dept Entomol, S-10405 Stockholm, Sweden. [Porter, Teresita M.] McMaster Univ, Dept Biol, Hamilton, ON L8S 4K1, Canada. [Jumpponen, Ari] Kansas State Univ, Div Biol, Manhattan, KS 66506 USA. [Vaishampayan, Parag] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA USA. [Ovaskainen, Otso] Univ Helsinki, Dept Biosci, FI-00014 Helsinki, Finland. [Bengtsson-Palme, Johan] Univ Gothenburg, Sahlgrenska Acad, Dept Neurosci & Physiol, S-40530 Gothenburg, Sweden. [Larsson, Karl-Henrik] Univ Oslo, Nat Hist Museum, Dept Res & Collect, N-0318 Oslo, Norway. RP Nilsson, RH (reprint author), Univ Gothenburg, Dept Biol & Environm Sci, Box 461, S-40530 Gothenburg, Sweden. EM henrik.nilsson@bioenv.gu.se RI Ovaskainen, Otso/D-9119-2012; Hartmann, Martin/M-9371-2016; Eriksson, Karl/D-7811-2015 OI Ovaskainen, Otso/0000-0001-9750-4421; Hartmann, Martin/0000-0001-8069-5284; Eriksson, Karl/0000-0001-7437-7175 FU Swedish Research Council of Environment, Agricultural Sciences, and Spatial Planning (FORMAS) [215-2011-498]; ETF [8235, 9286]; FIBIR; Life Science Area of Advance at Chalmers University of Technology; Swedish Research Council (VR); FORMAS; Intramural Research Program of the NIH, National Library of Medicine; Government of Canada through Genome Canada; Ontario Genomics Institute [OGI-050]; Department of Energy's Biological and Environmental Research Program [ER65000]; Gothenburg Bioinformatics Network FX RHN acknowledges financial support from Swedish Research Council of Environment, Agricultural Sciences, and Spatial Planning (FORMAS, 215-2011-498). LT and UK received financial support from ETF grants 8235, 9286, and FIBIR. EK acknowledges support from the Life Science Area of Advance at Chalmers University of Technology, the Swedish Research Council (VR), and FORMAS. CLS was supported in part by the Intramural Research Program of the NIH, National Library of Medicine. TMP acknowledges financial support from the Government of Canada through Genome Canada and the Ontario Genomics Institute through the Biomonitoring 2.0 project (OGI-050). AJ acknowledges financial support from Department of Energy's Biological and Environmental Research Program (Award #ER65000). Yann Bertrand and Chris Quince are acknowledged for valuable input on the manuscript. Support from the Gothenburg Bioinformatics Network is gratefully acknowledged. NR 53 TC 36 Z9 38 U1 2 U2 10 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1314-4057 EI 1314-4049 J9 MYCOKEYS JI MycoKeys PY 2012 IS 4 BP 37 EP 63 DI 10.3897/mycokeys.4.3606 PG 27 WC Mycology SC Mycology GA V39TU UT WOS:000209434100004 ER PT B AU Wilson, WC Atkinson, GM AF Wilson, W. C. Atkinson, G. M. BE Laudon, M Romanowicz, B TI Temperature and Strain Response of a Surface Acoustic Wave Sensor SO NANOTECHNOLOGY 2012, VOL 2: ELECTRONICS, DEVICES, FABRICATION, MEMS, FLUIDICS AND COMPUTATIONAL LA English DT Proceedings Paper CT NSTI Nanotechnology Conference and Expo (Nanotech 2012) CY JUN 18-21, 2012 CL Santa Clara, CA SP ACCT Canada, Anaheim Ctr New Energy Technol, Angel Capital Assoc, Antenna Syst Magazine, Appl Mat, Arsenal Venture Partners, Austin Energy, AUTM, BASF, Battery Power Magazine, Carbon Credit Capital, CHInano2011, Clean Technol & Sustainable Ind, Org CTSI, Circuits Multi Projets, Constellat Energy, Eco Business com, EcoSeed, European Patent Off, Fraunhofer TechBridge, GigaOM, Green Blog Network, Greenberg Traurig, Hitachi High Technol Am Inc, Inst Civil Engineers, Insight InterAsia, IOP Publish, Jackson Walker LLP, Japan Technol Grp, Kauffman Fdn, Lam Res Corp, Licens Execut Soc, Lux Res, Mead Westvaco, MEMS Ind Grp, Nano Sci & Technol Inst, nano tech Japan, Natl Grid, Natl Venture Capital Assoc, Nanotechnol Ind Assoc, NE Utilities, PPG Ind, SciTech Patent Art, Shell GameChanger, SK Innovat, So California Edison, Taylor & Francis Grp LLC - CRC Press, TechConnect, Texas Nanotechnol Initiat, Env Business Cluster, Natl Assoc Seed & Venture, Funds NASVF, Zyvex Technol DE Multifunctional; sensor; Surface Acoustic Wave; SAW; strain; temperature; Langasite AB A multifunctional temperature and strain sensor is being investigated. The sensor has been fabricated on a Langasite substrate and uses Surface Acoustic Wave (SAW) technology. The SAW sensor responds to a single physical change by changing both the frequency and the phase. However, when two physical parameters change, such as temperature and strain, the effects are combined making it difficult to separate out a single measurement. A common solution to this issue is to measure temperature using a second sensor. While devices such as these have been developed, none provide temperature and strain from a single device. We have identified regions where only a thermal response is present in the phase data for SAW devices on Langasite. The measurement of temperature alone allows us to compensate the strain measurements and achieve temperature and strain from a single device. C1 [Wilson, W. C.] NASA, Langley Res Ctr, Hampton, VA 23666 USA. [Atkinson, G. M.] Virginia Commonwealth Univ, Richmond, VA USA. RP Wilson, WC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23666 USA. EM w.c.wilson@larc.nasa.gov; gmatkins@vcu.edu NR 13 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4665-6275-2 PY 2012 BP 211 EP 214 PG 4 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Physics, Applied SC Engineering; Science & Technology - Other Topics; Physics GA BG7DY UT WOS:000391249200056 ER PT S AU Kuiper, TBH Majid, WA Martinez, S Garcia-Miro, C Rizzo, JR AF Kuiper, T. B. H. Majid, W. A. Martinez, S. Garcia-Miro, C. Rizzo, J. R. BE Peck, AB Seaman, RL Comeron, F TI Remote Observing with NASA's Deep Space Network SO OBSERVATORY OPERATIONS: STRATEGIES, PROCESSES, AND SYSTEMS IV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Observatory Operations - Strategies, Processes and Systems IV CY JUL 04-06, 2012 CL Amsterdam, NETHERLANDS SP SPIE DE Deep Space Network; radio astronomy; remote observing; monitor and control; ssh tunnels AB The Deep Space Network (DSN) communicates with spacecraft as far away as the boundary between the Solar System and the interstellar medium. To make this possible, large sensitive antennas at Canberra, Australia, Goldstone, California, and Madrid, Spain, provide for constant communication with interplanetary missions. We describe the procedures for radioastronomical observations using this network. Remote access to science monitor and control computers by authorized observers is provided by two-factor authentication through a gateway at the Jet Propulsion Laboratory (JPL) in Pasadena. To make such observations practical, we have devised schemes based on SSH tunnels and distributed computing. At the very minimum, one can use SSH tunnels and VNC (Virtual Network Computing, a remote desktop software suite) to control the science hosts within the DSN Flight Operations network. In this way we have controlled up to three telescopes simultaneously. However, X-window updates can be slow and there are issues involving incompatible screen sizes and multi-screen displays. Consequently, we are now developing SSH tunnel-based schemes in which instrument control and monitoring, and intense data processing, are done on-site by the remote DSN hosts while data manipulation and graphical display are done at the observer's host. We describe our approaches to various challenges, our experience with what worked well and lessons learned, and directions for future development. C1 [Kuiper, T. B. H.; Majid, W. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Kuiper, TBH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM kuiper@jpl.nasa.gov RI Rizzo, J. Ricardo/N-5879-2014 OI Rizzo, J. Ricardo/0000-0002-8443-6631 FU Jet Propulsion Laboratory, California Institute of Technology; 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. NR 2 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-9149-7 J9 PROC SPIE PY 2012 VL 8448 AR 84480T DI 10.1117/12.925201 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BDA90 UT WOS:000312389300027 ER PT S AU Chao, TH Lu, TT Davis, SR Rommel, SD Farca, G Luey, B Martin, A Anderson, MH AF Chao, Tien-Hsin Lu, Thomas T. Davis, Scott R. Rommel, Scott D. Farca, George Luey, Ben Martin, Alan Anderson, Michael H. BE Casasent, DP Chao, TH TI Compact Liquid Crystal Waveguide Fourier Transform Spectrometer for Real-time Gas Sensing in NIR Spectral Band SO OPTICAL PATTERN RECOGNITION XXIII SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optical Pattern Recognition XXIII CY APR 26-27, 2012 CL Baltimore, MD SP SPIE DE Solid-state Fourier transform spectrometer; liquid crystal clad waveguide; monolithic spectrometer; near-IR spectrometer; electro-optic FTIR; gas sensing AB Jet Propulsion Lab and Vescent Photonics Inc. and are jointly developing an innovative ultra-compact (volume < 10 cm(3)), ultra-low power (<10(-3) Watt-hours per measurement and zero power consumption when not measuring), completely non-mechanical Liquid Crystal Waveguide Fourier Transform Spectrometer (LCWFTS) that will be suitable for a variety of remote-platform, in-situ measurements. These devices are made possible by novel electro-evanescent waveguide architecture, enabling "monolithic chip-scale" Electro Optic-FTS (EO-FTS) sensors. The potential performance of these EO-FTS sensors include: i) a spectral range throughout 0.4-5 mu m (25000 - 2000 cm(-1)), ii) high-resolution (Delta lambda <= 0.1 nm), iii) high-speed (< 1 ms) measurements, and iv) rugged integrated optical construction. This performance potential enables the detection and quantification of a large number of different atmospheric gases simultaneously in the same air mass and the rugged construction will enable deployment on previously inaccessible platforms. The sensor construction is also amenable for analyzing aqueous samples on remote floating or submerged platforms. We have reported [1] a proof-of-principle prototype LCWFTS sensor that has been demonstrated in the near-IR (range of 1450-1600 nm) with a 5 nm resolution. In this paper, we will report the recently built and tested LCWFTS test bed and the demonstration of a real-time gas sensing applications. C1 [Chao, Tien-Hsin; Lu, Thomas T.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Chao, TH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration; National Oceanic and Atmospheric Administration FX The research described in this paper was supported by contracts from both the National Aeronautics and Space Administration and the National Oceanic and Atmospheric Administration. NR 8 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-9076-6 J9 PROC SPIE PY 2012 VL 8398 AR UNSP 83980H DI 10.1117/12.923481 PG 13 WC Computer Science, Artificial Intelligence; Engineering, Electrical & Electronic; Optics SC Computer Science; Engineering; Optics GA BAJ45 UT WOS:000304343500015 ER PT J AU Watson, A Ahumada, A AF Watson, A. Ahumada, A. TI Contrast thresholds for letter identification as a function of size SO PERCEPTION LA English DT Meeting Abstract C1 [Watson, A.; Ahumada, A.] NASA, Ames Res Ctr, Washington, DC USA. EM andrew.b.watson@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU PION LTD PI LONDON PA 207 BRONDESBURY PARK, LONDON NW2 5JN, ENGLAND SN 0301-0066 EI 1468-4233 J9 PERCEPTION JI Perception PY 2012 VL 41 SU S BP 52 EP 52 PG 1 WC Ophthalmology; Psychology; Psychology, Experimental SC Ophthalmology; Psychology GA V31WA UT WOS:000208912500160 ER PT J AU Breed, M Venter, C Harding, AK Johnson, TJ AF Breed, M. Venter, C. Harding, A. K. Johnson, T. J. BE VanRensburg, JJ TI The Effect of Different Magnetospheric Structures on Predictions of Gamma-ray Pulsar Light Curves SO PROCEEDINGS OF SAIP2012: THE 57TH ANNUAL CONFERENCE OF THE SOUTH AFRICAN INSTITUTE OF PHYSICS LA English DT Proceedings Paper CT 57th Annual Conference of the South-African-Institute-of-Physics (SAIP) CY JUL 09-13, 2012 CL Univ Pretoria, Phys Dept, Pretoria, SOUTH AFRICA SP South African Inst Phys HO Univ Pretoria, Phys Dept ID LARGE-AREA TELESCOPE; OUTER MAGNETOSPHERE; RADIATION; POLARIZATION; MODELS; FIELD; GAPS AB The second pulsar catalogue of the Fermi Large Area Telescope (LAT) will contain in excess of 100 gamma-ray pulsars. The light curves (LCs) of these pulsars exhibit a variety of shapes, and also different relative phase lags with respect to their radio pulses, hinting at distinct underlying emission properties (e.g., inclination and observer angles) for the individual pulsars. Detailed geometric modelling of the radio and gamma-ray LCs may provide constraints on the B-field structure and emission geometry. We used different B-field solutions, including the static vacuum dipole and the retarded vacuum dipole, in conjunction with an existing geometric modelling code, and constructed radiation sky maps and LCs for several different pulsar parameters. Standard emission geometries were assumed, namely the two-pole caustic (TPC) and outer gap (OG) models. The sky maps and LCs of the various B-field and radiation model combinations were compared to study their effect on the resulting LCs. As an application, we compared our model LCs with Fermi LAT data for the Vela pulsar, and inferred the most probable configuration in this case, thereby constraining Vela's high-altitude magnetic structure and system geometry. C1 [Breed, M.; Venter, C.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Harding, A. K.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Johnson, T. J.] Naval Res Lab, High Energy Space Environm Branch, Washington, DC USA. RP Breed, M (reprint author), North West Univ, Ctr Space Res, Potchefstroom Campus,Private Bag X6001, ZA-2520 Potchefstroom, South Africa. EM 20574266@nwu.ac.za NR 19 TC 0 Z9 0 U1 0 U2 0 PU SOUTH AFRICAN INST PHYSICS PI LYNNWOOD RIDGE PA POSTNET STE 165, PRIVATE BAG X025, LYNNWOOD RIDGE, 0040, SOUTH AFRICA BN 978-1-77592-070-0 PY 2012 BP 316 EP 321 PG 6 WC Physics, Applied; Physics, Multidisciplinary SC Physics GA BE1GH UT WOS:000367878700055 ER PT J AU Seyffert, AS Venter, C Johnson, TJ Harding, AK AF Seyffert, A. S. Venter, C. Johnson, T. J. Harding, A. K. BE VanRensburg, JJ TI The anatomy of gamma-ray pulsar light curves SO PROCEEDINGS OF SAIP2012: THE 57TH ANNUAL CONFERENCE OF THE SOUTH AFRICAN INSTITUTE OF PHYSICS LA English DT Proceedings Paper CT 57th Annual Conference of the South-African-Institute-of-Physics (SAIP) CY JUL 09-13, 2012 CL Univ Pretoria, Phys Dept, Pretoria, SOUTH AFRICA SP South African Inst Phys HO Univ Pretoria, Phys Dept ID 2MASS REDSHIFT SURVEY; LARGE-AREA TELESCOPE; PERSEUS SUPERCLUSTER; MILKY-WAY; AVOIDANCE; GALAXIES; ZONE; EXTENSION; UNIVERSE; CATALOG AB To obtain constraints on the inclination angle (alpha, between the magnetic and rotation axes) and observer angle (zeta, line-of-sight relative to the rotation axis) of a gamma-ray pulsar from its observed light curve (LC), we make use of geometric models detailing the position and extent of emission regions (acceleration gaps) located in the magnetosphere. We do this by generating a sky map of the relative emission intensity for a range of a, and at each a extracting a set of LCs covering the entire range of zeta. This effectively yields an atlas of LCs characterised by a specific set of model parameters, such as pulsar period, gap width and position, and radial gap extent. This atlas can then be used to obtain fits to observed pulsar LCs (including rough errors on alpha and zeta) by eye through a systematic search of the possible (alpha,zeta) solution space. In the case of radio-loud gamma-ray pulsars, significantly better constraints on the viewing geometry (alpha and zeta values) can be obtained by doing this not only for the observed gamma-ray LC, but concurrently for the observed radio LC. This multiwavelength approach has been used successfully to obtain constraints on the viewing geometries of 6 LAT pulsars [1]. It is crucial, however, to understand how the set of model parameters which characterizes an LC atlas, influences the shapes and properties of the LCs contained in that atlas, since such an understanding enables improved parameter constraints, and directs future model refinement. A simple first approach is to vary these parameters and study the changes they bring about in the LCs. This approach proves useful in some respects (and is indeed adequate for understanding the LC atlases produced by the relatively simple radio models). However, due to the complex structure of many of the produced gamma-ray LCs (sometimes displaying up to 4 individual peaks), this approach doesn't give a comprehensive enough understanding of how all the LCs are produced in terms of the underlying magnetospheric structure and accelerator geometry. In this paper we explore a second approach to investigating the interplay between the model parameters and the LC atlas. In this approach we do not attempt to understand how the set of model parameters influences the LC shapes directly, but rather, more fundamentally, investigate how the set of model parameters affects the sky maps from which the latter are extracted. This allows us to also recognise structure within the atlas itself, as we are now able to attribute certain features of the LCs to specific features on the sky map, meaning that we not only understand how the structure of single LCs come about, but how their structure changes as we move through (alpha,zeta)-space, and why. C1 [Seyffert, A. S.; Venter, C.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Johnson, T. J.] Naval Res Lab, High Energy Space Environm Branch, Washington, DC USA. [Harding, A. K.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Seyffert, AS (reprint author), North West Univ, Ctr Space Res, Potchefstroom Campus,Private Bag X6001, ZA-2520 Potchefstroom, South Africa. EM 20126999@nwu.ac.za NR 33 TC 0 Z9 0 U1 0 U2 0 PU SOUTH AFRICAN INST PHYSICS PI LYNNWOOD RIDGE PA POSTNET STE 165, PRIVATE BAG X025, LYNNWOOD RIDGE, 0040, SOUTH AFRICA BN 978-1-77592-070-0 PY 2012 BP 373 EP 379 PG 7 WC Physics, Applied; Physics, Multidisciplinary SC Physics GA BE1GH UT WOS:000367878700065 ER PT B AU Tse, L Ganapathi, G Wirz, R Lavine, A AF Tse, Louis Ganapathi, Gani Wirz, Richard Lavine, Adrienne GP ASME TI SYSTEM MODELING FOR A SUPERCRITICAL THERMAL ENERGY STORAGE SYSTEM SO PROCEEDINGS OF THE ASME 6TH INTERNATIONAL CONFERENCE ON ENERGY SUSTAINABILITY - 2012, PTS A AND B LA English DT Proceedings Paper CT 6th ASME International Conference on Energy Sustainability CY JUL 23-26, 2012 CL San Diego, CA SP ASME, Adv Energy Syst Div, ASME, Solar Energy Div ID POWER-PLANTS; SOLAR; TIME AB This paper describes a thermodynamic model that simulates the discharge cycle of a single-tank thermal energy storage (TES) system using supercritical fluid in a concentrating solar power plant. Current state-of-the-art TES design utilizes a two-tank system with molten nitrate salts; one major problem is the high cost of the fluid. The alternate design explored here involves the use of less expensive fluids at supercritical temperatures and pressures. By cycling the storage fluid between a relatively low temperature two-phase state and a high temperature supercritical state, a large excursion in internal energy can be accessed which includes both sensible heat and latent heat of vaporization. Supercritical storage allows for the consideration of fluids that are significantly cheaper than molten salts; however, a supercritical TES system requires high pressures and temperatures that necessitate a relatively high cost containment vessel that represents a large fraction of the system capital cost. To mitigate this cost, the proposed design utilizes a single-tank TES system, effectively halving the required wall material. A single-tank approach also significantly reduces the complexity of the system in comparison to the two-tank systems, which require expensive pumps and external heat exchangers. However, a single-tank approach also results in a loss of turbine power output as the storage fluid temperature declines over time during the discharge cycle. The thermodynamic model is used to evaluate system performance; in particular it predicts the reduction in energy output of the single-tank system relative to a conventional two-tank storage system. Tank wall material volume is also presented and it is shown that there is an optimum average fluid density that generates a given turbine energy output while minimizing the required tank wall material and associated capital cost. Overall, this study illustrates opportunities to further improve current solar thermal technologies. The single-tank supercritical fluid system shows great promise for decreasing the cost of thermal energy storage, and ensuring that renewable energy can become a significant part of the national and global energy portfolio. C1 [Tse, Louis; Wirz, Richard; Lavine, Adrienne] Univ Calif Los Angeles, Mech & Aerosp Engn Dept, Los Angeles, CA 90095 USA. [Ganapathi, Gani] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Tse, L (reprint author), Univ Calif Los Angeles, Mech & Aerosp Engn Dept, Los Angeles, CA 90095 USA. FU Southern California Gas Company [DEAR0000140, 5660021607] FX This effort was supported by ARPA-E Award DEAR0000140 and Grant No. 5660021607 from the Southern California Gas Company. NR 17 TC 0 Z9 0 U1 0 U2 2 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4481-6 PY 2012 BP 689 EP + PG 2 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA BA4HE UT WOS:000335710300082 ER PT B AU Ganapathi, GB Wirz, R AF Ganapathi, Gani B. Wirz, Richard GP ASME TI HIGH DENSITY THERMAL ENERGY STORAGE WITH SUPERCRITICAL FLUIDS SO PROCEEDINGS OF THE ASME 6TH INTERNATIONAL CONFERENCE ON ENERGY SUSTAINABILITY - 2012, PTS A AND B LA English DT Proceedings Paper CT 6th ASME International Conference on Energy Sustainability CY JUL 23-26, 2012 CL San Diego, CA SP ASME, Adv Energy Syst Div, ASME, Solar Energy Div AB A novel approach to storing thermal energy with supercritical fluids is being investigated, which if successful, promises to transform the way thermal energy is captured and utilized. The use of supercritical fluids allows cost-affordable high-density storage with a combination of latent heat and sensible heat in the two-phase as well as the supercritical state. This technology will enhance penetration of several thermal power generation applications and high temperature water for commercial use if the overall cost of the technology can be demonstrated to be lower than the current state-of-the-art molten salt using sodium nitrate and potassium nitrate eutectic mixtures. An additional attraction is that the volumetric storage density of a supercritical fluid can be higher than a two-tank molten salt system due to the high compressibilities in the supercritical state. This paper looks at different elements for determining the feasibility of this storage concept - thermodynamics of supercritical state with a specific example, naphthalene, fluid and system cost and a representative storage design. A modular storage vessel design based on a shell and heat exchanger concept allows the cost to be minimized as there is no need for a separate pump for transferring fluid from one tank to another as in the molten salt system. Since the heat exchangers are internal to the tank, other advantages such as lower parasitic heat loss, easy fabrication can be achieved. Results from the study indicate that the fluid cost can be reduced by a factor of ten or even twenty depending on the fluid and thermodynamic optimization of loading factor. Results for naphthalene operating between 290 degrees C and 475 degrees C, indicate that the fluid cost is approximately $3/kWh compared with $25-$50/kWh for molten salt. When the storage container costs are factored in, the overall system cost is still very attractive. Studies for a 12-hr storage indicate that for operating at temperatures between 290-450 degrees C, the cost for a molten salt system can vary between $66/kWh to $184/kWh depending on molten salt cost of $2/kg or a more recent quote of $8/kg. In contrast, the cost for a 12-hr supercritical storage system can be as low as $40/kWh. By using less expensive materials than SS 316L, it is possible to reduce the costs even further. C1 [Ganapathi, Gani B.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Wirz, Richard] Univ Calif Los Angeles, Los Angeles, CA USA. RP Ganapathi, GB (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. FU Southern California Gas Company [DE-AR0000140, 5660021607] FX Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract. with the National Aeronautics and Space Administration. This effort was supported by ARPA-E Award DE-AR0000140 and Grant No. 5660021607 from the Southern California Gas Company. The authors also want to thank their team members for helping out on this project. NR 5 TC 0 Z9 0 U1 0 U2 3 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4481-6 PY 2012 BP 697 EP + PG 2 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA BA4HE UT WOS:000335710300083 ER PT B AU Trease, B Arvidson, R Lindemann, R Bennett, K Zhou, F Iagnemma, K Senatore, C Van Dyke, L AF Trease, Brian Arvidson, Raymond Lindemann, Randel Bennett, Keith Zhou, Feng Iagnemma, Karl Senatore, Carmine Van Dyke, Lauren GP ASME TI DYNAMIC MODELING AND SOIL MECHANICS FOR PATH PLANNING OF THE MARS EXPLORATION ROVERS SO PROCEEDINGS OF THE ASME INTERNATIONAL DESIGN ENGINEERING TECHNICAL CONFERENCES AND COMPUTERS AND INFORMATION IN ENGINEERING CONFERENCE - 2011, VOL 6, PTS A AND B LA English DT Proceedings Paper CT ASME International Design Engineering Technical Conferences/Computers Information in Engineering Conference CY AUG 12-15, 2012 CL Chicago, IL SP ASME, Design Engn Div, ASME, Comp & Informat Engn Div AB To help minimize risk of high sinkage and slippage during drives and to better understand soil properties and rover terramechanics from drive data, a multidisciplinary team was formed under the Mars Exploration Rover (MER) project to develop and utilize dynamic computer-based models for rover drives over realistic terrains. The resulting tool, named ARTEMIS (Adams-based Rover Terramechanics and Mobility Interaction Simulator), consists of the dynamic model, a library of terramechanics subroutines, and the high-resolution digital elevation maps of the Mars surface. A 200-element model of the rovers was developed and validated for drop tests before launch, using MSC-Adams dynamic modeling software. Newly modeled terrain-rover interactions include the rut-formation effect of deformable soils, using the classical Bekker-Wong implementation of compaction resistances and bull-dozing effects. The paper presents the details and implementation of the model with two case studies based on actual MER telemetry data. In its final form, ARTEMIS will be used in a predictive manner to assess terrain navigability and will become part of the overall effort in path planning and navigation for both Martian and lunar rovers. C1 [Trease, Brian] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Arvidson, Raymond; Bennett, Keith; Zhou, Feng; Van Dyke, Lauren] Washington Univ, St Louis, MO USA. [Lindemann, Randel] Caltech jPL, Pasadena, CA USA. [Iagnemma, Karl; Senatore, Carmine] MIT, Cambridge, MA USA. RP Trease, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 23 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-5483-9 PY 2012 BP 755 EP + PG 3 WC Engineering, Mechanical; Robotics SC Engineering; Robotics GA BA4KW UT WOS:000335932600082 ER PT B AU Mazhar, H Seidl, A Shotwell, R Quadrelli, MB Negrut, D Jain, A AF Mazhar, Hammad Seidl, Andrew Shotwell, Rebecca Quadrelli, Marco B. Negrut, Dan Jain, Abhinandan GP ASME TI GRANULAR DYNAMICS SIMULATION ON MULTIPLE GPUS USING DOMAIN DECOMPOSITION SO PROCEEDINGS OF THE ASME INTERNATIONAL DESIGN ENGINEERING TECHNICAL CONFERENCES AND COMPUTERS AND INFORMATION IN ENGINEERING CONFERENCE 2012, VOL 2, PTS A AND B LA English DT Proceedings Paper CT ASME International Design Engineering Technical Conferences/Computers Information in Engineering Conference CY AUG 12-15, 2012 CL Chicago, IL SP ASME, Design Engn Div, ASME, Comp & Informat Engn Div ID RIGID-BODY DYNAMICS; FRICTION AB This paper describes the software infrastructure needed to enable massive multi-body simulation using multiple GPUs. Utilizing a domain decomposition approach, a large system made up of billions of bodies can be split into self-contained subdomains which are then transferred to different GPUs and solved in parallel. Parallelism is enabled on multiple levels, first on the CPU through OpenMP and secondly on the GPU through NVIDIA CUDA (Compute Unified Device Architecture). This heterogeneous software infrastructure can be extended to networks of computers using MPI (Message Passing Interface) as each subdomain is self-contained. This paper will discuss the implementation of the spatial subdivision algorithm used for subdomain creation along with the algorithms used for collision detection and constraint solution. C1 [Mazhar, Hammad; Seidl, Andrew; Shotwell, Rebecca; Negrut, Dan] Univ Wisconsin Madison, Madison, WI 53706 USA. [Quadrelli, Marco B.; Jain, Abhinandan] Calif Inst, Jet Prop Lab, Pasadena, CA USA. RP Mazhar, H (reprint author), Univ Wisconsin Madison, Madison, WI 53706 USA. NR 13 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4501-1 PY 2012 BP 801 EP + PG 2 WC Computer Science, Interdisciplinary Applications; Engineering, Multidisciplinary SC Computer Science; Engineering GA BA4KX UT WOS:000335932700089 ER PT B AU Brown, C AF Brown, Clifford GP ASME TI JET-SURFACE INTERACTION TEST: FAR-FIELD NOISE RESULTS SO PROCEEDINGS OF THE ASME TURBO EXPO 2012, VOL 1 LA English DT Proceedings Paper CT ASME Turbo Expo 2012 CY JUN 11-15, 2012 CL Copenhagen, DENMARK SP Int Gas Turbine Inst ID TRAILING-EDGE; TURBULENT-FLOW; AERODYNAMIC NOISE; SOUND AB Many configurations proposed for the next generation of aircraft rely on the wing or other aircraft surfaces to shield the engine noise from the observers on the ground. However, the ability to predict the shielding effect and any new noise sources that arise from the high-speed jet flow interacting with a hard surface is currently limited. Furthermore, quality experimental data from jets with surfaces nearby suitable for developing and validating noise prediction methods are usually tied to a particular vehicle concept and, therefore, very complicated. The Jet/Surface Interaction Test was intended to supply a high quality set of data covering a wide range of surface geometries and positions and jet flows to researchers developing aircraft noise prediction tools. During phase one, the goal was to measure the noise of a jet near a simple planar surface while varying the surface length and location in order to: (1) validate noise prediction schemes when the surface is acting only as a jet noise shield and when the jet/surface interaction is creating additional noise, and (2) determine regions of interest for more detailed tests in phase two. To meet these phase one objectives, a flat plate was mounted on a two-axis traverse in two distinct configurations: (1) as a shield between the jet and the observer (microphone array) and (2) as a reflecting surface on the opposite side of the jet from the observer. The surface was moved through axial positions 2 <= x(TE)/D-j <= 20 (measured at the surface trailing edge, x(TE), and normalized by the jet diameter, D-j) and radial positions 1 <= h/D-j <= 20. Far-field and phased array noise data were acquired at each combination of axial and radial surface location using two nozzles and at 8 different jet exit conditions across several flow regimes (subsonic cold, subsonic hot, underexpanded, ideally expanded, and overexpanded supersonic cold). The far-field noise results, discussed here, show where the surface shields some of the jet noise and, depending on the location of the surface and the created as a surface extends downstream and approaches the jet plume. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Brown, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 23 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4467-0 PY 2012 BP 357 EP 369 PG 13 WC Engineering, Mechanical SC Engineering GA BA4HH UT WOS:000335720700034 ER PT B AU Podboy, GG AF Podboy, Gary G. GP ASME TI JET-SURFACE INTERACTION TEST: PHASED ARRAY NOISE SOURCE LOCALIZATION RESULTS SO PROCEEDINGS OF THE ASME TURBO EXPO 2012, VOL 1 LA English DT Proceedings Paper CT ASME Turbo Expo 2012 CY JUN 11-15, 2012 CL Copenhagen, DENMARK SP Int Gas Turbine Inst AB An experiment was conducted to investigate the effect that a planar surface located near a jet flow has on the noise radiated to the far-field. Two different configurations were tested: 1) a shielding configuration in which the surface was located between the jet and the far-field microphones, and 2) a reflecting configuration in which the surface was mounted on the opposite side of the jet, and thus the jet noise was free to reflect off the surface toward the microphones. Both conventional far-field microphone and phased array noise source localization measurements were obtained. This paper discusses phased array results, while a companion paper(1) discusses far-field results. The phased array data show that the axial distribution of noise sources in a jet can vary greatly depending on the jet operating condition and suggests that it would first be necessary to know or be able to predict this distribution in order to be able to predict the amount of noise reduction to expect from a given shielding configuration. The data obtained on both subsonic and supersonic jets show that the noise sources associated with a given frequency of noise tend to move downstream, and therefore, would become more difficult to shield, as jet Mach number increases. The noise source localization data obtained on cold, shock-containing jets suggests that the constructive interference of sound waves that produces noise at a given frequency within a broadband shock noise hump comes primarily from a small number of shocks, rather than from all the shocks at the same time. The reflecting configuration data illustrates that the law of reflection must be satisfied in order for jet noise to reflect off of a surface to an observer, and depending on the relative locations of the jet, the surface, and the observer, only some of the jet noise sources may satisfy this requirement. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Podboy, GG (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 15 TC 0 Z9 0 U1 0 U2 2 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4467-0 PY 2012 BP 381 EP 414 PG 34 WC Engineering, Mechanical SC Engineering GA BA4HH UT WOS:000335720700036 ER PT B AU Simon, DL Armstrong, JB AF Simon, Donald L. Armstrong, Jeffrey B. GP ASME TI AN INTEGRATED APPROACH FOR AIRCRAFT ENGINE PERFORMANCE ESTIMATION AND FAULT DIAGNOSTICS SO PROCEEDINGS OF THE ASME TURBO EXPO 2012, VOL 1 LA English DT Proceedings Paper CT ASME Turbo Expo 2012 CY JUN 11-15, 2012 CL Copenhagen, DENMARK SP Int Gas Turbine Inst AB A Kalman filter-based approach for integrated on-line aircraft engine performance estimation and gas path fault diagnostics is presented. This technique is specifically designed for underdetermined estimation problems where there are more unknown system parameters representing deterioration and faults than available sensor measurements. A previously developed methodology is applied to optimally design a Kalman filter to estimate a vector of tuning parameters, appropriately sized to enable estimation. The estimated tuning parameters can then be transformed into a larger vector of health parameters representing system performance deterioration and fault effects. The results of this study show that basing fault isolation decisions solely on the estimated health parameter vector does not provide ideal results. Furthermore, expanding the number of the health parameters to address additional gas path faults causes a decrease in the estimation accuracy of those health parameters representative of turbomachinery performance deterioration. However, improved fault isolation performance is demonstrated through direct analysis of the estimated tuning parameters produced by the Kalman filter. This was found to provide equivalent or superior accuracy compared to the conventional fault isolation approach based on the analysis of sensed engine outputs, while simplifying online implementation requirements. Results from the application of these techniques to an aircraft engine simulation are presented and discussed. C1 [Simon, Donald L.] NASA, Glenn Res Ctr, 21000 Brookpark Rd,MS 77-1, Cleveland, OH 44135 USA. [Armstrong, Jeffrey B.] ASRC Aerosp Corp, Cleveland, OH 44135 USA. RP Simon, DL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd,MS 77-1, Cleveland, OH 44135 USA. NR 21 TC 1 Z9 1 U1 0 U2 1 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4467-0 PY 2012 BP 935 EP + PG 3 WC Engineering, Mechanical SC Engineering GA BA4HH UT WOS:000335720700091 ER PT B AU May, RD Garg, S AF May, Ryan D. Garg, Sanjay GP ASME TI REDUCING CONSERVATISM IN AIRCRAFT ENGINE RESPONSE USING CONDITIONALLY ACTIVE MIN-MAX LIMIT REGULATORS SO PROCEEDINGS OF THE ASME TURBO EXPO 2012, VOL 1 LA English DT Proceedings Paper CT ASME Turbo Expo 2012 CY JUN 11-15, 2012 CL Copenhagen, DENMARK SP Int Gas Turbine Inst AB Current aircraft engine control logic uses a Min-Max control selection structure to prevent the engine from exceeding any safety or operational limits during transients due to throttle commands. This structure is inherently conservative and produces transient responses that are slower than necessary. In order to utilize the existing safety margins more effectively, a modification to this architecture is proposed, referred to as a Conditionally Active (CA) limit regulator. This concept uses the existing Min-Max architecture with the modification that limit regulators are active only when the operating point is close to a particular limit. This paper explores the use of CA limit regulators using a publicly available commercial aircraft engine simulation. The improvement in thrust response while maintaining all necessary safety limits is demonstrated in a number of cases. C1 [May, Ryan D.] ASRC Aerosp Corp, Cleveland, OH 44135 USA. [Garg, Sanjay] NASA Glenn Res Ctr, Cleveland, OH USA. RP May, RD (reprint author), ASRC Aerosp Corp, Cleveland, OH 44135 USA. EM ryan.d.may@nasa.gov; sanjay.garg@nasa.gov FU NASA Aviation Safety Program's Vehicle Systems Safety Technologies Project FX The authors would like to thank the NASA Aviation Safety Program's Vehicle Systems Safety Technologies Project for funding this work. NR 9 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4467-0 PY 2012 BP 959 EP + PG 2 WC Engineering, Mechanical SC Engineering GA BA4HH UT WOS:000335720700093 ER PT B AU Klettlinger, JLS AF Klettlinger, Jennifer Lindsey Suder GP ASME TI EFFECT OF AROMATIC CONCENTRATION OF A FISCHER-TROPSCH FUEL ON THERMAL STABILITY SO PROCEEDINGS OF THE ASME TURBO EXPO 2012, VOL 2, PTS A AND B LA English DT Proceedings Paper CT ASME Turbo Expo 2012 CY JUN 11-15, 2012 CL Copenhagen, DENMARK SP Int Gas Turbine Inst AB Fischer-Tropsch (F-T) jet fuel composition differs from petroleum-based, conventional commercial jet fuel because of differences in feedstock and production methodology. Fischer-Tropsch fuel typically has a lower aromatic and sulfur content and consists primarily of iso and normal parafins The ASTM D3241 specification for Jet Fuel Thermal Oxidation Test (JFTOT) break point testing method was used to test the breakpoint of a baseline commercial grade F-T jet fuel, and various blends of this F-T fuel with an aromatic solution. The goal of this research is to determine the effect of aromatic content on the thermal stability of Fischer-Tropsch fuel. The testing completed in this report was supported by the NASA Fundamental Aeronautics Subsonics Fixed Wing Project. C1 NASA, Lewis Res Ctr, Cleveland, OH 44135 USA. RP Klettlinger, JLS (reprint author), NASA, Lewis Res Ctr, Cleveland, OH 44135 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4468-7 PY 2012 BP 401 EP 408 PG 8 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA BA4HI UT WOS:000335720800039 ER PT B AU Bhargava, A Liscinsky, D McKinney, R Anderson, B Petzold, A Miake-Lye, RC AF Bhargava, Anuj Liscinsky, David McKinney, Randal Anderson, Bruce Petzold, Andreas Miake-Lye, Richard C. GP ASME TI CHARACTERIZING PARTICULATE MATTER EMISSIONS FROM AIRCRAFT ENGINES SO PROCEEDINGS OF THE ASME TURBO EXPO 2012, VOL 2, PTS A AND B LA English DT Proceedings Paper CT ASME Turbo Expo 2012 CY JUN 11-15, 2012 CL Copenhagen, DENMARK SP Int Gas Turbine Inst ID INHALED ULTRAFINE PARTICLES; AEROSOLS; PARTEMIS AB Research in the areas of particulate matter (PM) emissions impacts on both climate and human health are currently very active, however there are a large number of variables and response times. As a better understanding of the contribution of aviation PM emissions is developed, new aircraft engines will need to be designed for reduced PM emissions. In order to do this, measurement methods for different PM metrics like mass, number, size distribution, volatile precursors and composition need to be developed followed by measurements for existing engines to assess their environmental impact. Relevant literature will be reviewed to show that it is necessary to control emissions of nanometer-size particles from a total "number count" as well as a "mass" perspective. Several activities to develop a measurement method and evaluate its effectiveness will be discussed. The results are being used to develop standard measurement methods for aircraft PM emissions which will allow the design of lower emission combustors. C1 [Bhargava, Anuj; McKinney, Randal] Pratt & Whitney, E Hartford, CT 06108 USA. [Liscinsky, David] United Technol Res Ctr, East Hartford, CT USA. [Anderson, Bruce] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Petzold, Andreas] DLR, Inst Phys Atnnosphare, Oberpfaffenhofen, Germany. [Miake-Lye, Richard C.] Aerodyne Res Inc, Billerica, MA USA. RP Bhargava, A (reprint author), Pratt & Whitney, E Hartford, CT 06108 USA. RI Petzold, Andreas/J-2347-2012 OI Petzold, Andreas/0000-0002-2504-1680 NR 30 TC 0 Z9 0 U1 0 U2 1 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4468-7 PY 2012 BP 1185 EP + PG 3 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA BA4HI UT WOS:000335720800110 ER PT B AU Thomas, AE Saxena, NT Shouse, DT Neuroth, C Lynch, A Frayne, CW Stutrud, JS Corporan, E Hankins, T Hendricks, RC AF Thomas, Anna E. Saxena, Nikita T. Shouse, Dale T. Neuroth, Craig Lynch, Amy Frayne, Charles W. Stutrud, Jeffrey S. Corporan, Edwin Hankins, Terry Hendricks, Robert C. GP ASME TI HEATING AND EFFICIENCY COMPARISON OF A FISCHER-TROPSCH (FT) FUEL, JP-8+100, AND BLENDS IN A THREE-CUP COMBUSTOR SECTOR SO PROCEEDINGS OF THE ASME TURBO EXPO 2012, VOL 2, PTS A AND B LA English DT Proceedings Paper CT ASME Turbo Expo 2012 CY JUN 11-15, 2012 CL Copenhagen, DENMARK SP Int Gas Turbine Inst AB In order to realize alternative fueling for military and commercial use, the industry has set forth guidelines that must be met by each fuel. These aviation fueling requirements are outlined in MIL-DTL-83133F(2008) or ASTM D 7566-Annex standards and are classified as "drop-in" fuel replacements. This paper provides combustor performance data for synthetic-paraffinic-kerosene- (SPK-) type (Fisher-Tropsch. (FT)) fuel and blends with JP-8+100, relative to JP-8+100 as baseline fueling. Data were taken at various nominal inlet conditions: 75 psia (0.52 MPa) at 500 degrees F (533 K), 125 psia (0.86 MPa.) at 625 degrees F (603 K), 175 psia (1.21 MPa) at 725 degrees F (658 K), and 225 psia (1.55 MPa) at 790 degrees F (694 K). Combustor performance analysis assessments were made for the change in flame temperatures, combustor efficiency, wall temperatures, and exhaust plane temperatures at 3%, 4%, and 5% combustor pressure drop (%Delta P) for fuel:air ratios (F/A) ranging from 0.010 to 0.025. Significant general trends show lower liner temperatures and higher flame and combustor outlet temperatures with increases in FT fueling relative to JP-8+100 fueling. The latter affects both turbine efficiency and blade/vane life. In general, 100% SPK-FT fuel and blends with JP-8+100 produce less particulates and less smoke and have lower thermal impact on combustor hardware. C1 [Thomas, Anna E.] Georgia Inst Technol, Atlanta, GA 30332 USA. [Saxena, Nikita T.] Tufts Univ, Medford, MA 02155 USA. [Shouse, Dale T.; Neuroth, Craig; Lynch, Amy; Frayne, Charles W.; Stutrud, Jeffrey S.; Corporan, Edwin; Hankins, Terry] AFRL WPAFB, Wright Patterson AFB, OH 45433 USA. [Hendricks, Robert C.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Thomas, AE (reprint author), Georgia Inst Technol, Atlanta, GA 30332 USA. EM aet4@gatech.edu; Nikita.saxena@tufts.edu; dale.shouse@wpafb.af.mil; Robert.C.Hendricks@nasa.gov NR 8 TC 0 Z9 0 U1 0 U2 2 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4468-7 PY 2012 BP 1439 EP + PG 3 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA BA4HI UT WOS:000335720800133 ER PT B AU Ibrahim, MB Vinci, S Kartuzova, O Volino, RJ AF Ibrahim, Mounir B. Vinci, Samuel Kartuzova, Olga Volino, Ralph J. GP ASME TI CFD SIMULATIONS OF UNSTEADY WAKES ON A HIGHLY LOADED LOW PRESSURE TURBINE AIRFOIL (L1A) SO PROCEEDINGS OF THE ASME TURBO EXPO 2012, VOL 4, PTS A AND B LA English DT Proceedings Paper CT ASME Turbo Expo 2012 CY JUN 11-15, 2012 CL Copenhagen, DENMARK SP Int Gas Turbine Inst ID TRANSITION; FLOWS; LIFT AB A study of a very high lift, low-pressure turbine airfoil in the presence of unsteady wakes was performed computationally and compared against experimental results. The experiments were conducted in a low speed wind tunnel under high (4.9%) and then low (0.6%) freestream turbulence intensity conditions with a flow coefficient (zeta)of 0.7. The experiments were done on a linear cascade with wakes that were produced from moving rods upstream of the cascade with the rod to blade spacing varied from 1 to 1.6 to 2. In the present study two different Reynolds numbers (25,000 and 50,000, based on the suction surface length and the nominal exit velocity from the cascade) were considered. The experimental and computational data have shown that in cases without wakes, the boundary layer separated and did not reattach. The CFD was performed with Large Eddy Simulation (LES) and Unsteady Reynolds-Averaged Navier-Stokes (URANS), Transition-SST, utilizing the finite-volume code ANSYS FLUENT under the same freestream turbulence and Reynolds number conditions as the experiment but only at a rod to blade spacing of 1. With wakes, separation was largely suppressed, particularly if the wake passing frequency was sufficiently high. Similar effect was predicted by 3D CFD simulations. Computational results for the pressure coefficients and velocity profiles were in a reasonable agreement with experimental ones for all cases examined. The 2D CFD efforts failed to capture the three dimensionality effects of the wake and thus were less consistent with the experimental data. As a further computational study, cases were run to simulate higher wake passing frequencies which were not run experimentally. The results of these computational cases showed that an initial 25% increase from the experimental dimensionless wake passing frequency of F=0.45 greatly reduced the size of the separation bubble, nearly completely suppressing it, however an additional 33% increase on top of this did not prove to have much of an effect. C1 [Ibrahim, Mounir B.; Vinci, Samuel] Cleveland State Univ, Dept Mech Engn, Cleveland, OH 44115 USA. [Kartuzova, Olga] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. [Volino, Ralph J.] US Naval Acad, Mech Engn Dept, Annapolis, MD 21402 USA. RP Ibrahim, MB (reprint author), Cleveland State Univ, Dept Mech Engn, Cleveland, OH 44115 USA. EM m.ibrahim@csuohio.edu; olga.kartuzova@nasa.gov; volino@usna.edu FU National Aeronautics and Space Administration FX This work was sponsored by the National Aeronautics and Space Administration. The grant monitor is Dr. James Heidmann of the NASA Glenn Research Center. The support of the United States Naval Academy Technical Support Department Shop and Fluids Laboratory is greatly appreciated. We greatly appreciate the computer time provided for us by the Ohio Super Computer (OSC). The OSC Computer Cluster has been made available as part of the Center's mission to support Ohio Universities. NR 20 TC 1 Z9 1 U1 0 U2 2 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4470-0 PY 2012 BP 843 EP + PG 4 WC Engineering, Mechanical SC Engineering GA BA4JP UT WOS:000335868900074 ER PT B AU Pai, SS Riha, DS AF Pai, Shantaram S. Riha, David S. GP ASME TI MODEL VERIFICATION AND VALIDATION CONCEPTS FOR A PROBABILISTIC FRACTURE ASSESSMENT MODEL TO PREDICT CRACKING OF KNIFE EDGE SEALS IN THE SPACE SHUTTLE MAIN ENGINE HIGH PRESSURE OXIDIZER SO PROCEEDINGS OF THE ASME TURBO EXPO 2012, VOL 7, PTS A AND B LA English DT Proceedings Paper CT ASME Turbo Expo 2012 CY JUN 11-15, 2012 CL Copenhagen, DENMARK SP Int Gas Turbine Inst AB Physics-based models are routinely used to predict the performance of engineered systems to make decisions such as when to retire system components, how to extend the life of an aging system, or if a new design will be safe or available. Model verification and validation (V&V) is a process to establish credibility in model predictions. Ideally, carefully controlled validation experiments will be designed and performed to validate models or submodels. In reality, time and cost constraints limit experiments and even model development. This paper describes elements of model V&V during the development and application of a probabilistic fracture assessment model to predict cracking in space shuttle main engine high-pressure oxidizer turbopump knife-edge seals. The objective of this effort was to assess the probability of initiating and growing a crack to a specified failure length in specific flight units for different usage and inspection scenarios. The probabilistic fracture assessment model developed in this investigation combined a series of submodels describing the usage, temperature history, flutter tendencies, tooth stresses and numbers of cycles, fatigue cracking, nondestructive inspection, and finally the probability of failure. The analysis accounted for unit-to-unit variations in temperature, flutter limit state, flutter stress magnitude, and fatigue life properties. The investigation focused on the calculation of relative risk rather than absolute risk between the usage scenarios. Verification predictions were first performed for three units with known usage and cracking histories to establish credibility in the model predictions. Then, numerous predictions were performed for an assortment of operating units that had flown recently or that were projected for future flights. Calculations were performed using two NASA-developed software tools: NESSUS (R) for the probabilistic analysis, and NASGRO (R) for the fracture mechanics analysis. The goal of these predictions was to provide additional information to guide decisions on the potential of reusing existing and installed units prior to the new design certification. C1 [Pai, Shantaram S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Riha, David S.] Southwest Res Inst, San Antonio, TX USA. RP Pai, SS (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 10 TC 0 Z9 0 U1 0 U2 2 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4473-1 PY 2012 BP 459 EP + PG 2 WC Engineering, Mechanical SC Engineering GA BA4JO UT WOS:000335868800051 ER PT B AU Duffy, KP Choi, BB Provenza, AJ Min, JB Kray, N AF Duffy, Kirsten P. Choi, Benjamin B. Provenza, Andrew J. Min, James B. Kray, Nicholas GP ASME TI ACTIVE PIEZOELECTRIC VIBRATION CONTROL OF SUBSCALE COMPOSITE FAN BLADES SO PROCEEDINGS OF THE ASME TURBO EXPO 2012, VOL 7, PTS A AND B LA English DT Proceedings Paper CT ASME Turbo Expo 2012 CY JUN 11-15, 2012 CL Copenhagen, DENMARK SP Int Gas Turbine Inst AB As part of the Fundamental Aeronautics program, researchers at NASA Glenn Research Center (GRC) are investigating new technologies supporting the development of lighter, quieter, and more efficient fans for turbomachinery applications. High performance fan blades designed to achieve such goals will be subjected to higher levels of aerodynamic excitations which could lead to more serious and complex vibration problems. Piezoelectric materials have been proposed as a means of decreasing engine blade vibration either through a passive damping scheme, or as part of an active vibration control system. For polymer matrix fiber composite blades, the piezoelectric elements could be embedded within the blade material, protecting the brittle piezoceramic material from the airflow and from debris. To investigate this idea, spin testing was performed on two General Electric Aviation (GE) subscale composite fan blades in the NASA GRC Dynamic Spin Rig Facility. The first bending mode (1B) was targeted for vibration control. Because these subscale blades are very thin, the piezoelectric material was surface-mounted on the blades. Three thin piezoelectric patches were applied to each blade two actuator patches and one small sensor patch. These flexible macro-fiber-composite patches were placed in a location of high resonant strain for the 1B mode. The blades were tested up to 5000 rpm, with patches used as sensors, as excitation for the blade, and as part of open- and closed-loop vibration control. Results show that with a single actuator patch, active vibration control causes the damping ratio to increase from a baseline of 0.3% critical damping to about 1.0% damping at 0 RPM. As the rotor speed approaches 5000 RPM, the actively controlled blade damping ratio decreases to about 0.5% damping. This occurs primarily because of centrifugal blade stiffening, and can be observed by the decrease in the generalized electromechanical coupling with rotor speed. C1 [Duffy, Kirsten P.] Univ Toledo, Cleveland, OH 44192 USA. [Choi, Benjamin B.; Provenza, Andrew J.; Min, James B.] NASA Glenn Res Ctr, Cleveland, OH USA. [Kray, Nicholas] GE Aviat, Cleveland, OH USA. RP Duffy, KP (reprint author), Univ Toledo, Cleveland, OH 44192 USA. NR 22 TC 0 Z9 0 U1 1 U2 1 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4473-1 PY 2012 BP 1217 EP + PG 3 WC Engineering, Mechanical SC Engineering GA BA4JO UT WOS:000335868800122 ER PT B AU Hah, C Mueller, M Schiffer, HP AF Hah, Chunill Mueller, Martin Schiffer, Heinz-Peter GP ASME TI STUDY OF CONVECTIVE FLOW EFFECTS IN ENDWALL CASING TREATMENTS IN TRANSONIC COMPRESSOR ROTORS SO PROCEEDINGS OF THE ASME TURBO EXPO 2012, VOL 8, PTS A-C LA English DT Proceedings Paper CT ASME Turbo Expo 2012 CY JUN 11-15, 2012 CL Copenhagen, DENMARK SP Int Gas Turbine Inst AB The unsteady convective flow effects in a transonic compressor rotor with a circumferential-groove casing treatment are investigated in this paper. Experimental results show that the circumferential-groove casing treatment increases the compressor stall margin by almost 50% for the current transonic compressor rotor. Steady flow simulation of the current casing treatment, however, yields only a 15% gain in stall margin. The flow field at near-stall operation is highly unsteady due to several self-induced flow phenomena. These include shock oscillation, vortex shedding at the trailing edge, and interaction between the passage shock and the tip clearance vortex. The primary focus of the current investigation is to assess the effects of flow unsteadiness and unsteady flow convection on the circumferential-groove casing treatment. Unsteady Reynolds-averaged Navier-Stokes (URANS) and Large Eddy Simulation (LES) techniques were applied in addition to steady Reynolds-averaged Navier-Stokes (RANS) to simulate the flow field at near-stall operation and to determine changes in stall margin. The current investigation reveals that unsteady flow effects are as important as steady flow effects on the performance of the circumferential grooves casing treatment in extending the stall margin of the current transonic compressor rotor. The primary unsteady flow mechanism is unsteady flow injection from the grooves into the main flow near the casing. Flows moving into and out of the grooves are caused due to local pressure difference near the grooves. As the pressure field becomes transient due to self-induced flow oscillation, flow injection from the grooves also becomes unsteady. The unsteady flow simulation shows that this unsteady flow injection from the grooves is substantial and contributes significantly to extending the compressor stall margin. Unsteady flows into and out of the grooves have as large a role as steady flows in the circumferential grooves. While the circumferential-groove casing treatment seems to be a steady flow device, unsteady flow effects should be included to accurately assess its performance as the flow is transient at near-stall operation. C1 [Hah, Chunill] NASA, Glenn Res Ctr, MS 5-11, Cleveland, OH 44135 USA. [Mueller, Martin; Schiffer, Heinz-Peter] Tech Univ Darmstadt, D-64287 Darmstadt, Germany. RP Hah, C (reprint author), NASA, Glenn Res Ctr, MS 5-11, Cleveland, OH 44135 USA. FU U.S. Government FX This work is in part a work of the U.S. Government. ASME disclaims all interest in the U.S. Government's contributions. NR 22 TC 0 Z9 0 U1 0 U2 1 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4474-8 PY 2012 BP 95 EP + PG 3 WC Engineering, Mechanical SC Engineering GA BA4HJ UT WOS:000335720900009 ER PT B AU Kulkarni, S Celestina, ML Adamczyk, JJ AF Kulkarni, Sameer Celestina, Mark L. Adamczyk, John J. GP ASME TI DEVELOPMENT AND APPLICATIONS OF A STAGE STACKING PROCEDURE SO PROCEEDINGS OF THE ASME TURBO EXPO 2012, VOL 8, PTS A-C LA English DT Proceedings Paper CT ASME Turbo Expo 2012 CY JUN 11-15, 2012 CL Copenhagen, DENMARK SP Int Gas Turbine Inst AB The preliminary design of multistage axial compressors in gas turbine engines is typically accomplished with mean-line methods. These methods, which rely on empirical correlations, estimate compressor performance well near the design point, but may become less reliable off-design. For land-based applications of gas turbine engines, off-design performance estimates are becoming increasingly important, as turbine plant operators desire peaking or load-following capabilities and hot-day operability. The current work develops a one-dimensional stage stacking procedure. This includes a newly-defined blockage term, which is used to estimate the off-design performance and operability range of a 13-stage axial compressor. The new blockage term is defined to give mathematical closure on static pressure, and values of blockage are shown to collapse to a curve as functions of stage inlet flow coefficient and corrected speed. Utility of the stage stacking procedure is demonstrated by estimation of the minimum corrected speed which allows stable operation of the compressor Further utility of the stage stacking procedure is demonstrated with a bleed sensitivity study, which estimates a bleed schedule to expand the compressor's operating range. C1 [Kulkarni, Sameer; Celestina, Mark L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Adamczyk, John J.] NASA, Glenn Res Ctr, DRA, Cleveland, OH 44135 USA. RP Kulkarni, S (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. FU NASA; Graduate 310 Student Researchers Program (GSRP) through a Reimbursable Space Act Agreement between NASA Glenn Research Center; Siemens Energy, Inc. FX The authors would like to thank Dr. Matthew D. Montgomery, Dr. Eric E. Donahoo, Mr. Paul S. Spedaler, Mr. David Wasdell, and Dr. Christian Cornelius of Siemens Energy, Inc. and Dr. Choon S. Tan of the Massachusetts Institute of Technology for useful suggestions during many technical discussions throughout the course of this work. The authors would like to acknowledge Mr. Richard A. Mulac of NASA Glenn Research Center for his technical assistance in running the CFD and meshing software. The first author would like to acknowledge funding of this work by the NASA Graduate 310 Student Researchers Program (GSRP) through a Reimbursable Space Act Agreement between NASA Glenn Research Center and Siemens Energy, Inc. NR 13 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4474-8 PY 2012 BP 301 EP + PG 2 WC Engineering, Mechanical SC Engineering GA BA4HJ UT WOS:000335720900027 ER PT B AU Liou, MS Lee, BJ AF Liou, Meng-Sing Lee, Byung Joon GP ASME TI CHARACTERIZATION OF AERODYNAMIC PERFORMANCE OF BOUNDARY-LAYER-INGESTING INLET UNDER CROSSWIND SO PROCEEDINGS OF THE ASME TURBO EXPO 2012, VOL 8, PTS A-C LA English DT Proceedings Paper CT ASME Turbo Expo 2012 CY JUN 11-15, 2012 CL Copenhagen, DENMARK SP Int Gas Turbine Inst AB NASA has been studying future transport concepts, envisioned to be technically realizable in the timeframe of 2020-2030, to meet environmental and performance goals. One concept receiving considerable interest involves a propulsion system embedded into a hybrid wingbody aircraft. While offering significant advantages in fuel savings and noise reduction by this concept, there are several technical challenges that are not encountered in the current fleet and must be overcome so as to deliver target performance and operability. One of these challenges is associated with an inlet system that ingests a significantly thick boundary layer, developing along the wingbody surface, into a serpentine diffuser before the flow meeting fan blades. The flow is subject to considerable total pressure loss and distorted at the fan face, much more significantly than in the inlet system of conventional aircraft. In our previous studies [1, 2], we have shown that through innovative design changes on the airframe surface, it is possible to simultaneously increase total pressure recovery and decrease distortion in the flow, without resorting to conventional penalty-ridden flow control concepts, such as vortex generator or boundary layer bleeding/suction. In the current study, we are interested in understanding the following issues: how the embedded propulsion system performs under a crosswind condition by studying in detail the flow characteristics of two inlets, the baseline and another optimized previously under the cruise condition. With the insight, it is hoped that it can help in the follow-on study by devising effective strategies to minimize flow distortion arising from the integration of an embedded-engine system into an airframe to the level acceptable to the operation of engine fan. C1 [Liou, Meng-Sing] NASA Glenn Res Ctr, Aeroprop Div, Cleveland, OH 44135 USA. RP Liou, MS (reprint author), NASA Glenn Res Ctr, Aeroprop Div, Cleveland, OH 44135 USA. EM meng-sing.liou@nasa.gov; mdo.bjlee@gmail.com NR 28 TC 0 Z9 0 U1 0 U2 1 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4474-8 PY 2012 BP 1977 EP 1989 PG 13 WC Engineering, Mechanical SC Engineering GA BA4HJ UT WOS:000335720901012 ER PT S AU Grieves, MW AF Grieves, Michael W. BE Rivest, L Bouras, A Louhichi, B TI Virtually Indistinguishable Systems Engineering and PLM SO PRODUCT LIFECYCLE MANAGEMENT: TOWARDS KNOWLEDGE-RICH ENTERPRISES (PLM 2012) SE IFIP Advances in Information and Communication Technology LA English DT Proceedings Paper CT 9th IFIP WG 5.1 International Conference on Product Lifecycle Management (PLM) CY JUL 09-11, 2012 CL Univ Quebec, Ecole Technologie Superieure, Montreal, CANADA SP Int Federat Informat Proc Working Grp 5 1, PCO Innovat, Dassault Syst, Audros, Strategy Consulting & Innovat Prod Engn Inc, GPA, Lab Ingn Produits Procedes & Syst, CRIAQ HO Univ Quebec, Ecole Technologie Superieure DE Product Lifecycle Management; PLM; Systems Engineering; Model-based Engineering; MBSE; Product Development AB This paper proposes that Systems Engineering and Product Lifecycle Management are closely related. In fact, the contention is that one of the threads that has led to the formation of Product Lifecycle Management is Systems Engineering. Product Lifecycle Management extends Systems Engineering and uses many of its methodologies and processes. However, this connection between these two areas has not gotten the proper attention from either industry or academia. Cross-pollinating Product Lifecycle Management and Systems Engineering would benefit both disciplines.. The paper is based on the author's observation and work at large organizations with significant Systems Engineering disciplines, such as NASA, the United States' Department of Defense, Boeing Corporation, Lockheed Martin, and others. The discrepancy between Systems Engineering claims of being involved in the entire product lifecycle versus the reality of Systems Engineering ending its involvement with the product at requirement verification informs the perspective of this paper. C1 [Grieves, Michael W.] NASA, MSFC, Huntsville, AL 35812 USA. [Grieves, Michael W.] Florida Inst Technol, Melbourne, FL 32901 USA. RP Grieves, MW (reprint author), NASA, MSFC, Huntsville, AL 35812 USA. EM mgrieves@ameritech.net NR 14 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 1868-4238 BN 978-3-642-35758-9 J9 IFIP ADV INF COMM TE PY 2012 VL 388 BP 226 EP 242 PG 17 WC Computer Science, Artificial Intelligence; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications; Computer Science, Software Engineering; Robotics SC Computer Science; Robotics GA BD7LE UT WOS:000363260500020 ER PT S AU Santos, E Koop, D Maxwell, T Doutriaux, C Ellqvist, T Potter, G Freire, J Williams, D Silva, CT AF Santos, Emanuele Koop, David Maxwell, Thomas Doutriaux, Charles Ellqvist, Tommy Potter, Gerald Freire, Juliana Williams, Dean Silva, Claudio T. BE Groth, P Frew, J TI Designing a Provenance-Based Climate Data Analysis Application SO PROVENANCE AND ANNOTATION OF DATA AND PROCESSES, IPAW 2012 SE Lecture Notes in Computer Science LA English DT Proceedings Paper CT 4th International Provenance and Annotation Workshop (IPAW) CY JUN 19-21, 2012 CL Univ California, Bren Sch Environm Sci & Management, Santa Barbara, CA HO Univ California, Bren Sch Environm Sci & Management AB Climate scientists have made substantial progress in understanding Earth's climate system, particularly at global and continental scales. Climate research is now focused on understanding climate changes over wider ranges of time and space scales. These efforts are generating ultra-scale data sets at very high spatial resolution. An insightful analysis in climate science depends on using software tools to discover, access, manipulate, and visualize the data sets of interest. These data exploration tasks can be complex and time-consuming, and they frequently involve many resources from both the modeling and observational climate communities. Because of the complexity of the explorations, provenance is critical, allowing scientists to ensure reproducibility, revisit existing computational pipelines, and more easily share analyses and results. In addition, as the results of this work can impact policy, having provenance available is important for decision-making. In this paper we describe, UV-CDAT, a workflow-based, provenance-enabled system that integrates climate data analysis libraries and visualization tools in an end-to-end application, making it easier for scientists to integrate and use a wide array of tools. C1 [Santos, Emanuele; Koop, David; Ellqvist, Tommy; Freire, Juliana; Silva, Claudio T.] NYU, Polytech Inst, New York, NY 10003 USA. [Maxwell, Thomas; Potter, Gerald] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Doutriaux, Charles; Williams, Dean] Lawrence Livermore Natl Lab, Lawrence, KS USA. RP Santos, E (reprint author), NYU, Polytech Inst, New York, NY 10003 USA. FU U.S. Department of Energy (DOE) Office of Biological and Environmental Research (BER) FX This project has been funded by the U.S. Department of Energy (DOE) Office of Biological and Environmental Research (BER). This is a large project involving many institutions, including LLNL, LBNL, Los Alamos, ORNL, Kitware, NYU-Poly, SCI-Utah, and NASA. NR 4 TC 2 Z9 2 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 978-3-642-34222-6 J9 LECT NOTES COMPUT SC PY 2012 VL 7525 BP 214 EP 219 PG 6 WC Computer Science, Information Systems; Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BB6XF UT WOS:000345094300018 ER PT S AU Hua, H Wilson, B Manipon, G Pan, L Fetzer, E AF Hua, Hook Wilson, Brian Manipon, Gerald Pan, Lei Fetzer, Eric BE Groth, P Frew, J TI Improving the Understanding of Provenance and Reproducibility of a Multi-Sensor Merged Climate Data Record SO PROVENANCE AND ANNOTATION OF DATA AND PROCESSES, IPAW 2012 SE Lecture Notes in Computer Science LA English DT Proceedings Paper CT 4th International Provenance and Annotation Workshop (IPAW) CY JUN 19-21, 2012 CL Univ California, Bren Sch Environm Sci & Management, Santa Barbara, CA HO Univ California, Bren Sch Environm Sci & Management DE provenance; semantic; open provenance model; reproducibility; multi-sensor; data fusion; climate data; web services; faceted navigation; visualization C1 [Hua, Hook; Wilson, Brian; Manipon, Gerald; Pan, Lei; Fetzer, Eric] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hua, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM hook.hua@jpl.nasa.gov; bdwilson@jpl.nasa.gov; gmanipon@jpl.nasa.gov; lei.pan@jpl.nasa.gov; eric.j.fetzer@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 978-3-642-34222-6 J9 LECT NOTES COMPUT SC PY 2012 VL 7525 BP 236 EP 236 PG 1 WC Computer Science, Information Systems; Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BB6XF UT WOS:000345094300024 ER PT B AU Rose, KA Fabrizio, MC Phelan, BA AF Rose, Kenneth A. Fabrizio, Mary C. Phelan, Beth A. BE Jennings, CA Lauer, TE Vondracek, B TI Determining Authorship: Why Is Something that Seems so Simple Often so Difficult? SO SCIENTIFIC COMMUNICATION FOR NATURAL RESOURCE PROFESSIONALS LA English DT Article; Book Chapter ID CITATION ANALYSIS; INDEX; RESPONSIBILITY; FACULTY; SCIENCE; CREDIT C1 [Rose, Kenneth A.] Louisiana State Univ, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70816 USA. [Fabrizio, Mary C.] Virginia Inst Marine Sci, Dept Fisheries Sci, Gloucester Point, VA 23062 USA. [Phelan, Beth A.] NOAA, Natl Marine Fisheries Serv, Northeast Fisheries Sci Ctr, Highlands, NJ 07732 USA. RP Rose, KA (reprint author), Louisiana State Univ, Dept Oceanog & Coastal Sci, Energy Coast & Environm Bldg, Baton Rouge, LA 70816 USA. EM karose@lsu.edu NR 35 TC 0 Z9 0 U1 2 U2 8 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE, STE 110, BETHESDA, MD 20814-2199 USA BN 978-1-934874-28-8 PY 2012 BP 7 EP 18 PG 12 WC Education, Scientific Disciplines SC Education & Educational Research GA BA5DU UT WOS:000336557800002 ER PT S AU Giannakopoulou, D Rakamaric, Z Raman, V AF Giannakopoulou, Dimitra Rakamaric, Zvonimir Raman, Vishwanath BE Mine, A Schmidt, D TI Symbolic Learning of Component Interfaces SO STATIC ANALYSIS, SAS 2012 SE Lecture Notes in Computer Science LA English DT Proceedings Paper CT 19th International Static Analysis Symposium (SAS) CY SEP 11-13, 2012 CL Deauville, FRANCE SP CNRS, Ecole Normale Superieure, INRIA ID COMPOSITIONAL VERIFICATION; L-ASTERISK; GENERATION AB Given a white-box component C with specified unsafe states, we address the problem of automatically generating an interface that captures safe orderings of invocations of C's public methods. Method calls in the generated interface are guarded by constraints on their parameters. Unlike previous work, these constraints are generated automatically through an iterative refinement process. Our technique, named PSYCO ( Predicate-based SYmbolic COmpositional reasoning), employs a novel combination of the L* automata learning algorithm with symbolic execution. The generated interfaces are three-valued, capturing whether a sequence of method invocations is safe, unsafe, or its effect on the component state is unresolved by the symbolic execution engine. We have implemented PSYCO as a new prototype tool in the JPF open-source software model checking platform, and we have successfully applied it to several examples. C1 [Giannakopoulou, Dimitra] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Rakamaric, Zvonimir] Univ Utah, Sch Comp, Salt Lake City, UT 84112 USA. [Raman, Vishwanath] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA. RP Giannakopoulou, D (reprint author), NASA Ames Res Ctr, Moffett Field, CA 94035 USA. EM dimitra.giannakopoulou@nasa.gov; zvonimir.rakamaric@gmail.com; vishwa.raman@sv.cmu.edu FU NASA CMU [NNA10DE60C] FX This research was supported by the NASA CMU grant NNA10DE60C. NR 23 TC 6 Z9 6 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 978-3-642-33125-1 J9 LECT NOTES COMPUT SC PY 2012 VL 7460 BP 248 EP 264 PG 17 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BB3IR UT WOS:000342807500018 ER PT S AU Jovanovic, VM Bull, M Diner, DJ Geier, S Rheingans, B AF Jovanovic, V. M. Bull, M. Diner, D. J. Geier, S. Rheingans, B. BE Shortis, M ElSheimy, N TI AUTOMATED DATA PRODUCTION FOR A NOVEL AIRBORNE MULTIANGLE SPECTROPOLARIMETRIC IMAGER (AIRMSPI) SO XXII ISPRS CONGRESS, TECHNICAL COMMISSION I SE International Archives of the Photogrammetry Remote Sensing and Spatial Information Sciences LA English DT Proceedings Paper CT 22nd Congress of the International-Society-for-Photogrammetry-and-Remote-Sensing CY AUG 25-SEP 01, 2012 CL Melbourne, AUSTRALIA SP Int Soc Photogrammetry & Remote Sensing, Hexagon, ESRI, RMIT Univ, Sch Math Geospatial Sci DE Polarization; Multi-angle; Calibration; Orthorectification; Pushbroom; Bundle-adjustment; Mapping; NASA-ER2 ID INSTRUMENT DESCRIPTION AB A novel polarimetric imaging technique making use of rapid retardance modulation has been developed by JPL as a part of NASA's Instrument Incubator Program. It has been built into the Airborne Multiangle SpectroPolarimetric Imager (AirMSPI) under NASA's Airborne Instrument Technology Transition Program, and is aimed primarily at remote sensing of the amounts and microphysical properties of aerosols and clouds. AirMSPI includes an 8-band (355, 380, 445, 470, 555, 660, 865, 935 nm) pushbroom camera that measures polarization in a subset of the bands (470, 660, and 865 nm). The camera is mounted on a gimbal and acquires imagery in a configurable set of along-track viewing angles ranging between +67 degrees and -67 degrees relative to nadir. As a result, near simultaneous multi-angle, multi-spectral, and polarimetric measurements of the targeted areas at a spatial resolution ranging from 7 m to 20 m (depending on the viewing angle) can be derived. An automated data production system is being built to support high data acquisition rate in concert with co-registration and orthorectified mapping requirements. To date, a number of successful engineering checkout flights were conducted in October 2010, August-September 2011, and January 2012. Data products resulting from these flights will be presented. C1 [Jovanovic, V. M.; Bull, M.; Diner, D. J.; Geier, S.; Rheingans, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jovanovic, VM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Veljko.Jovanoviic@jpl.nasa.gov NR 10 TC 2 Z9 2 U1 0 U2 0 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLE 1E, GOTTINGEN, 37081, GERMANY SN 2194-9034 J9 INT ARCH PHOTOGRAMM PY 2012 VL 39-B1 BP 33 EP 38 PG 6 WC Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA BD1OS UT WOS:000358208700007 ER PT S AU Ouml;zen, H Fox, N Gurbuz, SZ Deadman, A Behnert, I Harris, P Yua, L Griffith, D Kaewmanee, M Prakobya, A Musana, C Ponzoni, F Lee, D Lee, Y Boucher, Y Viallefont, F Rolland, P Helder, D Leigh, L Thome, K Sterckx, S Knaeps, E Raeymaekers, D Henry, P AF Ozen, Hilal Fox, Nigel Gurbuz, S. Z. Deadman, A. Behnert, I. Harris, P. Yua, L. Griffith, D. Kaewmanee, M. Prakobya, A. Musana, C. Ponzoni, F. Lee, D. Lee, Y. Boucher, Y. Viallefont, F. Rolland, P. Helder, D. Leigh, L. Thome, K. Sterckx, S. Knaeps, E. Raeymaekers, D. Henry, P. BE Shortis, M ElSheimy, N TI PRELIMINARY RESULTS OF THE COMPARISON OF SATELLITE IMAGERS USING TUZ GOLU AS A REFERENCE STANDARD SO XXII ISPRS CONGRESS, TECHNICAL COMMISSION I SE International Archives of the Photogrammetry Remote Sensing and Spatial Information Sciences LA English DT Proceedings Paper CT 22nd Congress of the International-Society-for-Photogrammetry-and-Remote-Sensing CY AUG 25-SEP 01, 2012 CL Melbourne, AUSTRALIA SP Int Soc Photogrammetry & Remote Sensing, Hexagon, ESRI, RMIT Univ, Sch Math Geospatial Sci DE Remote Sensing; Satellite; Sensor; Calibration; Comparison AB Earth surfaces, such as deserts, salt lakes, and playas, have been widely used in the vicarious radiometric calibration of optical earth observation satellites. In 2009, the Infrared and Visible Optical Sensors (IVOS) sub-group of the Committee of Earth Observation Satellites (CEOS) Working Group on Calibration and Validation (WGCV) designated eight LANDNET reference sites to focus international efforts, facilitate traceability and enable the establishment of measurement "best practices." With support from the European Space Agency (ESA), one of the LANDNET sites, the Tuz Golu salt lake located in central Turkey, was selected to host a cross-comparison of measurement instrumentation and methodologies conducted by 11 different ground teams across the globe. This paper provides an overview of the preliminary results of the cross-comparison of the ground-based spectral measurements made during the CEOS Land Comparison 13-27 August, 2010 with the simultaneous satellite image data acquisitions of the same site. C1 [Ozen, Hilal; Gurbuz, S. Z.] TUBITAK UZAY, TR-06531 Ankara, Turkey. [Fox, Nigel; Deadman, A.; Behnert, I.; Harris, P.] Natl Phys Lab, Teddington TW11 0LW, Middx, England. [Gurbuz, S. Z.] TOBB ETU, Dept Elect & Elect Engn, Sogutozu Ankara, Turkey. [Yua, L.] CMA, Beijing, Peoples R China. [Griffith, D.] CSIR, ZA-0184 Silverton, South Africa. [Kaewmanee, M.; Prakobya, A.; Musana, C.] GISTDA, Bangkok 10210, Thailand. [Ponzoni, F.] INPE, BR-12630000 Cachoeira Paulista, SP, Brazil. [Lee, D.; Lee, Y.] KARI, Taejon, South Korea. [Boucher, Y.; Viallefont, F.; Rolland, P.] Off Natl Etud & Rech Aerosp, FR-31055 Toulouse, France. [Helder, D.; Leigh, L.] S Dakota State Univ, Elect Engn, Brookings, SD 57007 USA. [Thome, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sterckx, S.; Knaeps, E.; Raeymaekers, D.] VITO, BE-2400 Mol, Belgium. [Henry, P.] CNES, F-31401 Toulouse, France. RP Ouml;zen, H (reprint author), TUBITAK UZAY, METU Campus, TR-06531 Ankara, Turkey. EM hilal.ozen@uzay.tubitak.gov.tr; nigel.fox@npl.co.uk; sevgi.gurbuz@uzay.tubitak.gov.tr; andrew.deadman@npl.co.uk; liyuan@cma.gov.cn; dgriffith@csir.co.za; Mkaewmanee@eoc.gistda.or.th; amornprk@eoc.gistda.or.th; chaichat@eoc.gistda.or.th; flavio@dsr.inpe.br; dglee@kari.re.kr; yhlee@kari.re.kr; yannick.boucher@onera.fr; francoise.viallefont@onera.fr; philippe.rolland@onera.fr; dennis.helder@sdstate.edu; larry.leigh@sdstate.edu; kurtis.thome@nasa.gov; sindy.sterckx@vito.be; els.knaeps@vito.be; dries.raymaekers@vito.be; patrice.henry@cnes.fr NR 8 TC 0 Z9 0 U1 0 U2 2 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLE 1E, GOTTINGEN, 37081, GERMANY SN 2194-9034 J9 INT ARCH PHOTOGRAMM PY 2012 VL 39-B1 BP 145 EP 148 PG 4 WC Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA BD1OS UT WOS:000358208700027 ER PT S AU Meyer, DJ Tachikawa, T Abrams, M Crippen, R Krieger, T Gesch, D Carabajal, C AF Meyer, D. J. Tachikawa, T. Abrams, M. Crippen, R. Krieger, T. Gesch, D. Carabajal, C. BE Shortis, M Madden, M TI SUMMARY OF THE VALIDATION OF THE SECOND VERSION OF THE ASTER GDEM SO XXII ISPRS CONGRESS, TECHNICAL COMMISSION IV SE International Archives of the Photogrammetry Remote Sensing and Spatial Information Sciences LA English DT Proceedings Paper CT 22nd Congress of the International-Society-for-Photogrammetry-and-Remote-Sensing CY AUG 25-SEP 01, 2012 CL Melbourne, AUSTRALIA SP Int Soc Photogrammetry & Remote Sensing, Hexagon, ESRI, RMIT Univ, Sch Math Geospatial Sci DE ASTER; Global Digital Elevation Model; Accuracy; DEM/DTM; Comparison; Geodesy; Global-Environmental-Databases; Land Cover; Mapping; Satellite AB On October 17, 2011, NASA and the Ministry of Economy, Trade and Industry (METI) of Japan released the second version of the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) Global Digital Elevation Model (GDEM) to users worldwide at no charge as a contribution to the Global Earth Observing System of Systems (GEOSS). The first version of the ASTER GDEM, released on June 29, 2009, was compiled from over 1.2 million scene-based DEMs covering land surfaces between 83 degrees N and 83 degrees S latitudes. The second version (GDEM2) incorporates 260,000 additional scenes to improve coverage, a smaller correlation kernel to yield higher spatial resolution, and improved water masking. As with GDEM1, US and Japanese partners collaborated to validate GDEM2. Its absolute accuracy was within -0.20 meters on average when compared against 18,000 geodetic control points over the conterminous US (CONUS), with an accuracy of 17 meters at the 95% confidence level. The Japan study noted the GDEM2 differed from the 10-meter national elevation grid by -0.7 meters over bare areas, and by 7.4 meters over forested areas. The CONUS study noted a similar result, with the GDEM2 determined to be about 8 meters above the 1 arc-second US National Elevation Database (NED) over most forested areas, and more than a meter below NED over bare areas. A global ICESat study found the GDEM2 to be on average within 3 meters of altimeter-derived control. The Japan study noted a horizontal displacement of 0.23 pixels in GDEM2. A study from the US National Geospatial Intelligence Agency also determined horizontal displacement and vertical accuracy as compared to the 1 arc-second Shuttle Radar Topography Mission DEM. US and Japanese studies estimated the horizontal resolution of the GDEM2 to be between 71 and 82 meters. Finally, the number of voids and artifacts noted in GDEM1 were substantially reduced in GDEM2. C1 [Meyer, D. J.; Gesch, D.] US Geol Survey, Earth Resource Observat & Sci Ctr, Sioux Falls, SD 57030 USA. [Tachikawa, T.] Earth Remote Sensing Data Anal Ctr, Tokyo, Japan. [Abrams, M.; Crippen, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Krieger, T.] US Natl Geospatial Intelligence Agcy, St Louis, MO USA. [Carabajal, C.] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA. RP Meyer, DJ (reprint author), US Geol Survey, Earth Resource Observat & Sci Ctr, Sioux Falls, SD 57030 USA. EM dmeyer@usgs.gov; tatikawa@ersdac.or.jp; mabrams@jpl.nasa.gov; robert.e.crippen@jpl.nasa.gov; Tabitha.L.Krieger@nga.mil; gesch@usgs.gov; Claudia.C.Carabajal@nasa.gov NR 7 TC 4 Z9 4 U1 0 U2 1 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLE 1E, GOTTINGEN, 37081, GERMANY SN 2194-9034 J9 INT ARCH PHOTOGRAMM PY 2012 VL 39-B4 BP 291 EP 293 PG 3 WC Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA BD1OW UT WOS:000358212000054 ER PT S AU Kiang, RK Soebiyanto, RP AF Kiang, R. K. Soebiyanto, R. P. BE Shortis, M Shimoda, H Cho, K TI MAPPING THE RISKS OF MALARIA, DENGUE AND INFLUENZA USING SATELLITE DATA SO XXII ISPRS CONGRESS, TECHNICAL COMMISSION VIII SE International Archives of the Photogrammetry Remote Sensing and Spatial Information Sciences LA English DT Proceedings Paper CT 22nd Congress of the International-Society-for-Photogrammetry-and-Remote-Sensing CY AUG 25-SEP 01, 2012 CL Melbourne, AUSTRALIA SP Int Soc Photogrammetry & Remote Sensing, Hexagon, ESRI, RMIT Univ, Sch Math Geospatial Sci DE Malaria; Dengue; Influenza; satellite; remote sensing ID SEASONAL INFLUENZA; TRANSMISSION AB It has long been recognized that environment and climate may affect the transmission of infectious diseases. The effects are most obvious for vector-borne infectious diseases, such as malaria and dengue, but less so for airborne and contact diseases, such as seasonal influenza. In this paper, we examined the meteorological and environmental parameters that influence the transmission of malaria, dengue and seasonal influenza. Remotely sensed parameters that provide such parameters were discussed. Both statistical and biologically inspired, processed based models can be used to model the transmission of these diseases utilizing the remotely sensed parameters as input. Examples were given for modelling malaria in Thailand, dengue in Indonesia, and seasonal influenza in Hong Kong. C1 [Kiang, R. K.; Soebiyanto, R. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Soebiyanto, R. P.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA. RP Kiang, RK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Richard.kiang@nasa.gov; radina.p.soebiyanto@nasa.gov NR 19 TC 0 Z9 0 U1 0 U2 0 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLE 1E, GOTTINGEN, 37081, GERMANY SN 2194-9034 J9 INT ARCH PHOTOGRAMM PY 2012 VL 39-B8 BP 83 EP 86 PG 4 WC Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA BD1OR UT WOS:000358207600016 ER PT S AU Torrusio, S Lagerloef, G Rabolli, M LeVine, D AF Torrusio, S. Lagerloef, G. Rabolli, M. LeVine, D. BE Shortis, M Shimoda, H Cho, K TI SAC-D AQUARIUS A SATELLITE FOR OCEAN, CLIMATE AND ENVIRONMENT. ONE YEAR OF DATA. SO XXII ISPRS CONGRESS, TECHNICAL COMMISSION VIII SE International Archives of the Photogrammetry Remote Sensing and Spatial Information Sciences LA English DT Proceedings Paper CT 22nd Congress of the International-Society-for-Photogrammetry-and-Remote-Sensing CY AUG 25-SEP 01, 2012 CL Melbourne, AUSTRALIA SP Int Soc Photogrammetry & Remote Sensing, Hexagon, ESRI, RMIT Univ, Sch Math Geospatial Sci DE SAC-D Aquarius; ocean salinity; microwave radiometers; optical sensors; international mission; observatory AB The SAC-D/Aquarius satellite was launched in June 10, 2011. It's a joint mission between Argentina (through CONAE) and US (NASA). This satellite is a true Observatory with a suite of sensors for Earth Observation, its weight is 1400 kg, sun-synchronous orbit at 657 km (6 pm ascendant node), revisit of seven days. Other space agencies have contributed with instruments and support (facilities and ground segment), as CNES, CSI, ASI and AEB/INPE. The primary objective is to monitor global variations in ocean surface salinity (SSS) in order to improve the knowledge about ocean circulation, water cycle and climate. The SSS is performed with Aquarius instrument (NASA). Other oceanic and atmospheric parameters are measured with a MWR, from CONAE, in K and Ka band, as wind speed, rain rate, sea ice, water vapour and liquid water in clouds. The thermal camera (NIRST) estimates sea surface temperature and detect high temperature events (fires and volcanic eruptions). The High Sensitivity Camera (HSC) generates night images (very useful for fishery activity monitoring in the sea, studying of electrical storms, polar auroras and urban application). The DCS (Data Collection System, from CONAE) can receive meteorological and environmental data from ground platforms and distribute among users. The TDP (Technological Demonstration Package, from CONAE) measures different parameters of satellite position and velocity. Other two important instruments are ROSA (from Italy) and CARMEN 1 (from France). The first is an atmospheric sounder, it allows elaborating atmospheric profiles of temperature, pressure and humidity, and the second has detectors for studies of space debris and the effects of radiation on electronic devices. This work provides a review of the first year of data, including the status of calibration and validation, other finding and at the same time we want to present the progress in the active educational and outreach program including the information of SAC-D Aquarius Mission. C1 [Torrusio, S.; Rabolli, M.] CONAE, Natl Commiss Space Act, RA-1063 Buenos Aires, DF, Argentina. [Lagerloef, G.] Earth & Space Res, Seattle, WA USA. [LeVine, D.] NASA Headquarters, Washington, DC USA. RP Torrusio, S (reprint author), CONAE, Natl Commiss Space Act, Avda Paseo Colon 751, RA-1063 Buenos Aires, DF, Argentina. EM storrusio@conae.gov.ar; lager@esr.org; mrabolli@conae.gov.ar; David.M.LeVine@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLE 1E, GOTTINGEN, 37081, GERMANY SN 2194-9034 J9 INT ARCH PHOTOGRAMM PY 2012 VL 39-B8 BP 551 EP 554 PG 4 WC Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA BD1OR UT WOS:000358207600101 ER PT J AU Baluchamy, S Ravichandran, P Ramesh, V He, ZH Zhang, Y Hall, JC Jejelowo, O Gridley, DS Wu, HL Ramesh, GT AF Baluchamy, Sudhakar Ravichandran, Prabakaran Ramesh, Vani He, Zhenhua Zhang, Ye Hall, Joseph C. Jejelowo, Olufisayo Gridley, Daila S. Wu, Honglu Ramesh, Govindarajan T. TI Reactive oxygen species mediated tissue damage in high energy proton irradiated mouse brain SO MOLECULAR AND CELLULAR BIOCHEMISTRY LA English DT Article DE Proton; Reactive oxygen species (ROS); Lipid peroxidation; Antioxidants; Tissue damage ID GENE-EXPRESSION PROFILE; LUNG EPITHELIAL-CELLS; FACTOR-KAPPA-B; IONIZING-RADIATION; OXIDATIVE STRESS; MEMORY IMPAIRMENT; SPACE RADIATION; APOPTOSIS; EXPOSURE; MELATONIN AB Although radiation related research has been conducted extensively, the molecular toxicology and cellular mechanisms affected by proton radiation remain poorly understood. We recently reported that the high energy protons induce cell death through activation of apoptotic signaling genes; caspase 3 and 8 (Baluchamy et al. J Biol Chem 285:24769-24774, 2010). In this study, we investigated the effect of different doses of protons in in vivo mouse system, particularly, brain tissues. A significant dose-dependent induction of reactive oxygen species and lipid peroxidation and reduction of antioxidants; glutathione and superoxide dismutase were observed in proton irradiated mouse brain as compared to control brain. Furthermore, histopathology studies on proton irradiated mouse brain showed significant tissue damage as compared to control brain. Together, our in vitro and in vivo results suggest that proton irradiation alters oxidant and antioxidant levels in the cells to cause proton mediated DNA/tissue damage followed by apoptotic cell death. C1 [Ravichandran, Prabakaran; Ramesh, Vani; Hall, Joseph C.; Ramesh, Govindarajan T.] Norfolk State Univ, Mol Toxicol Lab, Ctr Biotechnol & Biomed Sci, Dept Biol, Norfolk, VA 23504 USA. [Baluchamy, Sudhakar] Pondicherry Univ, Dept Biotechnol, Pondicherry 605014, India. [He, Zhenhua] Univ Houston Clear Lake City, Dept Biol Sci, Houston, TX 77058 USA. [Zhang, Ye; Wu, Honglu] NASA, Lyndon B Johnson Space Ctr, Radiat Biophys Lab, Houston, TX 77058 USA. [Jejelowo, Olufisayo] Texas So Univ, Dept Biol, Houston, TX 77004 USA. [Gridley, Daila S.] Loma Linda Univ, Med Ctr, Dept Radiat Med, Loma Linda, CA 92354 USA. [Zhang, Ye; Wu, Honglu] NASA, Lyndon B Johnson Space Ctr, Core Bioanalyt Lab, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. RP Ramesh, GT (reprint author), Norfolk State Univ, Mol Toxicol Lab, Ctr Biotechnol & Biomed Sci, Dept Biol, Norfolk, VA 23504 USA. EM gtramesh@nsu.edu RI Gridley, Daila/P-7711-2015 FU NASA [NNX08BA47A: NCC-1-02038: NIH 1P20MD001822-1] FX The authors would like to thank Mrs. Ramya Gopikrishnan and Mr. Santosh Biradar for helpful suggestions. This study was supported by NASA funding NNX08BA47A: NCC-1-02038: NIH 1P20MD001822-1 to Dr. G. T, R. NR 33 TC 4 Z9 5 U1 0 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0300-8177 J9 MOL CELL BIOCHEM JI Mol. Cell. Biochem. PD JAN PY 2012 VL 360 IS 1-2 BP 189 EP 195 DI 10.1007/s11010-011-1056-2 PG 7 WC Cell Biology SC Cell Biology GA 857MO UT WOS:000297722800020 PM 21948272 ER PT J AU Wang, W Shu, CW Yee, HC Sjogreen, B AF Wang, Wei Shu, Chi-Wang Yee, H. C. Sjoegreen, Bjoern TI High order finite difference methods with subcell resolution for advection equations with stiff source terms SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Stiff reaction term; Shock capturing; Detonation; WENO; ENO subcell resolution ID HYPERBOLIC CONSERVATION-LAWS; RANDOM PROJECTION METHOD; REACTION-CONVECTION EQUATIONS; STATE NUMERICAL-SOLUTIONS; SHOCK-CAPTURING SCHEMES; NONLINEAR SOURCE TERMS; EFFICIENT IMPLEMENTATION; DIMENSIONAL DETONATIONS; DYNAMICAL-APPROACH; WAVE-PROPAGATION AB A new high order finite-difference method utilizing the idea of Harten ENO subcell resolution method is proposed for chemical reactive flows and combustion. In reaction problems, when the reaction time scale is very small, e.g., orders of magnitude smaller than the fluid dynamics time scales, the governing equations will become very stiff. Wrong propagation speed of discontinuity may occur due to the underresolved numerical solution in both space and time. The present proposed method is a modified fractional step method which solves the convection step and reaction step separately. In the convection step, any high order shock-capturing method can be used. In the reaction step, an ODE solver is applied but with the computed flow variables in the shock region modified by the Harten subcell resolution idea. For numerical experiments, a fifth-order finite-difference WENO scheme and its anti-diffusion WENO variant are considered. A wide range of 1D and 2D scalar and Euler system test cases are investigated. Studies indicate that for the considered test cases, the new method maintains high order accuracy in space for smooth flows, and for stiff source terms with discontinuities, it can capture the correct propagation speed of discontinuities in very coarse meshes with reasonable CFL numbers. (C) 2011 Elsevier Inc. All rights reserved. C1 [Wang, Wei] Florida Int Univ, Dept Math & Stat, Miami, FL 33199 USA. [Shu, Chi-Wang] Brown Univ, Div Appl Math, Providence, RI 02912 USA. [Yee, H. C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sjoegreen, Bjoern] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. RP Wang, W (reprint author), Florida Int Univ, Dept Math & Stat, Miami, FL 33199 USA. EM weiwang1@fiu.edu RI Shu, Chi-Wang/A-3216-2013 OI Shu, Chi-Wang/0000-0001-7720-9564 FU DOE/SciDAC SAP [DE-AI02-06ER25796]; US Department of Energy at Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; ARO [W911NF-08-1-0520]; NASA FX The authors acknowledge the support of the DOE/SciDAC SAP Grant DE-AI02-06ER25796. The work by Bjorn Sjogreen was performed under the auspices of the US Department of Energy at Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. The research of C.-W. Shu is also partially supported by ARO Grant W911NF-08-1-0520. The research of H.C. Yee is also partially supported by the NASA Fundamental Aeronautics Hypersonic program. NR 34 TC 19 Z9 21 U1 1 U2 15 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 EI 1090-2716 J9 J COMPUT PHYS JI J. Comput. Phys. PD JAN 1 PY 2012 VL 231 IS 1 BP 190 EP 214 DI 10.1016/j.jcp.2011.08.031 PG 25 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 846ZN UT WOS:000296941800012 ER PT J AU Klenzing, J Simoes, F Ivanov, S Heelis, RA Bilitza, D Pfaff, R Rowland, D AF Klenzing, J. Simoes, F. Ivanov, S. Heelis, R. A. Bilitza, D. Pfaff, R. Rowland, D. TI Topside equatorial ionospheric density and composition during and after extreme solar minimum SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INTERNATIONAL REFERENCE IONOSPHERE; ELECTRON-DENSITY; INDEX; MODEL AB During the recent solar minimum, solar activity reached the lowest levels observed during the space age. This extremely low solar activity has accompanied a number of unexpected observations in the Earth's ionosphere-thermosphere system when compared to previous solar minima. Among these are the fact that the ionosphere is significantly contracted beyond expectations based on empirical models. Altitude profiles of ion density and composition measurements near the magnetic dip equator are constructed from the Communication/Navigation Outage Forecast System (C/NOFS) satellite to characterize the shape of the topside ionosphere during the recent solar minimum and into the new solar cycle. The variation of the profiles with respect to local time, season, and solar activity are compared to the IRI-2007 model. Building on initial results reported by Heelis et al. (2009), here we describe the extent of the contracted ionosphere, which is found to persist throughout 2009. The shape of the ionosphere during 2010 is found to be consistent with observations from previous solar minima. C1 [Klenzing, J.; Simoes, F.; Bilitza, D.; Pfaff, R.; Rowland, D.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Heelis, R. A.] Univ Texas Dallas, Ctr Space Sci, Richardson, TX 75080 USA. [Ivanov, S.] Georgia Inst Technol, Dept Phys, Atlanta, GA 30332 USA. [Bilitza, D.] George Mason Univ, Space Weather Lab, Fairfax, VA 22030 USA. RP Klenzing, J (reprint author), NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM jeffrey.klenzing@nasa.gov RI Simoes, Fernando/D-7731-2012; Klenzing, Jeff/E-2406-2011; Rowland, Douglas/F-5589-2012; Pfaff, Robert/F-5703-2012 OI Klenzing, Jeff/0000-0001-8321-6074; Rowland, Douglas/0000-0003-0948-6257; Pfaff, Robert/0000-0002-4881-9715 FU NASA at Goddard Space Flight Center; NASA [NAS5-01068, NNX10AM94G, NNX09AJ74G S04]; USAF FX J.K. and F.S. are supported by appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The work performed by S. I. at Goddard Space Flight Center was made possible by the NASA Education Office through the Undergraduate Student Research Program managed by the Universities Space Research Association. The work at the University of Texas at Dallas is supported by NASA grant NAS5-01068 and NASA grant NNX10AM94G. D. B. is supported through NASA grant NNX09AJ74G S04. The Communication/Navigation Outage Forecast System (C/NOFS) mission, conceived and developed by the Air Force Research Laboratory, is sponsored and executed by the USAF Space Test Program. F10.7, Ri12, and IG12 are provided by the UK World Data Center, and Kp is provided through CDAWeb/GSFC. NR 32 TC 24 Z9 24 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 31 PY 2011 VL 116 AR A12330 DI 10.1029/2011JA017213 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 871UC UT WOS:000298762200008 ER PT J AU Santos-Costa, D Bolton, SJ Sault, RJ Thorne, RM Levin, SM AF Santos-Costa, D. Bolton, S. J. Sault, R. J. Thorne, R. M. Levin, S. M. TI VLA observations at 6.2 cm of the response of Jupiter's electron belt to the July 2009 event SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SYNCHROTRON RADIO-EMISSION; LONG-TERM VARIATIONS; SHOEMAKER-LEVY 9; RADIATION BELTS; SL9 IMPACTS; COMET SHOEMAKER-LEVY-9; MODEL-CALCULATIONS; MAGNETIC-FIELD; FLUX-DENSITY; SL-9 AB We present and analyze observations made with the Very Large Array in 2009. The observations show significant fluctuations in the emission radiated by Jupiter's electron belt between July and September. Intensity variations of 10 up to 40% in the radiation at 6.2 cm were found to be too important to be the results of data errors. The numerical reconstruction of equatorial brightness distributions indicates that the fluctuations were related to the 2009 July impact. The computed tomographic-like maps demonstrate that the formation and subsequent longitudinal dispersion and change in intensity of an impact-related synchrotron "hot spot" were the cause of the fluctuations. By examining the time profile of the longitude-averaged total flux density, we find that the changes in the radiation-belt emission lasted for about 100 days. C1 [Santos-Costa, D.; Bolton, S. J.] SW Res Inst, Dept Space Sci, San Antonio, TX 78238 USA. [Sault, R. J.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. [Thorne, R. M.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Levin, S. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Santos-Costa, D (reprint author), SW Res Inst, Dept Space Sci, San Antonio, TX 78238 USA. EM daniel.santoscosta@swri.edu; scott.bolton@swri.edu; rsault@nrao.edu; rmt@atmos.ucla.edu; steven.levin@jpl.nasa.gov FU NASA [NNG05GR39G]; Juno mission FX This research work was carried out at Southwest Research Institute (TX, USA), the University of Melbourne (Australia) and at the Very Large Array radio astronomy observatory (NM, USA). This work was performed under NASA grant NNG05GR39G and supported by the Juno mission. Radio measurements were made possible at the VLA in 2009 with the approval of the NRAO Observing Proposal ID AS985 and ToO ID AS997. NR 67 TC 1 Z9 1 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 31 PY 2011 VL 116 AR A12236 DI 10.1029/2011JA016921 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 871UC UT WOS:000298762200004 ER PT J AU Choi, DS Dundas, CM AF Choi, D. S. Dundas, C. M. TI Measurements of Martian dust devil winds with HiRISE SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MARS PATHFINDER; THRESHOLD; VORTICES; CAMERA; CYCLE AB We report wind measurements within Martian dust devils observed in plan view from the High Resolution Imaging Science Experiment (HiRISE) orbiting Mars. The central color swath of the HiRISE instrument has three separate charge-coupled devices (CCDs) and color filters that observe the surface in rapid cadence. Active features, such as dust devils, appear in motion when observed by this region of the instrument. Our image animations reveal clear circulatory motion within dust devils that is separate from their translational motion across the Martian surface. Both manual and automated tracking of dust devil clouds reveal tangential winds that approach 20-30 m s(-1) in some cases. These winds are sufficient to induce a similar to 1% decrease in atmospheric pressure within the dust devil core relative to ambient, facilitating dust lifting by reducing the threshold wind speed for particle elevation. Finally, radial velocity profiles constructed from our automated measurements test the Rankine vortex model for dust devil structure. Our profiles successfully reveal the solid body rotation component in the interior, but fail to conclusively illuminate the profile in the outer regions of the vortex. One profile provides evidence for a velocity decrease as a function of r(-1/2), instead of r(-1), suggestive of surface friction effects. However, other profiles do not support this observation, or do not contain enough measurements to produce meaningful insights. Citation: Choi, D. S., and C. M. Dundas (2011), Measurements of Martian dust devil winds with HiRISE, Geophys. Res. Lett., 38, L24206, doi: 10.1029/2011GL049806. C1 [Choi, D. S.] NASA, ORAU, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dundas, C. M.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. RP Choi, DS (reprint author), NASA, ORAU, Goddard Space Flight Ctr, Code 693,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM david.s.choi@nasa.gov RI Choi, David/C-5215-2012; OI Dundas, Colin/0000-0003-2343-7224 FU Mars Reconnaissance Orbiter Project; NASA [NNX09AD98G] FX We thank two anonymous referees for constructive comments that improved this paper. This work was supported by the Mars Reconnaissance Orbiter Project and NASA grant NNX09AD98G. We thank the HiRISE team for planning and acquiring the images used in this work. We also thank Laszlo Kestay, Moses Milazzo, Paul Geissler, Randy Kirk, Ingrid Daubar Spitale, Adam Showman, Emily Rauscher, and Matt Balme for helpful discussions. NR 20 TC 14 Z9 14 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 31 PY 2011 VL 38 AR L24206 DI 10.1029/2011GL049806 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 871TP UT WOS:000298760900002 ER PT J AU Shim, JS Kuznetsova, M Rastatter, L Hesse, M Bilitza, D Butala, M Codrescu, M Emery, B Foster, B Fuller-Rowell, T Huba, J Mannucci, AJ Pi, X Ridley, A Scherliess, L Schunk, RW Stephens, P Thompson, DC Zhu, L Anderson, D Chau, JL Sojka, JJ Rideout, B AF Shim, J. S. Kuznetsova, M. Rastaetter, L. Hesse, M. Bilitza, D. Butala, M. Codrescu, M. Emery, B. Foster, B. Fuller-Rowell, T. Huba, J. Mannucci, A. J. Pi, X. Ridley, A. Scherliess, L. Schunk, R. W. Stephens, P. Thompson, D. C. Zhu, L. Anderson, D. Chau, J. L. Sojka, J. J. Rideout, B. TI CEDAR Electrodynamics Thermosphere Ionosphere (ETI) Challenge for systematic assessment of ionosphere/thermosphere models: NmF2, hmF2, and vertical drift using ground-based observations SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID GENERAL-CIRCULATION MODEL; HIGH-LATITUDE IONOSPHERE; COUPLED ELECTRODYNAMICS; LOWER ATMOSPHERE; PHYSICAL MODELS; ART.; SATELLITE; MIDDLE; RADAR; VELOCITIES AB Objective quantification of model performance based on metrics helps us evaluate the current state of space physics modeling capability, address differences among various modeling approaches, and track model improvements over time. The Coupling, Energetics, and Dynamics of Atmospheric Regions (CEDAR) Electrodynamics Thermosphere Ionosphere (ETI) Challenge was initiated in 2009 to assess accuracy of various ionosphere/thermosphere models in reproducing ionosphere and thermosphere parameters. A total of nine events and five physical parameters were selected to compare between model outputs and observations. The nine events included two strong and one moderate geomagnetic storm events from GEM Challenge events and three moderate storms and three quiet periods from the first half of the International Polar Year (IPY) campaign, which lasted for 2 years, from March 2007 to March 2009. The five physical parameters selected were NmF2 and hmF2 from ISRs and LEO satellites such as CHAMP and COSMIC, vertical drifts at Jicamarca, and electron and neutral densities along the track of the CHAMP satellite. For this study, four different metrics and up to 10 models were used. In this paper, we focus on preliminary results of the study using ground-based measurements, which include NmF2 and hmF2 from Incoherent Scatter Radars (ISRs), and vertical drifts at Jicamarca. The results show that the model performance strongly depends on the type of metrics used, and thus no model is ranked top for all used metrics. The analysis further indicates that performance of the model also varies with latitude and geomagnetic activity level. C1 [Shim, J. S.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Butala, M.; Mannucci, A. J.; Pi, X.; Stephens, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Codrescu, M.; Fuller-Rowell, T.] NOAA, Space Weather Predict Ctr, Boulder, CO 80305 USA. [Chau, J. L.] Inst Geofis Peru, Radio Observat Jicamarca, Lima, Peru. [Emery, B.; Foster, B.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80301 USA. [Huba, J.] USN, Div Plasma Phys, Res Lab, Washington, DC 20375 USA. [Rideout, B.] MIT, Haystack Observ, Westford, MA 01886 USA. [Ridley, A.] Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA. [Scherliess, L.; Schunk, R. W.; Zhu, L.; Sojka, J. J.] Utah State Univ, Ctr Atmospher & Space Sci, Logan, UT 84322 USA. [Thompson, D. C.] USAF, Res Lab, Albuquerque, NM 87117 USA. [Anderson, D.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80305 USA. RP Shim, JS (reprint author), Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, NASA Goddard Space Flight Ctr, Bldg 21,251,Mail Code 674, Greenbelt, MD 20771 USA. EM jasoon.shim@nasa.gov RI Hesse, Michael/D-2031-2012; Rastaetter, Lutz/D-4715-2012; Kuznetsova, Maria/F-6840-2012; Chau, Jorge/C-7568-2013; Ridley, Aaron/F-3943-2011; Scherliess, Ludger/A-7499-2016 OI Rastaetter, Lutz/0000-0002-7343-4147; Chau, Jorge/0000-0002-2364-8892; Ridley, Aaron/0000-0001-6933-8534; Scherliess, Ludger/0000-0002-7388-5255 FU National Science Foundation (NSF) through Cornell University [0905448]; NSF FX The Jicamarca Radio Observatory is a facility of the Instituto Geofisico del Peru operated with support from National Science Foundation (NSF) award AGS-0905448 through Cornell University. The Millstone Hill incoherent scatter radar is supported by the NSF. This study made use of the CEDAR Data Base at the National Center for Atmospheric Research, which is supported by the NSF. NR 48 TC 23 Z9 23 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD DEC 31 PY 2011 VL 9 AR S12003 DI 10.1029/2011SW000727 PG 17 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 871TH UT WOS:000298760100002 ER PT J AU Chan, MA Comiso, JC AF Chan, Mark Aaron Comiso, Josefino C. TI Cloud features detected by MODIS but not by CloudSat and CALIOP SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ALGORITHM AB The ability to characterize the global cloud cover from space has been greatly enhanced by the availability of MODIS, CloudSat, and CALIOP data. The three sensors provide good complementary information about clouds. In this study, we investigated unexpected observations of certain types of clouds apparent in the MODIS data but not detected by CloudSat and CALIOP. Several examples are presented and generally these undetected clouds are geometrically thin, low-level clouds. In particular, they are located in the Arctic region and have optical thicknesses of less than 14, top height altitudes of below 2.5 km, and layer thickness of less than 1 km. CloudSat may miss such low-level clouds because of its coarse vertical resolution of about 500 m and it has limited sensitivity near the surface. Unexpectedly, CALIOP with a much higher vertical resolution of 30 m also misses these clouds and this is due to the cloud's geometrically thin nature and surface proximity. Citation: Chan, M. A., and J. C. Comiso (2011), Cloud features detected by MODIS but not by CloudSat and CALIOP, Geophys. Res. Lett., 38, L24813, doi:10.1029/2011GL050063. C1 [Chan, Mark Aaron; Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chan, Mark Aaron] De La Salle Univ, Ctr Engn & Sustainable Dev Res, Manila, Philippines. RP Chan, MA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM markaaron.c.chan@nasa.gov; josefino.c.comiso@nasa.gov FU NASA FX We would like to thank the MODIS, Cloudsat, and CALIPSO science team for providing excellent and accessible data products that made this study possible. These data were obtained from the NASA Langley Research Center Atmospheric Science Data Center (http://eosweb.larc.nasa.gov/), NASA LAADS Web (http://ladsweb.nascom.nasa.gov/), and NASA CloudSat data processing center (http://cloudsat.cira.colostate.edu/). The NASA Cryospheric Sciences program in part funds this project. NR 11 TC 9 Z9 11 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 30 PY 2011 VL 38 AR L24813 DI 10.1029/2011GL050063 PG 8 WC Geosciences, Multidisciplinary SC Geology GA 871TM UT WOS:000298760600005 ER PT J AU Peters-Lidard, CD Kumar, SV Mocko, DM Tian, YD AF Peters-Lidard, Christa D. Kumar, Sujay V. Mocko, David M. Tian, Yudong TI Estimating evapotranspiration with land data assimilation systems SO HYDROLOGICAL PROCESSES LA English DT Article DE land surface modelling; land data assimilation systems; evapotranspiration; soil moisture assimilation ID SOUTHERN GREAT-PLAINS; SOIL-MOISTURE; SURFACE MODEL; PARAMETERIZATION SCHEMES; INFORMATION-SYSTEM; ENSEMBLE APPROACH; BIOSPHERE MODEL; SNOW COVER; PROJECT; NLDAS AB Advancements in both land surface models (LSMs) and land surface data assimilation, especially over the last decade, have substantially advanced the ability of land data assimilation systems (LDASs) to estimate evapotranspiration (ET). This article provides a historical perspective on international LSM intercomparison efforts and the development of LDASs, both of which have improved LSM ET skill. In addition, an assessment of ET estimates for current LDASs is provided along with current research that demonstrates improvement in LSM ET estimates due to assimilating satellite-based soil moisture products. Using the Ensemble Kalman Filter in the Land Information System, we assimilate both NASA and Land Parameter Retrieval Model soil moisture products into the Noah LSM Version 3.2 with the North American LDAS Phase 2 (NLDAS-2), forcing to mimic the NLDAS-2 configuration. Through comparisons with two global reference ET products, one based on interpolated flux tower data and one from a new satellite ET algorithm, over the NLDAS-2 domain, we demonstrate improvement in ET estimates only when assimilating the LPRM soil moisture product. Copyright (C) 2011 John Wiley & Sons, Ltd. C1 [Peters-Lidard, Christa D.; Kumar, Sujay V.; Mocko, David M.; Tian, Yudong] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. [Kumar, Sujay V.; Mocko, David M.] Sci Applicat Int Corp, Beltsville, MD USA. [Tian, Yudong] Earth Syst Sci Interdisciplinary Ctr, College Pk, MD USA. RP Peters-Lidard, CD (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Code 614-3, Greenbelt, MD 20771 USA. EM christa.peters@nasa.gov RI Kumar, Sujay/B-8142-2015; Peters-Lidard, Christa/E-1429-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876 FU NASA Earth Science Technology Office [AIST-08-077]; NASA Energy and Water Cycle Study; Air Force Weather Agency; NOAA Climate Program Office; NASA Center for Climate Simulation FX We gratefully acknowledge the financial support from the NASA Earth Science Technology Office (Advanced Information System Technology program award AIST-08-077), the NASA Energy and Water Cycle Study, the Air Force Weather Agency, and the NOAA Climate Program Office. The efforts of the NLDAS participants in generating the surface forcing are greatly appreciated. Some of the data used in this effort were acquired as part of the activities of NASA's Science Mission Directorate and are archived and distributed by the GES DISC. Computing was supported by the resources at the NASA Center for Climate Simulation. NR 62 TC 39 Z9 39 U1 0 U2 21 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 DEC 30 PY 2011 VL 25 IS 26 SI SI BP 3979 EP 3992 DI 10.1002/hyp.8387 PG 14 WC Water Resources SC Water Resources GA 867TL UT WOS:000298477300002 ER PT J AU Rodell, M McWilliams, EB Famiglietti, JS Beaudoing, HK Nigro, J AF Rodell, Matthew McWilliams, Eric B. Famiglietti, James S. Beaudoing, Hiroko K. Nigro, Joseph TI Estimating evapotranspiration using an observation based terrestrial water budget SO HYDROLOGICAL PROCESSES LA English DT Article DE evapotranspiration; remote sensing; GRACE; water budget ID DATA ASSIMILATION SYSTEM; MODEL; PRECIPITATION; VARIABILITY; GRACE; ALGORITHM; FRAMEWORK; STATES; SITES; MODIS AB Evapotranspiration (ET) is difficult to measure at the scales of climate models and climate variability. While satellite retrieval algorithms do exist, their accuracy is limited by the sparseness of in situ observations available for calibration and validation, which themselves may be unrepresentative of 500?m and larger scale satellite footprints and grid pixels. Here, we use a combination of satellite and ground-based observations to close the water budgets of seven continental scale river basins (Mackenzie, Fraser, Nelson, Mississippi, Tocantins, Danube, and Ubangi), estimating mean ET as a residual. For any river basin, ET must equal total precipitation minus net runoff minus the change in total terrestrial water storage (TWS), in order for mass to be conserved. We make use of precipitation from two global observation-based products, archived runoff data, and TWS changes from the Gravity Recovery and Climate Experiment (GRACE) satellite mission. We demonstrate that while uncertainty in the water budget-based estimates of monthly ET is often too large for those estimates to be useful, the uncertainty in the mean annual cycle is small enough that it is practical for evaluating other ET products. Here, we evaluate five land surface model simulations, two operational atmospheric analyses, and a recent global reanalysis product based on our results. An important outcome is that the water budget-based ET time series in two tropical river basins, one in Brazil and the other in central Africa, exhibit a weak annual cycle, which may help to resolve debate about the strength of the annual cycle of ET in such regions and how ET is constrained throughout the year. The methods described will be useful for water and energy budget studies, weather and climate model assessments, and satellite-based ET retrieval optimization. Copyright (C) 2011 John Wiley & Sons, Ltd. C1 [Rodell, Matthew; Beaudoing, Hiroko K.; Nigro, Joseph] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD USA. [McWilliams, Eric B.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Beaudoing, Hiroko K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Nigro, Joseph] Sci Syst & Applicat Inc, Lanham, MD USA. RP Rodell, M (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD USA. EM matthew.rodell@nasa.gov RI Rodell, Matthew/E-4946-2012 OI Rodell, Matthew/0000-0003-0106-7437 FU NASA; NASA Goddard Space Flight Center's Summer Institute in Earth Sciences FX The authors thank Sean Swenson and Felix Landerer for detailed discussion on GRACE errors. GRACE land data were processed by Sean Swenson, supported by the NASA MEASURES Program, and are available at http://grace.jpl.nasa.gov. The GRDC and U.S. Army Corps of Engineers are gratefully acknowledged for providing river gauge data used in this study. This work was funded by NASA's Energy and Water Cycle Study program and NASA Goddard Space Flight Center's Summer Institute in Earth Sciences program. NR 39 TC 24 Z9 24 U1 7 U2 47 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 DEC 30 PY 2011 VL 25 IS 26 SI SI BP 4082 EP 4092 DI 10.1002/hyp.8369 PG 11 WC Water Resources SC Water Resources GA 867TL UT WOS:000298477300010 ER PT J AU Zhang, K Kimball, JS Kim, Y McDonald, KC AF Zhang, Ke Kimball, John S. Kim, Youngwook McDonald, Kyle C. TI Changing freeze-thaw seasons in northern high latitudes and associated influences on evapotranspiration SO HYDROLOGICAL PROCESSES LA English DT Article DE freeze thaw; evapotranspiration; cryosphere; growing season; non-frozen season; global warming; vegetation; boreal; Arctic ID SOIL THERMAL DYNAMICS; CLIMATE-CHANGE; BOREAL; FOREST; VEGETATION; SCALE; PRODUCTIVITY; LANDSCAPE; MODIS; CO2 AB Seasonal frozen states in the northern terrestrial cryosphere limit vegetation photosynthetic activities and evapotranspiration (ET) through cold temperature constraints to biological processes and chemical unavailability of water as a result of being frozen. Seasonal transitions of the landscape between predominantly frozen and thawed conditions are analogous to a biospheric and hydrological on/off switch, with marked differences in ET, vegetation productivity and other biological activity between largely dormant winter and active summer conditions. We investigated changes in freezethaw (FT) seasons and ET from 1983 to 2006 and their connections in the northern cryosphere by analyzing independent satellite remote sensing derived FT and ET records. Our findings show that the northern cryosphere (>= 40 degrees N) has experienced advancing (-2.5 days/decade; P = 0.005) and lengthening (3.5 days/decade; P = 0.007) non-frozen season trends over the 24-year period, coinciding with an upward trend (6.4 mm/year/decade; P = 0.014) in regional mean annual ET over the same period. Regional average timing of spring primary thaw and the annual non-frozen period are highly correlated with regional annual ET (vertical bar r vertical bar >= 0.75; P < 0.001), with corresponding impacts to annual ET of approximately 0.6 and 0.5% per day, respectively. The impact of primary fall freeze timing on ET is relatively minor compared with primary spring thaw timing. Earlier onset of the non-frozen season generally promotes annual ET in colder areas but appears to suppress summer ET by increasing drought stress in the southernmost parts of the domain where water supply is the leading constraint to ET. The cumulative effect of future freeze-thaw changes on ET in the region will largely depend on future changes of large-scale atmosphere circulations and rates of vegetation disturbance and adaptation to continued warming. Copyright (C) 2011 John Wiley & Sons, Ltd. C1 [Zhang, Ke] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Zhang, Ke; Kimball, John S.; Kim, Youngwook] Univ Montana, Flathead Lake Biol Stn, Polson, MT 59860 USA. [Zhang, Ke; Kimball, John S.; Kim, Youngwook] Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. [McDonald, Kyle C.] CUNY City Coll, Dept Earth & Atmospher Sci, New York, NY 10031 USA. [McDonald, Kyle C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Zhang, K (reprint author), Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. EM kezhang@fas.harvard.edu RI Zhang, Ke/B-3227-2012 OI Zhang, Ke/0000-0001-5288-9372 FU NASA FX This work was supported by grants from the NASA Terrestrial Ecology and Hydrology programs and Making Earth Science Data Records for Use in Research Environments (MEaSUREs) program. NR 63 TC 21 Z9 22 U1 6 U2 45 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 DEC 30 PY 2011 VL 25 IS 26 SI SI BP 4142 EP 4151 DI 10.1002/hyp.8350 PG 10 WC Water Resources SC Water Resources GA 867TL UT WOS:000298477300015 ER PT J AU Painemal, D Zuidema, P AF Painemal, David Zuidema, Paquita TI Assessment of MODIS cloud effective radius and optical thickness retrievals over the Southeast Pacific with VOCALS-REx in situ measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SOLAR-RADIATION MEASUREMENTS; EFFECTIVE PARTICLE RADIUS; STRATOCUMULUS CLOUDS; MICROPHYSICAL PROPERTIES; SATELLITE RETRIEVALS; DROPLET GROWTH; LIQUID; ASTEX; DRIZZLE; APPROXIMATION AB Cloud microphysical observations collected in situ during the VAMOS Ocean-Cloud-Atmosphere-Land Study Regional Experiment within the Chile-Peru stratocumulus cloud deck during October-November 2008 were used to assess MODIS Level 2 cloud property retrievals. The in situ aircraft-derived cloud property values were constructed from the drop size distributions measured by the Cloud Droplet Probe (drop diameter <52 micron) and Two-Dimensional Cloud Probe (drop diameters up to 1600 micron) during 20 vertical profiles. Almost all of the MODIS cloud scenes were highly homogeneous. MODIS cloud optical thickness correlated well with the aircraft-derived value with a slight offset within instrumental/retrieval uncertainties. In contrast, the standard 2.1 micron-derived MODIS effective radius (r(e)) systematically exceeded the in situ cloud top r(e) by 15%-20%, for an absolute error that increased with droplet size. The individual effective radius retrievals at 1.6, 2.1, and 3.7 micron did not provide additional information on cloud vertical structure for our data sample. The secondarily derived MODIS liquid water path also exceeded the in situ value. A MODIS-derived cloud droplet number concentration (N-d) estimate agreed the best of the four MODIS variables with the aircraft observations. The analysis also highlighted a lack of agreement in published satellite-derived N-d values, despite drawing on the same sources. A best a priori formula choice for N-d is likely to vary regionally. Four sources of errors within the MODIS r(e) retrieval were investigated further: the cloud mode droplet size distribution breadth, the presence of a drizzle mode, above-cloud water vapor absorption, and sensor viewing angles. These processes combined conspired to explain most of the observed bias. The above-cloud water vapor paths were poorly specified, primarily because the cloud top heights are placed too high, and secondarily because the water vapor paths are unrealistic. Improvement of the above-cloud water vapor path specification can most easily and systematically improve the MODIS effective radius and liquid water path retrievals. C1 [Painemal, David; Zuidema, Paquita] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. RP Painemal, D (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA. EM david.painemal@nasa.gov RI Zuidema, Paquita/C-9659-2013 OI Zuidema, Paquita/0000-0003-4719-372X FU National Science Foundation [0745470]; NOAA CPPA [NA07OAR43310270] FX Funding support from the National Science Foundation (Large-Scale Dynamics Grant #0745470) and the NOAA CPPA Program Grant NA07OAR43310270 is gratefully acknowledged. We are indebted to the staff and instrument scientists of the Research Aviation Facility and the National Center for Atmospheric Research involved in the aircraft C-130 operation. Wyoming Cloud Radar data set was generously provided by David Leon. This paper further benefited from discussions with Bruce Albrecht, Graham Feingold, and Peter Minnett. We thank three anonymous reviewers for their careful reading of this manuscript and their valuable comments. MODIS retrievals were obtained from the NR 56 TC 53 Z9 53 U1 4 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 30 PY 2011 VL 116 AR D24206 DI 10.1029/2011JD016155 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 871ON UT WOS:000298747600001 ER PT J AU Imai, M Imai, K Higgins, CA Thieman, JR AF Imai, Masafumi Imai, Kazumasa Higgins, Charles A. Thieman, James R. TI Comparison between Cassini and Voyager observations of Jupiter's decametric and hectometric radio emissions SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND CONTROL; ASTRONOMY OBSERVATIONS; TIME-DEPENDENCE; OUTER PLANETS; RADIATION; FREQUENCY; POLARIZATION; GALILEO; SPACECRAFT; CYCLOTRON AB In this paper, we attempt to clarify the relationship between Jovian hectometric (HOM) and non-Io-related decametric (non-Io-DAM) radio structure. For that purpose, we extend the analysis by including more data and investigating statistical properties of the Jovian DAM and HOM radio emissions based on Cassini and Voyager observations, especially below 16 MHz. We have investigated these emissions observed by the Cassini, Voyager 1, and Voyager 2 spacecraft for specific Jovigraphic latitudes in the range of -3.7 degrees-7.3 degrees and local times in the range of 0.76-21.4 hours. We show a statistical comparison of Cassini, Voyager 1, and Voyager 2 data for occurrence probability in Central Meridian Longitude (CML) versus Io phase and in CML versus Frequency. The main results are as follows: (1) the detailed frequency structures of non-Io-related components can be seen for different spacecraft's local time and Jovigraphic latitude, (2) the high frequency of HOM extends up to near 10 MHz, and (3) a new DAM component, named the non-Io-D, appears from 40 degrees to 60 degrees CML in the frequency range of 7-11 MHz. On the basis of additional information of different behaviors of non-Io-B and non-Io-A structures in longitude depending on pre- and post-encounter of Cassini data, we improved the DAM angular beaming model that shows the cone half-angle of the emitting cone decreases as a function of frequency. We conclude that the changing beaming angle is not affected by Jovigraphic latitude of the spacecraft, but rather due to different local time of the source regions. C1 [Imai, Masafumi] Kochi Natl Coll Technol, Adv Course Mech & Elect Engn, Nankoku, Kochi 7838508, Japan. [Imai, Kazumasa] Kochi Natl Coll Technol, Dept Elect Engn & Informat Sci, Nankoku, Kochi 7838508, Japan. [Higgins, Charles A.] Middle Tennessee State Univ, Dept Phys & Astron, Murfreesboro, TN 37132 USA. [Thieman, James R.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Imai, M (reprint author), Kyoto Univ, Dept Geophys, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan. EM masafumi@jupiter.jp; imai@ee.kochi-ct.ac.jp; chiggins@mtsu.edu; james.r.thieman@nasa.gov RI Imai, Masafumi/S-8736-2016 OI Imai, Masafumi/0000-0002-2814-4036 FU Ministry of Education, Culture, Sports, Science and Technology [19340142] FX The authors are pleased to acknowledge the Cassini RPWS team for access to the Cassini data at the Planetary Data System (PDS) and J. Groene (University of Iowa) for creating Cassini and Voyager ephemeris tables. The authors are especially grateful to J.E.P. Connerney for providing the VIT4 magnetic field model and A. Lecacheux and P. Zarka for numerous discussions. M.I. would like to acknowledge support from M. Fujimoto (JAXA) during a four-month visit to the Observatoire de Paris-Meudon. This work was supported by the Ministry of Education, Culture, Sports, Science and Technology, Grant-in-Aid for Scientific Research (B), 19340142. NR 60 TC 1 Z9 1 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 30 PY 2011 VL 116 AR A12233 DI 10.1029/2011JA016456 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 871UB UT WOS:000298762100001 ER PT J AU Spencer, E Kasturi, P Patra, S Horton, W Mays, ML AF Spencer, E. Kasturi, P. Patra, S. Horton, W. Mays, M. L. TI Influence of solar wind-magnetosphere coupling functions on the Dst index SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID TRANSPOLAR POTENTIAL SATURATION; TAIL CURRENT CONTRIBUTION; INNER MAGNETOSPHERE; GEOMAGNETIC STORMS; RING CURRENT; MAGNETIC STORM; CURRENT SYSTEM; 2-PHASE DECAY; HILL MODEL; ART. AB In this paper we investigate the role of different solar wind magnetosphere coupling functions on the Dst index calculated by the low-order nonlinear dynamical WINDMI model. In our previous work we have shown that the geotail current dynamics has a significant role in the two-phase decay of the Dst index. During that investigation we used the rectified solar wind electric field v(x)B(z) as a baseline for the simulations and analysis. Here we include an evaluation of four other coupling functions in addition to the rectified vB(s). These coupling functions emphasize different physical mechanisms to explain the energy transfer into the magnetosphere due to solar wind velocity, dynamic pressure, magnetic field, and Mach number. One coupling function is due to Siscoe, another by Borovsky, and two by Newell. Our results indicate that for a majority of cases, at most only v(x), B(y), and B(z) are needed to sufficiently account for the supply of energy to the ring current and geotail current components that contribute to the Dst index. The more complex coupling functions sometimes perform extremely well on storm data sets but at other times do not reproduce the Dst index faithfully. The AL index was used as an additional constraint on the allowable geotail current dynamics and to further differentiate between coupling functions when the Dst performance was similar. The solar wind dynamic pressure contribution appears to be correctly accounted for through the calculation of the Dmp formula of Burton et al. (1975). The degree to which the B(y) component affects the Dst index is not entirely clear from our results, but in most cases its inclusion slightly overemphasizes the ring current contribution and slightly underemphasizes the geotail current contribution. C1 [Spencer, E.; Kasturi, P.; Patra, S.] Utah State Univ, Ctr Space Engn, Logan, UT 84322 USA. [Horton, W.] Univ Texas Austin, Space & Geophys Lab, Austin, TX 78712 USA. [Mays, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. RP Spencer, E (reprint author), Utah State Univ, Ctr Space Engn, Logan, UT 84322 USA. EM espencer@engineering.usu.edu FU NSF [NSF-0720201, 0964692]; Applied Research Laboratory at the University of Texas FX This work was partially supported under NSF grant NSF-0720201. The solar wind plasma and magnetic field data were obtained from ACE instrument data at the NASA CDA Web site. The geomagnetic indices used were obtained from the World Data Center for Geomagnetism in Kyoto, Japan. W. Horton acknowledges support from the Applied Research Laboratory at the University of Texas and from NSF grant 0964692. NR 32 TC 4 Z9 4 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 30 PY 2011 VL 116 AR A12235 DI 10.1029/2011JA016780 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 871UB UT WOS:000298762100002 ER PT J AU Han, SC Sauber, J Riva, R AF Han, Shin-Chan Sauber, Jeanne Riva, Riccardo TI Contribution of satellite gravimetry to understanding seismic source processes of the 2011 Tohoku-Oki earthquake SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SUMATRA-ANDAMAN EARTHQUAKE; PACIFIC COAST; SURFACE-WAVES; GRAVITY; GRACE; JAPAN; SLIP AB The 2011 great Tohoku-Oki earthquake, apart from shaking the ground, perturbed the motions of satellites orbiting some hundreds km away above the ground, such as GRACE, due to coseismic change in the gravity field. Significant changes in inter-satellite distance were observed after the earthquake. These unconventional satellite measurements were inverted to examine the earthquake source processes from a radically different perspective that complements the analyses of seismic and geodetic ground recordings. We found the 'average' slip located up-dip of the hypocenter but within the lower crust, as characterized by a limited range of bulk and shear moduli. The GRACE data constrained a group of earthquake source parameters that yield increasing dip (7-16 degrees +/- 2 degrees) and, simultaneously, decreasing moment magnitude (9.17-9.02 +/- 0.04) with increasing source depth (15-24 km). The GRACE solution includes the cumulative moment released over a month and demonstrates a unique view of the long-wavelength gravimetric response to all mass redistribution processes associated with the dynamic rupture and short-term postseismic mechanisms to improve our understanding of the physics of megathrusts. Citation: Han, S.-C., J. Sauber, and R. Riva (2011), Contribution of satellite gravimetry to understanding seismic source processes of the 2011 Tohoku-Oki earthquake, Geophys. Res. Lett., 38, L24312, doi:10.1029/2011GL049975. C1 [Han, Shin-Chan; Sauber, Jeanne] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Han, Shin-Chan] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA. [Riva, Riccardo] Delft Univ Technol, Fac Aerosp Engn, NL-2629 HS Delft, Netherlands. RP Han, SC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA. EM shin-chan.han@nasa.gov RI Sauber, Jeanne/D-7684-2012; Han, Shin-Chan/A-2022-2009 FU NASA FX This work was supported by NASA Earth Surface and Interior program and GRACE projects. We thank DLR for providing the GRACE telemetry data and JPL for producing the high-quality Level-1B products. We are indebted to Emile Okal for his original suggestion for using gravitational normal mode and its formulation. We thank Fred Pollitz, Richard Gross, Junkee Rhie, Meridith Nettles, Chen Ji, and Nick Schmerr for valuable discussion on earthquake modeling and Scott Luthcke and David Rowlands for helping with GRACE L1B data processing. We thank the reviewers for constructive and thorough comments to improve this manuscript. Finally, we acknowledge the information provided by Group on Earth Observations (GEO) through the GEO geohazards supersite website http://supersites.earthobservations.org/. The GRACE gravity solution in terms of spherical harmonic coefficients is available from AGU website. NR 29 TC 24 Z9 26 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 29 PY 2011 VL 38 AR L24312 DI 10.1029/2011GL049975 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 871TD UT WOS:000298759700006 ER PT J AU Abadie, J Abbott, BP Abbott, R Abernathy, M Accadia, T Acernese, F Adams, C Adhikari, R Ajith, P Allen, B Allen, GS Ceron, EA Amin, RS Anderson, SB Anderson, WG Antonucci, F Arain, MA Araya, MC Aronsson, M Arun, KG Aso, Y Aston, SM Astone, P Atkinson, D Aufmuth, P Aulbert, C Babak, S Baker, P Ballardin, G Ballmer, S Barker, D Barnum, S Barone, F Barr, B Barriga, P Barsotti, L Barsuglia, M Barton, MA Bartos, I Bassiri, R Bastarrika, M Bauchrowitz, J Bauer, TS Behnke, B Beker, MG Belletoile, A Benacquista, M Bertolini, A Betzwieser, J Beveridge, N Beyersdorf, PT Bigotta, S Bilenko, IA Billingsley, G Birch, J Birindelli, S Biswas, R Bitossi, M Bizouard, MA Black, E Blackburn, JK Blackburn, L Blair, D Bland, B Blom, M Boccara, C Bock, O Bodiya, TP Bondarescu, R Bondu, F Bonelli, L Bonnand, R Bork, R Born, M Bose, S Bosi, L Bouhou, B Boyle, M Braccini, S Bradaschia, C Brady, PR Braginsky, VB Brau, JE Breyer, J Bridges, DO Brillet, A Brinkmann, M Brisson, V Britzger, M Brooks, AF Brown, DA Budzynski, R Bulik, T Bulten, HJ Buonanno, A Burguet-Castell, J Burmeister, O Buskulic, D Buy, C Byer, RL Cadonati, L Cagnoli, G Cain, J Calloni, E Camp, JB Campagna, E Campsie, P Cannizzo, J Cannon, K Canuel, B Cao, J Capano, C Carbognani, F Caride, S Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Cella, G Cepeda, C Cesarini, E Chalermsongsak, T Chalkley, E Charlton, P Chassande-Mottin, E Chelkowski, S Chen, Y Chincarini, A Christensen, N Chua, SSY Chung, CTY Clark, D Clark, J Clayton, JH Cleva, F Coccia, E Colacino, CN Colas, J Colla, A Colombini, M Conte, R Cook, D Corbitt, TR Cornish, N Corsi, A Costa, CA Coulon, JP Coward, DM Coyne, DC Creighton, JDE Creighton, TD Cruise, AM Culter, RM Cumming, A Cunningham, L Cuoco, E Dahl, K Danilishin, SL Dannenberg, R D'Antonio, S Danzmann, K Das, K Dattilo, V Daudert, B Davier, M Davies, G Davis, A Daw, EJ Day, R Dayanga, T De Rosa, R DeBra, D Degallaix, J del Prete, M Dergachev, V DeRosa, R DeSalvo, R Devanka, P Dhurandhar, S Di Fiore, L Di Lieto, A Di Palma, I Emilio, MD Di Virgilio, A Diaz, M Dietz, A Donovan, F Dooley, KL Doomes, EE Dorsher, S Douglas, ESD Drago, M Drever, RWP Driggers, JC Dueck, J Dumas, JC Eberle, T Edgar, M Edwards, M Effler, A Ehrens, P Engel, R Etzel, T Evans, M Evans, T Fafone, V Fairhurst, S Fan, Y Farr, BF Fazi, D Fehrmann, H Feldbaum, D Ferrante, I Fidecaro, F Finn, LS Fiori, I Flaminio, R Flanigan, M Flasch, K Foley, S Forrest, C Forsi, E Fotopoulos, N Fournier, JD Franc, J Frasca, S Frasconi, F Frede, M Frei, M Frei, Z Freise, A Frey, R Fricke, TT Friedrich, D Fritschel, P Frolov, VV Fulda, P Fyffe, M Galimberti, M Gammaitoni, L Garofoli, JA Garufi, F Gemme, G Genin, E Gennai, A Gholami, I Ghosh, S Giaime, JA Giampanis, S Giardina, KD Giazotto, A Gill, C Goetz, E Goggin, LM Gonzalez, G Gorodetsky, ML Gossler, S Gouaty, R Graef, C Granata, M Grant, A Gras, S Gray, C Greenhalgh, RJS Gretarsson, AM Greverie, C Grosso, R Grote, H Grunewald, S Guidi, GM Gustafson, EK Gustafson, R Hage, B Hall, P Hallam, JM Hammer, D Hammond, G Hanks, J Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Haughian, K Hayama, K Hayau, JF Hayler, T Heefner, J Heitmann, H Hello, P Heng, IS Heptonstall, AW Hewitson, M Hild, S Hirose, E Hoak, D Hodge, KA Holt, K Hosken, DJ Hough, J Howell, EJ Hoyland, D Huet, D Hughey, B Husa, S Huttner, SH Huynh-Dinh, T Ingram, DR Inta, R Isogai, T Ivanov, A Jaranowski, P Johnson, WW Jones, DI Jones, G Jones, R Ju, L Kalmus, P Kalogera, V Kandhasamy, S Kanner, JB Katsavounidis, E Kawabe, K Kawamura, S Kawazoe, F Kells, W Keppel, DG Khalaidovski, A Khalili, FY Khazanov, EA Kim, H King, PJ Kinzel, DL Kissel, JS Klimenko, S Kondrashov, V Kopparapu, R Koranda, S Kowalska, I Kozak, D Krause, T Kringel, V Krishnamurthy, S Krishnan, B Krolak, A Kuehn, G Kullman, J Kumar, R Kwee, P Landry, M Lang, M Lantz, B 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Zweizig, J. CA LIGO Sci Collaboration Virgo Collaboration TI Directional Limits on Persistent Gravitational Waves Using LIGO S5 Science Data SO PHYSICAL REVIEW LETTERS LA English DT Article ID ROTATING NEUTRON-STARS; STRING COSMOLOGY; SPECTRUM AB The gravitational-wave (GW) sky may include nearby pointlike sources as well as stochastic backgrounds. We perform two directional searches for persistent GWs using data from the LIGO S5 science run: one optimized for pointlike sources and one for arbitrary extended sources. Finding no evidence to support the detection of GWs, we present 90% confidence level (C.L.) upper-limit maps of GW strain power with typical values between 2 - 20 x 10(-50) strain(2) Hz(-1) and 5 - 35 x 10(-49) strain(2) Hz(-1) sr(-1) for pointlike and extended sources, respectively. The latter result is the first of its kind. We also set 90% C.L. limits on the narrow-band root-mean-square GW strain from interesting targets including Sco X-1, SN 1987A and the Galactic center as low as approximate to 7 - 10(-25) in the most sensitive frequency range near 160 Hz. C1 [Abadie, J.; Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Anderson, S. B.; Araya, M. C.; Aronsson, M.; Aso, Y.; Ballmer, S.; Betzwieser, J.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cannon, K.; Cepeda, C.; Chalermsongsak, T.; Coyne, D. C.; Dannenberg, R.; Daudert, B.; Dergachev, V.; DeSalvo, R.; Driggers, J. C.; Ehrens, P.; Engel, R.; Etzel, T.; Gustafson, E. K.; Hanna, C.; Heefner, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Kalmus, P.; Kells, W.; Keppel, D. G.; King, P. J.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lindquist, P. E.; Mageswaran, M.; Mailand, K.; Mak, C.; Maros, E.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Mitra, S.; Nash, T.; Ogin, G. H.; Osthelder, C.; Patel, P.; Pedraza, M.; Robertson, N. A.; Sannibale, V.; Searle, A. C.; Seifert, F.; Sengupta, A. S.; Singer, A.; Smith, M. R.; Stochino, A.; Taylor, R.; Torrie, C. I.; Turner, L.; Vass, S.; Villar, A. E.; Wallace, L.; Ward, R. L.; Weinstein, A. J.; Whitcomb, S. E.; Willems, P. A.; Yamamoto, H.; Yeaton-Massey, D.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Babak, S.; Behnke, B.; Gholami, I.; Grunewald, S.; Krishnan, B.; Leaci, P.; Papa, M. A.; Peralta, C.; Radke, T.; Robinson, E. L.; Santamaria, L.; Schutz, B. F.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Allen, B.; Aulbert, C.; Bauchrowitz, J.; Bertolini, A.; Bock, O.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Burmeister, O.; Dahl, K.; Danzmann, K.; Degallaix, J.; Di Palma, I.; Dueck, J.; Eberle, T.; Fehrmann, H.; Frede, M.; Friedrich, D.; Giampanis, S.; Gossler, S.; Graef, C.; Grote, H.; Hewitson, M.; Kawazoe, F.; Khalaidovski, A.; Kim, H.; Kringel, V.; Kuehn, G.; Kullman, J.; Lastzka, N.; Leong, J.; Lueck, H.; Machenschalk, B.; Mehmet, M.; Messenger, C.; Mors, K.; Mossavi, K.; Mueller-Ebhardt, H.; Pareja, M.; Pickenpack, M.; Pletsch, H. J.; Prijatelj, M.; Prix, R.; Puncken, O.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schulz, B.; Steinlechner, S.; Tarabrin, S. P.; Taylor, J. R.; Veltkamp, C.; Wanner, A.; Weinert, M.; Wessels, P.; Westphal, T.; Willke, B.; Winkelmann, L.; Winkler, W.; Yamamoto, K.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Roberts, P.; Summerscales, T. 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Acernese, Fausto/E-4989-2010; Toncelli, Alessandra/A-5352-2012; Gammaitoni, Luca/B-5375-2009; Prato, Mirko/D-8531-2012; OI Coccia, Eugenio/0000-0002-6669-5787; Hallam, Jonathan Mark/0000-0002-7087-0461; Vetrano, Flavio/0000-0002-7523-4296; Nishizawa, Atsushi/0000-0003-3562-0990; calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Sorazu, Borja/0000-0002-6178-3198; Fairhurst, Stephen/0000-0001-8480-1961; Matichard, Fabrice/0000-0001-8982-8418; Milano, Leopoldo/0000-0001-9487-5876; Husa, Sascha/0000-0002-0445-1971; Farr, Ben/0000-0002-2916-9200; Swinkels, Bas/0000-0002-3066-3601; Guidi, Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431; Santamaria, Lucia/0000-0002-5986-0449; Jaranowski, Piotr/0000-0001-8085-3414; Stein, Leo/0000-0001-7559-9597; Pinto, Innocenzo M./0000-0002-2679-4457; Ward, Robert/0000-0001-5503-5241; Vedovato, Gabriele/0000-0001-7226-1320; Ricci, Fulvio/0000-0001-5475-4447; Whelan, John/0000-0001-5710-6576; Gehring, Tobias/0000-0002-4311-2593; mosca, simona/0000-0001-7869-8275; Frasconi, Franco/0000-0003-4204-6587; Sigg, Daniel/0000-0003-4606-6526; Ferrante, Isidoro/0000-0002-0083-7228; Bondu, Francois/0000-0001-6487-5197; Cella, Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167; Frey, Raymond/0000-0003-0341-2636; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; McClelland, David/0000-0001-6210-5842; Vecchio, Alberto/0000-0002-6254-1617; Finn, Lee Samuel/0000-0002-3937-0688; Graef, Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168; Shaddock, Daniel/0000-0002-6885-3494; Postiglione, Fabio/0000-0003-0628-3796; Rocchi, Alessio/0000-0002-1382-9016; Martelli, Filippo/0000-0003-3761-8616; Howell, Eric/0000-0001-7891-2817; Vicere, Andrea/0000-0003-0624-6231; Vocca, Helios/0000-0002-1200-3917; Miao, Haixing/0000-0003-4101-9958; Losurdo, Giovanni/0000-0003-0452-746X; Danilishin, Stefan/0000-0001-7758-7493; Allen, Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; Steinlechner, Sebastian/0000-0003-4710-8548; Pitkin, Matthew/0000-0003-4548-526X; prodi, giovanni/0000-0001-5256-915X; Gorodetsky, Michael/0000-0002-5159-2742; Punturo, Michele/0000-0001-8722-4485; Puppo, Paola/0000-0003-4677-5015; Gemme, Gianluca/0000-0002-1127-7406; Marchesoni, Fabio/0000-0001-9240-6793; Strain, Kenneth/0000-0002-2066-5355; Neri, Igor/0000-0002-9047-9822; Acernese, Fausto/0000-0003-3103-3473; Toncelli, Alessandra/0000-0003-4400-8808; Gammaitoni, Luca/0000-0002-4972-7062; Prato, Mirko/0000-0002-2188-8059; Principe, Maria/0000-0002-6327-0628; Papa, M.Alessandra/0000-0002-1007-5298; Douglas, Ewan/0000-0002-0813-4308; Kanner, Jonah/0000-0001-8115-0577; Aulbert, Carsten/0000-0002-1481-8319; Di Paolo Emilio, Maurizio/0000-0002-9558-3610; PERSICHETTI, GIANLUCA/0000-0001-8424-9791; Freise, Andreas/0000-0001-6586-9901; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Veitch, John/0000-0002-6508-0713; Zweizig, John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517; Pathak, Devanka/0000-0002-1768-8353; Granata, Massimo/0000-0003-3275-1186 FU Australian Research Council; Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Educacion y Ciencia; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Foundation for Fundamental Research on Matter; Polish Ministry of Science and Higher Education; Foundation for Polish Science; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; The National Aeronautics and Space Administration; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P. Sloan Foundation; Netherlands Organisation for Scientific Research FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Educacion y Ciencia, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. NR 27 TC 50 Z9 50 U1 3 U2 40 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD DEC 29 PY 2011 VL 107 IS 27 AR 271102 DI 10.1103/PhysRevLett.107.271102 PG 9 WC Physics, Multidisciplinary SC Physics GA 869PT UT WOS:000298611000007 PM 22243300 ER PT J AU Inostroza, N Huang, XC Lee, TJ AF Inostroza, Natalia Huang, Xinchuan Lee, Timothy J. TI Accurate ab initio quartic force fields of cyclic and bent HC2N isomers SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SHELL COUPLED-CLUSTER; BASIS-SET CONVERGENCE; MOLECULAR-STRUCTURE; VIBRATIONAL FREQUENCIES; SPECTROSCOPIC CONSTANTS; PARAMAGNETIC RESONANCE; ROVIBRATIONAL ENERGIES; PROJECTION OPERATORS; ELECTRON CORRELATION; TRIPLE EXCITATIONS AB Highly correlated ab initio quartic force fields (QFFs) are used to calculate the equilibrium structures and predict the spectroscopic parameters of three HC2N isomers. Specifically, the ground state quasilinear triplet and the lowest cyclic and bent singlet isomers are included in the present study. Extensive treatment of correlation effects were included using the singles and doubles coupled-cluster method that includes a perturbational estimate of the effects of connected triple excitations, denoted as CCSD(T). Dunning's correlation-consistent basis sets cc-pVXZ, X = 3,4,5, were used, and a three-point formula for extrapolation to the one-particle basis set limit was used. Core-correlation and scalar relativistic corrections were also included to yield highly accurate QFFs. The QFFs were used together with second-order perturbation theory (PT) (with proper treatment of Fermi resonances) and variational methods to solve the nuclear Schrodinger equation. The quasilinear nature of the triplet isomer is problematic, and it is concluded that a QFF is not adequate to describe properly all of the fundamental vibrational frequencies and spectroscopic constants (though some constants not dependent on the bending motion are well reproduced by PT). On the other hand, this procedure (a QFF together with either PT or variational methods) leads to highly accurate fundamental vibrational frequencies and spectroscopic constants for the cyclic and bent singlet isomers of HC2N. All three isomers possess significant dipole moments, 3.05 D, 3.06 D, and 1.71 D, for the quasilinear triplet, the cyclic singlet, and the bent singlet isomers, respectively. It is concluded that the spectroscopic constants determined for the cyclic and bent singlet isomers are the most accurate available, and it is hoped that these will be useful in the interpretation of high-resolution astronomical observations or laboratory experiments. (C) 2011 American Institute of Physics. [doi: 10.1063/1.3671389] C1 [Inostroza, Natalia] Univ Chile, Fac Ciencias, Dept Fis, Santiago 3425, Chile. [Inostroza, Natalia; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. RP Lee, TJ (reprint author), NASA, Ames Res Ctr, Mail Stop 245-1, Moffett Field, CA 94035 USA. EM Natalia.p.Inostrozapino@nasa.gov; Xinchuan.Huang-1@nasa.gov; Timothy.J.Lee@nasa.gov RI Inostroza, Natalia/A-1507-2013; HUANG, XINCHUAN/A-3266-2013; Lee, Timothy/K-2838-2012 FU NASA [08-APRA08-0050, 10-APRA10-0096]; NASA/SETI Institute [NNX09AI49A]; Fondecyt [3110007]; NASA Ames Research Center FX T.J.L. and X. H. gratefully acknowledge support from NASA Grant Nos. 08-APRA08-0050 and 10-APRA10-0096. X. H. also acknowledges support from the NASA/SETI Institute Cooperative Agreement NNX09AI49A. N.I. wants to acknowledge the Fondecyt grants 3110007 and P. Fuentealba for helpful advice. Support from Timothy J. Lee and NASA Ames Research Center is also gratefully acknowledged. NR 60 TC 24 Z9 24 U1 0 U2 11 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 28 PY 2011 VL 135 IS 24 AR 244310 DI 10.1063/1.3671389 PN 2011 PG 13 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 870AC UT WOS:000298640500025 PM 22225159 ER PT J AU Hoffman, MJ Catania, GA Neumann, TA Andrews, LC Rumrill, JA AF Hoffman, M. J. Catania, G. A. Neumann, T. A. Andrews, L. C. Rumrill, J. A. TI Links between acceleration, melting, and supraglacial lake drainage of the western Greenland Ice Sheet SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article ID HAUT GLACIER DAROLLA; SUBGLACIAL WATER-PRESSURE; HIGH-VELOCITY EVENT; SURFACE MELT; OUTLET GLACIER; ABLATION ZONE; SWITZERLAND; FLOW; MOTION; SYSTEM AB The impact of increasing summer melt on the dynamics and stability of the Greenland Ice Sheet is not fully understood. Mounting evidence suggests seasonal evolution of subglacial drainage mitigates or counteracts the ability of surface runoff to increase basal sliding. Here, we compare subdaily ice velocity and uplift derived from nine Global Positioning System stations in the upper ablation zone in west Greenland to surface melt and supraglacial lake drainage during summer 2007. Starting around day 173, we observe speedups of 6-41% above spring velocity lasting similar to 40 days accompanied by sustained surface uplift at most stations, followed by a late summer slowdown. After initial speedup, we see a spatially uniform velocity response across the ablation zone and strong diurnal velocity variations during periods of melting. Most lake drainages were undetectable in the velocity record, and those that were detected only perturbed velocities for similar to 1 day, suggesting preexisting drainage systems could efficiently drain large volumes of water. The dynamic response to melt forcing appears to (1) be driven by changes in subglacial storage of water that is delivered in diurnal and episodic pulses, and (2) decrease over the course of the summer, presumably as the subglacial drainage system evolves to greater efficiency. The relationship between hydrology and ice dynamics observed is similar to that observed on mountain glaciers, suggesting that seasonally large water pressures under the ice sheet largely compensate for the greater ice thickness considered here. Thus, increases in summer melting may not guarantee faster seasonal ice flow. C1 [Hoffman, M. J.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Hoffman, M. J.; Neumann, T. A.] NASA, Cryospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Catania, G. A.] Univ Texas Austin, Inst Geophys, Austin, TX 78759 USA. [Catania, G. A.; Andrews, L. C.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA. [Rumrill, J. A.] So Connecticut State Univ, Dept Earth Sci, New Haven, CT 06515 USA. RP Hoffman, MJ (reprint author), Los Alamos Natl Lab, Fluid Dynam Grp, POB 1663, Los Alamos, NM 87545 USA. EM mhoffman@lanl.gov RI Catania, Ginny/B-9787-2008; Neumann, Thomas/D-5264-2012; Andrews, Lauren/D-8274-2017 OI Andrews, Lauren/0000-0003-3727-4737 FU NASA [NNG06GA83G] FX We thank VECO, Michelle Koutnik and Jamin Greenbaum for assistance in the field, Koni Steffen's group at the Cooperative Institute for Research in Environmental Sciences (CIRES) for providing GC-Net weather data, Matt King for advice on processing the GPS data, and Jamie Clark for assistance with Landsat imagery. This work was funded by NASA grant NNG06GA83G to Neumann and Catania. Landsat data are distributed by the U.S. Geological Survey (USGS) Earth Resources Observation and Science (EROS) Center, and MODIS data are distributed by the Land Processes Distributed Active Archive Center (LP DAAC), located at the USGS EROS Center (lpdaac.usgs.gov). We thank three anonymous reviewers for their thoughtful, in-depth reviews that substantially improved the manuscript. NR 71 TC 57 Z9 58 U1 0 U2 34 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD DEC 28 PY 2011 VL 116 AR F04035 DI 10.1029/2010JF001934 PG 16 WC Geosciences, Multidisciplinary SC Geology GA 871RS UT WOS:000298756000001 ER PT J AU Le, G Burke, WJ Pfaff, RF Freudenreich, H Maus, S Luhr, H AF Le, Guan Burke, William J. Pfaff, Robert F. Freudenreich, Henry Maus, Stefan Luehr, Hermann TI C/NOFS measurements of magnetic perturbations in the low-latitude ionosphere during magnetic storms SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID TIME MAGNETOSPHERIC CURRENTS; RING CURRENT; INNER MAGNETOSPHERE; GEOMAGNETIC STORMS; TAIL CURRENT; FIELD; DST; EARTH; DISTURBANCE AB The Vector Electric Field Investigation suite on the C/NOFS satellite includes a fluxgate magnetometer to monitor the Earth's magnetic fields in the low-latitude ionosphere. Measurements yield full magnetic vectors every second over the range of +/- 45,000 nT with a one-bit resolution of 1.37 nT ( 16 bit A/D) in each component. The sensor's primary responsibility is to support calculations of both V x B and E x B with greater accuracy than can be obtained using standard magnetic field models. The data also contain information about large-scale current systems that, when analyzed in conjunction with electric field measurements, promise to significantly expand understanding of equatorial electrodynamics. We first compare in situ measurements with the POMME (Potsdam Magnetic Model of the Earth) model to establish in-flight sensor "calibrations" and to compute magnetic residuals. At low latitudes the residuals are predominately products of the storm time ring current. Since C/NOFS provides a complete coverage of all local times every 97 min, magnetic field data allow studies of the temporal evolution and local time variations of storm time ring current. The analysis demonstrates the feasibility of using instrumented spacecraft in low-inclination orbits to extract a timely proxy for the provisional Dst index and to specify the ring current's evolution. C1 [Le, Guan; Pfaff, Robert F.; Freudenreich, Henry] NASA, Space Weather Lab, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Burke, William J.] USAF, Space Vehicles Directorate, Res Lab, Hanscom AFB, MA 01731 USA. [Burke, William J.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02167 USA. [Maus, Stefan] NOAA, Natl Geophys Data Ctr, Boulder, CO 80305 USA. [Luehr, Hermann] GFZ German Res Ctr Geosci, D-14473 Potsdam, Germany. RP Le, G (reprint author), NASA, Space Weather Lab, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM guan.le@nasa.gov RI Le, Guan/C-9524-2012; Pfaff, Robert/F-5703-2012; OI Le, Guan/0000-0002-9504-5214; Pfaff, Robert/0000-0002-4881-9715; Maus, Stefan/0000-0002-9604-3878 FU Air Force Office of Scientific Research (AFOSR) FX We thank Kenneth Bromund, Steve Martin, and Carmen Liebrecht for assistance in processing the C/NOFS magnetometer data. We thank the World Data Center for Geomagnetism and Space Magnetism at Kyoto University for providing Dst indices. The OMNI data are obtained from the OMNIWeb at National Space Science Data Center, NASA Goddard Space Flight Center. GSFC authors received support from the Air Force Office of Scientific Research (AFOSR) to carry out this research. NR 27 TC 5 Z9 5 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 28 PY 2011 VL 116 AR A12230 DI 10.1029/2011JA017026 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 871TT UT WOS:000298761300006 ER PT J AU Smialek, JL AF Smialek, James L. TI Moisture-Induced TBC Spallation on Turbine Blade Samples SO SURFACE & COATINGS TECHNOLOGY LA English DT Article DE TBC; alumina scales; moisture; hydrogen; oxide-metal adhesion ID THERMAL BARRIER COATINGS AB Delayed failure of TBCs is a widely observed laboratory phenomenon, although many of the early observations went unreported. "The weekend effect" or "DeskTop Spallation" (DTS) is characterized by initial survival of a TBC after accelerated laboratory thermal cycling, followed by failure when exposed to ambient humidity or water. Once initiated, failure can progress to completion quite dramatically in less than a second. To this end, the water drop test and digital video recordings have become useful techniques in studies at NASA (Smialek, Zhu, Cuy), DECHMA (Rudolphi, Renusch, Schutze), and CNRS Toulouse/SNECMA (Deneux, Cadoret, Hervier, Monceau). In the present study the results for a commercial turbine blade, with a standard EB-PVD 7YSZ TBC top coat and Pt-aluminide diffusion bond coat are reported. Cut sections were intermittently oxidized at 1100 degrees, 1150 degrees, and 1200 degrees C and monitored by weight change and visual appearance. Failures were distributed widely over a 5-100 hr time range, decreasing with oxidation temperature. At some opportune times, failure was captured by video recording, documenting the appearance and speed of the moisture-induced spallation process. The failure interfaces exhibited, on the TBC side, alumina scale grains (decorated with Ta-rich oxide particles) and, on the exposed bare metal surface of the blade, imprints from the scale grains (with alumina islands and streamers). The phenomenon is based on moisture-induced delamination at the alumina scale bond coat interface. Cycling damage is a contributing factor as cracking allows access of moisture to this interface, while high strain energy provides the driving force for spallation. It has been proposed that moisture reacts with aluminum in the bond coat and releases hydrogen atoms that 'embrittle' the interface. A modified chemical viewpoint of scale adhesion results, including a negative synergistic effect with interfacial sulfur. Published by Elsevier B.V. C1 NASA Glenn Res Ctr, Washington, DC USA. RP Smialek, JL (reprint author), NASA Glenn Res Ctr, Washington, DC USA. EM James.L.Smialek@grc.nasa.gov NR 15 TC 8 Z9 8 U1 2 U2 14 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 DEC 25 PY 2011 VL 206 IS 7 BP 1577 EP 1585 DI 10.1016/j.surfcoat.2011.07.015 PG 9 WC Materials Science, Coatings & Films; Physics, Applied SC Materials Science; Physics GA 871BB UT WOS:000298711500011 ER PT J AU Mu, M Randerson, JT van der Werf, GR Giglio, L Kasibhatla, P Morton, D Collatz, GJ DeFries, RS Hyer, EJ Prins, EM Griffith, DWT Wunch, D Toon, GC Sherlock, V Wennberg, PO AF Mu, M. Randerson, J. T. van der Werf, G. R. Giglio, L. Kasibhatla, P. Morton, D. Collatz, G. J. DeFries, R. S. Hyer, E. J. Prins, E. M. Griffith, D. W. T. Wunch, D. Toon, G. C. Sherlock, V. Wennberg, P. O. TI Daily and 3-hourly variability in global fire emissions and consequences for atmospheric model predictions of carbon monoxide SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID COLUMN OBSERVING NETWORK; BOREAL FOREST; SATELLITE-OBSERVATIONS; VERTICAL-DISTRIBUTION; RADIATIVE POWER; CENTRAL-AMERICA; SOUTH-AMERICA; NORTH-AMERICA; DIURNAL FIRE; BURNED AREA AB Attribution of the causes of atmospheric trace gas and aerosol variability often requires the use of high resolution time series of anthropogenic and natural emissions inventories. Here we developed an approach for representing synoptic-and diurnal-scale temporal variability in fire emissions for the Global Fire Emissions Database version 3 (GFED3). We disaggregated monthly GFED3 emissions during 2003-2009 to a daily time step using Moderate Resolution Imaging Spectroradiometer (MODIS)-derived measurements of active fires from Terra and Aqua satellites. In parallel, mean diurnal cycles were constructed from Geostationary Operational Environmental Satellite (GOES) Wildfire Automated Biomass Burning Algorithm (WF_ABBA) active fire observations. Daily variability in fires varied considerably across different biomes, with short but intense periods of daily emissions in boreal ecosystems and lower intensity (but more continuous) periods of burning in savannas. These patterns were consistent with earlier field and modeling work characterizing fire behavior dynamics in different ecosystems. On diurnal timescales, our analysis of the GOES WF_ABBA active fires indicated that fires in savannas, grasslands, and croplands occurred earlier in the day as compared to fires in nearby forests. Comparison with Total Carbon Column Observing Network (TCCON) and Measurements of Pollution in the Troposphere (MOPITT) column CO observations provided evidence that including daily variability in emissions moderately improved atmospheric model simulations, particularly during the fire season and near regions with high levels of biomass burning. The high temporal resolution estimates of fire emissions developed here may ultimately reduce uncertainties related to fire contributions to atmospheric trace gases and aerosols. Important future directions include reconciling top-down and bottom up estimates of fire radiative power and integrating burned area and active fire time series from multiple satellite sensors to improve daily emissions estimates. C1 [Mu, M.; Randerson, J. T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Morton, D.; Collatz, G. J.] NASA, Goddard Space Flight Ctr, Biospher Sci Res Code 614 4, Greenbelt, MD 20771 USA. [DeFries, R. S.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Giglio, L.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Griffith, D. W. T.] Univ Wollongong, Sch Chem, Wollongong, NSW 2522, Australia. [Hyer, E. J.] USN, Res Lab, Marine Meteorol Div, Monterey, CA 93943 USA. [Kasibhatla, P.] Duke Univ, Nicholas Sch Environm & Earth Sci, Durham, NC 27708 USA. [Prins, E. M.] Univ Wisconsin, Madison Cooperat Inst Meteorol Satellite Studies, Madison, WI 53706 USA. [Sherlock, V.] Natl Inst Water & Atmospher Res Ltd, Wellington 6021, New Zealand. [Toon, G. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [van der Werf, G. R.] Vrije Univ Amsterdam, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands. [Wunch, D.; Wennberg, P. O.] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. RP Mu, M (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. EM mmu@uci.edu; jranders@uci.edu; guido.van.der.werf@falw.vu.nl; giglio@hermes.geog.umd.edu; psk9@duke.edu; douglas.morton@nasa.gov; george.j.collatz@nasa.gov; rd2402@columbia.edu; edward.hyer@nrlmry.navy.mil; elaine.prins@ssec.wisc.edu; griffith@uow.edu.au; dwunch@caltech.edu; geoffrey.c.toon@jpl.nasa.gov; v.sherlock@niwa.co.nz; wennberg@gps.caltech.edu RI Wennberg, Paul/A-5460-2012; collatz, george/D-5381-2012; Morton, Douglas/D-5044-2012; Hyer, Edward/E-7734-2011; van der Werf, Guido/M-8260-2016; OI Hyer, Edward/0000-0001-8636-2026; van der Werf, Guido/0000-0001-9042-8630; Kasibhatla, Prasad/0000-0003-3562-3737 FU NASA [NNX08AF64G, NNX10AT83G, NNX08A186G]; EU [218793]; Orbiting Carbon Observatory Program [NAS7-03001]; DOE/ARM; Atmospheric CO2 Observations from Space Program; New Zealand Foundation for Research, Science and Technology [CO1X0204, CO1X0406] FX This research was supported by NASA grants NNX08AF64G and NNX10AT83G and the EU Seventh Research Framework Programme (MACC project, contract 218793). The time series described here is publicly available on the Global Fire Emissions Database server (www.globalfiredata.org). We thank E. Lyons for contributing to the development of the daily fire emissions time series. E. J. Hyer and E. Prins acknowledge support from the NASA Interdisciplinary Studies Program. U.S. funding for TCCON comes from NASA's Terrestrial Ecology Program (NNX08A186G), the Orbiting Carbon Observatory Program (NAS7-03001), the DOE/ARM Program and the Atmospheric CO2 Observations from Space Program. Some of the research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The Lauder TCCON measurements were funded by New Zealand Foundation for Research, Science and Technology contracts CO1X0204 and CO1X0406. We thank B. Connor and J. Robinson for their contributions to the Lauder CO time series. NR 110 TC 85 Z9 86 U1 2 U2 31 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 DEC 24 PY 2011 VL 116 AR D24303 DI 10.1029/2011JD016245 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 868AQ UT WOS:000298496300003 ER PT J AU Grin, D Dore, O Kamionkowski, M AF Grin, Daniel Dore, Olivier Kamionkowski, Marc TI Do Baryons Trace Dark Matter in the Early Universe? SO PHYSICAL REVIEW LETTERS LA English DT Article ID MICROWAVE; POLARIZATION; REIONIZATION; ANISOTROPY AB Baryon-density perturbations of large amplitude may exist if they are compensated by dark-matter perturbations such that the total density is unchanged. Primordial abundances and galaxy clusters allow these compensated isocurvature perturbations (CIPs) to have amplitudes as large as similar to 10%. CIPs will modulate the power spectrum of cosmic microwave background (CMB) fluctuations-those due to the usual adiabatic perturbations-as a function of position on the sky. This leads to correlations between different spherical-harmonic coefficients of the temperature and/or polarization maps, and induces polarization B modes. Here, the magnitude of these effects is calculated and techniques to measure them are introduced. While a CIP of this amplitude can be probed on large scales with existing data, forthcoming CMB experiments should improve the sensitivity to CIPs by at least an order of magnitude. C1 [Grin, Daniel] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. [Dore, Olivier; Kamionkowski, Marc] CALTECH, Pasadena, CA 91125 USA. [Dore, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Grin, D (reprint author), Inst Adv Study, Sch Nat Sci, Olden Lane, Princeton, NJ 08540 USA. OI Kamionkowski, Marc/0000-0001-7018-2055 FU NSF [AST-0807044]; DoE [DE-FG03-92-ER40701]; NASA [NNX10AD04G] FX We thank G. Holder, T. L. Smith, M. LoVerde, C. Chiang, K. M. Smith, M. Zaldarriaga, and D. N. Spergel for stimulating conversations. We thank B. Jones and A. Fraisse for providing Spider parameters. D. G. was supported by NSF AST-0807044 and M. K. by DoE DE-FG03-92-ER40701 and NASA NNX10AD04G. Part of this research was carried out at the Jet Propulsion Laboratory, Caltech, under a contract with NASA. NR 25 TC 8 Z9 8 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD DEC 22 PY 2011 VL 107 IS 26 AR 261301 DI 10.1103/PhysRevLett.107.261301 PG 4 WC Physics, Multidisciplinary SC Physics GA 869PA UT WOS:000298609000004 PM 22243148 ER PT J AU Knudsen, DJ Burchill, JK Donovan, EF Uritsky, VM AF Knudsen, D. J. Burchill, J. K. Donovan, E. F. Uritsky, V. M. TI Advection of magnetic energy as a source of power for auroral arcs SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ELECTRIC-FIELDS; CURRENTS; RADAR; ELECTRODYNAMICS; IONOSPHERE; MOTION; MODEL AB We examine the energetics of a system wherein large-scale magnetospheric convection causes plasma to flow across two-dimensional sheets of field-aligned current (FAC). This scenario requires that the FACs be held stationary or move slowly relative to the background flow, for example through their connection to conductivity enhancements in the lower ionosphere. The key result is that plasma convection across quasi-static current sheets at speed V(d) implies cross-field transport of magnetic energy at a rate proportional to V(d)delta B(2)/2 mu(0), where delta B is the magnetic perturbation associated with the FAC. Poynting's theorem shows that this energy is available to enhance the field-aligned component of Poynting flux, to accelerate particles via electric fields, or both. We show that, for nominal values of field-aligned current (similar to 10 mu A/m(2)) and cross-current-sheet convection (similar to 100 m/s), the net field-aligned energy flux made available through cross-field advection can contribute of the order of 1 mW/m(2) to auroral energy fluxes (electromagnetic plus particle), and conceivably can dominate the energy budget in more intense arcs. While our analysis is applied to an idealized, quasi-static, two-dimensional system, the mechanism it illustrates could play an important role in more dynamic and highly-structured auroral forms as well. Citation: Knudsen, D. J., J. K. Burchill, E. F. Donovan, and V. M. Uritsky (2011), Advection of magnetic energy as a source of power for auroral arcs, Geophys. Res. Lett., 38, L24103, doi:10.1029/2011GL049661. C1 [Knudsen, D. J.; Burchill, J. K.; Donovan, E. F.; Uritsky, V. M.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Knudsen, D. J.; Uritsky, V. M.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Knudsen, DJ (reprint author), Univ Calgary, Dept Phys & Astron, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada. EM knudsen@ucalgary.ca OI Donovan, Eric/0000-0002-8557-4155 FU Natural Sciences and Engineering Research Council of Canada FX The authors acknowledge valuable discussions with William Lotko, Scott Boardsen, Tom Moore, and James Slavin. This work was supported in part by the Natural Sciences and Engineering Research Council of Canada. NR 21 TC 4 Z9 4 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 21 PY 2011 VL 38 AR L24103 DI 10.1029/2011GL049661 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 868BQ UT WOS:000298498900001 ER PT J AU Park, RS Asmar, SW Buffington, BB Bills, B Campagnola, S Chodas, PW Folkner, WM Konopliv, AS Petropoulos, AE AF Park, Ryan S. Asmar, Sami W. Buffington, Brent B. Bills, Bruce Campagnola, Stefano Chodas, Paul W. Folkner, William M. Konopliv, Alex S. Petropoulos, Anastassios E. TI Detecting tides and gravity at Europa from multiple close flybys SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID OCEAN; SPACECRAFT AB This paper presents the expected accuracy of the tides and gravity of Europa that can be measured by tracking a spacecraft during close flybys of Europa. A reference trajectory was designed for flyby science observations and consists of a total of 36 flybys of Europa at 100 km altitude. Earth-based Doppler measurements were created during +/- 2 hours of each periapsis passage and were simulated with realistic dynamical and measurement assumptions. The result shows that the degree 2 tidal Love number, k(2), can be estimated to sigma(k2) = 0.045 and sigma(k2) = 0.009 (1-sigma formal uncertainty) assuming X-band and Ka-band tracking capabilities, respectively, which is sufficient to confirm the existence of a global subsurface ocean. Citation: Park, R. S., S. W. Asmar, B. B. Buffington, B. Bills, S. Campagnola, P. W. Chodas, W. M. Folkner, A. S. Konopliv, and A. E. Petropoulos (2011), Detecting tides and gravity at Europa from multiple close flybys, Geophys. Res. Lett., 38, L24202, doi:10.1029/2011GL049842. C1 [Park, Ryan S.; Asmar, Sami W.; Buffington, Brent B.; Bills, Bruce; Campagnola, Stefano; Chodas, Paul W.; Folkner, William M.; Konopliv, Alex S.; Petropoulos, Anastassios E.] Jet Prop Lab, Pasadena, CA 91101 USA. RP Park, RS (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91101 USA. EM ryan.s.park@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 14 TC 3 Z9 3 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 21 PY 2011 VL 38 AR L24202 DI 10.1029/2011GL049842 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 868BQ UT WOS:000298498900004 ER PT J AU Pike, WT Staufer, U Hecht, MH Goetz, W Parrat, D Sykulska-Lawrence, H Vijendran, S Madsen, MB AF Pike, W. T. Staufer, U. Hecht, M. H. Goetz, W. Parrat, D. Sykulska-Lawrence, H. Vijendran, S. Madsen, M. B. TI Quantification of the dry history of the Martian soil inferred from in situ microscopy SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID PARTICLE-SIZE DISTRIBUTION; MARS; FRAGMENTATION; DIVERSITY; MINERALS; DUST AB The particle size distribution (PSD) of a Martian soil sample, a useful indicator of the underlying soil formation processes, has been determined using optical and atomic-force microscopy data acquired by the Phoenix Mars lander. In particular, the presence and fraction of clay-sized particles in the PSD reflects the extent of aqueous interaction with the soil. Two size populations have been identified for the Martian sample: Larger, mostly rounded grains; and small reddish fines, notably with a very low mass proportion in the clay-size range below 2 mu m. These fines reflect the smallest-scale formation processes, and indicate a single method of production for the particles up to 11 mu m, a much larger value than that expected for the aqueous interaction of clay formation; this suggests the fines are predominantly the product of global aeolian weathering under very dry conditions. The proportion of clay-sized soils can be used to estimate that there has been much less than 5,000 years exposure to liquid water over the history of the soil. From the perspective of the PSD, lunar regolith, rather than terrestrial soil, is the best analog to Martian soil. A globally homogenous soil with such a PSD would be an unlikely habitat for the propagation of life on Mars. Citation: Pike, W. T., U. Staufer, M. H. Hecht, W. Goetz, D. Parrat, H. Sykulska-Lawrence, S. Vijendran, and M. B. Madsen (2011), Quantification of the dry history of the Martian soil inferred from in situ microscopy, Geophys. Res. Lett., 38, L24201, doi:10.1029/2011GL049896. C1 [Pike, W. T.; Sykulska-Lawrence, H.; Vijendran, S.] Univ London Imperial Coll Sci Technol & Med, Dept Elect & Elect Engn, London SW7 2AZ, England. [Goetz, W.] Max Planck Inst Solar Syst Res, D-31791 Katlenburg Lindau, Germany. [Hecht, M. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Madsen, M. B.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Staufer, U.; Parrat, D.] Univ Neuchatel, Inst Microtechnol, CH-2002 Neuchatel, Switzerland. [Staufer, U.] Delft Univ Technol, Micro & Nano Engn Lab, Delft, Netherlands. RP Pike, WT (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Elect & Elect Engn, London SW7 2AZ, England. EM michael.h.hecht@jpl.nasa.gov RI Madsen, Morten/D-2082-2011; Staufer, Urs/J-6866-2016 OI Madsen, Morten/0000-0001-8909-5111; Staufer, Urs/0000-0002-3519-6467 FU UK Science and Technology Facilities Council; Danish Research Agency; Wolfermann-Nageli Foundation, Switzerland; Space Center at EPFL, Switzerland; Swiss National Science Foundation; National Aeronautics and Space Administration; Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA FX We dedicate this paper to the late Thomas P. Meloy, whose passion for the physics of particles defined these experiments. We thank T. Akiyama, D. Muller, S. Gautsch, H. R. Hidber, L. Howald, P. Niedermann, S. F. Hviid, J.-M. Morookian, E. Hemmig and C. Charalambos for technical assistance, and Michael Velbel and our reviewers for helpful comments on the earlier versions. Financial support from the UK Science and Technology Facilities Council, the Danish Research Agency, the Wolfermann-Nageli Foundation, Switzerland, the Space Center at EPFL, Switzerland, the Swiss National Science Foundation, and the National Aeronautics and Space Administration is gratefully acknowledged. Part of the research reported here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 31 TC 18 Z9 18 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 21 PY 2011 VL 38 AR L24201 DI 10.1029/2011GL049896 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 868BQ UT WOS:000298498900005 ER PT J AU Ackermann, M Ajello, M Allafort, A Antolini, E Atwood, WB Axelsson, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bloom, ED Bonamente, E Borgland, AW Bottacini, E Bouvier, A Bregeon, J Brigida, M Bruel, P Buehler, R Burnett, TH Buson, S Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cavazzuti, E Cecchi, C Charles, E Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Costamante, L Cutini, S de Angelis, A Palma, F Dermer, CD Digel, SW do Couto e Silva, E Drell, PS Dubois, R Escande, L Favuzzi, C Fegan, SJ Ferrara, EC Finke, J Focke, WB Fortin, P Frailis, M Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giebels, B Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Gustafsson, M Hadasch, D Hayashida, M Hays, E Healey, SE Horan, D Hou, X Hughes, RE Iafrate, G Johannesson, G Johnson, AS Johnson, WN Kamae, T Katagiri, H Kataoka, J Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Madejski, GM Mazziotta, MN McConville, W McEnery, JE Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Moretti, E Morselli, A Moskalenko, IV Murgia, S Nakamori, T Naumann-Godo, M Nolan, PL Norris, JP Nuss, E Ohno, M Ohsugi, T Okumura, A Omodei, N Orienti, M Orlando, E Ormes, JF Ozaki, M Paneque, D Parent, D Pesce-Rollins, M Pierbattista, M Piranomonte, S Piron, F Pivato, G Porter, TA Raino, S Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Ritz, S Rochester, LS Romani, RW Roth, M Sanchez, DA Sbarra, C Scargle, JD Schalk, TL Sgro, C Shaw, MS Siskind, EJ Spandre, G Spinelli, P Strong, AW Suson, DJ Tajima, H Takahashi, H Takahashi, T Tanaka, T Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Torres, DF Tosti, G Troja, E Uchiyama, Y Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Wallace, E Wang, P Winer, BL Wood, DL Wood, KS Zimmer, S AF Ackermann, M. Ajello, M. Allafort, A. Antolini, E. Atwood, W. B. Axelsson, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Bottacini, E. Bouvier, A. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Burnett, T. H. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Charles, E. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Costamante, L. Cutini, S. de Angelis, A. de Palma, F. Dermer, C. D. Digel, S. W. do Couto e Silva, E. Drell, P. S. Dubois, R. Escande, L. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Finke, J. Focke, W. B. Fortin, P. Frailis, M. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giebels, B. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Gustafsson, M. Hadasch, D. Hayashida, M. Hays, E. Healey, S. E. Horan, D. Hou, X. Hughes, R. E. Iafrate, G. Johannesson, G. Johnson, A. S. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Knodlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Madejski, G. M. Mazziotta, M. N. McConville, W. McEnery, J. E. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Moretti, E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Naumann-Godo, M. Nolan, P. L. Norris, J. P. Nuss, E. Ohno, M. Ohsugi, T. Okumura, A. Omodei, N. Orienti, M. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Parent, D. Pesce-Rollins, M. Pierbattista, M. Piranomonte, S. Piron, F. Pivato, G. Porter, T. A. Raino, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Ritz, S. Rochester, L. S. Romani, R. W. Roth, M. Sanchez, D. A. Sbarra, C. Scargle, J. D. Schalk, T. L. Sgro, C. Shaw, M. S. Siskind, E. J. Spandre, G. Spinelli, P. Strong, A. W. Suson, D. J. Tajima, H. Takahashi, H. Takahashi, T. Tanaka, T. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Uchiyama, Y. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Wallace, E. Wang, P. Winer, B. L. Wood, D. L. Wood, K. S. Zimmer, S. TI THE SECOND CATALOG OF ACTIVE GALACTIC NUCLEI DETECTED BY THE FERMI LARGE AREA TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; catalogs; galaxies: active; gamma rays: galaxies ID GAMMA-RAY EMISSION; VLBA CALIBRATOR SURVEY; EXTRAGALACTIC BACKGROUND LIGHT; NRAO PMN SURVEYS; ALL-SKY SURVEY; BL-LACERTAE OBJECTS; ENERGY COSMIC-RAYS; SPECTRUM RADIO-SOURCES; SPACE-TELESCOPE; BLAZAR SEQUENCE AB The second catalog of active galactic nuclei (AGNs) detected by the Fermi Large Area Telescope (LAT) in two years of scientific operation is presented. The second LAT AGN catalog (2LAC) includes 1017 gamma-ray sources located at high Galactic latitudes (vertical bar b vertical bar > 10 degrees) that are detected with a test statistic (TS) greater than 25 and associated statistically with AGNs. However, some of these are affected by analysis issues and some are associated with multiple AGNs. Consequently, we define a Clean Sample which includes 886 AGNs, comprising 395 BL Lacertae objects (BL Lac objects), 310 flat-spectrum radio quasars (FSRQs), 157 candidate blazars of unknown type (i.e., with broadband blazar characteristics but with no optical spectral measurement yet), 8 misaligned AGNs, 4 narrow-line Seyfert 1 (NLS1s), 10 AGNs of other types, and 2 starburst galaxies. Where possible, the blazars have been further classified based on their spectral energy distributions (SEDs) as archival radio, optical, and X-ray data permit. While almost all FSRQs have a synchrotron-peak frequency < 10(14) Hz, about half of the BL Lac objects have a synchrotron-peak frequency > 10(15) Hz. The 2LAC represents a significant improvement relative to the first LAT AGN catalog (1LAC), with 52% more associated sources. The full characterization of the newly detected sources will require more broadband data. Various properties, such as gamma-ray fluxes and photon power-law spectral indices, redshifts, gamma-ray luminosities, variability, and archival radio luminosities and their correlations are presented and discussed for the different blazar classes. The general trends observed in 1LAC are confirmed. C1 [Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; de Angelis, A.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Healey, S. E.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Healey, S. E.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Antolini, E.; Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Antolini, E.; Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Atwood, W. B.; Bouvier, A.; Razzano, M.; Ritz, S.; Schalk, T. L.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Bouvier, A.; Razzano, M.; Ritz, S.; Schalk, T. L.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Axelsson, M.; Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Axelsson, M.; Conrad, J.; Larsson, S.; Moretti, E.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Axelsson, M.; Moretti, E.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Iafrate, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Gustafsson, M.; Rando, R.; Sbarra, C.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Pivato, G.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Monte, C.; Raino, S.; Spinelli, P.] M Merlin Univ Politecn Bari, Dipartimento Fis, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Fortin, P.; Giebels, B.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Burnett, T. H.; Roth, M.; Wallace, E.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cavazzuti, E.; Cutini, S.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Frascati, Italy. [Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Ciprini, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univ & Particules Montpellier, Montpellier, France. [Conrad, J.; Larsson, S.; Zimmer, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [de Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dermer, C. D.; Finke, J.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Escande, L.; Lott, B.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France. [Ferrara, E. C.; Gehrels, N.; Hays, E.; Loparco, F.; McConville, W.; McEnery, J. E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Frailis, M.; Iafrate, G.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Fukazawa, Y.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Hayashida, M.] Kyoto Univ, Grad Sch, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hou, X.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Katagiri, H.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan. [Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knodlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Knodlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France. [Loparco, F.; McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Loparco, F.; McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Moiseev, A. A.] Ctr Res & Explorat Space Sci & Technol CRESST, Greenbelt, MD 20771 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. [Ohno, M.; Okumura, A.; Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Parent, D.; Razzaque, S.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Piranomonte, S.] Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Torres, D. F.] ICREA, Barcelona, Spain. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA. RP Ackermann, M (reprint author), Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. EM elisabetta.cavazzuti@asdc.asi.it; sarac@slac.stanford.edu; charles.dermer@nrl.navy.mil; lott@cenbg.in2p3.fr; gasparrini@asdc.asi.it RI Thompson, David/D-2939-2012; Gehrels, Neil/D-2971-2012; Johnson, Neil/G-3309-2014; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Morselli, Aldo/G-6769-2011; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Funk, Stefan/B-7629-2015; Loparco, Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; OI Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; giglietto, nicola/0000-0002-9021-2888; Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Loparco, Francesco/0000-0002-1173-5673; Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Piranomonte, Silvia/0000-0002-8875-5453; Giordano, Francesco/0000-0002-8651-2394; giommi, paolo/0000-0002-2265-5003; De Angelis, Alessandro/0000-0002-3288-2517; Iafrate, Giulia/0000-0002-6185-8292; Frailis, Marco/0000-0002-7400-2135; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; Rando, Riccardo/0000-0001-6992-818X; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Axelsson, Magnus/0000-0003-4378-8785; Giroletti, Marcello/0000-0002-8657-8852; Moretti, Elena/0000-0001-5477-9097; Cutini, Sara/0000-0002-1271-2924; Berenji, Bijan/0000-0002-4551-772X; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726 FU K. A. Wallenberg Foundation; National Aeronautics and Space Administration FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation.; This work is partly based on optical spectroscopy observations performed at Telescopio Nazionale Galileo, La Palma, Canary Islands (proposal AOT20/09B and AOT21/10A). Part of this work is based on archival data, software or online services provided by the ASI Science Data Center (ASDC). 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. NR 174 TC 325 Z9 329 U1 1 U2 25 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 DEC 20 PY 2011 VL 743 IS 2 AR 171 DI 10.1088/0004-637X/743/2/171 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400073 ER PT J AU Ballard, S Fabrycky, D Fressin, F Charbonneau, D Desert, JM Torres, G Marcy, G Burke, CJ Isaacson, H Henze, C Steffen, JH Ciardi, DR Howell, SB Cochran, WD Endl, M Bryson, ST Rowe, JF Holman, MJ Lissauer, JJ Jenkins, JM Still, M Ford, EB Christiansen, JL Middour, CK Haas, MR Li, J Hall, JR McCauliff, S Batalha, NM Koch, DG Borucki, WJ AF Ballard, Sarah Fabrycky, Daniel Fressin, Francois Charbonneau, David Desert, Jean-Michel Torres, Guillermo Marcy, Geoffrey Burke, Christopher J. Isaacson, Howard Henze, Christopher Steffen, Jason H. Ciardi, David R. Howell, Steven B. Cochran, William D. Endl, Michael Bryson, Stephen T. Rowe, Jason F. Holman, Matthew J. Lissauer, Jack J. Jenkins, Jon M. Still, Martin Ford, Eric B. Christiansen, Jessie L. Middour, Christopher K. Haas, Michael R. Li, Jie Hall, Jennifer R. McCauliff, Sean Batalha, Natalie M. Koch, David G. Borucki, William J. TI THE KEPLER-19 SYSTEM: A TRANSITING 2.2 R-circle plus PLANET AND A SECOND PLANET DETECTED VIA TRANSIT TIMING VARIATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; stars: individual (Kepler-19, KOI-84, KIC 2571238) ID EARTH GJ 1214B; 1ST 4 MONTHS; LIGHT CURVES; TERRESTRIAL PLANETS; EXTRASOLAR PLANETS; BINARY STARS; INITIAL CHARACTERISTICS; TRANSMISSION SPECTRUM; PERIOD VARIATIONS; FALSE POSITIVES AB We present the discovery of the Kepler-19 planetary system, which we first identified from a 9.3 day periodic transit signal in the Kepler photometry. From high-resolution spectroscopy of the star, we find a stellar effective temperature T-eff = 5541 +/- 60 K, a metallicity [Fe/H] = -0.13 +/- 0.06, and a surface gravity log(g) = 4.59 +/- 0.10. We combine the estimate of T-eff and [Fe/H] with an estimate of the stellar density derived from the photometric light curve to deduce a stellar mass of M-star = 0.936 +/- 0.040 M-circle dot and a stellar radius of R-star = 0.850 +/- 0.018 R-circle dot (these errors do not include uncertainties in the stellar models). We rule out the possibility that the transits result from an astrophysical false positive by first identifying the subset of stellar blends that reproduce the precise shape of the light curve. Using the additional constraints from the measured color of the system, the absence of a secondary source in the high-resolution spectrum, and the absence of a secondary source in the adaptive optics imaging, we conclude that the planetary scenario is more than three orders of magnitude more likely than a blend. The blend scenario is independently disfavored by the achromaticity of the transit: we measure a transit depth with Spitzer at 4.5 mu m of 547(-110)(+113) ppm, consistent with the depth measured in the Kepler optical bandpass of 567 +/- 6 ppm (corrected for stellar limb darkening). We determine a physical radius of the planet Kepler-19b of R-p = 2.209 +/- 0.048 R-circle plus; the uncertainty is dominated by uncertainty in the stellar parameters. From radial velocity observations of the star, we find an upper limit on the planet mass of 20.3 M-circle plus, corresponding to a maximum density of 10.4 g cm(-3). We report a significant sinusoidal deviation of the transit times from a predicted linear ephemeris, which we conclude is due to an additional perturbing body in the system. We cannot uniquely determine the orbital parameters of the perturber, as various dynamical mechanisms match the amplitude, period, and shape of the transit timing signal and satisfy the host star's radial velocity limits. However, the perturber in these mechanisms has a period less than or similar to 160 days and mass less than or similar to 6 M-Jup, confirming its planetary nature as Kepler-19c. We place limits on the presence of transits of Kepler-19c in the available Kepler data. C1 [Ballard, Sarah; Fressin, Francois; Charbonneau, David; Desert, Jean-Michel; Torres, Guillermo; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabrycky, Daniel] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Marcy, Geoffrey; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Jenkins, Jon M.; Li, Jie] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Howell, Steven B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Cochran, William D.; Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA. [Hall, Jennifer R.; McCauliff, Sean] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. RP Ballard, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sballard@cfa.harvard.edu FU NASA; W. M. Keck Foundation FX We thank the Spitzer team at IPAC and in particular Nancy Silbermann for scheduling the Spitzer observations of this program. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. 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 thank the many people who generously gave so much of their time to make this mission a success. 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. NR 105 TC 67 Z9 67 U1 5 U2 27 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 200 DI 10.1088/0004-637X/743/2/200 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400102 ER PT J AU Firoz, KA Moon, YJ Park, SH Kudela, K Islam, JN Dorman, LI AF Firoz, Kazi A. Moon, Y. -J. Park, S. -H. Kudela, K. Islam, Jamal N. Dorman, Lev I. TI ON THE POSSIBLE MECHANISMS OF TWO GROUND-LEVEL ENHANCEMENT EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar-terrestrial relations; Sun: X-rays; gamma rays ID CORONAL MASS EJECTIONS; RELATIVISTIC PROTON PRODUCTION; III RADIO-BURSTS; COSMIC-RAYS; SOLAR-FLARE; ACCELERATION; SUN; HELIOSPHERE; PARTICLES; RADIATION AB We have carried out a case study on the possible mechanism of ground-level enhancement (GLE) occurrence. For this, we have considered two GLE events (GLE69 and GLE70) and scrutinized their relationships with simultaneous soft/hard X-rays as well as solar energetic particle (SEP) fluxes of different energy bands. Although most of the energy bands of the flares maintain strong correlations (r >= 0.8) with the GLEs, depending only on this evidence we could not precisely imply that GLEs can be caused by solar flares. So, we have attempted to understand possible relativistic energies of the GLEs, which have been determined by availing the relativistic traversing time and velocities of the particles along the nominal path of Archimedean spiral magnetic field lines. Results suggest that the energy released from accelerated particles in high-energy (gamma-ray) solar flares might sometimes cause the GLE. We found that during hard X-ray flares <= 7MeV, the relativistic energy (<= 0.23 GeV) of GLE69 was much less than 1 GeV whereas during SEP flares >30 MeV the possible relativistic energy of GLE69 amounts to similar to 2.78 GeV, and this makes us believe that GLE69 might be caused by the energy released from particle accelerations in high-energy solar flares. On the contrary, during hard X-ray (<= 7 MeV) as well as gamma-ray solar flares (>30 MeV) the relativistic energy of GLE70 amounts to <=similar to 0.35 GeV, indicating that the GLE70 was presumably not caused by the released energy from accelerated particles in the solar flare. Alternatively, the released energy from particle accelerations in solar radio emission type II burst concomitant coronal-mass-ejection-driven shocks seems to have been responsible for causing the GLE70. C1 [Firoz, Kazi A.; Islam, Jamal N.] Univ Chittagong, Res Ctr Math & Phys Sci, Chittagong 4331, Bangladesh. [Moon, Y. -J.] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi Do, South Korea. [Moon, Y. -J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Park, S. -H.] Korea Astron & Space Sci Inst, Solar & Space Weather Res Grp, Taejon 305348, South Korea. [Kudela, K.] Slovak Acad Sci, Inst Expt Phys, Kosice 04001, Slovakia. [Dorman, Lev I.] Russian Acad Sci, Cosm Ray Dept, NV Pushkov IZMIRAN, Moscow 142190, Russia. [Dorman, Lev I.] Techn & Israel Space Agcy, Cosm Ray & Space Weather Ctr, Emilio Segre Observ, Haifa, Israel. RP Firoz, KA (reprint author), Univ Chittagong, Res Ctr Math & Phys Sci, Chittagong 4331, Bangladesh. RI Moon, Yong-Jae/E-1711-2013; Park, Sung-Hong/K-1578-2014 OI Park, Sung-Hong/0000-0001-9149-6547 FU National Research Foundation of the Republic of Korea [R31-10016]; Ministry of Education, Science, and Technology; Korea Research Foundation [KRF-2008-314-C00158, 20090071744, 20100014501]; Korean Government (MOEHRD); VEGA grant agency [2/0081/10] FX We are grateful to the anonymous reviewer for constructive comments that indeed improved the quality of the paper. Thanks to the PIs of RHESSI/GOES/WIND-WAVES/RSTN/Yohkoh/NOAA/ONM for providing observational data. Special thanks to Professor Brian R. Dennis and Dr. Kim Tolbert for explaining RHESSI instrumentations and commands under the SSW workbench. This work has been financed by the WCU Program (No. R31-10016) through the National Research Foundation of the Republic of Korea funded by the Ministry of Education, Science, and Technology and by the Korea Research Foundation Grant (KRF-2008-314-C00158, 20090071744, and 20100014501) funded by the Korean Government (MOEHRD, Basic Research Promotion Fund). K. K. is supported by VEGA grant agency project 2/0081/10. NR 61 TC 6 Z9 6 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 190 DI 10.1088/0004-637X/743/2/190 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400092 ER PT J AU France, K McCray, R Penton, SV Kirshner, RP Challis, P Laming, JM Bouchet, P Chevalier, R Garnavich, PM Fransson, C Heng, K Larsson, J Lawrence, S Lundqvist, P Panagia, N Pun, CSJ Smith, N Sollerman, J Sonneborn, G Sugerman, B Wheeler, JC AF France, Kevin McCray, Richard Penton, Steven V. Kirshner, Robert P. Challis, Peter Laming, J. Martin Bouchet, Patrice Chevalier, Roger Garnavich, Peter M. Fransson, Claes Heng, Kevin Larsson, Josefin Lawrence, Stephen Lundqvist, Peter Panagia, Nino Pun, Chun S. J. Smith, Nathan Sollerman, Jesper Sonneborn, George Sugerman, Ben Wheeler, J. Craig TI HST-COS OBSERVATIONS OF HYDROGEN, HELIUM, CARBON, AND NITROGEN EMISSION FROM THE SN 1987A REVERSE SHOCK SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; shock waves; supernovae: individual (SN 1987A) ID HUBBLE-SPACE-TELESCOPE; BALMER-DOMINATED SHOCKS; SUPERNOVA REMNANT 1987A; INNER CIRCUMSTELLAR RING; VELOCITY LY-ALPHA; X-RAY; LINE EMISSION; TEMPERATURE EQUILIBRATION; SPECTROGRAPH OBSERVATIONS; MACH NUMBER AB We present the most sensitive ultraviolet observations of Supernova 1987A to date. Imaging spectroscopy from the Hubble Space Telescope-Cosmic Origins Spectrograph shows many narrow (Delta upsilon similar to 300 km s(-1)) emission lines from the circumstellar ring, broad (Delta upsilon similar to 10-20 x 103 km s(-1)) emission lines from the reverse shock, and ultraviolet continuum emission. The high signal-to-noise ratio (>40 per resolution element) broad Ly alpha emission is excited by soft X-ray and EUV heating of mostly neutral gas in the circumstellar ring and outer supernova debris. The ultraviolet continuum at lambda > 1350 angstrom can be explained by H I two-photon (2s (2)S(1/2)-1s (2)S(1/2)) emission from the same region. We confirm our earlier, tentative detection of N V lambda 1240 emission from the reverse shock and present the first detections of broad He II lambda 1640, C IV lambda 1550, and N IV] lambda 1486 emission lines from the reverse shock. The helium abundance in the high-velocity material is He/H = 0.14 +/- 0.06. The N V/H alpha line ratio requires partial ion-electron equilibration (T(e)/T(p) approximate to 0.14-0.35). We find that the N/C abundance ratio in the gas crossing the reverse shock is significantly higher than that in the circumstellar ring, a result that may be attributed to chemical stratification in the outer envelope of the supernova progenitor. The N/C abundance may have been stratified prior to the ring expulsion, or this result may indicate continued CNO processing in the progenitor subsequent to the expulsion of the circumstellar ring. C1 [France, Kevin; Penton, Steven V.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [McCray, Richard] Univ Colorado, JILA, Boulder, CO 80309 USA. [McCray, Richard] NIST, Boulder, CO 80309 USA. [Kirshner, Robert P.; Challis, Peter] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Laming, J. Martin] USN, Res Lab, Washington, DC 20375 USA. [Bouchet, Patrice] DSM IRFU SAp CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Chevalier, Roger] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Garnavich, Peter M.] Univ Notre Dame, Notre Dame, IN 46556 USA. [Fransson, Claes; Larsson, Josefin; Lundqvist, Peter; Sollerman, Jesper] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Heng, Kevin] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Lawrence, Stephen] Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11549 USA. [Panagia, Nino] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Panagia, Nino] INAF CT, Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Pun, Chun S. J.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Sonneborn, George] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sugerman, Ben] Goucher Coll, Dept Phys & Astron, Baltimore, MD 21204 USA. [Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP France, K (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA. EM kevin.france@colorado.edu OI Sollerman, Jesper/0000-0003-1546-6615; /0000-0003-0065-2933; Heng, Kevin/0000-0003-1907-5910 FU NASA [NNX08AC146, NAS5-98043, NAS5-26555]; HST program [GO 12241]; NASA through a grant from the Space Telescope Science Institute [GO-12241] FX We thank Svetozar Zhekov formaking his X-ray shock model available, and K.F. and S.V.P. thank James Green for enjoyable discussions about the spectroscopic imaging capabilities of COS. We thank Dave Arnett for helpful advice regarding progenitor envelope structure. This work was supported by NASA grants NNX08AC146 and NAS5-98043 to the University of Colorado at Boulder. Data were obtained as part of HST program GO 12241. Support for program GO-12241 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. NR 59 TC 11 Z9 11 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 186 DI 10.1088/0004-637X/743/2/186 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400088 ER PT J AU Harding, AK Muslimov, AG AF Harding, Alice K. Muslimov, Alex G. TI PULSAR PAIR CASCADES IN MAGNETIC FIELDS WITH OFFSET POLAR CAPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; gamma rays: stars; magnetic fields; stars: neutron ID GAMMA-RAY PULSARS; LARGE-AREA TELESCOPE; ROTATION-POWERED PULSARS; HIGH-ENERGY EMISSION; X-RAY; MILLISECOND PULSARS; LIGHT CURVES; PARTICLE-ACCELERATION; OUTER MAGNETOSPHERE; RADIO PULSARS AB Neutron star magnetic fields may have polar caps (PCs) that are offset from the dipole axis, through field-line sweepback near the light cylinder or non-symmetric currents within the star. The effects of such offsets on electron-positron pair cascades are investigated, using simple models of dipole magnetic fields with small distortions that shift the PCs by different amounts or directions. Using a Monte Carlo pair cascade simulation, we explore the changes in the pair spectrum, multiplicity, and energy flux across the PC, as well as the trends in pair flux and pair energy flux with spin-down luminosity, L(sd). We also give an estimate of the distribution of heating flux from returning positrons on the PC for different offsets. We find that even modest offsets can produce significant increases in pair multiplicity, especially for pulsars that are near or beyond the pair death lines for centered PCs, primarily because of higher accelerating fields. Pair spectra cover several decades in energy, with the spectral range of millisecond pulsars (MSPs) two orders of magnitude higher than for normal pulsars, and PC offsets allow significant extension of all spectra to lower pair energies. We find that the total PC pair luminosity L(pair) is proportional to L(sd), with L(pair) similar to 10(-3) L(sd) for normal pulsars and L(pair) similar to 10(-2) L(sd) for MSPs. Remarkably, the total PC heating luminosity for even large offsets increases by less than a factor of two, even though the PC area increases by much larger factors, because most of the heating occurs near the magnetic axis. C1 [Harding, Alice K.; Muslimov, Alex G.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Muslimov, Alex G.] Univ Space Res Assoc, CRESST, Columbia, MD 21044 USA. RP Harding, AK (reprint author), NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Harding, Alice/D-3160-2012 FU NASA; Fermi Guest Investigator Program; Universities Space Research Association FX We acknowledge support from the NASA Astrophysics Theory and Fundamental Physics Program, the Fermi Guest Investigator Program, and the Universities Space Research Association. A.K.H. also thanks the Aspen Center for Physics. NR 65 TC 32 Z9 32 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 181 DI 10.1088/0004-637X/743/2/181 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400083 ER PT J AU Huber, D Bedding, TR Stello, D Hekker, S Mathur, S Mosser, B Verner, GA Bonanno, A Buzasi, DL Campante, TL Elsworth, YP Hale, SJ Kallinger, T Aguirre, VS Chaplin, WJ De Ridder, J Garcia, RA Appourchaux, T Frandsen, S Houdek, G Molenda-Zakowicz, J Monteiro, MJPFG Christensen-Dalsgaard, J Gilliland, RL Kawaler, SD Kjeldsen, H Broomhall, AM Corsaro, E Salabert, D Sanderfer, DT Seader, SE Smith, JC AF Huber, D. Bedding, T. R. Stello, D. Hekker, S. Mathur, S. Mosser, B. Verner, G. A. Bonanno, A. Buzasi, D. L. Campante, T. L. Elsworth, Y. P. Hale, S. J. Kallinger, T. Aguirre, V. Silva Chaplin, W. J. De Ridder, J. Garcia, R. A. Appourchaux, T. Frandsen, S. Houdek, G. Molenda-Zakowicz, J. Monteiro, M. J. P. F. G. Christensen-Dalsgaard, J. Gilliland, R. L. Kawaler, S. D. Kjeldsen, H. Broomhall, A. M. Corsaro, E. Salabert, D. Sanderfer, D. T. Seader, S. E. Smith, J. C. TI TESTING SCALING RELATIONS FOR SOLAR-LIKE OSCILLATIONS FROM THE MAIN SEQUENCE TO RED GIANTS USING KEPLER DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: late-type; stars: oscillations; techniques: photometric ID 1ST 4 MONTHS; DELTA-SCUTI; STELLAR OSCILLATIONS; INITIAL CHARACTERISTICS; BOLOMETRIC CORRECTIONS; ASTEROSEISMIC ANALYSIS; RADIUS DETERMINATION; INSTABILITY STRIP; MAGNETIC ACTIVITY; MODE LIFETIMES AB We have analyzed solar-like oscillations in similar to 1700 stars observed by the Kepler Mission, spanning from the main sequence to the red clump. Using evolutionary models, we test asteroseismic scaling relations for the frequency of maximum power (nu(max)), the large frequency separation (Delta nu), and oscillation amplitudes. We show that the difference of the Delta nu-nu(max) relation for unevolved and evolved stars can be explained by different distributions in effective temperature and stellar mass, in agreement with what is expected from scaling relations. For oscillation amplitudes, we show that neither (L/M)(s) scaling nor the revised scaling relation by Kjeldsen & Bedding is accurate for red-giant stars, and demonstrate that a revised scaling relation with a separate luminosity-mass dependence can be used to calculate amplitudes from the main sequence to red giants to a precision of similar to 25%. The residuals show an offset particularly for unevolved stars, suggesting that an additional physical dependency is necessary to fully reproduce the observed amplitudes. We investigate correlations between amplitudes and stellar activity, and find evidence that the effect of amplitude suppression is most pronounced for subgiant stars. Finally, we test the location of the cool edge of the instability strip in the Hertzsprung-Russell diagram using solar-like oscillations and find the detections in the hottest stars compatible with a domain of hybrid stochastically excited and opacity driven pulsation. C1 [Huber, D.; Bedding, T. R.; Stello, D.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Stello, D.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Hekker, S.; Verner, G. A.; Elsworth, Y. P.; Hale, S. J.; Chaplin, W. J.; Broomhall, A. M.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Mathur, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Mosser, B.] Univ Denis, Univ Paris 06, CNRS, Observ Paris,LESIA, F-92195 Meudon, France. [Verner, G. A.] Queen Mary Univ London, Astron Unit, London E1 4NS, England. [Bonanno, A.; Corsaro, E.] INAF, Osservatorio Astrofis Catania, Catania, Italy. [Buzasi, D. L.] Eureka Sci, Oakland, CA 94602 USA. [Campante, T. L.; Monteiro, M. J. P. F. G.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Campante, T. L.; Frandsen, S.; Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, Danish AsteroSeismol Ctr DASC, DK-8000 Aarhus C, Denmark. [Kallinger, T.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Kallinger, T.; Houdek, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Aguirre, V. Silva] Max Planck Inst Astrophys, D-85748 Garching, Germany. [De Ridder, J.] KULeuven, Inst Sterrenkunde, Louvain, Belgium. [Garcia, R. A.] Univ Paris 7 Diderot, Lab AIM, CEA DSM CNRS, IRFU SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France. [Appourchaux, T.] Univ Paris 11, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. [Molenda-Zakowicz, J.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Salabert, D.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice 4, France. [Seader, S. E.; Smith, J. C.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Huber, D (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. EM dhuber@physics.usyd.edu.au RI Monteiro, Mario J.P.F.G./B-4715-2008; Hale, Steven/E-3472-2015; OI Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776; Kawaler, Steven/0000-0002-6536-6367; Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Hale, Steven/0000-0002-6402-8382; Kallinger, Thomas/0000-0003-3627-2561; Bonanno, Alfio/0000-0003-3175-9776; Bedding, Timothy/0000-0001-5943-1460 FU Australian Research Council; Netherlands Organisation for Scientific Research (NWO); National Science Foundation; Austrian FWF [P21205-N16]; polish Ministry [N N203 405139]; NASA FX The authors gratefully acknowledge the Kepler Science Team and everyone involved in the Kepler mission for their tireless efforts which have made this paper possible. Funding for the Kepler Mission is provided by NASA's Science Mission Directorate. We thank V. Antoci for helpful comments on the manuscript and discussions on HD 187547. D. S. and T. R. B. acknowledge support by the Australian Research Council. S. H. acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO). NCAR is partially supported by the National Science Foundation. H. G. acknowledges support by the Austrian FWF Project P21205-N16. J.M.-Z. acknowledges the polish Ministry grant N N203 405139. NR 97 TC 126 Z9 127 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 DEC 20 PY 2011 VL 743 IS 2 AR 143 DI 10.1088/0004-637X/743/2/143 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400045 ER PT J AU Hunana, P Laveder, D Passot, T Sulem, PL Borgogno, D AF Hunana, P. Laveder, D. Passot, T. Sulem, P. L. Borgogno, D. TI REDUCTION OF COMPRESSIBILITY AND PARALLEL TRANSFER BY LANDAU DAMPING IN TURBULENT MAGNETIZED PLASMAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); solar wind; turbulence ID SOLAR-WIND FLUCTUATIONS; PROTON TEMPERATURE ANISOTROPY; WEAKLY COLLISIONAL PLASMAS; MAGNETOHYDRODYNAMIC TURBULENCE; MHD TURBULENCE; ALFVEN-WAVE; INCOMPRESSIBLE MAGNETOHYDRODYNAMICS; DENSITY-FLUCTUATIONS; ASTROPHYSICAL GYROKINETICS; HALL-MAGNETOHYDRODYNAMICS AB Three-dimensional numerical simulations of decaying turbulence in a magnetized plasma are performed using a so-called finite Larmor radius (FLR)-Landau fluid model which incorporates linear Landau damping and FLR corrections. It is shown that compared to simulations of compressible Hall-MHD, linear Landau damping is responsible for significant damping of magnetosonic waves, which is consistent with the linear kinetic theory. Compressibility of the fluid and parallel energy cascade along the ambient magnetic field are also significantly inhibited when the beta parameter is not too small. In contrast with Hall-MHD, the FLR-Landau fluid model can therefore correctly describe turbulence in collisionless plasmas such as solar wind, providing an interpretation for its nearly incompressible behavior. C1 [Hunana, P.; Laveder, D.; Passot, T.; Sulem, P. L.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice 4, France. [Hunana, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Borgogno, D.] Politecn Torino, Dipartimento Energet, I-10138 Turin, Italy. RP Hunana, P (reprint author), Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, BP 4229, F-06304 Nice 4, France. EM peter.hunana@nasa.gov RI Hunana, Peter/H-6239-2012 FU INSU-CNRS "Programme Soleil-Terre"; OCA; NASA; European Community FX The support of INSU-CNRS "Programme Soleil-Terre" is acknowledged. Computations were performed on the Mesocentre SIGAMM machine hosted by the Observatoire de la Cote d'Azur (OCA) and on the JADE cluster of the CINES computational facilities. P. H. was supported by an OCA Poincare fellowship and by the NASA Postdoctoral Program. The work of D. B. was supported by the European Community under the contract of Association between EURATOM and ENEA. The views and opinions expressed herein do not necessarily reflect those of the European Commission. NR 89 TC 14 Z9 14 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 DEC 20 PY 2011 VL 743 IS 2 AR 128 DI 10.1088/0004-637X/743/2/128 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400030 ER PT J AU Kang, MJ Choi, MH Bieging, JH Rho, J Lee, JE Tsai, CW AF Kang, Miju Choi, Minho Bieging, John H. Rho, Jeonghee Lee, Jeong-Eun Tsai, Chao-Wei TI SUBMILLIMETER OBSERVATIONS OF DENSE CLUMPS IN THE INFRARED DARK CLOUD G049.40-00.01 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (G049.40-00.01); ISM: structure; stars: formation ID FORMING COMPLEX W51; MASS STAR-FORMATION; DUST-TEMPERATURE; GALACTIC PLANE; CORES; FRAGMENTATION; CANDIDATES; CLUSTERS; HERSCHEL; CATALOG AB We obtained 350 and 850 mu m continuum maps of the infrared dark cloud G049.40-00.01. Twenty-one dense clumps were identified within G049.40-00.01 based on the 350 mu m continuum map with an angular resolution of about 9 ''.6. We present submillimeter continuum maps and report physical properties of the clumps. The masses of clumps range from 50 to 600 M-circle dot. About 70% of the clumps are associated with bright 24 mu m emission sources, and they may contain protostars. The two most massive clumps show extended, enhanced 4.5 mu m emission indicating vigorous star-forming activity. The clump-size-mass distribution suggests that many of them are forming high-mass stars. G049.40-00.01 contains numerous objects in various evolutionary stages of star formation, from pre-protostellar clumps to H II regions. C1 [Kang, Miju; Choi, Minho] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Bieging, John H.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Rho, Jeonghee] NASA, SOFIA Sci Ctr, USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lee, Jeong-Eun] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Gyeonggi, South Korea. [Tsai, Chao-Wei] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. RP Kang, MJ (reprint author), Korea Astron & Space Sci Inst, 776 Daedeokdaero, Taejon 305348, South Korea. EM mjkang@kasi.re.kr RI Lee , Jeong-Eun/E-2387-2013 FU National Research Foundation of Korea (NRF); Ministry of Education, Science and Technology (MEST) of the Korean government [2011-0015816]; NRF [AST-0540882]; MEST [2011-0004781]; NASA FX We thank Hiroko Shinnaga and Michael Dunham for helpful discussions. M.K. and M.C. were supported by the Core Research Program of the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science and Technology (MEST) of the Korean government (grant number 2011-0015816). J.-E.L. was supported by the Basic Science Research Program through NRF funded by MEST (grant number 2011-0004781). 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. Caltech Submillimeter Observatory (CSO) is supported through NSF grant AST-0540882. NR 44 TC 2 Z9 2 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 198 DI 10.1088/0004-637X/743/2/198 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400100 ER PT J AU Madhusudhan, N Mousis, O Johnson, TV Lunine, JI AF Madhusudhan, Nikku Mousis, Olivier Johnson, Torrence V. Lunine, Jonathan I. TI CARBON-RICH GIANT PLANETS: ATMOSPHERIC CHEMISTRY, THERMAL INVERSIONS, SPECTRA, AND FORMATION CONDITIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: general; planets and satellites: individual (WASP-12b) ID COLLISION-INDUCED ABSORPTION; BRIGHT K-STAR; HOT JUPITERS; SOLAR-SYSTEM; TEMPERATURE INVERSION; EXOPLANET ATMOSPHERES; CHEMICAL-EQUILIBRIUM; EXTRASOLAR PLANETS; INTERSTELLAR ICES; EMISSION-SPECTRUM AB The recent inference of a carbon-rich atmosphere, with C/O >= 1, in the hot Jupiter WASP-12b motivates the exotic new class of carbon-rich planets (CRPs). We report a detailed study of the atmospheric chemistry and spectroscopic signatures of carbon-rich giant (CRG) planets, the possibility of thermal inversions in their atmospheres, the compositions of icy planetesimals required for their formation via core accretion, and the apportionment of ices, rock, and volatiles in their envelopes. Our results show that CRG atmospheres probe a unique region in composition space, especially at high temperature (T). For atmospheres with C/O >= 1, and T greater than or similar to 1400 K in the observable atmosphere, most of the oxygen is bound up in CO, while H(2)O is depleted and CH(4) is enhanced by up to two or three orders of magnitude each, compared to equilibrium compositions with solar abundances (C/O = 0.54). These differences in the spectroscopically dominant species for the different C/O ratios cause equally distinct observable signatures in the spectra. As such, highly irradiated transiting giant exoplanets form ideal candidates to estimate atmospheric C/O ratios and to search for CRPs. We also find that the C/O ratio strongly affects the abundances of TiO and VO, which have been suggested to cause thermal inversions in highly irradiated hot Jupiter atmospheres. A C/O = 1 yields TiO and VO abundances of similar to 100 times lower than those obtained with equilibrium chemistry assuming solar abundances, at P similar to 1 bar. Such a depletion is adequate to rule out thermal inversions due to TiO/VO even in the most highly irradiated hot Jupiters, such as WASP-12b. We estimate the compositions of the protoplanetary disk, the planetesimals, and the envelope of WASP-12b, and the mass of ices dissolved in the envelope, based on the observed atmospheric abundances. Adopting stellar abundances (C/O = 0.44) for the primordial disk composition and low-temperature formation conditions (T less than or similar to 30 K) for WASP-12b lead to a C/O ratio of 0.27 in accreted planetesimals, and, consequently, in the planet's envelope. In contrast, a C/O ratio of 1 in the envelope of WASP-12b requires a substantial depletion of oxygen in the disk, i.e., by a factor of similar to 0.41 for the same formation conditions. This scenario also satisfies the constraints on the C/H and O/H ratios reported for WASP-12b. If, alternatively, hotter conditions prevailed in a stellar composition disk such that only H2O is condensed, the remaining gas can potentially have a C/O similar to 1. However, a high C/O in WASP-12b caused predominantly by gas accretion would preclude superstellar C/H ratios which also fit the data. C1 [Madhusudhan, Nikku] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Mousis, Olivier] Observ Besancon, Inst UTINAM, CNRS UMR 6213, F-25010 Besancon, France. [Johnson, Torrence V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lunine, Jonathan I.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Madhusudhan, N (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. EM nmadhu@astro.princeton.edu FU NASANNX07AG80G; JPL/Spitzer Agreements [1328092, 1348668, 1312647]; CNES; Italian program "Incentivazione alla mobilita' di studiosi straineri e italiani residenti all'estero." FX This study was supported in part by NASA grant NNX07AG80G. N.M. also acknowledges support through JPL/Spitzer Agreements 1328092, 1348668, and 1312647. O.M. acknowledges support from CNES. Most of the work was done while J.I.L. was a Visiting Professor at the University of Rome "Tor Vergata," and his contribution was financed within the scope of the Italian program "Incentivazione alla mobilita' di studiosi straineri e italiani residenti all'estero." N.M. thanks Marc Kuchner, Sara Seager, Drake Deming, Adam Burrows, Julianne Moses, Ruth Murray-Clay, Dimitar Sasselov, Aki Roberge, Adam Showman, Joe Harrington, Geoff Marcy, and Erik Petigura for helpful discussions. NR 75 TC 57 Z9 57 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 191 DI 10.1088/0004-637X/743/2/191 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400093 ER PT J AU Mainzer, A Grav, T Bauer, J Masiero, J McMillan, RS Cutri, RM Walker, R Wright, E Eisenhardt, P Tholen, DJ Spahr, T Jedicke, R Denneau, L DeBaun, E Elsbury, D Gautier, T Gomillion, S Hand, E Mo, W Watkins, J Wilkins, A Bryngelson, GL Molina, AD Desai, S Camus, MG Hidalgo, SL Konstantopoulos, I Larsen, JA Maleszewski, C Malkan, MA Mauduit, JC Mullan, BL Olszewski, EW Pforr, J Saro, A Scotti, JV Wasserman, LH AF Mainzer, A. Grav, T. Bauer, J. Masiero, J. McMillan, R. S. Cutri, R. M. Walker, R. Wright, E. Eisenhardt, P. Tholen, D. J. Spahr, T. Jedicke, R. Denneau, L. DeBaun, E. Elsbury, D. Gautier, T. Gomillion, S. Hand, E. Mo, W. Watkins, J. Wilkins, A. Bryngelson, G. L. Del Pino Molina, A. Desai, S. Gomez Camus, M. Hidalgo, S. L. Konstantopoulos, I. Larsen, J. A. Maleszewski, C. Malkan, M. A. Mauduit, J. -C. Mullan, B. L. Olszewski, E. W. Pforr, J. Saro, A. Scotti, J. V. Wasserman, L. H. TI NEOWISE OBSERVATIONS OF NEAR-EARTH OBJECTS: PRELIMINARY RESULTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: planetary systems; minor planets, asteroids: general; planets and satellites: general; surveys ID THERMAL-MODEL CALIBRATION; INFRARED-SURVEY-EXPLORER; JUPITER-FAMILY COMETS; MAIN-BELT ASTEROIDS; APPROACHING ASTEROIDS; SUFFICIENT SOURCE; DISTRIBUTIONS; HAZARD; METEORITES; PHOTOMETRY AB With the NEOWISE portion of the Wide-field Infrared Survey Explorer (WISE) project, we have carried out a highly uniform survey of the near-Earth object (NEO) population at thermal infrared wavelengths ranging from 3 to 22 mu m, allowing us to refine estimates of their numbers, sizes, and albedos. The NEOWISE survey detected NEOs the same way whether they were previously known or not, subject to the availability of ground-based follow-up observations, resulting in the discovery of more than 130 new NEOs. The survey's uniform sensitivity, observing cadence, and image quality have permitted extrapolation of the 428 near-Earth asteroids (NEAs) detected by NEOWISE during the fully cryogenic portion of the WISE mission to the larger population. We find that there are 981 +/- 19 NEAs larger than 1 km and 20,500 +/- 3000 NEAs larger than 100 m. We show that the Spaceguard goal of detecting 90% of all 1 km NEAs has been met, and that the cumulative size distribution is best represented by a broken power law with a slope of 1.32 +/- 0.14 below 1.5 km. This power-law slope produces similar to 13,200 +/- 1900 NEAs with D > 140 m. Although previous studies predict another break in the cumulative size distribution below D similar to 50-100 m, resulting in an increase in the number of NEOs in this size range and smaller, we did not detect enough objects to comment on this increase. The overall number for the NEA population between 100 and 1000 m is lower than previous estimates. The numbers of near-Earth comets and potentially hazardous NEOs will be the subject of future work. C1 [Mainzer, A.; Bauer, J.; Masiero, J.; Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Grav, T.; Mo, W.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Bauer, J.; Cutri, R. M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Maleszewski, C.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Walker, R.] Monterey Inst Res Astron, Monterey, CA USA. [Wright, E.; Malkan, M. A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Tholen, D. J.; Jedicke, R.; Denneau, L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Spahr, T.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA. [DeBaun, E.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Elsbury, D.] Univ Calif Santa Barbara, Santa Barbara, CA 93103 USA. [Gautier, T.] Cornell Univ, Ithaca, NY 14853 USA. [Gomillion, S.] Embry Riddle Aeronaut Univ, Dept Engn Phys, Daytona Beach, FL 32114 USA. [Hand, E.] Univ Missouri, Dept Mech Engn, Kansas City, MO 64110 USA. [Watkins, J.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Wilkins, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Bryngelson, G. L.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Del Pino Molina, A.; Hidalgo, S. L.] Inst Astrofis Canarias, E-38200 Tenerife, Canary Islands, Spain. [Desai, S.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Gomez Camus, M.] Univ Andres Bello, Fac Ingn, Dept Ciencias Fis, Santiago, Chile. [Konstantopoulos, I.; Mullan, B. L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Larsen, J. A.] USN Acad, Dept Phys, Annapolis, MD 21402 USA. [Mauduit, J. -C.] CALTECH, Infrared Proc & Anal Ctr, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Olszewski, E. W.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Pforr, J.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Saro, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Wasserman, L. H.] Lowell Observ, Flagstaff, AZ 86001 USA. RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM amainzer@jpl.nasa.gov RI Pforr, Janine/J-3967-2015; del Pino Molina, Andres/I-7976-2016; OI Pforr, Janine/0000-0002-3414-8391; del Pino Molina, Andres/0000-0003-4922-5131; Konstantopoulos, Iraklis/0000-0003-2177-0146; Masiero, Joseph/0000-0003-2638-720X; Hidalgo, Sebastian/0000-0002-0002-9298 FU National Aeronautics and Space Administration; Planetary Science Division of the National Aeronautics and Space Administration FX This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. We thank our referee, Dr. Alan Harris of DLR, for his thoughtful comments which materially improved this work. We also thank Dr. Alan Harris of the Space Sciences Institute for useful conversations. We gratefully acknowledge the extraordinary services specific to NEOWISE contributed by the International Astronomical Union's Minor Planet Center, operated by the Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for Astronomical Telegrams, operated by Harvard University. We also thank the worldwide community of dedicated amateur and professional astronomers devoted to minor planet follow-up observations. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 67 TC 98 Z9 98 U1 0 U2 20 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 156 DI 10.1088/0004-637X/743/2/156 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400058 ER PT J AU Mennesson, B Hanot, C Serabyn, E Liewer, K Martin, SR Mawet, D AF Mennesson, B. Hanot, C. Serabyn, E. Liewer, K. Martin, S. R. Mawet, D. TI HIGH-CONTRAST STELLAR OBSERVATIONS WITHIN THE DIFFRACTION LIMIT AT THE PALOMAR HALE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; instrumentation: high angular resolution; stars: individual (alpha Boo, alpha Her, beta Peg, beta And, alpha Ori, rho Per, alpha Aur, chi Cyg) ID CHI-CYGNI; BEAM COMBINER; GIANTS; STARS; LIGHT; VEGA; INTERFEROMETRY; SPECTROSCOPY; CONSTRAINTS; COMPANIONS AB We report on high-accuracy high-resolution (<20 mas) stellar observations obtained with the Palomar Fiber Nuller (PFN), a near-infrared (similar or equal to 2.2 mu m) interferometric coronagraph installed at the Palomar Hale telescope. The PFN uses destructive interference between two elliptical (3m x 1.5m) sub-apertures of the primary to reach high dynamic range inside the diffraction limit of the full telescope. In order to validate the PFN's instrumental approach and its data reduction strategy, based on the newly developed "Null Self-Calibration" (NSC) method, we observed a sample of eight well-characterized bright giants and supergiants. The quantity measured is the source astrophysical null depth, or equivalently the object's visibility at the PFN 3.2m interferometric baseline. For the bare stars alpha Boo, alpha Her, beta And, and alpha Aur, PFN measurements are in excellent agreement with previous stellar photosphere measurements from long baseline interferometry. For the mass-losing stars beta Peg, alpha Ori, rho Per, and chi Cyg, circumstellar emission and/or asymmetries are detected. Overall, these early observations demonstrate the PFN's ability to measure astrophysical null depths below 10(-2) (limited by stellar diameters), with 1 sigma uncertainties as low as a few 10(-4). Such visibility accuracy is unmatched at this spatial resolution in the near-infrared and translates into a contrast better than 10(-3) within the diffraction limit. With further improvements anticipated in 2011/2012, a state-of-the-art infrared science camera and a new extreme adaptive optics system, the PFN should provide a unique tool for the detection of hot debris disks and young self-luminous sub-stellar companions in the immediate vicinity of nearby stars. C1 [Mennesson, B.; Serabyn, E.; Liewer, K.; Martin, S. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hanot, C.] Univ Liege, AEOS, B-4000 Liege, Belgium. [Mawet, D.] European So Observ, Santiago 19, Chile. RP Mennesson, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM bertrand.mennesson@jpl.nasa.gov FU NASA FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. The data presented are based on observations obtained at the Hale Telescope, Palomar Observatory, as part of a continuing collaboration between Caltech, NASA/JPL, and Cornell University. We thank the Palomar Observatory staff for their assistance in mounting the PFN and conducting the observations at the Hale telescope. NR 40 TC 6 Z9 6 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 178 DI 10.1088/0004-637X/743/2/178 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400080 ER PT J AU Noble, SC Krolik, JH Schnittman, JD Hawley, JF AF Noble, Scott C. Krolik, Julian H. Schnittman, Jeremy D. Hawley, John F. TI RADIATIVE EFFICIENCY AND THERMAL SPECTRUM OF ACCRETION ONTO SCHWARZSCHILD BLACK HOLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; magnetohydrodynamics (MHD); radiative transfer; X-rays: binaries ID MICROQUASAR XTE J1550-564; DOMINATED ACCRETION; DISK-ACCRETION; SPIN; SIMULATIONS; EVOLUTION; INSTABILITY; TURBULENCE; TRANSPORT; FLOWS AB Recent general relativistic magnetohydrodynamic (MHD) simulations of accretion onto black holes (BHs) have shown that, contrary to the basic assumptions of the Novikov-Thorne (NT) model, there can be substantial magnetic stress throughout the plunging region. Additional dissipation and radiation can therefore be expected. We use data from a particularly well-resolved simulation of accretion onto a non-spinning BH to compute both the radiative efficiency of such a flow and its spectrum if all emitted light is radiated with a thermal spectrum whose temperature matches the local effective temperature. This disk is geometrically thin enough (H/r similar or equal to 0.06) that little heat is retained in the flow. In terms of light reaching infinity (i.e., after allowance for all relativistic effects and for photon capture by the BH), we find that the radiative efficiency is at least similar or equal to 6%-10% greater than predicted by the NT model (complete radiation of all heat might yield another similar or equal to 6%). We also find that the spectrum more closely resembles the NT prediction for a/M similar or equal to 0.2-0.3 than for the correct value, a/M = 0. As a result, if the spin of a non-spinning BH is inferred by model fitting to an NT model with known BH mass, distance, and inclination, the inferred a/M is too large by similar or equal to 0.2-0.3. C1 [Noble, Scott C.] Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 USA. [Krolik, Julian H.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Schnittman, Jeremy D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hawley, John F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Noble, SC (reprint author), Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 USA. EM scn@astro.rit.edu; jhk@jhu.edu; jeremy.d.schnittman@nasa.gov; jh8h@virginia.edu RI Schnittman, Jeremy/D-3168-2012 FU National Science Foundation (NSF) [AST-0507455, AST-0908336, AST-0908869, AST-1028087]; NASA [NNX09AD14G] FX This work was partially supported by NSF grants AST-0507455 and AST-0908336 (J.H.K.), NASA grant NNX09AD14G and NSF grant AST-0908869 (J.F.H.), and AST-1028087 (S.C.N.). The ThinHR simulation was carried out on the Teragrid Ranger system at the Texas Advance Computing Center, which is supported in part by the National Science Foundation. Some of the post-process ray tracing was run on the Johns Hopkins Homewood High-Performance Computing Center cluster. NR 45 TC 34 Z9 34 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 115 DI 10.1088/0004-637X/743/2/115 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400017 ER PT J AU Parent, D Kerr, M den Hartog, PR Baring, MG DeCesar, ME Espinoza, CM Gotthelf, EV Harding, AK Johnston, S Kaspi, VM Livingstone, M Romani, RW Stappers, BW Watters, K Weltevrede, P Abdo, AA Burgay, M Camilo, F Craig, HA Freire, PCC Giordano, F Guillemot, L Hobbs, G Keith, M Kramer, M Lyne, AG Manchester, RN Noutsos, A Possenti, A Smith, DA AF Parent, D. Kerr, M. den Hartog, P. R. Baring, M. G. DeCesar, M. E. Espinoza, C. M. Gotthelf, E. V. Harding, A. K. Johnston, S. Kaspi, V. M. Livingstone, M. Romani, R. W. Stappers, B. W. Watters, K. Weltevrede, P. Abdo, A. A. Burgay, M. Camilo, F. Craig, H. A. Freire, P. C. C. Giordano, F. Guillemot, L. Hobbs, G. Keith, M. Kramer, M. Lyne, A. G. Manchester, R. N. Noutsos, A. Possenti, A. Smith, D. A. TI OBSERVATIONS OF ENERGETIC HIGH MAGNETIC FIELD PULSARS WITH THE FERMI LARGE AREA TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: stars; pulsars: general; pulsars: individual (PSR J1119-6127, PSR J1718-3718, PSR J1734-3333, PSR J1846-0258) ID GAMMA-RAY PULSARS; SUPERNOVA REMNANT G292.2-0.5; RAPIDLY SPINNING PULSARS; ROTATION-POWERED PULSAR; X-RAY; LIGHT CURVES; OUTER MAGNETOSPHERE; SPACE-TELESCOPE; RADIO-EMISSION; GALACTIC PLANE AB We report the detection of gamma-ray pulsations from the high-magnetic-field rotation-powered pulsar PSR J1119-6127 using data from the Fermi Large Area Telescope. The gamma-ray light curve of PSR J1119-6127 shows a single, wide peak offset from the radio peak by 0.43 +/- 0.02 in phase. Spectral analysis suggests a power law of index 1.0 +/- 0.3(-0.2)(+0.4) with an energy cutoff at 0.8 +/- 0.2(-0.5)(+2.0) GeV. The first uncertainty is statistical and the second is systematic. We discuss the emission models of PSR J1119-6127 and demonstrate that despite the object's high surface magnetic field-near that of magnetars-the field strength and structure in the gamma-ray emitting zone are apparently similar to those of typical young pulsars. Additionally, we present upper limits on the gamma-ray pulsed emission for the magnetically active PSR J1846-0258 in the supernova remnant Kesteven 75 and two other energetic high-B pulsars, PSRs J1718-3718 and J1734-3333. We explore possible explanations for the non-detection of these three objects, including peculiarities in their emission geometry. C1 [Parent, D.; Abdo, A. A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Kerr, M.; den Hartog, P. R.; Romani, R. W.; Watters, K.; Craig, H. A.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Kerr, M.; den Hartog, P. R.; Romani, R. W.; Craig, H. A.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [DeCesar, M. E.; Harding, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [DeCesar, M. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [DeCesar, M. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Espinoza, C. M.; Stappers, B. W.; Weltevrede, P.; Kramer, M.; Lyne, A. G.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Gotthelf, E. V.; Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Johnston, S.; Hobbs, G.; Keith, M.; Manchester, R. N.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Kaspi, V. M.; Livingstone, M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Burgay, M.; Possenti, A.] INAF Cagliari Astron Observ, I-09012 Capoterra, CA, Italy. [Freire, P. C. C.; Guillemot, L.; Kramer, M.; Noutsos, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Giordano, F.] M Merlin Univ Politecn Bari, Dipartimento Fis, I-70126 Bari, Italy. [Giordano, F.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Smith, D. A.] Univ Bordeaux 1, CNRS IN2p3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. RP Parent, D (reprint author), George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. EM dmnparent@gmail.com; kerrm@stanford.edu; hartog@stanford.edu RI Harding, Alice/D-3160-2012; OI Burgay, Marta/0000-0002-8265-4344 FU Commonwealth of Australia; Science and Technology Facilities Council of the United Kingdom FX The Parkes radio telescope is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by the CSIRO. The Lovell Telescope is owned and operated by the University of Manchester as part of the Jodrell Bank Centre for Astrophysics with support from the Science and Technology Facilities Council of the United Kingdom. NR 83 TC 13 Z9 13 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 170 DI 10.1088/0004-637X/743/2/170 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400072 ER PT J AU Pilyavsky, G Mahadevan, S Kane, SR Howard, AW Ciardi, DR de Pree, C Dragomir, D Fischer, D Henry, GW Jensen, ELN Laughlin, G Marlowe, H Rabus, M von Braun, K Wright, JT Wang, XSX AF Pilyavsky, Genady Mahadevan, Suvrath Kane, Stephen R. Howard, Andrew W. Ciardi, David R. de Pree, Chris Dragomir, Diana Fischer, Debra Henry, Gregory W. Jensen, Eric L. N. Laughlin, Gregory Marlowe, Hannah Rabus, Markus von Braun, Kaspar Wright, Jason T. Wang, Xuesong X. TI A SEARCH FOR THE TRANSIT OF HD 168443b: IMPROVED ORBITAL PARAMETERS AND PHOTOMETRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HD 168443); techniques: photometric; techniques: radial velocities ID BROWN-DWARF COMPANIONS; PLANETARY TRANSITS; RADIAL-VELOCITY; TRANSMISSION SPECTRUM; HIPPARCOS PHOTOMETRY; DATA SET; STARS; PRECISION; EXOPLANETS; CALIFORNIA AB The discovery of transiting planets around bright stars holds the potential to greatly enhance our understanding of planetary atmospheres. In this work we present the search for transits of HD 168443b, a massive planet orbiting the bright star HD 168443 (V = 6.92) with a period of 58.11 days. The high eccentricity of the planetary orbit (e = 0.53) significantly enhances the a priori transit probability beyond that expected for a circular orbit, making HD168443 a candidate for our ongoing Transit Ephemeris Refinement and Monitoring Survey. Using additional radial velocities from Keck High Resolution Echelle Spectrometer, we refined the orbital parameters of this multi-planet system and derived a new transit ephemeris for HD 168443b. The reduced uncertainties in the transit window make a photometric transit search practicable. Photometric observations acquired during predicted transit windows were obtained on three nights. Cerro Tololo Inter-American Observatory 1.0 m photometry acquired on 2010 September 7 had the required precision to detect a transit but fell just outside of our final transit window. Nightly photometry from the T8 0.8 m automated photometric telescope at Fairborn Observatory, acquired over a span of 109 nights, demonstrates that HD 168443 is constant on a timescale of weeks. Higher-cadence photometry on 2011 April 28 and June 25 shows no evidence of a transit. We are able to rule out a non-grazing transit of HD 168443b. C1 [Pilyavsky, Genady; Mahadevan, Suvrath; Wright, Jason T.; Wang, Xuesong X.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Mahadevan, Suvrath; Wright, Jason T.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Kane, Stephen R.; Ciardi, David R.; Dragomir, Diana; von Braun, Kaspar] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Howard, Andrew W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Howard, Andrew W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [de Pree, Chris; Marlowe, Hannah] Agnes Scott Coll, Dept Phys & Astron, Decatur, GA 30030 USA. [Dragomir, Diana] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Fischer, Debra] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Jensen, Eric L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Laughlin, Gregory] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Rabus, Markus] Pontificia Univ Catolica Chile, Dept Aston & Astrofis, Santiago 22, Chile. RP Pilyavsky, G (reprint author), Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. EM gcp5017@psu.edu; suvrath@astro.psu.edu RI Kane, Stephen/B-4798-2013; Howard, Andrew/D-4148-2015; OI Fischer, Debra/0000-0003-2221-0861; Howard, Andrew/0000-0001-8638-0320; Dragomir, Diana/0000-0003-2313-467X; Jensen, Eric/0000-0002-4625-7333; Wright, Jason/0000-0001-6160-5888; Ciardi, David/0000-0002-5741-3047 FU Center for Exoplanets and Habitable Worlds; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; NASA; NSF [AST-0721386]; Tennessee State University; Tennessee Centers of Excellence; ALMA-CONICYT [31090015, 31080021] FX This work made use of the SIMBAD database (operated at CDS, Strasbourg, France), NASA's Astrophysics Data System Bibliographic Services, and the NASA Star and Exoplanet Database (NStED). This work was partially supported by funding from the Center for Exoplanets and Habitable Worlds, supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. The authors thank Andres Jordan for providing support for the observations at CTIO. G. W. H. acknowledges support from NASA, NSF, Tennessee State University, and the Tennessee Centers of Excellence Program. E.L.N.J. acknowledges support from NSF Grant AST-0721386. M. R. acknowledges support from ALMA-CONICYT projects 31090015 and 31080021. We thank the referee for insightful comments that helped us to improve this paper. Finally, the authors wish to 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 58 TC 9 Z9 9 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 162 DI 10.1088/0004-637X/743/2/162 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400064 ER PT J AU Smith, RG Charnley, SB Pendleton, YJ Wright, CM Maldoni, MM Robinson, G AF Smith, R. G. Charnley, S. B. Pendleton, Y. J. Wright, C. M. Maldoni, M. M. Robinson, G. TI ON THE FORMATION OF INTERSTELLAR WATER ICE: CONSTRAINTS FROM A SEARCH FOR HYDROGEN PEROXIDE ICE IN MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; ISM: abundances; ISM: clouds; ISM: lines and bands; ISM: molecules; molecular processes ID 3 MICRON SPECTRA; H2O ICE; INFRARED-SPECTROSCOPY; ABSORPTION FEATURES; STAR-FORMATION; DUST GRAINS; DARK CLOUDS; 10 K; OXYGEN; GAS AB Recent surface chemistry experiments have shown that the hydrogenation of molecular oxygen on interstellar dust grains is a plausible formation mechanism, via hydrogen peroxide (H(2)O(2)), for the production of water (H(2)O) ice mantles in the dense interstellar medium. Theoretical chemistry models also predict the formation of a significant abundance of H(2)O(2) ice in grain mantles by this route. At their upper limits, the predicted and experimental abundances are sufficiently high that H(2)O(2) should be detectable in molecular cloud ice spectra. To investigate this further, laboratory spectra have been obtained for H(2)O(2)/H(2)O ice films between 2.5 and 200 mu m, from 10 to 180 K, containing 3%, 30%, and 97% H(2)O(2) ice. Integrated absorbances for all the absorption features in low-temperature H(2)O(2) ice have been derived from these spectra. For identifying H(2)O(2) ice, the key results are the presence of unique features near 3.5, 7.0, and 11.3 mu m. Comparing the laboratory spectra with the spectra of a group of 24 protostars and field stars, all of which have strong H(2)O ice absorption bands, no absorption features are found that can definitely be identified with H(2)O(2) ice. In the absence of definite H(2)O(2) features, the H(2)O(2) abundance is constrained by its possible contribution to the weak absorption feature near 3.47 mu m found on the long-wavelength wing of the 3 mu m H(2)O ice band. This gives an average upper limit for H(2)O(2), as a percentage of H(2)O, of 9% +/- 4%. This is a strong constraint on parameters for surface chemistry experiments and dense cloud chemistry models. C1 [Smith, R. G.; Wright, C. M.; Robinson, G.] Univ New S Wales, Sch Phys Environm & Math Sci, Australian Def Force Acad, Canberra, ACT 2600, Australia. [Charnley, S. B.] NASA, Astrochem Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pendleton, Y. J.] NASA, Lunar Sci Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Maldoni, M. M.] Geosci Australia, Canberra, ACT 2601, Australia. RP Smith, RG (reprint author), Univ New S Wales, Sch Phys Environm & Math Sci, Australian Def Force Acad, Canberra, ACT 2600, Australia. EM r.smith@adfa.edu.au; Steven.B.Charnley@nasa.gov; yvonne.pendleton@nasa.gov; c.wright@adfa.edu.au; g.robinson@adfa.edu.au RI Charnley, Steven/C-9538-2012 FU Australian Research Council [DP0345227]; NASA FX This work would not have been possible without the contribution of Vernon Edge who prepared all of the H2O2/H2O samples and helped in numerous other ways with the experiments. C.M.W. acknowledges support from Australian Research Council Discovery Project DP0345227. S.B.C. acknowledges support from NASA's Exobiology and Evolutionary Biology Program. NR 61 TC 10 Z9 10 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 131 DI 10.1088/0004-637X/743/2/131 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400033 ER PT J AU Trump, JR Weiner, BJ Scarlata, C Kocevski, DD Bell, EF McGrath, EJ Koo, DC Faber, SM Laird, ES Mozena, M Rangel, C Yan, RB Yesuf, H Atek, H Dickinson, M Donley, JL Dunlop, JS Ferguson, HC Finkelstein, SL Grogin, NA Hathi, NP Juneau, S Kartaltepe, JS Koekemoer, AM Nandra, K Newman, JA Rodney, SA Straughn, AN Teplitz, HI AF Trump, Jonathan R. Weiner, Benjamin J. Scarlata, Claudia Kocevski, Dale D. Bell, Eric F. McGrath, Elizabeth J. Koo, David C. Faber, S. M. Laird, Elise S. Mozena, Mark Rangel, Cyprian Yan, Renbin Yesuf, Hassen Atek, Hakim Dickinson, Mark Donley, Jennifer L. Dunlop, James S. Ferguson, Henry C. Finkelstein, Steven L. Grogin, Norman A. Hathi, Nimish P. Juneau, Stephanie Kartaltepe, Jeyhan S. Koekemoer, Anton M. Nandra, Kirpal Newman, Jeffrey A. Rodney, Steven A. Straughn, Amber N. Teplitz, Harry I. TI A CANDELS WFC3 GRISM STUDY OF EMISSION-LINE GALAXIES AT z similar to 2: A MIX OF NUCLEAR ACTIVITY AND LOW-METALLICITY STAR FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: active; galaxies: evolution; quasars: emission lines ID DEEP FIELD-SOUTH; HIGH-REDSHIFT GALAXIES; YALE-CHILE MUSYC; FORMING GALAXIES; GALACTIC NUCLEI; X-RAY; PHYSICAL CONDITIONS; HOST GALAXIES; MULTIWAVELENGTH SURVEY; PHOTOMETRIC REDSHIFTS AB We present Hubble Space Telescope Wide Field Camera 3 (WFC3) slitless grism spectroscopy of 28 emission-line galaxies at z similar to 2, in the GOODS-S region of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. The high sensitivity of these grism observations, with > 1 sigma detections of emission lines to f > 2.5 x 10(-18) erg s(-1) cm(-2), means that the galaxies in the sample are typically similar to 7 times less massive (median M(*) = 10(9.5) M(circle dot)) than previously studied z similar to 2 emission-line galaxies. Despite their lower mass, the galaxies have [O III]/H beta ratios which are very similar to previously studied z similar to 2 galaxies and much higher than the typical emission-line ratios of local galaxies. The WFC3 grism allows for unique studies of spatial gradients in emission lines, and we stack the two-dimensional spectra of the galaxies for this purpose. In the stacked data the [O III] emission line is more spatially concentrated than the H beta emission line with 98.1% confidence. We additionally stack the X-ray data (all sources are individually undetected), and find that the average L([O III])/L(0.5-10) (keV) ratio is intermediate between typical z similar to 0 obscured active galaxies and star-forming galaxies. Together the compactness of the stacked [O III] spatial profile and the stacked X-ray data suggest that at least some of these low-mass, low-metallicity galaxies harbor weak active galactic nuclei. C1 [Trump, Jonathan R.; Kocevski, Dale D.; McGrath, Elizabeth J.; Koo, David C.; Faber, S. M.; Mozena, Mark; Yesuf, Hassen] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Weiner, Benjamin J.; Juneau, Stephanie] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Scarlata, Claudia] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. [Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Laird, Elise S.; Rangel, Cyprian] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Yan, Renbin] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Atek, Hakim; Teplitz, Harry I.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Dickinson, Mark; Kartaltepe, Jeyhan S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Donley, Jennifer L.; Ferguson, Henry C.; Grogin, Norman A.; Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Dunlop, James S.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Finkelstein, Steven L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Hathi, Nimish P.] Carnegie Observ, Pasadena, CA 91101 USA. [Nandra, Kirpal] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Rodney, Steven A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Straughn, Amber N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Trump, JR (reprint author), Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RI Hathi, Nimish/J-7092-2014; OI Hathi, Nimish/0000-0001-6145-5090; Koekemoer, Anton/0000-0002-6610-2048; Bell, Eric/0000-0002-5564-9873 FU NASA [NAS 5-26555]; NASAHST [GO12060.10-A]; Chandra Grant [G08-9129A]; NSF [AST-0808133]; NASA HST [GO 12099] FX Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc., under NASA contract NAS 5-26555.; J.R.T. and the other authors at UC Santa Cruz acknowledge support from NASAHST Grant GO12060.10-A, Chandra Grant G08-9129A, and NSF Grant AST-0808133. We thank Stephanie LaMassa for access to her data and Shelley Wright for helpful discussions. We additionally thank the anonymous referee for helpful commentswhich improved the quality of themanuscript. We thank A. Reiss (P.I.) and his SN team for acquiring the grism data and acknowledge support from NASA HST grant GO 12099. NR 63 TC 37 Z9 37 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 144 DI 10.1088/0004-637X/743/2/144 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400046 ER PT J AU Weisskopf, MC Tennant, AF Yakovlev, DG Harding, A Zavlin, VE O'Dell, SL Elsner, RF Becker, W AF Weisskopf, Martin C. Tennant, Allyn F. Yakovlev, Dmitry G. Harding, Alice Zavlin, Vyacheslav E. O'Dell, Stephen L. Elsner, Ronald F. Becker, Werner TI CHANDRA PHASE-RESOLVED X-RAY SPECTROSCOPY OF THE CRAB PULSAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; ISM: general; stars: individual (Crab Nebula); techniques: spectroscopic; X-rays: stars ID AREA TELESCOPE OBSERVATIONS; FERMI-LAT OBSERVATIONS; NEUTRON-STAR STRUCTURE; VELA PULSAR; ACCRETED ENVELOPES; SYNCHROTRON NEBULA; GEMINGA PULSAR; GAMMA-RAYS; EMISSION; EQUATION AB We present a new study of the X-ray spectral properties of the Crab Pulsar. The superb angular resolution of the Chandra X-Ray Observatory enables distinguishing the pulsar from the surrounding nebulosity. Analysis of the spectrum as a function of pulse phase allows the least-biased measure of interstellar X-ray extinction due primarily to photoelectric absorption and secondarily to scattering by dust grains in the direction of the Crab Nebula. We modify previous findings that the line of sight to the Crab is underabundant in oxygen and provide measurements with improved accuracy and less bias. Using the abundances and cross sections from Wilms et al. we find [O/H] = (5.28 +/- 0.28) x 10(-4) (4.9 x 10(-4) is solar abundance). We also measure for the first time the impact of scattering of flux out of the image by interstellar grains. We find tau(scat) = 0.147 +/- 0.043. Analysis of the spectrum as a function of pulse phase also measures the X-ray spectral index even at pulse minimum-albeit with increasing statistical uncertainty. The spectral variations are, by and large, consistent with a sinusoidal variation. The only significant variation from the sinusoid occurs over the same phase range as some rather abrupt behavior in the optical polarization magnitude and position angle. We also compare these spectral variations to those observed in gamma-rays and conclude that our measurements are both a challenge and a guide to future modeling and will thus eventually help us understand pair cascade processes in pulsar magnetospheres. The data are also used to set new, and less biased, upper limits to the surface temperature of the neutron star for different models of the neutron star atmosphere. We discuss how such data are best connected to theoretical models of neutron star cooling and neutron star interiors. The data restrict the neutrino emission rate in the pulsar core and the amount of light elements in the heat-blanketing envelope. The observations allow the pulsar, irrespective of the composition of its envelope, to have a neutrino emission rate higher than similar to 0.2 of the standard rate of a non-superfluid star cooling via the modified Urca process. The observations also allow the rate to be lower but now with a limited amount of accreted matter in the envelope. C1 [Weisskopf, Martin C.; Tennant, Allyn F.; O'Dell, Stephen L.; Elsner, Ronald F.] NASA, Dept Space Sci, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Yakovlev, Dmitry G.] Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Yakovlev, Dmitry G.] St Petersburg Polytech Univ, Lab Astrophys Objects Extreme Energy Release, St Petersburg 195251, Russia. [Harding, Alice] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zavlin, Vyacheslav E.] NASA, Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. [Becker, Werner] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. RP Weisskopf, MC (reprint author), NASA, Dept Space Sci, Marshall Space Flight Ctr, VP62, Huntsville, AL 35812 USA. RI Harding, Alice/D-3160-2012; OI O'Dell, Stephen/0000-0002-1868-8056 FU Russian Foundation for Basic Research [11-02-00253a, 11-02-12082-ofi-m-2011]; Rosnauka [NSh 3769.2012.2]; Ministry of Education and Science of the Russian Federation [11.G34.31.001] FX We acknowledge our tremendous debt to Leon Van Speybroeck for his remarkable contributions to the development of the Chandra optics, to Harvey Tananbaum for his superb stewardship of the Chandra X-ray Center, and to Steve Murray and Michael Juda for their support in successfully configuring the HRC shutter for this measurement. D.Y. acknowledges support by the Russian Foundation for Basic Research, grants 11-02-00253a and 11-02-12082-ofi-m-2011; Rosnauka, grant NSh 3769.2012.2; and Ministry of Education and Science of the Russian Federation, contract 11.G34.31.001. NR 52 TC 13 Z9 13 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 139 DI 10.1088/0004-637X/743/2/139 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863PO UT WOS:000298178400041 ER PT J AU Livingstone, MA Scholz, P Kaspi, VM Ng, CY Gavriil, FP AF Livingstone, M. A. Scholz, P. Kaspi, V. M. Ng, C. -Y. Gavriil, Fotis P. TI THE SPIN-DOWN OF SWIFT J1822.3-1606: A NEW GALACTIC MAGNETAR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE pulsars: individual (Swift J1822.3-1606); stars: magnetars; stars: neutron; X-rays: bursts ID SOFT GAMMA REPEATER; X-RAY PULSARS; NEUTRON-STARS; 1E 1547.0-5408; SGR 0501+4516; EMISSION; OUTBURST; VARIABILITY; QUIESCENCE; GLITCHES AB On 2011 July 14, a new magnetar candidate, Swift J1822.3-1606, was identified via a rate trigger on the Swift/Burst Alert Telescope. Here we present an initial analysis of the X-ray properties of the source, using data from the Rossi X-ray Timing Explorer, Swift, and the Chandra X-ray Observatory, spanning 2011 July 16-October 8. We measure a precise spin period of P = 8.43771968(6) s and a spin-down rate of (P)over dot = 2.54(22) x 10(-13), at MJD 55761.0, corresponding to an inferred surface dipole magnetic field of B = 4.7(2) x 10(13) G, the second lowest thus far measured for a magnetar, though similar to those of 1E 2259+586 and several high-magnetic field radio pulsars. We show that the flux decay in the 1-10 keV band is best fit by a double exponential with timescales of 9 +/- 1 and 55 +/- 9 days. The pulsed count rate decay in the 2-10 keV band, by contrast, is better fit by a single exponential decay with timescale 15.9 +/- 0.2 days. After increasing from similar to 35% for similar to 20 days after the onset of the outburst, the pulsed fraction in the 2-10 keV band remained constant at similar to 45%. We argue that these properties confirm this source to be a new member of the class of objects known as magnetars. We consider the distribution of magnetar periods and inferred dipole magnetic field strengths, showing that the former appears flat in the 2-12 s range, while the latter appears peaked in the 10(14)-10(15) G range. C1 [Livingstone, M. A.; Scholz, P.; Kaspi, V. M.; Ng, C. -Y.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Gavriil, Fotis P.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Gavriil, Fotis P.] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA. RP Livingstone, MA (reprint author), McGill Univ, Dept Phys, Rutherford Phys Bldg,3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM maggie@physics.mcgill.ca RI Ng, Chi Yung/A-7639-2013 OI Ng, Chi Yung/0000-0002-5847-2612 FU NSERC; FQRNT; CRAQ; CIFAR; Killam Research Fellowship FX We thank the Chandra and Swift teams for scheduling ToO observations. This research utilized data obtained from HEASARC, provided by NASA-GSFC. V.M.K. holds the Lorne Trottier Chair in Astrophysics and Cosmology and a Canada Research Chair. This work is supported by NSERC via a Discovery Grant, by FQRNT and CRAQ, by CIFAR, and a Killam Research Fellowship. C.Y.N. is a Tomlinson and CRAQ postdoctoral fellow. NR 40 TC 14 Z9 14 U1 0 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 20 PY 2011 VL 743 IS 2 AR L38 DI 10.1088/2041-8205/743/2/L38 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 863HD UT WOS:000298152500013 ER PT J AU Morooka, MW Wahlund, JE Eriksson, AI Farrell, WM Gurnett, DA Kurth, WS Persoon, AM Shafiq, M Andre, M Holmberg, MKG AF Morooka, M. W. Wahlund, J. -E. Eriksson, A. I. Farrell, W. M. Gurnett, D. A. Kurth, W. S. Persoon, A. M. Shafiq, M. Andre, M. Holmberg, M. K. G. TI Dusty plasma in the vicinity of Enceladus SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SATURNS MAGNETOSPHERE; ROTATION PERIOD; SOLAR-SYSTEM; ELECTRON-DENSITY; CASSINI RADIO; E-RING; PARTICLES; DYNAMICS AB We present in situ Cassini Radio Plasma Wave Science observations in the vicinity of Enceladus and in the E ring of Saturn that indicate the presence of dusty plasma. The four flybys of Enceladus in 2008 revealed the following cold plasma characteristics: (1) there is a large plasma density (both ions and electrons) within the Enceladus plume region, (2) no plasma wake effect behind Enceladus was detected, (3) electron densities are generally much lower than the ion densities in the E ring (n(e)/n(i) < 0.5) as well as in the plume (n(e)/n(i) < 0.01), and (4) the average bulk ion drift speed is significantly less than the corotation speed and is instead close to the Keplerian speed. These signatures result from half or more of the electrons being attached to dust grains and by the interaction between the surrounding cold plasma and the predominantly negatively charged submicrometer-sized dust grains. The dust and plasma properties estimated from the observations clearly show that the dust-plasma interaction is collective. This strong dust-plasma coupling appears not only in the Enceladus plume but also in the Enceladus torus, typically from about 20 R(E) (similar to 5000 km) north and about 60 R(E) (similar to 15,000 km) south of Enceladus. We also suggest that the dust-plasma interaction in the E ring is the cause of the planetary spin-modulated dynamics of Saturn's magnetosphere at large. C1 [Morooka, M. W.; Wahlund, J. -E.; Eriksson, A. I.; Shafiq, M.; Andre, M.; Holmberg, M. K. G.] Swedish Inst Space Phys, SE-75121 Uppsala, Sweden. [Farrell, W. M.] NASA, Goddard Space Flight Ctr, Planetary Magnetospheres Lab, Greenbelt, MD 20771 USA. [Gurnett, D. A.; Kurth, W. S.; Persoon, A. M.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. RP Morooka, MW (reprint author), Swedish Inst Space Phys, POB 537, SE-75121 Uppsala, Sweden. EM morooka@irfu.se RI Farrell, William/I-4865-2013; OI Kurth, William/0000-0002-5471-6202 FU Swedish National Space Board (SNSB); NASA FX The Swedish National Space Board (SNSB) supports the RPWS/LP instrument on board Cassini, and the research at the University of Iowa is supported by a NASA contract. NR 48 TC 51 Z9 51 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 20 PY 2011 VL 116 AR A12221 DI 10.1029/2011JA017038 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 868SR UT WOS:000298546200001 ER PT J AU Jin, ZH Qiao, YL Wang, YJ Fang, YH Yi, WN AF Jin, Zhonghai Qiao, Yanli Wang, Yingjian Fang, Yonghua Yi, Weining TI A new parameterization of spectral and broadband ocean surface albedo SO OPTICS EXPRESS LA English DT Article ID REFLECTANCE; DEPENDENCE; WHITECAPS; CLIMATE; WATERS AB A simple yet accurate parameterization of spectral and broadband ocean surface albedo has been developed. To facilitate the parameterization and its applications, the albedo is parameterized for the direct and diffuse incident radiation separately, and then each of them is further divided into two components: the contributions from surface and water, respectively. The four albedo components are independent of each other, hence, altering one will not affect the others. Such a designed parameterization scheme is flexible for any future update. Users can simply replace any of the adopted empirical formulations (e.g., the relationship between foam reflectance and wind speed) as desired without a need to change the parameterization scheme. The parameterization is validated by in situ measurements and can be easily implemented into a climate or radiative transfer model. (C) 2011 Optical Society of America C1 [Jin, Zhonghai] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Jin, Zhonghai] NASA, Langley Res Ctr, Hampton, VA 23666 USA. [Qiao, Yanli; Fang, Yonghua; Yi, Weining] Chinese Acad Sci, Anhui Inst Opt & Fine Mech, Key Lab Opt Calibrat & Characterizat, Hefei 230031, Anhui, Peoples R China. [Wang, Yingjian] Chinese Acad Sci, Anhui Inst Opt & Fine Mech, Key Lab Atmospher Composit & Opt Radiat, Hefei 230031, Anhui, Peoples R China. RP Jin, ZH (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA. EM Zhonghai.jin@nasa.gov FU NASA; director foundation FX We thank the CERES COVE team at NASA Langley Center for the observation data. Particularly, Ken Rutledge kindly provided us two years of carefully calibrated data of spectral and broadband irradiances. Mr. Jun Wu helped to prepare some of the figures. We also thank the three anonymous reviewers for their thoughtful comments. The initiation of this study was supported by NASA's CERES project. It was continued and finished at the Hefei Institutes of Physical Science at the Chinese Academy of Sciences (CASHIPS) and supported by the director foundation to the Key Laboratory of Optical Calibration and Characterization at CASHIPS. NR 18 TC 10 Z9 10 U1 1 U2 9 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD DEC 19 PY 2011 VL 19 IS 27 BP 26429 EP 26443 DI 10.1364/OE.19.026429 PG 15 WC Optics SC Optics GA 903WB UT WOS:000301151500058 PM 22274228 ER PT J AU Ji, Q Tsay, SC Lau, KM Hansell, RA Butler, JJ Cooper, JW AF Ji, Q. Tsay, S. -C. Lau, K. M. Hansell, R. A. Butler, J. J. Cooper, J. W. TI A novel nonintrusive method to resolve the thermal dome effect of pyranometers: Radiometric calibration and implications SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID RADIATIVE PROPERTIES; COSINE RESPONSE; AEROSOLS; OFFSET AB Traditionally the calibration equation for pyranometers assumes that the measured solar irradiance is solely proportional to the thermopile's output voltage; therefore, only a single calibration factor is derived. This causes additional measurement uncertainties because it does not capture sufficient information to correctly account for a pyranometer's thermal effect. In our updated calibration equation, temperatures from the pyranometer's dome and case are incorporated to describe the instrument's thermal behavior, and a new set of calibration constants are determined, thereby reducing measurement uncertainties. In this paper, we demonstrate why a pyranometer's uncertainty using the traditional calibration equation is always larger than a few percent, but with the new approach can become much less than 1% after the thermal issue is resolved. The highlighted calibration results are based on NIST traceable light sources under controlled laboratory conditions. The significance of the new approach lends itself to not only avoiding the uncertainty caused by a pyranometer's thermal effect but also the opportunity to better isolate and characterize other instrumental artifacts, such as angular response and nonlinearity of the thermopile, to further reduce additional uncertainties. We also discuss some of the implications, including an example of how the thermal issue can potentially impact climate studies by evaluating aerosol's direct radiative effect using field measurements with and without considering the pyranometer's thermal effect. The results of radiative transfer model simulation show that a pyranometer's thermal effect on solar irradiance measurements at the surface can be translated into a significant alteration of the calculated distribution of solar energy inside the column atmosphere. C1 [Ji, Q.; Hansell, R. A.] Univ Maryland, ESSIC, College Pk, MD 20740 USA. [Ji, Q.; Tsay, S. -C.; Lau, K. M.; Hansell, R. A.; Butler, J. J.; Cooper, J. W.] NASA, Div Earth Sci, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cooper, J. W.] Sigma Space Corp, Lanham, MD 20706 USA. RP Ji, Q (reprint author), Univ Maryland, ESSIC, College Pk, MD 20740 USA. EM qiang.ji-1@nasa.gov RI Lau, William /E-1510-2012; Butler, James/D-4188-2013; Tsay, Si-Chee/J-1147-2014; Hansell, Richard/J-2065-2014 OI Lau, William /0000-0002-3587-3691; FU NASA; NASA Goddard Space Flight Center's Internal Research and Development FX This research is supported by NASA Radiation Science Program, managed by Hal B. Maring. It is also partially supported by the NASA Goddard Space Flight Center's Internal Research and Development. We thank SMARTLabs team for conducting field measurements (see http://smartlabs.gsfc.nasa.gov); CFL team for supporting laboratory calibration (see http://cf.gsfc.nasa.gov); and BORCAL team for providing outdoor calibration (see http://www.nrel.gov/aim/borcal.html). NR 24 TC 9 Z9 9 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 17 PY 2011 VL 116 AR D24105 DI 10.1029/2011JD016466 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 864QU UT WOS:000298255700007 ER PT J AU Kurita, N Noone, D Risi, C Schmidt, GA Yamada, H Yoneyama, K AF Kurita, Naoyuki Noone, David Risi, Camille Schmidt, Gavin A. Yamada, Hiroyuki Yoneyama, Kunio TI Intraseasonal isotopic variation associated with the Madden-Julian Oscillation SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GENERAL-CIRCULATION MODEL; CUMULUS PARAMETERIZATION; WATER-VAPOR; INDIAN-OCEAN; ASIAN DUST; PART I; PRECIPITATION; VARIABILITY; MJO; SIMULATION AB The Madden-Julian Oscillation (MJO) is the dominant mode of intraseasonal variability in the tropical atmosphere. This study examines the evolution of the hydrologic regime from before the onset of the MJO (pre-onset period) to the MJO onset period, using deuterated water vapor (HDO) measurements from the Tropospheric Emission Spectrometer (TES) and from ground-based stations. Ground-based observations reveal a clear transition between high HDO/H2O isotope ratios during the pre-onset period to a period of repeated abrupt decreases in the HDO/H2O isotope ratio associated with intense convection. Each observed minimum in the HDO/H2O ratio corresponded to a maximum in stratiform rainfall fraction, which was derived independently from radar precipitation coverage area. The ground-based observations are consistent with the satellite observations of the HDO/H2O ratio. In order to attribute the mechanisms that bring about the isotopic changes within the MJO convection, an isotope-enabled general circulation model (GCM) constrained by observed meteorological fields was used to simulate this MJO period. The GCM reproduced many of the observed isotopic features that accompanied the onset of an MJO. After the development of deep convection, large-scale stratiform cloud cover appears, and isotope ratios respond, as a consequence of diffusive exchange between stratiform raindrops and the surrounding vapor. In this diffusive exchange process, heavy isotopes tend to become enriched in precipitation and depleted in the surrounding vapor, and thus successive stratiform rainfall results in decreasing isotope values in the middle and lower troposphere. On the basis of these characteristics, isotope tracers can be used to partition stratiform and convective rainfall from observed isotope data and to validate the simulated proportions of convective/stratiform rainfall. C1 [Kurita, Naoyuki; Yamada, Hiroyuki; Yoneyama, Kunio] Japan Agcy Marine Earth Sci & Technol JAMSTEC, Yokosuka, Kanagawa 2370061, Japan. [Noone, David; Risi, Camille] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Noone, David; Risi, Camille] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Schmidt, Gavin A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Kurita, N (reprint author), Japan Agcy Marine Earth Sci & Technol JAMSTEC, 2-15 Natsushima Cho, Yokosuka, Kanagawa 2370061, Japan. EM nkurita@jamstec.go.jp RI Schmidt, Gavin/D-4427-2012; Kurita, Naoyuki/C-6120-2014 OI Schmidt, Gavin/0000-0002-2258-0486; FU Ministry of the Environment, Japan [RF-0083]; NASA [07-NEWS07-0020, NNX08AR23G] FX This research was supported by the Global Environment Research Fund RF-0083 of the Ministry of the Environment, Japan, and by grants from NASA Energy and Water cycle Study (07-NEWS07-0020) and the NASA Atmospheric Composition program (NNX08AR23G). We thank N. Sato for providing the OLR anomaly data, T. Ushiyama for providing the radar echo data, J. Worden for his help in designing the model-TES comparison methodology, D. Brown for his help in the TES data processing, and M. Berkelhammer for editing of this paper. NR 66 TC 43 Z9 43 U1 0 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 17 PY 2011 VL 116 AR D24101 DI 10.1029/2010JD015209 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 864QU UT WOS:000298255700001 ER PT J AU Burlaga, LF Ness, NF Stone, E McDonald, FB AF Burlaga, L. F. Ness, N. F. Stone, E. McDonald, F. B. TI Voyager observations of magnetic fields and cosmic rays in the heliosheath SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MERGED INTERACTION REGIONS; 3-KHZ RADIO EMISSIONS; TERMINATION SHOCK; OUTER HELIOSPHERE; SOLAR-WIND; MODULATION; HELIOPAUSE; SIMULATION; 11-YEAR; AU AB The major features of the profile of >70 MeV/nuc cosmic ray intensity (CRI) observed by Voyager 1 (V1) in the heliosheath from 2005.8-2010.24 are described by the empirical "CR-B" relation as the cumulative effect of variations of the magnetic field strength B. The CRI profile observed by Voyager 2 (V2) from 2008.60 to 2010.28 in the heliosheath is also described by the CR-B relation. On a smaller scale, of the order of a hundred days, a sequence of 3 CRI decreases observed by V1 during 2006 was interpreted as the effect of a propagating interplanetary shock first interacting with the termination shock, then moving past V1, and finally reflecting from the heliopause and propagating back to V1. Our observations show that the second CRI decrease in this sequence began during the passage of a "Global Merged Interaction Region" (GMIR), similar to 40 days after the arrival of the GMIR and its possible shock. The first and third CRI decreases in the sequence were associated with local enhancements of B. The magnetic field observations associated with the second sequence of 3 cosmic ray intensity decreases observed by V1 in 2007/2008 are more difficult to reconcile with the scenario of Webber et al. (2009) and the CR-B relation. The discrepancy might indicate the importance of latitudinal effects. C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McDonald, F. B.] Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. [Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Stone, E.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91109 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA. EM lburlagahsp@verizon.net; nfnudel@yahoo.com; esa@srl.caltech.edu; fmcdonald@umd.edu FU NASA [NASA NNX 07AW09G, NASA NNX 09AT41G] FX T. McClanahan and S. Kramer provided support in the processing of the data. Daniel Berdichevsky computed the zero level offsets for the instruments. N. F. Ness was partially supported by NASA grants NASA NNX 07AW09G and NASA NNX 09AT41G to the Catholic University of America. NR 30 TC 8 Z9 8 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 17 PY 2011 VL 116 AR A12104 DI 10.1029/2011JA016914 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 864TM UT WOS:000298263000003 ER PT J AU Menietti, JD Mutel, RL Christopher, IW Hutchinson, KA Sigwarth, JB AF Menietti, J. D. Mutel, R. L. Christopher, I. W. Hutchinson, K. A. Sigwarth, J. B. TI Simultaneous radio and optical observations of auroral structures: Implications for AKR beaming SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID KILOMETRIC RADIATION; VIKING OBSERVATIONS; CYCLOTRON MASER; SOURCE REGIONS; EMISSION CONE; GENERATION; SATELLITE; MODEL AB Polar spacecraft observations of auroral kilometric radiation (AKR) spectra, combined with simultaneous optical images of the auroral oval at the source foot points, show a strong correlation with discrete auroral features. We discuss several examples of distinctive "V"-shaped profiles in time-frequency AKR spectra for which the time of nadir passage (bottom of V) coincides with the spacecraft crossing field lines connected to discrete auroral arcs. These results support models of AKR emission originating in density cavities with radiation initially confined to a "tangent plane" but strongly refracted upward in a frequency-dependent manner. The inferred spatial distributions of AKR sources are closely coincident with field lines connecting discrete auroral arcs, indicating that discrete arcs are highly correlated with robust AKR emission on the same field lines, as first suggested by Gurnett (1974) several decades ago. C1 [Menietti, J. D.; Mutel, R. L.; Christopher, I. W.; Hutchinson, K. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Sigwarth, J. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Menietti, JD (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. EM john-menietti@uiowa.edu; robert-mutel@uiowa.edu; iver-christopher@uiowa.edu; kent-hutchinson@uiowa.edu FU NSF [ATM-0407155]; NASA [NNX07AI24G]; Goddard Space Flight Center FX We wish to thank J. Barnholdt and K. Kurth for clerical assistance. This work was supported by NSF award ATM-0407155 and by NASA grant NNX07AI24G with Goddard Space Flight Center. We thank R. Dvorsky for providing VIS images with explanation. NR 26 TC 7 Z9 7 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 17 PY 2011 VL 116 AR A12219 DI 10.1029/2011JA017168 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 864TM UT WOS:000298263000006 ER PT J AU Ubelmann, C Fu, LL AF Ubelmann, Clement Fu, Lee-Lueng TI Cyclonic eddies formed at the Pacific tropical instability wave fronts SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID EASTERN EQUATORIAL PACIFIC; LONG WAVES; OCEAN; ATLANTIC; VORTEX; IMPACT; MODEL AB Sea surface temperature images and surface drifter observations are compared to the results from a high-resolution numerical simulation to study the properties of cyclonic eddies generated at the density front of the tropical instability waves in the tropical Pacific Ocean. These cyclonic eddies, of which the diameter is about 30-100 km and the vertical extent is limited to the upper 100 m in depth, have physical characteristics similar to those of smaller submesoscale eddies at the midlatitudes according to the model. They have highly coherent structures below the surface, carrying cold and salty upwelled equatorial water probably rich in marine life. The stretching and tilting of the upper layer of the ocean provides the main mechanism responsible for the intense cyclonic vorticity of the eddies, involving complex evolution of the density field into occluded fronts. C1 [Ubelmann, Clement; Fu, Lee-Lueng] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ubelmann, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM clement.ubelmann@jpl.nasa.gov; lee-lueng.fu@jpl.nasa.gov FU National Aeronautic and Space Administration; Jason-1 Project; OSTM/Jason-2 Project FX The authors thank Dimitris Menemenlis and the ECCO2 Group for their help with setting the model simulation, as well as James C. McWilliams of UCLA for constructive discussions about the frontal processes. The PODAAC center, the GDP Drifter Data Assembly Center, and the NASA Ocean Color Group are acknowledged for providing high-resolution sea surface temperature, drifter, and ocean color observations, respectively. A special thank is addressed to Jorge Vasquez of JPL for fruitful discussions about the SST products. The research presented in the paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautic and Space Administration. Support from the Jason-1 and OSTM/Jason-2 Projects is acknowledged. NR 24 TC 3 Z9 4 U1 2 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC 16 PY 2011 VL 116 AR C12021 DI 10.1029/2011JC007204 PG 11 WC Oceanography SC Oceanography GA 864PV UT WOS:000298253100002 ER PT J AU Grin, D Dore, O Kamionkowski, M AF Grin, Daniel Dore, Olivier Kamionkowski, Marc TI Compensated isocurvature perturbations and the cosmic microwave background SO PHYSICAL REVIEW D LA English DT Article ID PROBE WMAP OBSERVATIONS; INFLATIONARY UNIVERSE SCENARIO; DARK-MATTER COSMOGONY; DIGITAL SKY SURVEY; POWER SPECTRUM; DENSITY PERTURBATIONS; ANISOTROPIES; POLARIZATION; FLUCTUATIONS; CONSTRAINTS AB Measurements of cosmic microwave background (CMB) anisotropies constrain isocurvature fluctuations between photons and nonrelativistic particles to be subdominant to adiabatic fluctuations. Perturbations in the relative number densities of baryons and dark matter, however, are surprisingly poorly constrained. In fact, baryon-density perturbations of fairly large amplitude may exist if they are compensated by dark-matter perturbations, so that the total density remains unchanged. These compensated isocurvature perturbations (CIPs) leave no imprint on the CMB at observable scales, at linear order. B modes in the CMB polarization are generated at reionization through the modulation of the optical depth by CIPs, but this induced polarization is small. The strongest known constraint <= 10% to the CIP amplitude comes from galaxy-cluster baryon fractions. Here, it is shown that modulation of the baryon density by CIPs at and before the decoupling of Thomson scattering at z similar to 1100 gives rise to CMB effects several orders of magnitude larger than those considered before. Polarization B modes are induced, as are correlations between temperature/polarization spherical-harmonic coefficients of different lm. It is shown that the CIP field at the surface of last scatter can be measured with these off-diagonal correlations. The sensitivity of ongoing and future experiments to these fluctuations is estimated. Data from the WMAP, ACT, SPT, and Spider experiments will be sensitive to fluctuations with amplitude similar to 5-10%. The Planck satellite and Polarbear experiment will be sensitive to fluctuations with amplitude similar to 3%. SPTPol, ACTPol, and future space-based polarization methods will probe amplitudes as low as similar to 0.4%-0.6%. In the cosmic-variance limit, the smallest CIPs that could be detected with the CMB are of amplitude similar to 0.05%. C1 [Grin, Daniel] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. [Dore, Olivier; Kamionkowski, Marc] CALTECH, Pasadena, CA 91125 USA. [Dore, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Grin, D (reprint author), Inst Adv Study, Sch Nat Sci, Olden Lane, Princeton, NJ 08540 USA. OI Kamionkowski, Marc/0000-0001-7018-2055 FU Institute for Advanced Study by the National Science Foundation [AST-0807044]; Miller Institute for Basic Research in Science; DoE [DE-FG03-92-ER40701]; NASA [NNX10AD04G]; Gordon Foundation; Betty Moore Foundation FX We acknowledge useful conversations with C. Chiang, C. Dvorkin, G. Holder, M. LoVerde, K. M. Smith, T.L. Smith, D.N. Spergel, and M. Zaldarriaga. We thank B. Jones and A. Fraisse for providing updated parameters for Spider forecasting. D.G. was supported at the Institute for Advanced Study by the National Science Foundation (AST-0807044) and is grateful for the hospitality of the Aspen Center for Physics, where part of this work was completed. M.K. thanks the support of the Miller Institute for Basic Research in Science and the hospitality of the Department of Physics at the University of California, where part of this work was completed. This work was supported at Caltech by DoE DE-FG03-92-ER40701, NASA NNX10AD04G, and the Gordon and Betty Moore 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. NR 98 TC 16 Z9 16 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD DEC 16 PY 2011 VL 84 IS 12 AR 123003 DI 10.1103/PhysRevD.84.123003 PG 21 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 870CJ UT WOS:000298646400001 ER PT J AU Righter, K AF Righter, K. TI Reply to the Comment by Palme et al. on "Prediction of metal-silicate partition coefficients for siderophile elements: An update and assessment of PT conditions for metal-silicate equilibrium during accretion of the Earth" SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article ID DEEP MAGMA-OCEAN; CORE FORMATION; MELT COMPOSITION; HIGH-PRESSURES; NI; TEMPERATURE; NICKEL; COBALT; CONSTRAINTS; FEO C1 NASA, Lyndon B Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA. RP Righter, K (reprint author), NASA, Lyndon B Johnson Space Ctr, Mailcode KT, 2101 NASA Pkwy, Houston, TX 77058 USA. EM kevin.righter-1@nasa.gov NR 25 TC 3 Z9 3 U1 1 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 DEC 15 PY 2011 VL 312 IS 3-4 BP 519 EP 521 DI 10.1016/j.epsl.2011.10.011 PG 3 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 880ID UT WOS:000299399900027 ER PT J AU Li, LM Nixon, CA Achterberg, RK Smith, MA Gorius, NJP Jiang, X Conrath, BJ Gierasch, PJ Simon-Miller, AA Flasar, FM Baines, KH Ingersoll, AP West, RA Vasavada, AR Ewald, SP AF Li, Liming Nixon, Conor A. Achterberg, Richard K. Smith, Mark A. Gorius, Nicolas J. P. Jiang, Xun Conrath, Barney J. Gierasch, Peter J. Simon-Miller, Amy A. Flasar, F. Michael Baines, Kevin H. Ingersoll, Andrew P. West, Robert A. Vasavada, Ashwin R. Ewald, Shawn P. TI The global energy balance of Titan SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID COMPOSITE INFRARED SPECTROMETER; INTERNAL HEAT; ALBEDO; TEMPERATURE; ATMOSPHERE; DYNAMICS; SATURN; PHOTOMETRY; JUPITER; BUDGET AB The global energy budget of planets and their moons is a critical factor to influence the climate change on these objects. Here we report the first measurement of the global emitted power of Titan. Long-term (2004-2010) observations conducted by the Composite Infrared Spectrometer (CIRS) onboard Cassini reveal that the total emitted power by Titan is (2.84 +/- 0.01) x 10(14) watts. Together with previous measurements of the global absorbed solar power of Titan, the CIRS measurements indicate that the global energy budget of Titan is in equilibrium within measurement error. The uncertainty in the absorbed solar energy places an upper limit on the energy imbalance of 6.0%. Citation: Li, L., et al. (2011), The global energy balance of Titan, Geophys. Res. Lett., 38, L23201, doi: 10.1029/2011GL050053. C1 [Li, Liming; Smith, Mark A.; Jiang, Xun] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA. [Nixon, Conor A.; Achterberg, Richard K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Gorius, Nicolas J. P.; Simon-Miller, Amy A.; Flasar, F. Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Conrath, Barney J.; Gierasch, Peter J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Baines, Kevin H.; West, Robert A.; Vasavada, Ashwin R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ingersoll, Andrew P.; Ewald, Shawn P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Li, LM (reprint author), Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA. EM lli7@mail.uh.edu RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; Simon, Amy/C-8020-2012 OI Nixon, Conor/0000-0001-9540-9121; Simon, Amy/0000-0003-4641-6186 FU NASA FX NASA Outer Planets Research Program funded this work. We are grateful for valuable comments and suggestions on this work from Christopher P. McKay and the other anonymous reviewer. NR 30 TC 6 Z9 6 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 15 PY 2011 VL 38 AR L23201 DI 10.1029/2011GL050053 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 864TA UT WOS:000298261800008 ER PT J AU Subramanian, AC Jochum, M Miller, AJ Murtugudde, R Neale, RB Waliser, DE AF Subramanian, Aneesh C. Jochum, Markus Miller, Arthur J. Murtugudde, Raghu Neale, Richard B. Waliser, Duane E. TI The Madden-Julian Oscillation in CCSM4 SO JOURNAL OF CLIMATE LA English DT Article ID INDIAN-SUMMER MONSOON; MJO SIMULATION DIAGNOSTICS; GENERAL-CIRCULATION MODELS; COUPLED EQUATORIAL WAVES; STOCHASTIC MIXING MODEL; EL-NINO; INTRASEASONAL OSCILLATIONS; OCEAN DIPOLE; MOMENTUM TRANSPORT; INTERANNUAL VARIABILITY AB This study assesses the ability of the Community Climate System Model, version 4 (CCSM4) to represent the Madden-Julian oscillation (MJO), the dominant mode of intraseasonal variability in the tropical atmosphere. The U.S. Climate Variability and Predictability (CLIVAR) MJO Working Group's prescribed diagnostic tests are used to evaluate the model's mean state, variance, and wavenumber frequency characteristics in a 20-yr simulation of the intraseasonal variability in zonal winds at 850 hPa (U850) and 200 hPa (U200), and outgoing longwave radiation (OLR). Unlike its predecessor, CCSM4 reproduces a number of aspects of MJO behavior more realistically. The CCSM4 produces coherent, broadbanded, and energetic patterns in eastward-propagating intraseasonal zonal winds and OLR in the tropical Indian and Pacific Oceans that are generally consistent with MJO characteristics. Strong peaks occur in power spectra and coherence spectra with periods between 20 and 100 days and zonal wavenumbers between 1 and 3. Model MJOs, however, tend to be more broadbanded in frequency than in observations. Broad-scale patterns, as revealed in combined EOFs of U850, U200, and OLR, are remarkably consistent with observations and indicate that large-scale convergence convection coupling occurs in the simulated MJO. Relations between MJO in the model and its concurrence with other climate states are also explored. MJO activity (defined as the percentage of time the MJO index exceeds 1.5) is enhanced during El Nino events compared to La Nina events, both in the model and observations. MJO activity is increased during periods of anomalously strong negative meridional wind shear in the Asian monsoon region and also during strong negative Indian Ocean zonal mode states, in both the model and observations. C1 [Subramanian, Aneesh C.; Miller, Arthur J.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Jochum, Markus; Neale, Richard B.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Murtugudde, Raghu] Univ Maryland, College Pk, MD 20742 USA. [Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Subramanian, AC (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM acsubram@ucsd.edu RI jochum, markus/F-8237-2013; jochum, markus/C-2960-2015; Subramanian, Aneesh/D-9484-2017 OI jochum, markus/0000-0003-2690-3139; Subramanian, Aneesh/0000-0001-7805-0102 FU ONR [N00014-10-1-0541]; NOAA; DOE [25322A]; NSF [OCE06-47815]; SUNNY FX This research forms a part of the Ph.D. dissertation of AS. We gratefully acknowledge funding from ONR (Grant N00014-10-1-0541), NOAA (Grant NA17RJ1231 through ECPC), DOE (Grant 25322A), and NSF (Grant OCE06-47815). The views expressed herein are those of the authors and do not necessarily reflect the views of these agencies. This research was initiated during a visit by AS to NCAR funded by the SUNNY (Scripps/UCSD/NCAR's New and Young) Program. AS acknowledges NCAR's computational support for simulations conducted for this study. We thank Paul Roundy and the other two referees for their careful reviews and important comments that significantly improved the manuscript. We also thank Mitch Moncrieff for his erudite comments and criticism of this work. AS extends heartfelt thanks to Dennis Shea for his help with NCL and for providing some of the observational data used in this analysis, and to Bruce Cornuelle for his many invaluable gems of wisdom on science and data analysis. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 87 TC 37 Z9 38 U1 1 U2 12 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD DEC 15 PY 2011 VL 24 IS 24 BP 6261 EP 6282 DI 10.1175/JCLI-D-11-00031.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 863XJ UT WOS:000298201300001 ER PT J AU Wong, S Fetzer, EJ Kahn, BH Tian, BJ Lambrigtsen, BH Ye, HC AF Wong, Sun Fetzer, Eric J. Kahn, Brian H. Tian, Baijun Lambrigtsen, Bjorn H. Ye, Hengchun TI Closing the Global Water Vapor Budget with AIRS Water Vapor, MERRA Reanalysis, TRMM and GPCP Precipitation, and GSSTF Surface Evaporation SO JOURNAL OF CLIMATE LA English DT Article ID HEATING PROFILES; SATELLITE; VALIDATION; MOISTURE; TEMPERATURE; RETRIEVALS; PACIFIC; FLUXES; OCEANS AB The authors investigate if atmospheric water vapor from remote sensing retrievals obtained from the Atmospheric Infrared Sounder/Advanced Microwave Sounding Unit (AIRS) and the water vapor budget from the NASA Goddard Space Flight Center (GSFC) Modern Era Retrospective-analysis for Research and Applications (MERRA) are physically consistent with independently synthesized precipitation data from the 'rropical Rainfall Measuring Mission (TRMM) or the Global Precipitation Climatology Project (GPCP) and evaporation data from the Goddard Satellite-based Surface Turbulent Fluxes (GSSTF). The atmospheric total water vapor sink (Sigma) is estimated from AIRS water vapor retrievals with MERRA winds (AIRS-MERRA Sigma) as well as directly from the MER RA water vapor budget (MERRA-MERRA Sigma). The global geographical distributions as well as the regional wavelet amplitude spectra of Sigma are then compared with those of TRMM or GPCP precipitation minus GSSTF surface evaporation (TRMM-GSSTF and GPCP GSSTF P - E, respectively). The AIRS-MERRA and MERRA-MERRA Sigma s reproduce the main large-scale patterns of global P - E, including the locations and variations of the ITCZ, summertime monsoons, and midlatitude storm tracks in both hemispheres. The spectra of regional temporal variations in Sigma are generally consistent with those of observed P - E. including the annual and semiannual cycles, and intraseasonal variations. Both AIRS MERRA and MERRA MERRA Sigma s have smaller amplitudes for the intraseasonal variations over the tropical oceans. The MERRA P - E has spectra similar to that of MERRA MERRA Sigma in most of the regions except in tropical Africa. The averaged TRMM GSSTF and GPCP GSSTF P - E over the ocean are more negative compared to the AIRS MERRA, MERRA MERRA Sigma s, and MERRA P - E. C1 [Wong, Sun; Fetzer, Eric J.; Kahn, Brian H.; Tian, Baijun; Lambrigtsen, Bjorn H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ye, Hengchun] Calif State Univ Los Angeles, Dept Geog & Urban Anal, Los Angeles, CA 90032 USA. RP Wong, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sun.wong@jpl.nasa.gov RI Tian, Baijun/A-1141-2007 OI Tian, Baijun/0000-0001-9369-2373 FU JPL AIRS; NASA Energy and Water Cycle Study (NEWS); NASA MEaSUREs FX We thank Michael Bosilovich at NASA Goddard Space Flight Center for the discussion about the MERRA water vapor product. We are grateful to Chung-Lin Shie at NASA Goddard Space Flight Center for the discussion of the usage of GSSTF2b data. We thank NASA Making Earth Science Data Records for Use in Research Environments (MEaSUREs) for supporting the data, and Goddard Earth Sciences Data and Information Services Center (GES DISC) for distributing the data used in this work. The AIRS, MERRA, TRMM 3B42, and GSSTF2b datasets used in this work can be downloaded from GES DISC. (The GPCP data can be downloaded from the Web site http://precip.gsfc.nasa.gov.) We also thank three anonymous reviewers for comments that improved the manuscript. The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This work is supported by the JPL AIRS project, NASA Energy and Water Cycle Study (NEWS), and NASA MEaSUREs. NR 37 TC 18 Z9 18 U1 2 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 DEC 15 PY 2011 VL 24 IS 24 BP 6307 EP 6321 DI 10.1175/2011JCLI4154.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 863XJ UT WOS:000298201300003 ER PT J AU Reichle, RH Koster, RD De Lannoy, GJM Forman, BA Liu, Q Mahanama, SPP Toure, A AF Reichle, Rolf H. Koster, Randal D. De Lannoy, Gabrielle J. M. Forman, Barton A. Liu, Qing Mahanama, Sarith P. P. Toure, Ally TI Assessment and Enhancement of MERRA Land Surface Hydrology Estimates SO JOURNAL OF CLIMATE LA English DT Article ID DATA ASSIMILATION SYSTEM; CATCHMENT-BASED APPROACH; ERA-INTERIM REANALYSIS; SNOW WATER EQUIVALENT; GLOBAL SOIL-MOISTURE; SATELLITE-OBSERVATIONS; GAUGE OBSERVATIONS; FORECAST SYSTEM; FORCING DATA; PRECIPITATION AB The Modern-Era Retrospective Analysis for Research and Applications (MERRA) is a state-of-the-art reanalysis that provides, in addition to atmospheric fields, global estimates of soil moisture, latent heat flux, snow, and runoff for 1979 present. This study introduces a supplemental and improved set of land surface hydrological fields ("MERRA-Land") generated by rerunning a revised version of the land component of the MERRA system. Specifically, the MERRA-Land estimates benefit from corrections to the precipitation forcing with the Global Precipitation Climatology Project pentad product (version 2.1) and from revised parameter values in the rainfall interception model, changes that effectively correct for known limitations in the MERRA surface meteorological forcings. The skill (defined as the correlation coefficient of the anomaly time series) in land surface hydrological fields from MERRA and MERRA-Land is assessed here against observations and compared to the skill of the state-of-the-art ECMWF Re-Analysis-Interim (ERA-I). MERRA-Land and ERA-I root zone soil moisture skills (against in situ observations at 85 U.S. stations) are comparable and significantly greater than that of MERRA. Throughout the Northern Hemisphere, MERRA and MERRA-Land agree reasonably well with in situ snow depth measurements (from 583 stations) and with snow water equivalent from an independent analysis. Runoff skill (against naturalized stream flow observations from 18 U.S. basins) of MERRA and MERRA-Land is typically higher than that of ERA-I. With a few exceptions, the MERRA-Land data appear more accurate than the original MERRA estimates and are thus recommended for those interested in using MERRA output for land surface hydrological studies. C1 [Reichle, Rolf H.; Koster, Randal D.; De Lannoy, Gabrielle J. M.; Forman, Barton A.; Liu, Qing; Mahanama, Sarith P. P.; Toure, Ally] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [De Lannoy, Gabrielle J. M.; Toure, Ally] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [De Lannoy, Gabrielle J. M.] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium. [Forman, Barton A.] Oak Ridge Associated Univ, Oak Ridge, TN USA. [Liu, Qing; Mahanama, Sarith P. P.] Sci Applicat Int Corp, Beltsville, MD USA. RP Reichle, RH (reprint author), NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Mail Code 610-1,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM rolf.reichle@nasa.gov RI Reichle, Rolf/E-1419-2012; Koster, Randal/F-5881-2012; Forman, Barton/I-2227-2012 OI Koster, Randal/0000-0001-6418-6383; FU NASA; ACRIMSAT satellites; Research Foundation Flanders (FWO), Belgium FX Funding for this work was provided by the NASA program on Earth System Science Research using data and products from the Terra, Aqua, and ACRIMSAT satellites. G. De Lannoy is a postdoctoral research fellow supported by the Research Foundation Flanders (FWO), Belgium. B. Forman is a fellow supported by the NASA Postdoctoral Program. Computing was supported by the NASA High End Computing Program. We are grateful for access to the many datasets that supported this work and highly appreciate all those who made them possible, including personnel at USDA, NASA/GSFC, NOAA Climate Prediction Center, Environment Canada, Deutscher Wetterdienst, U.S. Army Corps of Engineers, U.S. Bureau of Reclamation, Columbia River Basin Climate Change Scenarios Database, California Data Exchange Commission, and the European Centre for Medium-Range Weather Forecasts. Thanks also go to G. Huffman and P. Xie for their advice on precipitation data, to M. Tedesco and J. Miller for processing the WMO snow depth data, to T. Martin and G. Starr for the US-SP3 site FLUXNET data, to R. Brown, M. Sturm, and B. Brasnett for the CMC snow analysis data and their support of our study, to D. Miralles for the interception loss fraction data, to C. Jimenez and the GEWEX-LANDFLUX scientists for the multiproduct latent heat data, and to E. Maurer for his assistance in obtaining naturalized streamflow data. Thanks to M. Bosilovich and three anonymous reviewers for many helpful comments. NR 58 TC 173 Z9 176 U1 4 U2 46 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD DEC 15 PY 2011 VL 24 IS 24 BP 6322 EP 6338 DI 10.1175/JCLI-D-10-05033.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 863XJ UT WOS:000298201300004 ER PT J AU Kato, S Wielicki, BA Rose, FG Liu, X Taylor, PC Kratz, DP Mlynczak, MG Young, DF Phojanamongkolkij, N Sun-Mack, S Miller, WF Chen, Y AF Kato, Seiji Wielicki, Bruce A. Rose, Fred G. Liu, Xu Taylor, Patrick C. Kratz, David P. Mlynczak, Martin G. Young, David F. Phojanamongkolkij, Nipa Sun-Mack, Sunny Miller, Walter F. Chen, Yan TI Detection of Atmospheric Changes in Spatially and Temporally Averaged Infrared Spectra Observed from Space SO JOURNAL OF CLIMATE LA English DT Article ID RADIATIVE-TRANSFER MODEL; OPTICAL-THICKNESS; INDEPENDENT PIXEL; CLOUD PROPERTIES; ICE CLOUDS; RETRIEVAL; ALGORITHM; REFLECTANCE; ULTRAVIOLET; PARAMETERS AB Variability present at a satellite instrument sampling scale (small-scale variability) has been neglected in earlier simulations of atmospheric and cloud property change retrievals using spatially and temporally averaged spectral radiances. The effects of small-scale variability in the atmospheric change detection process are evaluated in this study. To simulate realistic atmospheric variability, top-of-the-atmosphere nadir-view longwave spectral radiances are computed at a high temporal (instantaneous) resolution with a 20-km field-of-view using cloud properties retrieved from Moderate Resolution Imaging Spectroradiometer (MODIS) measurements, along with temperature humidity profiles obtained from reanalysis. Specifically, the effects of the variability on the necessary conditions for retrieving atmospheric changes by a linear regression are tested. The percentage error in the annual 10 degrees zonal mean spectral radiance difference obtained by assuming linear combinations of individual perturbations expressed as a root-mean-square (RMS) difference computed over wavenumbers between 200 and 2000 cm(-1) is 10%-15% for most of the 10 degrees zones. However, if cloud fraction perturbation is excluded, the RMS difference decreases to less than 2%. Monthly and annual 10 degrees zonal mean spectral radiances change linearly with atmospheric property perturbations, which occur when atmospheric properties are perturbed by an amount approximately equal to the variability of the10 degrees zonal monthly deseasonalized anomalies or by a climate-model-predicted decadal change. Nonlinear changes in the spectral radiances of magnitudes similar to those obtained through linear estimation can arise when cloud heights and droplet radii in water cloud change. The spectral shapes computed by perturbing different atmospheric and cloud properties are different so that linear regression can separate individual spectral radiance changes from the sum of the spectral radiance change. When the effects of small-scale variability are treated as noise, however, the error in retrieved cloud properties is large. The results suggest the importance of considering small-scale variability in inferring atmospheric and cloud property changes from the satellite-observed zonally and annually averaged spectral radiance difference. C1 [Kato, Seiji; Wielicki, Bruce A.; Liu, Xu; Taylor, Patrick C.; Kratz, David P.; Mlynczak, Martin G.; Young, David F.] NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA. [Rose, Fred G.; Sun-Mack, Sunny; Miller, Walter F.] Sci Syst & Applicat Inc, Hampton, VA USA. [Phojanamongkolkij, Nipa] NASA, Aeronaut Syst Engn Branch, Langley Res Ctr, Hampton, VA 23681 USA. RP Kato, S (reprint author), NASA, Climate Sci Branch, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM seiji.kato@nasa.gov RI Mlynczak, Martin/K-3396-2012; Taylor, Patrick/D-8696-2015; Richards, Amber/K-8203-2015; OI Taylor, Patrick/0000-0002-8098-8447; Rose, Fred G/0000-0003-0769-0772 FU NASA Science Directorate through the CLARREO FX We thank Drs. Stephen Leroy, John Dykema, Yi Huang, Xianglei Huang, Robert Knuteson, Norman Loeb, and Oleg Dubovik for helpful discussions and suggestions and two anonymous reviewers for constructive and very helpful comments. We also thank Ms. Amber Richards for proofreading the manuscript. The work was supported by the NASA Science Directorate through the CLARREO project. NR 48 TC 12 Z9 12 U1 0 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD DEC 15 PY 2011 VL 24 IS 24 BP 6392 EP 6407 DI 10.1175/JCLI-D-10-05005.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 863XJ UT WOS:000298201300008 ER PT J AU Emili, E Lyapustin, A Wang, Y Popp, C Korkin, S Zebisch, M Wunderle, S Petitta, M AF Emili, E. Lyapustin, A. Wang, Y. Popp, C. Korkin, S. Zebisch, M. Wunderle, S. Petitta, M. TI High spatial resolution aerosol retrieval with MAIAC: Application to mountain regions SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID PARTICULATE MATTER; OPTICAL-THICKNESS; VALIDATION; SATELLITE; POLLUTION; EUROPE; IMPACT; LAND; PM10 AB Aerosol spatial distribution in populated mountain areas is very heterogeneous and often characterized by scales of variability of several kilometers. Satellites provide an effective tool to map aerosols on an operational basis, but most of the aerosol products intended for continental/global applications have a coarse spatial resolution (10-18 km). The Multiangle Implementation of Atmospheric Correction (MAIAC) is a recently developed algorithm for the Moderate Resolution Imaging Spectroradiometer (MODIS), which provides Aerosol Optical Depth (AOD) at a high resolution of 1 km. We analyze the quality and potential of MAIAC AOD in the Alpine region and we derive high resolution AOD maps for the years 2008 and 2009. Cloudiness and snow in mountain regions occasionally lead to an overestimation of AOD due to unresolved cloud and snow pixel contamination. Therefore, we developed a filter that almost preserves the spatial resolution of the product to ensure the good accuracy of MAIAC AOD for air-quality and climatological applications. The AOD is validated with AERONET measurements in the region and compared to the standard MODIS AOD product (MOD04). Similar accuracies are found for both products (RMSE = 0.05) but with MAIAC providing about 50% more observations at the examined locations, because of its higher spatial resolution and less restrictive filtering. Comparison with ground measurements of aerosol mass (PM10) shows that MAIAC AOD can be used to detect the fine scales of aerosol variability (2-3 km) in the mountains. Finally, AOD maps for the Alpine region demonstrate that topography is correlated with the average aerosol spatial distribution. C1 [Emili, E.; Wunderle, S.] Univ Bern, Remote Sensing Grp, Inst Geog, CH-3012 Bern, Switzerland. [Lyapustin, A.; Wang, Y.; Korkin, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zebisch, M.; Petitta, M.] European Acad, Inst Appl Remote Sensing, I-39100 Bolzano, Italy. [Popp, C.] Empa, Swiss Fed Labs Mat Sci & Technol, CH-8600 Dubendorf, Switzerland. RP Emili, E (reprint author), Univ Bern, Remote Sensing Grp, Inst Geog, Hallerstr 12, CH-3012 Bern, Switzerland. EM emanuele.emili@giub.unibe.ch RI Lyapustin, Alexei/H-9924-2014 OI Lyapustin, Alexei/0000-0003-1105-5739 FU Armasuisse, Science and Technology; autonomous province of Bolzano (Italy); NASA; NOAA GOES-R FX This research was supported by the Armasuisse, Science and Technology, and the autonomous province of Bolzano (Italy). The work of A. Lyapustin, Y. Wang, and S. Korkin was funded by the NASA Terrestrial Ecology Program (D. Wickland), NASA Applications Program (L. Friedl and B. Doorn), and in part by the NOAA GOES-R program (M. Goldberg). We thank the AERONET PIs for providing sun-photometers data, NABEL and APPA for providing PM10 data. We thank Lorraine Remer and two anonymous reviewers for valuable comments which helped to improve the manuscript. We also thank Armin Costa and Roberto Monsorno for the technical support. NR 30 TC 12 Z9 12 U1 2 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 15 PY 2011 VL 116 AR D23211 DI 10.1029/2011JD016297 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 864QQ UT WOS:000298255300006 ER PT J AU Manizza, M Follows, MJ Dutkiewicz, S Menemenlis, D McClelland, JW Hill, CN Peterson, BJ Key, RM AF Manizza, M. Follows, M. J. Dutkiewicz, S. Menemenlis, D. McClelland, J. W. Hill, C. N. Peterson, B. J. Key, R. M. TI A model of the Arctic Ocean carbon cycle SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID GENERAL-CIRCULATION-MODEL; DISSOLVED ORGANIC-MATTER; SEA CO2 FLUX; GLOBAL OCEAN; BARENTS SEA; BIOGEOCHEMISTRY MODELS; WATER; ICE; DYNAMICS; ATLANTIC AB A three dimensional model of Arctic Ocean circulation and mixing, with a horizontal resolution of 18 km, is overlain by a biogeochemical model resolving the physical, chemical and biological transport and transformations of phosphorus, alkalinity, oxygen and carbon, including the air-sea exchange of dissolved gases and the riverine delivery of dissolved organic carbon. The model qualitatively captures the observed regional and seasonal trends in surface ocean PO4, dissolved inorganic carbon, total alkalinity, and pCO(2). Integrated annually, over the basin, the model suggests a net annual uptake of 59 Tg C a(-1), within the range of published estimates based on the extrapolation of local observations (20-199 Tg C a(-1)). This flux is attributable to the cooling (increasing solubility) of waters moving into the basin, mainly from the subpolar North Atlantic. The air-sea flux is regulated seasonally and regionally by sea-ice cover, which modulates both air-sea gas transfer and the photosynthetic production of organic matter, and by the delivery of riverine dissolved organic carbon (RDOC), which drive the regional contrasts in pCO(2) between Eurasian and North American coastal waters. Integrated over the basin, the delivery and remineralization of RDOC reduces the net oceanic CO2 uptake by similar to 10%. C1 [Manizza, M.; Follows, M. J.; Dutkiewicz, S.; Hill, C. N.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Menemenlis, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [McClelland, J. W.] Univ Texas Austin, Inst Marine Sci, Port Aransas, TX 78373 USA. [Peterson, B. J.] Marine Biol Lab, Ctr Ecosyst, Woods Hole, MA 02543 USA. [Key, R. M.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. RP Manizza, M (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM mmanizza@ucsd.edu RI McClelland, James/C-5396-2008 OI McClelland, James/0000-0001-9619-8194 FU NASA; National Science Foundation [ARC-0531119, ARC-0806229]; NOAA [NA08OAR4310820, NA08OAR4320752] FX This study has been carried out as part of ECCO2 and SASS (Synthesis of the Arctic System Science) projects funded by NASA and NSF, respectively. MM and MJF are grateful for support from the National Science Foundation (ARC-0531119 and ARC-0806229) for financial support. MM also acknowledges NASA for providing computer time, the use of the computing facilities at NAS center and also the Scripps post-doctoral program for further financial support that helped to complete the manuscript. RMK also acknowledges NOAA for support (NA08OAR4310820 and NA08OAR4320752). Oliver Jahn kindly provided interpolated phosphate fields for model initialization and Stuart Goldberg nicely helped us with the plots of the CARINA data set by using Ocean Data View. NR 71 TC 12 Z9 12 U1 1 U2 28 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC 15 PY 2011 VL 116 AR C12020 DI 10.1029/2011JC006998 PG 19 WC Oceanography SC Oceanography GA 864PU UT WOS:000298253000002 ER PT J AU Millan, L Thomas, I Bowles, N AF Millan, L. Thomas, I. Bowles, N. TI Lunar regolith thermal gradients and emission spectra: Modeling and validation SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID PARTICULATE PLANETARY SURFACES; SIMULATED LUNAR; SCATTERING; CONDUCTIVITY; SILICATES; GRAPHITE; GRAINS; BANDS AB The retrieval of surface composition from IR measurements of airless bodies requires a model capable of computing the significant thermal gradients present in the top few hundred microns of the regolith. In this study we introduce a model which reproduces most of the features found in controlled experiments made in the simulated lunar environment emission chamber (SLEEC). Although the model presented here is forced by a lower boundary held at a fixed temperature, we conclude that a similar algorithm driven by solar illumination may be used as a forward model to retrieve composition, particle size and effective thermal conductivity from IR measurements of airless bodies. C1 [Millan, L.; Thomas, I.; Bowles, N.] Univ Oxford, Clarendon Lab, Atmospher Ocean & Planetary Phys, Oxford OX1 3PU, England. RP Millan, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM lmillan@jpl.nasa.gov RI Millan, Luis/J-2759-2015 FU NASA; UK Science and Technology Facilities Council; Diviner Lunar Radiometer Experiment science budget FX We thank G. Thomas and M. Munro for their help with setting up and running DISORT and the Oxford Mie code. This research was carried out in part at the University of Oxford and at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work was supported by the UK Science and Technology Facilities Council and the Diviner Lunar Radiometer Experiment science budget. NR 25 TC 1 Z9 1 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 15 PY 2011 VL 116 AR E12003 DI 10.1029/2011JE003874 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 864QE UT WOS:000298254000001 ER PT J AU Kumar, PK Desai, U Monroe, JA Lagoudas, DC Karaman, I Bigelow, G Noebe, RD AF Kumar, Parikshith K. Desai, Uri Monroe, James A. Lagoudas, Dimitris C. Karaman, Ibrahim Bigelow, Glen Noebe, Ronald D. TI Experimental investigation of simultaneous creep, plasticity and transformation of Ti50.5Pd30Ni19.5 high temperature shape memory alloy during cyclic actuation SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article DE Thermomechanical characterization; Shape memory alloys; Creep; Phase transformation ID DEFORMATION-MECHANISM MAP; BEHAVIOR; LOAD; TI AB The influence of inelastic phenomena (i.e. plasticity and viscoplasticity) on the phase transformation and the cyclic actuation behavior of a Ti50.5Pd30Ni19.5 high temperature shape memory alloy (HTSMA) was investigated by thermomechanical testing. Standard creep and constant stress thermal cycling experiments were conducted to study the rate-independent and rate-dependent irrecoverable strain generation both individually and simultaneously with the phase transformation. Based on a preliminary power-law fit of the creep data from the creep tests, the varying creep rates and stress exponents suggest that the mechanism for creep deformation changes with both stress level and temperature within the likely operating range for the alloy. The load-biased thermal cycling tests show that the material performance can be significantly affected by rate independent plasticity strains generated during transformation, rate dependent viscoplastic strains as well as factors such as retained martensite accumulation. To consolidate these inelastic mechanisms, a combined phase transformation-deformation diagram was constructed to show the phase transformation along with the plastic and viscoplastic regions within the operational range of the HTSMA. (C) 2011 Published by Elsevier B.V. C1 [Kumar, Parikshith K.; Desai, Uri; Lagoudas, Dimitris C.] Texas A&M Univ, Dept Aerosp Engn, College Stn, TX 77843 USA. [Monroe, James A.; Karaman, Ibrahim] Texas A&M Univ, Dept Mech Engn, College Stn, TX 77843 USA. [Lagoudas, Dimitris C.; Karaman, Ibrahim] Texas A&M Univ, Mat Sci & Engn Interdisciplinary Grad Program, College Stn, TX 77843 USA. [Bigelow, Glen; Noebe, Ronald D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Lagoudas, DC (reprint author), Texas A&M Univ, Dept Aerosp Engn, College Stn, TX 77843 USA. EM lagoudas@tamu.edu RI Karaman, Ibrahim/E-7450-2010; OI Karaman, Ibrahim/0000-0001-6461-4958; Lagoudas, Dimitris/0000-0002-0194-5933 FU NASA; API Janet Hurst [NNX07AB56A] FX Financial support for this work was provided by the NASA Fundamental Aeronautics Program, Subsonic Fixed Wing Project, under API Janet Hurst, and in part through contract number NNX07AB56A. NR 38 TC 13 Z9 13 U1 1 U2 13 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD DEC 15 PY 2011 VL 530 BP 117 EP 127 DI 10.1016/j.msea.2011.09.051 PG 11 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 865KZ UT WOS:000298311100014 ER PT J AU Battistoni, G Broggi, F Brugger, M Campanella, M Carboni, M Empl, A Fasso, A Gadioli, E Cerutti, F Ferrari, A Ferrari, A Lantz, M Mairani, A Margiotta, M Morone, C Muraro, S Parodi, K Patera, V Pelliccioni, M Pinsky, L Ranft, J Roesler, S Rollet, S Sala, PR Santana, M Sarchiapone, L Sioli, M Smirnov, G Sommerer, F Theis, C Trovati, S Villari, R Vincke, H Vincke, H Vlachoudis, V Vollaire, J Zapp, N AF Battistoni, Giuseppe Broggi, Francesco Brugger, Markus Campanella, Mauro Carboni, Massimo Empl, Anton Fasso, Alberto Gadioli, Ettore Cerutti, Francesco Ferrari, Alfredo Ferrari, Anna Lantz, Matthias Mairani, Andrea Margiotta, M. Morone, Cristina Muraro, Silvia Parodi, Katia Patera, Vincenzo Pelliccioni, Mauricio Pinsky, Larry Ranft, Johannes Roesler, Stefan Rollet, Sofia Sala, Paola R. Santana, Mario Sarchiapone, Lucia Sioli, Massimiliano Smirnov, George Sommerer, Florian Theis, Christian Trovati, Stefania Villari, R. Vincke, Heinz Vincke, Helmut Vlachoudis, Vasilis Vollaire, Joachim Zapp, Neil TI Applications of FLUKA Monte Carlo code for nuclear and accelerator physics SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 10th European Conference on Accelerators in Applied Research and Technology (ECAART) CY SEP 13-17, 2010 CL Athens, GREECE SP Aristotle Univ Thessaloniki, Fac Sci, Natl Tech Univ Athens, Natl Ctr Sci Res Demokritos, Natl Kapodistrian Univ Athens, Training Ctr Natl Bank Greece, Int Atom Energy Agcy, High Voltage Engn, Natl Electrostat Corp, Oxford Microbeams Ltd, Mesytec GmbH, MegaLab Co DE FLORA; Simulation; nTOF; LHC AB FLUKA is a general purpose Monte Carlo code capable of handling all radiation components from thermal energies (for neutrons) or 1 key (for all other particles) to cosmic ray energies and can be applied in many different fields. Presently the code is maintained on Linux. The validity of the physical models implemented in FLUKA has been benchmarked against a variety of experimental data over a wide energy range, from accelerator data to cosmic ray showers in the Earth atmosphere. FLUKA is widely used for studies related both to basic research and to applications in particle accelerators, radiation protection and dosimetry, including the specific issue of radiation damage in space missions, radiobiology (including radiotherapy) and cosmic ray calculations. After a short description of the main features that make FLUKA valuable for these topics, the present paper summarizes some of the recent applications of the FLUKA Monte Carlo code in the nuclear as well high energy physics. In particular it addresses such topics as accelerator related applications. (C) 2011 Elsevier B.V. All rights reserved. C1 [Brugger, Markus; Cerutti, Francesco; Ferrari, Alfredo; Roesler, Stefan; Smirnov, George; Theis, Christian; Trovati, Stefania; Vincke, Heinz; Vincke, Helmut; Vlachoudis, Vasilis; Vollaire, Joachim] CERN, CH-1211 Geneva 23, Switzerland. [Battistoni, Giuseppe; Broggi, Francesco; Campanella, Mauro; Gadioli, Ettore; Muraro, Silvia; Sala, Paola R.] Ist Nazl Fis Nucl, I-20133 Milan, Italy. [Fasso, Alberto; Santana, Mario] SLAC, Stanford, CA USA. [Ranft, Johannes] Univ Siegen, Siegen, Germany. [Carboni, Massimo] Ist Nazl Fis Nucl, Legnaro, Italy. [Ferrari, Anna; Patera, Vincenzo; Pelliccioni, Mauricio; Villari, R.] Ist Nazl Fis Nucl, Frascati, Italy. [Morone, Cristina] Ist Nazl Fis Nucl, Rome, Italy. [Morone, Cristina] Univ Roma Tor Vergata, Rome, Italy. [Margiotta, M.; Sioli, Massimiliano] Ist Nazl Fis Nucl, I-40126 Bologna, Italy. [Margiotta, M.; Sioli, Massimiliano] Univ Bologna, Bologna, Italy. [Parodi, Katia; Sommerer, Florian] HIT, Heidelberg, Germany. [Empl, Anton; Pinsky, Larry] Univ Houston, Houston, TX USA. [Zapp, Neil] NASA, Houston, TX USA. [Parodi, Katia; Sommerer, Florian] ARC Seibersdorf, Seibersdorf, Austria. [Lantz, Matthias] Riken Lab, Wako, Saitama, Japan. RP Vlachoudis, V (reprint author), CERN, CH-1211 Geneva 23, Switzerland. EM Vasilis.Vlachoudis@cern.ch RI sala, paola/E-2868-2013; Morone, Maria Cristina/P-4407-2016; Battistoni, Giuseppe/B-5264-2012; OI sala, paola/0000-0001-9859-5564; Morone, Maria Cristina/0000-0002-0200-0632; Battistoni, Giuseppe/0000-0003-3484-1724; Carboni, Massimo/0000-0003-4296-3799; , Sofia/0000-0002-4389-3641 NR 21 TC 7 Z9 7 U1 3 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD DEC 15 PY 2011 VL 269 IS 24 BP 2850 EP 2856 DI 10.1016/j.nimb.2011.04.028 PG 7 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 866EO UT WOS:000298363500003 ER PT J AU Panciera, R Walker, JP Kalma, J Kim, E AF Panciera, Rocco Walker, Jeffrey P. Kalma, Jetse Kim, Edward TI A proposed extension to the soil moisture and ocean salinity level 2 algorithm for mixed forest and moderate vegetation pixels SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE SMOS; SMOS Level 2; Passive microwave; Soil moisture; Spatial heterogeneity ID BAND MICROWAVE EMISSION; BRIGHTNESS TEMPERATURE; HYDROLOGY EXPERIMENT; LAND SURFACES; SMOS MISSION; CROP FIELDS; RETRIEVAL; HETEROGENEITY; RADIOMETRY; CATCHMENTS AB The Soil Moisture and Ocean Salinity (SMOS) mission, launched in November 2009, provides global maps of soil moisture and ocean salinity by measuring the L-band (1.4 GHz) emission of the Earth's surface with a spatial resolution of 40-50 km. Uncertainty in the retrieval of soil moisture over large heterogeneous areas such as SMOS pixels is expected, due to the non-linearity of the relationship between soil moisture and the microwave emission. The current baseline soil moisture retrieval algorithm adopted by SMOS and implemented in the SMOS Level 2 (SMOS L2) processor partially accounts for the sub-pixel heterogeneity of the land surface, by modelling the individual contributions of different pixel fractions to the overall pixel emission. This retrieval approach is tested in this study using airborne L-band data over an area the size of a SMOS pixel characterised by a mix Eucalypt forest and moderate vegetation types (grassland and crops), with the objective of assessing its ability to correct for the soil moisture retrieval error induced by the land surface heterogeneity. A preliminary analysis using a traditional uniform pixel retrieval approach shows that the sub-pixel heterogeneity of land cover type causes significant errors in soil moisture retrieval (7.7%v/v RMSE, 2%v/v bias) in pixels characterised by a significant amount of forest (40-60%). Although the retrieval approach adopted by SMOS partially reduces this error, it is affected by errors beyond the SMOS target accuracy, presenting in particular a strong dry bias when a fraction of the pixel is occupied by forest (4.1%v/v RMSE, -3.1%v/v bias). An extension to the SMOS approach is proposed that accounts for the heterogeneity of vegetation optical depth within the SMOS pixel. The proposed approach is shown to significantly reduce the error in retrieved soil moisture (2.8%v/v RMSE, -03%v/v bias) in pixels characterised by a critical amount of forest (40-60%), at the limited cost of only a crude estimate of the optical depth of the forested area (better than 35% uncertainty). This study makes use of an unprecedented data set of airborne L-band observations and ground supporting data from the National Airborne Field Experiment 2005 (NAFE'05), which allowed accurate characterisation of the land surface heterogeneity over an area equivalent in size to a SMOS pixel. (C) 2011 Elsevier Inc. All rights reserved. C1 [Panciera, Rocco] Univ Melbourne, CRC Spatial Informat, Carlton, Vic 3053, Australia. [Walker, Jeffrey P.] Monash Univ, Dept Civil Engn, Clayton, Vic 3800, Australia. [Kalma, Jetse] Univ Newcastle, Sch Engn, Callaghan, NSW 2308, Australia. [Kim, Edward] NASA, Goddard Space Flight Ctr, Washington, DC USA. RP Panciera, R (reprint author), Univ Melbourne, CRC Spatial Informat, POB 672, Carlton, Vic 3053, Australia. EM panr@unimelb.edu.au RI Walker, Jeffrey/D-2624-2009 FU Australian Research Council FX The National Airborne Field Experiment 2005 was made possible through infrastructure (LE0453434) and research (DP0557543) funding from the Australian Research Council, and the collaboration of a large number of scientists from throughout Australia, United States and Europe. The authors wish to thank Phillip Maisongrande and Gilles Boulet at the Centre d'Etudes Spatiales de la BIOsphere (CESBIO) for the supervised classification of the Landsat 5 Thematic Mapper scene, and Cristina Martinez for providing the laser mastersizer soil particle analysis data. NR 49 TC 8 Z9 8 U1 2 U2 15 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 DEC 15 PY 2011 VL 115 IS 12 BP 3343 EP 3354 DI 10.1016/j.rse.2011.07.017 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 865LB UT WOS:000298311300032 ER PT J AU Lee, H Beighley, RE Alsdorf, D Jung, HC Shum, CK Duan, JB Guo, JY Yamazaki, D Andreadis, K AF Lee, Hyongki Beighley, R. Edward Alsdorf, Douglas Jung, Hahn Chul Shum, C. K. Duan, Jianbin Guo, Junyi Yamazaki, Dai Andreadis, Konstantinos TI Characterization of terrestrial water dynamics in the Congo Basin using GRACE and satellite radar altimetry SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Congo; Wetland; Water storage; GRACE; Satellite Radar Altimetry ID STORAGE CHANGES; AMAZON; AFRICA; VARIABILITY; VALIDATION; RAINFALL; SYSTEM; FOREST AB The Congo Basin is the world's third largest in size (similar to 3.7 million km(2)), and second only to the Amazon River in discharge (similar to 40,200 m(3) s(-1) annual average). However, the hydrological dynamics of seasonally flooded wetlands and floodplains remains poorly quantified. Here, we separate the Congo wetland into four 3 degrees x 3 degrees regions, and use remote sensing measurements (i.e., GRACE, satellite radar altimeter, GPCP, JERS-1, SRTM, and MODIS) to estimate the amounts of water filling and draining from the Congo wetland, and to determine the source of the water. We find that the amount of water annually filling and draining the Congo wetlands is 111 km(3), which is about one-third the size of the water volumes found on the mainstem Amazon floodplain. Based on amplitude comparisons among the water volume changes and timing comparisons among their fluxes, we conclude that the local upland runoff is the main source of the Congo wetland water, not the fluvial process of river-floodplain water exchange as in the Amazon. Our hydraulic analysis using altimeter measurements also supports our conclusion by demonstrating that water surface elevations in the wetlands are consistently higher than the adjacent river water levels. Our research highlights differences in the hydrology and hydrodynamics between the Congo wetland and the mainstem Amazon floodplain. (C) 2011 Elsevier Inc. All rights reserved. C1 [Lee, Hyongki; Alsdorf, Douglas; Shum, C. K.; Duan, Jianbin; Guo, Junyi] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. [Lee, Hyongki; Alsdorf, Douglas; Shum, C. K.; Andreadis, Konstantinos] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA. [Beighley, R. Edward] FM Global, Struct Hazards & Response Res, Norwood, MA USA. [Jung, Hahn Chul] NASA, Hydrol Sci Branch Code 614 3, Goddard Space Flight Ctr, Greenbelt, MD USA. [Yamazaki, Dai] Univ Tokyo, Dept Civil Engn, Tokyo 113, Japan. RP Lee, H (reprint author), Univ Houston, Dept Civil & Environm Engn, N107 Engn Bldg 1, Houston, TX 77204 USA. EM hlee@uh.edu RI Yamazaki, Dai/J-3029-2012 OI Yamazaki, Dai/0000-0002-6478-1841 FU NASA; Ohio State University FX This research is funded by NASA's Terrestrial Hydrology Program and by Ohio State University's Climate, Water and Carbon Program. We thank 3 anonymous reviewers for providing constructive comments. Some of the figures are prepared using the GMT graphics package (Wessel and Smith, EOS, 1991). NR 28 TC 30 Z9 30 U1 4 U2 53 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC 15 PY 2011 VL 115 IS 12 BP 3530 EP 3538 DI 10.1016/j.rse.2011.08.015 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 865LB UT WOS:000298311300047 ER PT J AU Privette, CV Khalilian, A Torres, O Katzberg, S AF Privette, Charles V., III Khalilian, Ahmad Torres, Omar Katzberg, Stephen TI Utilizing space-based GPS technology to determine hydrological properties of soils SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Remote sensing; Soil moisture; Site-specific irrigation; GPS ID SMEX02 AB Competition for limited water resources is one of the most critical issues being faced by irrigated agriculture in the United States. Site-specific irrigation applies irrigation water to match the needs of individual management zones within a field, significantly reducing water consumption, runoff, and nutrient leaching in ground water. Remote sensing for real-time and continuous soil moisture measurements at specific depths is essential for success of site-specific irrigation system. The overall objective of this study was to investigate the feasibility of utilizing a GPS-based sensor technology to determine site-specific information such as the soil moisture condition by recording the GPS signal reflected from the earth's surface. A modified GPS Delay Mapping Receiver (DMR) tracks and measures the direct, line-of-sight, Right-Hand-Circularly Polarized signal of a GPS satellite. It also simultaneously measures the delayed, earth-reflected, near-specular, Left-Hand-Circularly Polarized GPS signal. These measurements can be used to estimate the surface scattering coefficient and path delays between the direct and reflected GPS signals. Over land, scattering coefficients can be used to estimate changes in soil moisture contents. Our results showed that the space-based technology has a great potential for determining soil volumetric moisture contents in the pursuit of site-specific irrigation management. There were strong correlations between the GPS reflectivity measurements and soil moisture contents. The GPS reflectivity increased as the soil moisture contents increased. Careful analysis of the test data showed very conclusively that the sensitivity of L-Band signal (1.575 GHz) to soil moisture contents changed with soil type and sampling depth. The sensitivity decreased with sampling depth in light soils and increased in heavy soils. (C) 2011 Elsevier Inc. All rights reserved. C1 [Privette, Charles V., III] Clemson Univ, Clemson, SC 29634 USA. [Khalilian, Ahmad] Clemson Univ, Edisto REC, Blackville, SC USA. [Torres, Omar] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Katzberg, Stephen] S Carolina State Univ, Orangeburg, SC USA. RP Privette, CV (reprint author), Clemson Univ, 247 McAdams Hall, Clemson, SC 29634 USA. EM privett@clemson.edu; akhlln@clemson.edu; omar.torres@nasa.gov; SJkatzberg@scsu.edu FU South Carolina Agricultural Experiment Station, Clemson University [5925] FX The authors acknowledge the funding support of the South Carolina Space Grant Consortium. Technical Contribution No. 5925 of the South Carolina Agricultural Experiment Station, Clemson University is also acknowledged. NR 15 TC 2 Z9 2 U1 0 U2 13 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 DEC 15 PY 2011 VL 115 IS 12 BP 3582 EP 3586 DI 10.1016/j.rse.2011.08.019 PG 5 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 865LB UT WOS:000298311300051 ER PT J AU Naesset, E Gobakken, T Solberg, S Gregoire, TG Nelson, R Stahl, G Weydahl, D AF Naesset, Erik Gobakken, Terje Solberg, Svein Gregoire, Timothy G. Nelson, Ross Stahl, Goran Weydahl, Dan TI Model-assisted regional forest biomass estimation using LiDAR and InSAR as auxiliary data: A case study from a boreal forest area SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Forest monitoring; Laser scanning; SAR; Probability sampling ID LASER SCANNER DATA; AIRBORNE LASER; RAIN-FOREST; TOPOGRAPHY MISSION; FOOTPRINT LIDAR; SHUTTLE RADAR; BAND SAR; INVENTORY; CANOPY; HEIGHT AB There is a need for accurate inventory methods that produce relevant and timely information on the forest resources and carbon stocks for forest management planning and for implementation of national strategies under the United Nations Collaborative Program on Reduced Emissions from Deforestation and Forest Degradation in Developing Countries (REDD). Such methods should produce information that is consistent across various geographical scales. Airborne scanning Light Detection and Ranging (LiDAR) is among the most promising remote sensing technologies for estimation of forest resource information such as timber volume and biomass, while acquisition of three dimensional data with Interferometric Synthetic Aperture Radar (InSAR) from space is seen as a relevant option for inventory in the tropics because of its ability to "see through the clouds" and its potential for frequent updates at low costs. Based on a stratified probability sample of 201 field survey plots collected in a 960 km(2) boreal forest area in Norway, we demonstrate how total above-ground biomass (AGB) can be estimated at three distinct geographical levels in such a way that the estimates at a smaller level always sum up to the estimate at a larger level. The three levels are (1) a district (the entire study area), (2) a village, local community or estate level, and (3) a stand or patch level. The LiDAR and InSAR data were treated as auxiliary information in the estimation. At the two largest geographical levels model-assisted estimators were employed. A model-based estimation was conducted at the smallest level. Estimates of AGB and corresponding error estimates based on (1) the field sample survey were compared with estimates obtained by using (2) LiDAR and (3) InSAR data as auxiliary information. For the entire study area, the estimates of AGB were 116.0, 101.2, and 111.3 Mg ha(-1), respectively. Corresponding standard error estimates were 3.7, 1.6, and 3.2 Mg ha(-1). At the smallest geographical level (stand) an independent validation on 35 large field plots was carried out. RMSE values of 17.1-17.3 Mg ha(-1) and 42.6-53.2 Mg ha(-1) were found for LiDAR and InSAR, respectively. A time lag of six years between acquisition of InSAR data and field inventory has introduced some errors. Significant differences between estimates and reference values were found, illustrating the risk of using pure model-based methods in the estimation when there is a lack of fit in the models. We conclude that the examined remote sensing techniques can provide biomass estimates with smaller estimated errors than a field-based sample survey. The improvement can be highly significant, especially for LiDAR. (C) 2011 Elsevier Inc. All rights reserved. C1 [Naesset, Erik; Gobakken, Terje] Norwegian Univ Life Sci, Dept Ecol & Nat Resource Management, NO-1432 As, Norway. [Solberg, Svein] Norwegian Forest & Landscape Inst, NO-1431 As, Norway. [Gregoire, Timothy G.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Nelson, Ross] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Stahl, Goran] Swedish Univ Agr Sci, Dept Forest Resource Management, SE-90183 Umea, Sweden. [Weydahl, Dan] Norwegian Def Res Estab, Land & Airsyst Div, NO-2027 Kjeller, Norway. RP Naesset, E (reprint author), Norwegian Univ Life Sci, Dept Ecol & Nat Resource Management, POB 5003, NO-1432 As, Norway. EM erik.naesset@umb.no RI chen, zhu/K-5923-2013; Nelson, Ross/H-8266-2014 FU Research Council of Norway [184636/S30] FX This research has been funded by the Research Council of Norway (project #184636/S30: "Effects of changing climate on the alpine tree line and mountain forest carbon pools along 1500 km N-S and elevation gradients"). We wish to thank Viken Forest Owners Association for giving access to stand maps and data collected in the field sample survey, and to Blom Geomatics for collecting and processing the airborne laser scanner data. We are also grateful to our colleagues at the Norwegian University of Life Sciences, Dr. Ole Martin Bollandsas, Mr. Marius Hauglin, and Mr. Vegard Lien for collection and estimation of field data at the large sample plots, and to Dr. Johannes Breidenbach for valuable comments on an early draft of this article. Finally, we wish to thank the four anonymous reviewers who all provided comprehensive and relevant comments which significantly improved the manuscript. NR 68 TC 56 Z9 60 U1 5 U2 58 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC 15 PY 2011 VL 115 IS 12 BP 3599 EP 3614 DI 10.1016/j.rse.2011.08.021 PG 16 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 865LB UT WOS:000298311300053 ER PT J AU Ranson, KJ Montesano, PM Nelson, R AF Ranson, K. J. Montesano, P. M. Nelson, R. TI Object-based mapping of the circumpolar taiga-tundra ecotone with MODIS tree cover SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Taiga-tundra ecotone; MODIS; VCF; CAVM; CAPI ID RECENT CLIMATE-CHANGE; ARCTIC FOREST-TUNDRA; SATELLITE DATA; TEMPERATURE-CHANGE; TRANSITION ZONE; SHRUB EXPANSION; HIGH-LATITUDES; BOREAL FOREST; VEGETATION; PERMAFROST AB The circumpolar taiga-tundra ecotone was delineated using an image-segmentation-based mapping approach with multi-annual MODIS Vegetation Continuous Fields (VCF) tree cover data. Circumpolar tree canopy cover (TCC) throughout the ecotone was derived by averaging MODIS VCF data from 2000 to 2005 and adjusting the averaged values using linear equations relating MODIS TCC to Quickbird-derived tree cover estimates. The adjustment helped mitigate VCFs overestimation of tree cover in lightly forested regions. An image segmentation procedure was used to group pixels representing similar tree cover into polygonal features (segmentation objects) that form the map of the transition zone. Each polygon represents an area much larger than the 500 m MODIS pixel and characterizes the patterns of sparse forest patches on a regional scale. Those polygons near the boreal/tundra interface with either (1) mean adjusted TCC values from 5 to 20%, or (2) mean adjusted TCC values <5% but with a standard deviation >5% were used to identify the ecotone. Comparisons of the adjusted average tree cover data were made with (1) two existing tree line definitions aggregated for each 1 longitudinal interval in North America and Eurasia, (2) Landsat-derived Canadian proportion of forest cover for Canada, and (3) with canopy cover estimates extracted from airborne profiling lidar data that transected 1238 of the TCC polygons. The adjusted TCC from MODIS VCF shows, on average, <12% TCC for all but one regional zone at the intersection with independently delineated tree lines. Adjusted values track closely with Canadian proportion of forest cover data in areas of low tree cover. A comparison of the 1238 TCC polygons with profiling lidar measurements yielded an overall accuracy of 67.7%. Published by Elsevier Inc. C1 [Ranson, K. J.; Nelson, R.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Montesano, P. M.] Sigma Space Corp, Lanham, MD 20706 USA. RP Nelson, R (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. EM Ross.F.Nelson@nasa.gov RI Ranson, Kenneth/G-2446-2012; Nelson, Ross/H-8266-2014 OI Ranson, Kenneth/0000-0003-3806-7270; FU NASA's Earth Science Division FX This work was supported by the NASA's Earth Science Division as part of the International Polar Year program. NR 55 TC 14 Z9 15 U1 1 U2 25 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC 15 PY 2011 VL 115 IS 12 BP 3670 EP 3680 DI 10.1016/j.rse.2011.09.006 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 865LB UT WOS:000298311300059 ER PT J AU Gillespie, AR Abbott, EA Gilson, L Hulley, G Jimenez-Munoz, JC Sobrino, JA AF Gillespie, Alan R. Abbott, Elsa A. Gilson, Laura Hulley, Glynn Jimenez-Munoz, Juan-C. Sobrino, Jose A. TI Residual errors in ASTER temperature and emissivity standard products AST08 and AST05 SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE ASTER; Emissivity; Temperature; AST05; AST08; Validation ID SPACEBORNE THERMAL EMISSION; REFLECTION RADIOMETER ASTER; INFRARED MULTISPECTRAL DATA; ATMOSPHERIC CORRECTION; SURFACE-TEMPERATURE; SEPARATION ALGORITHM; VALIDATION; LAND; IMAGERY; MODIS AB Land surface temperature and emissivity are independent variables, and the thermal-infrared spectral radiance measured in remote sensing is dependent on both. Therefore the inverse Planck equation is under-determined, with two unknowns and a single measurement. Practical inversion algorithms designed to calculate temperature and emissivity from the measurements cannot do a perfect job of separation, and recovered temperature and emissivity may co-vary. For ASTER images, validation studies of recovered temperature and emissivity, regarded individually, have shown that they are within the precision and accuracy limits predicted in designing the ASTER TES algorithm used to calculate the standard products AST05 and AST08. Nevertheless, a closer look at emissivity recovered for water targets shows that emissivity appears to vary, incorrectly, as a function of temperature. One cause of this is electronic striping; another is incomplete characterization of atmospheric temperature and humidity profiles used in compensation for atmospheric absorption and path radiance. The linkage varies from band to band, with the greatest emissivity effect of 0.0003 K(-1) for ASTER band 12 (9.1 mu m) relative to band 13 (10.6 mu m). Although this inaccuracy in emissivity is small, it can approach or exceed the inaccuracy prediction of +/- 0.015 for the standard product when the entire gamut of terrestrial water and land temperatures is examined. Therefore, spatial filtering and upgrading the atmosphere compensation algorithm to use watervapor scaling should be considered in making AST05 and AST08. (C) 2011 Elsevier Inc. All rights reserved. C1 [Gillespie, Alan R.; Gilson, Laura] Univ Washington, Seattle, WA 98195 USA. [Abbott, Elsa A.; Hulley, Glynn] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Jimenez-Munoz, Juan-C.; Sobrino, Jose A.] Univ Valencia, E-46100 Burjassot, Spain. RP Gillespie, AR (reprint author), Univ Washington, Seattle, WA 98195 USA. EM arg3@uw.edu RI Sobrino, Jose/M-1585-2014; Jimenez-Munoz, Juan Carlos/K-2903-2015 OI Sobrino, Jose/0000-0003-3787-9373; Jimenez-Munoz, Juan Carlos/0000-0001-7562-4895 NR 34 TC 22 Z9 24 U1 5 U2 20 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC 15 PY 2011 VL 115 IS 12 BP 3681 EP 3694 DI 10.1016/j.rse.2011.09.007 PG 14 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 865LB UT WOS:000298311300060 ER PT J AU Pan, XJ Mannino, A Marshall, HG Filippino, KC Mulholland, MR AF Pan, Xiaoju Mannino, Antonio Marshall, Harold G. Filippino, Katherine C. Mulholland, Margaret R. TI Remote sensing of phytoplankton community composition along the northeast coast of the United States SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE CHEMTAX; Phytoplankton community; Remote sensing; United States northeast coast; MODIS-Aqua ID SATELLITE OCEAN COLOR; CHESAPEAKE BAY; CLIMATE-CHANGE; EASTERN COAST; PRIMARY PRODUCTIVITY; PIGMENT DISTRIBUTION; USA; CHLOROPHYLL; ATLANTIC; CHEMTAX AB Satellite imagery has proven to be a powerful tool for measuring chlorophyll a in surface waters. While this provides an estimate of total phytoplankton biomass, it does not distinguish between phytoplankton groups, many of which have functional differences and therefore affect biogeochemical cycles differently. Phytoplankton pigment analysis has been used to quantify a wide range of photosynthetic and accessory pigments, and chemotaxonomic analysis (e.g. CHEMTAX) has been used to successfully quantify functional taxonomic groups in nature based on pigment distributions. Here, we combine CHEMTAX analysis with satellite-derived distributions of specific phytoplankton pigments to describe the distributions of particular components of the phytoplankton community in the northeast coast of the United States from space. The spatial and seasonal variations in phytoplankton community structure elucidated through satellite remote sensing methods generally agreed with observations of abundance estimates of cell counts. Diatoms were generally the most abundant phytoplankton in this region, especially during Winter-Spring and in the inner shelf, but phytoplankton populations shifted to increasing abundance of other taxa during Summer, especially offshore. While still preliminary, satellite-derived taxa-specific information with proper regional controls holds promise for providing information on phytoplankton abundance to a taxonomic group level which would greatly improve our understanding of the impacts of human activity and climate change on ecosystems. (C) 2011 Elsevier Inc. All rights reserved. C1 [Pan, Xiaoju; Mannino, Antonio] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Marshall, Harold G.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. [Filippino, Katherine C.; Mulholland, Margaret R.] Old Dominion Univ, Dept Ocean Earth & Atmospher Sci, Norfolk, VA 23529 USA. RP Pan, XJ (reprint author), Acad Sinica, Res Ctr Environm Changes, Taipei 115, Taiwan. EM xpanx001@gmail.com RI Mannino, Antonio/I-3633-2014; Mulholland, Margaret/E-8480-2011 OI Mulholland, Margaret/0000-0001-8819-189X FU NASA FX This research was supported by an appointment to the NASA Post-doctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The work was supported by the NASA Ocean Biology and Biogeochemistry Program, Interdisciplinary Science, Biodiversity, New Investigator Program, Carbon Cycle Science and Earth Observing System programs. We thank M. Twardowski for planning the New York Bight cruises. We are grateful to T. Egerton and C. Burbage at Old Dominion University (ODU) and D. Borkman at University of Rhode Island for providing phytoplankton cell count data, and R. Zimmerman at ODU for his HPLC data submitted to the NASA SeaBASS database. We thank the captains and crews of R/V Cape Henlopen, Hugh R. Sharp, Gulf Challenger, Connecticut, and Fay Slover. We are grateful to L Van Heukelem and C. Thomas at Horn Point Laboratory for analyzing HPLC pigments, and the Ocean Biology Processing Group (OBPG) at GSFC for satellite data processing and distribution. NR 57 TC 7 Z9 8 U1 4 U2 35 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 DEC 15 PY 2011 VL 115 IS 12 BP 3731 EP 3747 DI 10.1016/j.rse.2011.09.011 PG 17 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 865LB UT WOS:000298311300064 ER PT J AU Hulley, GC Hook, SJ Schneider, P AF Hulley, Glynn C. Hook, Simon J. Schneider, Philipp TI Optimized split-window coefficients for deriving surface temperatures from inland water bodies SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Surface temperature; Lakes; Split-window coefficients; Warming; MODIS; ATSR; AVHRR ID HIGH-RESOLUTION RADIOMETER; TRACK SCANNING RADIOMETER; THERMAL INFRARED DATA; IN-FLIGHT VALIDATION; SEA-SURFACE; CLIMATE-CHANGE; LAKE TAHOE; EMISSIVITY; ALGORITHM; REFLECTION AB Large inland water bodies constituting lakes, reservoirs and inland-seas are excellent proxy indicators for climate change. Using thermal infrared satellite data, a recent study found that a global set of inland water bodies showed significant warming in seasonal nighttime lake Surface Water Temperatures (LSWTs) between 1985 and 2009. Split-window land surface temperature (LST) retrievals are typically tuned for a broad range of land surface emissivities and global atmospheric conditions, and are not optimized for inland water body surfaces, whereas split-window sea-surface temperatures (SSTs) are only tuned for a single emissivity (water), but over ocean atmospheres. Over inland water bodies, these two approaches can lead to region dependent errors in LSWTs, spurious trends, and inconsistencies between sensors in the long-term temperature record of inland water bodies. To address this issue, the primary goal of this paper was to develop a methodology for deriving a set of optimized split-window coefficients, individually tuned for the regional atmospheric conditions of 169 globally distributed, saline and freshwater inland water bodies from multiple satellite sensors including the Moderate Resolution Imaging Spectroradiometer (MODIS) on Terra and Aqua; Along Track Scanning Radiometer (ATSR) including ATSR-1, ATSR-2, AATSR; and Advanced Very High Resolution Radiometer (AVHRR-3). The new Inland Water-body Surface Temperature (IWbST) v1.0 algorithm was applied to Terra MODIS and Advanced Along Track Scanning Radiometer (AATSR) data and validated with in situ water temperature data from sites with widely contrasting atmospheric conditions: Lake Tahoe in California/Nevada, a high-elevation cool and dry site, and the Salton Sea in California, a low-elevation warm and humid site. Analysis showed improved accuracy in LSWTs in terms of bias and RMSE when compared to the standard MODIS LST and AATSR SST products. For example, the IWbST RMSE at Salton Sea was reduced by 0.4 K when compared to the operational MODIS product. For the AATSR data, the IWbST RMSE was reduced by 036 K at Tahoe and 0.29 K at Salton Sea when compared to results obtained using the operational AATSR split-window coefficients. The IWbST improvements are significant in relation to the current accuracy of water temperature retrievals from space (<0.5 K), and will enable the derivation of long-term, accurate LSWFs consistently across multiple sensors for climate studies. (C) 2011 Published by Elsevier Inc. C1 [Hulley, Glynn C.; Hook, Simon J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Schneider, Philipp] Norwegian Inst Air Res, Oslo, Norway. RP Hulley, GC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM glynn.hulley@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under the contract with the National Aeronautics and Space Administration. NR 65 TC 17 Z9 21 U1 1 U2 17 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC 15 PY 2011 VL 115 IS 12 BP 3758 EP 3769 DI 10.1016/j.rse.2011.09.014 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 865LB UT WOS:000298311300066 ER PT J AU Lazio, TJW MacDowall, RJ Burns, JO Jones, DL Weiler, KW Demaio, L Cohen, A Dalal, NP Polisensky, E Stewart, K Bale, S Gopalswamy, N Kaiser, M Kasper, J AF Lazio, T. Joseph W. MacDowall, R. J. Burns, Jack O. Jones, D. L. Weiler, K. W. Demaio, L. Cohen, A. Dalal, N. Paravastu Polisensky, E. Stewart, K. Bale, S. Gopalswamy, N. Kaiser, M. Kasper, J. TI The Radio Observatory on the Lunar Surface for Solar studies SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Heliophysics; Instrumentation: interferometers; Moon; Particle acceleration; Radio astronomy ID CORONAL MASS EJECTIONS; CYGNUS-A; BURSTS; EMISSION; INTERPLANETARY; ACCELERATION; DENSITY; EVENTS; ARRAY; SPACECRAFT AB The Radio Observatory on the Lunar Surface for Solar studies (ROLSS) is a concept for a near-side low radio frequency imaging interferometric array designed to study particle acceleration at the Sun and in the inner heliosphere. The prime science mission is to image the radio emission generated by Type II and III solar radio burst processes with the aim of determining the sites at and mechanisms by which the radiating particles are accelerated. Specific questions to be addressed include the following: (1) Isolating the sites of electron acceleration responsible for Type II and III solar radio bursts during coronal mass ejections (CMEs); and (2) Determining if and the mechanism(s) by which multiple, successive CMEs produce unusually efficient particle acceleration and intense radio emission. Secondary science goals include constraining the density of the lunar ionosphere by searching for a low radio frequency cutoff to solar radio emission and constraining the low energy electron population in astrophysical sources. Key design requirements on ROLSS include the operational frequency and angular resolution. The electron densities in the solar corona and inner heliosphere are such that the relevant emission occurs at frequencies below 10 MHz. Second, resolving the potential sites of particle acceleration requires an instrument with an angular resolution of at least 2 degrees, equivalent to a linear array size of approximately 1000 m. Operations would consist of data acquisition during the lunar day, with regular data downlinks. No operations would occur during lunar night. ROLSS is envisioned as an interferometric array, because a single aperture would be impractically large. The major components of the ROLSS array are 3 antenna arms arranged in a Y shape, with a central electronics package (CEP) located at the center. The Y configuration for the antenna arms both allows for the formation of reasonably high dynamic range images on short time scales as well as relatively easy deployment. Each antenna arm is a linear strip of polyimide film (e.g., Kapton (TM)) on which 16 science antennas are located by depositing a conductor (e.g., silver). The antenna arms can be rolled for transport, with deployment consisting of unrolling the rolls. Each science antenna is a single polarization dipole. The arms also contain transmission lines for carrying the radio signals from the science antennas to the CEP. The CEP itself houses the receivers for the science antennas, the command and data handling hardware, and, mounted externally, the downlink antenna. We have conducted two experiments relevant to the ROLSS concept. First, we deployed a proof-of-concept science antenna. Comparison of the impedance of the antenna feed points with simulations showed a high level of agreement, lending credence to the antenna concept. Second, we exposed a sample of space-qualified polyimide film, with a silver coating on one side, to temperature cycling and UV exposure designed to replicate a year on the lunar surface. No degradation of the polyimide film's material or electric properties was found. Both of these tests support the notion of using polyimide-film based antennas. The prime science mission favors an equatorial site, and a site on the limb could simplify certain aspects of the instrument design. A site on the lunar near side is sufficient for meeting the science goals. While the site should be of relatively low relief topography, the entire site does not have to be flat as the fraction of the area occupied by the antenna arms is relatively small (similar to 0.3%). Further, the antenna arms do not have to lay flat as deviations of +/- 1 m are still small relative to the observational wavelengths. Deployment could be accomplished either with astronauts, completely robotically, or via a combination of crewed and robotic means. Future work for the ROLSS concept includes more exhaustive testing of the radio frequency (RF) and environmental suitability of polyimide film-based science antennas, ultra-low power electronics in order to minimize the amount of power storage needed, batteries with a larger temperature range for both survival and operation, and rovers (robotic, crewed, or both) for deployment. The ROLSS array could also serve as the precursor to a larger array on the far side of the Moon for astrophysical and cosmological studies. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Lazio, T. Joseph W.; Weiler, K. W.; Polisensky, E.; Stewart, K.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Lazio, T. Joseph W.; MacDowall, R. J.; Burns, Jack O.; Jones, D. L.; Weiler, K. W.] NASA, Ames Res Ctr, Lunar Sci Inst, Sunnyvale, CA 94089 USA. [MacDowall, R. J.; Demaio, L.; Gopalswamy, N.; Kaiser, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Burns, Jack O.] Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Jones, D. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cohen, A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Bale, S.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Bale, S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Kasper, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lazio, TJW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Joseph.Lazio@jpl.nasa.gov RI Bale, Stuart/E-7533-2011; MacDowall, Robert/D-2773-2012; Gopalswamy, Nat/D-3659-2012; Kasper, Justin/D-1152-2010 OI Bale, Stuart/0000-0002-1989-3596; Kasper, Justin/0000-0002-7077-930X FU NASA [NNA09DB30A] FX We thank J. Schmidt for helpful discussions about the implementation of CME models for ROLSS, the crew of the GSFC IDL for their assistance in refining the design, and the editor for her patience and assistance in making sure that this manuscript was published. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The ROLSS concept study was funded by the NASA Lunar Sortie Science Opportunities (LSSO) program. The LUNAR consortium is funded by the NASA Lunar Science Institute (via Cooperative Agreement NNA09DB30A) to investigate concepts for astrophysical observatories on the Moon. NR 46 TC 7 Z9 8 U1 0 U2 5 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD DEC 15 PY 2011 VL 48 IS 12 BP 1942 EP 1957 DI 10.1016/j.asr.2011.07.006 PG 16 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 847UP UT WOS:000296998300003 ER PT J AU Bryson, KL Peeters, Z Salama, F Foing, B Ehrenfreund, P Ricco, AJ Jessberger, E Bischoff, A Breitfellner, M Schmidt, W Robert, F AF Bryson, K. L. Peeters, Z. Salama, F. Foing, B. Ehrenfreund, P. Ricco, A. J. Jessberger, E. Bischoff, A. Breitfellner, M. Schmidt, W. Robert, F. TI The ORGANIC experiment on EXPOSE-R on the ISS: Flight sample preparation and ground control spectroscopy SO ADVANCES IN SPACE RESEARCH LA English DT Article DE PAHS; EXPOSE-R; ISS; Astrobiology ID POLYCYCLIC AROMATIC-HYDROCARBONS; DIFFUSE INTERSTELLAR-MEDIUM; ABSORPTION-SPECTRA; THIN-FILMS; INFRARED-SPECTRA; PERYLENE C20H12; PAHS; C-60; BANDS; C-70 AB In March of 2009, the ORGANIC experiment integrated into the European multi-user facility EXPOSE-R, containing experiments dedicated to Astrobiology, was mounted through Extra Vehicular Activity (EVA) externally on the International Space Station (ISS). The experiment exposed organic samples of astronomical interest for a duration of 97 weeks (similar to 22 months) to the space environment. The samples that were returned to Earth in spring 2011, received a total UV radiation dose during their exposure including direct solar irradiation of >2500 h, exceeding the limits of laboratory simulations. We report flight sample preparation and pre-flight ultraviolet-visible (UV-Vis) characterization of the ORGANIC samples, which include 11 polycyclic aromatic hydrocarbons (PAHs) and three fullerenes. The corresponding time-dependent ground control monitoring experiments for ORGANIC measured over similar to 19 months are presented and the results anticipated upon return of the samples are discussed. We present the first UV-Vis spectrum of solid circobiphenyl (C38H16). Further, we present the first published UV-Vis spectra of diphenanthro[9,10-b',10'-d]thiophene (C28H16S), dinaphtho[8,1,2-abc,2',1',8'-klm]coronene (C36H16), tetrabenzo[de,no,st,c'd']heptacene (C42H22), and dibenzo[jk,a'b']octacene (C40H22) in solid phase and in solution. The results of the ORGANIC experiment are expected to enhance our knowledge of the evolution and degradation of large carbon-containing molecules in space environments. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Bryson, K. L.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Peeters, Z.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Bryson, K. L.; Salama, F.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Foing, B.] European Space Agcy, ESTEC, NL-2200 AG Noordwijk, Netherlands. [Ehrenfreund, P.] Leiden Univ, Leiden Inst Chem, NL-2300 RA Leiden, Netherlands. [Ehrenfreund, P.] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA. [Ricco, A. J.] NASA, Ames Res Ctr, Small Spacecraft Div, Moffett Field, CA 94035 USA. [Jessberger, E.; Bischoff, A.] Inst Planetol, D-48149 Munster, Germany. [Breitfellner, M.] ESA, European Space Astron Ctr ESAC, Madrid 28080, Spain. [Schmidt, W.] Inst PAH Forsch, D-86926 Greifenberg, Germany. [Robert, F.] CNRS, Museum Natl Hist Nat, INSU, LMCM,UMR 7202, F-75231 Paris 05, France. RP Bryson, KL (reprint author), Bay Area Environm Res Inst, 560 3rd St W, Sonoma, CA 95476 USA. EM kathryn.bryson@nasa.gov RI Ricco, Antonio/A-5273-2010; Bryson, Kathryn/I-6914-2012; Salama, Farid/A-8787-2009; OI Salama, Farid/0000-0002-6064-4401; Ricco, Antonio/0000-0002-2355-4984 FU ESA; NASA's Science Mission Directorate through the Astronomy and Physics Research and Analysis; Netherlands Space Office NSO; NASA Astrobiology Institute FX The authors acknowledge the support of ESA Human Spaceflight and Microgravity Program and NASA's Science Mission Directorate through the Astronomy and Physics Research and Analysis and NASA Astrobiology Institute programs. We acknowledge the NASA Astrobiology Institute and the Netherlands Space Office NSO as funding sources. The authors thank E. Monaghan and D. Wills for their support in the flight preparations. The authors acknowledge the outstanding technical support provided by R. Walker in the Astrophysics and Astrochemistry Laboratory at NASA Ames Research Center. NR 51 TC 5 Z9 5 U1 1 U2 14 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD DEC 15 PY 2011 VL 48 IS 12 BP 1980 EP 1996 DI 10.1016/j.asr.2011.07.017 PG 17 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 847UP UT WOS:000296998300006 ER PT J AU Drouin, BJ Yu, SS Pearson, JC Gupta, H AF Drouin, Brian J. Yu, Shanshan Pearson, John C. Gupta, Harshal TI Terahertz spectroscopy for space applications: 2.5-2.7 THz spectra of HD, H2O and NH3 SO JOURNAL OF MOLECULAR STRUCTURE LA English DT Article DE Rotational spectroscopy; Terahertz spectroscopy; Atmospheric species; Astrophysical species ID HERSCHEL/HIFI OBSERVATIONS; ROTATIONAL SPECTRUM; HETERODYNE INSTRUMENT; FREQUENCY-MEASUREMENT; INTERSTELLAR OH+; G10.6-0.4 W31C; SIGHT-LINE; WATER; STATE; EMISSION AB At the Jet Propulsion Laboratory (JPL) a vibrant THz development program supports the construction of space-based spectroscopic instruments. The recent successes of the Aura's Microwave Limb Sounder (0.1-2.5 THz) and Herschel's Heterodyne Instrument for the Far-Infrared (0.5-1.9 THz) have demonstrated the wide range of molecular astro- and geophysics accessible when remote sensing from a space platform. With access to the THz spectral range these instruments readily observe the rotational spectra of small molecules, and the laboratory spectroscopy of these molecules is then utilized to convert the remote observation into physical quantities such as density and temperature. At the JPL millimeter and submillimeter spectroscopy laboratory we utilize the same technology developed for the space missions in order to make new or improved spectroscopic measurements that support these remote sensing objectives. By virtue of the improvements in technology these new measurements often result in improved structural understanding for the species of interest. We present an overview of the space applications and report a series of improved measurements in the 2.5-2.7 THz range obtained with our most recent hardware under development for sub-orbital/orbital astronomy. Published by Elsevier B.V. C1 [Drouin, Brian J.; Yu, Shanshan; Pearson, John C.; Gupta, Harshal] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Drouin, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM brian.j.drouin@jpl.nasa.gov RI Yu, Shanshan/D-8733-2016 FU National Aeronautics and Space Administration FX The authors thank Shuhui Wang for providing the EMLS OH figures. This paper presents research carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 60 TC 18 Z9 18 U1 1 U2 29 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-2860 J9 J MOL STRUCT JI J. Mol. Struct. PD DEC 14 PY 2011 VL 1006 IS 1-3 BP 2 EP 12 DI 10.1016/j.molstruc.2011.05.062 PG 11 WC Chemistry, Physical SC Chemistry GA 877AF UT WOS:000299148200002 ER PT J AU Krasnicki, A Kisiel, Z Drouin, BJ Pearson, JC AF Krasnicki, Adam Kisiel, Zbigniew Drouin, Brian J. Pearson, John C. TI Terahertz spectroscopy of isotopic acrylonitrile SO JOURNAL OF MOLECULAR STRUCTURE LA English DT Article DE THz rotational spectrum; Isotopic species; Interstate perturbations; Structure ID DEPENDENCE MOLECULAR-STRUCTURES; VINYL CYANIDE; ROTATIONAL SPECTRUM; HYPERFINE-STRUCTURE; MICROWAVE-SPECTRUM; H2C=CH-CN; CONSTANTS; STATES AB Rotational spectra of four isotopically enriched, singly substituted species of acrylonitrile have been studied up to 1.2 THz. Extensive analysis of the spectra recorded for (H2C)-C-13=CHCN, H2C=(CHCN)-C-13, H2C=(CHCN)-N-15, and H2C=CDCN, revealed the presence of the same characteristic perturbations between the ground state and the nu(11) = 1 excited vibrational state, that have recently been identified in the parent molecule. For this reason transitions in nu(11) = 1 have also been assigned in each of the four isotopic species and a coupled state analysis of g.s. and nu(11) = 1 was performed on a total of around 3000 lines for each species. The derived precise values of E(nu(11), = 1) are found to be consistent with estimates from anharmonic force field calculations. In addition, transitions for six new doubly substituted isotopic species of acrylonitrile, (H2C)-C-13=(CHCN)-C-13, (H2C)-C-13=(CHCN)-C-13, H2C=(CHCN)-C-13-C-13, (H2C)-C-13=(CHCN)-N-15, H2C=(CHCN)-C-13-N-15, and H2C=(CHCN)-C-13-N-15, have been assigned, and their ground state spectroscopic constants have been determined. Rotational constants for all known isotopic species of acrylonitrile have been combined with ab initio calculation of vibration-rotation constants in the first evaluation of the r(e)(SE) geometry of this molecule. (C) 2011 Elsevier B.V. All rights reserved. C1 [Krasnicki, Adam; Kisiel, Zbigniew] Polish Acad Sci, Inst Phys, PL-02668 Warsaw, Poland. [Drouin, Brian J.; Pearson, John C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kisiel, Z (reprint author), Polish Acad Sci, Inst Phys, Al Lotnikow 32-46, PL-02668 Warsaw, Poland. EM kisiel@ifpan.edu.pl RI Kisiel, Zbigniew/K-8798-2016 OI Kisiel, Zbigniew/0000-0002-2570-3154 FU Polish Ministry of Science and Higher Education [N-N202-0541-33]; National Aeronautics and Space Administration FX This paper presents research carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The Warsaw authors acknowledge financial support from the Polish Ministry of Science and Higher Education, Grant No. N-N202-0541-33. NR 30 TC 10 Z9 10 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-2860 J9 J MOL STRUCT JI J. Mol. Struct. PD DEC 14 PY 2011 VL 1006 IS 1-3 BP 20 EP 27 DI 10.1016/j.molstruc.2011.05.050 PG 8 WC Chemistry, Physical SC Chemistry GA 877AF UT WOS:000299148200004 ER PT J AU Schriver, D Travnicek, PM Anderson, BJ Ashour-Abdalla, M Baker, DN Benna, M Boardsen, SA Gold, RE Hellinger, P Ho, GC Korth, H Krimigis, SM McNutt, RL Raines, JM Richard, RL Slavin, JA Solomon, SC Starr, RD Zurbuchen, TH AF Schriver, David Travnicek, Pavel M. Anderson, Brian J. Ashour-Abdalla, Maha Baker, Daniel N. Benna, Mehda Boardsen, Scott A. Gold, Robert E. Hellinger, Petr Ho, George C. Korth, Haje Krimigis, Stamatios M. McNutt, Ralph L., Jr. Raines, Jim M. Richard, Robert L. Slavin, James A. Solomon, Sean C. Starr, Richard D. Zurbuchen, Thomas H. TI Quasi-trapped ion and electron populations at Mercury SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MESSENGERS 1ST FLYBY; MAGNETIC-FIELD; MAGNETOSPHERE; INSTRUMENT; PROTONS AB Mariner 10 and MESSENGER spacecraft observations have established that Mercury has an intrinsic magnetic field and magnetosphere. Following the March 2011 insertion of MESSENGER into orbit around Mercury, measurements show that ions and electrons with typical energies of about 1-10 keV form an equatorially centered distribution of plasma at 1.4 R-M radial distance (where R-M is Mercury's radius) around a substantial portion of the planet in local time from morning through night and into the afternoon sector. Coincident with the detection of plasma around Mercury, an observed drop in the total magnetic pressure is attributable to the ion and electron thermal pressure. Additionally, intense waves near the ion cyclotron frequency were observed at the same location as the quasi-trapped particle population, which are likely a result of anisotropic distributions created by the large loss cone (>30 degrees) at these radial distances. Citation: Schriver, D., et al. (2011), Quasi-trapped ion and electron populations at Mercury, Geophys. Res. Lett., 38, L23103, doi:10.1029/2011GL049629. C1 [Schriver, David; Ashour-Abdalla, Maha; Richard, Robert L.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Anderson, Brian J.; Gold, Robert E.; Ho, George C.; Korth, Haje; Krimigis, Stamatios M.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Baker, Daniel N.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. [Benna, Mehda] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Boardsen, Scott A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Travnicek, Pavel M.; Hellinger, Petr] AS CR, Astron Inst, Prague 14131, Czech Republic. [Travnicek, Pavel M.; Hellinger, Petr] AS CR, Inst Atmospher Phys, Prague 14131, Czech Republic. [Raines, Jim M.; Slavin, James A.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Travnicek, Pavel M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Schriver, D (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. EM dave@igpp.ucla.edu RI Benna, Mehdi/F-3489-2012; Ho, George/G-3650-2015; Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; Hellinger, Petr/F-5267-2014; Travnicek, Pavel/G-8608-2014; McNutt, Ralph/E-8006-2010 OI Ho, George/0000-0003-1093-2066; Slavin, James/0000-0002-9206-724X; Hellinger, Petr/0000-0002-5608-0834; McNutt, Ralph/0000-0002-4722-9166 FU NASA MESSENGER [NNX07AR62G, NNX07AV79G, NNX09AD41G]; Czech Ministry of Education [ME09009] FX This work was supported by NASA MESSENGER grants NNX07AR62G, NNX07AV79G, and NNX09AD41G and contract ME09009 from the Czech Ministry of Education. Computing was carried out with NASA Advanced Supercomputing systems, NSF NCAR Frost Blue Gene, and the computing facility at the Institute of Atmospheric Physics, Prague, Czech Republic. NR 26 TC 16 Z9 16 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 14 PY 2011 VL 38 AR L23103 DI 10.1029/2011GL049629 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 864SW UT WOS:000298261400003 ER PT J AU Vincent, P Buckley, SM Yang, D Carle, SF AF Vincent, P. Buckley, S. M. Yang, D. Carle, S. F. TI Anomalous transient uplift observed at the Lop Nor, China nuclear test site using satellite radar interferometry time-series analysis SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EXPLOSIONS; SUBSIDENCE; CALIFORNIA; LOCATIONS; VALLEY AB Anomalous uplift is observed at the Lop Nor, China nuclear test site using ERS satellite SAR data. Using an InSAR time-series analysis method, we show that an increase in absolute uplift with time is observed between 1997 and 1999. The signal is collocated with past underground nuclear tests. Due to the collocation in space with past underground tests we postulate a nuclear test-related hydrothermal source for the uplift signal. A possible mechanism is presented that can account for the observed transient uplift and is consistent with documented thermal regimes associated with underground nuclear tests conducted at the Nevada National Security Site (NNSS) (formerly the Nevada Test Site). Citation: Vincent, P., S. M. Buckley, D. Yang, and S. F. Carle (2011), Anomalous transient uplift observed at the Lop Nor, China nuclear test site using satellite radar interferometry time-series analysis, Geophys. Res. Lett., 38, L23306, doi:10.1029/2011GL049302. C1 [Vincent, P.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Buckley, S. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Carle, S. F.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. [Yang, D.] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78731 USA. [Yang, D.] Univ Texas Austin, Ctr Space Res, Austin, TX 78731 USA. RP Vincent, P (reprint author), Oregon State Univ, Coll Earth Ocean & Atmospher Sci, 104 COAS Adm Bldg, Corvallis, OR 97331 USA. EM pvincent@coas.oregonstate.edu FU U.S. Department of Energy [DE-FC52-03NA995661, W-7405-ENG-482] FX This work was supported by the U.S. Department of Energy Contract Numbers DE-FC52-03NA995661 and W-7405-ENG-482. The authors would like to thank helpful reviews by David Hafemeister and an anonymous reviewer. NR 24 TC 1 Z9 1 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 14 PY 2011 VL 38 AR L23306 DI 10.1029/2011GL049302 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 864SW UT WOS:000298261400001 ER PT J AU Du, AM Tsurutani, BT Sun, W AF Du, A. M. Tsurutani, B. T. Sun, W. TI Solar wind energy input during prolonged, intense northward interplanetary magnetic fields: A new coupling function SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID STORM SUDDEN COMMENCEMENTS; GEOMAGNETIC STORMS; SUBSTORMS; SHOCK; MAGNETOSPHERE; EVENTS; CLOUDS; MODEL; POLAR; IMF AB Sudden energy release (ER) events in the midnight sector auroral zone during intense (B > 10 nT), long-duration (T > 3 h), northward (N = B-z > 0 nT) IMF magnetic clouds (MCs) during solar cycle 23 (SC23) have been examined in detail. The MCs with northward-then-southward (NS) IMFs were analyzed separately from MCs with southward-then-northward (SN) configurations. It is found that there is a lack of ER/substorms during the N field intervals of NS clouds. In sharp contrast, ER events do occur during the N field portions of SN MCs. From the above two results it is reasonable to conclude that the latter ER events represent residual energy remaining from the preceding S portions of the SN MCs. We derive a new solar wind-magnetosphere coupling function during northward IMFs: E-NIMF = alpha N (1/12) V-7/3 B-1/2 + beta V vertical bar Dst(min)vertical bar. The first term on the right-hand side of the equation represents the energy input via "viscous interaction," and the second term indicates the residual energy stored in the magnetotail. It is empirically found that the magnetotail/magnetosphere/ionosphere can store energy for a maximum of similar to 4 h before it has dissipated away. This concept is defining one for ER/substorm energy storage. Our scenario indicates that the rate of solar wind energy injection into the magnetotail/magnetosphere/ionosphere for storage determines the potential form of energy release into the magnetosphere/ionosphere. This may be more important to understand solar wind-magnetosphere coupling than the dissipation mechanism itself (in understanding the form of the release). The concept of short-term energy storage is also applied for the solar case. It is argued that it may be necessary to identify the rate of energy input into solar magnetic loop systems to be able to predict the occurrence of solar flares. C1 [Du, A. M.] Chinese Acad Sci, Inst Geol & Geophys, Beijing 100029, Peoples R China. [Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sun, W.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. RP Du, AM (reprint author), Chinese Acad Sci, Inst Geol & Geophys, Beijing 100029, Peoples R China. EM amdu@mail.iggcas.ac.cn FU NSFC [41031066, 41174122]; OPWSRP [201005017]; NASA FX We acknowledge the CDAWeb for access to the ACE, Polar, IMAGE, and GOES data. SOPA energetic proton and electron spin-averaged differential flux measurements are afforded by Los Alamos National Laboratory. We especially thank S. B. Mende and Harald Frey for the use of IMAGE FUV WIC data. The AE data are provided by the World Data Center for Geomagnetism at Kyoto University. This work was supported by NSFC grants (41031066), NSFC (41174122) and supported by OPWSRP (201005017). Portions of the work were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 51 TC 19 Z9 20 U1 4 U2 18 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 DEC 14 PY 2011 VL 116 AR A12215 DI 10.1029/2011JA016718 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 864TI UT WOS:000298262600002 ER PT J AU Navarro-Gonzalez, R Mckay, CP AF Navarro-Gonzalez, Rafael McKay, Christopher P. TI Reply to comment by Biemann and Bada on "Reanalysis of the Viking results suggests perchlorate and organics at midlatitudes on Mars" SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Editorial Material ID CHROMATOGRAPH-MASS SPECTROMETER; SOILS; DEHYDROGENATION; AROMATIZATION; CATALYSTS; PHOENIX; SEARCH; DESERT C1 [Navarro-Gonzalez, Rafael] Univ Nacl Autonoma Mexico, Lab Quim Plasmas & Estudios Planetarios, Inst Ciencias Nucl, Mexico City, DF, Mexico. [McKay, Christopher P.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Navarro-Gonzalez, R (reprint author), Univ Nacl Autonoma Mexico, Lab Quim Plasmas & Estudios Planetarios, Inst Ciencias Nucl, Ciudad Univ,Apartado Postal 70-543, Mexico City, DF, Mexico. EM navarro@nucleares.unam.mx RI Gonzalez, Rafael/D-1748-2009 NR 24 TC 2 Z9 2 U1 3 U2 19 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 13 PY 2011 VL 116 AR E12002 DI 10.1029/2011JE003880 PG 6 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 864QD UT WOS:000298253900002 ER PT J AU Vanderveld, RA Caldwell, RR Rhodes, J AF Vanderveld, R. Ali Caldwell, Robert R. Rhodes, Jason TI Second-order weak lensing from modified gravity SO PHYSICAL REVIEW D LA English DT Article ID POST-NEWTONIAN APPROXIMATION; COSMOLOGICAL PARAMETERS; POWER SPECTRUM; BISPECTRUM; DEFLECTION; SHEAR AB We explore the sensitivity of weak gravitational lensing to second-order corrections to the spacetime metric within a cosmological adaptation of the parametrized post-Newtonian framework. Whereas one might expect nonlinearities of the gravitational field to introduce non-Gaussianity into the statistics of the lensing convergence field, we show that such corrections are actually always small within a broad class of scalar-tensor theories of gravity. We show this by first computing the weak lensing convergence within our parametrized framework to second order in the gravitational potential, and then computing the relevant post-Newtonian parameters for scalar-tensor gravity theories. In doing so we show that this potential systematic factor is generically negligible, thus clearing the way for weak lensing to provide a direct tracer of mass on cosmological scales for a wide class of gravity theories despite uncertainties in the precise nature of the departures from general relativity. C1 [Vanderveld, R. Ali; Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vanderveld, R. Ali; Rhodes, Jason] CALTECH, Pasadena, CA 91125 USA. [Vanderveld, R. Ali] Univ Chicago, Enrico Fermi Inst, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Caldwell, Robert R.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. RP Vanderveld, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Caldwell, Robert/0000-0001-7490-7463 FU NASA; JPL Strategic University Research Partnership (SURP); Kavli Institute for Cosmological Physics at the University of Chicago through NSF [PHY-0114422 \, PHY-0551142]; Kavli Foundation FX We thank Wayne Hu, Mark Wyman, Scott Dodelson, and Christopher Berry for useful conversations. This research was carried out in part at the Jet Propulsion Laboratory, run by the California Institute of Technology under a contract from NASA, and Dartmouth College and was funded through the JPL Strategic University Research Partnership (SURP) Program. We also acknowledge the support of the Kavli Institute for Cosmological Physics at the University of Chicago through NSF Grant Nos. PHY-0114422 and PHY-0551142 and an endowment from the Kavli Foundation and its founder Fred Kavli. NR 36 TC 6 Z9 6 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD DEC 12 PY 2011 VL 84 IS 12 AR 123510 DI 10.1103/PhysRevD.84.123510 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 860HD UT WOS:000297938500003 ER PT J AU Beichman, CA Lisse, CM Tanner, AM Bryden, G Akeson, RL Ciardi, DR Boden, AF Dodson-Robinson, SE Salyk, C Wyatt, MC AF Beichman, C. A. Lisse, C. M. Tanner, A. M. Bryden, G. Akeson, R. L. Ciardi, D. R. Boden, A. F. Dodson-Robinson, S. E. Salyk, C. Wyatt, M. C. TI MULTI-EPOCH OBSERVATIONS OF HD 69830: HIGH-RESOLUTION SPECTROSCOPY AND LIMITS TO VARIABILITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: planetary systems; Kuiper belt: general; planets and satellites: dynamical evolution and stability; planet-disk interactions; stars: individual (HD 69830); zodiacal dust ID SPITZER-SPACE-TELESCOPE; SOLAR-TYPE STARS; SUN-LIKE STARS; INFRARED INTERFEROMETRIC SURVEY; DEBRIS DISKS; HOT DUST; ABSOLUTE CALIBRATION; EPSILON-ERIDANI; COLLISIONAL EVOLUTION; SIZE DISTRIBUTIONS AB The main-sequence solar-type star HD 69830 has an unusually large amount of dusty debris orbiting close to three planets found via the radial velocity technique. In order to explore the dynamical interaction between the dust and planets, we have performed multi-epoch photometry and spectroscopy of the system over several orbits of the outer dust. We find no evidence for changes in either the dust amount or its composition, with upper limits of 5%-7% (1 sigma per spectral element) on the variability of the dust spectrum over 1 year, 3.3% (1 sigma) on the broadband disk emission over 4 years, and 33% (1 sigma) on the broadband disk emission over 24 years. Detailed modeling of the spectrum of the emitting dust indicates that the dust is located outside of the orbits of the three planets and has a composition similar to main-belt, C-type asteroids in our solar system. Additionally, we find no evidence for a wide variety of gas species associated with the dust. Our new higher signal-to-noise spectra do not confirm our previously claimed detection of H(2)O ice leading to a firm conclusion that the debris can be associated with the break-up of one or more C-type asteroids formed in the dry, inner regions of the protoplanetary disk of the HD 69830 system. The modeling of the spectral energy distribution and high spatial resolution observations in the mid-infrared are consistent with a similar to 1 AU location for the emitting material. C1 [Beichman, C. A.; Tanner, A. M.; Bryden, G.; Akeson, R. L.; Ciardi, D. R.] CALTECH, Jet Prop Lab, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Lisse, C. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Tanner, A. M.] MSU, Dept Phys & Astron, Mississippi State, MS 39762 USA. [Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Boden, A. F.] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. [Dodson-Robinson, S. E.; Salyk, C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Wyatt, M. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Beichman, CA (reprint author), CALTECH, Jet Prop Lab, NASA Exoplanet Sci Inst, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM chas@pop.jpl.nasa.gov RI Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Ciardi, David/0000-0002-5741-3047 FU National Aeronautics and Space Administration FX We are grateful to an anonymous referee for a careful reading of this manuscript that led to significant improvements. This publication makes use of services provided by the NASA Exoplanet Science Institute at the California Institute of Technology (NExScI) and data products from the NASA/NExScI Star & Exoplanet Database (NStED), the Two Micron All Sky Survey (2MASS), and the NASA/IPAC Infrared Science Archive (IRSA). Thanks to Ben Oppenheimer, Dimitar Sasselov, and Dave Latham for their hospitality and support during extended visits to AMNH and CfA, respectively. Some of the research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The Keck Interferometer is funded by the National Aeronautics and Space Administration as part of its Exoplanet Exploration program. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Government sponsorship acknowledged. NR 78 TC 14 Z9 14 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2011 VL 743 IS 1 AR 85 DI 10.1088/0004-637X/743/1/85 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 853EF UT WOS:000297408300085 ER PT J AU Chung, SM Eisenhardt, PR Gonzalez, AH Stanford, SA Brodwin, M Stern, D Jarrett, T AF Chung, Sun Mi Eisenhardt, Peter R. Gonzalez, Anthony H. Stanford, Spencer A. Brodwin, Mark Stern, Daniel Jarrett, Thomas TI A WISE VIEW OF STAR FORMATION IN LOCAL GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: evolution; galaxies: star formation; infrared: galaxies ID INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; LOW-DENSITY ENVIRONMENTS; FORMATION RATES; INFRARED GALAXIES; H-ALPHA; LUMINOSITY FUNCTIONS; DATA RELEASE; EVOLUTION; DEPENDENCE AB We present results from a systematic study of star formation in local galaxy clusters using 22 mu m data from the Wide-field Infrared Survey Explorer ( WISE). The 69 systems in our sample are drawn from the Cluster Infall Regions Survey, and all have robust mass determinations. The all-sky WISE data enable us to quantify the amount of star formation, as traced by 22 mu m, as a function of radius well beyond R-200, and investigate the dependence of total star formation rate upon cluster mass. We find that the fraction of star-forming galaxies increases with cluster radius but remains below the field value even at 3R(200). We also find that there is no strong correlation between the mass-normalized total specific star formation rate and cluster mass, indicating that the mass of the host cluster does not strongly influence the total star formation rate of cluster members. C1 [Chung, Sun Mi; Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Eisenhardt, Peter R.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Stanford, Spencer A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Brodwin, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jarrett, Thomas] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Chung, SM (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA. EM schung@astro.ufl.edu FU National Aeronautics and Space Administration FX This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The authors thank Emilio Donoso for his help and advice on navigating the SDSS database. We also thank the anonymous referee for a careful reading and comments which improved the paper. NR 56 TC 18 Z9 18 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2011 VL 743 IS 1 AR 34 DI 10.1088/0004-637X/743/1/34 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 853EF UT WOS:000297408300034 ER PT J AU Cushing, MC Kirkpatrick, JD Gelino, CR Griffith, RL Skrutskie, MF Mainzer, A Marsh, KA Beichman, CA Burgasser, AJ Prato, LA Simcoe, RA Marley, MS Saumon, D Freedman, RS Eisenhardt, PR Wright, EL AF Cushing, Michael C. Kirkpatrick, J. Davy Gelino, Christopher R. Griffith, Roger L. Skrutskie, Michael F. Mainzer, A. Marsh, Kenneth A. Beichman, Charles A. Burgasser, Adam J. Prato, Lisa A. Simcoe, Robert A. Marley, Mark S. Saumon, D. Freedman, Richard S. Eisenhardt, Peter R. Wright, Edward L. TI THE DISCOVERY OF Y DWARFS USING DATA FROM THE WIDE-FIELD INFRARED SURVEY EXPLORER (WISE) SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; infrared: stars; stars: individual (UGPS J072227.51-054031.2, WISEPC J014807.25, 720258.8, WISEP J041022.71+150248.5, WISEPC J140518.40+553421.5, WISEP J154151.65225025.2, WISEP J173835.52+273258.9, WISEP J182831.08+265037.8, WISEPC J205628.90+145953.3); stars: low-mass ID COOL BROWN DWARF; SUBSTELLAR MASS FUNCTION; SPITZER-SPACE-TELESCOPE; ADAPTIVE OPTICS SYSTEM; KECK-II-TELESCOPE; SKY SURVEY 2MASS; T-DWARFS; CHEMICAL-EQUILIBRIUM; SPECTRAL CLASSIFICATION; ECHELLE SPECTROGRAPH AB We present the discovery of seven ultracool brown dwarfs identified with the Wide-field Infrared Survey Explorer (WISE). Near-infrared spectroscopy reveals deep absorption bands of H2O and CH4 that indicate all seven of the brown dwarfs have spectral types later than UGPS J072227.51-054031.2, the latest-type T dwarf currently known. The spectrum of WISEP J182831.08+ 265037.8 is distinct in that the heights of the J- and H-band peaks are approximately equal in units of f lambda, so we identify it as the archetypal member of the Y spectral class. The spectra of at least two of the other brown dwarfs exhibit absorption on the blue wing of the H-band peak that we tentatively ascribe to NH3. These spectral morphological changes provide a clear transition between the T dwarfs and the Y dwarfs. In order to produce a smooth near-infrared spectral sequence across the T/Y dwarf transition, we have reclassified UGPS 0722-05 as the T9 spectral standard and tentatively assign WISEP J173835.52+ 273258.9 as the Y0 spectral standard. In total, six of the seven new brown dwarfs are classified as Y dwarfs: four are classified as Y0, one is classified as Y0 (pec?), and WISEP J1828+ 2650 is classified as > Y0. We have also compared the spectra to the model atmospheres of Marley and Saumon and infer that the brown dwarfs have effective temperatures ranging from 300 K to 500 K, making them the coldest spectroscopically confirmed brown dwarfs known to date. C1 [Kirkpatrick, J. Davy; Gelino, Christopher R.; Griffith, Roger L.; Marsh, Kenneth A.; Beichman, Charles A.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Burgasser, Adam J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Burgasser, Adam J.; Simcoe, Robert A.] MIT, Cambridge, MA 02139 USA. [Prato, Lisa A.] Lowell Observ, Flagstaff, AZ 86001 USA. [Marley, Mark S.; Freedman, Richard S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Saumon, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Wright, Edward L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Cushing, Michael C.; Mainzer, A.; Eisenhardt, Peter R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cushing, MC (reprint author), Univ Toledo, Dept Phys & Astron, 2801 W Bancroft St, Toledo, OH 43606 USA. EM michael.cushing@gmail.com RI Marley, Mark/I-4704-2013; OI Marley, Mark/0000-0002-5251-2943 FU NASA; National Aeronautics and Space Administration; National Science Foundation; Alfred P. Sloan Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; W. M. Keck Foundation; Harvard University Milton Fund; University of Virginia; SAO; University of California, Berkeley; NOAO through the Telescope System Instrumentation Program (TSIP) [2010B-0184]; National Aeronautics and Space Administration [NNG06GH50G]; Chris and Warren Hellman Fellowship FX We thank Tom Jarrett for guidance with the WIRC data reduction, Barry Rothberg, and Norbert Pirzkal for their guidance in reducing the HST/WFC3 data, and Ben Burningham, Sandy Leggett, and Mike Liu for providing digital copies of late-type T dwarf spectra. We also thank Mauricio Martinez, Jorge Araya, and Nidia Morrell for observing support at Magellan. M. S. M. and D. S. acknowledge the support of the NASA ATP program. This publication makes use of data products from the Wide-field Infrared Survey Explorer, the Two Micron All Sky Survey (2MASS), and the Sloan Digital Sky Survey (SDSS). The Wide-field Infrared Survey Explorer 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. 2MASS is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. SDSS is funded 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. This research has made use of the NASA/IPAC Infrared Science Archive (IRSA), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Our research has also benefited from the M, L, and T dwarf compendium housed at DwarfArchives. org whose server was funded by a NASA Small Research Grant, administered by the American Astronomical Society and the SpeX Prism Spectral Libraries, maintained by Adam Burgasser at http://www.browndwarfs.org/spexprism. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This paper also includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile and the Peters Automated Infrared Imaging Telescope (PAIRITEL) which is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, the camera loan from the University of Virginia, and the continued support of the SAO and the University of California, Berkeley. Magellan telescope time was granted by NOAO (Proposal ID 2010B-0184, P. I. Mainzer), through the Telescope System Instrumentation Program (TSIP). TSIP is funded by NSF. 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. Partial support for PAIRITEL operations and this work comes from National Aeronautics and Space Administration grant NNG06GH50G. A.J.B. acknowledges support from the Chris and Warren Hellman Fellowship Program. Finally, this research was supported (in part) by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. NR 93 TC 143 Z9 144 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2011 VL 743 IS 1 AR 50 DI 10.1088/0004-637X/743/1/50 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 853EF UT WOS:000297408300050 ER PT J AU Keisler, R Reichardt, CL Aird, KA Benson, BA Bleem, LE Carlstrom, JE Chang, CL Cho, HM Crawford, TM Crites, AT de Haan, T Dobbs, MA Dudley, J George, EM Halverson, NW Holder, GP Holzapfel, WL Hoover, S Hou, Z Hrubes, JD Joy, M Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D McMahon, JJ Mehl, J Meyer, SS Millea, M Mohr, JJ Montroy, TE Natoli, T Padin, S Plagge, T Pryke, C Ruhl, JE Schaffer, KK Shaw, L Shirokoff, E Spieler, HG Staniszewski, Z Stark, AA Story, K van Engelen, A Vanderlinde, K Vieira, JD Williamson, R Zahn, O AF Keisler, R. Reichardt, C. L. Aird, K. A. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Cho, H. M. Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. Dudley, J. George, E. M. Halverson, N. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hou, Z. Hrubes, J. D. Joy, M. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. McMahon, J. J. Mehl, J. Meyer, S. S. Millea, M. Mohr, J. J. Montroy, T. E. Natoli, T. Padin, S. Plagge, T. Pryke, C. Ruhl, J. E. Schaffer, K. K. Shaw, L. Shirokoff, E. Spieler, H. G. Staniszewski, Z. Stark, A. A. Story, K. van Engelen, A. Vanderlinde, K. Vieira, J. D. Williamson, R. Zahn, O. TI A MEASUREMENT OF THE DAMPING TAIL OF THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM WITH THE SOUTH POLE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmological parameters; cosmology: observations ID ATACAMA COSMOLOGY TELESCOPE; BIG-BANG NUCLEOSYNTHESIS; MASSIVE GALAXY CLUSTERS; PRIMORDIAL NUCLEOSYNTHESIS; OBSERVED GROWTH; CONSTRAINTS; ANISOTROPIES; POLARIZATION; TEMPERATURE; ABUNDANCE AB We present a measurement of the angular power spectrum of the cosmic microwave background (CMB) using data from the South Pole Telescope (SPT). The data consist of 790 deg(2) of sky observed at 150 GHz during 2008 and 2009. Here we present the power spectrum over the multipole range 650 < l < 3000, where it is dominated by primary CMB anisotropy. We combine this power spectrum with the power spectra from the seven-year Wilkinson Microwave Anisotropy Probe (WMAP) data release to constrain cosmological models. We find that the SPT and WMAP data are consistent with each other and, when combined, are well fit by a spatially flat, Lambda CDM cosmological model. The SPT+WMAP constraint on the spectral index of scalar fluctuations is n(s) = 0.9663 +/- 0.0112. We detect, at similar to 5 sigma significance, the effect of gravitational lensing on the CMB power spectrum, and find its amplitude to be consistent with the Lambda CDM cosmological model. We explore a number of extensions beyond the Lambda CDM model. Each extension is tested independently, although there are degeneracies between some of the extension parameters. We constrain the tensor-to-scalar ratio to be r < 0.21 (95% CL) and constrain the running of the scalar spectral index to be dn(s)/d ln k = -0.024 +/- 0.013. We strongly detect the effects of primordial helium and neutrinos on the CMB; a model without helium is rejected at 7.7 sigma, while a model without neutrinos is rejected at 7.5 sigma. The primordial helium abundance is measured to be Y-p = 0.296 +/- 0.030, and the effective number of relativistic species is measured to be N-eff = 3.85 +/- 0.62. The constraints on these models are strengthened when the CMB data are combined with measurements of the Hubble constant and the baryon acoustic oscillation feature. Notable improvements include n(s) = 0.9668 +/- 0.0093, r < 0.17 (95% CL), and N-eff = 3.86 +/- 0.42. The SPT+WMAP data show a mild preference for low power in the CMB damping tail, and while this preference may be accommodated by models that have a negative spectral running, a high primordial helium abundance, or a high effective number of relativistic species, such models are disfavored by the abundance of low-redshift galaxy clusters. C1 [Keisler, R.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Hoover, S.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Natoli, T.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Keisler, R.; Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Meyer, S. S.; Natoli, T.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Reichardt, C. L.; George, E. M.; Holzapfel, W. L.; Lee, A. T.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Aird, K. A.; Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Hrubes, J. D.; Leitch, E. M.; Luong-Van, D.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [de Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Hou, Z.; Knox, L.; Millea, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Joy, M.] NASA Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA. [Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 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. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA. [Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA. RP Keisler, R (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. EM rkeisler@uchicago.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937, ANT-0130612, AST-1009811, 0709498]; NSF Physics Frontier Center [PHY-0114422]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; NASA [51275.01]; KICP; Alfred P. Sloan; Yale University; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX The South Pole Telescope is supported by the National Science Foundation through grants ANT-0638937 and ANT-0130612. 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. 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. We acknowledge use of the FNAL-KICP Joint Cluster. R. Keisler acknowledges support from NASA Hubble Fellowship grant HF-51275.01. B. A. Benson is supported by a KICP Fellowship. M. Dobbs acknowledges support from an Alfred P. Sloan Research Fellowship. L. Shaw acknowledges the support of Yale University and NSF grant AST-1009811. M. Millea and L. Knox acknowledge the support of NSF grant 0709498. 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. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. NR 72 TC 354 Z9 354 U1 6 U2 22 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2011 VL 743 IS 1 AR 28 DI 10.1088/0004-637X/743/1/28 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 853EF UT WOS:000297408300028 ER PT J AU Rangwala, N Maloney, PR Glenn, J Wilson, CD Rykala, A Isaak, K Baes, M Bendo, GJ Boselli, A Bradford, CM Clements, DL Cooray, A Fulton, T Imhof, P Kamenetzky, J Madden, SC Mentuch, E Sacchi, N Sauvage, M Schirm, MRP Smith, MWL Spinoglio, L Wolfire, M AF Rangwala, Naseem Maloney, Philip R. Glenn, Jason Wilson, Christine D. Rykala, Adam Isaak, Kate Baes, Maarten Bendo, George J. Boselli, Alessandro Bradford, Charles M. Clements, D. L. Cooray, Asantha Fulton, Trevor Imhof, Peter Kamenetzky, Julia Madden, Suzanne C. Mentuch, Erin Sacchi, Nicola Sauvage, Marc Schirm, Maximilien R. P. Smith, M. W. L. Spinoglio, Luigi Wolfire, Mark TI OBSERVATIONS OF Arp 220 USING HERSCHEL-SPIRE: AN UNPRECEDENTED VIEW OF THE MOLECULAR GAS IN AN EXTREME STAR FORMATION ENVIRONMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: ISM; galaxies: starburst; ISM: molecules; line: identification; molecular processes; techniques: spectroscopic ID ULTRALUMINOUS INFRARED GALAXIES; INTER-STELLAR CLOUDS; INTERSTELLAR-MEDIUM; ATOMIC CARBON; C-II; FORMING REGIONS; HIGH-REDSHIFT; ENERGY-DISTRIBUTIONS; SUBMILLIMETER GALAXY; STARBURST GALAXIES AB We present Herschel Spectral and Photometric Imaging Receiver Fourier Transform Spectrometer (Herschel SPIRE-FTS) observations of Arp 220, a nearby ultra-luminous infrared galaxy. The FTS provides continuous spectral coverage from 190 to 670 mu m, a wavelength region that is either very difficult to observe or completely inaccessible from the ground. The spectrum provides a good measurement of the continuum and detection of several molecular and atomic species. We detect luminous CO (J = 4-3 to 13-12) and water rotational transitions with comparable total luminosity similar to 2 x 10(8) L-circle dot; very high-J transitions of HCN (J = 12-11 to 17-16) in absorption; strong absorption features of rare species such as OH+, H2O+, and HF; and atomic lines of [C I] and [N II]. The modeling of the continuum shows that the dust is warm, with T = 66 K, and has an unusually large optical depth, with tau(dust) similar to 5 at 100 mu m. The total far-infrared luminosity of Arp 220 is L-FIR similar to 2 x 10(12) L-circle dot. Non-LTE modeling of the extinction corrected CO rotational transitions shows that the spectral line energy distribution of CO is fit well by two temperature components: cold molecular gas at T similar to 50 K and warm molecular gas at T similar to 1350(-100)(+280) K (the inferred temperatures are much lower if CO line fluxes are not corrected for dust extinction). These two components are not in pressure equilibrium. The mass of the warm gas is 10% of the cold gas, but it dominates the CO luminosity. The ratio of total CO luminosity to the total FIR luminosity is L-CO/L-FIR similar to 10(-4) (the most luminous lines, such as J = 6-5, have L-CO,L-J=6-5/L-FIR similar to 10(-5)). The temperature of the warm gas is in excellent agreement with the observations of H-2 rotational lines. At 1350 K, H-2 dominates the cooling (similar to 20 L-circle dot M-circle dot(-1)) in the interstellar medium compared to CO (similar to 0.4 L-circle dot M-circle dot(-1)). We have ruled out photodissociation regions, X-ray-dominated regions, and cosmic rays as likely sources of excitation of this warm molecular gas, and found that only a non-ionizing source can heat this gas; the mechanical energy from supernovae and stellar winds is able to satisfy the large energy budget of similar to 20 L-circle dot M-circle dot(-1). Analysis of the very high-J lines of HCN strongly indicates that they are solely populated by infrared pumping of photons at 14 mu m. This mechanism requires an intense radiation field with T > 350 K. We detect a massive molecular outflow in Arp 220 from the analysis of strong P Cygni line profiles observed in OH+, H2O+, and H2O. The outflow has a mass greater than or similar to 10(7) M-circle dot and is bound to the nuclei with velocity less than or similar to 250 km s(-1). The large column densities observed for these molecular ions strongly favor the existence of an X-ray luminous AGN (10(44) erg s(-1)) in Arp 220. C1 [Rangwala, Naseem; Maloney, Philip R.; Glenn, Jason; Kamenetzky, Julia] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA. [Wilson, Christine D.; Mentuch, Erin; Schirm, Maximilien R. P.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Rykala, Adam; Smith, M. W. L.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Isaak, Kate] ESTEC, ESA Astrophys Mission Div, NL-2200 AG Noordwijk, Netherlands. [Baes, Maarten] Univ Ghent, Sterrenkundig Observatorium, B-9000 Ghent, Belgium. [Bendo, George J.] Univ Manchester, Sch Phys & Astron, Jordell Bank Ctr Astrophys, UK ALMA Reg Ctr Node, Manchester M13 9PL, Lancs, England. [Boselli, Alessandro] CNRS, UMR6110, Lab Astrophys Marseille, F-13388 Marseille, France. [Bradford, Charles M.] JPL, Pasadena, CA 91109 USA. [Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Fulton, Trevor; Imhof, Peter] Blue Sky Spect Inc, Lethbridge, AB T1J 0N9, Canada. [Madden, Suzanne C.; Sauvage, Marc] CEA, Lab AIM, Irfu SAp, F-91191 Gif Sur Yvette, France. [Sacchi, Nicola; Spinoglio, Luigi] INAF, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. [Wolfire, Mark] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Rangwala, N (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 1255 38th St, Boulder, CO 80303 USA. RI Baes, Maarten/I-6985-2013; OI Baes, Maarten/0000-0002-3930-2757; Spinoglio, Luigi/0000-0001-8840-1551 FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA) FX We thank our anonymous referee for constructive comments that have strengthened this paper. We are grateful to the FTS/ICC team for helping us with the FTS data reduction and understanding the instrumental effects. We thank Harshal Gupta from JPL for helping us with important line identifications. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM(France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). NR 105 TC 110 Z9 110 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 DEC 10 PY 2011 VL 743 IS 1 AR 94 DI 10.1088/0004-637X/743/1/94 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 853EF UT WOS:000297408300094 ER PT J AU Schaffer, KK Crawford, TM Aird, KA Benson, BA Bleem, LE Carlstrom, JE Chang, CL Cho, HM Crites, AT de Haan, T Dobbs, MA George, EM Halverson, NW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D McMahon, JJ Mehl, J Meyer, SS Mohr, JJ Montroy, TE Padin, S Plagge, T Pryke, C Reichardt, CL Ruhl, JE Shirokoff, E Spieler, HG Stalder, B Staniszewski, Z Stark, AA Story, K Vanderlinde, K Vieira, JD Williamson, R AF Schaffer, K. K. Crawford, T. M. Aird, K. A. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Cho, H. M. Crites, A. T. de Haan, T. Dobbs, M. A. George, E. M. Halverson, N. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. McMahon, J. J. Mehl, J. Meyer, S. S. Mohr, J. J. Montroy, T. E. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Ruhl, J. E. Shirokoff, E. Spieler, H. G. Stalder, B. Staniszewski, Z. Stark, A. A. Story, K. Vanderlinde, K. Vieira, J. D. Williamson, R. TI THE FIRST PUBLIC RELEASE OF SOUTH POLE TELESCOPE DATA: MAPS OF A 95 deg(2) FIELD FROM 2008 OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; methods: data analysis; surveys ID MICROWAVE BACKGROUND ANISOTROPIES; ZELDOVICH POWER SPECTRUM; GALAXY CLUSTERS; SOURCE CATALOG; SUBMILLIMETER; RADIO; SIMULATIONS; PARAMETERS; COSMOLOGY; SKY AB The South Pole Telescope (SPT) has nearly completed a 2500 deg(2) survey of the southern sky in three frequency bands. Here, we present the first public release of SPT maps and associated data products. We present arcminute-resolution maps at 150 GHz and 220 GHz of an approximately 95 deg(2) field centered at R. A. 82 degrees.7, decl. -55 degrees. The field was observed to a depth of approximately 17 mu K arcmin at 150 GHz and 41 mu K arcmin at 220 GHz during the 2008 austral winter season. Two variations on map filtering and map projection are presented, one tailored for producing catalogs of galaxy clusters detected through their Sunyaev-Zel'dovich effect signature and one tailored for producing catalogs of emissive sources. We describe the data processing pipeline, and we present instrument response functions, filter transfer functions, and map noise properties. All data products described in this paper are available for download at http://pole.uchicago.edu/public/data/maps/ra5h30dec-55 and from the NASA Legacy Archive for Microwave Background Data Analysis server. This is the first step in the eventual release of data from the full 2500 deg(2) SPT survey. C1 [Schaffer, K. K.; Crawford, T. M.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crites, A. T.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Schaffer, K. K.; Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Pryke, C.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Crawford, T. M.; Carlstrom, J. E.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Meyer, S. S.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [de Haan, T.; Dobbs, M. A.; Holder, G. P.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 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, Dept Space Sci, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA. [Lueker, M.; Padin, S.; Staniszewski, Z.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Univ, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schaffer, KK (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM kschaf2@saic.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937, ANT-0130612, AST-1009012, AST-1009649, MRI-0723073]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; KICP; Alfred P. Sloan Research Fellowships; NASA [HF-51275.01]; DFG [TR33]; NASA Office of Space Science FX The South Pole Telescope is supported by the National Science Foundation through grants ANT-0638937 and ANT-0130612. 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. 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. Partial support at Harvard is provided by NSF grants AST-1009012, AST-1009649, and MRI-0723073. B. A. B. is supported by a KICP Fellowship. M. D. and N.H. acknowledge support from Alfred P. Sloan Research Fellowships. R. K. acknowledges support from NASA Hubble Fellowship grant HF-51275.01. J.J.M. acknowledges support from the DFG supported Excellence Cluster Universe and the transregio program TR33: Dark Universe. B. S. acknowledges partial support from the Brinson Foundation. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. NR 42 TC 38 Z9 39 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2011 VL 743 IS 1 AR 90 DI 10.1088/0004-637X/743/1/90 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 853EF UT WOS:000297408300090 ER PT J AU Scowcroft, V Freedman, WL Madore, BF Monson, AJ Persson, SE Seibert, M Rigby, JR Sturch, L AF Scowcroft, Victoria Freedman, Wendy L. Madore, Barry F. Monson, Andrew J. Persson, S. E. Seibert, Mark Rigby, Jane R. Sturch, Laura TI THE CARNEGIE HUBBLE PROGRAM: THE LEAVITT LAW AT 3.6 mu m AND 4.5 mu m IN THE LARGE MAGELLANIC CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; Magellanic Clouds; stars: distances; stars: variables: Cepheids ID GRAVITATIONAL LENSING EXPERIMENT.; PERIOD-LUMINOSITY RELATIONS; SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; CLASSICAL CEPHEIDS; GALACTIC CEPHEIDS; LMC DATA; CONSTANT; OGLE; DISTANCE AB The Carnegie Hubble Program is designed to improve the extragalactic distance scale using data from the post-cryogenic era of Spitzer. The ultimate goal is a determination of the Hubble constant to an accuracy of 2%. This paper is the first in a series on the Cepheid population of the Large Magellanic Cloud, and focusses on the period-luminosity (PL) relations (Leavitt laws) that will be used, in conjunction with observations of Milky Way Cepheids, to set the slope and zero point of the Cepheid distance scale in the mid-infrared. To this end, we have obtained uniformly sampled light curves for 85 LMC Cepheids, having periods between 6 and 140 days. PL and period-color relations are presented in the 3.6 mu m and 4.5 mu m bands. We demonstrate that the 3.6 mu m band is a superb distance indicator. The cyclical variation of the [3.6]-[4.5] color has been measured for the first time. We attribute the amplitude and phase of the color curves to the dissociation and recombination of CO molecules in the Cepheid's atmosphere. The CO affects only the 4.5 mu m flux making it a potential metallicity indicator. C1 [Scowcroft, Victoria; Freedman, Wendy L.; Madore, Barry F.; Monson, Andrew J.; Persson, S. E.; Seibert, Mark] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sturch, Laura] Boston Univ, Dept Astron, Boston, MA 02215 USA. RP Scowcroft, V (reprint author), Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA. EM vs@obs.carnegiescience.edu; wendy@obs.carnegiescience.edu; barry@obs.carnegiescience.edu; amonson@obs.carnegiescience.edu; persson@obs.carnegiescience.edu; mseibert@obs.carnegiescience.edu; jane.r.rigby@nasa.gov; lsturch@bu.edu RI Rigby, Jane/D-4588-2012 OI Rigby, Jane/0000-0002-7627-6551 FU NASA FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. 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. We thank the staff of the Spitzer Science Center, and in particular Nancy Silbermann, for their assistance with scheduling such a large and complex project. Without their help, this project would not have been possible. NR 31 TC 25 Z9 25 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2011 VL 743 IS 1 AR 76 DI 10.1088/0004-637X/743/1/76 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 853EF UT WOS:000297408300076 ER PT J AU Sterling, AC Moore, RL Harra, LK AF Sterling, Alphonse C. Moore, Ronald L. Harra, Louise K. TI LATERAL OFFSET OF THE CORONAL MASS EJECTIONS FROM THE X-FLARE OF 2006 DECEMBER 13 AND ITS TWO PRECURSOR ERUPTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: coronal mass ejections (CMEs); Sun: flares; Sun: heliosphere; Sun: UV radiation; Sun: X-rays, gamma rays ID SOLAR-FLARES; ENERGY-RELEASE; MAGNETIC EXPLOSION; ACTIVE-REGION; HINODE; ACCELERATION; FLUX; FILAMENT; SCENARIO; FIELDS AB Two GOES sub-C-class precursor eruptions occurred within similar to 10 hr prior to and from the same active region as the 2006 December 13 X4.3-class flare. Each eruption generated a coronal mass ejection (CME) with center laterally far offset (greater than or similar to 45 degrees) from the co-produced bright flare. Explaining such CME-to-flare lateral offsets in terms of the standard model for solar eruptions has been controversial. Using Hinode/X-Ray Telescope (XRT) and EUV Imaging Spectrometer (EIS) data, and Solar and Heliospheric Observatory (SOHO)/Large Angle and Spectrometric Coronagraph (LASCO) and Michelson Doppler Imager (MDI) data, we find or infer the following. (1) The first precursor was a "magnetic-arch-blowout" event, where an initial standard-model eruption of the active region's core field blew out a lobe on one side of the active region's field. (2) The second precursor began similarly, but the core-field eruption stalled in the side-lobe field, with the side-lobe field erupting similar to 1 hr later to make the CME either by finally being blown out or by destabilizing and undergoing a standard-model eruption. (3) The third eruption, the X-flare event, blew out side lobes on both sides of the active region and clearly displayed characteristics of the standard model. (4) The two precursors were offset due in part to the CME originating from a side-lobe coronal arcade that was offset from the active region's core. The main eruption (and to some extent probably the precursor eruptions) was offset primarily because it pushed against the field of the large sunspot as it escaped outward. (5) All three CMEs were plausibly produced by a suitable version of the standard model. C1 [Sterling, Alphonse C.; Moore, Ronald L.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Harra, Louise K.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Sterling, AC (reprint author), JAXA Inst Space & Astronaut Sci, Hinode Grp, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. EM alphonse.sterling@nasa.gov; ron.moore@nasa.gov; lkh@mssl.ucl.ac.uk OI Harra, Louise/0000-0001-9457-6200 FU NASA's Office of Space Science; JAXA (Japan); NAOJ (Japan); STFC (UK); NASA (USA); ESA (Norway); NSC (Norway) FX We thank an anonymous referee for insightful comments. A. C. S. and R. L. M. were supported by funding from NASA's Office of Space Science through the Solar Physics Supporting Research and Technology Program, the Heliophysics Guest Investigator Program, and the Living With a Star Targeted Research & Technology Program. Hinode is a Japanese mission developed and launched by ISAS/JAXA, collaborating with NAOJ as a domestic partner, NASA and STFC (UK) as international partners. Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/JAXA. This team mainly consists of scientists from institutes in the partner countries. Support for the post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK), NASA (USA), ESA, and NSC (Norway). NR 48 TC 7 Z9 7 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2011 VL 743 IS 1 AR 63 DI 10.1088/0004-637X/743/1/63 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 853EF UT WOS:000297408300063 ER PT J AU Weisskopf, MC Romani, RW Razzano, M Belfiore, A Parkinson, PS Ray, PS Kerr, M Harding, A Swartz, DA Carraminana, A Ziegler, M Becker, W De Luca, A Dormody, M Thompson, DJ Kanbach, G Elsner, RF O'Dell, SL Tennant, AF AF Weisskopf, Martin C. Romani, Roger W. Razzano, Massimiliano Belfiore, Andrea Parkinson, Pablo Saz Ray, Paul S. Kerr, Matthew Harding, Alice Swartz, Douglas A. Carraminana, Alberto Ziegler, Marcus Becker, Werner De Luca, Andrea Dormody, Michael Thompson, David J. Kanbach, Gottfried Elsner, Ronald F. O'Dell, Stephen L. Tennant, Allyn F. TI THE IDENTIFICATION OF THE X-RAY COUNTERPART TO PSR J2021+4026 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (PSR J2021+4026); supernovae: individual (SNR 78.2+2.1); X-rays: general ID LARGE-AREA TELESCOPE; UNIDENTIFIED EGRET SOURCES; BLIND FREQUENCY SEARCHES; PULSAR WIND NEBULA; SLOT GAPS; SUPERNOVA REMNANT; POLAR CAPS; OUTER MAGNETOSPHERE; GEMINGA PULSAR; NEUTRON-STARS AB We report the probable identification of the X-ray counterpart to the gamma-ray pulsar PSR J2021+4026 using imaging with the Chandra X-ray Observatory Advanced CCD Imaging Spectrometer and timing analysis with the Fermi satellite. Given the statistical and systematic errors, the positions determined by both satellites are coincident. The X-ray source position is R. A. 20(h)21(m)30(s).733, decl. +40 degrees 26'46 ''.04 (J2000) with an estimated uncertainty of 1 ''.3 combined statistical and systematic error. Moreover, both the X-ray to gamma-ray and the X-ray to optical flux ratios are sensible assuming a neutron star origin for the X-ray flux. The X-ray source has no cataloged infrared-to-visible counterpart and, through new observations, we set upper limits to its optical emission of i' > 23.0 mag and r' > 25.2 mag. The source exhibits an X-ray spectrum with most likely both a power law and a thermal component. We also report on the X-ray and visible light properties of the 43 other sources detected in our Chandra observation. C1 [Weisskopf, Martin C.; Elsner, Ronald F.; O'Dell, Stephen L.; Tennant, Allyn F.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Romani, Roger W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Razzano, Massimiliano] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Razzano, Massimiliano; Belfiore, Andrea; Parkinson, Pablo Saz; Ziegler, Marcus; Dormody, Michael] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Razzano, Massimiliano] Univ Pisa, Dipartimento Fis, I-56127 Pisa, Italy. [Belfiore, Andrea; De Luca, Andrea] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy. [Belfiore, Andrea] Univ Pavia, Dipartimento Fis Teor & Nucl DFNT, I-27100 Pavia, Italy. [Kerr, Matthew] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Ray, Paul S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Harding, Alice] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Swartz, Douglas A.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. [Carraminana, Alberto] Inst Nacl Astrofis Opt & Electr, Puebla 72840, Mexico. [Becker, Werner; Kanbach, Gottfried] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [De Luca, Andrea] IUSS, I-27100 Pavia, Italy. [De Luca, Andrea] Ist Nazl Fis Nucl, I-27100 Pavia, Italy. [Thompson, David J.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. RP Weisskopf, MC (reprint author), NASA, George C Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA. RI Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; Saz Parkinson, Pablo Miguel/I-7980-2013; OI Thompson, David/0000-0001-5217-9135; O'Dell, Stephen/0000-0002-1868-8056; De Luca, Andrea/0000-0001-6739-687X; Ray, Paul/0000-0002-5297-5278 FU National Aeronautics Space Administration [NAS8-03060, NNX08AW30G]; Chandra X-ray Observatory Center [GO0-11086A]; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX The work of M. C. W., D. A. S., R. F. E., S. L. O., and A. F. T. is supported by the Chandra Program. The Chandra data were obtained in response to proposal number 11500575 by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. Support for this work was also provided to P. S. P. in response to this proposal through Chandra Award Number GO0-11086A issued by the Chandra X-ray Observatory Center. The work of R. W. R. was supported in part by NASA grant NNX08AW30G. The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. Our analyses utilized software tools provided by the CXC in the application package CIAO and from the High-Energy Astrophysics Science Archive Research Center (HEASARC, operated by the NASA Goddard Space Flight Center, Greenbelt, MD, and by the Smithsonian Astrophysical Observatory, Cambridge, MA). We also thank Mike Wolff for a careful critique of the manuscript. NR 59 TC 8 Z9 8 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2011 VL 743 IS 1 AR 74 DI 10.1088/0004-637X/743/1/74 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 853EF UT WOS:000297408300074 ER PT J AU ZuHone, JA Markevitch, M Lee, D AF ZuHone, J. A. Markevitch, M. Lee, D. TI SLOSHING OF THE MAGNETIZED COOL GAS IN THE CORES OF GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: intracluster medium; methods: numerical; X-rays: galaxies: clusters ID ANISOTROPIC THERMAL CONDUCTION; DIFFUSE RADIO-EMISSION; FARADAY-ROTATION MAPS; FIELD POWER SPECTRUM; X-RAY-PROPERTIES; COLD FRONTS; COMA CLUSTER; MAGNETOHYDRODYNAMIC SIMULATIONS; PARTICLE REACCELERATION; INTRACLUSTER MEDIUM AB X-ray observations of many clusters of galaxies reveal the presence of edges in surface brightness and temperature, known as "cold fronts." In relaxed clusters with cool cores, these edges have been interpreted as evidence for the "sloshing" of the core gas in the cluster's gravitational potential. The smoothness of these edges has been interpreted as evidence for the stabilizing effect of magnetic fields "draped" around the front surfaces. To check this hypothesis, we perform high-resolution magnetohydrodynamics simulations of magnetized gas sloshing in galaxy clusters initiated by encounters with subclusters. We go beyond previous works on the simulation of cold fronts in a magnetized intracluster medium by simulating their formation in realistic, idealized mergers with high resolution (Delta x similar to 2 kpc). Our simulations sample a parameter space of plausible initial magnetic field strengths and field configurations. In the simulations, we observe strong velocity shears associated with the cold fronts amplifying the magnetic field along the cold front surfaces, increasing the magnetic field strength in these layers by up to an order of magnitude, and boosting the magnetic pressure up to near-equipartition with thermal pressure in some cases. In these layers, the magnetic field becomes strong enough to stabilize the cold fronts against Kelvin-Helmholtz instabilities, resulting in sharp, smooth fronts as those seen in observations of real clusters. These magnetic fields also result in strong suppression of mixing of high-and low-entropy gases in the cluster, seen in our simulations of mergers in the absence of a magnetic field. As a result, the heating of the core due to sloshing is very modest and is unable to stave off a cooling catastrophe. C1 [ZuHone, J. A.; Markevitch, M.] NASA, Astrophys Sci Div, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [ZuHone, J. A.; Markevitch, M.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Lee, D.] Univ Chicago, Dept Astron, ASC Flash Ctr, Chicago, IL 60637 USA. RP ZuHone, JA (reprint author), NASA, Astrophys Sci Div, High Energy Astrophys Lab, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. FU NASA; ASC/Alliances Center for Astrophysical Thermonuclear Flashes at the University of Chicago FX We thank the anonymous referee for helpful and constructive comments and suggestions. J.A.Z. thanks Ian Parrish, Bill Forman, Eric Hallman, and Mateusz Ruszkowski for useful discussions and advice. Calculations were performed using the computational resources of the Smithsonian Insitution's Hendron Data Center, Argonne National Laboratory, and the National Institute for Computational Sciences at the University of Tennessee. Analysis of the simulation data was carried out using the AMR analysis and visualization toolset yt (Turk et al. 2011), which is available for download at http://yt.enzotools.org, and for which Matthew Turk provided considerable help toward getting it working for the analysis for this paper. J.A.Z. is supported by the NASA Postdoctoral Program. The software used in this work was in part developed by the DOE-supported ASC/Alliances Center for Astrophysical Thermonuclear Flashes at the University of Chicago. NR 88 TC 50 Z9 50 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2011 VL 743 IS 1 AR 16 DI 10.1088/0004-637X/743/1/16 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 853EF UT WOS:000297408300016 ER PT J AU Campbell, MD Rose, K Boswell, K Cowan, J AF Campbell, Matthew D. Rose, Kenneth Boswell, Kevin Cowan, James TI Individual-based modeling of an artificial reef fish community: Effects of habitat quantity and degree of refuge SO ECOLOGICAL MODELLING LA English DT Article DE IBM; Movement; Bioenergetics; Red snapper; Artificial reefs; Competition; Predation prey halos ID GULF-OF-MEXICO; PINFISH LAGODON-RHOMBOIDES; RED SNAPPER; NORTHERN GULF; LUTJANUS-CAMPECHANUS; PREDATION RISK; UNITED-STATES; NATURAL REEF; GROWTH; ASSEMBLAGES AB Artificial reefs are often deployed as fishery management tools, and yet there is substantial lack of understanding and agreement on how reefs affect fish population and community dynamics. We developed and applied a multi-species, individual-based model to examine the long-term effects of increasing number of reefs on fish weight, abundance, and biomass. The model simulated the population dynamics of three fish species for 50 years on a 2-dimensional spatial grid. Growth, mortality, and movement were computed each hour for individuals of red snapper (Lutjanus campechanus), a croaker-like species (Micropogonias chromis), and a pinfish-like species (Lagodon rhomboides). We also included individuals of two other species (bluefish - Pomatomus saltatrix and a generic jack-like species), but only simulated their hourly movement and their effects on prey and predation of the focal species. The densities of five prey groups were simulated independently in each cell. Our results showed that increasing the number of reefs generally produced higher biomass, but at the cost of slower growth, and smaller individuals. Abundance was higher under fixed-AR recruitment and maximum refuge treatments. In all treatments there were diminishing returns on abundance and biomass with increasing number of artificial reefs. Experiment 2 showed that model results based on regularly spaced reefs were consistent with a real layout of reefs currently being sampled in the northern Gulf of Mexico. Management strategies for determining the habitat-value of reefs in the Gulf of Mexico should consider the number of reefs and the local spatial layout of the reefs to ensure they are optimally arranged. Field experiments performed should assist in resolving how fish recruit to artificial reefs and help determine their roles as fish refuges. Published by Elsevier B.V. C1 [Campbell, Matthew D.; Rose, Kenneth; Boswell, Kevin; Cowan, James] Louisiana State Univ, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70808 USA. RP Campbell, MD (reprint author), Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS USA. EM matthew.d.campbell@noaa.gov RI boswell, kevin/B-6380-2016; OI boswell, kevin/0000-0002-2037-1541; Campbell, Matthew/0000-0002-0087-5291 NR 51 TC 17 Z9 18 U1 1 U2 39 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3800 J9 ECOL MODEL JI Ecol. Model. PD DEC 10 PY 2011 VL 222 IS 23-24 BP 3895 EP 3909 DI 10.1016/j.ecolmodel.2011.10.009 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 867LE UT WOS:000298455100009 ER PT J AU Zhai, Y Cummer, SA Green, JL Reinisch, BW Kaiser, ML Reiner, MJ Goetz, K AF Zhai, Y. Cummer, S. A. Green, J. L. Reinisch, B. W. Kaiser, M. L. Reiner, M. J. Goetz, K. TI Magnetospheric radio tomographic imaging with IMAGE and Wind SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID IONOSPHERIC TOMOGRAPHY; ELECTRON-DENSITY; MAGNETIC-FIELD; PLASMA IMAGER; SPACECRAFT AB Recent theoretical studies have shown the feasibility and potential scientific value of radio tomographic imaging of Earth's magnetosphere by measuring Faraday rotation and phase difference (or group delay) of coherent radio wave signals. On 15 August 2000, a 6 W linearly polarized 828 kHz signal transmitted by the Radio Plasma Imager (RPI) on the IMAGE spacecraft was clearly detected by WAVES X and Z antennas on Wind spacecraft. Following our previous analysis of the path-integrated product change of the magnetic field and plasma density based on the spin rate measurement, we report here Faraday rotation measured from absolute antenna orientation using the phase difference between the spin-phase modeled RPI signal and the WAVES X-and Z-antenna received RPI signals. The new approach gives Faraday rotation without the mod (pi) ambiguity. The average electron density extracted along a typical signal propagation path over a 1 hour measurement window agrees well with empirical models of the northern polar region derived from years of measurements. Finally, we demonstrate preliminary 2-D radio tomographic imaging of magnetospheric plasma density using the Faraday rotation measurement. C1 [Zhai, Y.] Princeton Univ, Princeton Plasma Phys Lab, Princeton, NJ 08543 USA. [Reinisch, B. W.] Univ Massachusetts, Ctr Atmospher Res, Lowell, MA 01854 USA. [Kaiser, M. L.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Cummer, S. A.] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA. [Goetz, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Green, J. L.] NASA Headquarters, Planetary Sci Div, Washington, DC 20546 USA. [Reiner, M. J.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. RP Zhai, Y (reprint author), Princeton Univ, Princeton Plasma Phys Lab, POB 451, Princeton, NJ 08543 USA. EM yzhai@pppl.gov; cummer@ee.duke.edu RI Cummer, Steven/A-6118-2008 OI Cummer, Steven/0000-0002-0002-0613 FU NASA Geospace Sciences [NNX07AGU14G] FX This research was supported by NASA Geospace Sciences grant NNX07AGU14G. NR 23 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 10 PY 2011 VL 116 AR A12208 DI 10.1029/2011JA016743 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 860WQ UT WOS:000297979400002 ER PT J AU Barth, AJ Pancoast, A Thorman, SJ Bennert, VN Sand, DJ Li, WD Canalizo, G Filippenko, AV Gates, EL Greene, JE Malkan, MA Stern, D Treu, T Woo, JH Assef, RJ Bae, HJ Brewer, BJ Buehler, T Cenko, SB Clubb, KI Cooper, MC Diamond-Stanic, AM Hiner, KD Honig, SF Joner, MD Kandrashoff, MT Laney, CD Lazarova, MS Nierenberg, AM Park, D Silverman, JM Son, D Sonnenfeld, A Tollerud, EJ Walsh, JL Walters, R da Silva, RL Fumagalli, M Gregg, MD Harris, CE Hsiao, EY Lee, J Lopez, L Rex, J Suzuki, N Trump, JR Tytler, D Worseck, G Yesuf, HM AF Barth, Aaron J. Pancoast, Anna Thorman, Shawn J. Bennert, Vardha N. Sand, David J. Li, Weidong Canalizo, Gabriela Filippenko, Alexei V. Gates, Elinor L. Greene, Jenny E. Malkan, Matthew A. Stern, Daniel Treu, Tommaso Woo, Jong-Hak Assef, Roberto J. Bae, Hyun-Jin Brewer, Brendon J. Buehler, Tabitha Cenko, S. Bradley Clubb, Kelsey I. Cooper, Michael C. Diamond-Stanic, Aleksandar M. Hiner, Kyle D. Hoenig, Sebastian F. Joner, Michael D. Kandrashoff, Michael T. Laney, C. David Lazarova, Mariana S. Nierenberg, A. M. Park, Dawoo Silverman, Jeffrey M. Son, Donghoon Sonnenfeld, Alessandro Tollerud, Erik J. Walsh, Jonelle L. Walters, Richard da Silva, Robert L. Fumagalli, Michele Gregg, Michael D. Harris, Chelsea E. Hsiao, Eric Y. Lee, Jeffrey Lopez, Liliana Rex, Jacob Suzuki, Nao Trump, Jonathan R. Tytler, David Worseck, Gabor Yesuf, Hassen M. TI THE LICK AGN MONITORING PROJECT 2011: REVERBERATION MAPPING OF MARKARIAN 50 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual (Mrk 50); galaxies: nuclei ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; BROAD-LINE REGION; M-BH-SIGMA(ASTERISK) RELATION; VELOCITY DISPERSION; CONTINUUM EMISSION; SEYFERT-1 GALAXIES; RADIATION PRESSURE; ARP 151; VARIABILITY AB The Lick AGN Monitoring Project 2011 observing campaign was carried out over the course of 11 weeks in spring 2011. Here we present the first results from this program, a measurement of the broad-line reverberation lag in the Seyfert 1 galaxy Mrk 50. Combining our data with supplemental observations obtained prior to the start of the main observing campaign, our data set covers a total duration of 4.5 months. During this time, Mrk 50 was highly variable, exhibiting a maximum variability amplitude of a factor of similar to 4 in the U-band continuum and a factor of similar to 2 in the H beta line. Using standard cross-correlation techniques, we find that H beta and H gamma lag the V-band continuum by tau(cen) = 10.64(-0.93)(+0.82) and 8.43(-1.28)(+1.30) days, respectively, while the lag of He II lambda 4686 is unresolved. The H beta line exhibits a symmetric velocity-resolved reverberation signature with shorter lags in the high-velocity wings than in the line core, consistent with an origin in a broad-line region (BLR) dominated by orbital motion rather than infall or outflow. Assuming a virial normalization factor of f = 5.25, the virial estimate of the black hole mass is (3.2 +/- 0.5) x 10(7) M-circle dot. These observations demonstrate that Mrk 50 is among the most promising nearby active galaxies for detailed investigations of BLR structure and dynamics. C1 [Barth, Aaron J.; Thorman, Shawn J.; Cooper, Michael C.; Tollerud, Erik J.; Walsh, Jonelle L.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Pancoast, Anna; Bennert, Vardha N.; Sand, David J.; Treu, Tommaso; Brewer, Brendon J.; Hoenig, Sebastian F.; Nierenberg, A. M.; Sonnenfeld, Alessandro; Harris, Chelsea E.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bennert, Vardha N.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93407 USA. [Sand, David J.] Global Telescope Network, Las Cumbres Observ, Santa Barbara, CA 93117 USA. [Li, Weidong; Filippenko, Alexei V.; Cenko, S. Bradley; Clubb, Kelsey I.; Kandrashoff, Michael T.; Silverman, Jeffrey M.; Rex, Jacob] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Canalizo, Gabriela; Hiner, Kyle D.; Lazarova, Mariana S.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Gates, Elinor L.] Lick Observ, Mt Hamilton, CA 95140 USA. [Greene, Jenny E.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Malkan, Matthew A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Stern, Daniel; Assef, Roberto J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Woo, Jong-Hak; Park, Dawoo; Son, Donghoon] Seoul Natl Univ, Astron Program, Dept Phys & Astron, Seoul 151742, South Korea. [Bae, Hyun-Jin] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Bae, Hyun-Jin] Yonsei Univ, Ctr Galaxy Evolut Res, Seoul 120749, South Korea. [Buehler, Tabitha; Joner, Michael D.; Laney, C. David] Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA. [Diamond-Stanic, Aleksandar M.; Lee, Jeffrey; Lopez, Liliana; Tytler, David] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA. [Silverman, Jeffrey M.; Hsiao, Eric Y.; Suzuki, Nao] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA. [Walsh, Jonelle L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Walters, Richard] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. [da Silva, Robert L.; Fumagalli, Michele; Trump, Jonathan R.; Worseck, Gabor; Yesuf, Hassen M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Gregg, Michael D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Gregg, Michael D.] Lawrence Livermore Natl Lab, IGPP, Livermore, CA 94550 USA. RP Barth, AJ (reprint author), Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA. EM barth@uci.edu RI Woo, Jong-Hak/A-2790-2014; Bae, Hyun-Jin/J-8037-2015; Fumagalli, Michele/K-9510-2015; OI Bae, Hyun-Jin/0000-0001-5134-5517; Fumagalli, Michele/0000-0001-6676-3842; Tollerud, Erik/0000-0002-9599-310X; Hoenig, Sebastian/0000-0002-6353-1111; Worseck, Gabor/0000-0003-0960-3580; Barth, Aaron/0000-0002-3026-0562 FU NSF [AST-1107812, 1107865, 1108665, 1108835, AST-0618209]; Packard Research Fellowship FX We are extremely grateful to the Lick Observatory staff for their outstanding support during our observing run. The Lick AGN Monitoring Project 2011 is supported by NSF grants AST-1107812, 1107865, 1108665, and 1108835. T.T. acknowledges a Packard Research Fellowship. The West Mountain Observatory receives support from NSF grant AST-0618209. We thank Brad Peterson for a helpful referee report. NR 44 TC 35 Z9 35 U1 1 U2 17 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 10 PY 2011 VL 743 IS 1 AR L4 DI 10.1088/2041-8205/743/1/L4 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 852QN UT WOS:000297372600004 ER PT J AU Gull, TR Madura, TI Groh, JH Corcoran, MF AF Gull, Theodore R. Madura, Thomas I. Groh, Jose H. Corcoran, Michael F. TI IMAGING THE TIME EVOLUTION OF ETA CARINAE'S COLLIDING WINDS WITH HST SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: atmospheres; stars: individual (Eta Carinae); stars: mass-loss; stars: variables: general; stars: winds, outflows; supergiants ID HOMUNCULUS-NEBULA; EMISSION-LINES; BINARY; COMPANION; VARIABILITY; PARAMETERS; COLLISION; SPECTRUM; MINIMUM; EVENTS AB We report new Hubble Space Telescope/Space Telescope Imaging Spectrograph observations that map the high-ionization forbidden line emission in the inner arcsecond of EtaCar, the first that fully image the extended wind-wind interaction region of the massive colliding wind binary. These observations were obtained after the 2009.0 periastron at orbital phases 0.084, 0.163, and 0.323 of the 5.54 year spectroscopic cycle. We analyze the variations in brightness and morphology of the emission, and find that blueshifted emission (-400 to -200 km s(-1)) is symmetric and elongated along the northeast-southwest axis, while the redshifted emission (+100 to +200 km s(-1)) is asymmetric and extends to the north-northwest. Comparison with synthetic images generated from a three-dimensional (3D) dynamical model strengthens the 3D orbital orientation found by Madura et al., with an inclination of i approximate to 138 degrees, an argument of periapsis of omega approximate to 270 degrees, and an orbital axis that is aligned at the same position angle on the sky as the symmetry axis of the Homunculus, 312 degrees. We discuss the potential that these and future mappings have for constraining the stellar parameters of the companion star and the long-term variability of the system. C1 [Gull, Theodore R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Madura, Thomas I.; Groh, Jose H.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Corcoran, Michael F.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Corcoran, Michael F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corcoran, Michael F.] Univ Space Res Assoc, Columbia, MD 21044 USA. RP Gull, TR (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 667, Greenbelt, MD 20771 USA. EM Theodore.R.Gull@nasa.gov RI Gull, Theodore/D-2753-2012 OI Gull, Theodore/0000-0002-6851-5380 FU NASA through Space Telescope Science Institute; NASA [NAS 5-26555] FX Support for program 12013 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 33 TC 16 Z9 16 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 10 PY 2011 VL 743 IS 1 AR L3 DI 10.1088/2041-8205/743/1/L3 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 852QN UT WOS:000297372600003 ER PT J AU Mushotzky, RF Edelson, R Baumgartner, W Gandhi, P AF Mushotzky, R. F. Edelson, R. Baumgartner, W. Gandhi, P. TI KEPLER OBSERVATIONS OF RAPID OPTICAL VARIABILITY IN ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: active; galaxies: Seyfert ID BLACK-HOLES; QUASAR VARIABILITY; TIME VARIABILITY; LIGHT CURVES; FLUCTUATIONS; ACCRETION; GALAXIES; SPECTRUM; CATALOG; SAMPLE AB Over three quarters in 2010-2011, Kepler monitored optical emission from four active galactic nuclei (AGNs) with similar to 30 minute sampling, >90% duty cycle, and less than or similar to 0.1% repeatability. These data determined the AGN optical fluctuation power spectral density (PSD) functions over a wide range in temporal frequency. Fits to these PSDs yielded power-law slopes of -2.6 to -3.3, much steeper than typically seen in the X-rays. We find evidence that individual AGNs exhibit intrinsically different PSD slopes. The steep PSD fits are a challenge to recent AGN variability models but seem consistent with first-order magnetorotational instability theoretical calculations of accretion disk fluctuations. C1 [Mushotzky, R. F.; Edelson, R.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mushotzky, R. F.; Baumgartner, W.] NASA, High Energy Astrophys Lab, GSFC, Greenbelt, MD 20771 USA. [Gandhi, P.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. RP Mushotzky, RF (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM richard@astro.umd.edu FU Kepler GO program FX We thank the Kepler team for their efforts to make the data accessible and tractable and the Kepler GO program for funding, Matt Malkan for extensive contributions to the identification of new Kepler AGNs, Simon Vaughan for valuable help with PSD measurements, and Aaron Barth and the LAMP team for early access to their data. NR 33 TC 70 Z9 70 U1 0 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 10 PY 2011 VL 743 IS 1 AR L12 DI 10.1088/2041-8205/743/1/L12 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 852QN UT WOS:000297372600012 ER PT J AU Rodriguez-Nieva, JF Bringa, EM Cassidy, TA Johnson, RE Caro, A Fama, M Loeffler, MJ Baragiola, RA Farkas, D AF Rodriguez-Nieva, J. F. Bringa, E. M. Cassidy, T. A. Johnson, R. E. Caro, A. Fama, M. Loeffler, M. J. Baragiola, R. A. Farkas, D. TI SPUTTERING FROM A POROUS MATERIAL BY PENETRATING IONS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE atomic processes; methods: numerical; molecular processes; planets and satellites: surfaces; radiation mechanisms: general ID MOLECULAR-DYNAMICS; DUST GRAINS; COSMIC-RAYS; REGOLITH; MODEL; I. AB Porous materials are ubiquitous in the universe and weathering of porous surfaces plays an important role in the evolution of planetary and interstellar materials. Sputtering of porous solids in particular can influence atmosphere formation, surface reflectivity, and the production of the ambient gas around materials in space. Several previous studies and models have shown a large reduction in the sputtering of a porous solid compared to the sputtering of the non-porous solid. Using molecular dynamics simulations we study the sputtering of a nanoporous solid with 55% of the solid density. We calculate the electronic sputtering induced by a fast, penetrating ion, using a thermal spike representation of the deposited energy. We find that sputtering for this porous solid is, surprisingly, the same as that for a full-density solid, even though the sticking coefficient is high. C1 [Rodriguez-Nieva, J. F.] Univ Nacl Cuyo, Inst Balseiro, RA-8400 San Carlos De Bariloche, Rio Negro, Argentina. [Bringa, E. M.] Univ Nacl Cuyo, CONICET, RA-5500 Mendoza, Argentina. [Bringa, E. M.] Univ Nacl Cuyo, Inst Ciencias Basicas, RA-5500 Mendoza, Argentina. [Cassidy, T. A.] CalTech JPL, Pasadena, CA 91109 USA. [Johnson, R. E.; Fama, M.; Baragiola, R. A.] Univ Virginia, Lab Atom & Surface Phys, Charlottesville, VA 22903 USA. [Caro, A.] Los Alamos Natl Lab, Los Alamos, NM USA. [Loeffler, M. J.] NASA, Goddard Space Flight Ctr, Astrochem Branch, Greenbelt, MD 20771 USA. [Farkas, D.] Virginia Tech, Dept Mat Sci, Blacksburg, VA 24061 USA. RP Rodriguez-Nieva, JF (reprint author), Univ Nacl Cuyo, Inst Balseiro, RA-8400 San Carlos De Bariloche, Rio Negro, Argentina. RI Loeffler, Mark/C-9477-2012; OI Fama, Marcelo/0000-0003-3476-4669 FU CONICET; Comision Nacional de Energia Atomica (CNEA); NSF; [PICT2009-0092] FX M. B. thanks support from CONICET and grant PICT2009-0092. J.F.R.N. thanks support from the Comision Nacional de Energia Atomica (CNEA) for a scholarship. R.A.B. thanks NSF Astronomy for financial support. NR 26 TC 9 Z9 9 U1 3 U2 21 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 10 PY 2011 VL 743 IS 1 AR L5 DI 10.1088/2041-8205/743/1/L5 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 852QN UT WOS:000297372600005 ER PT J AU Thalmann, C Janson, M Buenzli, E Brandt, TD Wisniewski, JP Moro-Martin, A Usuda, T Schneider, G Carson, J McElwain, MW Grady, CA Goto, M Abe, L Brandner, W Dominik, C Egner, S Feldt, M Fukue, T Golota, T Guyon, O Hashimoto, J Hayano, Y Hayashi, M Hayashi, S Henning, T Hodapp, KW Ishii, M Iye, M Kandori, R Knapp, GR Kudo, T Kusakabe, N Kuzuhara, M Matsuo, T Miyama, S Morino, JI Nishimura, T Pyo, TS Serabyn, E Suto, H Suzuki, R Takahashi, YH Takami, M Takato, N Terada, H Tomono, D Turner, EL Watanabe, M Yamada, T Takami, H Tamura, M AF Thalmann, C. Janson, M. Buenzli, E. Brandt, T. D. Wisniewski, J. P. Moro-Martin, A. Usuda, T. Schneider, G. Carson, J. McElwain, M. W. Grady, C. A. Goto, M. Abe, L. Brandner, W. Dominik, C. Egner, S. Feldt, M. Fukue, T. Golota, T. Guyon, O. Hashimoto, J. Hayano, Y. Hayashi, M. Hayashi, S. Henning, T. Hodapp, K. W. Ishii, M. Iye, M. Kandori, R. Knapp, G. R. Kudo, T. Kusakabe, N. Kuzuhara, M. Matsuo, T. Miyama, S. Morino, J. -I. Nishimura, T. Pyo, T. -S. Serabyn, E. Suto, H. Suzuki, R. Takahashi, Y. H. Takami, M. Takato, N. Terada, H. Tomono, D. Turner, E. L. Watanabe, M. Yamada, T. Takami, H. Tamura, M. TI IMAGES OF THE EXTENDED OUTER REGIONS OF THE DEBRIS RING AROUND HR 4796 A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; planetary systems; stars: individual (HR 4796 A); techniques: high angular resolution ID CIRCUMSTELLAR DISK; BETA-PICTORIS; DUST DEBRIS; SUBSTELLAR COMPANION; PLANET; YOUNG; STAR; DISCOVERY; SIGNATURES; EVOLUTION AB We present high-contrast images of HR 4796 A taken with Subaru/HiCIAO in the H band, resolving the debris disk in scattered light. The application of specialized angular differential imaging methods allows us to trace the inner edge of the disk with high precision and reveals a pair of "streamers" extending radially outward from the ansae. Using a simple disk model with a power-law surface brightness profile, we demonstrate that the observed streamers can be understood as part of the smoothly tapered outer boundary of the debris disk, which is most visible at the ansae. Our observations are consistent with the expected result of a narrow planetesimal ring being ground up in a collisional cascade, yielding dust with a wide range of grain sizes. Radiation forces leave large grains in the ring and push smaller grains onto elliptical or even hyperbolic trajectories. We measure and characterize the disk's surface brightness profile, and confirm the previously suspected offset of the disk's center from the star's position along the ring's major axis. Furthermore, we present first evidence for an offset along the minor axis. Such offsets are commonly viewed as signposts for the presence of unseen planets within a disk's cavity. Our images also offer new constraints on the presence of companions down to the planetary mass regime (similar to 9 M-Jup at 0.'' 5, similar to 3 M-Jup at 1 ''). C1 [Thalmann, C.; Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Janson, M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. [Buenzli, E.] Swiss Fed Inst Technol, Inst Astron, Zurich, Switzerland. [Brandt, T. D.; Knapp, G. R.; Turner, E. L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Wisniewski, J. P.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Moro-Martin, A.] CAB CSIC INTA, Dept Astrophys, Madrid, Spain. [Usuda, T.; Egner, S.; Golota, T.; Guyon, O.; Hayano, Y.; Hayashi, M.; Hayashi, S.; Ishii, M.; Nishimura, T.; Pyo, T. -S.; Takato, N.; Terada, H.; Tomono, D.; Takami, H.] Subaru Telescope, Hilo, HI USA. [Schneider, G.] Univ Arizona, Steward Observ, Tucson, AZ USA. [Carson, J.] Coll Charleston, Charleston, SC 29401 USA. [McElwain, M. W.; Grady, C. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Grady, C. A.] Eureka Sci Inc, Oakland, CA 94602 USA. [Goto, M.; Brandner, W.; Feldt, M.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Abe, L.] Lab Hippolyte Fizeau, Nice, France. [Fukue, T.; Hashimoto, J.; Iye, M.; Kandori, R.; Kudo, T.; Kusakabe, N.; Kuzuhara, M.; Matsuo, T.; Miyama, S.; Morino, J. -I.; Suto, H.; Suzuki, R.; Tamura, M.] Natl Astron Observ Japan, Tokyo, Japan. [Hodapp, K. W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Kuzuhara, M.; Takahashi, Y. H.] Univ Tokyo, Dept Astron, Tokyo 113, Japan. [Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Turner, E. L.] Univ Tokyo, Inst Phys & Math Universe, Tokyo, Japan. [Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido, Japan. [Yamada, T.] Tohoku Univ, Astron Inst, Sendai, Miyagi 980, Japan. RP Thalmann, C (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. EM thalmann@uva.nl RI McElwain, Michael/D-3607-2012; Turner, Edwin/A-4295-2011; MIYAMA, Shoken/A-3598-2015; OI McElwain, Michael/0000-0003-0241-8956; Buenzli, Esther/0000-0003-3306-1486 FU Swiss National Science Foundation (SNSF); US National Science Foundation [AST-1009203, DGE-0646086]; Japanese MEXT [22000005] FX We thank David Lafreniere for generously providing us with the source code for his LOCI algorithm, and Jean-Charles Augereau for his GRaTer code. The authors acknowledge partial support from the Swiss National Science Foundation (SNSF), US National Science Foundation grants AST-1009203 and DGE-0646086, and a Japanese MEXT Grant-in-Aid for Specially Promoted Research (No. 22000005). NR 46 TC 43 Z9 43 U1 0 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 10 PY 2011 VL 743 IS 1 AR L6 DI 10.1088/2041-8205/743/1/L6 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 852QN UT WOS:000297372600006 ER PT J AU Zima, HP James, ML Springer, PL AF Zima, Hans P. James, Mark L. Springer, Paul L. TI Fault-tolerant on-board computing for robotic space missions SO CONCURRENCY AND COMPUTATION-PRACTICE & EXPERIENCE LA English DT Article DE space-borne computing; fault tolerance; introspection ID CHAPEL AB This paper describes an approach to providing software fault tolerance for future deep-space robotic National Aeronautics and Space Administration missions, which will require a high degree of autonomy supported by an enhanced on-board computational capability. We focus on introspection-based adaptive fault tolerance guided by the specific requirements of applications. Introspection supports monitoring of the program execution with the goal of identifying, locating, and analyzing errors. Fault tolerance assertions for the introspection system can be provided by the user, domain-specific knowledge, or via the results of static or dynamic program analysis. This work is part of an on-going project at the Jet Propulsion Laboratory in Pasadena, California. Copyright (C) 2011 John Wiley & Sons, Ltd. C1 [Zima, Hans P.; James, Mark L.; Springer, Paul L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zima, Hans P.] Univ Vienna, Inst Comp Sci, Vienna, Austria. RP Zima, HP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM zima@jpl.nasa.gov FU National Aeronautics and Space Administration; internal Research and Technology Development program FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and funded through the internal Research and Technology Development program. NR 25 TC 1 Z9 1 U1 0 U2 5 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1532-0626 J9 CONCURR COMP-PRACT E JI Concurr. Comput.-Pract. Exp. PD DEC 10 PY 2011 VL 23 IS 17 BP 2192 EP 2204 DI 10.1002/cpe.1768 PG 13 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA 849SJ UT WOS:000297145100013 ER PT J AU Nickerson, CA Ott, CM Castro, SL Garcia, VM Molina, TC Briggler, JT Pitt, AL Tavano, JJ Byram, JK Barrila, J Nickerson, MA AF Nickerson, Cheryl A. Ott, C. Mark Castro, Sarah L. Garcia, Veronica M. Molina, Thomas C. Briggler, Jeffrey T. Pitt, Amber L. Tavano, Joseph J. Byram, J. Kelly Barrila, Jennifer Nickerson, Max A. TI Evaluation of Microorganisms Cultured from Injured and Repressed Tissue Regeneration Sites in Endangered Giant Aquatic Ozark Hellbender Salamanders SO PLOS ONE LA English DT Article ID CRYPTOBRANCHUS-ALLEGANIENSIS-BISHOPI; ANTIMICROBIAL PEPTIDE DEFENSES; FUNGUS BATRACHOCHYTRIUM-DENDROBATIDIS; CHYTRID FUNGUS; CUTANEOUS BACTERIA; ENVIRONMENTAL-CONDITIONS; GRANULICATELLA-ADIACENS; BASIDIOBOLUS-RANARUM; AMPHIBIAN DECLINES; PLETHODON-CINEREUS AB Investigation into the causes underlying the rapid, global amphibian decline provides critical insight into the effects of changing ecosystems. Hypothesized and confirmed links between amphibian declines, disease, and environmental changes are increasingly represented in published literature. However, there are few long-term amphibian studies that include data on population size, abnormality/injury rates, disease, and habitat variables to adequately assess changes through time. We cultured and identified microorganisms isolated from abnormal/injured and repressed tissue regeneration sites of the endangered Ozark Hellbender, Cryptobranchus alleganiensis bishopi, to discover potential causative agents responsible for their significant decline in health and population. This organism and our study site were chosen because the population and habitat of C. a. bishopi have been intensively studied from 1969-2009, and the abnormality/injury rate and apparent lack of regeneration were established. Although many bacterial and fungal isolates recovered were common environmental organisms, several opportunistic pathogens were identified in association with only the injured tissues of C. a. bishopi. Bacterial isolates included Aeromonas hydrophila, a known amphibian pathogen, Granulicetella adiacens, Gordonai terrae, Stenotrophomonas maltophilia, Aerococcus viridans, Streptococcus pneumoniae and a variety of Pseudomonads, including Pseudomonas aeruginosa, P. stutzeri, and P. alcaligenes. Fungal isolates included species in the genera Penicillium, Acremonium, Cladosporium, Curvularia, Fusarium, Streptomycetes, and the Class Hyphomycetes. Many of the opportunistic pathogens identified are known to form biofilms. Lack of isolation of the same organism from all wounds suggests that the etiological agent responsible for the damage to C. a. bishopi may not be a single organism. To our knowledge, this is the first study to profile the external microbial consortia cultured from a Cryptobranchid salamander. The incidence of abnormalities/injury and retarded regeneration in C. a. bishopi may have many contributing factors including disease and habitat degradation. Results from this study may provide insight into other amphibian population declines. C1 [Nickerson, Cheryl A.; Barrila, Jennifer] Arizona State Univ, Sch Life Sci, Biodesign Inst, Ctr Infect Dis & Vaccinol, Tempe, AZ 85287 USA. [Ott, C. Mark] NASA, Lyndon B Johnson Space Ctr, Habitabil & Environm Factors Div, Houston, TX 77058 USA. [Castro, Sarah L.] Univ Texas Med Branch, Dept Microbiol & Immunol, Galveston, TX USA. [Garcia, Veronica M.; Molina, Thomas C.] Wyle Labs, EASI, Houston, TX USA. [Briggler, Jeffrey T.] Missouri Dept Conservat, Jefferson City, MO USA. [Pitt, Amber L.; Tavano, Joseph J.; Byram, J. Kelly; Nickerson, Max A.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. RP Nickerson, CA (reprint author), Arizona State Univ, Sch Life Sci, Biodesign Inst, Ctr Infect Dis & Vaccinol, Tempe, AZ 85287 USA. EM maxn@flmnh.ufl.edu FU NASA [NNX07AM16G, NCC2-1362]; St. Louis Zoological Park; Reptile and Amphibian Conservation Corps FX NASA student grant NNX07AM16G, NASA grant NCC2-1362, The St. Louis Zoological Park, and The Reptile and Amphibian Conservation Corps. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 89 TC 5 Z9 5 U1 1 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 DEC 9 PY 2011 VL 6 IS 12 AR e28906 DI 10.1371/journal.pone.0028906 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 870JO UT WOS:000298665600014 PM 22205979 ER PT J AU Lindenmaier, R Strong, K Batchelor, RL Bernath, PF Chabrillat, S Chipperfield, MP Daffer, WH Drummond, JR Feng, W Jonsson, AI Kolonjari, F Manney, GL McLinden, C Menard, R Walker, KA AF Lindenmaier, R. Strong, K. Batchelor, R. L. Bernath, P. F. Chabrillat, S. Chipperfield, M. P. Daffer, W. H. Drummond, J. R. Feng, W. Jonsson, A. I. Kolonjari, F. Manney, G. L. McLinden, C. Menard, R. Walker, K. A. TI A study of the Arctic NOy budget above Eureka, Canada SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID FOURIER-TRANSFORM SPECTROMETER; DELTA-EDDINGTON APPROXIMATION; MIDDLE ATMOSPHERE MODEL; TOTAL REACTIVE NITROGEN; ACE-FTS; STRATOSPHERIC OZONE; POLAR VORTEX; SATELLITE-OBSERVATIONS; CHLORINE RESERVOIRS; UPPER TROPOSPHERE AB [1] Four years of trace gas measurements have been acquired using the Bruker 125HR Fourier Transform Infrared (FTIR) spectrometer installed at the Polar Environment Atmospheric Research Laboratory (PEARL) in the Canadian high Arctic. These have been compared with data from three models, namely the Canadian Middle Atmosphere Model Data Assimilation System (CMAM-DAS), the Global Environmental Multiscale stratospheric model with the online Belgium Atmospheric CHemistry package (GEM-BACH), and the off-line 3D chemical transport model SLIMCAT to assess the total reactive nitrogen, NOy, budget above Eureka, Nunavut (80.05 degrees N, 86.42 degrees W). The FTIR data have been also compared with satellite measurements by the Atmospheric Chemistry Experiment-Fourier Transform Spectrometer (ACE-FTS). The FTIR is able to measure four of the five primary species that form NOy: NO, NO2, HNO3, and ClONO2, while the fifth, N2O5, was obtained using the N2O5/(NO + NO2) ratio derived from the models and ACE-FTS. Combining these results, a four-year time series of NOy 15-40 km partial columns was calculated. Comparisons with each model were made, revealing mean differences (+/- standard error of the mean) relative to the FTIR of (-16.0 +/- 0.6)%, (5.5 +/- 1.0)%, and (-5.8 +/- 0.4)% for CMAM-DAS, GEM-BACH, and SLIMCAT, respectively. The mean difference between the ACE-FTS and FTIR NOy partial columns was (5.6 +/- 2.3)%. While we found no significant seasonal and interannual differences in the FTIR NOy stratospheric columns, the partial columns display nearly twice as much variability during the spring compared to the summer period. C1 [Lindenmaier, R.; Strong, K.; Jonsson, A. I.; Kolonjari, F.; Walker, K. A.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Batchelor, R. L.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80310 USA. [Bernath, P. F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Chabrillat, S.] Belgian Inst Space Aeron, Chem Weather Serv, B-1180 Brussels, Belgium. [Chipperfield, M. P.; Feng, W.] Univ Leeds, Sch Earth & Environm, Inst Climate & Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England. [Daffer, W. H.; Manney, G. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Drummond, J. R.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 1Z9, Canada. [McLinden, C.] Environm Canada, Air Qual Res Div, Downsview, ON M3H 5T4, Canada. [Menard, R.] Environm Canada, Air Qual Res Div, Dorval, PQ H9P 1J3, Canada. [Manney, G. L.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. RP Lindenmaier, R (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada. EM rodica@atmosp.physics.utoronto.ca RI Drummond, James/O-7467-2014; Bernath, Peter/B-6567-2012; Strong, Kimberly/D-2563-2012; Jonsson, Andreas/B-3887-2013; Chipperfield, Martyn/H-6359-2013; FENG, WUHU/B-8327-2008 OI Bernath, Peter/0000-0002-1255-396X; Jonsson, Andreas/0000-0003-0321-6213; Chipperfield, Martyn/0000-0002-6803-4149; FENG, WUHU/0000-0002-9907-9120 FU Nova Scotia Research Innovation Trust; Canadian Foundation for Climate and Atmospheric Sciences; Canadian Foundation for Innovation; Canadian Space Agency (CSA); Environment Canada (EC); Government of Canada; Natural Sciences and Engineering Research Council (NSERC); Ontario Innovation Trust; Polar Continental Shelf Program; Ontario Research Fund; Northern Scientific Training Program FX The authors wish to thank the staff at the Eureka weather station and CANDAC for the logistical and on-site support provided at Eureka. They also thank CANDAC/PEARL Operations Manager Pierre Fogal, and Ashley Harrett, Alexei Khmel, Paul Loewen, Keith MacQuarrie, Oleg Mikhailov, and Matt Okraszewski, the CANDAC operators, for their invaluable assistance in maintaining the instrument and taking measurements. CANDAC and PEARL are funded by the Atlantic Innovation Fund/Nova Scotia Research Innovation Trust, the Canadian Foundation for Climate and Atmospheric Sciences, the Canadian Foundation for Innovation, the Canadian Space Agency (CSA), Environment Canada (EC), Government of Canada International Polar Year funding, the Natural Sciences and Engineering Research Council (NSERC), the Ontario Innovation Trust, the Polar Continental Shelf Program, and the Ontario Research Fund. The authors wish to thank the CMAM-DAS group members Stephen Beagley, Michael Neish, Yulia Nezlin, Saroja Polavarapu, Shuzhan Ren, Yves Rochon, and Theodore Shepherd for their efforts to produce the analysis and for making the results available, and David Plummer at Environment Canada for helping us interpret some of the CMAM biases. We also thank Keeyoon Sung for his work compiling the a priori profiles and covariance matrices used in the FTIR retrievals. The Atmospheric Chemistry Experiment, also known as SCISAT, is a Canadian-led mission mainly supported by the CSA and NSERC. The Canadian Arctic ACE validation campaigns are supported by the CSA, EC, NSERC, and the Northern Scientific Training Program. NR 73 TC 2 Z9 2 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 DEC 8 PY 2011 VL 116 AR D23302 DI 10.1029/2011JD016207 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 861DB UT WOS:000297998100004 ER PT J AU Turk, FJ Park, KW Haddad, ZS Rodriguez, P Hudak, DR AF Turk, F. Joseph Park, Kyung-Won Haddad, Ziad S. Rodriguez, Peter Hudak, David R. TI Constraining CloudSat-based snowfall profiles using surface observations and C-band ground radar SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SINGLE-SCATTERING PROPERTIES; RAINDROP SIZE DISTRIBUTION; MICROWAVE-FREQUENCIES; PRECIPITATION PROFILES; MICROPHYSICS SCHEME; VIDEO DISDROMETER; ICE PARTICLES; SEA-ICE; PART I; RADIOMETER AB The CloudSat Precipitation Radar, launched in 2006, provides vertical profiles of W-band (94 GHz) reflectivity and is sensitive to falling snow through all but the most intense precipitating cloud structures. Precipitation retrievals of falling snow are affected by a wide diversity of factors describing the medium, such as snow particle shape, size, and composition, which in turn are controlled by ambient factors including the environmental temperature and humidity. Because satellite-based radiometric sounders such as the Microwave Humidity Sounder (MHS) operate without the benefit of coordinated space radar observations, microphysical descriptions of the snow particle medium derived from CloudSat or other radar observations are beneficial to passive microwave (PMW) radiometer-only snowfall retrieval methods. At the coarse scale of these PMW observations, the radiative signal due to the snow is relatively weak compared to the contributions from the atmosphere and the land surface emissivity. Using the C-band (5 GHz) polarization-agile King City radar (WKR) operated by Environment Canada, we examined the vertical structure of winter precipitation events from coordinated overpasses of CloudSat and NOAA 18 (MHS). Two-dimensional video disdrometer observations are used to limit (constrain) the range of the drop-size distribution parameters that are provided through a priori databases to dual-frequency (C/W-band) radar retrieval. Bayesian retrievals using the constrained database produce water content profiles that more closely replicate the observed radar reflectivity profiles and transition smoothly between the single-frequency (CloudSat only) and dual-frequency regions. C1 [Turk, F. Joseph; Park, Kyung-Won; Haddad, Ziad S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rodriguez, Peter; Hudak, David R.] Environm Canada, Cloud Phys & Severe Weather Res Sect, Toronto, ON L7B 1A3, Canada. RP Turk, FJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jturk@jpl.nasa.gov FU NASA's CloudSat mission; NASA's Precipitation Measurement Missions (PMM); National Aeronautics and Space Administration FX We acknowledge support from NASA's CloudSat mission through Hal Maring and from NASA's Precipitation Measurement Missions (PMM) through Ramesh Kakar. We thank Gwo-Jong Huang from Colorado State University for his assistance with 2DVD data analysis and Guosheng Liu from Florida State University for expanding the low-frequency range of his snow particle database. CloudSat data were made available via the CloudSat Data Processing Center (DPC) managed by the Cooperative Institute for Research in the Atmosphere (CIRA) at Colorado State University. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 48 TC 4 Z9 4 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 8 PY 2011 VL 116 AR D23205 DI 10.1029/2011JD016126 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 861DB UT WOS:000297998100002 ER PT J AU Ackermann, M Ajello, M Albert, A Atwood, WB Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bloom, ED Bonamente, E Borgland, AW Bregeon, J Brigida, M Bruel, P Buehler, R Burnett, TH Buson, S Caliandro, GA Cameron, RA Canadas, B Caraveo, PA Casandjian, JM Cecchi, C Charles, E Chekhtman, A Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S de Angelis, A de Palma, F Dermer, CD Digel, SW Silva, EDE Drell, PS Drlica-Wagner, A Falletti, L Favuzzi, C Fegan, SJ Ferrara, EC Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Guiriec, S Gustafsson, M Hadasch, D Hayashida, M Hays, E Hughes, RE Jeltema, TE Johannesson, G Johnson, RP Johnson, AS Kamae, T Katagiri, H Kataoka, J Knodlseder, J Kuss, M Lande, J Latronico, L Lionetto, AM Garde, ML Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Madejski, GM Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mitthumsiri, W Mizuno, T Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Naumann-Godo, M Norris, JP Nuss, E Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Ozaki, M Paneque, D Parent, D Pesce-Rollins, M Pierbattista, M Piron, F Pivato, G Porter, TA Profumo, S Raino, S Razzano, M Reimer, A Reimer, O Ritz, S Roth, M Sadrozinski, HFW Sbarra, C Scargle, JD Schalk, TL Sgro, C Siskind, EJ Spandre, G Spinelli, P Strigari, L Suson, DJ Tajima, H Takahashi, H Tanaka, T Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Torres, DF Troja, E Uchiyama, Y Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Wood, M Yang, Z Zimmer, S Kaplinghat, M Martinez, GD AF Ackermann, M. Ajello, M. Albert, A. Atwood, W. B. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Burnett, T. H. Buson, S. Caliandro, G. A. Cameron, R. A. Canadas, B. Caraveo, P. A. Casandjian, J. M. Cecchi, C. Charles, E. Chekhtman, A. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. de Angelis, A. de Palma, F. Dermer, C. D. Digel, S. W. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Falletti, L. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Guiriec, S. Gustafsson, M. Hadasch, D. Hayashida, M. Hays, E. Hughes, R. E. Jeltema, T. E. Johannesson, G. Johnson, R. P. Johnson, A. S. Kamae, T. Katagiri, H. Kataoka, J. Knoedlseder, J. Kuss, M. Lande, J. Latronico, L. Lionetto, A. M. Garde, M. Llena Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Madejski, G. M. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Naumann-Godo, M. Norris, J. P. Nuss, E. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Parent, D. Pesce-Rollins, M. Pierbattista, M. Piron, F. Pivato, G. Porter, T. A. Profumo, S. Raino, S. Razzano, M. Reimer, A. Reimer, O. Ritz, S. Roth, M. Sadrozinski, H. F. -W. Sbarra, C. Scargle, J. D. Schalk, T. L. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Strigari, L. Suson, D. J. Tajima, H. Takahashi, H. Tanaka, T. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Torres, D. F. Troja, E. Uchiyama, Y. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Wood, M. Yang, Z. Zimmer, S. Kaplinghat, M. Martinez, G. D. CA Fermi-LAT Collaboration TI Constraining Dark Matter Models from a Combined Analysis of Milky Way Satellites with the Fermi Large Area Telescope SO PHYSICAL REVIEW LETTERS LA English DT Article ID DWARF SPHEROIDAL GALAXIES; COMPLETE SPECTROSCOPIC SURVEY; GAMMA-RAY EMISSION; LOCAL GROUP; SEGUE 1; KINEMATICS; SEARCH; HALO AB Satellite galaxies of the Milky Way are among the most promising targets for dark matter searches in gamma rays. We present a search for dark matter consisting of weakly interacting massive particles, applying a joint likelihood analysis to 10 satellite galaxies with 24 months of data of the Fermi Large Area Telescope. No dark matter signal is detected. Including the uncertainty in the dark matter distribution, robust upper limits are placed on dark matter annihilation cross sections. The 95% confidence level upper limits range from about 10(-26) cm(3) s(-1) at 5 GeV to about 5 x 10(-23) cm(3) s(-1) at 1 TeV, depending on the dark matter annihilation final state. For the first time, using gamma rays, we are able to rule out models with the most generic cross section (similar to 3 x 10(-26) cm(3) s(-1) for a purely s-wave cross section), without assuming additional boost factors. C1 [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Strigari, L.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Strigari, L.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Albert, A.; Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Atwood, W. B.; Jeltema, T. E.; Johnson, R. P.; Profumo, S.; Razzano, M.; Ritz, S.; Sadrozinski, H. F. -W.; Schalk, T. L.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Jeltema, T. E.; Johnson, R. P.; Profumo, S.; Razzano, M.; Ritz, S.; Sadrozinski, H. F. -W.; Schalk, T. L.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.] Univ Paris Diderot, CEA Saclay, CNRS, CEA,IRFU,Lab AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Gustafsson, M.; Sbarra, C.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Pivato, G.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Burnett, T. H.; Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain. [Canadas, B.; Lionetto, A. M.; Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Canadas, B.; Lionetto, A. M.; Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA. [Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Cohen-Tanugi, J.; Falletti, L.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34095 Montpellier, France. [Conrad, J.; Garde, M. Llena; Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Garde, M. Llena; Yang, Z.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dermer, C. D.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ferrara, E. C.; Gehrels, N.; Hays, E.; McEnery, J. E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fukazawa, Y.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Katagiri, H.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, IRAP, UPS OMP, GAHEC, Toulouse, France. [Lott, B.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Parent, D.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Torres, D. F.] ICREA, Barcelona 08010, Spain. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Kaplinghat, M.; Martinez, G. D.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA. RP Ackermann, M (reprint author), Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. EM johann.cohen-tanugi@lupm.in2p3.fr; conrad@fysik.su.se; maja.garde@fysik.su.se RI Hays, Elizabeth/D-3257-2012; Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Thompson, David/D-2939-2012; Morselli, Aldo/G-6769-2011; Reimer, Olaf/A-3117-2013; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Ozaki, Masanobu/K-1165-2013; OI Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Giordano, Francesco/0000-0002-8651-2394; De Angelis, Alessandro/0000-0002-3288-2517; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Strigari, Louis/0000-0001-5672-6079; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; Giroletti, Marcello/0000-0002-8657-8852; Cutini, Sara/0000-0002-1271-2924; Berenji, Bijan/0000-0002-4551-772X; giglietto, nicola/0000-0002-9021-2888; Thompson, David/0000-0001-5217-9135; Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; lubrano, pasquale/0000-0003-0221-4806; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726 FU LAT; NASA, United States; DOE, United States; CEA/Irfu, France; IN2P3/CNRS in France; ASI, Italy; INFN, Italy; MEXT, Japan; KEK, Japan; JAXA, Japan; K.A. Wallenberg Foundation; Swedish Research Council; National Space Board in Sweden; INAF in Italy; CNES in France; NASA [NNX09AD09G] FX The Fermi-LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States; CEA/Irfu and IN2P3/CNRS in France; ASI and INFN in Italy; MEXT, KEK, and JAXA in Japan; and the K.A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. External collaborators M. Kaplinghat and G. D. Martinez acknowledge support from NASA Grant No. NNX09AD09G. NR 34 TC 366 Z9 366 U1 4 U2 26 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD DEC 8 PY 2011 VL 107 IS 24 AR 241302 DI 10.1103/PhysRevLett.107.241302 PG 6 WC Physics, Multidisciplinary SC Physics GA 858LC UT WOS:000297797700002 PM 22242987 ER PT J AU Zhai, CX Shao, MK Goullioud, R Nemati, B AF Zhai, Chengxing Shao, Mike Goullioud, Renaud Nemati, Bijan TI Micro-pixel accuracy centroid displacement estimation and detector calibration SO PROCEEDINGS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE precision astrometry; point spread function reconstruction; pixel response calibration; centroid estimation ID CHARGE-COUPLED-DEVICE; PHOTOMETRY AB Conventional centroid estimation fits a template point spread function (PSF) to image data. Because the PSF is typically not known to high accuracy, systematic errors exist. Here, we present an accurate centroid displacement estimation algorithm by reconstructing the PSF from Nyquist-sampled images. In absence of inter-pixel response variations, this method can estimate centroid displacement between two 32 x 32 images to sub-micropixel accuracy. Inter-pixel response variations can be calibrated in Fourier space by using laser metrology. The inter-pixel variations of Fourier transforms of the pixel response functions can be conveniently expressed in terms of powers of spatial wavenumbers. Calibrating up to the third-order terms in the expansion, the displacement estimation is accurate to a few micro-pixels. This algorithm is applicable to a new mission concept of performing mirco-arcsecond level relative astrometry using a 1m telescope for detecting terrestrial exoplanets and high-precision photometry missions. C1 [Zhai, Chengxing; Shao, Mike; Goullioud, Renaud; Nemati, Bijan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Zhai, CX (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM chengxing.zhai@jpl.nasa.gov FU National Aeronautics and Space Administration FX This work was prepared at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. (C) 2011 California Institute of Technology. Government sponsorship acknowledged. NR 8 TC 17 Z9 19 U1 0 U2 3 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-5021 J9 P ROY SOC A-MATH PHY JI Proc. R. Soc. A-Math. Phys. Eng. Sci. PD DEC 8 PY 2011 VL 467 IS 2136 BP 3550 EP 3569 DI 10.1098/rspa.2011.0255 PG 20 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 842HC UT WOS:000296585800011 ER PT J AU Fortenberry, RC Huang, XC Francisco, JS Crawford, TD Lee, TJ AF Fortenberry, Ryan C. Huang, Xinchuan Francisco, Joseph S. Crawford, T. Daniel Lee, Timothy J. TI Vibrational frequencies and spectroscopic constants from quartic force fields for cis-HOCO: The radical and the anion SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID TRANS-HOCO; DISSOCIATIVE PHOTODETACHMENT; POLYATOMIC-MOLECULES; ANALYTIC EVALUATION; TRIPLE EXCITATIONS; ENERGY GRADIENTS; WAVE-FUNCTIONS; BASIS-SETS; ABSORPTION; SPECTRUM AB The use of accurate quartic force fields together with vibrational configuration interaction recently predicted gas phase fundamental vibrational frequencies of the trans-HOCO radical to within 4 cm(-1) of experimental results for the two highest frequency modes. Utilizing the same approach, we are providing a full list of fundamental vibrational frequencies and spectroscopic constants for the cis-HOCO system in both radical and anionic forms. Our predicted geometrical parameters of the cis-HOCO radical match experiment and previous computation to better than 1% deviation, and previous theoretical work agrees equally well for the anion. Correspondence between vibrational perturbation theory and variational vibrational configuration interaction for prediction of the frequencies of each mode is strong, better than 5 cm(-1), except for the torsional motion, similar to what has been previously identified in the trans-HOCO radical. Among other considerations, our results are immediately applicable to dissociative photodetachment experiments which initially draw on the cis-HOCO anion since it is the most stable conformer of the anion and is used to gain insight into the portion of the OH + CO potential surface where the HOCO radical is believed to form, and we are also providing highly accurate electron binding energies relevant to these experiments. (C) 2011 American Institute of Physics. [doi:10.1063/1.3663615] C1 [Fortenberry, Ryan C.; Crawford, T. Daniel] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA. [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. [Francisco, Joseph S.] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA. [Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Fortenberry, RC (reprint author), Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA. EM Xinchuan.Huang-1@nasa.gov; crawdad@vt.edu; Timothy.J.Lee@nasa.gov RI HUANG, XINCHUAN/A-3266-2013; Lee, Timothy/K-2838-2012; Crawford, Thomas/A-9271-2017 OI Crawford, Thomas/0000-0002-7961-7016 FU U.S. National Science Foundation [CHE-1058420]; Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) [CHE-0741927]; NASA [08-APRA08-0050, 10-APRA10-0096]; NASA/SETI Institute [NNX09AI49A] FX The work undertaken by R. C. F. and T. D. C. is supported by the U.S. National Science Foundation through award CHE-1058420 and through a Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) award CHE-0741927. T.J.L. and X. H. gratefully acknowledge funding from NASA Grant No. 08-APRA08-0050 and NASA Grant No. 10-APRA10-0096. X. H. also acknowledges support from the NASA/SETI Institute Cooperative Agreement NNX09AI49A. Dr. Andrew Simmonett of the University of Georgia once more allowed us to use his CheMVP program in the creation of Fig. 1. NR 57 TC 41 Z9 41 U1 1 U2 10 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 7 PY 2011 VL 135 IS 21 AR 214303 DI 10.1063/1.3663615 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 867YM UT WOS:000298490700016 PM 22149788 ER PT J AU Karydis, VA Kumar, P Barahona, D Sokolik, IN Nenes, A AF Karydis, V. A. Kumar, P. Barahona, D. Sokolik, I. N. Nenes, A. TI On the effect of dust particles on global cloud condensation nuclei and cloud droplet number SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GROUND-BASED MEASUREMENTS; LONG-RANGE TRANSPORT; MINERAL DUST; RADIATIVE PROPERTIES; AFRICAN DUST; MARINE STRATOCUMULUS; ACTIVATION KINETICS; AEROSOL ACTIVATION; MODEL SIMULATIONS; SULFATE AEROSOL AB Aerosol-cloud interaction studies to date consider aerosol with a substantial fraction of soluble material as the sole source of cloud condensation nuclei (CCN). Emerging evidence suggests that mineral dust can act as good CCN through water adsorption onto the surface of particles. This study provides a first assessment of the contribution of insoluble dust to global CCN and cloud droplet number concentration (CDNC). Simulations are carried out with the NASA Global Modeling Initiative chemical transport model with an online aerosol simulation, considering emissions from fossil fuel, biomass burning, marine, and dust sources. CDNC is calculated online and explicitly considers the competition of soluble and insoluble CCN for water vapor. The predicted annual average contribution of insoluble mineral dust to CCN and CDNC in cloud-forming areas is up to 40 and 23.8%, respectively. Sensitivity tests suggest that uncertainties in dust size distribution and water adsorption parameters modulate the contribution of mineral dust to CDNC by 23 and 56%, respectively. Coating of dust by hygroscopic salts during the atmospheric aging causes a twofold enhancement of the dust contribution to CCN; the aged dust, however, can substantially deplete in-cloud supersaturation during the initial stages of cloud formation and can eventually reduce CDNC. Considering the hydrophilicity from adsorption and hygroscopicity from solute is required to comprehensively capture the dust-warm cloud interactions. The framework presented here addresses this need and can be easily integrated in atmospheric models. C1 [Karydis, V. A.; Sokolik, I. N.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Kumar, P.; Nenes, A.] Georgia Inst Technol, Sch Chem & Biomol Engn, Atlanta, GA 30332 USA. [Barahona, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Barahona, D.] IM Syst Inc, Rockville, MD USA. RP Karydis, VA (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, 311 Ferst Dr, Atlanta, GA 30332 USA. EM athanasios.nenes@gatech.edu RI Barahona, Donifan/G-4157-2011 FU NASA-ACMAP; ConocoPhillips; NOAA FX We would like to acknowledge support from NASA-ACMAP, ConocoPhillips, and NOAA. We are also thankful for the important comments by three anonymous reviewers, which have helped to improve the quality of the manuscript. NR 112 TC 46 Z9 46 U1 3 U2 41 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 DEC 7 PY 2011 VL 116 AR D23204 DI 10.1029/2011JD016283 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 861CX UT WOS:000297997700003 ER PT J AU Hasegawa, A Tsurutani, BT AF Hasegawa, Akira Tsurutani, Bruce T. TI Mirror Mode Expansion in Planetary Magnetosheaths: Bohm-like Diffusion SO PHYSICAL REVIEW LETTERS LA English DT Article ID MAGNETIC-FIELD; SOLAR-WIND; MAGNETOPAUSE; PLASMA; MAGNETOSPHERE; DEPLETION; EVOLUTION; WAVES AB Observed scale sizes of mirror modes in planetary magnetosheaths tend to be equal or larger than those that correspond to the maximum growth rate of the mirror instability: 9 rho(p) (proton gyroradius). These phenomena can be accounted for by introducing a diffusion process (Bohm) that shifts the spectra to lower wave numbers as the mode convects away from the source to the observation point. The theory is applied to data obtained in the magnetosheaths of Earth, Jupiter, Saturn, and the heliosheath, and shown to provide reasonable agreement to past spacecraft observations. Further observational tests of the theory are suggested. C1 [Hasegawa, Akira] Osaka Univ, Suita, Osaka, Japan. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hasegawa, A (reprint author), Osaka Univ, Yamadaoka 2-1, Suita, Osaka, Japan. FU NASA FX Portions of this work were performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. A. H. thanks Professors Zhihong Lin and Liu Chen of the Department of Physics and Astrophysics of the University of California, Irvine for their stimulating discussions and hospitality, during which this Letter was completed. NR 24 TC 6 Z9 6 U1 0 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD DEC 7 PY 2011 VL 107 IS 24 AR 245005 DI 10.1103/PhysRevLett.107.245005 PG 4 WC Physics, Multidisciplinary SC Physics GA 858KV UT WOS:000297796800010 PM 22243008 ER PT J AU Catherinot, J Prigent, C Maurer, R Papa, F Jimenez, C Aires, F Rossow, WB AF Catherinot, J. Prigent, C. Maurer, R. Papa, F. Jimenez, C. Aires, F. Rossow, W. B. TI Evaluation of "all weather" microwave-derived land surface temperatures with in situ CEOP measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID INFRARED SATELLITE-OBSERVATIONS; HIGH-RESOLUTION RADIOMETER; TRACK SCANNING RADIOMETER; BAYESIAN STATISTICS; WATER-VAPOR; ISCCP; RETRIEVAL; EMISSIVITIES; INFORMATION; VALIDATION AB Land surface skin temperature Ts plays a key role in meteorological and climatological processes but the availability and the accuracy of Ts measurements over land are still limited, especially under cloudy conditions. Ts estimates from infrared satellite observations can only be derived under clear sky. Passive microwave measurements are much less affected by clouds and can provide Ts regardless of the cloud conditions. A neural network inversion including first guess information has been previously developed to retrieve Ts, along with atmospheric water vapor, cloud liquid water, and surface emissivities over land from Special Sensor Microwave/Imager measurements, with a spatial resolution of 0.25 x 0.25, at least twice daily. In this study, Ts estimates are evaluated through careful comparisons with in situ measurements in different environments over a full annual cycle. Under clear sky conditions, the quality of our microwave neural network retrieval is equivalent to the infrared International Satellite Cloud Climatology Project products, for most in situ stations, with errors similar to 3 K as compared to in situ measurements. The performance of the microwave algorithm is similar under clear and cloudy conditions, confirming the potential of the microwaves under clouds. The Ts accuracy does not depend upon the surface emissivity, as the variability of this parameter is accounted for in the processing. Our microwave Ts have been calculated for more than 15 years (1993 to mid-2008). These "all weather" Ts are a very valuable complement to the IR-derived Ts, for use in atmospheric and surface models. C1 [Catherinot, J.; Papa, F.; Rossow, W. B.] CUNY City Coll, NOAA, Cooperat Remote Sensing Sci & Technol Ctr, New York, NY 10031 USA. [Catherinot, J.; Prigent, C.; Jimenez, C.; Aires, F.] CNRS, Observ Paris, Lab Etud Rayonnement & Matiere Astrophys, F-75014 Paris, France. [Maurer, R.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Aires, F.] Estellus, F-75002 Paris, France. RP Catherinot, J (reprint author), CUNY City Coll, NOAA, Cooperat Remote Sensing Sci & Technol Ctr, New York, NY 10031 USA. EM catherine.prigent@obspm.fr RI Papa, Fabrice/D-3695-2009; Rossow, William/F-3138-2015 OI Papa, Fabrice/0000-0001-6305-6253; FU NASA [NNXD7A090G]; NASA Energy and Water Study (NEWS) FX The authors wish to thank Thomas Holmes and Tom Jackson for their careful reading of the manuscript and their very valuable comments. They are also thankful to three anonymous reviewers for their careful reading and interesting suggestions. Work on this study by Catherinot and Rossow was supported by NASA grant NNXD7A090G, the NASA Energy and Water Study (NEWS). NR 34 TC 5 Z9 5 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 6 PY 2011 VL 116 AR D23105 DI 10.1029/2011JD016439 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 861CU UT WOS:000297997400001 ER PT J AU Feng, Z Dong, XQ Xi, BK Schumacher, C Minnis, P Khaiyer, M AF Feng, Zhe Dong, Xiquan Xi, Baike Schumacher, Courtney Minnis, Patrick Khaiyer, Mandana TI Top-of-atmosphere radiation budget of convective core/stratiform rain and anvil clouds from deep convective systems SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ENVIRONMENTAL-CONDITIONS; MEASUREMENT PROGRAM; RADAR REFLECTIVITY; IRIS HYPOTHESIS; DIURNAL CYCLE; SQUALL LINES; WATER-VAPOR; WARM POOL; PRECIPITATION; TRMM AB A new hybrid classification algorithm to objectively identify Deep Convective Systems (DCSs) in radar and satellite observations has been developed. This algorithm can classify the convective cores (CC), stratiform rain (SR) area and nonprecipitating anvil cloud (AC) from the identified DCSs through an integrative analysis of ground-based scanning radar and geostationary satellite data over the Southern Great Plains. In developing the algorithm, AC is delineated into transitional, thick, and thin components. While there are distinct physical/dynamical differences among these subcategories, their top-of-atmosphere (TOA) radiative fluxes are not significantly different. Therefore, these anvil subcategories are grouped as total anvil, and the radiative impact of each DCS component on the TOA radiation budget is quantitatively estimated. We found that more DCSs occurred during late afternoon, producing peak AC fraction right after sunset. AC covers 3 times the area of SR and almost an order of magnitude larger than CC. The average outgoing longwave (LW) irradiances are almost identical for CC and SR, while slightly higher for AC. Compared to the clear-sky average, the reflected shortwave (SW) fluxes for the three DCS components are greater by a factor of 2-3 and create a strong cooling effect at TOA. The calculated SW and LW cloud radiative forcing (CRF) of AC contribute up to 31% of total NET CRF, while CC and SR contribute only 4 and 11%, respectively. The hybrid classification further lays the groundwork for studying the life cycle of DCS and improvements in geostationary satellite IR-based precipitation retrievals. C1 [Feng, Zhe; Dong, Xiquan; Xi, Baike] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA. [Minnis, Patrick; Khaiyer, Mandana] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Schumacher, Courtney] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. RP Feng, Z (reprint author), Univ N Dakota, Dept Atmospher Sci, 4149 Univ Ave,Box 9006, Grand Forks, ND 58202 USA. EM dong@aero.und.edu RI Minnis, Patrick/G-1902-2010; Schumacher, Courtney/B-8968-2011; Feng, Zhe/D-9531-2013; Feng, Zhe/E-1877-2015 OI Minnis, Patrick/0000-0002-4733-6148; Dong, Xiquan/0000-0002-3359-6117; Schumacher, Courtney/0000-0003-3612-485X; Feng, Zhe/0000-0002-7540-9017 FU NASA Energy and Water Cycle Study (NEWS) [NNX07AW05G]; NASA [NNX10AI05G]; DOE Office of Science, Office of Biological and Environmental Research [DE-AI02-07ER64546] FX We would like to thank Ed Zipser, Bing Lin, and an anonymous reviewer for their constructive comments and suggestions in improving the manuscript. Carrie Langston at the National Severe Storm Laboratory provided invaluable help in the NEXRAD NMQ data product. This research was primarily supported by NASA Energy and Water Cycle Study (NEWS) project managed by Jared Entin. The University of North Dakota authors were supported by NEWS project under Grant NNX07AW05G, and supported by NASA CERES project under grant NNX10AI05G. The satellite analyses were also supported by DOE Office of Science, Office of Biological and Environmental Research, through contract DE-AI02-07ER64546. NR 64 TC 22 Z9 22 U1 4 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 6 PY 2011 VL 116 AR D23202 DI 10.1029/2011JD016451 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 861CU UT WOS:000297997400002 ER PT J AU Favata, M AF Favata, Marc TI The gravitational-wave memory from eccentric binaries SO PHYSICAL REVIEW D LA English DT Article ID BLACK-HOLE COLLISIONS; CORE-COLLAPSE SUPERNOVAE; POST-NEWTONIAN MOTION; ZERO-FREQUENCY-LIMIT; COMPACT BINARIES; POINT-MASSES; SPECTRAL-ANALYSIS; RADIATION; SYSTEMS; ORBITS AB The nonlinear gravitational-wave memory causes a time-varying but nonoscillatory correction to the gravitational-wave polarizations. It arises from gravitational-waves that are sourced by gravitational-waves. Previous considerations of the nonlinear memory effect have focused on quasicircular binaries. Here I consider the nonlinear memory from Newtonian orbits with arbitrary eccentricity. Expressions for the waveform polarizations and spin-weighted spherical-harmonic modes are derived for elliptic, hyperbolic, parabolic, and radial orbits. In the hyperbolic, parabolic, and radial cases the nonlinear memory provides a 2.5 post-Newtonian (PN) correction to the leading-order waveforms. This is in contrast to the elliptical and quasicircular cases, where the nonlinear memory corrects the waveform at leading (0PN) order. This difference in PN order arises from the fact that the memory builds up over a short "scattering" time scale in the hyperbolic case, as opposed to a much longer radiation-reaction time scale in the elliptical case. The nonlinear memory corrections presented here complete our knowledge of the leading-order (Peters-Mathews) waveforms for elliptical orbits. These calculations are also relevant for binaries with quasicircular orbits in the present epoch which had, in the past, large eccentricities. Because the nonlinear memory depends sensitively on the past evolution of a binary, I discuss the effect of this early-time eccentricity on the value of the late-time memory in nearly circularized binaries. I also discuss the observability of large "memory jumps" in a binary's past that could arise from its formation in a capture process. Lastly, I provide estimates of the signal-to-noise ratio of the linear and nonlinear memories from hyperbolic and parabolic binaries. C1 [Favata, Marc] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Favata, Marc] CALTECH, Pasadena, CA 91125 USA. RP Favata, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM favata@tapir.caltech.edu FU NASA; National Science Foundation [PHY05-51164] FX This research was supported through an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. Early phases of this work were also supported by the National Science Foundation under Grant No. PHY05-51164 to the Kavli Institute for Theoretical Physics. I am grateful to Yanbei Chen for useful discussions and to K. G. Arun, Curt Cutler, Xinyi Guo, and Bala Iyer for their helpful comments on this manuscript. NR 97 TC 6 Z9 6 U1 1 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 DEC 6 PY 2011 VL 84 IS 12 AR 124013 DI 10.1103/PhysRevD.84.124013 PG 24 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 858IU UT WOS:000297790900002 ER PT J AU Melin, F Zibordi, G Berthon, JF Bailey, S Franz, B Voss, K Flora, S Grant, M AF Melin, Frederic Zibordi, Giuseppe Berthon, Jean-Francois Bailey, Sean Franz, Bryan Voss, Kenneth Flora, Stephanie Grant, Mike TI Assessment of MERIS reflectance data as processed with SeaDAS over the European seas SO OPTICS EXPRESS LA English DT Article ID WATER-LEAVING RADIANCES; OCEAN-COLOR PRODUCTS; INHERENT OPTICAL-PROPERTIES; ATMOSPHERIC CORRECTION; VICARIOUS CALIBRATION; COASTAL SITE; SEAWIFS DATA; AERONET-OC; VALIDATION; MODIS AB The uncertainties associated with MERIS remote sensing reflectance (R-RS) data derived from the SeaWiFS Data Analysis System (SeaDAS) are assessed with field observations. In agreement with the strategy applied for other sensors, a vicarious calibration is conducted using in situ data from the Marine Optical BuoY offshore Hawaii, and leads to vicarious adjustment factors departing from 1 by 0.2% to 1.6%. The three field data sets used for validation have been collected at fixed stations in the northern Adriatic Sea and the Baltic Sea, and in a variety of European waters in the Baltic, Black, Mediterranean and North Seas. Excluding Baltic waters, the mean absolute relative difference vertical bar psi vertical bar between satellite and field data is 10-14% for the spectral interval 490-560 nm, 16-18% at 443 nm, and 24-26% at 413 nm. In the Baltic Sea, the vertical bar psi vertical bar values are much higher for the blue bands characterized by low R-RS amplitudes, but similar or lower at 560 and 665 nm. For the three validation sets, the root-mean-square differences decrease from approximately 0.0013 sr(-1) at 413 nm to 0.0002 sr(-1) at 665 nm, and are found similar or lower than those obtained for SeaWiFS or MODIS-Aqua. As derived from SeaDAS, the R-RS records associated with these three missions thus provide a multi-mission data stream of consistent accuracy. (C) 2011 Optical Society of America C1 [Melin, Frederic; Zibordi, Giuseppe; Berthon, Jean-Francois] EC Joint Res Ctr, I-21027 Ispra, Italy. [Bailey, Sean] Futuretech Corp, Greenbelt, MD 20771 USA. [Bailey, Sean; Franz, Bryan] NASA, Goddard Space Flight Ctr, Ocean Biol Proc Grp 614 8, Greenbelt, MD 20771 USA. [Voss, Kenneth] Univ Miami, Coral Gables, FL 33124 USA. [Flora, Stephanie] Moss Landing Marine Labs, Moss Landing, CA 95039 USA. [Grant, Mike] Plymouth Marine Lab, Plymouth PL1 3DH, Devon, England. RP Melin, F (reprint author), EC Joint Res Ctr, TP272,Via Fermi 2749, I-21027 Ispra, Italy. EM frederic.melin@jrc.ec.europa.eu RI Franz, Bryan/D-6284-2012; Voss, Kenneth /A-5328-2013; Bailey, Sean/D-3077-2017 OI Franz, Bryan/0000-0003-0293-2082; Voss, Kenneth /0000-0002-7860-5080; Bailey, Sean/0000-0001-8339-9763 FU NOAA FX This work is contributing to the Ocean Colour Climate Change Initiative (OC-CCI) of the European Space Agency. The authors wish to thank the AERONET team members for their continuous effort in supporting AERONET-OC. MOBY is currently supported by NOAA. NR 54 TC 11 Z9 11 U1 1 U2 8 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD DEC 5 PY 2011 VL 19 IS 25 BP 25657 EP 25671 DI 10.1364/OE.19.025657 PG 15 WC Optics SC Optics GA 857FN UT WOS:000297702400083 PM 22273959 ER PT J AU Bandfield, JL Ghent, RR Vasavada, AR Paige, DA Lawrence, SJ Robinson, MS AF Bandfield, Joshua L. Ghent, Rebecca R. Vasavada, Ashwin R. Paige, David A. Lawrence, Samuel J. Robinson, Mark S. TI Lunar surface rock abundance and regolith fines temperatures derived from LRO Diviner Radiometer data SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID THERMAL INFRARED-SPECTRA; WAVELENGTH RADAR; MOON; DEPOSITS AB Surface temperatures derived from thermal infrared measurements provide a means of understanding the physical properties of the lunar surface. The contrasting thermophysical properties between rocks and regolith fines cause multiple temperatures to be present within the field of view of nighttime multispectral data returned from the Lunar Reconnaissance Orbiter (LRO) Diviner Radiometer between 60 degrees N/S latitudes. Regolith temperatures are influenced by the presence of rocks in addition to factors such as the thermophysical properties of the regolith fines, latitude and local slopes, and radiative heating from adjacent crater walls. Preliminary comparisons of derived rock concentrations with LRO Camera images show both qualitative and quantitative agreement. Although comparisons of derived rock concentrations with circular polarization ratio radar data sets display general similarities, there are clear differences between the two data sets in the relative magnitude and areal extent of rocky signatures. Several surface units can be distinguished based on their regolith temperature and rock concentration values and distributions including maria and highlands surfaces, rocky impact craters, rilles, and wrinkle ridges, dark mantled deposits, and isolated cold surfaces. Rock concentrations are correlated with crater age and rocks are only preserved on the youngest surfaces or where steep slopes occur and mass wasting prevents mantling with fines. The presence of rocky surfaces excavated by young impacts allows for the estimation of minimum regolith thickness from the size of the impact. The derived rock concentrations confirm the presence of thicker regolith cover in the highlands and in locations of radar-dark haloes. C1 [Bandfield, Joshua L.] Univ Washington, Seattle, WA 98195 USA. [Ghent, Rebecca R.] Univ Toronto, Ctr Earth Sci, Dept Geol, Toronto, ON M5S 3B1, Canada. [Lawrence, Samuel J.; Robinson, Mark S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA. [Paige, David A.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Vasavada, Ashwin R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bandfield, JL (reprint author), Univ Washington, Johnson Hall 070,Box 351310, Seattle, WA 98195 USA. EM joshband@u.washington.edu FU spacecraft and Diviner operations teams at Goddard Space Flight Center, Jet Propulsion Laboratory; UCLA; NASA [NNX08AT73G] FX We would like to thank the spacecraft and Diviner operations teams at Goddard Space Flight Center, Jet Propulsion Laboratory, and UCLA for their support. Comments from Sylvain Piqueux and an anonymous reviewer were quite constructive and we hope that the manuscript has been significantly improved as a result of our efforts to address them. Support to J.L.B. for this work was provided by NASA grant NNX08AT73G under the Lunar Reconnaissance Orbiter Participating Scientist Program. NR 35 TC 47 Z9 51 U1 0 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 3 PY 2011 VL 116 AR E00H02 DI 10.1029/2011JE003866 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 856OO UT WOS:000297652600001 ER PT J AU Small, JD Jiang, JH Su, H Zhai, CX AF Small, Jennifer D. Jiang, Jonathan H. Su, Hui Zhai, Chengxing TI Relationship between aerosol and cloud fraction over Australia SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CONVECTIVE CLOUDS; SMOKE; INVIGORATION; AMAZON; LAND; RETRIEVAL; OCEAN; COVER AB We study the relationships between aerosols, clouds, and large scale dynamics over a north coastal Australia (NCA) region and a southeast Australia (SEA) region during the period 2002-2009 to evaluate the applicability of the aerosol microphysics-radiation-effect (MRE) theory proposed by Koren et al. (2008) in a low aerosol environment. We use aerosol optical depth (tau(a)), fire counts, and cloud fraction (f(c)) from Aqua-MODIS, and NCEP Reanalysis vertical velocities at 500 mb (w(500)) as a proxy for dynamic regime. In the NCA we find a monotonic increase fc (35%, absolute fc) as a function of increasing tau(a). In the SEA, we find that fc initially increases by 25% with increasing tau(a), followed by a slow systematic decrease (similar to 18%) with higher tau(a). We show that the MRE theory proposed by Koren et al. (2008) adequately represents the variation of fc with tau(a) in both the NCA and SEA. By conditionally sorting data by w(500) we investigate the role dynamics plays in controlling the tau(a)-fc relationship and the rate at which fc changes with tau(a). We find that the MRE theory can be used to empirically fit both -w(500) and +w(500) observations. By analyzing meteorological parameters from the NCEP Reanalysis, we find that variations in local meteorology are not likely the cause of the observed relationships of tau(a) and fc during biomass burning seasons. However, additional factors such as aerosol type and cloud type may play a role. Citation: Small, J. D., J. H. Jiang, H. Su, and C. Zhai (2011), Relationship between aerosol and cloud fraction over Australia, Geophys. Res. Lett., 38, L23802, doi: 10.1029/2011GL049404. C1 [Small, Jennifer D.; Jiang, Jonathan H.; Su, Hui; Zhai, Chengxing] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Small, JD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jennifer.d.small@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology, under NASA; NASA; Aura project FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We thank the support by NASA Atmospheric Composition Modeling Analysis Program (ACMAP) and the Aura project. NR 25 TC 11 Z9 11 U1 0 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 2 PY 2011 VL 38 AR L23802 DI 10.1029/2011GL049404 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 856JD UT WOS:000297635200002 ER PT J AU Hosokawa, T Omukai, K Yoshida, N Yorke, HW AF Hosokawa, Takashi Omukai, Kazuyuki Yoshida, Naoki Yorke, Harold W. TI Protostellar Feedback Halts the Growth of the First Stars in the Universe SO SCIENCE LA English DT Article ID INITIAL MASS FUNCTION; POPULATION-III; PRIMORDIAL PROTOSTARS; CDM UNIVERSE; STELLAR; ACCRETION; EVOLUTION; DISKS; NUCLEOSYNTHESIS AB The first stars fundamentally transformed the early universe by emitting the first light and by producing the first heavy elements. These effects were predetermined by the mass distribution of the first stars, which is thought to have been fixed by a complex interplay of gas accretion and protostellar radiation. We performed radiation-hydrodynamics simulations that followed the growth of a primordial protostar through to the early stages as a star with thermonuclear burning. The circumstellar accretion disk was evaporated by ultraviolet radiation from the star when its mass was 43 times that of the Sun. Such massive primordial stars, in contrast to the often-postulated extremely massive stars, may help explain the fact that there are no signatures of the pair-instability supernovae in abundance patterns of metal-poor stars in our galaxy. C1 [Hosokawa, Takashi; Yorke, Harold W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hosokawa, Takashi; Omukai, Kazuyuki] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan. [Yoshida, Naoki] Univ Tokyo, Todai Inst Adv Study, Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan. RP Hosokawa, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM hosokwtk@gmail.com FU Japan Society for the Promotion of Science for Research Abroad; Ministry of Education, Science and Culture of Japan [19047004, 2168407, 21244021, 20674003]; NASA FX We thank T. Nakamura, K. Nomoto, S. Inutsuka, and N. Turner for stimulating discussions on this topic. Comments by an anonymous referee helped improve the manuscript. T. H. appreciates the support by Fellowship of the Japan Society for the Promotion of Science for Research Abroad. The present work is supported in part by the grants-in-aid by the Ministry of Education, Science and Culture of Japan (19047004, 2168407, 21244021:KO, 20674003:NY). Portions of this research were conducted at the Jet Propulsion Laboratory, California Institute of Technology, which is supported by NASA. Data analysis was (in part) carried out on the general-purpose PC farm at Center for Computational Astrophysics (CfCA) of National Astronomical Observatory of Japan. NR 27 TC 197 Z9 198 U1 0 U2 7 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD DEC 2 PY 2011 VL 334 IS 6060 BP 1250 EP 1253 DI 10.1126/science.1207433 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 855HD UT WOS:000297553600043 PM 22075723 ER PT J AU Ramsey, E Rangoonwala, A Suzuoki, Y Jones, CE AF Ramsey, Elijah, III Rangoonwala, Amina Suzuoki, Yukihiro Jones, Cathleen E. TI Oil Detection in a Coastal Marsh with Polarimetric Synthetic Aperture Radar (SAR) SO REMOTE SENSING LA English DT Article DE Gulf of Mexico; Deepwater Horizon oil spill; PolSAR and multi-polarization radar data; decomposition classification; coastal marsh; polarimetric signature analysis ID UNSUPERVISED CLASSIFICATION; DECOMPOSITION; POLLUTION AB The National Aeronautics and Space Administration's airborne Uninhabited Aerial Vehicle Synthetic Aperture Radar (UAVSAR) was deployed in June 2010 in response to the Deepwater Horizon oil spill in the Gulf of Mexico. UAVSAR is a fully polarimetric L-band Synthetic Aperture Radar (SAR) sensor for obtaining data at high spatial resolutions. Starting a month prior to the UAVSAR collections, visual observations confirmed oil impacts along shorelines within northeastern Barataria Bay waters in eastern coastal Louisiana. UAVSAR data along several flight lines over Barataria Bay were collected on 23 June 2010, including the repeat flight line for which data were collected in June 2009. Our analysis of calibrated single-look complex data for these flight lines shows that structural damage of shoreline marsh accompanied by oil occurrence manifested as anomalous features not evident in pre-spill data. Freeman-Durden (FD) and Cloude-Pottier (CP) decompositions of the polarimetric data and Wishart classifications seeded with the FD and CP classes also highlighted these nearshore features as a change in dominant scattering mechanism. All decompositions and classifications also identify a class of interior marshes that reproduce the spatially extensive changes in backscatter indicated by the pre- and post-spill comparison of multi-polarization radar backscatter data. FD and CP decompositions reveal that those changes indicate a transform of dominant scatter from primarily surface or volumetric to double or even bounce. Given supportive evidence that oil-polluted waters penetrated into the interior marshes, it is reasonable that these backscatter changes correspond with oil exposure; however, multiple factors prevent unambiguous determination of whether UAVSAR detected oil in interior marshes. C1 [Ramsey, Elijah, III] US Geol Survey, Natl Wetlands Res Ctr, Lafayette, LA USA. [Rangoonwala, Amina] IAP World Serv Inc, Cape Canaveral, FL 32920 USA. [Suzuoki, Yukihiro] ASci Corp Inc, Mclean, VA 22101 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 USA. EM ramseye@usgs.gov; rangoonwalaa@usgs.gov; yukihirosuzuoki@gmail.com; cathleen.e.jones@jpl.nasa.gov NR 32 TC 25 Z9 25 U1 1 U2 32 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD DEC PY 2011 VL 3 IS 12 BP 2630 EP 2662 DI 10.3390/rs3122630 PG 33 WC Remote Sensing SC Remote Sensing GA 978PD UT WOS:000306755300005 ER PT J AU Breinnger, DR Bolt, MR Legare, ML Drese, JH Stolen, ED AF Breinnger, David R. Bolt, M. Rebecca Legare, Michael L. Drese, John H. Stolen, Eric D. TI Factors Influencing Home-Range Sizes of Eastern Indigo Snakes in Central Florida SO JOURNAL OF HERPETOLOGY LA English DT Article ID SPATIAL ECOLOGY; DRYMARCHON-COUPERI; HOPLOCEPHALUS-BUNGAROIDES; HABITAT SPECIFICITY; POPULATION-DYNAMICS; ROAD MORTALITY; CONSERVATION; MOVEMENTS; LANDSCAPES; GEORGIA AB Wide-ranging snake species are particularly sensitive to landscape fragmentation, and understanding area requirements is important for their conservation. We used radiotelemetry to quantify how Eastern Indigo Snake home-range sizes were influenced by sex, land cover, and the length of time (weeks) individuals were radio tracked. We found that Eastern Indigo Snakes had the largest home ranges among other snake species studied. Female home ranges averaged 44 and 76 ha, respectively, for kernel and minimum convex polygon estimators. Male home ranges averaged 156 and 202 ha, respectively, for kernel and minimum convex polygon estimators. Many animal species respond to habitat fragmentation by using larger areas than in unfragmented landscapes, but we found that Indigo Snakes in fragmented landscapes used much smaller areas. The length of time that snakes were tracked had almost no influence on home-range size compared to sex and land cover type. Our results suggest that maintaining populations of this large wide-ranging predator will require large conservation areas with minimum fragmentation. C1 [Breinnger, David R.; Bolt, M. Rebecca; Drese, John H.; Stolen, Eric D.] NASA, Ecol Programs, Kennedy Space Ctr, FL 32899 USA. [Legare, Michael L.] US Fish & Wildlife Serv, Merritt Isl Natl Wildlife Refuge, Titusville, FL 32782 USA. RP Breinnger, DR (reprint author), NASA, Ecol Programs, Mail Code IHA-300, Kennedy Space Ctr, FL 32899 USA. EM david.r.breininger@nasa.gov FU The Bailey Wildlife Foundation; National Aeronautics and Space Administration; U.S. Fish and Wildlife Service FX The Bailey Wildlife Foundation, National Aeronautics and Space Administration, and U.S. Fish and Wildlife Service funded this study. We thank G. Bailey, M. Bailey, J. Berish, P. Burger, M. Burgman, K. Gorman, C. Hall, R. Koester, L. LaClaire, P. Moler, R. Seigel, S. Brisbin, and B. Summerfield. We also thank about 60 natural resource professionals who helped us capture Indigo Snakes for radio tracking studies. NR 67 TC 8 Z9 9 U1 4 U2 40 PU SOC STUDY AMPHIBIANS REPTILES PI ST LOUIS PA C/O ROBERT D ALDRIDGE, ST LOUIS UNIV, DEPT BIOLOGY, 3507 LACLEDE, ST LOUIS, MO 63103 USA SN 0022-1511 EI 1937-2418 J9 J HERPETOL JI J. Herpetol. PD DEC PY 2011 VL 45 IS 4 BP 484 EP 490 PG 7 WC Zoology SC Zoology GA 966YS UT WOS:000305873900016 ER PT J AU Callaghan, TV Johansson, M Brown, RD Groisman, PY Labba, N Radionov, V Barry, RG Bulygina, ON Essery, RLH Frolov, DM Golubev, VN Grenfell, TC Petrushina, MN Razuvaev, VN Robinson, DA Romanov, P Shindell, D Shmakin, AB Sokratov, SA Warren, S Yang, DQ AF Callaghan, Terry V. Johansson, Margareta Brown, Ross D. Groisman, Pavel Ya Labba, Niklas Radionov, Vladimir Barry, Roger G. Bulygina, Olga N. Essery, Richard L. H. Frolov, D. M. Golubev, Vladimir N. Grenfell, Thomas C. Petrushina, Marina N. Razuvaev, Vyacheslav N. Robinson, David A. Romanov, Peter Shindell, Drew Shmakin, Andrey B. Sokratov, Sergey A. Warren, Stephen Yang, Daquing TI The Changing Face of Arctic Snow Cover: A Synthesis of Observed and Projected Changes SO AMBIO LA English DT Article DE Snow depth; Snow water equivalent; Snow cover duration; Snow cover extent ID CLIMATE-CHANGE; NORTHERN EURASIA; DENSITY-DEPENDENCE; SVALBARD REINDEER; POPULATION; SIMULATION; PRECIPITATION; TEMPERATURE; HEMISPHERE; DYNAMICS AB Analysis of in situ and satellite data shows evidence of different regional snow cover responses to the widespread warming and increasing winter precipitation that has characterized the Arctic climate for the past 40-50 years. The largest and most rapid decreases in snow water equivalent (SWE) and snow cover duration (SCD) are observed over maritime regions of the Arctic with the highest precipitation amounts. There is also evidence of marked differences in the response of snow cover between the North American and Eurasian sectors of the Arctic, with the North American sector exhibiting decreases in snow cover and snow depth over the entire period of available in situ observations from around 1950, while widespread decreases in snow cover are not apparent over Eurasia until after around 1980. However, snow depths are increasing in many regions of Eurasia. Warming and more frequent winter thaws are contributing to changes in snow pack structure with important implications for land use and provision of ecosystem services. Projected changes in snow cover from Global Climate Models for the 2050 period indicate increases in maximum SWE of up to 15% over much of the Arctic, with the largest increases (15-30%) over the Siberian sector. In contrast, SCD is projected to decrease by about 10-20% over much of the Arctic, with the smallest decreases over Siberia (<10%) and the largest decreases over Alaska and northern Scandinavia (30-40%) by 2050. These projected changes will have far-reaching consequences for the climate system, human activities, hydrology, and ecology. C1 [Callaghan, Terry V.] Royal Swedish Acad Sci, S-10405 Stockholm, Sweden. [Johansson, Margareta] Lund Univ, Dept Earth & Ecosyst Sci, Div Phys Geog & Ecosyst Anal, S-22362 Lund, Sweden. [Brown, Ross D.] Environm Canada, Div Climate Res, Ouranos Climate Consortium, Montreal, PQ H3A 1B9, Canada. [Groisman, Pavel Ya] NOAA, NESDIS Natl Climat Data Ctr, Asheville, NC 28801 USA. [Labba, Niklas] Gaisi Sami Ctr, N-9042 Lakselvbukt, Laksvatn, Norway. [Radionov, Vladimir] AARI, St Petersburg 199397, Russia. [Barry, Roger G.] Univ Colorado, NSIDC, CIRES, Boulder, CO 80309 USA. [Bulygina, Olga N.] All Russian Res Inst Hydrometeorol Informat, World Data Ctr RIHMI WDC, Climatol Dept, Obninsk 249035, Kaluga Region, Russia. [Essery, Richard L. H.] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland. [Frolov, D. M.; Golubev, Vladimir N.] Moscow MV Lomonosov State Univ, Fac Geog, Lab Snow Avalanches & Mudflows, Moscow 119991, Russia. [Grenfell, Thomas C.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Petrushina, Marina N.] Moscow MV Lomonosov State Univ, Dept Phys Geog & Landscapes, Fac Geog, Moscow 119991, Russia. [Razuvaev, Vyacheslav N.] RIHMI WDC, Obninsk 249035, Kaluga Region, Russia. [Robinson, David A.] Rutgers State Univ, Dept Geog, Piscataway, NJ 08854 USA. [Romanov, Peter] NOAA, NESDIS, Camp Springs, MD 20746 USA. [Shindell, Drew] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Shmakin, Andrey B.] Inst Geog, Moscow 119017, Russia. [Sokratov, Sergey A.] Moscow MV Lomonosov State Univ, Fac Geog, Nat Risks Assessment Lab, Moscow 119991, Russia. [Warren, Stephen] Univ Washington, Dept Atmospher Sci & Earth & Space Sci, Seattle, WA 98195 USA. [Yang, Daquing] Univ Alaska Fairbanks, Water & Environm Res Ctr, Fairbanks, AK USA. RP Callaghan, TV (reprint author), Royal Swedish Acad Sci, S-10405 Stockholm, Sweden. EM terry_callaghan@btinternet.com; margareta.johansson@nateko.lu.se; ross.brown@ec.gc.ca; Pasha.Groisman@noaa.gov; n.labba@gmail.com; vradion@aari.ru; rbarry@nsidc.org; bulygina@meteo.ru; ressery@staffmail.ed.ac.uk; denisfrolovm@mail.ru; golubev@geol.msu.ru; tcg@atmos.washington.edu; mnpetrushina@mail.ru; razuvaev@meteo.ru; david.robinson@rutgers.edu; Peter.Romanov@noaa.gov; drew.t.shindell@nasa.gov; ashmakin@igras.ru; sokratov@nral.org; sgw@uw.edu; dyang3@alaska.edu RI Callaghan, Terens/N-7640-2014; Golubev, Vladimir/K-1678-2012; Petrushina, Marina/K-2103-2012; Romanov, Peter/F-5622-2010; Sokratov, Sergey/A-6602-2011; Frolov, Denis/O-2426-2013; Bulygina, Olga/H-1251-2016 OI Barry, Roger/0000-0001-9239-0859; Essery, Richard/0000-0003-1756-9095; Romanov, Peter/0000-0002-2153-8307; Sokratov, Sergey/0000-0001-9265-2935; FU Swedish Environmental Protection Agency [08/210]; Swedish Research Council FORMAS [204-2009-45] FX We wish to thank the various national funding agencies that made this review possible, specifically the Swedish Environmental Protection Agency (grant number 08/210) and the Swedish Research Council FORMAS (grant number 204-2009-45) who helped to directly support this publication. We also gratefully acknowledge the Arctic Monitoring and Assessment Program Secretariat and the SWIPA Integration Team in helping to produce the original SWIPA report and the various contributing SWIPA chapter authors including all contributing authors for the SWIPA snow chapter. Finally, we thank reviewers of the SWIPA snow chapter, particularly Barry Goodison. NR 70 TC 70 Z9 72 U1 14 U2 105 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0044-7447 EI 1654-7209 J9 AMBIO JI Ambio PD DEC PY 2011 VL 40 SU 1 BP 17 EP 31 DI 10.1007/s13280-011-0212-y PG 15 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 959BM UT WOS:000305284800004 ER PT J AU Chamis, CC AF Chamis, Christos C. TI Assuring life in composite systems SO SCIENCE AND ENGINEERING OF COMPOSITE MATERIALS LA English DT Article DE dynamic buckling; finite elements; integrated modules; smart material; uncertainties effects AB A computational simulation method is presented to assure life in composite systems by using dynamic buckling of smart composite shells as an example. The combined use of composite mechanics, finite element computer codes, and probabilistic analysis enable the effective assessment of the dynamic buckling load of smart composite shells. A universal plot is generated to estimate the dynamic buckling load of composite shells at various load rates and probabilities. The shell structure is also evaluated with smart fibers embedded in the plies right below the outer plies. The results show that, on the average, the use of smart fibers improved the shell buckling resistance by about 10% at different probabilities and delayed the buckling occurrence time. The probabilistic sensitivities results indicate that uncertainties in the fiber volume ratio and ply thickness have major effects on the buckling load. The uncertainties in the electric field strength and smart material volume fraction have moderate effects and thereby in the assured life of the shell. C1 NASA, Res & Technol Directorate, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Chamis, CC (reprint author), NASA, Res & Technol Directorate, Glenn Res Ctr, Cleveland, OH 44135 USA. EM Christos.C.Chamis@nasa.gov NR 8 TC 0 Z9 0 U1 0 U2 0 PU WALTER DE GRUYTER & CO PI BERLIN PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY SN 0334-181X J9 SCI ENG COMPOS MATER JI Sci. Eng. Compos. Mater. PD DEC PY 2011 VL 18 IS 4 SI SI BP 231 EP 240 DI 10.1515/SECM.2011.046 PG 10 WC Materials Science, Composites SC Materials Science GA 942QM UT WOS:000304061900005 ER PT J AU Sweetser, TH Broschart, SB Angelopoulos, V Whiffen, GJ Folta, DC Chung, MK Hatch, SJ Woodard, MA AF Sweetser, Theodore H. Broschart, Stephen B. Angelopoulos, Vassilis Whiffen, Gregory J. Folta, David C. Chung, Min-Kun Hatch, Sara J. Woodard, Mark A. TI ARTEMIS Mission Design SO SPACE SCIENCE REVIEWS LA English DT Review DE ARTEMIS; THEMIS; Low-energy transfer; Lissajous orbits; Lunar science; Lunar mission; Heliophysics; Magnetosphere ID STATION-KEEPING STRATEGIES; LIBRATION POINT ORBITS; PERIODIC-ORBITS AB The ARTEMIS mission takes two of the five THEMIS spacecraft beyond their prime mission objectives and reuses them to study the Moon and the lunar space environment. Although the spacecraft and fuel resources were tailored to space observations from Earth orbit, sufficient fuel margins, spacecraft capability, and operational flexibility were present that with a circuitous, ballistic, constrained-thrust trajectory, new scientific information could be gleaned from the instruments near the Moon and in lunar orbit. We discuss the challenges of ARTEMIS trajectory design and describe its current implementation to address both heliophysics and planetary science objectives. In particular, we explain the challenges imposed by the constraints of the orbiting hardware and describe the trajectory solutions found in prolonged ballistic flight paths that include multiple lunar approaches, lunar flybys, low-energy trajectory segments, lunar Lissajous orbits, and low-lunar-periapse orbits. We conclude with a discussion of the risks that we took to enable the development and implementation of ARTEMIS. C1 [Sweetser, Theodore H.; Broschart, Stephen B.; Angelopoulos, Vassilis; Whiffen, Gregory J.; Chung, Min-Kun; Hatch, Sara J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Folta, David C.; Woodard, Mark A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sweetser, TH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-121, Pasadena, CA 91109 USA. EM Ted.Sweetser@jpl.nasa.gov FU National Aeronautics and Space Administration FX The work described in this paper was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 25 TC 23 Z9 23 U1 0 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD DEC PY 2011 VL 165 IS 1-4 BP 27 EP 57 DI 10.1007/s11214-012-9869-1 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 929ZE UT WOS:000303103700003 ER PT J AU Sibeck, DG Angelopoulos, V Brain, DA Delory, GT Eastwood, JP Farrell, WM Grimm, RE Halekas, JS Hasegawa, H Hellinger, P Khurana, KK Lillis, RJ Oieroset, M Phan, TD Raeder, J Russell, CT Schriver, D Slavin, JA Travnicek, PM Weygand, JM AF Sibeck, D. G. Angelopoulos, V. Brain, D. A. Delory, G. T. Eastwood, J. P. Farrell, W. M. Grimm, R. E. Halekas, J. S. Hasegawa, H. Hellinger, P. Khurana, K. K. Lillis, R. J. Oieroset, M. Phan, T. -D. Raeder, J. Russell, C. T. Schriver, D. Slavin, J. A. Travnicek, P. M. Weygand, J. M. TI ARTEMIS Science Objectives SO SPACE SCIENCE REVIEWS LA English DT Review DE ARTEMIS; Moon; Reconnection; Particle acceleration; Turbulence; Wake; Lunar surface; Lunar core; Dust; Electric fields; Crustal anomalies ID INTERPLANETARY MAGNETIC-FIELD; EARTHS BOW SHOCK; KELVIN-HELMHOLTZ INSTABILITY; SOLAR-WIND INTERACTION; LUNAR PLASMA WAKE; 3-DIMENSIONAL MHD SIMULATIONS; PROSPECTOR MAGNETOMETER DATA; DISTANT GEOMAGNETIC TAIL; FLUX-TRANSFER EVENTS; IN-CELL SIMULATIONS AB NASA's two spacecraft ARTEMIS mission will address both heliospheric and planetary research questions, first while in orbit about the Earth with the Moon and subsequently while in orbit about the Moon. Heliospheric topics include the structure of the Earth's magnetotail; reconnection, particle acceleration, and turbulence in the Earth's magnetosphere, at the bow shock, and in the solar wind; and the formation and structure of the lunar wake. Planetary topics include the lunar exosphere and its relationship to the composition of the lunar surface, the effects of electric fields on dust in the exosphere, internal structure of the Moon, and the lunar crustal magnetic field. This paper describes the expected contributions of ARTEMIS to these baseline scientific objectives. C1 [Sibeck, D. G.; Farrell, W. M.; Slavin, J. A.] NASA, GSFC, Greenbelt, MD 20771 USA. [Angelopoulos, V.] Univ Calif Los Angeles, IGPP, Los Angeles, CA 90095 USA. [Brain, D. A.; Delory, G. T.; Halekas, J. S.; Lillis, R. J.; Oieroset, M.; Phan, T. -D.] UCB, Berkeley, CA USA. [Eastwood, J. P.] Univ London Imperial Coll Sci Technol & Med, London, England. [Grimm, R. E.] SWRI, Boulder, CO USA. [Hasegawa, H.] ISAS, Sagamihara, Kanagawa, Japan. [Hellinger, P.; Travnicek, P. M.] Astron Inst, Prague, Czech Republic. [Raeder, J.] UNH, Durham, NH USA. RP Sibeck, DG (reprint author), NASA, GSFC, Code 674, Greenbelt, MD 20771 USA. EM david.g.sibeck@nasa.gov RI Hasegawa, Hiroshi/A-1192-2007; Sibeck, David/D-4424-2012; Slavin, James/H-3170-2012; Russell, Christopher/E-7745-2012; Farrell, William/I-4865-2013; Hellinger, Petr/F-5267-2014; Travnicek, Pavel/G-8608-2014; Lillis, Robert/A-3281-2008; OI Hasegawa, Hiroshi/0000-0002-1172-021X; Halekas, Jasper/0000-0001-5258-6128; Slavin, James/0000-0002-9206-724X; Russell, Christopher/0000-0003-1639-8298; Hellinger, Petr/0000-0002-5608-0834; Lillis, Robert/0000-0003-0578-517X; Grimm, Robert/0000-0002-7588-1194 FU NASA [NAS5-02099]; THEMIS MODA; STFC at Imperial College FX Work at UCB and UCLA was supported by NASA Contract NAS5-02099. Work at NASA/GSFC was supported by THEMIS MO&DA. J.P.E. is supported by an STFC Advanced Fellowship at Imperial College. NR 224 TC 30 Z9 30 U1 1 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD DEC PY 2011 VL 165 IS 1-4 BP 59 EP 91 DI 10.1007/s11214-011-9777-9 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 929ZE UT WOS:000303103700004 ER PT J AU Halekas, JS Angelopoulos, V Sibeck, DG Khurana, KK Russell, CT Delory, GT Farrell, WM McFadden, JP Bonnell, JW Larson, D Ergun, RE Plaschke, F Glassmeier, KH AF Halekas, J. S. Angelopoulos, V. Sibeck, D. G. Khurana, K. K. Russell, C. T. Delory, G. T. Farrell, W. M. McFadden, J. P. Bonnell, J. W. Larson, D. Ergun, R. E. Plaschke, F. Glassmeier, K. H. TI First Results from ARTEMIS, a New Two-Spacecraft Lunar Mission: Counter-Streaming Plasma Populations in the Lunar Wake SO SPACE SCIENCE REVIEWS LA English DT Review DE Moon; Lunar wake; Counter-streaming distributions ID IN-CELL SIMULATIONS; UPSTREAM ULF WAVES; SOLAR-WIND; MAGNETIC-FIELDS; MOON; EXPANSION; THEMIS; ELECTRONS; VACUUM; MAGNETOMETER AB We present observations from the first passage through the lunar plasma wake by one of two spacecraft comprising ARTEMIS (Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon's Interaction with the Sun), a new lunar mission that re-tasks two of five probes from the THEMIS magnetospheric mission. On Feb 13, 2010, ARTEMIS probe P1 passed through the wake at similar to 3.5 lunar radii downstream from the Moon, in a region between those explored by Wind and the Lunar Prospector, Kaguya, Chandrayaan, and Chang'E missions. ARTEMIS observed interpenetrating proton, alpha particle, and electron populations refilling the wake along magnetic field lines from both flanks. The characteristics of these distributions match expectations from self-similar models of plasma expansion into vacuum, with an asymmetric character likely driven by a combination of a tilted interplanetary magnetic field and an anisotropic incident solar wind electron population. On this flyby, ARTEMIS provided unprecedented measurements of the interpenetrating beams of both electrons and ions naturally produced by the filtration and acceleration effects of electric fields set up during the refilling process. ARTEMIS also measured electrostatic oscillations closely correlated with counter-streaming electron beams in the wake, as previously hypothesized but never before directly measured. These observations demonstrate the capability of the comprehensively instrumented ARTEMIS spacecraft and the potential for new lunar science from this unique two spacecraft constellation. C1 [Halekas, J. S.; Delory, G. T.; McFadden, J. P.; Bonnell, J. W.; Larson, D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Halekas, J. S.; Delory, G. T.; Farrell, W. M.] NASA, Ames Res Ctr, NASAs Lunar Sci Inst, Moffett Field, CA 94035 USA. [Angelopoulos, V.; Khurana, K. K.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Sibeck, D. G.; Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ergun, R. E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. [Plaschke, F.; Glassmeier, K. H.] Inst Geophys & Extraterr Phys, Braunschweig, Germany. RP Halekas, JS (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM jazzman@ssl.berkeley.edu RI Sibeck, David/D-4424-2012; Russell, Christopher/E-7745-2012; Farrell, William/I-4865-2013; OI Russell, Christopher/0000-0003-1639-8298; Halekas, Jasper/0000-0001-5258-6128 FU NASA's Lunar Science Institute; German Ministerium fur Wirtschaft und Technologie; Deutsches Zentrum fur Luft- und Raumfahrt [50QP0402] FX We wish to acknowledge the extraordinary team of scientists and engineers that made the THEMIS/ARTEMIS missions a reality. We thank R. Lepping, K. Ogilvie, and CDAWEB for providing Wind key parameter data. We also acknowledge NASA's Lunar Science Institute for supporting JSH, WMF, and GTD. FP and KHG acknowledge financial support by the German Ministerium fur Wirtschaft und Technologie and the Deutsches Zentrum fur Luft- und Raumfahrt under grant 50QP0402 is acknowledged. NR 43 TC 22 Z9 22 U1 1 U2 10 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD DEC PY 2011 VL 165 IS 1-4 BP 93 EP 107 DI 10.1007/s11214-010-9738-8 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 929ZE UT WOS:000303103700005 ER PT J AU Simoncini, E Russell, MJ Kleidon, A AF Simoncini, E. Russell, M. J. Kleidon, A. TI Modeling Free Energy Availability from Hadean Hydrothermal Systems to the First Metabolism SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Article DE Hydrothermal systems; Free energy generation; Thermodynamics; Disequilibrium; Metabolism; Emergence of Life AB Off-axis Hydrothermal Systems (HSs) are seen as the possible setting for the emergence of life. As the availability of free energy is a general requirement to drive any form of metabolism, we ask here under which conditions free energy generation by geologic processes is greatest and relate these to the conditions found at off-axis HSs. To do so, we present a conceptual model in which we explicitly capture the energetics of fluid motion and its interaction with exothermic reactions to maintain a state of chemical disequilibrium. Central to the interaction is the temperature at which the exothermic reactions take place. This temperature not only sets the equilibrium constant of the chemical reactions and thereby the distance of the actual state to chemical equilibrium, but these reactions also shape the temperature gradient that drives convection and thereby the advection of reactants to the reaction sites and the removal of the products that relate to geochemical free energy generation. What this conceptual model shows is that the positive feedback between convection and the chemical kinetics that is found at HSs favors a greater rate of free energy generation than in the absence of convection. Because of the lower temperatures and because the temperature of reactions is determined more strongly by these dynamics rather than an external heat flux, the conditions found at off-axis HSs should result in the greatest rates of geochemical free energy generation. Hence, we hypothesize from these thermodynamic considerations that off-axis HSs seem most conducive for the emergence of protometabolic pathways as these provide the greatest, abiotic generation rates of chemical free energy. C1 [Simoncini, E.; Kleidon, A.] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [Russell, M. J.] CALTECH, JPL, Pasadena, CA 91109 USA. RP Simoncini, E (reprint author), Max Planck Inst Biogeochem, Hans Knoll Str 10, D-07745 Jena, Germany. EM esimon@bgc-jena.mpg.de RI Kleidon, Axel/O-7843-2014 OI Kleidon, Axel/0000-0002-3798-0730 FU Helmholtz Alliance "Planetary Evolution and Life"; National Aeronautics and Space Administration; NASA Astrobiology Institute (NAI - Icy Worlds); US Government FX Authors benefited from discussions at the 1st meeting of the NAI-sponsored Thermodynamics Disequilibrium and Evolution Focus Group. ES and AK acknowledge the Helmholtz Alliance "Planetary Evolution and Life" for funding this research. MJR's contribution was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration with support from the NASA Astrobiology Institute (NAI - Icy Worlds). US Government sponsorship acknowledged. NR 3 TC 7 Z9 8 U1 1 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD DEC PY 2011 VL 41 IS 6 SI SI BP 529 EP 532 DI 10.1007/s11084-011-9251-4 PG 4 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 909UL UT WOS:000301590600005 PM 22139512 ER PT J AU Parker, ET Cleaves, HJ Callahan, MP Dworkin, JP Glavin, DP Lazcano, A Bada, JL AF Parker, Eric T. Cleaves, H. James Callahan, Michael P. Dworkin, Jason P. Glavin, Daniel P. Lazcano, Antonio Bada, Jeffrey L. TI Enhanced Synthesis of Alkyl Amino Acids in Miller's 1958 H2S Experiment SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Article DE Stanley Miller; Spark discharge; Hydrogen sulfide ID SPARK DISCHARGE EXPERIMENT; HYDROXYL RADICALS; HYDROGEN ABSTRACTION; SULFIDE; PEPTIDES AB Stanley Miller's 1958 H2S-containing experiment, which included a simulated prebiotic atmosphere of methane (CH4), ammonia (NH3), carbon dioxide (CO2), and hydrogen sulfide (H2S) produced several alkyl amino acids, including the alpha-, beta-, and gamma-isomers of aminobutyric acid (ABA) in greater relative yields than had previously been reported from his spark discharge experiments. In the presence of H2S, aspartic and glutamic acids could yield alkyl amino acids via the formation of thioimide intermediates. Radical chemistry initiated by passing H2S through a spark discharge could have also enhanced alkyl amino acid synthesis by generating alkyl radicals that can help form the aldehyde and ketone precursors to these amino acids. We propose mechanisms that may have influenced the synthesis of certain amino acids in localized environments rich in H2S and lightning discharges, similar to conditions near volcanic systems on the early Earth, thus contributing to the prebiotic chemical inventory of the primordial Earth. C1 [Parker, Eric T.; Bada, Jeffrey L.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Cleaves, H. James] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Callahan, Michael P.; Dworkin, Jason P.; Glavin, Daniel P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Lazcano, Antonio] Univ Nacl Autonoma Mexico, Fac Ciencias, Mexico City 04510, DF, Mexico. RP Bada, JL (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, 8615 Kennel Way, La Jolla, CA 92093 USA. EM jbada@ucsd.edu RI Callahan, Michael/D-3630-2012; Glavin, Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012; OI Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997; Cleaves, Henderson/0000-0003-4101-0654 FU National Aeronautics and Space Administration (NASA) Astrobiology Institute (NAI); Goddard Center for Astrobiology; NAI; CONACYT Mexico [50520-Q]; DGAPA-UNAM; UC Mexus-CONACYT; NSF [CHE-1004570]; NASA FX We thank Mandeville Special Collections in the UC San Diego Geisel Library for making Miller's original laboratory notebooks accessible. The authors thank the National Aeronautics and Space Administration (NASA) Astrobiology Institute (NAI) and the Goddard Center for Astrobiology for grant support. M.P.C. and H.J.C. acknowledge support from the NAI Postdoctoral Program administered by Oak Ridge Associated Universities. A. L. is grateful for support provided by CONACYT Mexico (Project 50520-Q), and by a DGAPA-UNAM and a UC Mexus-CONACYT Fellowship. We also thank Jamie Elsila and Facundo Fernandez for additional analytical support. J.L.B. and H.J.C. are affiliated with the Center for Chemical Evolution at the Georgia Institute of Technology, supported by the National Science Foundation (NSF) and the NASA Astrobiology Program, under NSF Grant CHE-1004570. NR 16 TC 3 Z9 3 U1 1 U2 21 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD DEC PY 2011 VL 41 IS 6 SI SI BP 569 EP 574 DI 10.1007/s11084-011-9253-2 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 909UL UT WOS:000301590600012 PM 22139514 ER PT J AU Bar-Cohen, Y AF Bar-Cohen, Yoseph TI Biological Senses as Inspiring Model for Biomimetic Sensors SO IEEE SENSORS JOURNAL LA English DT Article DE Biologically inspired sensors; biomimetics; receptors; robotics; senses; sensors ID ELECTRONIC NOSES; RECOGNITION; TONGUES; ARRAY; ODOR AB Organisms are using numerous sensors, known as receptors and/or senses, to control every aspect of their life and functions. These nature's sensors have been improved over millions of years of evolution to make them enormously effective. They provide information that is used to warn against excessive and/or dangerous conditions; sense location in space; assure the control of the size of their bodies and organs and at what point to stop growing; etc. Recognizing the capability of biological sensors, scientists and engineers are making great efforts to mimic them or using them as a model for inspiration. While some successes have been reported and biologically inspired sensors are being used in the control of various systems, biological sensors are still far superior in many ways. This manuscript provides an introductory review of some of the biological sensors and their mimicked functionality version. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bar-Cohen, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM yosi@jpl.nasa.gov FU National Aeronautics and Space Administration (NASA) FX Some of the research reported in this manuscript was conducted at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with National Aeronautics and Space Administration (NASA). NR 58 TC 6 Z9 6 U1 2 U2 19 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1530-437X EI 1558-1748 J9 IEEE SENS J JI IEEE Sens. J. PD DEC PY 2011 VL 11 IS 12 BP 3194 EP 3201 DI 10.1109/JSEN.2011.2167321 PG 8 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Physics, Applied SC Engineering; Instruments & Instrumentation; Physics GA 913LD UT WOS:000301878500001 ER PT J AU Son, KA Yang, BH Prokopuk, N Moon, JS Liao, AN Katona, TM Khan, MA AF Son, Kyung-Ah Yang, Baohua Prokopuk, Nicholas Moon, Jeong S. Liao, Anna Katona, Thomas M. Khan, M. Asif TI RF GaN HEMT Sensors for Detection of Caustic Chemicals SO IEEE SENSORS JOURNAL LA English DT Article DE Chemical; Cl-2; GaN; HCl; HEMT; microsensor; RF; toxic industrial chemical AB For future wireless sensor network applications, highspeed RF GaN HEMTs (high electron mobility transistor) are investigated for toxic industrial chemical detection, for the first time. RF GaN HEMTs with a Pt-based gate metal show reliable, repeatable, and distinctive responses toward Cl gas and HCl vapor at room temperature. C1 [Son, Kyung-Ah; Yang, Baohua; Liao, Anna] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Prokopuk, Nicholas] USN, AirWarfare Ctr, China Lake, CA 93555 USA. [Moon, Jeong S.] HRL Labs, Malibu, CA 90265 USA. [Katona, Thomas M.; Khan, M. Asif] Univ S Carolina, Dept Elect Engn, Columbia, SC 29208 USA. RP Son, KA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM kson@jpl.nasa.gov FU U.S. Defense Threat Reduction Agency through the U.S. Army Research Office (ARO) FX This work was supported in part by the U.S. Defense Threat Reduction Agency through the U.S. Army Research Office (ARO) and monitored by Dr. S. J. Lee and Dr. J. J. Becker of ARO. The associate editor coordinating the review of this paper and approving it for publication was Prof. Evgeny Katz. NR 11 TC 1 Z9 1 U1 1 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1530-437X J9 IEEE SENS J JI IEEE Sens. J. PD DEC PY 2011 VL 11 IS 12 BP 3476 EP 3478 DI 10.1109/JSEN.2011.2160978 PG 3 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Physics, Applied SC Engineering; Instruments & Instrumentation; Physics GA 913LD UT WOS:000301878500040 ER PT J AU Lauenstein, JM Goldsman, N Liu, S Titus, JL Ladbury, RL Kim, HS Phan, AM LaBel, KA Zafrani, M Sherman, P AF Lauenstein, Jean-Marie Goldsman, Neil Liu, Sandra Titus, Jeffrey L. Ladbury, Raymond L. Kim, Hak S. Phan, Anthony M. LaBel, Kenneth A. Zafrani, Max Sherman, Phillip TI Effects of Ion Atomic Number on Single-Event Gate Rupture (SEGR) Susceptibility of Power MOSFETs SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE Heavy ion; power MOSFET; single-event gate rupture (SEGR) AB The relative importance of heavy-ion interaction with the oxide, charge ionized in the epilayer, and charge ionized in the drain substrate, on the bias for SEGR failure in vertical power MOSFETs is experimentally investigated. The results indicate that both the charge ionized in the epilayer and the ion atomic number are important parameters of SEGR failure. Implications on SEGR hardness assurance are discussed. C1 [Lauenstein, Jean-Marie; Ladbury, Raymond L.; LaBel, Kenneth A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Goldsman, Neil] Univ Maryland, Dept Elect Engn, College Pk, MD 20742 USA. [Liu, Sandra; Zafrani, Max; Sherman, Phillip] Int Rectifier Corp, El Segundo, CA 90245 USA. [Titus, Jeffrey L.] NAVSEA Crane Div, Crane, IN 47522 USA. RP Lauenstein, JM (reprint author), NASA, Goddard Space Flight Ctr, Code 561-4, Greenbelt, MD 20771 USA. EM jean.m.lauenstein@nasa.gov; neil@umd.edu; sliu1@irf.com; jeffrey.titus@navy.mil; raymond.l.ladbury@nasa.gov; hak.s.kim@nasa.gov; anthony.m.phan@nasa.gov; kenneth.a.label@nasa.gov; mzafran1@irf.com; psherma1@irf.com NR 16 TC 10 Z9 10 U1 0 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 2628 EP 2636 DI 10.1109/TNS.2011.2171995 PN 1 PG 9 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400012 ER PT J AU McNulty, PJ Poole, KF Scheick, LZ Yow, S AF McNulty, Peter J. Poole, Kelvin F. Scheick, Leif Z. Yow, Sushan TI Role of Process Variation in the Radiation Response of FGMOS Devices SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE FGMOS; process variation; radiation effects; single-event effects; soft errors ID MEMORY AB UV erasure times are measured and used to determine the degree of process variation across the die of FGMOS memories. Analysis of data obtained following exposure to ionizing radiation separates SEU-like mechanisms that generate anomalous decreases in erasure time from the uniform effects of TID C1 [McNulty, Peter J.; Yow, Sushan] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Poole, Kelvin F.] Clemson Univ, Dept Elect & Comp Engn, Clemson, SC 29634 USA. [Scheick, Leif Z.] Caltech Univ, Jet Prop Lab, Pasadena, CA 91109 USA. RP McNulty, PJ (reprint author), Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. EM mpeter@g.clemson.edu; poole@clemson.edu; leif.z.scheick@jpl.nasa.gov; betaorix@yahoo.com.sg NR 8 TC 1 Z9 1 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 2673 EP 2679 DI 10.1109/TNS.2011.2172987 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400018 ER PT J AU Rodbell, KP Heidel, DF Pellish, JA Marshall, PW Tang, HHK Murray, CE LaBel, KA Gordon, MS Stawiasz, KG Schwank, JR Berg, MD Kim, HS Friendlich, MR Phan, AM Seidleck, CM AF Rodbell, Kenneth P. Heidel, David F. Pellish, Jonathan A. Marshall, Paul W. Tang, Henry H. K. Murray, Conal E. LaBel, Kenneth A. Gordon, Michael S. Stawiasz, Kevin G. Schwank, James R. Berg, Melanie D. Kim, Hak S. Friendlich, Mark. R. Phan, Anthony M. Seidleck, Christina M. TI 32 and 45 nm Radiation-Hardened-by-Design (RHBD) SOI Latches SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE 32 nm and 45 nm SOI hardened latches; angle dependent cross-section distributions; heavy ion modeling; sensitive node separation; silicon-on-insulator technology (SOI); single event upset (SEU); single event effects (SEE); track structures ID SINGLE-EVENT-UPSETS; ION TRACKS; HEAVY-ION; SILICON; ENERGY; ELECTRON AB Single event upset (SEU) experimental heavy ion data and modeling results for CMOS, silicon-on-insulator (SOI), 32 nm and 45 nm stacked and DICE latches are presented. Novel data analysis is shown to be important for hardness assurance where Monte Carlo modeling with a realistic heavy ion track structure, along with a new visualization aid (the Angular Dependent Cross-section Distribution, ADCD), allows one to quickly assess the improvements, or limitations, of a particular latch design. It was found to be an effective technique for making SEU predictions for alternative 32 nm SOI latch layouts. C1 [Rodbell, Kenneth P.; Heidel, David F.; Tang, Henry H. K.; Murray, Conal E.; Gordon, Michael S.; Stawiasz, Kevin G.] IBM TJ Watson Res Ctr, Yorktown Hts, NY 10598 USA. [Pellish, Jonathan A.; LaBel, Kenneth A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Marshall, Paul W.] NASA, Brookneal, VA 24528 USA. [Schwank, James R.] Sandia Natl Labs, Albuquerque, NM 87175 USA. [Berg, Melanie D.; Kim, Hak S.; Friendlich, Mark. R.; Phan, Anthony M.; Seidleck, Christina M.] MEI Technol, Seabrook, MD 20706 USA. RP Rodbell, KP (reprint author), IBM TJ Watson Res Ctr, Yorktown Hts, NY 10598 USA. EM rodbell@us.ibm.com NR 28 TC 22 Z9 22 U1 1 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 2702 EP 2710 DI 10.1109/TNS.2011.2171715 PN 1 PG 9 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400022 ER PT J AU Seifert, N Gill, B Pellish, JA Marshall, PW LaBel, KA AF Seifert, Norbert Gill, Balkaran Pellish, Jonathan A. Marshall, Paul W. LaBel, Kenneth A. TI The Susceptibility of 45 and 32 nm Bulk CMOS Latches to Low-Energy Protons SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE Logic; protons; radiation; SER; single event; soft error ID SINGLE-EVENT-UPSETS; ION TRACK; SOI SRAM; SILICON; TECHNOLOGY; PARTICLES; IMPACT AB We measured low-energy proton radiation induced soft error rates (SER) of standard and reduced-SER (RSER) latches, manufactured in 32 nm and 45 nm bulk CMOS technologies, and conclude that sequential logic elements built in these technologies are not yet susceptible. Further, our results demonstrate that at proton energies where direct ionization dominates, critical charge (Qcrit) plays a far bigger role than at proton energies above the nuclear reaction threshold. C1 [Seifert, Norbert; Gill, Balkaran] Intel Corp, Hillsboro, OR 97124 USA. [Pellish, Jonathan A.; LaBel, Kenneth A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Marshall, Paul W.] NASA, Brookneal, VA 24528 USA. RP Seifert, N (reprint author), Intel Corp, Hillsboro, OR 97124 USA. EM Norbert.Seifert@intel.com; balkaran.gill@intel.com; jonathan.a.pellish@nasa.gov; pwmarshall@aol.com NR 29 TC 11 Z9 11 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 2711 EP 2718 DI 10.1109/TNS.2011.2171004 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400023 ER PT J AU Johnston, A Swimm, R Harris, RD Thorbourn, D AF Johnston, Allan Swimm, Randall Harris, Richard D. Thorbourn, Dennis TI Dose Rate Effects in Linear Bipolar Transistors SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE Annealing; bipolar transistor; dose-rate effects; total dose damage ID GAIN DEGRADATION; CIRCUITS; DEVICES; TRANSPORT; OXIDES; SPACE; ELDRS AB Dose rate effects are examined in linear bipolar transistors at high and low dose rates. At high dose rates, approximately 50% of the damage anneals at room temperature, even though these devices exhibit enhanced damage at low dose rate. The unexpected recovery of a significant fraction of the damage after tests at high dose rate requires changes in existing test standards. Tests at low temperature with a one-second radiation pulse width show that damage continues to increase for more than 3000 seconds afterward, consistent with predictions of the CTRW model for oxides with a thickness of 700 nm, the thickness of the oxide over the emitter-base junction of pnp transistors in this process. C1 [Johnston, Allan; Swimm, Randall; Harris, Richard D.; Thorbourn, Dennis] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Johnston, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM allan.h.johnston@jpl.nasa.gov; randall.t.swimm@jpl.nasa.gov; dennis.thorbourn@jpl.nasa.gov NR 23 TC 10 Z9 10 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 2816 EP 2823 DI 10.1109/TNS.2011.2168979 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400038 ER PT J AU Oldham, TR Chen, D Friendlich, M Carts, MA Seidleck, CM LaBel, KA AF Oldham, T. R. Chen, D. Friendlich, M. Carts, M. A. Seidleck, C. M. LaBel, K. A. TI Effect of Radiation Exposure on the Retention of Commercial NAND Flash Memory SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE CMOS; nonvolatile memory; radiation effects; reliability; retention AB We have compared the data retention of irradiated commercial NAND flash memories with that of unirradiated controls. For parts aged by baking at high temperature, there was a statistically significant difference between irradiated samples and unirradiated controls. For parts aged by repetitive Program/Erase (P/E) cycling, the effect of radiation was not statistically significant. C1 [Oldham, T. R.] Dell Serv Fed Govt Inc, Seabrook, MD 20706 USA. [Chen, D.; Carts, M. A.; LaBel, K. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Friendlich, M.; Seidleck, C. M.] MEI Technol Inc, Seabrook, MD 20706 USA. RP Oldham, TR (reprint author), Dell Serv Fed Govt Inc, Seabrook, MD 20706 USA. EM timothy.r.oldham@nasa.gov NR 23 TC 11 Z9 11 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 2904 EP 2910 DI 10.1109/TNS.2011.2172816 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400050 ER PT J AU Esqueda, IS Barnaby, HJ Adell, PC Rax, BG Hjalmarson, HP McLain, ML Pease, RL AF Esqueda, Ivan S. Barnaby, Hugh J. Adell, Philippe C. Rax, Bernard G. Hjalmarson, Harold P. McLain, Michael L. Pease, Ronald L. TI Modeling Low Dose Rate Effects in Shallow Trench Isolation Oxides SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE Bipolar; CMOS; dose rate; enhanced low dose rate sensitivity (ELDRS); interface traps; shallow trench isolation (STI); silicon dioxide; total ionizing dose (TID) ID RATE SENSITIVITY ELDRS; BIPOLAR-TRANSISTORS; INTERFACE STATES; PHYSICAL MODEL; MOS DEVICES; RADIATION; HYDROGEN; IRRADIATION; MECHANISMS AB Low dose rate experiments on field-oxide-field-effect-transistors (FOXFETs) fabricated in a 90 nm CMOS technology indicate that there is a dose rate enhancement factor (EF) associated with radiation-induced degradation. One dimensional (1-D) numerical calculations are used to investigate the key mechanisms responsible for the dose rate dependent buildup of radiation-induced defects in shallow trench isolation (STI) oxides. Calculations of damage EF indicate that oxide thickness, distribution of hole traps and hole capture cross-section affect dose rate sensitivity. The dose rate sensitivity of STI oxides is compared with the sensitivity of bipolar base oxides using model calculations. C1 [Esqueda, Ivan S.; Barnaby, Hugh J.] Arizona State Univ, Sch Elect Comp & Energy Engn, Tempe, AZ 85287 USA. [Adell, Philippe C.; Rax, Bernard G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hjalmarson, Harold P.; McLain, Michael L.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Pease, Ronald L.] RLP Res, Los Lunas, NM 87031 USA. RP Esqueda, IS (reprint author), Arizona State Univ, Sch Elect Comp & Energy Engn, Tempe, AZ 85287 USA. EM ivans@asu.edu; hbarnaby@asu.edu; philippe.c.adell@jpl.nasa.gov; hphjalm@sandia.gov; lsrlpease@wildblue.net NR 29 TC 7 Z9 8 U1 0 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 2945 EP 2952 DI 10.1109/TNS.2011.2168569 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400056 ER PT J AU Schwank, JR Shaneyfelt, MR Dodd, PE McMorrow, D Warner, JH Ferlet-Cavrois, V Gouker, PM Melinger, JS Pellish, JA Rodbell, KP Heidel, DF Marshall, PW LaBel, K Swanson, SE AF Schwank, James R. Shaneyfelt, Marty R. Dodd, Paul E. McMorrow, Dale Warner, Jeffrey H. Ferlet-Cavrois, Veronique Gouker, Pascale M. Melinger, Joseph S. Pellish, Jonathan A. Rodbell, Kenneth P. Heidel, David F. Marshall, Paul W. LaBel, KennethA. Swanson, Scot E. TI Comparison of Single and Two-Photon Absorption for Laser Characterization of Single-Event Upsets in SOI SRAMs SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE Hardness assurance; heavy-ion testing; laser testing; single-event upset; threshold LET; two-photon absorption ID CHARGE COLLECTION; ION ENERGY; HEAVY-ION; CIRCUITS; IMPACT AB The laser pulse energy thresholds for single-event upset measured by single photon and two photon absorption are measured and compared for Sandia SRAMs and DPSRAMs, and IBM 45-nm SRAMs for devices with and without the back substrate removed. These results are also compared to heavy-ion results taken on the same devices. Sandia SRAM data taken on different test dates resulted in considerably different TPA laser pulse energy thresholds even though the TPA system was calibrated using standard techniques each test date. These differences are believed to be due to changes in laser spot size. This shows that it is imperative to develop a calibration procedure that monitors all relevant laser parameters if TPA is to be used as a routine quantitative tool. Removing the back substrate makes a very large difference in TPA laser pulse energy threshold. This large difference is likely due to either displacement currents generated in the back substrate by TPA and/or nonlinear optical effects which can reduce the laser pulse irradiance in the active region. Nevertheless, the mechanism does not appear to affect the qualitative nature of TPA measurements. Both SPA and TPA laser measurements were used to estimate the heavy-ion threshold LETs of the Sandia DPSRAMs and 45-nm IBM SRAMs. Both SPA and TPA overestimated the heavy-ion threshold LET of the IBM 45-nm SRAMs (likely due to the large laser spot size compared to the size of the SRAM cell), but reasonably estimated the threshold LETs of the Sandia DPSRAMs. For the first time, TPA laser pulse energy (squared) is directly compared to SPA laser pulse energy at threshold. There is reasonable quantitative agreement between the charge required to induce upsets by TPA and SPA with the back substrate removed. C1 [Schwank, James R.; Shaneyfelt, Marty R.; Dodd, Paul E.; Swanson, Scot E.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [McMorrow, Dale; Warner, Jeffrey H.; Melinger, Joseph S.] USN, Res Lab, Washington, DC 20375 USA. [Ferlet-Cavrois, Veronique] ESA ESTEC, NL-2200 AG Noordwijk, Netherlands. [Gouker, Pascale M.] MIT, Lincoln Lab, Lexington, MA 02420 USA. [Pellish, Jonathan A.; LaBel, KennethA.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rodbell, Kenneth P.; Heidel, David F.] IBM Corp, Thomas J Watson Res Ctr, Yorktown Hts, NY 10598 USA. [Marshall, Paul W.] NASA, Brookneal, VA 24528 USA. RP Schwank, JR (reprint author), Sandia Natl Labs, POB 5800, Albuquerque, NM 87185 USA. EM schwanjr@sandia.gov NR 14 TC 3 Z9 3 U1 2 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 2968 EP 2975 DI 10.1109/TNS.2011.2171006 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400059 ER PT J AU Buchner, S Kanyogoro, N McMorrow, D Foster, CC O'Neill, PM Nguyen, KV AF Buchner, S. Kanyogoro, N. McMorrow, D. Foster, C. C. O'Neill, Patrick M. Nguyen, Kyson V. TI Variable Depth Bragg Peak Method for Single Event Effects Testing SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE Bragg peak; heavy ions; silicon-on-insulator; single event upset AB The Variable Depth Bragg Peak (VDBP) method for measuring the Single Event Effects (SEE) cross-section of an integrated circuit (IC) in a closed package as a function of ion linear energy transfer (LET) is described. The method uses long-range, high-energy heavy ions that can penetrate the package and deposit charge in the device's sensitive volume (SV), the depth of which is not known. A series of calibrated energy degraders is used to vary the depth of the Bragg peak relative to the device's sensitive volume. When the Bragg peak is located at the sensitive volume, the measured SEE cross-section is a maximum, as is the LET, which is calculated using a Monte Carlo-based program, TRIM that takes both straggling and spread in beam energy and angle into account. Degrader thickness is varied and the change in LET is calculated while the corresponding cross-section is measured. Good agreement was obtained between the LET-dependence of the single event upset (SEU) cross-section for a 4 Mbit memory in an unopened package using the above method and that for an identical de-lidded part previously measured. C1 [Buchner, S.; Kanyogoro, N.] USN, SDS, Res Lab, Washington, DC 20375 USA. [Foster, C. C.] Foster Consulting Serv LLC, University Pl, WA 98466 USA. [O'Neill, Patrick M.] NASA, JSC, Houston, TX 77058 USA. [Nguyen, Kyson V.] Jacobs Technol, Houston, TX 77258 USA. RP Buchner, S (reprint author), USN, SDS, Res Lab, Washington, DC 20375 USA. EM fosterchc@nventure.com; patrick.m.oneill@nasa.gov; kyson.v.nguyen@nasa.gov NR 7 TC 10 Z9 10 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 2976 EP 2982 DI 10.1109/TNS.2011.2170587 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400060 ER PT J AU Chen, DK Pease, R Kruckmeyer, K Forney, J Phan, A Carts, M Cox, S Burns, S Albarian, R Holcombe, B Little, B Salzman, J Chaumont, G Duperray, H Ouellet, A Buchner, S LaBel, K AF Chen, Dakai Pease, Ronald Kruckmeyer, Kirby Forney, James Phan, Anthony Carts, Martin Cox, Stephen Burns, Sam Albarian, Rafi Holcombe, Bruce Little, Bradley Salzman, James Chaumont, Geraldine Duperray, Herve Ouellet, Al Buchner, Stephen LaBel, Kenneth TI Enhanced Low Dose Rate Sensitivity at Ultra-Low Dose Rates SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE Bipolar; dose rate; ELDRS; radiation hardness ID BIPOLAR LINEAR CIRCUITS; DROPOUT VOLTAGE REGULATOR; PASSIVATION LAYERS; MOLECULAR-HYDROGEN; GAIN DEGRADATION; RATE RESPONSE; DEVICES; ELDRS; IRRADIATION; MECHANISMS AB We present results on the effects of ELDRS at dose rates of 10, 5, 1, and 0.5 mrad(Si)/s for a variety of commercial, radiation hardened, and ELDRS-free devices. We observed low dose rate enhancement below 10 mrad(Si)/s in several different part types. The magnitudes of the low dose rate enhancement varied substantially. The most notable case showed dose rate sensitivity in the functional failures for a commercial voltage regulator, with initial failures occurring after 10 krad(Si) for the parts irradiated at 0.5 mrad(Si)/s. Radiation hardened and ELDRS-free devices also showed ELDRS at the ultra-low dose rates. An ELDRS-free high power regulator showed a low dose rate enhancement factor of x33 after 10 krad(Si) for parts irradiated at 0.5 mrad(Si)/s. The enhanced degradation at the ultra-low dose rates present challenges for hardness assurance. C1 [Chen, Dakai; Carts, Martin; Cox, Stephen; LaBel, Kenneth] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pease, Ronald] RLP Res, Los Lunas, NM 87031 USA. [Kruckmeyer, Kirby] Natl Semicond Corp, Santa Clara, CA 95052 USA. [Forney, James; Phan, Anthony] MEI Tech Inc, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Burns, Sam; Albarian, Rafi] Linear Technol Corp, Milpitas, CA 95035 USA. [Holcombe, Bruce; Little, Bradley; Salzman, James] Texas Instruments Inc, Sherman, TX 75090 USA. [Chaumont, Geraldine; Duperray, Herve] ST Microelect Inc, F-35208 Rennes 2, France. [Ouellet, Al] ST Microelect Inc, Lexington, MA 02421 USA. [Buchner, Stephen] USN, Res Lab, Washington, DC USA. RP Chen, DK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM dakai.chen-1@nasa.gov; lsrl-pease@wildblue.net; kirby.kruckmeyer@nsc.com; james.d.forney@nasa.gov; ralbarian@linear.com; salzman@ti.com; geraldine.chaumont@st.com; herve.duperray@st.com; ouellet@st.com; Stephen.buchner.ctr@nrl.navy.mil NR 24 TC 9 Z9 9 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 2983 EP 2990 DI 10.1109/TNS.2011.2171720 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400061 ER PT J AU Liu, S Lauenstein, JM Ferlet-Cavrois, V Marec, R Hernandez, F Scheick, L Bezerra, F Muschitiello, M Poivey, C Sukhaseum, N Coquelet, L Cao, H Carrier, D Brisebois, MA Mangeret, R Ecoffet, R LaBel, K Zafrani, M Sherman, P AF Liu, Sandra Lauenstein, Jean-Marie Ferlet-Cavrois, Veronique Marec, Ronan Hernandez, Francisco Scheick, Leif Bezerra, Francoise Muschitiello, Michele Poivey, Christian Sukhaseum, Nicolas Coquelet, Lemuel Cao, Huy Carrier, Douglass Brisebois, Mark A. Mangeret, Renaud Ecoffet, Robert LaBel, Ken Zafrani, Max Sherman, Phillip TI Effects of Ion Species on SEB Failure Voltage of Power DMOSFET SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE Heavy ion species; power MOSFET; single event burnout; single event effect ID SINGLE-EVENT BURNOUT; ENERGY; MOSFETS; SEGR AB This paper presents and explains test results showing the effect of ion species on the single event burnout (SEB) failure voltage using a SEB sensitive engineering power double diffused metal oxide silicon field effect transistor (DMOSFET). The analyses show the determining factor of tested SEB failure voltage is the ion species itself rather than test or beam conditions such as initial beam energy, surface linear energy transfer (LET), ion range, or ionized charge. Also, results from five test facilities and five test setups are compared to determine if there will be differences in test results when different test setups or different heavy ion accelerator facilities were used. C1 [Liu, Sandra; Cao, Huy] Int Rectifier Corp, El Segundo, CA 90245 USA. [Lauenstein, Jean-Marie; LaBel, Ken] NASA, GSFC, Greenbelt, MD 20771 USA. [Ferlet-Cavrois, Veronique; Muschitiello, Michele; Poivey, Christian] European Space Agcy, ESA ESTEC, NL-2200 AG Noordwijk, Netherlands. [Marec, Ronan] Thales Alenia Space, F-337873103 Tollouse, France. [Hernandez, Francisco; Mangeret, Renaud] EADS Astrium SAS, F-31402 Toulouse 4, France. [Scheick, Leif] Jet Prop Lab, Pasadena, CA 91109 USA. [Bezerra, Francoise; Ecoffet, Robert] CNES, Toulouse 9, France. [Sukhaseum, Nicolas; Coquelet, Lemuel] TRAD, F-31674 Labege, France. RP Liu, S (reprint author), Int Rectifier Corp, El Segundo, CA 90245 USA. EM sliu1@irf.com; jean.m.lauenstein@nasa.gov; ronan.marec@thalesaleniaspace.com; francisco.hernandez@astrium.eads.net; leif.z.scheick@jpl.nasa.gov; Francoise.Bezerra@cnes.fr; lemuel.coquelet@trad.fr; hcao1@irf.com; dcarrie1@irf.com; mbriseb1@irf.com; Robert.Ecoffet@cnes.fr; mzafran1@irf.com; PSHERMA1@irf.com NR 13 TC 15 Z9 15 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 2991 EP 2997 DI 10.1109/TNS.2011.2172958 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400062 ER PT J AU Ladbury, R Triggs, B AF Ladbury, R. Triggs, B. TI A Bayesian Approach for Total Ionizing Dose Hardness Assurance SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE Probabilistic risk assessment; quality assurance radiation hardness assurance methodology; radiation effects; reliability estimation AB We develop a Bayesian RHA methodology for TID. The method is capable of using a broad variety of data for improved qualification and risk mitigation. C1 [Ladbury, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Triggs, B.] Semicoa Corp, Rad Hard Program Qual, Costa Mesa, CA 92626 USA. RP Ladbury, R (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM raymond.l.ladbury.1@gsfc.nasa.gov NR 12 TC 6 Z9 6 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 3004 EP 3010 DI 10.1109/TNS.2011.2172461 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400064 ER PT J AU Adell, PC Liu, T Vermeire, B Bakkaloglu, B Aveline, D AF Adell, Philippe C. Liu, Tao Vermeire, Bert Bakkaloglu, Bertan Aveline, David TI An SET-Free, All-Digital Controlled Point-of-Load Regulator for Next-Generation Power Systems: ADC-POL SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE Digital control; power distribution; radiation hardening; single event transients (SETs) ID SINGLE-EVENT TRANSIENTS; VOLTAGE REGULATORS; CONVERTERS AB This paper presents a digitally controlled programmable point-of-load regulator for next-generation power systems. A novel digital control scheme was designed to minimize single-event effect (SEE)-induced transient effects. By effectively programming the loop transmission, the POL can trade off transient response time with SET robustness. The IC works with 1 to 5.5 V input voltage, 1-4.5V regulated output voltage, high efficiency (peak efficiency at 94%) and power of up to 5 W. The design was fabricated in the AMI i2t100 0.7 mu m complimentary, metal-oxide semiconductor (CMOS) process and characterized with the Jet Propulsion Laboratory (JPL) pulsed laser system. C1 [Adell, Philippe C.; Aveline, David] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Liu, Tao; Bakkaloglu, Bertan] Arizona State Univ, A Fulton Sch Engn, Tempe, AZ 85287 USA. [Vermeire, Bert] Space Micro, San Diego, CA 92121 USA. RP Adell, PC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM philippe.c.adell@jpl.nasa.gov; tao.liu@asu.edu; bert.vermeire@asu.edu; bertan.bakkaloglu@asu.edu; david.ave-line@jpl.nasa.gov NR 12 TC 3 Z9 3 U1 1 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 3011 EP 3017 DI 10.1109/TNS.2011.2172459 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400065 ER PT J AU Clark, LT Patterson, DW Hindman, ND Holbert, KE Maurya, S Guertin, SM AF Clark, Lawrence T. Patterson, Dan W. Hindman, Nathan D. Holbert, Keith E. Maurya, Satendra Guertin, Steven M. TI A Dual Mode Redundant Approach for Microprocessor Soft Error Hardness SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE Dual mode redundancy; error correction; radiation hardening; register files; sequential logic circuits; single event effects; soft errors; total ionizing dose ID FLIP-FLOP; CIRCUITS; TECHNOLOGIES AB A dual mode redundant (DMR) logic data path with instruction restart that detects errors at register file (RF) write-back is presented. The DMR RF allows SEU correction using parity to detect RF entry nibbles that are correct in one copy but not the other. Detection and backing out incorrect write data are also described. The radiation hardened by design (RHBD) circuits are implemented in 90 nm CMOS. The DMR microarchitecture is described, including pipelining, error handling, and the associated hardware. Heavy ion and proton testing validate the approach. Experimentally measured cross sections and examples of errors due to pipeline SET or RF SEU are shown. Critical node spacing and the mitigation of multiple node collection are also described. C1 [Clark, Lawrence T.; Patterson, Dan W.; Hindman, Nathan D.; Holbert, Keith E.; Maurya, Satendra] Arizona State Univ, Sch Elect Comp & Energy Engn, Tempe, AZ 85287 USA. [Guertin, Steven M.] NASA, Jet Prop Labs, Pasadena, CA 91109 USA. RP Clark, LT (reprint author), Arizona State Univ, Sch Elect Comp & Energy Engn, Tempe, AZ 85287 USA. EM lawrence.clark@asu.edu; dan.patterson@asu.edu; nathan.hindman@asu.edu; holbert@asu.edu; steven.m.guertin@jpl.nasa.gov RI Holbert, Keith/B-6518-2008; OI Holbert, Keith/0000-0002-2772-1954 NR 21 TC 8 Z9 8 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 3018 EP 3025 DI 10.1109/TNS.2011.2168828 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400066 ER PT J AU Horst, SJ Phillips, SD Cressler, JD Kruckmeyer, K Eddy, R Aude, A O'Farrell, P Zhang, BY Wilcox, E LaBel, K AF Horst, Stephen J. Phillips, Stanley D. Cressler, John D. Kruckmeyer, Kirby Eddy, Robert Aude, Arlo O'Farrell, Patrick Zhang, Benyong Wilcox, Edward LaBel, Ken TI A Study of Total Dose Mitigation Approaches for Charge Pumps in Phase-Locked Loop Applications SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE Charge pumps; frequency synthesizer; HBT; radiation effects; radiation hardening; SiGe; silicon-germanium ID CMOS TECHNOLOGIES; CIRCUITS; DESIGN AB An analysis of charge pump design for improved radiation tolerance of phase locked loops is presented. Two radiation-hardened-by-design approaches are considered to mitigate the total ionizing dose damage of the circuit, and a thick-film SOI SiGe process technology has been used to reduce charge collection of single event strikes. The results show that a modified design approach to implement the charge pump using SiGe HBTs can provide advantages in radiation tolerance to improve tri-state leakage performance, particularly for missions expecting large accumulated doses. C1 [Horst, Stephen J.; Phillips, Stanley D.; Cressler, John D.] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. [Kruckmeyer, Kirby; Eddy, Robert; Aude, Arlo; O'Farrell, Patrick; Zhang, Benyong] Natl Semicond Corp, Santa Clara, CA 95052 USA. [Wilcox, Edward; LaBel, Ken] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Horst, SJ (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. EM shorst@gatech.edu NR 22 TC 2 Z9 2 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 3038 EP 3045 DI 10.1109/TNS.2011.2170200 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400069 ER PT J AU Sabra, MS Weller, RA Mendenhall, MH Reed, RA Clemens, MA Barghouty, AF AF Sabra, M. S. Weller, Robert A. Mendenhall, Marcus H. Reed, Robert A. Clemens, Michael A. Barghouty, A. F. TI Validation of Nuclear Reaction Codes for Proton-Induced Radiation Effects: The Case for CEM03 SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT IEEE Radiation Effects Data Workshop (REDW)/48th IEEE International Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 25-29, 2011 CL Las Vegas, NV SP Inst Elect & Elect Engineers (IEEE), IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE Fission reaction; Geant4; MRED; nuclear physics simulation; proton-induced reaction ID MODELS; FRAGMENTATION; COLLISIONS; ENERGY AB Experimental cross-section data for the interaction of protons with Al, Co, and Au at intermediate energies are compared with the predictions of the nuclear reaction models CEM03, BIC, Bertini INC, and INCL-ABLA. Fission cross-section data for the interaction of protons with W and Au in the energy range 50 MeV-3 GeV are also compared with the considered models. The study reveals that all of the models are satisfactory in limited ranges. However, of these, the CEM03 code from Los Alamos exhibits the broadest applicability for radiation effects computations. C1 [Sabra, M. S.; Weller, Robert A.; Mendenhall, Marcus H.; Reed, Robert A.] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37235 USA. [Clemens, Michael A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Barghouty, A. F.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. RP Sabra, MS (reprint author), Vanderbilt Univ, Dept Elect Engn & Comp Sci, 221 Kirkland Hall, Nashville, TN 37235 USA. EM m.sabra@vanderbilt.edu; robert.a.weller@vanderbilt.edu; marcus.h.mendenhall@vanderbilt.edu; robert.a.reed@vanderbilt.edu; michael.a.clemens@vanderbilt.edu; abdulnasser.f.barghouty@nasa.gov NR 17 TC 4 Z9 4 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 3134 EP 3138 DI 10.1109/TNS.2011.2169989 PN 1 PG 5 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905QN UT WOS:000301287400081 ER PT J AU Edmonds, LD AF Edmonds, Larry D. TI Extension of the ADC Charge-Collection Model to Include Multiple Junctions SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE ADC model; ambipolar diffusion; ambipolar diffusion with a cutoff; charge collection; drift-diffusion ID TRANSPORT AB The ADC charge-collection model was derived for silicon diodes containing a single reverse-biased p-n junction. The present paper extends the model to include two junctions, and the goal is to estimate how collected charge is shared between them. The extended model identifies the conditions needed to produce either of three possibilities. One possibility is that charge is shared by both junctions, and the total collected charge from the two junctions is less than the total amount of liberated charge. A second possibility is that collected charge is shared by both junctions, and the total collected charge from the two junctions is equal to the total amount of liberated charge. The third possibility is that all liberated charge is collected by one junction, and no charge is collected by the other. Examples show excellent agreement with TCAD simulations. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Edmonds, LD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM larry.d.edmonds73@gmail.com FU National Aeronautics and Space Administration FX The research in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Reference herein to any specific commercial product, process, or service by trade name, manufacturer, or otherwise, does not constitute or imply its endorsement by the U.S. Government or the Jet Propulsion Laboratory, California Institute of Technology. Government sponsorship acknowledged. NR 6 TC 3 Z9 3 U1 2 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2011 VL 58 IS 6 BP 3333 EP 3342 DI 10.1109/TNS.2011.2168976 PN 2 PG 10 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 905PW UT WOS:000301285700018 ER PT J AU Conway, EM AF Conway, Erik M. TI Revolutionary Atmosphere: The Story of the Altitude Wind Tunnel and the Space Power Chambers SO ISIS LA English DT Book Review C1 [Conway, Erik M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Conway, EM (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD DEC PY 2011 VL 102 IS 4 BP 797 EP 798 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 890DZ UT WOS:000300126600064 ER PT J AU Terrile, RJ AF Terrile, Richard J. TI Pathways and Challenges to Innovation in Aerospace SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE LA English DT Article C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Terrile, RJ (reprint author), CALTECH, Jet Prop Lab, Mail Stop 301-355,4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration FX The work described herein was carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. NR 13 TC 2 Z9 2 U1 2 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0885-8985 J9 IEEE AERO EL SYS MAG JI IEEE Aerosp. Electron. Syst. Mag. PD DEC PY 2011 VL 26 IS 12 BP 4 EP 9 PG 6 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA 885XK UT WOS:000299814500002 ER PT J AU Seller, P Bell, S Cernik, RJ Christodoulou, C Egan, CK Gaskin, JA Jacques, S Pani, S Ramsey, BD Reid, C Sellin, PJ Scuffham, JW Speller, RD Wilson, MD Veale, MC AF Seller, P. Bell, S. Cernik, R. J. Christodoulou, C. Egan, C. K. Gaskin, J. A. Jacques, S. Pani, S. Ramsey, B. D. Reid, C. Sellin, P. J. Scuffham, J. W. Speller, R. D. Wilson, M. D. Veale, M. C. TI Pixellated Cd(Zn)Te high-energy X-ray instrument SO JOURNAL OF INSTRUMENTATION LA English DT Article; Proceedings Paper CT 9th International Conference on Position Sensitive Detectors CY SEP 12-16, 2011 CL Aberystwyth, WALES DE X-ray detectors; Pixelated detectors and associated VLSI electronics; X-ray detectors and telescopes; Gamma camera; SPECT; PET PET/CT; coronary CT angiography (CTA) ID NUCLEAR RADIATION DETECTOR; CDTE; DIFFRACTION; CHARGE AB We have developed a pixellated high energy X-ray detector instrument to be used in a variety of imaging applications. The instrument consists of either a Cadmium Zinc Telluride or Cadmium Telluride (Cd(Zn)Te) detector bump-bonded to a large area ASIC and packaged with a high performance data acquisition system. The 80 by 80 pixels each of 250 mu m by 250 mu m give better than 1 keV FWHM energy resolution at 59.5 keV and 1.5 keV FWHM at 141 keV, at the same time providing a high speed imaging performance. This system uses a relatively simple wire-bonded interconnection scheme but this is being upgraded to allow multiple modules to be used with very small dead space. The readout system and the novel interconnect technology is described and how the system is performing in several target applications. C1 [Seller, P.; Bell, S.; Wilson, M. D.; Veale, M. C.] Rutherford Appleton Lab, Dept Technol, Didcot OX11 0QX, Oxon, England. [Cernik, R. J.; Egan, C. K.; Jacques, S.] Univ Manchester, Sch Mat, Manchester M1 7HS, Lancs, England. [Christodoulou, C.; Reid, C.; Speller, R. D.] UCL, Dept Med Phys & Bioengn, London WC1E 6BT, England. [Pani, S.; Sellin, P. J.; Scuffham, J. W.] Univ Surrey, Dept Phys, Guildford GU2 7XH, Surrey, England. [Scuffham, J. W.] Royal Surrey Cty Hosp, Dept Nucl Med, Guildford GU2 7XX, Surrey, England. [Gaskin, J. A.; Ramsey, B. D.] NASA, Space Sci Technol Ctr, Huntsville, AL 35805 USA. RP Seller, P (reprint author), Rutherford Appleton Lab, Dept Technol, Harwell Sci & Innovat Campus, Didcot OX11 0QX, Oxon, England. EM paul.seller@stfc.ac.uk RI Jacques, Simon/C-6960-2009; OI Jacques, Simon/0000-0002-7275-5272; Veale, Matthew/0000-0001-5457-4884 NR 34 TC 40 Z9 40 U1 0 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-0221 J9 J INSTRUM JI J. Instrum. PD DEC PY 2011 VL 6 AR C12009 DI 10.1088/1748-0221/6/12/C12009 PG 12 WC Instruments & Instrumentation SC Instruments & Instrumentation GA 882BQ UT WOS:000299536600009 ER PT J AU Hochepied, JF Berger, MH Dynys, F Dessombz, A Sayir, A AF Hochepied, Jean-Francois Berger, Marie-Helene Dynys, Fred Dessombz, Arnaud Sayir, Ali TI Aqueous Co-precipitated Ti0.5Sn0.5O2 Nanopowders as Precursors for Dense Spinodally Decomposed Ceramics SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY LA English DT Article ID THERMOELECTRIC-MATERIALS; SYSTEM; TIO2-SNO2 AB Spinodal decomposition in the TiO2SnO2 system produces TiO2 rich/SnO2 rich nano-wide lamellae. The high density of coherent interfaces is expected to reduce thermal conductivity of the ceramic without blocking electron transport. These semiconductors could therefore be candidates for environmental friendly oxide thermo-electrics. However, dense materials are difficult to obtain by conventional sintering from a mixture of TiO2 and SnO2 powders due to evaporation of tin oxide. The article presents a novel route to produce, by aqueous co-precipitation, Ti0.5Sn0.5O2 nanopowders as precursors for dense ceramics. The nanostructure developed by spinodal decomposition inside the grains of the as obtained dense Ti0.5Sn0.5O2 ceramic is shown to be comparable to that of porous Ti0.5Sn0.5O2 ceramic obtained by conventional method. C1 [Hochepied, Jean-Francois; Dessombz, Arnaud] MINES ParisTech, Ctr Energet & Proc, SCPI, F-75272 Paris 06, France. [Berger, Marie-Helene] MINES ParisTech, CNRS, Ctr Mat, UMR 7633, F-91003 Evry, France. [Dynys, Fred; Sayir, Ali] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Hochepied, JF (reprint author), MINES ParisTech, Ctr Energet & Proc, SCPI, 60 Bd St Michel, F-75272 Paris 06, France. EM jean-francois.hochepied@mines-paristech.fr RI Berger, Marie-Helene/B-9785-2013; Dessombz, Arnaud/B-7149-2016 OI Dessombz, Arnaud/0000-0002-6610-4879 NR 7 TC 5 Z9 5 U1 2 U2 32 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-7820 J9 J AM CERAM SOC JI J. Am. Ceram. Soc. PD DEC PY 2011 VL 94 IS 12 BP 4226 EP 4230 DI 10.1111/j.1551-2916.2011.04797.x PG 5 WC Materials Science, Ceramics SC Materials Science GA 859BC UT WOS:000297848100026 ER PT J AU Arridge, CS Andre, N McAndrews, HJ Bunce, EJ Burger, MH Hansen, KC Hsu, HW Johnson, RE Jones, GH Kempf, S Khurana, KK Krupp, N Kurth, WS Leisner, JS Paranicas, C Roussos, E Russell, CT Schippers, P Sittler, EC Smith, HT Thomsen, MF Dougherty, MK AF Arridge, C. S. Andre, N. McAndrews, H. J. Bunce, E. J. Burger, M. H. Hansen, K. C. Hsu, H-W Johnson, R. E. Jones, G. H. Kempf, S. Khurana, K. K. Krupp, N. Kurth, W. S. Leisner, J. S. Paranicas, C. Roussos, E. Russell, C. T. Schippers, P. Sittler, E. C. Smith, H. T. Thomsen, M. F. Dougherty, M. K. TI Mapping Magnetospheric Equatorial Regions at Saturn from Cassini Prime Mission Observations SO SPACE SCIENCE REVIEWS LA English DT Review DE Cassini; Saturn; Magnetospheric regions; Plasma processes ID ION-CYCLOTRON WAVES; CAPS ELECTRON SPECTROMETER; LOW-FREQUENCY WAVES; SOLAR-WIND FLOW; MAGNETIC-FIELD; INNER MAGNETOSPHERE; E-RING; KILOMETRIC RADIATION; ORBIT INSERTION; ROTATION PERIOD AB Saturn's rich magnetospheric environment is unique in the solar system, with a large number of active magnetospheric processes and phenomena. Observations of this environment from the Cassini spacecraft has enabled the study of a magnetospheric system which strongly interacts with other components of the saturnian system: the planet, its rings, numerous satellites (icy moons and Titan) and various dust, neutral and plasma populations. Understanding these regions, their dynamics and equilibria, and how they interact with the rest of the system via the exchange of mass, momentum and energy is important in understanding the system as a whole. Such an understanding represents a challenge to theorists, modellers and observers. Studies of Saturn's magnetosphere based on Cassini data have revealed a system which is highly variable which has made understanding the physics of Saturn's magnetosphere all the more difficult. Cassini's combination of a comprehensive suite of magnetospheric fields and particles instruments with excellent orbital coverage of the saturnian system offers a unique opportunity for an in-depth study of the saturnian plasma and fields environment. In this paper knowledge of Saturn's equatorial magnetosphere will be presented and synthesised into a global picture. Data from the Cassini magnetometer, low-energy plasma spectrometers, energetic particle detectors, radio and plasma wave instrumentation, cosmic dust detectors, and the results of theory and modelling are combined to provide a multi-instrumental identification and characterisation of equatorial magnetospheric regions at Saturn. This work emphasises the physical processes at work in each region and at their boundaries. The result of this study is a map of Saturn's near equatorial magnetosphere, which represents a synthesis of our current understanding at the end of the Cassini Prime Mission of the global configuration of the equatorial magnetosphere. C1 [Arridge, C. S.; Jones, G. H.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Arridge, C. S.; Jones, G. H.] UCL Birkbeck, Ctr Planetary Sci, London WC1E 6BT, England. [Andre, N.] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Bunce, E. J.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Burger, M. H.; Sittler, E. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hansen, K. C.] Univ Michigan, Ctr Space Environm Modeling, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Hsu, H-W; Kempf, S.] Max Planck Inst Nucl Phys, D-69117 Heidelberg, Germany. [Johnson, R. E.] Univ Virginia, Engn Phys Program, Charlottesville, VA 22904 USA. [Johnson, R. E.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Andre, N.] Univ Toulouse, Inst Rech Astrophys & Planetol, UPS OMP, F-31028 Toulouse, France. [McAndrews, H. J.; Thomsen, M. F.] LANL, ISR 1, Space & Atmospher Sci Grp, Los Alamos, NM 87545 USA. [Khurana, K. K.; Leisner, J. S.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Krupp, N.; Roussos, E.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Kurth, W. S.; Leisner, J. S.; Schippers, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Paranicas, C.; Smith, H. T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Arridge, CS (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM csa@mssl.ucl.ac.uk RI Arridge, Christopher/A-2894-2009; Hansen, Kenneth/F-3693-2011; Russell, Christopher/E-7745-2012; Jones, Geraint/C-1682-2008; Paranicas, Christopher/B-1470-2016; Smith, Howard/H-4662-2016; Bunce, Emma/I-9067-2016; OI Kurth, William/0000-0002-5471-6202; Jones, Geraint/0000-0002-5859-1136; Roussos, Elias/0000-0002-5699-0678; Arridge, Christopher/0000-0002-0431-6526; Hansen, Kenneth/0000-0002-8502-1980; Russell, Christopher/0000-0003-1639-8298; Paranicas, Christopher/0000-0002-4391-8255; Smith, Howard/0000-0003-3537-3360; Bunce, Emma/0000-0002-9456-0345; KEMPF, SASCHA/0000-0001-5236-3004 FU International Space Science Institute (ISSI); CNES; STFC FX The authors acknowledge funding and support from the International Space Science Institute (ISSI) in carrying out this multi-instrument study, which supported the team for two visits to ISSI, Berne, Switzerland. All the authors acknowledge the hospitality and kindness of the ISSI support team for making their visits pleasant and productive. CSA was supported in this work by the STFC rolling grant to MSSL/UCL and an STFC postdoctoral fellowship. NA acknowledges the support from CNES. The authors acknowledge the efforts of everyone working on the Cassini project and particularly the MAPS instrument teams for making the Cassini/Huygens mission such a success. CSA thanks Abi Rymer for useful discussions, Fran Bagenal and Don Gurnett for comments on the manuscript, and Don Mitchell for assistance with Cassini MIMI data. NR 259 TC 14 Z9 14 U1 3 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD DEC PY 2011 VL 164 IS 1-4 BP 1 EP 83 DI 10.1007/s11214-011-9850-4 PG 83 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 885HH UT WOS:000299769100001 ER PT J AU Wolters, SD Rozitis, B Duddy, SR Lowry, SC Green, SF Snodgrass, C Hainaut, OR Weissman, P AF Wolters, Stephen D. Rozitis, Ben Duddy, Samuel R. Lowry, Stephen C. Green, Simon F. Snodgrass, Colin Hainaut, Olivier R. Weissman, Paul TI Physical characterization of low delta-V asteroid (175706) 1996 FG3 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: thermal; minor planets, asteroids: individual: (175706)1996FG3; infrared: general ID NEAR-EARTH ASTEROIDS; BINARY ASTEROIDS; THERMAL-MODEL; YARKOVSKY; FG(3); LIGHTCURVES; CALIBRATION; PHOTOMETRY; MAGNITUDE; TARGETS AB Asteroid (175706) 1996 FG3 is a binary asteroid and the baseline target for the proposed MarcoPolo-R sample return mission. We present thermal-infrared photometry obtained with the European Southern Observatory (ESO) Very Large Telescope using the VISIR instrument, together with optical photometry obtained with the ESO New Technology Telescope using the EFOSC2 instrument. An absolute visual magnitude HV= 17.833 +/- 0.024 and phase parameter G=-0.041 +/- 0.005 are derived. The near-Earth asteroid thermal model has been fitted to the measured fluxes to derive a geometric visual albedo pv= 0.046 +/- 0.014, effective diameter at the observed aspect Deff= 1.68 +/- 0.25 km and beaming parameter eta= 1.15 for phase angle a= 117. The advanced thermophysical model (ATPM) has been fitted to the measured fluxes to derive a more accurate effective diameter Deff= 1.71 +/- 0.07 km and albedo pv= 0.044 +/- 0.004. Based on the ATPM results, assuming the same albedo for primary and secondary, we derive a primary mean spherical diameter Dp= 1.69+0.18- 0.12 km, secondary diameter Ds= 0.51 +/- 0.03 km and a secondary orbital semimajor axis a= 2.8+1.7-0.7 km. A low surface thermal inertia G= 120 +/- 50 J m-2 s-1/2 K-1 was also derived, suggesting a dusty surface and raising questions as to the binary formation mechanism of this asteroid. These physical properties are used to predict a Yarkovsky drift in semimajor axis of -60+31-45 m yr-1. C1 [Wolters, Stephen D.; Rozitis, Ben; Green, Simon F.] Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. [Duddy, Samuel R.; Lowry, Stephen C.] Univ Kent, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NZ, Kent, England. [Snodgrass, Colin] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Hainaut, Olivier R.] European So Observ, D-85748 Garching, Germany. [Weissman, Paul] CALTECH, Jet Prop Lab, Planetary Ices Sect, Pasadena, CA 91109 USA. RP Wolters, SD (reprint author), Open Univ, Planetary & Space Sci Res Inst, Walton Hall, Milton Keynes MK7 6AA, Bucks, England. EM s.d.wolters@open.ac.uk; b.rozitis@open.ac.uk; s.duddy@kent.ac.uk; s.c.lowry@kent.ac.uk; s.f.green@open.ac.uk; snodgrass@mps.mpg.de; ohain-aut@eso.org; paul.r.weissman@jpl.nasa.gov RI Green, Simon/C-7408-2009; OI Snodgrass, Colin/0000-0001-9328-2905 FU UK Science and Technology Facilities Council; European Union [268421] FX The work of SDW and BR was funded by the UK Science and Technology Facilities Council. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 268421. We thank P. Pravec for his thorough and insightful review, and both Pravec and his collaborators for making it possible for us to refine our estimates through the application of their preliminary updated orbital model. NR 51 TC 20 Z9 22 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2011 VL 418 IS 2 BP 1246 EP 1257 DI 10.1111/j.1365-2966.2011.19575.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 860ZI UT WOS:000297987400045 ER PT J AU Tibbs, CT Flagey, N Paladini, R Compiegne, M Shenoy, S Carey, S Noriega-Crespo, A Dickinson, C Ali-Haimoud, Y Casassus, S Cleary, K Davies, RD Davis, RJ Hirata, CM Watson, RA AF Tibbs, C. T. Flagey, N. Paladini, R. Compiegne, M. Shenoy, S. Carey, S. Noriega-Crespo, A. Dickinson, C. Ali-Haimoud, Y. Casassus, S. Cleary, K. Davies, R. D. Davis, R. J. Hirata, C. M. Watson, R. A. TI Spitzer characterization of dust in an anomalous emission region: the Perseus cloud SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: general; ISM: abundances; dust,extinction; ISM: individual objects: Perseus cloud,IC 348; IC 348; infrared: ISM ID MULTIBAND IMAGING PHOTOMETER; MICROWAVE-ANISOTROPY-PROBE; CENTIMETER-WAVE CONTINUUM; INNER GALACTIC PLANE; INTERSTELLAR DUST; MOLECULAR CLOUD; INFRARED-EMISSION; SPACE-TELESCOPE; MODEL; RADIATION AB Anomalous microwave emission is known to exist in the Perseus cloud. One of the most promising candidates to explain this excess of emission is electric dipole radiation from rapidly rotating very small dust grains, commonly referred to as spinning dust. Photometric data obtained with the Spitzer Space Telescope have been reprocessed and used in conjunction with the dust emission model dustem to characterize the properties of the dust within the cloud. This analysis has allowed us to constrain spatial variations in the strength of the interstellar radiation field (?ISRF), the mass abundances of the polycyclic aromatic hydrocarbons (PAHs) and the very small grains (VSGs) relative to the big grains (YPAH and YVSG), the column density of hydrogen (NH) and the equilibrium dust temperature (Tdust). The parameter maps of YPAH, YVSG and ?ISRF are the first of their kind to be produced for the Perseus cloud, and we used these maps to investigate the physical conditions in which anomalous emission is observed. We find that in regions of anomalous emission the strength of the ISRF, and consequently the equilibrium temperature of the dust, is enhanced while there is no significant variation in the abundances of the PAHs and the VSGs or the column density of hydrogen. We interpret these results as an indication that the enhancement in ?ISRF might be affecting the properties of the small stochastically heated dust grains resulting in an increase in the spinning dust emission observed at 33 GHz. This is the first time that such an investigation has been performed, and we believe that this type of analysis creates a new perspective in the field of anomalous emission studies, and represents a powerful new tool for constraining spinning dust models. C1 [Tibbs, C. T.; Dickinson, C.; Davies, R. D.; Davis, R. J.; Watson, R. A.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Tibbs, C. T.; Flagey, N.; Paladini, R.; Compiegne, M.; Carey, S.; Noriega-Crespo, A.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Flagey, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Shenoy, S.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Ali-Haimoud, Y.; Cleary, K.; Hirata, C. M.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Casassus, S.] Univ Chile, Dept Astron, Santiago, Chile. RP Tibbs, CT (reprint author), Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. EM ctibbs@ipac.caltech.edu RI Casassus, Simon/I-8609-2016; OI Watson, Robert/0000-0002-5873-0124 FU NASA; JPL/Caltech; STFC; ERC IRG; FONDECYT [1100221]; Chilean Center for Astrophysics FONDAP [15010003]; [NASA/ADP ROSES-2009]; [09-ADP09-0059] FX We thank the anonymous referee for their careful reading of this paper and for providing useful comments. This work is based in part on archival data obtained 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 an award issued by JPL/Caltech. This work has been done within the framework of a NASA/ADP ROSES-2009 grant, no. 09-ADP09-0059. CD acknowledges support from an STFC Advanced Fellowship and an ERC IRG grant under the FP7. SC acknowledges support from FONDECYT grant 1100221, and from the Chilean Center for Astrophysics FONDAP 15010003. NR 60 TC 19 Z9 19 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2011 VL 418 IS 3 BP 1889 EP 1900 DI 10.1111/j.1365-2966.2011.19605.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 862JW UT WOS:000298088000033 ER PT J AU Khanzadyan, T Movsessian, TA Davis, CJ Magakian, TY Gredel, R Nikogossian, EH AF Khanzadyan, Tigran Movsessian, Tigran A. Davis, Chris J. Magakian, Tigran Yu. Gredel, Roland Nikogossian, Elena H. TI GM 2-4: a signpost for low- and intermediate-mass star formation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE circumstellar matter; ISM: individual objects: GM 2-4; ISM: jets and outflows; infrared: stars ID YOUNG STELLAR OBJECTS; INFRARED ARRAY CAMERA; HERBIG-HARO OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; MOLECULAR-HYDROGEN EMISSION; ULTRACOMPACT HII-REGIONS; SPITZER-SPACE-TELESCOPE; LUMINOUS IRAS SOURCES; ALL-SKY SURVEY; IMAGING SURVEY AB We present a multi-wavelength study of the region towards the GM 2-4 nebula and the nearby source IRAS 05373+2340. Our near-infrared H2 10 S(1) line observations reveal various shock-excited features which are part of several bipolar outflows. We identify candidates for the driving sources of the outflows from a comparison of the multi-waveband archival data sets and spectral energy distribution (SED) modelling. The SED spectral slope () for all the protostars in the field was then compared with the visual extinction map. This comparison suggests that star formation progresses from north-east to south-west across this region. C1 [Khanzadyan, Tigran] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Khanzadyan, Tigran] Natl Univ Ireland Galway, Dept Expt Phys, Ctr Astron, Galway, Ireland. [Khanzadyan, Tigran; Movsessian, Tigran A.; Magakian, Tigran Yu.; Nikogossian, Elena H.] Byurakan Astrophys Observ, Aragatsotn Reg 378433, Armenia. [Davis, Chris J.] Joint Astron Ctr, Hilo, HI 96720 USA. [Davis, Chris J.] NASA HQ, Div Astrophys, Washington, DC 20546 USA. [Gredel, Roland] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Khanzadyan, T (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM tkhanzadyan@mpifr-bonn.mpg.de FU Science Foundation Ireland (SFI); INTAS [03-51-4838]; ANSEF [PS-astroex 2517]; National Aeronautics and Space Administration; National Science Foundation FX TK acknowledges support of the Science Foundation Ireland (SFI) Research Frontiers award. This work was partly supported by INTAS grant 03-51-4838 and ANSEF grant PS-astroex 2517. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has also made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 39 TC 3 Z9 3 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2011 VL 418 IS 3 BP 1994 EP 2003 DI 10.1111/j.1365-2966.2011.19618.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 862JW UT WOS:000298088000043 ER PT J AU Ballo, L Braito, V Reeves, JN Sambruna, RM Tombesi, F AF Ballo, L. Braito, V. Reeves, J. N. Sambruna, R. M. Tombesi, F. TI The high-energy view of the broad-line radio galaxy 3C 111 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; quasars: individual: 3C 111; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRUM; BLACK-HOLE SPIN; PROBE WMAP OBSERVATIONS; PEAKED EMISSION-LINES; PHOTON IMAGING CAMERA; ULTRA-FAST OUTFLOWS; XMM-NEWTON; BEPPOSAX OBSERVATIONS; LIKELIHOOD RATIO AB We present the analysis of Suzaku and XMMNewton observations of the broad-line radio galaxy (BLRG) 3C 111. Its high-energy emission shows variability, a harder continuum with respect to the radio-quiet active galactic nucleus population, and weak reflection features. Suzaku found the source in a minimum flux level; a comparison with the XMMNewton data implies an increase of a factor of 2.5 in the 0.510 keV flux, in the 6 months separating the two observations. The iron K complex is detected in both data sets, with rather low equivalent width(s). The intensity of the iron K complex does not respond to the change in continuum flux. An ultrafast, high-ionization outflowing gas is clearly detected in the Suzaku/X-ray Imaging Spectrometer data; the absorber is most likely unstable. Indeed, during the XMMNewton observation, which was 6 months after, the absorber was not detected. No clear rollover in the hard X-ray emission is detected, probably due to the emergence of the jet as a dominant component in the hard X-ray band, as suggested by the detection above similar to 100 keV with the GSO onboard Suzaku, although the present data do not allow us to firmly constrain the relative contribution of the different components. The fluxes observed by the ?-ray satellites CGRO and Fermi would be compatible with the putative jet component if peaking at energies E similar to 100 MeV. In the X-ray band, the jet contribution to the continuum starts to be significant only above 10 keV. If the detection of the jet component in 3C 111 is confirmed, then its relative importance in the X-ray energy band could explain the different observed properties in the high-energy emission of BLRGs, which are otherwise similar in their other multiwavelength properties. Comparison between X-ray and ?-ray data taken at different epochs suggests that the strong variability observed for 3C 111 is probably driven by a change in the primary continuum. C1 [Ballo, L.] Inst Fis Cantabria CSIC UC, E-39005 Santander, Spain. [Braito, V.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Reeves, J. N.] Univ Keele, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Sambruna, R. M.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Tombesi, F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Tombesi, F.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Tombesi, F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Ballo, L (reprint author), Inst Fis Cantabria CSIC UC, Avda Los Castros S-N,Edif Juan Jorda, E-39005 Santander, Spain. EM ballo@ifca.unican.es RI XRAY, SUZAKU/A-1808-2009; OI Ballo, Lucia/0000-0002-5036-3497; Braito, Valentina/0000-0002-2629-4989 FU ESA Member States; USA, NASA; NASA; UK STFC research council; Spanish Ministry of Science and Innovation [AYA2009-08059] FX This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center, and from the NASA/IPAC Extragalactic Database which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This study is based on observations obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA(NASA), and XMM-Newton (an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA, NASA). We warmly thank the referee for her/his suggestions that significantly improved this paper. We are grateful to M. Ceballos, R. Saxton and S. Sembay for their help in handling the XMM-Newton data problems. We warmly thank V. Bianchin for reducing the INTEGRAL data. RMS acknowledges support from NASA through the Suzaku programme. VB acknowledges support from the UK STFC research council. LB acknowledges support from the Spanish Ministry of Science and Innovation through a 'Juan de la Cierva' fellowship. Financial support for this work was provided by the Spanish Ministry of Science and Innovation, through research grant AYA2009-08059. NR 84 TC 12 Z9 12 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2011 VL 418 IS 4 BP 2367 EP 2380 DI 10.1111/j.1365-2966.2011.19629.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 862JX UT WOS:000298088100021 ER PT J AU Smith, DJ Griffin, DW McPeters, RD Ward, PD Schuerger, AC AF Smith, David J. Griffin, Dale W. McPeters, Richard D. Ward, Peter D. Schuerger, Andrew C. TI Microbial survival in the stratosphere and implications for global dispersal SO AEROBIOLOGIA LA English DT Article DE Stratosphere; Natural selection; Dispersal; Spores; Aerobiology ID BACILLUS-SUBTILIS SPORES; SOLAR UV-RADIATION; SIMULATED MARTIAN ENVIRONMENTS; ABSORPTION CROSS-SECTIONS; SPACECRAFT SURFACES; BACTERIAL-SPORES; DEINOCOCCUS-RADIODURANS; ULTRAVIOLET-RADIATION; ESCHERICHIA-COLI; DNA-REPAIR AB Spores of Bacillus subtilis were exposed to a series of stratosphere simulations. In total, five distinct treatments measured the effect of reduced pressure, low temperature, high desiccation, and intense ultraviolet (UV) irradiation on stratosphere-isolated and ground-isolated B. subtilis strains. Environmental conditions were based on springtime data from a mid-latitude region of the lower stratosphere (20 km). Experimentally, each treatment consisted of the following independent or combined conditions: -70 degrees C, 56 mb, 10-12% relative humidity and 0.00421, 5.11, and 54.64 W/m(2) of UVC (200-280 nm), UVB 280-315 nm), UVA (315-400 nm), respectively. Bacteria were deposited on metal coupon surfaces in monolayers of similar to 1 x 10(6) spores and prepared with palagonite (particle size < 20 mu m). After 6 h of exposure to the stratosphere environment, 99.9% of B. subtilis spores were killed due to UV irradiation. In contrast, temperature, desiccation, and pressure simulations without UV had no effect on spore viability up through 96 h. There were no differences in survival between the stratosphere-isolated versus ground-isolated B. subtilis strains. Inactivation of most bacteria in our simulation indicates that the stratosphere can be a critical barrier to long-distance microbial dispersal and that survival in the upper atmosphere may be constrained by UV irradiation. C1 [Smith, David J.; Ward, Peter D.] Univ Washington, Dept Biol, Seattle, WA 98195 USA. [Smith, David J.; Ward, Peter D.] Univ Washington, Grad Program Astrobiol, Seattle, WA 98195 USA. [Griffin, Dale W.] US Geol Survey, Tallahassee, FL 32303 USA. [McPeters, Richard D.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20711 USA. [Schuerger, Andrew C.] Univ Florida, Dept Plant Pathol, Space Life Sci Lab, Kennedy Space Ctr, Gainesville, FL 32899 USA. RP Smith, DJ (reprint author), Univ Washington, Dept Biol, 24 Kincaid Hall,Box 351800, Seattle, WA 98195 USA. EM djsone@uw.edu; dgriffin@usgs.gov; richard.d.mcpeters@nasa.gov; argo@uw.edu; schuerg@ufl.edu RI McPeters, Richard/G-4955-2013 OI McPeters, Richard/0000-0002-8926-8462 FU National Science Foundation Integrative Graduate Education and Research Traineeship (IGERT) at the University of Washington Graduate Program in Astrobiology; NASA Kennedy Space Center (KSC) FX Our research was supported by the National Science Foundation Integrative Graduate Education and Research Traineeship (IGERT) program at the University of Washington Graduate Program in Astrobiology, and the Cooperative Education Program at NASA Kennedy Space Center (KSC). Critical resources came from the U. S. Geological Survey (USGS), NASA Goddard Space Flight Center and the University of Florida. The authors are grateful to Paul Hintze (NASA KSC) for his assistance with SEM imaging and energy-dispersive X-ray spectrometry and to Phillip Metzger and Luke Roberson (NASA KSC) who helped generate the dust analog. We also acknowledge John Frederick (University of Chicago) for guidance during our research. Any use of trade names is for descriptive purposes only and does not imply endorsement by the US Government. NR 67 TC 20 Z9 20 U1 0 U2 25 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0393-5965 EI 1573-3025 J9 AEROBIOLOGIA JI Aerobiologia PD DEC PY 2011 VL 27 IS 4 BP 319 EP 332 DI 10.1007/s10453-011-9203-5 PG 14 WC Biology; Environmental Sciences SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology GA 876IO UT WOS:000299101400005 ER PT J AU Campbell, JF Flood, MA Prasad, NS Hodson, WD AF Campbell, Joel F. Flood, Michael A. Prasad, Narasimha S. Hodson, Wade D. TI A low cost remote sensing system using PC and stereo equipment SO AMERICAN JOURNAL OF PHYSICS LA English DT Article ID MODULATION CW LIDAR; SEQUENCES AB A system using a personal computer, speaker, and a microphone is used to detect objects, and make crude measurements using a carrier modulated by a pseudorandom noise (PN) code. This system can be constructed using a personal computer and audio equipment commonly found in the laboratory or at home, or more sophisticated equipment that can be purchased at a reasonable cost. We demonstrate its value as an instructional tool for teaching concepts of remote sensing and digital signal processing. [DOI: 10.1119/1.3643704] C1 [Campbell, Joel F.; Flood, Michael A.; Prasad, Narasimha S.; Hodson, Wade D.] NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Campbell, JF (reprint author), NASA Langley Res Ctr, MS 488, Hampton, VA 23681 USA. EM joel.f.campbell@nasa.gov NR 9 TC 4 Z9 4 U1 0 U2 3 PU AMER ASSOC PHYSICS TEACHERS AMER INST PHYSICS PI MELVILLE PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA SN 0002-9505 J9 AM J PHYS JI Am. J. Phys. PD DEC PY 2011 VL 79 IS 12 BP 1240 EP 1245 DI 10.1119/1.3643704 PG 6 WC Education, Scientific Disciplines; Physics, Multidisciplinary SC Education & Educational Research; Physics GA 860GR UT WOS:000297937300006 ER PT J AU Aatrokoski, J Ade, PAR Aghanim, N Aller, HD Aller, MF Angelakis, E Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Berdyugin, A Bernard, JP Bersanelli, M Bhatia, R Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bucher, M Burigana, C Burrows, DN Cabella, P Capalbi, M Cappellini, B Cardoso, JF Catalano, A Cavazzuti, E Cayon, L Challinor, A Chamballu, A Chary, RR Chiang, LY Christensen, PR Clements, DL Colafrancesco, S Colombi, S Couchot, F Coulais, A Cutini, S Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Dickinson, C Dole, H Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Finelli, F Forni, O Frailis, M Franceschi, E Fuhrmann, L Galeotta, S Ganga, K Gargano, F Gasparrini, D Gehrels, N Giard, M Giardino, G Giglietto, N Giommi, P Giordano, F Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Harrison, D Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Jaffe, AH Juvela, M Keihanen, E Keskitalo, R King, O Kisner, TS Kneissl, R Knox, L Krichbaum, TP Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lavonen, N Lawrence, CR Leach, S Leonardi, R Leon-Tavares, J Linden-Vornle, M Lindfors, E Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Mann, R Maris, M Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Max-Moerbeck, W Mazziotta, MN Mazzotta, P Melchiorri, A Mendes, L Mennella, A Michelson, PF Mingaliev, M Mitra, S Miville-Deschenes, MA Moneti, A Monte, C Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Natoli, P Nestoras, I Netterfield, CB Nieppola, E Nilsson, K Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I O'Dwyer, IJ Osborne, S Pajot, F Partridge, B Pasian, F Patanchon, G Pavlidou, V Pearson, TJ Perdereau, O Perotto, L Perri, M Perrotta, F Piacentini, F Piat, M Plaszczynski, S Platania, P Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Prezeau, G Procopio, P Prunet, S Puget, JL Rachen, JP Raino, S Reach, WT Readhead, A Rebolo, R Reeves, R Reinecke, M Reinthal, R Renault, C Ricciardi, S Richards, J Riller, T Riquelme, D Ristorcelli, I Rocha, G Rosset, C Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Saarinen, J Sandri, M Savolainen, P Scott, D Seiffert, MD Sievers, A Sillanpaa, A Smoot, GF Sotnikova, Y Starck, JL Stevenson, M Stivoli, F Stolyarov, V Sudiwala, R Sygnet, JF Takalo, L Tammi, J Tauber, JA Terenzi, L Thompson, DJ Toffolatti, L Tomasi, M Tornikoski, M Torre, JP Tosti, G Tramacere, A Tristram, M Tuovinen, J Turler, M Turunen, M Umana, G Ungerechts, H Valenziano, L Valtaoja, E Varis, J Verrecchia, F Vielva, P Villa, F Vittorio, N Wandelt, BD Wu, J Yvon, D Zacchei, A Zensus, JA Zhou, X Zonca, A AF Aatrokoski, J. Ade, P. A. R. Aghanim, N. Aller, H. D. Aller, M. F. Angelakis, E. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Berdyugin, A. Bernard, J. -P. Bersanelli, M. Bhatia, R. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bucher, M. Burigana, C. Burrows, D. N. Cabella, P. Capalbi, M. Cappellini, B. Cardoso, J. -F. Catalano, A. Cavazzuti, E. Cayon, L. Challinor, A. Chamballu, A. Chary, R. -R. Chiang, L. -Y Christensen, P. R. Clements, D. L. Colafrancesco, S. Colombi, S. Couchot, F. Coulais, A. Cutini, S. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Dickinson, C. Dole, H. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Fuhrmann, L. Galeotta, S. Ganga, K. Gargano, F. Gasparrini, D. Gehrels, N. Giard, M. Giardino, G. Giglietto, N. Giommi, P. Giordano, F. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Harrison, D. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Jaffe, A. H. Juvela, M. Keihanen, E. Keskitalo, R. King, O. Kisner, T. S. Kneissl, R. Knox, L. Krichbaum, T. P. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lavonen, N. Lawrence, C. R. Leach, S. Leonardi, R. Leon-Tavares, J. Linden-Vornle, M. Lindfors, E. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Mann, R. Maris, M. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Max-Moerbeck, W. Mazziotta, M. N. Mazzotta, P. Melchiorri, A. Mendes, L. Mennella, A. Michelson, P. F. Mingaliev, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Monte, C. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Natoli, P. Nestoras, I. Netterfield, C. B. Nieppola, E. Nilsson, K. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. O'Dwyer, I. J. Osborne, S. Pajot, F. Partridge, B. Pasian, F. Patanchon, G. Pavlidou, V. Pearson, T. J. Perdereau, O. Perotto, L. Perri, M. Perrotta, F. Piacentini, F. Piat, M. Plaszczynski, S. Platania, P. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Prezeau, G. Procopio, P. Prunet, S. Puget, J. -L. Rachen, J. P. Raino, S. Reach, W. T. Readhead, A. Rebolo, R. Reeves, R. Reinecke, M. Reinthal, R. Renault, C. Ricciardi, S. Richards, J. Riller, T. Riquelme, D. Ristorcelli, I. Rocha, G. Rosset, C. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Saarinen, J. Sandri, M. Savolainen, P. Scott, D. Seiffert, M. D. Sievers, A. Sillanpaa, A. Smoot, G. F. Sotnikova, Y. Starck, J. -L. Stevenson, M. Stivoli, F. Stolyarov, V. Sudiwala, R. Sygnet, J. -F. Takalo, L. Tammi, J. Tauber, J. A. Terenzi, L. Thompson, D. J. Toffolatti, L. Tomasi, M. Tornikoski, M. Torre, J. -P. Tosti, G. Tramacere, A. Tristram, M. Tuovinen, J. Turler, M. Turunen, M. Umana, G. Ungerechts, H. Valenziano, L. Valtaoja, E. Varis, J. Verrecchia, F. Vielva, P. Villa, F. Vittorio, N. Wandelt, B. D. Wu, J. Yvon, D. Zacchei, A. Zensus, J. A. Zhou, X. Zonca, A. CA Planck Collaboration TI Planck early results. XV. Spectral energy distributions and radio continuum spectra of northern extragalactic radio sources SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; BL Lacertae objects: general; quasars: general; radiation mechanisms: non-thermal ID BL-LACERTAE OBJECTS; LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; GAMMA-RAY EMISSION; PRE-LAUNCH STATUS; SHOCKED RELATIVISTIC JETS; BURST ALERT TELESCOPE; PARTICLE-ACCELERATION; BLAZAR SEQUENCE; INTERSTELLAR EXTINCTION AB Spectral energy distributions (SEDs) and radio continuum spectra are presented for a northern sample of 104 extragalactic radio sources, based on the Planck Early Release Compact Source Catalogue (ERCSC) and simultaneous multifrequency data. The nine Planck frequencies, from 30 to 857 GHz, are complemented by a set of simultaneous observations ranging from radio to gamma-rays. This is the first extensive frequency coverage in the radio and millimetre domains for an essentially complete sample of extragalactic radio sources, and it shows how the individual shocks, each in their own phase of development, shape the radio spectra as they move in the relativistic jet. The SEDs presented in this paper were fitted with second and third degree polynomials to estimate the frequencies of the synchrotron and inverse Compton (IC) peaks, and the spectral indices of low and high frequency radio data, including the Planck ERCSC data, were calculated. SED modelling methods are discussed, with an emphasis on proper, physical modelling of the synchrotron bump using multiple components. Planck ERCSC data also suggest that the original accelerated electron energy spectrum could be much harder than commonly thought, with power-law index around 1.5 instead of the canonical 2.5. The implications of this are discussed for the acceleration mechanisms effective in blazar shocks. Furthermore in many cases the Planck data indicate that gamma-ray emission must originate in the same shocks that produce the radio emission. C1 [Aatrokoski, J.; Lahteenmaki, A.; Lavonen, N.; Leon-Tavares, J.; Nieppola, E.; Poutanen, T.; Savolainen, P.; Tammi, J.; Tornikoski, M.; Turunen, M.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Capalbi, M.; Cavazzuti, E.; Cutini, S.; Gasparrini, D.; Natoli, P.; Perri, M.; Polenta, G.; Verrecchia, F.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Giommi, P.] Agenzia Spaziale Italiana, Rome, Italy. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Gehrels, N.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.] Univ Paris 07, CNRS, UMR7164, Paris, France. [Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago 0355, Chile. [Bonavera, L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Bond, J. R.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse 4, France. [Chary, R. -R.; Ganga, K.; Pearson, T. J.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Challinor, A.] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England. [Starck, J. -L.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Juvela, M.; Keihanen, E.; Keskitalo, R.; Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Smoot, G. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Leonardi, R.; Lubin, P. M.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Giglietto, N.; Giordano, F.; Monte, C.; Raino, S.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Giglietto, N.; Giordano, F.; Monte, C.; Raino, S.] Politecn Bari, I-70126 Bari, Italy. [Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy. [Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Balbi, A.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Kneissl, R.] ESO Vitacura, European So Observ, Santiago, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] Planck Sci Off, ESAC, European Space Agcy, Madrid, Spain. [Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] Estec, European Space Agcy, NL-2201 AZ Noordwijk, Netherlands. [Nieppola, E.; Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio 21500, Finland. [Partridge, B.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA. [Kurki-Suonio, H.; Lahteenmaki, A.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland. [Umana, G.] INAF Osservatorio Astrofis Catania, Catania, Italy. [Bonaldi, A.; de Zotti, G.; Massardi, M.] INAF Osservatorio Astron Padova, Padua, Italy. [Colafrancesco, S.; Polenta, G.] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] INAF Osservatorio Astron Trieste, Trieste, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Procopio, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Bologna, Italy. [Bersanelli, M.; Cappellini, B.; Donzelli, S.; Maino, D.; Tomasi, M.] INAF IASF Milano, Milan, Italy. [Stivoli, F.] Univ Paris 11, INRIA, Lab Rech Informat, F-91405 Orsay, France. [Tramacere, A.; Turler, M.] Univ Geneva, ISDC Data Ctr Astrophys, Versoix, Switzerland. [Chamballu, A.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France. 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RP Lahteenmaki, A (reprint author), Aalto Univ, Metsahovi Radio Observ, Metsahovintie 114, Kylmala 02540, Finland. EM alien@kurp.hut.fi RI Mazziotta, Mario /O-8867-2015; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; bonavera, laura/E-9368-2017; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Pavlidou, Vasiliki/C-2944-2011; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Pearson, Timothy/N-2376-2015; Gruppuso, Alessandro/N-5592-2015; Gargano, Fabio/O-8934-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; de Gasperis, Giancarlo/C-8534-2012; Thompson, David/D-2939-2012; Gehrels, Neil/D-2971-2012; giglietto, nicola/I-8951-2012; Gregorio, Anna/J-1632-2012; Tosti, Gino/E-9976-2013; Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Lahteenmaki, Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Reeves, Rodrigo/H-2812-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; OI Tramacere, Andrea/0000-0002-8186-3793; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Galeotta, Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Angelakis, Emmanouil/0000-0001-7327-5441; Reach, William/0000-0001-8362-4094; Cutini, Sara/0000-0002-1271-2924; Gasparrini, Dario/0000-0002-5064-9495; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Perri, Matteo/0000-0003-3613-4409; Mazziotta, Mario /0000-0001-9325-4672; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; bonavera, laura/0000-0001-8039-3876; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; Melchiorri, Alessandro/0000-0001-5326-6003; Barreiro, Rita Belen/0000-0002-6139-4272; Pavlidou, Vasiliki/0000-0002-0870-1368; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Pearson, Timothy/0000-0001-5213-6231; Gruppuso, Alessandro/0000-0001-9272-5292; Gargano, Fabio/0000-0002-5055-6395; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; de Gasperis, Giancarlo/0000-0003-2899-2171; Thompson, David/0000-0001-5217-9135; giglietto, nicola/0000-0002-9021-2888; Vielva, Patricio/0000-0003-0051-272X; Reeves, Rodrigo/0000-0001-5704-271X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; giommi, paolo/0000-0002-2265-5003; Matarrese, Sabino/0000-0002-2573-1243; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Verrecchia, Francesco/0000-0003-3455-5082; Gregorio, Anna/0000-0003-4028-8785; de Bernardis, Paolo/0000-0001-6547-6446; Giordano, Francesco/0000-0002-8651-2394; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104 FU ESA; CNES; CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy); NASA; DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU); Academy of Finland [212656, 210338, 121148, 127740, 122352]; NSF; University of Michigan; Chinese National Natural Science Foundation [10633020, 10778714, 11073032]; National Basic Research Program of China (973 Program) [2007CB815403]; Commonwealth of Australia; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found via http://www.rssd.esa.int/Planck. The Mets hovi and Tuorla observing projects are supported by the Academy of Finland (grant numbers 212656, 210338, 121148, 127740 and 122352). UMRAO is supported by a series of grants from the NSF and NASA, and by the University of Michigan. This publication is partly 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. This research is partly based on observations with the 100-m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg, the IRAM 30-m telescope, and the Medicina (Noto) telescope operated by INAF - Istituto di Radioastronomia. This paper makes use of observations obtained at the Very Large Array (VLA) which is an instrument of the National Radio Astronomy Observatory (NRAO). The NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The observations at Xinglong station are supported by the Chinese National Natural Science Foundation grants 10633020, 10778714, and 11073032, and by the National Basic Research Program of China (973 Program) No. 2007CB815403. The OVRO 40-m monitoring program is supported in part by NASA. The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. Part of this work is based on archival data, software or on-line services provided by the ASI Science Data Center ASDC. We thank the Fermi LAT team reviewers, S. Ciprini and M. Giroletti, for their effort and valuable comments. NR 122 TC 69 Z9 69 U1 0 U2 14 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A15 DI 10.1051/0004-6361/201116466 PG 56 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100016 ER PT J AU Abergel, A Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Cabella, P Cardoso, JF Catalano, A Cayon, L Challinor, A Chamballu, A Chiang, LY Chiang, C Christensen, PR Clements, DL Colombi, S Couchot, F Coulais, A Crill, BP Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dickinson, C Dobashi, K Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Guillet, V Hansen, FK Harrison, D Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Jaffe, AH Jones, A Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leonardi, R Leroy, C Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Maffei, B Mandolesi, N Mann, R Maris, M Marshall, DJ Martin, P Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, P McGehee, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Pajot, F Paladini, R Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Prezeau, G Prunet, S Puget, JL Reach, WT Rebolo, R Reinecke, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, P Smoot, GF Starck, JL Stivoli, F Stolyarov, V Sudiwala, R Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Tristram, M Tuovinen, J Umana, G Valenziano, L Verstraete, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Yvon, D Zacchei, A Zonca, A AF Abergel, A. Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bhatia, R. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Cabella, P. Cardoso, J. -F. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chiang, L. -Y. Chiang, C. Christensen, P. R. Clements, D. L. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dickinson, C. Dobashi, K. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Guillet, V. Hansen, F. K. Harrison, D. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Jaffe, A. H. Jones, A. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leonardi, R. Leroy, C. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Mandolesi, N. Mann, R. Maris, M. Marshall, D. J. Martin, P. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. McGehee, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Pajot, F. Paladini, R. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Prezeau, G. Prunet, S. Puget, J. -L. Reach, W. T. Rebolo, R. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, P. Smoot, G. F. Starck, J. -L. Stivoli, F. Stolyarov, V. Sudiwala, R. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J. -P. Tristram, M. Tuovinen, J. Umana, G. Valenziano, L. Verstraete, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. XXV. Thermal dust in nearby molecular clouds SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE dust, extinction; ISM: structure; evolution; infrared: ISM; ISM: individual objects: Taurus-Auriga molecular cloud ID PRE-LAUNCH STATUS; OPTICAL-PROPERTIES; INTERSTELLAR DUST; SPECTRAL INDEX; TEMPERATURE-DEPENDENCE; INFRARED OBSERVATIONS; PHYSICAL-PROPERTIES; INITIAL HIGHLIGHTS; GALACTIC PLANE; COLD DUST AB Planck allows unbiased mapping of Galactic sub-millimetre and millimetre emission from the most diffuse regions to the densest parts of molecular clouds. We present an early analysis of the Taurus molecular complex, on line-of-sight-averaged data and without component separation. The emission spectrum measured by Planck and IRAS can be fitted pixel by pixel using a single modified blackbody. Some systematic residuals are detected at 353 GHz and 143 GHz, with amplitudes around -7% and +13%, respectively, indicating that the measured spectra are likely more complex than a simple modified blackbody. Significant positive residuals are also detected in the molecular regions and in the 217 GHz and 100 GHz bands, mainly caused by the contribution of the J = 2 -> 1 and J = 1 -> 0 (CO)-C-12 and (CO)-C-13 emission lines. We derive maps of the dust temperature T, the dust spectral emissivity index beta, and the dust optical depth at 250 mu m tau(250). The temperature map illustrates the cooling of the dust particles in thermal equilibrium with the incident radiation field, from 16-17 K in the diffuse regions to 13-14 K in the dense parts. The distribution of spectral indices is centred at 1.78, with a standard deviation of 0.08 and a systematic error of 0.07. We detect a significant T - beta anti-correlation. The dust optical depth map reveals the spatial distribution of the column density of the molecular complex from the densest molecular regions to the faint diffuse regions. We use near-infrared extinction and Hi data at 21-cm to perform a quantitative analysis of the spatial variations of the measured dust optical depth at 250 mu m per hydrogen atom tau(250)/N-H. We report an increase of tau(250)/N-H by a factor of about 2 between the atomic phase and the molecular phase, which has a strong impact on the equilibrium temperature of the dust particles. C1 [Abergel, A.; Aghanim, N.; Aumont, J.; Boulanger, F.; Douspis, M.; Guillet, V.; Jones, A.; Lagache, G.; Leroy, C.; Miville-Deschenes, M. -A.; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Torre, J. -P.; Verstraete, L.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France. [Poutanen, T.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.] Univ Paris 07, CNRS, UMR 7164, Paris, France. [Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile. [Bond, J. R.; Martin, P.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse 4, France. [Ganga, K.; McGehee, P.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Challinor, A.; Shellard, P.] Univ Cambridge, Ctr Math Sci, DAMTP, Cambridge CB3 0WA, England. [Starck, J. -L.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. [Dobashi, K.] Tokyo Gakugei Univ, Dept Astron & Earth Sci, Tokyo 1848501, Japan. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Juvela, M.; Keihanen, E.; Keskitalo, R.; Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Chiang, C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Smoot, G. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Leonardi, R.; Lubin, P. M.; Meinhold, P. R.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA. [Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy. [Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Balbi, A.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rebolo, R.; Rubino-Martin, J. A.] ULL, Dpto Astrofis, Tenerife 38206, Spain. [Kneissl, R.] European So Observ, ESO Vitacura, Santiago 19, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain. [Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands. [Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland. [Umana, G.] INAF Osservatorio Astrofis Catania, Catania, Italy. [Bonaldi, A.; de Zotti, G.] INAF Osservatorio Astron Padova, Padua, Italy. [Polenta, G.] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] INAF Osservatorio Astron Trieste, Trieste, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Tomasi, M.] INAF IASF Milano, Milan, Italy. [Stivoli, F.] Univ Paris 11, INRIA, Lab Rech Informat, F-91405 Orsay, France. [Desert, F. -X.] Univ Grenoble 1, CNRS, IPAG, INSU,UMR 5274, F-38041 Grenoble, France. [Chamballu, A.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France. [Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Univ Paris 06, CNRS, Inst Astrophys Spatiale, UMR8617, Paris, France. [Chiang, L. -Y.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Donzelli, S.; Eriksen, H. K.; Hansen, F. K.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Hildebrandt, S. R.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; Mitra, S.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Davies, R. D.; Davis, R. J.; Dickinson, C.; Maffei, B.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Catalano, A.; Coulais, A.; Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Arnaud, M.; Starck, J. -L.] IRFU Serv Astrophys CEA DSM CNRS Univ Paris Dider, CEA Saclay, Lab AIM, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, UMR 5141, Lab Traitement & Commun Informat, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Inst Natl Polytech Grenoble, CNRS, Lab Phys Subatom & Cosmol,IN2P3, F-38026 Grenoble, France. [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS, IN2P3, Lab Accelerateur Lineaire, F-91405 Orsay, France. [Borrill, J.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Banday, A. J.; Doerl, U.; Ensslin, T. A.; Hovest, W.; Matthai, F.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Tuovinen, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland. [Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Mann, R.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Paladini, R.] Spitzer Sci Ctr, Pasadena, CA USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Abergel, A (reprint author), Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, Batiment 121, F-91405 Orsay, France. EM alain.abergel@ias.u-psud.fr RI Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; OI Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Ricciardi, Sara/0000-0002-3807-4043; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; de Gasperis, Giancarlo/0000-0003-2899-2171; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272; Hivon, Eric/0000-0003-1880-2733; Savini, Giorgio/0000-0003-4449-9416; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Zacchei, Andrea/0000-0003-0396-1192 NR 89 TC 102 Z9 102 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A25 DI 10.1051/0004-6361/201116483 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100026 ER PT J AU Abergel, A Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Cabella, P Cardoso, JF Catalano, A Cayon, L Challinor, A Chamballu, A Chiang, LY Chiang, C Christensen, PR Colombi, S Couchot, F Coulais, A Crill, BP Cuttaia, F Dame, TM Danese, L Davies, RD Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dickinson, C Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Grenier, IA Gruppuso, A Hansen, FK Harrison, D Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Jaffe, TR Jaffe, AH Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leonardi, R Leroy, C Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Maffei, B Mandolesi, N Mann, R Maris, M Marshall, DJ Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, P McGehee, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Pajot, F Paladini, R Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reich, W Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, P Smoot, GF Starck, JL Stivoli, F Stolyarov, V Stompor, R Sudiwala, R Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Tristram, M Tuovinen, J Umana, G Valenziano, L Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Wilkinson, A Ysard, N Yvon, D Zacchei, A Zonca, A AF Abergel, A. Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J-P Bersanelli, M. Bhatia, R. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Cabella, P. Cardoso, J-F Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chiang, L-Y Chiang, C. Christensen, P. R. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Cuttaia, F. Dame, T. M. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J-M Desert, F-X Dickinson, C. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Grenier, I. A. Gruppuso, A. Hansen, F. K. Harrison, D. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Jaffe, T. R. Jaffe, A. H. Jones, W. C. Juvela, M. Keihaenen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J-M Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leonardi, R. Leroy, C. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Mandolesi, N. Mann, R. Maris, M. Marshall, D. J. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. McGehee, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Miville-Deschenes, M-A Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Pajot, F. Paladini, R. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Prezeau, G. Prunet, S. Puget, J-L Rachen, J. P. Reach, W. T. Rebolo, R. Reich, W. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, P. Smoot, G. F. Starck, J-L Stivoli, F. Stolyarov, V. Stompor, R. Sudiwala, R. Sygnet, J-F Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J-P Tristram, M. Tuovinen, J. Umana, G. Valenziano, L. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Wilkinson, A. Ysard, N. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. XXI. Properties of the interstellar medium in the Galactic plane SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: general; Galaxy: general; radio continuum: ISM; submillimeter: ISM; infrared: ISM; radiation mechanisms: general ID MICROWAVE-ANISOTROPY-PROBE; SPINNING DUST EMISSION; GAMMA-RAY EMISSION; MILKY-WAY; FOREGROUND EMISSION; INFRARED-EMISSION; WMAP OBSERVATIONS; MOLECULAR CLOUDS; EXCESS EMISSION; HII-REGIONS AB Planck has observed the entire sky from 30 GHz to 857 GHz. The observed foreground emission contains contributions from different phases of the interstellar medium (ISM). We have separated the observed Galactic emission into the different gaseous components (atomic, molecular and ionised) in each of a number of Galactocentric rings. This technique provides the necessary information to study dust properties (emissivity, temperature, etc.), as well as other emission mechanisms as a function of Galactic radius. Templates are created for various Galactocentric radii using velocity information from atomic (neutral hydrogen) and molecular ((CO)-C-12) observations. The ionised template is assumed to be traced by free-free emission as observed by WMAP, while 408 MHz emission is used to trace the synchrotron component. Gas emission not traced by the above templates, namely "dark gas", as evidenced using Planck data, is included as an additional template, the first time such a component has been used in this way. These templates are then correlated with each of the Planck frequency bands, as well as with higher frequency data from IRAS and DIRBE along with radio data at 1.4 GHz. The emission per column density of the gas templates allows us to create distinct spectral energy distributions (SEDs) per Galactocentric ring and in each of the gaseous tracers from 1.4 GHz to 25 THz (12 mu m). The resulting SEDs allow us to explore the contribution of various emission mechanisms to the Planck signal. Apart from the thermal dust and free-free emission, we have probed the Galaxy for anomalous (e.g., spinning) dust as well as synchrotron emission. We find the dust opacity in the solar neighbourhood, tau/N-H = 0.92 +/- 0.05x10(-25) cm(2) at 250 mu m, with no significant variation with Galactic radius, even though the dust temperature is seen to vary from over 25 K to under 14 K. Furthermore, we show that anomalous dust emission is present in the atomic, molecular and dark gas phases throughout the Galactic disk. Anomalous emission is not clearly detected in the ionised phase, as free-free emission is seen to dominate. The derived dust propeties associated with the dark gas phase are derived but do not allow us to reveal the nature of this phase. For all environments, the anomalous emission is consistent with rotation from polycyclic aromatic hydrocarbons (PAHs) and, according to our simple model, accounts for (25 +/- 5)% (statistical) of the total emission at 30 GHz. C1 [Banday, A. J.; Bernard, J-P; Forni, O.; Giard, M.; Jaffe, T. R.; Leroy, C.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP IRAP, F-31028 Toulouse 4, France. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, ESRIN, Frascati, Italy. [Bartlett, J. G.; Bucher, M.; Cardoso, J-F; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.; Stompor, R.] Univ Paris 07, CNRS, UMR7164, Paris, France. [Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Astrophys Grp, Cavendish Lab, Cambridge CB3 0HE, England. [Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile. [Bond, J. R.; Miville-Deschenes, M-A] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J-P; Forni, O.; Giard, M.; Jaffe, T. R.; Leroy, C.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse 4, France. [Lilje, P. B.] Univ Oslo, Ctr Math Applicat, Oslo, Norway. [Challinor, A.; Shellard, P.] Univ Cambridge, Ctr Math Sci, DAMTP, Cambridge CB3 0WA, England. [Starck, J-L; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Juvela, M.; Keihaenen, E.; Keskitalo, R.; Kurki-Suonio, H.; Poutanen, T.; Ysard, N.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Chiang, C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Smoot, G. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Leonardi, R.; Lubin, P. M.; Meinhold, P. R.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA. [Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy. [Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Balbi, A.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Kneissl, R.] European So Observ, ESO Vitacura, Santiago 19, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Sci Off, Madrid, Spain. [Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands. [Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kurki-Suonio, H.; Lahteenmaki, A.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland. [Umana, G.] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy. [Bonaldi, A.; de Zotti, G.] Osserv Astron Padova, INAF, Padua, Italy. [Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Tomasi, M.] INAF IASF Milano, Milan, Italy. [Stivoli, F.] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France. [Desert, F-X] Univ Grenoble 1, IPAG, CNRS INSU, UMR 5274, F-38041 Grenoble, France. [Chamballu, A.; Jaffe, A. H.; Mortlock, D.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Ganga, K.; McGehee, P.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, Inst Neel, CNRS, F-38041 Grenoble, France. [Abergel, A.; Aghanim, N.; Aumont, J.; Boulanger, F.; Douspis, M.; Lagache, G.; Leroy, C.; Miville-Deschenes, M-A; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J-L; Torre, J-P] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR8617, F-91405 Orsay, France. [Benabed, K.; Bouchet, F. R.; Cardoso, J-F; Colombi, S.; Delouis, J-M; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J-F; Wandelt, B. D.] Univ Paris 06, Inst Astrophys Paris, CNRS UMR7095, Paris, France. [Chiang, L-Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Donzelli, S.; Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Hildebrandt, S. R.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Davies, R. D.; Davis, R. J.; Dickinson, C.; Maffei, B.; Wilkinson, A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Catalano, A.; Coulais, A.; Lamarre, J-M] Observ Paris, LERMA, CNRS, F-75014 Paris, France. [Arnaud, M.; Grenier, I. A.; Starck, J-L] Univ Paris Diderot, Lab AIM, IRFU Serv Astrophys, CEA DSM,CNRS,CEA Saclay, F-91191 Gif Sur Yvette, France. [Cardoso, J-F] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France. [Cardoso, J-F] Telecom ParisTech, F-75634 Paris 13, France. [Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, CNRS IN2P3, Inst Natl Polytech Grenoble, F-38026 Grenoble, France. [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, Lab Accelerateur Lineaire, CNRS IN2P3, F-91405 Orsay, France. [Borrill, J.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Banday, A. J.; Doerl, U.; Ensslin, T. A.; Hovest, W.; Matthai, F.; Rachen, J. P.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Reich, W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland. [Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Mann, R.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Paladini, R.] Spitzer Sci Ctr, Pasadena, CA USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Marshall, DJ (reprint author), Univ Toulouse, UPS OMP IRAP, F-31028 Toulouse 4, France. EM douglas.marshall@irap.omp.eu RI Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; Gregorio, Anna/J-1632-2012; Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Lahteenmaki, Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Lilje, Per/A-2699-2012; de Gasperis, Giancarlo/C-8534-2012 OI Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Pasian, Fabio/0000-0002-4869-3227; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Masi, Silvia/0000-0001-5105-1439; Melchiorri, Alessandro/0000-0001-5326-6003; Reach, William/0000-0001-8362-4094; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Savini, Giorgio/0000-0003-4449-9416; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; de Gasperis, Giancarlo/0000-0003-2899-2171 NR 89 TC 76 Z9 76 U1 0 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A21 DI 10.1051/0004-6361/201116455 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100022 ER PT J AU Abergel, A Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Blagrave, K Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Cabella, P Cantalupo, CM Cardoso, JF Catalano, A Cayon, L Challinor, A Chamballu, A Chiang, LY Chiang, C Christensen, PR Clements, DL Colombi, S Couchot, F Coulais, A Crill, BP Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dickinson, C Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Harrison, D Helou, G Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Jaffe, AH Joncas, G Jones, A Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leonardi, R Leroy, C Linden-Vornle, M Lockman, FJ Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Maffei, B Maino, D Mandolesi, N Mann, R Maris, M Marshall, DJ Martin, P Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, P McGehee, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I O'Dwyer, IJ Osborne, S Pajot, F Paladini, R Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Goncalves, DP Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Reinecke, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, P Smoot, GF Starck, JL Stivoli, F Stolyarov, V Stompor, R Sudiwala, R Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Tristram, M Tuovinen, J Umana, G Valenziano, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Wilkinson, A Yvon, D Zacchei, A Zonca, A AF Abergel, A. Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bhatia, R. Blagrave, K. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Cabella, P. Cantalupo, C. M. Cardoso, J. -F. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chiang, L. -Y Chiang, C. Christensen, P. R. Clements, D. L. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dickinson, C. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Harrison, D. Helou, G. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Jaffe, A. H. Joncas, G. Jones, A. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leonardi, R. Leroy, C. Linden-Vornle, M. Lockman, F. J. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Maino, D. Mandolesi, N. Mann, R. Maris, M. Marshall, D. J. Martin, P. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. McGehee, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. O'Dwyer, I. J. Osborne, S. Pajot, F. Paladini, R. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Goncalves, D. Pinheiro Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, P. Smoot, G. F. Starck, J. -L. Stivoli, F. Stolyarov, V. Stompor, R. Sudiwala, R. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J. -P. Tristram, M. Tuovinen, J. Umana, G. Valenziano, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Wilkinson, A. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. XXIV. Dust in the diffuse interstellar medium and the Galactic halo SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE infrared: ISM; methods: data analysis; dust, extinction; submillimeter: ISM; Galaxy: halo; local insterstellar matter ID HIGH-VELOCITY CLOUD; ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; HUBBLE-SPACE-TELESCOPE; MOLECULAR-HYDROGEN; MILKY-WAY; CIRRUS CLOUDS; COMPLEX-C; H-I; INFRARED-EMISSION; LOW-METALLICITY AB This paper presents the first results from a comparison of Planck dust maps at 353, 545 and 857 GHz, along with IRAS data at 3000 9100 mu m) and 5000 GHz 960 mu m), with Green Bank Telescope 21-cm observations of H I in 14 fields covering more than 800 deg(2) at high Galactic latitude. The main goal of this study is to estimate the far-infrared to sub-millimeter (submm) emissivity of dust in the diffuse local interstellar medium (ISM) and in the intermediate-velocity (IVC) and high-velocity clouds (HVC) of the Galactic halo. Galactic dust emission for fields with average H I column density lower than 2 x 10(20) cm(-2) is well correlated with 21-cm emission because in such diffuse areas the hydrogen is predominantly in the neutral atomic phase. The residual emission in these fields, once the H I-correlated emission is removed, is consistent with the expected statistical properties of the cosmic infrared background fluctuations. The brighter fields in our sample, with an average H I column density greater than 2 x 10(20) cm(-2), show significant excess dust emission compared to the H I column density. Regions of excess lie in organized structures that suggest the presence of hydrogen in molecular form, though they are not always correlated with CO emission. In the higher H I column density fields the excess emission at 857 GHz is about 40% of that coming from the H I, but over all the high latitude fields surveyed the molecular mass faction is about 10%. Dust emission from IVCs is detected with high significance by this correlation analysis. Its spectral properties are consistent with, compared to the local ISM values, significantly hotter dust (T similar to 20K), lower submm dust opacity normalized per H-atom, and a relative abundance of very small grains to large grains about four times higher. These results are compatible with expectations for clouds that are part of the Galactic fountain in which there is dust shattering and fragmentation. Correlated dust emission in HVCs is not detected; the average of the 99.9% confidence upper limits to the emissivity is 0.15 times the local ISM value at 857 and 3000 GHz, in accordance with gas phase evidence for lower metallicity and depletion in these clouds. Unexpected anti-correlated variations of the dust temperature and emission cross-section per H atom are identified in the local ISM and IVCs, a trend that continues into molecular environments. This suggests that dust growth through aggregation, seen in molecular clouds, is active much earlier in the cloud condensation and star formation processes. C1 [Abergel, A.; Aghanim, N.; Aumont, J.; Boulanger, F.; Douspis, M.; Jones, A.; Lagache, G.; Leroy, C.; Miville-Deschenes, M. -A.; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Torre, J. -P.] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France. [Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.; Stompor, R.] Univ Paris 07, CNRS, UMR7164, Paris, France. [Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. 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R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, Paris, France. [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Donzelli, S.; Eriksen, H. K.; Hansen, F. K.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Hildebrandt, S. R.; Hoyland, R. J.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; O'Dwyer, I. J.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Davies, R. D.; Davis, R. 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R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Paladini, R.] Spitzer Sci Ctr, Pasadena, CA USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS, OMP, IRAP, F-31028 Toulouse 4, France. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Miville-Deschenes, MA (reprint author), Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, Batiment 121, F-91405 Orsay, France. EM mamd@ias.u-psud.fr RI Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Nati, Federico/I-4469-2016; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; Bouchet, Francois/B-5202-2014; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Lopez-Caniego, Marcos/M-4695-2013; OI Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Masi, Silvia/0000-0001-5105-1439; Melchiorri, Alessandro/0000-0001-5326-6003; de Bernardis, Paolo/0000-0001-6547-6446; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; de Gasperis, Giancarlo/0000-0003-2899-2171; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Savini, Giorgio/0000-0003-4449-9416 NR 101 TC 111 Z9 111 U1 0 U2 9 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A24 DI 10.1051/0004-6361/201116485 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100025 ER PT J AU Ade, PAR Aghanim, N Ansari, R Arnaud, M Ashdown, M Aumont, J Banday, AJ Bartelmann, M Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bock, JJ Bond, JR Borrill, J Bouchet, FR Boulanger, F Bradshaw, T Bucher, M Cardoso, JF Castex, G Catalano, A Challinor, A Chamballu, A Chary, RR Chen, X Chiang, C Church, S Clements, DL Colley, JM Colombi, S Couchot, F Coulais, A Cressiot, C Crill, BP Crook, M de Bernardis, P Delabrouille, J Delouis, JM Desert, FX Dolag, K Dole, H Dore, O Douspis, M Dunkley, J Efstathiou, G Filliard, C Forni, O Fosalba, P Ganga, K Giard, M Girard, D Giraud-Heraud, Y Gispert, R Gorski, KM Gratton, S Griffin, M Guyot, G Haissinski, J Harrison, D Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Hildebrandt, SR Hills, R Hivon, E Hobson, M Holmes, WA Huffenberger, KM Jaffe, AH Jones, WC Kaplan, J Kneissl, R Knox, L Kunz, M Lagache, G Lamarre, JM Lange, AE Lasenby, A Lavabre, A Lawrence, CR Le Jeune, M Leroy, C Lesgourgues, J Macias-Perez, JF MacTavish, CJ Maffei, B Mandolesi, N Mann, R Marleau, F Marshall, DJ Masi, S Matsumura, T McAuley, I McGehee, P Melin, JB Mercier, C Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Mortlock, D Murphy, A Nati, F Netterfield, CB Norgaard-Nielsen, HU North, C Noviello, F Novikov, D Osborne, S Pajot, F Patanchon, G Peacocke, T Pearson, TJ Perdereau, O Perotto, L Piacentini, F Piat, M Plaszczynski, S Pointecouteau, E Ponthieu, N Prezeau, G Prunet, S Puget, JL Reach, WT Remazeilles, M Renault, C Riazuelo, A Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rusholme, B Saha, R Santos, D Savini, G Schaefer, BM Shellard, P Spencer, L Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sutton, D Sygnet, JF Tauber, JA Thum, C Torre, JP Touze, F Tristram, M Van Leeuwen, F Vibert, L Vibert, D Wade, LA Wandelt, BD White, SDM Wiesemeyer, H Woodcraft, A Yurchenko, V Yvon, D Zacchei, A AF Ade, P. A. R. Aghanim, N. Ansari, R. Arnaud, M. Ashdown, M. Aumont, J. Banday, A. J. Bartelmann, M. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bock, J. J. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bradshaw, T. Bucher, M. Cardoso, J. -F. Castex, G. Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chen, X. Chiang, C. Church, S. Clements, D. L. Colley, J. -M. Colombi, S. Couchot, F. Coulais, A. Cressiot, C. Crill, B. P. Crook, M. de Bernardis, P. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dolag, K. Dole, H. Dore, O. Douspis, M. Dunkley, J. Efstathiou, G. Filliard, C. Forni, O. Fosalba, P. Ganga, K. Giard, M. Girard, D. Giraud-Heraud, Y. Gispert, R. Gorski, K. M. Gratton, S. Griffin, M. Guyot, G. Haissinski, J. Harrison, D. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Hildebrandt, S. R. Hills, R. Hivon, E. Hobson, M. Holmes, W. A. Huffenberger, K. M. Jaffe, A. H. Jones, W. C. Kaplan, J. Kneissl, R. Knox, L. Kunz, M. Lagache, G. Lamarre, J. -M. Lange, A. E. Lasenby, A. Lavabre, A. Lawrence, C. R. Le Jeune, M. Leroy, C. Lesgourgues, J. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Mandolesi, N. Mann, R. Marleau, F. Marshall, D. J. Masi, S. Matsumura, T. McAuley, I. McGehee, P. Melin, J. -B. Mercier, C. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Mortlock, D. Murphy, A. Nati, F. Netterfield, C. B. Norgaard-Nielsen, H. U. North, C. Noviello, F. Novikov, D. Osborne, S. Pajot, F. Patanchon, G. Peacocke, T. Pearson, T. J. Perdereau, O. Perotto, L. Piacentini, F. Piat, M. Plaszczynski, S. Pointecouteau, E. Ponthieu, N. Prezeau, G. Prunet, S. Puget, J. -L. Reach, W. T. Remazeilles, M. Renault, C. Riazuelo, A. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rusholme, B. Saha, R. Santos, D. Savini, G. Schaefer, B. M. Shellard, P. Spencer, L. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sutton, D. Sygnet, J. -F. Tauber, J. A. Thum, C. Torre, J. -P. Touze, F. Tristram, M. Van Leeuwen, F. Vibert, L. Vibert, D. Wade, L. A. Wandelt, B. D. White, S. D. M. Wiesemeyer, H. Woodcraft, A. Yurchenko, V. Yvon, D. Zacchei, A. CA Planck HFI Core Team TI Planck early results. VI. The High Frequency Instrument data processing SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; cosmic background radiation; methods: data analysis; surveys ID PRE-LAUNCH STATUS; IN-FLIGHT PERFORMANCE; MAP-MAKING METHOD; POWER SPECTRA; COMPONENT SEPARATION; SKY MAPS; MICROWAVE; MISSION; CALIBRATION; NOISE AB We describe the processing of the 336 billion raw data samples from the High Frequency Instrument (HFI) which we performed to produce six temperature maps from the first 295 days of Planck-HFI survey data. These maps provide an accurate rendition of the sky emission at 100, 143, 217, 353, 545 and 857GHz with an angular resolution ranging from 9.9 to 4.4'. The white noise level is around 1.5 mu K degree or less in the 3 main CMB channels (100-217 GHz). The photometric accuracy is better than 2% at frequencies between 100 and 353 GHz and around 7% at the two highest frequencies. The maps created by the HFI Data Processing Centre reach our goals in terms of sensitivity, resolution, and photometric accuracy. They are already sufficiently accurate and well-characterised to allow scientific analyses which are presented in an accompanying series of early papers. At this stage, HFI data appears to be of high quality and we expect that with further refinements of the data processing we should be able to achieve, or exceed, the science goals of the Planck project. C1 [Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Lesgourgues, J.; Moneti, A.; Prunet, S.; Riazuelo, A.; Sygnet, J. -F.; Wandelt, B. D.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, Paris, France. [Colley, J. -M.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Castex, G.; Catalano, A.; Colley, J. -M.; Cressiot, C.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Kaplan, J.; Le Jeune, M.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris 07, CNRS, UMR7164, Paris, France. [Ashdown, M.; Hills, R.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile. [Bond, J. R.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse 4, France. [Challinor, A.; Shellard, P.] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England. 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[Fosalba, P.] Fac Ciencies, CSIC IEEC, Inst Ciencies Espai, Bellaterra 08193, Spain. [Wiesemeyer, H.] Inst Radioastron Millimetrique IRAM, Granada 18012, Spain. [Thum, C.] Inst Radioastron Millimetr IRAM, F-38406 Grenoble, France. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Sutton, D.; Van Leeuwen, F.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Hildebrandt, S. R.] Inst Astrofis Canarias, Tenerife, Spain. [Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Prezeau, G.; Rocha, G.; Saha, R.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Maffei, B.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Catalano, A.; Coulais, A.; Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Arnaud, M.; Starck, J. -L.] Univ Paris Diderot, CNRS, Lab AIM, IRFU Serv Astrophys,CEA DSM,CEA Saclay, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, UMR 5141, Lab Traitement & Commun Informat, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Vibert, D.] Astrophys Lab, F-13388 Marseille 13, France. [Girard, D.; Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, Inst Natl Polytech Grenoble, CNRS IN2P3, F-38026 Grenoble, France. [Ansari, R.; Couchot, F.; Filliard, C.; Haissinski, J.; Henrot-Versille, S.; Lavabre, A.; Perdereau, O.; Plaszczynski, S.; Touze, F.; Tristram, M.] Univ Paris 11, Lab Accelerateur Lineaire, CNRS IN2P3, F-91405 Orsay, France. [Borrill, J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Banday, A. J.; Bartelmann, M.; Dolag, K.; Hernandez-Monteagudo, C.; Sunyaev, R.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [McAuley, I.; Murphy, A.; Peacocke, T.; Yurchenko, V.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Savini, G.] UCL, Opt Sci Lab, London, England. [Bradshaw, T.; Crook, M.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Mann, R.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ade, P. A. R.; Griffin, M.; North, C.; Spencer, L.; Sudiwala, R.; Woodcraft, A.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Church, S.; Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Bartelmann, M.; Schaefer, B. M.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Reach, W. T.] Stratospher Observ Infrared Astron, Univ Space Res Assoc, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Bouchet, FR (reprint author), Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, 98Bis Blvd Arago, Paris, France. EM bouchet@iap.fr RI Remazeilles, Mathieu/N-1793-2015; Bartelmann, Matthias/A-5336-2014; Bouchet, Francois/B-5202-2014; Battaner, Eduardo/P-7019-2014; Yvon, Dominique/D-2280-2015; Pearson, Timothy/N-2376-2015; Fosalba Vela, Pablo/I-5515-2016; Nati, Federico/I-4469-2016; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; OI Hivon, Eric/0000-0003-1880-2733; Savini, Giorgio/0000-0003-4449-9416; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Remazeilles, Mathieu/0000-0001-9126-6266; WANDELT, Benjamin/0000-0002-5854-8269; Huffenberger, Kevin/0000-0001-7109-0099; Bouchet, Francois/0000-0002-8051-2924; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Zacchei, Andrea/0000-0003-0396-1192; Pearson, Timothy/0000-0001-5213-6231; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Masi, Silvia/0000-0001-5105-1439 FU ESA member states FX Planck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states (in particular the lead countries France and Italy), with contributions from NASA (USA) and telescope reflectors provided by a collaboration between ESA and a scientific consortium led and funded by Denmark. NR 74 TC 100 Z9 100 U1 0 U2 9 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A6 DI 10.1051/0004-6361/201116462 PG 47 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100007 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Cabella, P Cardoso, JF Catalano, A Cayon, L Challinor, A Chamballu, A Chiang, LY Chiang, C Christensen, PR Clements, DL Colombi, S Couchot, F Coulais, A Crill, BP Cuttaia, F Dame, TM Danese, L Davies, RD Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dickinson, C Dobashi, K Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Falgarone, E Finelli, F Forni, O Fosalba, P Frailis, M Franceschi, E Fukui, Y Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Grenier, IA Gruppuso, A Hansen, FK Harrison, D Helou, G Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Jaffe, AH Jones, WC Juvela, M Kawamura, A Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leonardi, R Leroy, C Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Maffei, B Maino, D Mandolesi, N Mann, R Maris, M Martin, P Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, P McGehee, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I O'Dwyer, IJ Onishi, T Osborne, S Pajot, F Paladini, R Paradis, D Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Prezeau, G Prunet, S Puget, JL Reach, WT Reinecke, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, P Smoot, GF Starck, JL Stivoli, F Stolyarov, V Stompor, R Sudiwala, R Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Tristram, M Tuovinen, J Umana, G Valenziano, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Wilkinson, A Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bhatia, R. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Cabella, P. Cardoso, J. -F. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chiang, L. -Y Chiang, C. Christensen, P. R. Clements, D. L. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Cuttaia, F. Dame, T. M. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dickinson, C. Dobashi, K. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Falgarone, E. Finelli, F. Forni, O. Fosalba, P. Frailis, M. Franceschi, E. Fukui, Y. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Grenier, I. A. Gruppuso, A. Hansen, F. K. Harrison, D. Helou, G. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Jaffe, A. H. Jones, W. C. Juvela, M. Kawamura, A. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leonardi, R. Leroy, C. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Maino, D. Mandolesi, N. Mann, R. Maris, M. Martin, P. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. McGehee, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. O'Dwyer, I. J. Onishi, T. Osborne, S. Pajot, F. Paladini, R. Paradis, D. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Prezeau, G. Prunet, S. Puget, J. -L. Reach, W. T. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, P. Smoot, G. F. Starck, J. -L. Stivoli, F. Stolyarov, V. Stompor, R. Sudiwala, R. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J. -P. Tristram, M. Tuovinen, J. Umana, G. Valenziano, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Wilkinson, A. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. XIX. All-sky temperature and dust optical depth from Planck and IRAS. Constraints on the "dark gas" in our Galaxy SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE dust, extinction; ISM: clouds; evolution; solar neighborhood; Galaxy: general; submillimeter: ISM ID GALACTIC MOLECULAR CLOUDS; SENSITIVITY HI SURVEY; FINAL DATA RELEASE; MILKY-WAY; INTERSTELLAR-MEDIUM; MAGELLANIC-CLOUD; INFRARED CIRRUS; SPITZER SURVEY; OUTER GALAXY; GOULD BELT AB An all sky map of the apparent temperature and optical depth of thermal dust emission is constructed using the Planck-HFI (350 mu m to 2 mm) and IRAS (100 mu m) data. The optical depth maps are correlated with tracers of the atomic (H I) and molecular gas traced by CO. The correlation with the column density of observed gas is linear in the lowest column density regions at high Galactic latitudes. At high N-H, the correlation is consistent with that of the lowest N-H, for a given choice of the CO-to-H-2 conversion factor. In the intermediate N-H range, a departure from linearity is observed, with the dust optical depth in excess of the correlation. This excess emission is attributed to thermal emission by dust associated with a dark gas phase, undetected in the available H I and CO surveys. The 2D spatial distribution of the dark gas in the solar neighbourhood (vertical bar b(II)vertical bar > 10 degrees) is shown to extend around known molecular regions traced by CO. The average dust emissivity in the H I phase in the solar neighbourhood is found to be tau(D)/N-H(tot) = 5.2 x 10(-26) cm(2) at 857 GHz. It follows roughly a power law distribution with a spectral index beta = 1.8 all the way down to 3 mm, although the SED flattens slightly in the millimetre. Taking into account the spectral shape of the dust optical depth, the emissivity is consistent with previous values derived from FIRAS measurements at high latitudes within 10%. The threshold for the existence of the dark gas is found at N-H(tot) = (8.0 +/- 0.58) x 10(20) H cm(-2) (A(V) = 0.4 mag). Assuming the same high frequency emissivity for the dust in the atomic and the molecular phases leads to an average X-CO = (2.54 +/- 0.13) x 10(20) H-2 cm(-2)/(K km s(-1)). The mass of dark gas is found to be 28% of the atomic gas and 118% of the CO emitting gas in the solar neighbourhood. The Galactic latitude distribution shows that its mass fraction is relatively constant down to a few degrees from the Galactic plane. A possible explanation for the dark gas lies in a dark molecular phase, where H-2 survives photodissociation but CO does not. The observed transition for the onset of this phase in the solar neighbourhood (A(V) = 0.4 mag) appears consistent with recent theoretical predictions. It is also possible that up to half of the dark gas could be in atomic form, due to optical depth effects in the Hi measurements. C1 [Banday, A. 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[Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Hildebrandt, S. R.; Hoyland, R. J.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, Inst Fis Cantabria, CSIC, E-39005 Santander, Spain. [Davies, R. D.; Davis, R. J.; Dickinson, C.; Maffei, B.; Wilkinson, A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Catalano, A.; Coulais, A.; Falgarone, E.; Lamarre, J. -M.] Observ Paris, LERMA, CNRS, F-75014 Paris, France. [Arnaud, M.; Grenier, I. A.; Starck, J. -L.] Univ Paris Diderot, Lab AIM, IRFU, Serv Astrophys,CEA,DSM,CNRS,CEA Saclay, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, CNRS, IN2P3,Inst Natl Polytech Grenoble, F-38026 Grenoble, France. [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS, Lab Accelerateur Lineaire, IN2P3, F-91405 Orsay, France. [Borrill, J.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Banday, A. J.; Doerl, U.; Ensslin, T. A.; Hovest, W.; Matthai, F.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Tuovinen, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland. [Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Co Kildare, Ireland. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Mann, R.] Univ Edinburgh, SUPA, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Paladini, R.] Spitzer Sci Ctr, Pasadena, CA USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Bernard, JP (reprint author), Univ Toulouse, UPS, OMP, IRAP, F-31028 Toulouse 4, France. EM Jean-Philippe.Bernard@cesr.fr RI Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Fosalba Vela, Pablo/I-5515-2016; Novikov, Igor/N-5098-2015; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Lilje, Per/A-2699-2012; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; OI WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Scott, Douglas/0000-0002-6878-9840; Masi, Silvia/0000-0001-5105-1439; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Ricciardi, Sara/0000-0002-3807-4043; Pasian, Fabio/0000-0002-4869-3227; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; de Bernardis, Paolo/0000-0001-6547-6446; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Valenziano, Luca/0000-0002-1170-0104; Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; de Gasperis, Giancarlo/0000-0003-2899-2171; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Reach, William/0000-0001-8362-4094; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Savini, Giorgio/0000-0003-4449-9416; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794 NR 87 TC 158 Z9 158 U1 0 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 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A19 DI 10.1051/0004-6361/201116479 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100020 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Cabella, P Cantalupo, CM Cardoso, JF Catalano, A Cayon, L Challinor, A Chamballu, A Chary, RR Chiang, LY Christensen, PR Clements, DL Colombi, S Couchot, F Coulais, A Crill, BP Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dickinson, C Dobashi, K Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Falgarone, E Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Harrison, D Helou, G Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Jaffe, AH Joncas, G Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leonardi, R Leroy, C Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Maffei, B Mandolesi, N Mann, R Maris, M Marshall, DJ Martin, P Martinez-Gonzalez, E Marton, G Masi, S Matarrese, S Matthai, F Mazzotta, P McGehee, P Melchiorri, A Mendes, L Mennella, A Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Pajot, F Paladini, R Pasian, F Patanchon, G Pearson, TJ Pelkonen, VM Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Prezeau, G Prunet, S Puget, JL Reach, WT Rebolo, R Reinecke, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Smoot, GF Starck, JL Stivoli, F Stolyarov, V Sudiwala, R Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Toth, V Tristram, M Tuovinen, J Umana, G Valenziano, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Ysard, N Yvon, D Zacchei, A Zahorecz, S Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bhatia, R. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Cabella, P. Cantalupo, C. M. Cardoso, J. -F. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chary, R. -R. Chiang, L. -Y Christensen, P. R. Clements, D. L. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dickinson, C. Dobashi, K. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Falgarone, E. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Harrison, D. Helou, G. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Jaffe, A. H. Joncas, G. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leonardi, R. Leroy, C. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Mandolesi, N. Mann, R. Maris, M. Marshall, D. J. Martin, P. Martinez-Gonzalez, E. Marton, G. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. McGehee, P. Melchiorri, A. Mendes, L. Mennella, A. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Pajot, F. Paladini, R. Pasian, F. Patanchon, G. Pearson, T. J. Pelkonen, V. -M. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Prezeau, G. Prunet, S. Puget, J. -L. Reach, W. T. Rebolo, R. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Smoot, G. F. Starck, J. -L. Stivoli, F. Stolyarov, V. Sudiwala, R. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J. -P. Toth, V. Tristram, M. Tuovinen, J. Umana, G. Valenziano, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Ysard, N. Yvon, D. Zacchei, A. Zahorecz, S. Zonca, A. CA Planck Collaboration TI Planck early results. XXIII. The first all-sky survey of Galactic cold clumps SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; stars: formation; dust, extinction; submillimetre: ISM; ISM: general; catalogs ID INFRARED DARK CLOUDS; PRE-LAUNCH STATUS; LARGE-MAGELLANIC-CLOUD; YOUNG STELLAR OBJECTS; IN-FLIGHT PERFORMANCE; TELESCOPE BLAST 2005; C2D LEGACY CLOUDS; STAR-FORMATION; MILKY-WAY; MOLECULAR CLOUDS AB We present the statistical properties of the Cold Clump Catalogue of Planck Objects (C3PO), the first all-sky catalogue of cold objects, in terms of their spatial distribution, dust temperature, distance, mass, and morphology. We have combined Planck and IRAS data to extract 10 342 cold sources that stand out against a warmer environment. The sources are distributed over the whole sky, including in the Galactic plane, despite the confusion, and up to high latitudes (>30 degrees). We find a strong spatial correlation of these sources with ancillary data tracing Galactic molecular structures and infrared dark clouds where the latter have been catalogued. These cold clumps are not isolated but clustered in groups. Dust temperature and emissivity spectral index values are derived from their spectral energy distributions using both Planck and IRAS data. The temperatures range from 7K to 19K, with a distribution peaking around 13K. The data are inconsistent with a constant value of the associated spectral index beta over the whole temperature range: beta varies from 1.4 to 2.8, with a mean value around 2.1. Distances are obtained for approximately one third of the objects. Most of the detections lie within 2 kpc of the Sun, but more distant sources are also detected, out to 7 kpc. The mass estimates inferred from dust emission range from 0.4 M-circle dot to 2.4 x 10(5) M-circle dot. Their physical properties show that these cold sources trace a broad range of objects, from low-mass dense cores to giant molecular clouds, hence the "cold clump" terminology. This first statistical analysis of the C3PO reveals at least two colder populations of special interest with temperatures in the range 7 to 12K: cores that mostly lie close to the Sun; and massive cold clumps located in the inner Galaxy. We also describe the statistics of the early cold core (ECC) sample that is a subset of the C3PO, containing only the 915 most reliable detections. The ECC is delivered as a part of the Planck Early Release Compact Source Catalogue (ERCSC). C1 [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.] Univ Paris 07, CNRS, UMR7164, Paris, France. [Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile. [Bond, J. R.; Martin, P.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse 4, France. [Challinor, A.] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England. [Starck, J. -L.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Linden-Vornle, M.; Norgaard-Nielsen, H. 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[Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Nati, F.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy. [Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Balbi, A.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Marton, G.; Toth, V.; Zahorecz, S.] Eotvos Lorand Univ, Dept Astron, H-1117 Budapest, Hungary. [Kneissl, R.] ESO Vitacura, European So Observ, Santiago, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] Planck Sci Off, European Space Agcy, ESAC, Madrid, Spain. [Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] ESTEC, European Space Agcy, NL-2201 AZ Noordwijk, Netherlands. [Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland. [Umana, G.] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy. [Bonaldi, A.; de Zotti, G.] Osserv Astron Padova, INAF, Padua, Italy. [Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] IASF Bologna, INAF, Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Tomasi, M.] IASF Milano, INAF, Milan, Italy. 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D.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, Paris, France. [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Donzelli, S.; Hansen, F. K.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Henrot-Versille, S.; Hildebrandt, S. R.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; Mitra, S.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Davies, R. D.; Davis, R. J.; Dickinson, C.; Maffei, B.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Catalano, A.; Coulais, A.; Falgarone, E.; Lamarre, J. -M.] Observ Paris, LERMA, CNRS, F-75014 Paris, France. [Arnaud, M.; Starck, J. -L.] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM,IRFU,Serv Astrophys,CEA,DSM, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Inst Natl Polytech Grenoble, CNRS, Lab Phys Subat & Cosmol,IN2P3, F-38026 Grenoble, France. [Couchot, F.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS, Lab Accelerateur Lineaire, IN2P3, F-91405 Orsay, France. [Borrill, J.; Cantalupo, C. M.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Banday, A. J.; Doerl, U.; Ensslin, T. A.; Hovest, W.; Matthai, F.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Tuovinen, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland. [Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Mann, R.] Univ Edinburgh, Royal Observ, SUPA, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Paladini, R.] Spitzer Sci Ctr, Pasadena, CA USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Montier, L (reprint author), Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. EM Ludovic.Montier@irap.omp.eu RI Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Nati, Federico/I-4469-2016; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Toth, L. Viktor/C-8667-2017; Mazzotta, Pasquale/B-1225-2016; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Pearson, Timothy/N-2376-2015; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; OI Reach, William/0000-0001-8362-4094; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Savini, Giorgio/0000-0003-4449-9416; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Toth, L. Viktor/0000-0002-5310-4212; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Pearson, Timothy/0000-0001-5213-6231; de Gasperis, Giancarlo/0000-0003-2899-2171; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196 FU NASA Office of Space Science FX A description of the Planck Collaboration and a list of its members can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page=Planck_Collaborati on. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. This research makes use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 146 TC 88 Z9 88 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A23 DI 10.1051/0004-6361/201116472 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100024 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Cabella, P Cappellini, B Cardoso, JF Casassus, S Catalano, A Cayon, L Challinor, A Chamballu, A Chary, RR Chen, X Chiang, LY Chiang, C Christensen, PR Clements, DL Colombi, S Couchot, F Coulais, A Crill, BP Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Dickinson, C Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Genova-Santos, RT Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Harrison, D Helou, G Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Jaffe, TR Jaffe, AH Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leonardi, R Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Maffei, B Maino, D Mandolesi, N Mann, R Maris, M Marshall, DJ Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, P McGehee, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I O'Dwyer, IJ Osborne, S Pajot, F Paladini, R Partridge, B Pasian, F Patanchon, G Pearson, TJ Peel, M Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Plaszczynski, S Platania, P Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Prezeau, G Procopio, P Prunet, S Puget, JL Reach, WT Rebolo, R Reich, W Reinecke, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, P Smoot, GF Starck, JL Stivoli, F Stolyarov, V Stompor, R Sudiwala, R Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Tristram, M Tuovinen, J Umana, G Valenziano, L Varis, J Verstraete, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Watson, R Wilkinson, A Ysard, N Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J-P Bersanelli, M. Bhatia, R. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Cabella, P. Cappellini, B. Cardoso, J-F Casassus, S. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chary, R-R Chen, X. Chiang, L-Y Chiang, C. Christensen, P. R. Clements, D. L. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J-M Dickinson, C. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Genova-Santos, R. T. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Harrison, D. Helou, G. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Jaffe, T. R. Jaffe, A. H. Jones, W. C. Juvela, M. Keihaenen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Laehteenmaeki, A. Lamarre, J-M Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leonardi, R. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Maino, D. Mandolesi, N. Mann, R. Maris, M. Marshall, D. J. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. McGehee, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Mitra, S. Miville-Deschenes, M-A Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. O'Dwyer, I. J. Osborne, S. Pajot, F. Paladini, R. Partridge, B. Pasian, F. Patanchon, G. Pearson, T. J. Peel, M. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Plaszczynski, S. Platania, P. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Prezeau, G. Procopio, P. Prunet, S. Puget, J-L Reach, W. T. Rebolo, R. Reich, W. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, P. Smoot, G. F. Starck, J-L Stivoli, F. Stolyarov, V. Stompor, R. Sudiwala, R. Sygnet, J-F Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J-P Tristram, M. Tuovinen, J. Umana, G. Valenziano, L. Varis, J. Verstraete, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Watson, R. Wilkinson, A. Ysard, N. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. XX. New light on anomalous microwave emission from spinning dust grains SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: general; Galaxy: general; radiation mechanisms: general; radio continuum: ISM; submillimeter: ISM ID PROBE WMAP OBSERVATIONS; PRE-LAUNCH STATUS; POLYCYCLIC AROMATIC-HYDROCARBON; INTERSTELLAR RADIATION-FIELD; PERSEUS MOLECULAR-COMPLEX; CENTIMETER-WAVE CONTINUUM; INTER-STELLAR CLOUDS; ANISOTROPY-PROBE; FOREGROUND EMISSION; COSMOSOMAS EXPERIMENT AB Anomalous microwave emission (AME) has been observed by numerous experiments in the frequency range similar to 10-60 GHz. Using Planck maps and multi-frequency ancillary data, we have constructed spectra for two known AME regions: the Perseus and rho Ophiuchi molecular clouds. The spectra are well fitted by a combination of free-free radiation, cosmic microwave background, thermal dust, and electric dipole radiation from small spinning dust grains. The spinning dust spectra are the most precisely measured to date, and show the high frequency side clearly for the first time. The spectra have a peak in the range 20-40 GHz and are detected at high significances of 17.1 sigma for Perseus and 8.4 sigma for rho Ophiuchi. In Perseus, spinning dust in the dense molecular gas can account for most of the AME; the low density atomic gas appears to play a minor role. In rho Ophiuchi, the similar to 30 GHz peak is dominated by dense molecular gas, but there is an indication of an extended tail at frequencies 50-100 GHz, which can be accounted for by irradiated low density atomic gas. The dust parameters are consistent with those derived from other measurements. We have also searched the Planck map at 28.5 GHz for candidate AME regions, by subtracting a simple model of the synchrotron, free-free, and thermal dust. 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[Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Genova-Santos, R. T.; Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Kneissl, R.] European So Observ, ESO Vitacura, Santiago 19, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain. [Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands. [Partridge, B.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA. [Kurki-Suonio, H.; Laehteenmaeki, A.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland. [Umana, G.] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy. [Bonaldi, A.; de Zotti, G.] Osserv Astron Padova, INAF, Padua, Italy. [Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Procopio, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Bologna, Italy. [Bersanelli, M.; Cappellini, B.; Donzelli, S.; Maino, D.; Tomasi, M.] INAF IASF Milano, Milan, Italy. [Stivoli, F.] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France. [Chamballu, A.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Chary, R-R; Chen, X.; Ganga, K.; McGehee, P.; Pearson, T. J.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France. [Aghanim, N.; Aumont, J.; Boulanger, F.; Douspis, M.; Lagache, G.; Miville-Deschenes, M-A; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J-L; Torre, J-P; Verstraete, L.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France. [Benabed, K.; Bouchet, F. R.; Cardoso, J-F; Colombi, S.; Delouis, J-M; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J-F; Wandelt, B. D.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, Paris, France. [Chiang, L-Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Donzelli, S.; Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Genova-Santos, R. T.; Hildebrandt, S. R.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Platania, P.] CNR ENEA EURATOM Assoc, Ist Fis Plasma, Milan, Italy. [Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; Mitra, S.; O'Dwyer, I. J.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Catalano, A.; Coulais, A.; Lamarre, J-M] Observ Paris, LERMA, CNRS, F-75014 Paris, France. [Arnaud, M.; Starck, J-L] Univ Paris Diderot, CEA Saclay, Lab AIM, IRFU Serv Astrophys,CEA DSM,CNRS, F-91191 Gif Sur Yvette, France. [Cardoso, J-F] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France. [Cardoso, J-F] Telecom ParisTech, F-75634 Paris 13, France. [Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, CNRS IN2P3, Inst Natl Polytech Grenoble, F-38026 Grenoble, France. [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, Lab Accelerateur Lineaire, CNRS IN2P3, F-91405 Orsay, France. [Borrill, J.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Banday, A. J.; Doerl, U.; Ensslin, T. A.; Hovest, W.; Matthai, F.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Reich, W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland. [Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Mann, R.] Univ Edinburgh, Royal Observ, SUPA, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Paladini, R.] Spitzer Sci Ctr, Pasadena, CA USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Casassus, S.] Univ Chile, Santiago, Chile. [Banday, A. J.; Bernard, J-P; Forni, O.; Giard, M.; Jaffe, T. R.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Dickinson, C (reprint author), Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. EM Clive.Dickinson@manchester.ac.uk RI Gonzalez-Nuevo, Joaquin/I-3562-2014; Pearson, Timothy/N-2376-2015; Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Casassus, Simon/I-8609-2016; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; Martinez-Gonzalez, Enrique/E-9534-2015; Lilje, Per/A-2699-2012; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Lahteenmaki, Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; OI Ricciardi, Sara/0000-0002-3807-4043; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Pearson, Timothy/0000-0001-5213-6231; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; de Gasperis, Giancarlo/0000-0003-2899-2171; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272; Savini, Giorgio/0000-0003-4449-9416; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Watson, Robert/0000-0002-5873-0124; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Villa, Fabrizio/0000-0003-1798-861X; Peel, Mike/0000-0003-3412-2586; Galeotta, Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379 FU NASA Office of Space Science; National Aeronautics and Space Administration (NASA); ESA; CNES; CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy); DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU) FX We thank the referee, Doug Finkbeiner, for useful comments. We thank Justin Jonas for providing the 2326 MHz HartRAO map. We acknowledge the use of the MPIfR Survey Sampler website at http://www.mpifr-bonn.mpg.de/survey.html. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA); support for LAMBDA is provided by the NASA Office of Space Science. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research makes use of the SIMBAD database, operated at CDS, Strasbourg, France.; The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). A detailed description of the Planck Collaboration and a list of its members can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page=Planck_Collaborati on. NR 131 TC 103 Z9 103 U1 0 U2 9 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A20 DI 10.1051/0004-6361/201116470 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100021 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Cabella, P Cantalupo, CM Cardoso, JF Catalano, A Cayon, L Challinor, A Chamballu, A Chiang, LY Christensen, PR Clements, DL Colombi, S Couchot, F Coulais, A Crill, BP Cuttaia, F Danese, L Davies, RD de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dickinson, C Doi, Y Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Falgarone, E Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Harrison, D Helou, G Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Ikeda, N Jaffe, AH Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kitamura, Y Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leonardi, R Leroy, C Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Maffei, B Malinen, J Mandolesi, N Mann, R Maris, M Marshall, DJ Martin, P Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, P McGehee, P Melchiorri, A Mendes, L Mennella, A Meny, C Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Pagani, L Pajot, F Paladini, R Pasian, F Patanchon, G Pelkonen, VM Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Prezeau, G Prunet, S Puget, JL Reach, WT Rebolo, R Reinecke, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Smoot, GF Starck, JL Stivoli, F Stolyarov, V Sudiwala, R Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Toth, V Tristram, M Tuovinen, J Umana, G Valenziano, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Ysard, N Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bhatia, R. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Cabella, P. Cantalupo, C. M. Cardoso, J. -F. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chiang, L. -Y Christensen, P. R. Clements, D. L. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Cuttaia, F. Danese, L. Davies, R. D. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dickinson, C. Doi, Y. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Falgarone, E. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Harrison, D. Helou, G. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Ikeda, N. Jaffe, A. H. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kitamura, Y. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leonardi, R. Leroy, C. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Malinen, J. Mandolesi, N. Mann, R. Maris, M. Marshall, D. J. Martin, P. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. McGehee, P. Melchiorri, A. Mendes, L. Mennella, A. Meny, C. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Pagani, L. Pajot, F. Paladini, R. Pasian, F. Patanchon, G. Pelkonen, V. -M. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Prezeau, G. Prunet, S. Puget, J. -L. Reach, W. T. Rebolo, R. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Smoot, G. F. Starck, J. -L. Stivoli, F. Stolyarov, V. Sudiwala, R. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J. -P. Toth, V. Tristram, M. Tuovinen, J. Umana, G. Valenziano, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Ysard, N. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. XXII. The submillimetre properties of a sample of Galactic cold clumps SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; dust, extinction; stars: formation; ISM: structure; submillimeter: ISM; stars: protostars ID INFRARED DARK CLOUDS; PRE-LAUNCH STATUS; HELICAL MAGNETIC-FIELDS; ROSETTE MOLECULAR CLOUD; COMETARY GLOBULE CG-12; YOUNG STELLAR OBJECTS; IN-FLIGHT PERFORMANCE; C2D LEGACY CLOUDS; STAR-FORMATION; DENSE CORES AB We perform a detailed investigation of sources from the Cold Cores Catalogue of Planck Objects (C3PO). Our goal is to probe the reliability of the detections, validate the separation between warm and cold dust emission components, provide the first glimpse at the nature, internal morphology and physical characterictics of the Planck-detected sources. We focus on a sub-sample of ten sources from the C3PO list, selected to sample different environments, from high latitude cirrus to nearby (150 pc) and remote (2 kpc) molecular complexes. We present Planck surface brightness maps and derive the dust temperature, emissivity spectral index, and column densities of the fields. With the help of higher resolution Herschel and AKARI continuum observations and molecular line data, we investigate the morphology of the sources and the properties of the substructures at scales below the Planck beam size. The cold clumps detected by Planck are found to be located on large-scale filamentary (or cometary) structures that extend up to 20 pc in the remote sources. The thickness of these filaments ranges between 0.3 and 3 pc, for column densities N-H2 similar to 0.1 to 1.6 x 10(22) cm(-2), and with linear mass density covering a broad range, between 15 and 400 M-circle dot pc(-1). The dust temperatures are low (between 10 and 15K) and the Planck cold clumps correspond to local minima of the line-of-sight averaged dust temperature in these fields. These low temperatures are confirmed when AKARI and Herschel data are added to the spectral energy distributions. Herschel data reveal a wealth of substructure within the Planck cold clumps. In all cases (except two sources harbouring young stellar objects), the substructures are found to be colder, with temperatures as low as 7 K. Molecular line observations provide gas column densities which are consistent with those inferred from the dust. The linewidths are all supra-thermal, providing large virial linear mass densities in the range 10 to 300 M-circle dot pc(-1), comparable within factors of a few, to the gas linear mass densities. The analysis of this small set of cold clumps already probes a broad variety of structures in the C3PO sample, probably associated with different evolutionary stages, from cold and starless clumps, to young protostellar objects still embedded in their cold surrounding cloud. Because of the all-sky coverage and its sensitivity, Planck is able to detect and locate the coldest spots in massive elongated structures that may be the long-searched for progenitors of stellar clusters. C1 [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Marshall, D. J.; Meny, C.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.] Univ Paris 07, CNRS, UMR7164, Paris, France. [Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile. [Bond, J. R.; Martin, P.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Marshall, D. J.; Meny, C.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse 4, France. [Challinor, A.] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England. [Starck, J. -L.; Yvon, D.] CEA Saclay, DSM, SPP, F-91191 Gif Sur Yvette, France. [Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. [Doi, Y.] Univ Tokyo, Dept Earth Sci & Astron, Meguro Ku, Tokyo 1538902, Japan. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Juvela, M.; Keihanen, E.; Keskitalo, R.; Kurki-Suonio, H.; Malinen, J.; Poutanen, T.; Ysard, N.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Smoot, G. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Leonardi, R.; Lubin, P. M.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA. [Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Nati, F.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy. [Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Balbi, A.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Toth, V.] Eotvos Lorand Univ, Dept Astron, H-1117 Budapest, Hungary. [Kneissl, R.] ESO Vitacura, European So Observ, Santiago, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] Planck Sci Off, European Space Agcy, ESAC, Madrid, Spain. [Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] ESTEC, European Space Agcy, NL-2201 AZ Noordwijk, Netherlands. [Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland. [Umana, G.] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy. [Bonaldi, A.; de Zotti, G.] Osserv Astron Padova, INAF, Padua, Italy. [Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] IASF Bologna, INAF, Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Tomasi, M.] IASF Milano, INAF, Milan, Italy. [Stivoli, F.] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France. [Desert, F. -X.] Univ Grenoble 1, CNRS, IPAG, INSU,UMR 5274, F-38041 Grenoble, France. [Chamballu, A.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Ganga, K.; McGehee, P.; Pelkonen, V. -M.; Rusholme, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France. [Aghanim, N.; Aumont, J.; Boulanger, F.; Douspis, M.; Lagache, G.; Leroy, C.; Miville-Deschenes, M. -A.; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Torre, J. -P.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France. [Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, Paris, France. [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Ikeda, N.; Kitamura, Y.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Donzelli, S.; Hansen, F. K.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Hildebrandt, S. R.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; Mitra, S.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Davies, R. D.; Dickinson, C.; Maffei, B.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Catalano, A.; Coulais, A.; Falgarone, E.; Lamarre, J. -M.; Pagani, L.] Observ Paris, LERMA, CNRS, F-75014 Paris, France. [Arnaud, M.; Starck, J. -L.] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM,IRFU,Serv Astrophys,CEA,DSM, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Inst Natl Polytech Grenoble, CNRS, Lab Phys Subat & Cosmol,IN2P3, F-38026 Grenoble, France. [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS, Lab Accelerateur Lineaire, IN2P3, F-91405 Orsay, France. [Borrill, J.; Cantalupo, C. M.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Banday, A. J.; Doerl, U.; Ensslin, T. A.; Hovest, W.; Matthai, F.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Tuovinen, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland. [Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Mann, R.] Univ Edinburgh, Royal Observ, SUPA, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Paladini, R.] Spitzer Sci Ctr, Pasadena, CA USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Ristorcelli, I (reprint author), Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. EM isabelle.ristorcelli@irap.omp.eu RI Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Nati, Federico/I-4469-2016; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Toth, L. Viktor/C-8667-2017; Mazzotta, Pasquale/B-1225-2016; Gregorio, Anna/J-1632-2012; Doi, Yasuo/A-3395-2013; Toth, L. Viktor/J-8561-2013; Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Doi, Yasuo/G-2363-2011; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; de Gasperis, Giancarlo/C-8534-2012; OI Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Toth, L. Viktor/0000-0002-5310-4212; Mazzotta, Pasquale/0000-0002-5411-1748; Savini, Giorgio/0000-0003-4449-9416; Doi, Yasuo/0000-0001-8746-6548; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272; de Gasperis, Giancarlo/0000-0003-2899-2171; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733 FU ESA; CNES; CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy); National Aeronautics and Space Administration (NASA); DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU); National Science Foundation FX A description of the Planck Collaboration and a list of its members can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page=Planck_Collaborati on. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU) This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research is based on observations with AKARI, a JAXA project with the participation of ESA. NR 132 TC 66 Z9 66 U1 0 U2 11 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 DEC PY 2011 VL 536 AR A22 DI 10.1051/0004-6361/201116481 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100023 ER PT J AU Ade, PAR Aghanim, N Angelakis, E Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bucher, M Burigana, C Cabella, P Cappellini, B Cardoso, JF Catalano, A Cayon, L Challinor, A Chamballu, A Chary, RR Chen, X Chiang, LY Christensen, PR Clements, DL Colombi, S Couchot, F Coulais, A Crill, BP Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dickinson, C Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Finelli, F Forni, O Frailis, M Franceschi, E Fuhrmann, L Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Harrison, D Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Huynh, M Jaffe, AH Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Krichbaum, TP Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lavonen, N Lawrence, CR Leach, S Leahy, JP Leonardi, R Leon-Tavares, J Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Mann, R Maris, M Marleau, F Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Mingaliev, M Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Natoli, P Nestoras, I Netterfield, CB Nieppola, E Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Pajot, F Paladini, R Partridge, B Pasian, F Patanchon, G Pearson, TJ Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Plaszczynski, S Platania, P Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Prezeau, G Procopio, P Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Renault, C Ricciardi, S Riller, T Riquelme, D Ristorcelli, I Rocha, G Rosset, C Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sajina, A Sandri, M Savolainen, P Scott, D Seiffert, MD Sievers, A Smoot, GF Sotnikova, Y Starck, JL Stivoli, F Stolyarov, V Sudiwala, R Sygnet, JF Tammi, J Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tornikoski, M Torre, JP Tristram, M Tuovinen, J Turler, M Turunen, M Umana, G Ungerechts, H Valenziano, L Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Wilkinson, A Yvon, D Zacchei, A Zensus, JA Zonca, A AF Ade, P. A. R. Aghanim, N. Angelakis, E. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bhatia, R. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bucher, M. Burigana, C. Cabella, P. Cappellini, B. Cardoso, J. -F. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chary, R. -R. Chen, X. Chiang, L. -Y Christensen, P. R. Clements, D. L. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dickinson, C. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Fuhrmann, L. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Harrison, D. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Huynh, M. Jaffe, A. H. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Krichbaum, T. P. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J-M. Lasenby, A. Laureijs, R. J. Lavonen, N. Lawrence, C. R. Leach, S. Leahy, J. P. Leonardi, R. Leon-Tavares, J. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Mann, R. Maris, M. Marleau, F. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Mingaliev, M. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Natoli, P. Nestoras, I. Netterfield, C. B. Nieppola, E. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Pajot, F. Paladini, R. Partridge, B. Pasian, F. Patanchon, G. Pearson, T. J. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Plaszczynski, S. Platania, P. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Prezeau, G. Procopio, P. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Riquelme, D. Ristorcelli, I. Rocha, G. Rosset, C. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sajina, A. Sandri, M. Savolainen, P. Scott, D. Seiffert, M. D. Sievers, A. Smoot, G. F. Sotnikova, Y. Starck, J. -L. Stivoli, F. Stolyarov, V. Sudiwala, R. Sygnet, J. -F. Tammi, J. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tornikoski, M. Torre, J. -P. Tristram, M. Tuovinen, J. Turler, M. Turunen, M. Umana, G. Ungerechts, H. Valenziano, L. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Wilkinson, A. Yvon, D. Zacchei, A. Zensus, J. A. Zonca, A. CA Planck Collaboration TI Planck early results. XIV. ERCSC validation and extreme radio sources SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE surveys; radio continuum: galaxies; radiation mechanisms: general ID PRE-LAUNCH STATUS; COMPTON CATASTROPHE SCENARIO; LONG-TERM VARIABILITY; ALL-SKY SURVEY; EXTRAGALACTIC SOURCES; MULTIFREQUENCY OBSERVATIONS; BRIGHT SAMPLE; 3C 454.3; SPECTRUM; GHZ AB Planck's all-sky surveys at 30-857 GHz provide an unprecedented opportunity to follow the radio spectra of a large sample of extragalactic sources to frequencies 2-20 times higher than allowed by past, large-area, ground-based surveys. We combine the results of the Planck Early Release Compact Source Catalog (ERCSC) with quasi-simultaneous ground-based observations as well as archival data at frequencies below or overlapping Planck frequency bands, to validate the astrometry and photometry of the ERCSC radio sources and study the spectral features shown in this new frequency window opened by Planck. The ERCSC source positions and flux density scales are found to be consistent with the ground-based observations. We present and discuss the spectral energy distributions of a sample of "extreme" radio sources, to illustrate the richness of the ERCSC for the study of extragalactic radio sources. Variability is found to play a role in the unusual spectral features of some of these sources. C1 [Partridge, B.; Sajina, A.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA. [Lahteenmaki, A.; Lavonen, N.; Leon-Tavares, J.; Nieppola, E.; Poutanen, T.; Savolainen, P.; Tammi, J.; Tornikoski, M.; Turunen, M.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.] Univ Paris 07, CNRS, UMR 7164, Paris, France. [Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago 0355, Chile. [Bonavera, L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Bond, J. R.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse 4, France. [Crill, B. P.; Dore, O.; Hildebrandt, S. R.; Pearson, T. J.; Prezeau, G.; Rocha, G.; Seiffert, M. D.] CALTECH, Pasadena, CA 91125 USA. [Challinor, A.] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England. [Starck, J. -L.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Marleau, F.; Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Pierpaoli, E.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA USA. [Juvela, M.; Keihanen, E.; Keskitalo, R.; Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Smoot, G. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Leonardi, R.; Lubin, P. M.; Meinhold, P. R.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy. [Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Balbi, A.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Kneissl, R.] ESO Vitacura, European So Observ, Santiago 19001, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] Planck Sci Off, European Space Agcy, ESAC, Madrid, Spain. [Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] Estec, European Space Agcy, NL-2201 AZ Noordwijk, Netherlands. [Nieppola, E.] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio 21500, Finland. [Kurki-Suonio, H.; Lahteenmaki, A.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland. [Umana, G.] INAF Osservatorio Astrofis Catania, Catania, Italy. [Bonaldi, A.; de Zotti, G.; Massardi, M.] INAF Osservatorio Astron Padova, Padua, Italy. [Polenta, G.] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] INAF Osservatorio Astron Trieste, Trieste, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Procopio, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Bologna, Italy. [Bersanelli, M.; Cappellini, B.; Donzelli, S.; Maino, D.; Tomasi, M.] INAF IASF Milano, Milan, Italy. [Stivoli, F.] Univ Paris 11, Lab Rech Informat, INRIA, F-91405 Orsay, France. [Desert, F. -X.] Univ Grenoble 1, IPAG, CNRS INSU, UMR 5274, F-38041 Grenoble, France. [Turler, M.] Univ Geneva, ISDC Data Ctr Astrophys, Versoix, Switzerland. [Chamballu, A.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Chary, R. -R.; Chen, X.; Ganga, K.; Huynh, M.; Paladini, R.; Pearson, T. J.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France. [Aghanim, N.; Aumont, J.; Douspis, M.; Lagache, G.; Miville-Deschenes, M. -A.; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Torre, J. -P.] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, Orsay, France. [Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, Paris, France. [Riquelme, D.; Sievers, A.; Ungerechts, H.] Inst Radioastron Millimetrique IRAM, Granada 18012, Spain. [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Donzelli, S.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Hildebrandt, S. R.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] CSIC Univ Cantabria, Inst Fis Cantabria, Santander, Spain. [Platania, P.] CNR ENEA EURATOM Assoc, Ist Fis Plasma, Milan, Italy. [Bartlett, J. G.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Davies, R. D.; Davis, R. J.; Dickinson, C.; Leahy, J. P.; Maffei, B.; Wilkinson, A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Catalano, A.; Coulais, A.; Lamarre, J-M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Arnaud, M.; Starck, J. -L.] Univ Paris Diderot, CNRS, CEA DSM, IRFU Serv Astrophys,Lab AIM, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, UMR 5141, Lab Traitement & Commun Informat, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, CNRS IN2P3, Inst Natl Polytech Grenoble, F-38026 Grenoble, France. [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS IN2P3, Lab Accelerateur Lineaire, Orsay, France. [Borrill, J.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Banday, A. J.; Doerl, U.; Ensslin, T. A.; Hovest, W.; Matthai, F.; Rachen, J. P.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Angelakis, E.; Fuhrmann, L.; Krichbaum, T. P.; Nestoras, I.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland. [Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Baccigalupi, C.; Bonavera, L.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Mann, R.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Mingaliev, M.; Sotnikova, Y.] Russian Acad Sci, Special Astrophys Observ, Karachai Cherkessian 369167, Russia. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, Warsaw, Poland. RP Partridge, B (reprint author), Haverford Coll, Dept Astron, 370 Lancaster Ave, Haverford, PA 19041 USA. EM bpartrid@haverford.edu RI Pearson, Timothy/N-2376-2015; Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; bonavera, laura/E-9368-2017; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Lahteenmaki, Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; OI Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Pearson, Timothy/0000-0001-5213-6231; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; bonavera, laura/0000-0001-8039-3876; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Lopez-Caniego, Marcos/0000-0003-1016-9283; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; de Gasperis, Giancarlo/0000-0003-2899-2171; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Pierpaoli, Elena/0000-0002-7957-8993; Starck, Jean-Luc/0000-0003-2177-7794; Angelakis, Emmanouil/0000-0001-7327-5441; Reach, William/0000-0001-8362-4094; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379; Matarrese, Sabino/0000-0002-2573-1243; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196 FU Academy of Finland [212656, 210338, 121148]; National Aeronautics and Space Administration; ESA; CNES; CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy); DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU) FX A description of the Planck Collaboration and a list of its members can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page=Planck_Collaborati on. This paper makes use of observations obtained at the Very Large Array (VLA) which is an instrument of the National Radio Astronomy Observatory (NRAO). The NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research also makes use of observations with the 100 m telescope of the Max Planck Institut fur Radioastronomie (MPIfR), the 30 m telescope of Institut de Radioastronomie Millimetrique (IRAM), the Australia Telescope Compact Array (ATCA) and the 13.7 m telescope of the Metsahovi Radio Observatory. The Mets hovi observing project is supported by the Academy of Finland (grant numbers 212656, 210338 and 121148). We acknowledge the 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. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). NR 74 TC 50 Z9 50 U1 0 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A14 DI 10.1051/0004-6361/201116475 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100015 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Bucher, M Burigana, C Cabella, P Cardoso, JF Catalano, A Cayon, L Challinor, A Chamballu, A Chary, RR Chiang, LY Christensen, PR Clements, DL Colombi, S Couchot, F Coulais, A Crill, BP Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dickinson, C Dole, H Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Harrison, D Helou, G Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Jaffe, AH Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leonardi, R Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Madden, S Maffei, B Maino, D Mandolesi, N Mann, R Maris, M Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, P Melchiorri, A Mendes, L Mennella, A Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Pajot, F Partridge, B Pasian, F Patanchon, G Peel, M Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Prezeau, G Prunet, S Puget, JL Reach, WT Rebolo, R Reinecke, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Savini, G Scott, D Seiffert, MD Shellard, P Smoot, GF Starck, JL Stivoli, F Stolyarov, V Sudiwala, R Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Tristram, M Tuovinen, J Turler, M Umana, G Valenziano, L Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bhatia, R. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Bucher, M. Burigana, C. Cabella, P. Cardoso, J. -F. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chary, R. -R. Chiang, L. -Y Christensen, P. R. Clements, D. L. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dickinson, C. Dole, H. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Harrison, D. Helou, G. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Jaffe, A. H. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leonardi, R. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Madden, S. Maffei, B. Maino, D. Mandolesi, N. Mann, R. Maris, M. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. Melchiorri, A. Mendes, L. Mennella, A. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Pajot, F. Partridge, B. Pasian, F. Patanchon, G. Peel, M. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Prezeau, G. Prunet, S. Puget, J. -L. Reach, W. T. Rebolo, R. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Savini, G. Scott, D. Seiffert, M. D. Shellard, P. Smoot, G. F. Starck, J. -L. Stivoli, F. Stolyarov, V. Sudiwala, R. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J. -P. Tristram, M. Tuovinen, J. Tuerler, M. Umana, G. Valenziano, L. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. XVI. The Planck view of nearby galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: photometry; submillimeter: galaxies; infrared: galaxies; galaxies: ISM ID SPECTRAL ENERGY-DISTRIBUTIONS; PRE-LAUNCH STATUS; ULTRALUMINOUS INFRARED GALAXIES; DEGREE EXTRAGALACTIC SURVEY; DEEP SUBMILLIMETER SURVEY; FSC REDSHIFT CATALOG; HERSCHEL-ATLAS; MU-M; NUMBER COUNTS; COLD DUST AB The all-sky coverage of the Planck Early Release Compact Source Catalogue (ERCSC) provides an unsurpassed survey of galaxies at submillimetre (submm) wavelengths, representing a major improvement in the numbers of galaxies detected, as well as the range of far-IR/ submm wavelengths over which they have been observed. We here present the first results on the properties of nearby galaxies using these data. We match the ERCSC catalogue to IRAS-detected galaxies in the Imperial IRAS Faint Source Redshift Catalogue (IIFSCz), so that we can measure the spectral energy distributions (SEDs) of these objects from 60 to 850 mu m. This produces a list of 1717 galaxies with reliable associations between Planck and IRAS, from which we select a subset of 468 for SED studies, namely those with strong detections in the three highest frequency Planck bands and no evidence of cirrus contamination. The SEDs are fitted using parametric dust models to determine the range of dust temperatures and emissivities. We find evidence for colder dust than has previously been found in external galaxies, with T < 20K. Such cold temperatures are found using both the standard single temperature dust model with variable emissivity beta, or a two dust temperature model with beta fixed at 2. We also compare our results to studies of distant submm galaxies (SMGs) which have been claimed to contain cooler dust than their local counterparts. We find that including our sample of 468 galaxies significantly reduces the distinction between the two populations. Fits to SEDs of selected objects using more sophisticated templates derived from radiative transfer models confirm the presence of the colder dust found through parametric fitting. We thus conclude that cold (T < 20K) dust is a significant and largely unexplored component of many nearby galaxies. C1 [Chamballu, A.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.] Univ Paris 07, CNRS UMR7164, Paris, France. [Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Astrophys Grp, Cavendish Lab, Cambridge CB3 0HE, England. [Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile. [Bond, J. R.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse 4, France. [Challinor, A.; Shellard, P.] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England. [Starck, J. -L.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Juvela, M.; Keihanen, E.; Keskitalo, R.; Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Smoot, G. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Leonardi, R.; Lubin, P. M.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy. [Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Balbi, A.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Kneissl, R.] European So Observ, ESO Vitacura, Santiago 19, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain. [Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands. [Partridge, B.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA. [Kurki-Suonio, H.; Lahteenmaki, A.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland. [Umana, G.] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy. [Bonaldi, A.; de Zotti, G.] Osserv Astron Padova, INAF, Padua, Italy. [Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Maino, D.; Tomasi, M.] INAF IASF Milano, Milan, Italy. [Stivoli, F.] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France. [Desert, F. -X.] Univ Grenoble 1, IPAG, CNRS INSU, UMR 5274, F-38041 Grenoble, France. [Tuerler, M.] Univ Geneva, ISDC Data Ctr Astrophys, Versoix, Switzerland. [Chary, R. -R.; Ganga, K.; Rusholme, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France. [Aghanim, N.; Aumont, J.; Dole, H.; Douspis, M.; Lagache, G.; Miville-Deschenes, M. -A.; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Torre, J. -P.] Univ Paris 11, Inst Astrophys Spatiale, CNRS UMR 8617, F-91405 Orsay, France. [Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Univ Paris 06, Inst Astrophys Paris, CNRS UMR 7095, Paris, France. [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Donzelli, S.; Hansen, F. K.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Hildebrandt, S. R.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Davies, R. D.; Davis, R. J.; Dickinson, C.; Maffei, B.; Peel, M.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Catalano, A.; Coulais, A.; Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Arnaud, M.; Madden, S.; Starck, J. -L.] Univ Paris Diderot, CNRS, CEA Saclay, Lab AIM,IRFU Serv Astrophys,CEA DSM, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] Telecom ParisTech, CNRS UMR 5141, Lab Traitement & Commun Informat, F-75634 Paris 13, France. [Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.] Univ Grenoble 1, Inst Natl Polytech Grenoble, Lab Phys Subatom & Cosmol, CNRS IN2P3, F-38026 Grenoble, France. [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, Lab Accelerateur Lineaire, CNRS IN2P3, F-91405 Orsay, France. [Borrill, J.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Banday, A. J.; Doerl, U.; Ensslin, T. A.; Hovest, W.; Matthai, F.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland. [Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Mann, R.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Clements, DL (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2AZ, England. EM d.clements@imperial.ac.uk RI Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Lahteenmaki, Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014 OI Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Peel, Mike/0000-0003-3412-2586; Galeotta, Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Umana, Grazia/0000-0002-6972-8388; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Savini, Giorgio/0000-0003-4449-9416; de Gasperis, Giancarlo/0000-0003-2899-2171; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822 FU National Aeronautics and Space Administration (NASA); Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; ESA; CNES; CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy); DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU) FX 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. Use was also made of data from the Sloan Digital Sky Survey (SDSS) and the Two Micron All Sky Survey (2MASS). 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/. 2MASS is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.rssd.esa.int/index.php?project=PLANCK\&page=Planck_Collaborat ion. We thank the anonymous referee for many useful comments that have improved this paper. NR 94 TC 65 Z9 65 U1 0 U2 8 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 DEC PY 2011 VL 536 AR A16 DI 10.1051/0004-6361/201116454 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100017 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bock, JJ Bonaldi, A Bond, JR Borrill, J Bot, C Bouchet, FR Boulanger, F Bucher, M Burigana, C Cabella, P Cardoso, JF Catalano, A Cayon, L Challinor, A Chamballu, A Chiang, LY Chiang, C Christensen, PR Clements, DL Colombi, S Couchot, F Coulais, A Crill, BP Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dickinson, C Dobashi, K Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Finelli, F Forni, O Frailis, M Franceschi, E Fukui, Y Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Harrison, D Helou, G Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Jaffe, AH Jones, WC Juvela, M Kawamura, A Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leonardi, R Leroy, C Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Madden, S Maffei, B Mandolesi, N Mann, R Maris, M Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Onishi, T Osborne, S Pajot, F Paladini, R Paradis, D Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Prezeau, G Prunet, S Puget, JL Reach, WT Rebolo, R Reinecke, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Savini, G Scott, D Seiffert, MD Smoot, GF Starck, JL Stivoli, F Stolyarov, V Sudiwala, R Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Tristram, M Tuovinen, J Umana, G Valenziano, L Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Wilkinson, A Ysard, N Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bhatia, R. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bot, C. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Cabella, P. Cardoso, J. -F. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chiang, L. -Y Chiang, C. Christensen, P. R. Clements, D. L. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dickinson, C. Dobashi, K. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Fukui, Y. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Harrison, D. Helou, G. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Jaffe, A. H. Jones, W. C. Juvela, M. Kawamura, A. Keihaenen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leonardi, R. Leroy, C. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Madden, S. Maffei, B. Mandolesi, N. Mann, R. Maris, M. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Onishi, T. Osborne, S. Pajot, F. Paladini, R. Paradis, D. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Prezeau, G. Prunet, S. Puget, J. -L. Reach, W. T. Rebolo, R. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Savini, G. Scott, D. Seiffert, M. D. Smoot, G. F. Starck, J. -L. Stivoli, F. Stolyarov, V. Sudiwala, R. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J. -P. Tristram, M. Tuovinen, J. Umana, G. Valenziano, L. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Wilkinson, A. Ysard, N. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. XVII. Origin of the submillimetre excess dust emission in the Magellanic Clouds SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Magellanic Clouds; dust, extinction; ISM: structure; galaxies: ISM; infrared: galaxies; submillimeter: galaxies ID SPECTRAL ENERGY-DISTRIBUTION; PROBE WMAP OBSERVATIONS; HERSCHEL PHOTOMETRIC-OBSERVATIONS; GIANT MOLECULAR CLOUDS; FORMING DWARF GALAXIES; SPITZER SURVEY; INTERSTELLAR-MEDIUM; APERTURE SYNTHESIS; INFRARED-EMISSION; CENTIMETER EXCESS AB The integrated spectral energy distributions (SED) of the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) appear significantly flatter than expected from dust models based on their far-infrared and radio emission. The still unexplained origin of this millimetre excess is investigated here using the Planck data. The integrated SED of the two galaxies before subtraction of the foreground (Milky Way) and background (CMB fluctuations) emission are in good agreement with previous determinations, confirming the presence of the millimetre excess. In the context of this preliminary analysis we do not propose a full multi-component fitting of the data, but instead subtract contributions unrelated to the galaxies and to dust emission. The background CMB contribution is subtracted using an internal linear combination (ILC) method performed locally around the galaxies. The foreground emission from the Milky Way is subtracted as a Galactic Hi template, and the dust emissivity is derived in a region surrounding the two galaxies and dominated by Milky Way emission. After subtraction, the remaining emission of both galaxies correlates closely with the atomic and molecular gas emission of the LMC and SMC. The millimetre excess in the LMC can be explained by CMB fluctuations, but a significant excess is still present in the SMC SED. The Planck and IRAS-IRIS data at 100 mu m are combined to produce thermal dust temperature and optical depth maps of the two galaxies. The LMC temperature map shows the presence of a warm inner arm already found with the Spitzer data, but which also shows the existence of a previously unidentified cold outer arm. Several cold regions are found along this arm, some of which are associated with known molecular clouds. The dust optical depth maps are used to constrain the thermal dust emissivity power-law index (beta). The average spectral index is found to be consistent with beta = 1.5 and beta = 1.2 below 500 mu m for the LMC and SMC respectively, significantly flatter than the values observed in the Milky Way. Also, there is evidence in the SMC of a further flattening of the SED in the sub-mm, unlike for the LMC where the SED remains consistent with beta = 1.5. The spatial distribution of the millimetre dust excess in the SMC follows the gas and thermal dust distribution. Different models are explored in order to fit the dust emission in the SMC. It is concluded that the millimetre excess is unlikely to be caused by very cold dust emission and that it could be due to a combination of spinning dust emission and thermal dust emission by more amorphous dust grains than those present in our Galaxy. C1 [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Montier, L.; Paradis, D.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.] Univ Paris 07, CNRS UMR7164, Paris, France. [Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile. [Bond, J. R.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Montier, L.; Paradis, D.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse 4, France. [Challinor, A.] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England. [Starck, J. -L.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. [Dobashi, K.] Tokyo Gakugei Univ, Dept Astron & Earth Sci, Tokyo 1848501, Japan. [Onishi, T.] Osaka Prefecture Univ, Grad Sch Sci, Dept Phys Sci, Naka Ku, Sakai, Osaka 5998531, Japan. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Juvela, M.; Keihaenen, E.; Keskitalo, R.; Kurki-Suonio, H.; Poutanen, T.; Ysard, N.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Fukui, Y.; Kawamura, A.] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Chiang, C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Smoot, G. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Leonardi, R.; Lubin, P. M.; Meinhold, P. R.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Nati, F.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, Rome, Italy. [Bersanelli, M.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy. [Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Balbi, A.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Kneissl, R.] European So Observ, ESO Vitacura, Santiago 19, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain. [Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands. [Kurki-Suonio, H.; Lahteenmaki, A.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland. [Umana, G.] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy. [Bonaldi, A.; de Zotti, G.] Osserv Astron Padova, INAF, Padua, Italy. [Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Tomasi, M.] INAF IASF Milano, Milan, Italy. [Stivoli, F.] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France. [Desert, F. -X.] Univ Grenoble 1, IPAG, CNRS INSU, UMR 5274, F-38041 Grenoble, France. [Chamballu, A.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Ganga, K.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France. [Aghanim, N.; Aumont, J.; Boulanger, F.; Douspis, M.; Lagache, G.; Leroy, C.; Miville-Deschenes, M. -A.; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Torre, J. -P.] Univ Paris 11, Inst Astrophys Spatiale, CNRS UMR8617, Orsay, France. [Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Univ Paris 06, Inst Astrophys Paris, CNRS UMR7095, Paris, France. [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Donzelli, S.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Hildebrandt, S. R.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Davies, R. D.; Davis, R. J.; Dickinson, C.; Maffei, B.; Wilkinson, A.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. 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A.; Hovest, W.; Matthai, F.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland. [Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Bot, C.] CNRS, Observ Astronom Strasbourg, UMR 7550, F-67000 Strasbourg, France. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Mann, R.] Univ Edinburgh, Inst Astron, Royal Observ, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Paladini, R.] Spitzer Sci Ctr, Pasadena, CA USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, Warsaw, Poland. RP Bernard, JP (reprint author), Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. EM jean-philippe.bernard@cesr.fr RI Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Nati, Federico/I-4469-2016; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Lahteenmaki, Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; OI WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Ricciardi, Sara/0000-0002-3807-4043; Pasian, Fabio/0000-0002-4869-3227; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Masi, Silvia/0000-0001-5105-1439; Bot, Caroline/0000-0001-6118-2985; de Gasperis, Giancarlo/0000-0003-2899-2171; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Reach, William/0000-0001-8362-4094; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Savini, Giorgio/0000-0003-4449-9416; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794 NR 97 TC 90 Z9 90 U1 0 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A17 DI 10.1051/0004-6361/201116473 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100018 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Blagrave, K Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bucher, M Burigana, C Cabella, P Cardoso, JF Catalano, A Cayon, L Challinor, A Chamballu, A Chiang, LY Chiang, C Christensen, PR Clements, DL Colombi, S Couchot, F Coulais, A Crill, BP Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dole, H Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Fosalba, P Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Grain, J Gratton, S Gregorio, A Gruppuso, A Hansen, FK Harrison, D Helou, G Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Jaffe, AH Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leonardi, R Leroy, C Lilje, PB Linden-Vornle, M Lockman, FJ Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Maffei, B Maino, D Mandolesi, N Mann, R Maris, M Martin, P Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, P Melchiorri, A Mendes, L Mennella, A Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Novikov, D Novikov, I O'Dwyer, IJ Oliver, S Osborne, S Pajot, F Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Goncalves, DP Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, P Smoot, GF Starck, JL Stivoli, F Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Tristram, M Tuovinen, J Umana, G Valenziano, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD White, M Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bhatia, R. Blagrave, K. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bucher, M. Burigana, C. Cabella, P. Cardoso, J. -F. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chiang, L. -Y Chiang, C. Christensen, P. R. Clements, D. L. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dole, H. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Fosalba, P. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Grain, J. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Harrison, D. Helou, G. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Jaffe, A. H. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leonardi, R. Leroy, C. Lilje, P. B. Linden-Vornle, M. Lockman, F. J. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Maino, D. Mandolesi, N. Mann, R. Maris, M. Martin, P. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. Melchiorri, A. Mendes, L. Mennella, A. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Novikov, D. Novikov, I. O'Dwyer, I. J. Oliver, S. Osborne, S. Pajot, F. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Goncalves, D. Pinheiro Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, P. Smoot, G. F. Starck, J. -L. Stivoli, F. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J. -P. Tristram, M. Tuovinen, J. Umana, G. Valenziano, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. White, M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. XVIII. The power spectrum of cosmic infrared background anisotropies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE diffuse radiation; submillimeter: diffuse background; submillimeter: galaxies; cosmology: observations ID STAR-FORMATION HISTORY; SOUTH-POLE TELESCOPE; PRE-LAUNCH STATUS; MULTIBAND IMAGING PHOTOMETER; HALO OCCUPATION DISTRIBUTION; SUBMILLIMETER NUMBER COUNTS; HIGH GALACTIC LATITUDE; FUTURE LARGE SURVEYS; DEEP FIELD SOUTH; 500 MU-M AB Using Planck maps of six regions of low Galactic dust emission with a total area of about 140 deg(2), we determine the angular power spectra of cosmic infrared background (CIB) anisotropies from multipole l = 200 to l = 2000 at 217, 353, 545 and 857 GHz. We use 21-cm observations of Hi as a tracer of thermal dust emission to reduce the already low level of Galactic dust emission and use the 143 GHz Planck maps in these fields to clean out cosmic microwave background anisotropies. Both of these cleaning processes are necessary to avoid significant contamination of the CIB signal. We measure correlated CIB structure across frequencies. As expected, the correlation decreases with increasing frequency separation, because the contribution of high-redshift galaxies to CIB anisotropies increases with wavelengths. We find no significant difference between the frequency spectrum of the CIB anisotropies and the CIB mean, with Delta I/I = 15% from 217 to 857 GHz. In terms of clustering properties, the Planck data alone rule out the linear scale-and redshift-independent bias model. Non-linear corrections are significant. Consequently, we develop an alternative model that couples a dusty galaxy, parametric evolution model with a simple halo-model approach. It provides an excellent fit to the measured anisotropy angular power spectra and suggests that a different halo occupation distribution is required at each frequency, which is consistent with our expectation that each frequency is dominated by contributions from different redshifts. In our best-fit model, half of the anisotropy power at l = 2000 comes from redshifts z < 0.8 at 857 GHz and z < 1.5 at 545 GHz, while about 90% come from redshifts z > 2 at 353 and 217 GHz, respectively. C1 [Aghanim, N.; Aumont, J.; Dole, H.; Douspis, M.; Grain, J.; Lagache, G.; Leroy, C.; Miville-Deschenes, M. -A.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Torre, J. -P.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France. [Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Smoot, G. F.; Stompor, R.] Univ Paris 07, CNRS, UMR7164, Paris, France. [Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile. [Bonavera, L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Blagrave, K.; Bond, J. R.; Martin, P.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse, France. [Ganga, K.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Lilje, P. B.] Univ Oslo, Ctr Math Applicat, Oslo, Norway. [Challinor, A.; Shellard, P.] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England. [Starck, J. -L.; Yvon, D.] CEA Saclay, DSM, Irfu, SPP, F-91191 Gif Sur Yvette, France. [Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Netterfield, C. B.; Goncalves, D. Pinheiro] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Oliver, S.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Juvela, M.; Keihanen, E.; Keskitalo, R.; Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Chiang, C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Smoot, G. F.; White, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Leonardi, R.; Lubin, P. M.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA. [Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy. [Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Balbi, A.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Kneissl, R.] European So Observ, ESO Vitacura, Santiago 19, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain. [Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] Estec, European Space Agcy, NL-2201 AZ Noordwijk, Netherlands. [Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland. [Umana, G.] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy. [Bonaldi, A.; de Zotti, G.] Osserv Astron Padova, INAF, Padua, Italy. [Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] IASF Bologna, INAF, Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Maino, D.; Tomasi, M.] IASF Milano, INAF, Milan, Italy. [Stivoli, F.] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France. [Desert, F. -X.] Univ Grenoble 1, CNRS, IPAG, INSU,UMR 5274, F-38041 Grenoble, France. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France. [Chamballu, A.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, Paris, France. [Fosalba, P.] Fac Ciencies, Inst Ciencies Espai, CSIC, IEEC, Bellaterra 08193, Spain. [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Donzelli, S.; Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Hildebrandt, S. R.; Hoyland, R. J.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, Inst Fis Cantabria, CSIC, E-39005 Santander, Spain. [Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; Mitra, S.; O'Dwyer, I. J.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Davies, R. D.; Davis, R. J.; Maffei, B.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. 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[Borrill, J.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Tuovinen, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland. [Lockman, F. J.] NRAO, Green Bank, WV 24944 USA. [Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Co Kildare, Ireland. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Bonavera, L.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Mann, R.] Univ Edinburgh, SUPA, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS, OMP, IRAP, F-31028 Toulouse 4, France. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Lagache, G (reprint author), Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, Batiment 121, F-91405 Orsay, France. EM guilaine.lagache@ias.u-psud.fr RI Remazeilles, Mathieu/N-1793-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015; Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Fosalba Vela, Pablo/I-5515-2016; Novikov, Igor/N-5098-2015; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; bonavera, laura/E-9368-2017; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Lilje, Per/A-2699-2012; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Oliver, Seb/A-2479-2013; Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; OI Matarrese, Sabino/0000-0002-2573-1243; Ricciardi, Sara/0000-0002-3807-4043; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Masi, Silvia/0000-0001-5105-1439; Melchiorri, Alessandro/0000-0001-5326-6003; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; bonavera, laura/0000-0001-8039-3876; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; de Gasperis, Giancarlo/0000-0003-2899-2171; Oliver, Seb/0000-0001-7862-1032; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Savini, Giorgio/0000-0003-4449-9416; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115 FU ESA; CNES; CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy); NASA; DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU) FX This paper has made use of modelling tools that were made available by Matthieu Bethermin and Aurelie Penin. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.rssd.esa.int/Planck. NR 117 TC 126 Z9 127 U1 2 U2 14 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 DEC PY 2011 VL 536 AR A18 DI 10.1051/0004-6361/201116461 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100019 ER PT J AU Ade, PAR Aghanim, N Argueso, F Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Bernard, JP Bersanelli, M Bhatia, R Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bucher, M Burigana, C Cabella, P Cappellini, B Cardoso, JF Catalano, A Cayon, L Challinor, A Chamballu, A Chary, RR Chen, X Chiang, LY Christensen, PR Clements, DL Colafrancesco, S Colombi, S Couchot, F Crill, BP Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dickinson, C Dole, H Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Harrison, D Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Jaffe, AH Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lahteenmaki, A Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leahy, JP Leonardi, R Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Magliocchetti, M Maino, D Mandolesi, N Mann, R Maris, M Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I O'Dwyer, IJ Osborne, S Pajot, F Paladini, R Partridge, B Pasian, F Patanchon, G Pearson, TJ Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Plaszczynski, S Platania, P Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sajina, A Sandri, M Scott, D Seiffert, MD Serjeant, S Shellard, P Smoot, GF Starck, JL Stivoli, F Stolyarov, V Stompor, R Sudiwala, R Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Tristram, M Tuovinen, J Turler, M Umana, G Valenziano, L Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Wilkinson, A Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Argueeso, F. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Bernard, J-P. Bersanelli, M. Bhatia, R. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bucher, M. Burigana, C. Cabella, P. Cappellini, B. Cardoso, J-F. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chary, R-R. Chen, X. Chiang, L-Y. Christensen, P. R. Clements, D. L. Colafrancesco, S. Colombi, S. Couchot, F. Crill, B. P. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J-M. Desert, F-X. Dickinson, C. Dole, H. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Harrison, D. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Jaffe, A. H. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leahy, J. P. Leonardi, R. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Magliocchetti, M. Maino, D. Mandolesi, N. Mann, R. Maris, M. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Miville-Deschenes, M-A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. O'Dwyer, I. J. Osborne, S. Pajot, F. Paladini, R. Partridge, B. Pasian, F. Patanchon, G. Pearson, T. J. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Plaszczynski, S. Platania, P. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Prezeau, G. Prunet, S. Puget, J-L. Rachen, J. P. Rebolo, R. Reinecke, M. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sajina, A. Sandri, M. Scott, D. Seiffert, M. D. Serjeant, S. Shellard, P. Smoot, G. F. Starck, J-L. Stivoli, F. Stolyarov, V. Stompor, R. Sudiwala, R. Sygnet, J-F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J-P. Tristram, M. Tuovinen, J. Tuerler, M. Umana, G. Valenziano, L. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Wilkinson, A. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. XIII. Statistical properties of extragalactic radio sources in the Planck Early Release Compact Source Catalogue SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE surveys; radio continuum: general; galaxies: active ID PRE-LAUNCH STATUS; COEVAL OBSERVATIONS PROJECT; SOURCE COUNTS; GHZ; POLARIZATION; SAMPLE; ANISOTROPIES; PREDICTIONS; MISSION; FIELD AB The data reported in Planck's Early Release Compact Source Catalogue (ERCSC) are exploited to measure the number counts (dN/dS) of extragalactic radio sources at 30, 44, 70, 100, 143 and 217 GHz. Due to the full-sky nature of the catalogue, this measurement extends to the rarest and brightest sources in the sky. At lower frequencies (30, 44, and 70 GHz) our counts are in very good agreement with estimates based on WMAP data, being somewhat deeper at 30 and 70 GHz, and somewhat shallower at 44 GHz. Planck's source counts at 143 and 217 GHz join smoothly with the fainter ones provided by the SPT and ACT surveys over small fractions of the sky. An analysis of source spectra, exploiting Planck's uniquely broad spectral coverage, finds clear evidence of a steepening of the mean spectral index above about 70 GHz. This implies that, at these frequencies, the contamination of the CMB power spectrum by radio sources below the detection limit is significantly lower than previously estimated. C1 [Baccigalupi, C.; Bonavera, L.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kymala 02540, Finland. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Bartlett, J. G.; Bucher, M.; Cardoso, J-F.; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.; Stompor, R.] Univ Paris 07, CNRS, UMR7164, Paris, France. 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EM gnuevo@sissa.it RI Gonzalez-Nuevo, Joaquin/I-3562-2014; Pearson, Timothy/N-2376-2015; Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; bonavera, laura/E-9368-2017; Lilje, Per/A-2699-2012; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Lahteenmaki, Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015 OI Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Pierpaoli, Elena/0000-0002-7957-8993; Galeotta, Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Masi, Silvia/0000-0001-5105-1439; Melchiorri, Alessandro/0000-0001-5326-6003; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Magliocchetti, Manuela/0000-0001-9158-4838; Morgante, Gianluca/0000-0001-9234-7412; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Pearson, Timothy/0000-0001-5213-6231; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; bonavera, laura/0000-0001-8039-3876; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Frailis, Marco/0000-0002-7400-2135; de Gasperis, Giancarlo/0000-0003-2899-2171; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590 FU European Space Agency (ESA); NASA (USA); CNES; CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy); NASA; DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU) FX Planck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states (in particular the lead countries: France and Italy) with contributions from NASA (USA), and telescope reflectors provided in a collaboration between ESA and a scientific consortium led and funded by Denmark.; The Planck Collaboration thanks the referee, Ronald Ekers, for his insightful comments, which helped improve the paper. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). A description of the Planck Collaboration and a list of its members can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page=Planck_Collaborati on NR 61 TC 77 Z9 77 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A13 DI 10.1051/0004-6361/201116471 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100014 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartelmann, M Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Bourdin, H Brown, ML Bucher, M Burigana, C Cabella, P Cardoso, JF Catalano, A Cayon, L Challinor, A Chamballu, A Chiang, LY Chiang, C Chon, G Christensen, PR Churazov, E Clements, DL Colafrancesco, S Colombi, S Couchot, F Coulais, A Crill, BP Cuttaia, F Da Silva, A Dahle, H Danese, L de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Diego, JM Dolag, K Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Finelli, F Flores-Cacho, I Forni, O Frailis, M Franceschi, E Fromenteau, S Galeotta, S Ganga, K Genova-Santos, RT Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Harrison, D Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Jaffe, AH Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lamarre, JM Lanoux, J Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leonardi, R Liddle, A Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Maffei, B Maino, D Mandolesi, N Mann, R Maris, M Marleau, F Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, P Melchiorri, A Melin, JB Mendes, L Mennella, A Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Pajot, F Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Piffaretti, R Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Schaefer, BM Scott, D Seiffert, MD Shellard, P Smoot, GF Starck, JL Stivoli, F Stolyarov, V Sudiwala, R Sunyaev, R Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Tristram, M Tuovinen, J Valenziano, L Vibert, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD White, SDM White, M Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartelmann, M. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bhatia, R. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Bourdin, H. Brown, M. L. Bucher, M. Burigana, C. Cabella, P. Cardoso, J. -F. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chiang, L. -Y Chiang, C. Chon, G. Christensen, P. R. Churazov, E. Clements, D. L. Colafrancesco, S. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Cuttaia, F. Da Silva, A. Dahle, H. Danese, L. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Diego, J. M. Dolag, K. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Finelli, F. Flores-Cacho, I. Forni, O. Frailis, M. Franceschi, E. Fromenteau, S. Galeotta, S. Ganga, K. Genova-Santos, R. T. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Harrison, D. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Jaffe, A. H. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lanoux, J. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leonardi, R. Liddle, A. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Maino, D. Mandolesi, N. Mann, R. Maris, M. Marleau, F. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. Melchiorri, A. Melin, J. -B. Mendes, L. Mennella, A. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Pajot, F. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Piffaretti, R. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Schaefer, B. M. Scott, D. Seiffert, M. D. Shellard, P. Smoot, G. F. Starck, J. -L. Stivoli, F. Stolyarov, V. Sudiwala, R. Sunyaev, R. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J. -P. Tristram, M. Tuovinen, J. Valenziano, L. Vibert, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. White, S. D. M. White, M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. XI. Calibration of the local galaxy cluster Sunyaev-Zeldovich scaling relations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: interacluster medium; X-rays: galaxies: clusters; cosmology: observations ID X-RAY LUMINOSITY; SOUTH-POLE TELESCOPE; PRE-LAUNCH STATUS; ATACAMA COSMOLOGY TELESCOPE; STRUCTURE SURVEY REXCESS; XMM-NEWTON; REPRESENTATIVE SAMPLE; RX J1347-1145; TEMPERATURE PROFILES; PARAMETER-ESTIMATION AB We present precise Sunyaev-Zeldovich (SZ) effect measurements in the direction of 62 nearby galaxy clusters (z < 0.5) detected at high signal-to-noise in the first Planck all-sky data set. The sample spans approximately a decade in total mass, 2 x 10(14) M-circle dot < M-500 < 2 x 10(15) M-circle dot, where M-500 is the mass corresponding to a total density contrast of 500. Combining these high quality Planck measurements with deep XMM-Newton X-ray data, we investigate the relations between D-A(2) Y-500, the integrated Compton parameter due to the SZ effect, and the X-ray-derived gas mass M-g,M-500, temperature T-X, luminosity L-X,L-500, SZ signal analogue Y-X,Y-500 = M-g,M-500 x T-X, and total mass M-500. After correction for the effect of selection bias on the scaling relations, we find results that are in excellent agreement with both X-ray predictions and recently-published ground-based data derived from smaller samples. The present data yield an exceptionally robust, high-quality local reference, and illustrate Planck's unique capabilities for all-sky statistical studies of galaxy clusters. C1 [Arnaud, M.; Piffaretti, R.; Pratt, G. W.; Starck, J. -L.] Univ Paris Diderot, CEA Saclay, CEA, Lab AIM,IRFU,Serv Astrophys,DSM,CNRS, F-91191 Gif Sur Yvette, France. [Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Fromenteau, S.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.] Univ Paris 07, CNRS, UMR7164, Paris, France. [Ashdown, M.; Brown, M. L.; Chon, G.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile. [Bond, J. R.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse 4, France. [Dahle, H.; Lilje, P. B.] Univ Oslo, Ctr Math Applicat, Oslo, Norway. [Da Silva, A.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Challinor, A.; Shellard, P.] Univ Cambridge, Ctr Math Sci, DAMTP, Cambridge CB3 0WA, England. [Melin, J. -B.; Piffaretti, R.; Starck, J. -L.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Marleau, F.; Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Pierpaoli, E.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA USA. [Liddle, A.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Juvela, M.; Keihanen, E.; Keskitalo, R.; Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Chiang, C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Smoot, G. F.; White, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Leonardi, R.; Lubin, P. M.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA. [Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Balbi, A.; Bourdin, H.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Flores-Cacho, I.; Genova-Santos, R. T.; Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, Tenerife, Spain. [Kneissl, R.] European So Observ, ESO Vitacura, Santiago 19, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain. [Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands. [Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland. [Bonaldi, A.; de Zotti, G.] Osserv Astron Padova, INAF, Padua, Italy. [Colafrancesco, S.; Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Maino, D.; Tomasi, M.] INAF IASF Milano, Milan, Italy. [Stivoli, F.] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France. [Desert, F. -X.] Univ Grenoble 1, CNRS, IPAG, INSU,UMR 5274, F-38041 Grenoble, France. [Chamballu, A.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Ganga, K.; Rusholme, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France. [Aghanim, N.; Aumont, J.; Douspis, M.; Fromenteau, S.; Lagache, G.; Miville-Deschenes, M. -A.; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Torre, J. -P.; Vibert, L.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France. [Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, Paris, France. [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Dahle, H.; Donzelli, S.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Flores-Cacho, I.; Genova-Santos, R. T.; Hildebrandt, S. R.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Diego, J. M.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; Mitra, S.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Maffei, B.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Brown, M. L.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Catalano, A.; Coulais, A.; Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Cardoso, J. -F.] CNRS, UMR 5141, Lab Traitement & Commun Informat, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, CNRS, IN2P3, Lab Phys Subatom & Cosmol,Inst Natl Polytech Gren, F-38026 St Martin Dheres, France. [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, Lab Accelerateur Lineaire, CNRS, IN2P3, F-91405 Orsay, France. [Borrill, J.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Banday, A. J.; Bartelmann, M.; Churazov, E.; Dolag, K.; Doerl, U.; Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Matthai, F.; Rachen, J. P.; Reinecke, M.; Riller, T.; Sunyaev, R.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Chon, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Tuovinen, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland. [Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Mann, R.] Univ Edinburgh, Royal Observ, SUPA, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Churazov, E.; Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Bartelmann, M.; Schaefer, B. M.] Heidelberg Univ, Inst Theoret Phys, D-69120 Heidelberg, Germany. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Lanoux, J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Pratt, GW (reprint author), Univ Paris Diderot, CEA Saclay, CEA, Lab AIM,IRFU,Serv Astrophys,DSM,CNRS, Bat 709, F-91191 Gif Sur Yvette, France. EM gabriel.pratt@cea.fr RI Lilje, Per/A-2699-2012; Barreiro, Rita Belen/N-5442-2014; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Churazov, Eugene/A-7783-2013; Lopez-Caniego, Marcos/M-4695-2013; Da Silva, Antonio/A-2693-2010; Bartelmann, Matthias/A-5336-2014; Bouchet, Francois/B-5202-2014; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015; Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; OI Barreiro, Rita Belen/0000-0002-6139-4272; de Gasperis, Giancarlo/0000-0003-2899-2171; Da Silva, Antonio/0000-0002-6385-1609; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Pierpaoli, Elena/0000-0002-7957-8993; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Savini, Giorgio/0000-0003-4449-9416; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115; Matarrese, Sabino/0000-0002-2573-1243; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Masi, Silvia/0000-0001-5105-1439; Melchiorri, Alessandro/0000-0001-5326-6003; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104 FU ESA; CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy); NASA; DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU); USA (NASA); Centre National d'Etudes Spatiales (CNES) FX The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). The present work is partly based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). This research has made use of the following databases: SIMBAD, operated at CDS, Strasbourg, France; the NED database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; BAX, which is operated by the Laboratoire d'Astrophysique de Tarbes-Toulouse (LATT), under contract with the Centre National d'Etudes Spatiales (CNES). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.rssd.esa.int/Planck. NR 88 TC 110 Z9 110 U1 1 U2 10 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A11 DI 10.1051/0004-6361/201116458 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100012 ER PT J AU Ade, PAR Aghanim, N Ansari, R Arnaud, M Ashdown, M Aumont, J Banday, AJ Bartelmann, M Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bock, JJ Bond, JR Borrill, J Bouchet, FR Boulanger, F Bradshaw, T Breelle, E Bucher, M Camus, P Cardoso, JF Catalano, A Challinor, A Chamballu, A Charra, J Charra, M Chary, RR Chiang, C Church, S Clements, DL Colombi, S Couchot, F Coulais, A Cressiot, C Crill, BP Crook, M de Bernardis, P Delabrouille, J Delouis, JM Desert, FX Dolag, K Dole, H Dore, O Douspis, M Efstathiou, G Eng, P Filliard, C Forni, O Fosalba, P Fourmond, JJ Ganga, K Giard, M Girard, D Giraud-Heraud, Y Gispert, R Gorski, KM Gratton, S Griffin, M Guyot, G Haissinski, J Harrison, D Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Hildebrandt, SR Hills, R Hivon, E Hobson, M Holmes, WA Huffenberger, KM Jaffe, AH Jones, WC Kaplan, J Kneissl, R Knox, L Lagache, G Lamarre, JM Lami, P Lange, AE Lasenby, A Lavabre, A Lawrence, CR Leriche, B Leroy, C Longval, Y Macias-Perez, JF Maciaszek, T MacTavish, CJ Maffei, B Mandolesi, N Mann, R Mansoux, B Masi, S Matsumura, T McGehee, P Melin, JB Mercier, C Miville-Deschenes, MA Moneti, A Montier, L Mortlock, D Murphy, A Nati, F Netterfield, CB Norgaard-Nielsen, HU North, C Noviello, F Novikov, D Osborne, S Paine, C Pajot, F Patanchon, G Peacocke, T Pearson, TJ Perdereau, O Perotto, L Piacentini, F Piat, M Plaszczynski, S Pointecouteau, E Pons, R Ponthieu, N Prezeau, G Prunet, S Puget, JL Reach, WT Renault, C Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rusholme, B Santos, D Savini, G Schaefer, BM Shellard, P Spencer, L Starck, JL Stassi, P Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sygnet, JF Tauber, JA Thum, C Torre, JP Touze, F Tristram, M Van Leeuwen, F Vibert, L Vibert, D Wade, LA Wandelt, BD White, SDM Wiesemeyer, H Woodcraft, A Yurchenko, V Yvon, D Zacchei, A AF Ade, P. A. R. Aghanim, N. Ansari, R. Arnaud, M. Ashdown, M. Aumont, J. Banday, A. J. Bartelmann, M. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bhatia, R. Bock, J. J. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bradshaw, T. Breelle, E. Bucher, M. Camus, P. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Charra, J. Charra, M. Chary, R. -R. Chiang, C. Church, S. Clements, D. L. Colombi, S. Couchot, F. Coulais, A. Cressiot, C. Crill, B. P. Crook, M. de Bernardis, P. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dolag, K. Dole, H. Dore, O. Douspis, M. Efstathiou, G. Eng, P. Filliard, C. Forni, O. Fosalba, P. Fourmond, J. -J. Ganga, K. Giard, M. Girard, D. Giraud-Heraud, Y. Gispert, R. Gorski, K. M. Gratton, S. Griffin, M. Guyot, G. Haissinski, J. Harrison, D. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Hildebrandt, S. R. Hills, R. Hivon, E. Hobson, M. Holmes, W. A. Huffenberger, K. M. Jaffe, A. H. Jones, W. C. Kaplan, J. Kneissl, R. Knox, L. Lagache, G. Lamarre, J. -M. Lami, P. Lange, A. E. Lasenby, A. Lavabre, A. Lawrence, C. R. Leriche, B. Leroy, C. Longval, Y. Macias-Perez, J. F. Maciaszek, T. MacTavish, C. J. Maffei, B. Mandolesi, N. Mann, R. Mansoux, B. Masi, S. Matsumura, T. McGehee, P. Melin, J. -B. Mercier, C. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Mortlock, D. Murphy, A. Nati, F. Netterfield, C. B. Norgaard-Nielsen, H. U. North, C. Noviello, F. Novikov, D. Osborne, S. Paine, C. Pajot, F. Patanchon, G. Peacocke, T. Pearson, T. J. Perdereau, O. Perotto, L. Piacentini, F. Piat, M. Plaszczynski, S. Pointecouteau, E. Pons, R. Ponthieu, N. Prezeau, G. Prunet, S. Puget, J. -L. Reach, W. T. Renault, C. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rusholme, B. Santos, D. Savini, G. Schaefer, B. M. Shellard, P. Spencer, L. Starck, J. -L. Stassi, P. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sygnet, J. -F. Tauber, J. A. Thum, C. Torre, J. -P. Touze, F. Tristram, M. Van Leeuwen, F. Vibert, L. Vibert, D. Wade, L. A. Wandelt, B. D. White, S. D. M. Wiesemeyer, H. Woodcraft, A. Yurchenko, V. Yvon, D. Zacchei, A. CA Planck HFI Core Team TI Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation: detectors; methods: data analysis; instrumentation: photometers; cosmic background radiation; cosmology: observations ID PRE-LAUNCH STATUS; POWER SPECTRUM; BOOMERANG; HFI; BOLOMETERS; ANISOTROPY; MISSION; SYSTEM; CALIBRATION; CRYOCOOLER AB The Planck High Frequency Instrument (HFI) is designed to measure the temperature and polarization anisotropies of the cosmic microwave background and Galactic foregrounds in six similar to 30% bands centered at 100, 143, 217, 353, 545, and 857 GHz at an angular resolution of 10' (100 GHz), 7' (143 GHz), and 5' (217 GHz and higher). HFI has been operating flawlessly since launch on 14 May 2009, with the bolometers reaching 100 mK the first week of July. The settings of the readout electronics, including bolometer bias currents, that optimize HFI's noise performance on orbit are nearly the same as the ones chosen during ground testing. Observations of Mars, Jupiter, and Saturn have confirmed that the optical beams and the time responses of the detection chains are in good agreement with the predictions of physical optics modeling and pre-launch measurements. The Detectors suffer from a high flux of cosmic rays due to historically low levels of solar activity. As a result of the redundancy of Planck's observation strategy, the removal of a few percent of data contaminated by glitches does not significantly affect the instrumental sensitivity. The cosmic ray flux represents a significant and variable heat load on the sub-Kelvin stage. Temporal variation and the inhomogeneous distribution of the flux results in thermal fluctuations that are a probable source of low frequency noise. The removal of systematic effects in the time ordered data provides a signal with an average noise equivalent power that is 70% of the goal in the 0.6-2.5 Hz range. This is slightly higher than was achieved during the pre-launch characterization but better than predicted in the early phases of the project. The improvement over the goal is a result of the low level of instrumental background loading achieved by the optical and thermal design of the HFI. C1 [Catalano, A.; Coulais, A.; Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Bartlett, J. G.; Benoit, A.; Breelle, E.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Challinor, A.; Chamballu, A.; Cressiot, C.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Kaplan, J.; Patanchon, G.; Piat, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris 07, CNRS, UMR 7164, Paris, France. [Ashdown, M.; Hills, R.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile. [Bond, J. R.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Maciaszek, T.] CNES, F-31401 Toulouse 9, France. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Montier, L.; Pointecouteau, E.; Pons, R.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse 4, France. [Bock, J. J.; Crill, B. P.; Dore, O.; Helou, G.; Hildebrandt, S. R.; Matsumura, T.; Pearson, T. J.; Prezeau, G.; Rocha, G.] CALTECH, Pasadena, CA 91125 USA. [Challinor, A.; Shellard, P.] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England. [Melin, J. -B.; Starck, J. -L.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. [Chiang, C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA. [de Bernardis, P.; Masi, S.; Nati, F.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.] Univ Milan, Dipartimento Fis, Milan, Italy. [Kneissl, R.] ESO Vitacura, European So Observ, Santiago, Chile. [Tauber, J. A.] ESTEC, European Space Agcy, NL-2201 AZ Noordwijk, Netherlands. [Zacchei, A.] INAF Osservatorio Astron Trieste, Trieste, Italy. [Mandolesi, N.] INAF IASF Bologna, Bologna, Italy. [Bersanelli, M.] INAF IASF Milano, Milan, Italy. [Guyot, G.] CNRS, Inst Sci Univers, INSU, F-75794 Paris 16, France. [Desert, F. -X.] Univ Grenoble 1, Grenoble CNRS INSU 1, UMR 5274, IPAG, F-38041 Grenoble, France. [Chamballu, A.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Chary, R. -R.; Ganga, K.; Lange, A. E.; McGehee, P.; Pearson, T. J.; Rusholme, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Benoit, A.; Camus, P.] Univ Grenoble 1, CNRS, Inst Neel, F-38041 Grenoble, France. [Aghanim, N.; Aumont, J.; Boulanger, F.; Charra, J.; Charra, M.; Dole, H.; Douspis, M.; Eng, P.; Fourmond, J. -J.; Gispert, R.; Lagache, G.; Lami, P.; Leriche, B.; Leroy, C.; Longval, Y.; Mercier, C.; Miville-Deschenes, M. -A.; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Torre, J. -P.; Vibert, L.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France. [Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, Paris, France. [Fosalba, P.] Fac Ciencies, CSIC IEEC, Inst Ciencies Espai, Bellaterra 08193, Spain. [Wiesemeyer, H.] Inst Radioastron Millimetrique IRAM, Granada 18012, Spain. [Thum, C.] Inst Radioastron Millimetr IRAM, F-38406 Grenoble, France. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Van Leeuwen, F.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Hildebrandt, S. R.] Inst Astrofis Canarias, Tenerife, Spain. [Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Lawrence, C. R.; Paine, C.; Prezeau, G.; Rocha, G.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Maffei, B.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Arnaud, M.; Starck, J. -L.] Univ Paris Diderot, CNRS, DSM, Lab AIM,IRFU,Serv Astrophys,CEA, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris, France. [Vibert, D.] Lab Astrophys Marseille, F-13388 Marseille 13, France. [Girard, D.; Hildebrandt, S. R.; Macias-Perez, J. 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RP Lamarre, JM (reprint author), Observ Paris, CNRS, LERMA, 61 Ave Observ, F-75014 Paris, France. EM jean-michel.lamarre@obspm.fr RI Bartelmann, Matthias/A-5336-2014; Bouchet, Francois/B-5202-2014; Battaner, Eduardo/P-7019-2014; Yvon, Dominique/D-2280-2015; Pearson, Timothy/N-2376-2015; Fosalba Vela, Pablo/I-5515-2016; Nati, Federico/I-4469-2016; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; OI Pearson, Timothy/0000-0001-5213-6231; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Masi, Silvia/0000-0001-5105-1439; Hivon, Eric/0000-0003-1880-2733; Savini, Giorgio/0000-0003-4449-9416; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; WANDELT, Benjamin/0000-0002-5854-8269; Huffenberger, Kevin/0000-0001-7109-0099; Bouchet, Francois/0000-0002-8051-2924; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Zacchei, Andrea/0000-0003-0396-1192 FU CNES; CNRS; NASA; STFC; ASI; ESA; CNRS/INSU-IN2P3-INP (France); CNR; INAF (Italy); DoE (USA); UKSA (UK); CSIC; MICINN (Spain); Tekes; AoF (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); Swiss Funding Agency (Switzerland); Norwegian Funding Agency (Norway); FCT/MCTES (Portugal) FX The Planck HFI instrument (http://hfi.planck.fr/) was designed and built by an international consortium of laboratories, universities and institutes, with important contributions from the industry, under the leadership of the PI institute, IAS at Orsay, France. It was funded in particular by CNES, CNRS, NASA, STFC and ASI. The authors extend their gratitude to the numerous engineers and scientists, who have contributed to the design, development, construction or evaluation of the HFI instrument. A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.rssd.esa.int/index.php?project=PLANCK\&page=Planck_Collaborat ion. The Planck Collaboration acknowledges financial support from: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC and MICINN (Spain); Tekes and AoF (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); Swiss Funding Agency (Switzerland); Norwegian Funding Agency (Norway); and FCT/MCTES (Portugal). NR 68 TC 106 Z9 106 U1 0 U2 12 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A4 DI 10.1051/0004-6361/201116487 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100005 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Baker, M Balbi, A Banday, AJ Barreiro, RB Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhandari, P Bhatia, R Bock, JJ Bonaldi, A Bond, JR Borders, J Borrill, J Bouchet, FR Bowman, B Bradshaw, T Breelle, E Bucher, M Burigana, C Butler, RC Cabella, P Camus, P Cantalupo, CM Cappellini, B Cardoso, JF Catalano, A Cayon, L Challinor, A Chamballu, A Chambelland, JP Charra, J Charra, M Chiang, LY Chiang, C Christensen, PR Clements, DL Collaudin, B Colombi, S Couchot, F Coulais, A Crill, BP Crook, M Cuttaia, F Damasio, C Danese, L Davies, RD Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A Delabrouille, J Delouis, JM Desert, FX Dolag, K Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Filliard, C Finelli, F Foley, S Forni, O Fosalba, P Fourmond, JJ Frailis, M Franceschi, E Galeotta, S Ganga, K Gavila, E Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Guyot, G Harrison, D Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Hoyland, RJ Huffenberger, KM Israelsson, U Jaffe, AH Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lamarre, JM Lami, P Lasenby, A Laureijs, RJ Lavabre, A Lawrence, CR Leach, S Lee, R Leonardi, R Leroy, C Lilje, PB Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maciaszek, T MacTavish, CJ Maffei, B Maino, D Mandolesi, N Mann, R Maris, M Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, P McGehee, P Meinhold, PR Melchiorri, A Melot, F Mendes, L Mennella, A Miville-Deschenes, MA Moneti, A Montier, L Mora, J Morgante, G Morisset, N Mortlock, D Munshi, D Murphy, A Naselsky, P Nash, A Natoli, P Netterfield, CB Novikov, D Novikov, I O'Dwyer, IJ Osborne, S Pajot, F Pasian, F Patanchon, G Pearson, D Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Plaszczynski, S Platania, P Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Prezeau, G Prina, M Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Schaefer, BM Scott, D Seiffert, MD Shellard, P Smoot, GF Starck, JL Stassi, P Stivoli, F Stolyarov, V Stompor, R Sudiwala, R Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Tristram, M Tuovinen, J Valenziano, L Vibert, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Watson, C White, SDM Wilkinson, A Wilson, P Yvon, D Zacchei, A Zhang, B Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Baker, M. Balbi, A. Banday, A. J. Barreiro, R. B. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bhandari, P. Bhatia, R. Bock, J. J. Bonaldi, A. Bond, J. R. Borders, J. Borrill, J. Bouchet, F. R. Bowman, B. Bradshaw, T. Breelle, E. Bucher, M. Burigana, C. Butler, R. C. Cabella, P. Camus, P. Cantalupo, C. M. Cappellini, B. Cardoso, J. -F. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chambelland, J. P. Charra, J. Charra, M. Chiang, L. -Y. Chiang, C. Christensen, P. R. Clements, D. L. Collaudin, B. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Crook, M. Cuttaia, F. Damasio, C. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dolag, K. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Filliard, C. Finelli, F. Foley, S. Forni, O. Fosalba, P. Fourmond, J. -J. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Gavila, E. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Guyot, G. Harrison, D. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Israelsson, U. Jaffe, A. H. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lami, P. Lasenby, A. Laureijs, R. J. Lavabre, A. Lawrence, C. R. Leach, S. Lee, R. Leonardi, R. Leroy, C. Lilje, P. B. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maciaszek, T. MacTavish, C. J. Maffei, B. Maino, D. Mandolesi, N. Mann, R. Maris, M. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. McGehee, P. Meinhold, P. R. Melchiorri, A. Melot, F. Mendes, L. Mennella, A. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Mora, J. Morgante, G. Morisset, N. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Nash, A. Natoli, P. Netterfield, C. B. Novikov, D. Novikov, I. O'Dwyer, I. J. Osborne, S. Pajot, F. Pasian, F. Patanchon, G. Pearson, D. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Plaszczynski, S. Platania, P. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Prezeau, G. Prina, M. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Schaefer, B. M. Scott, D. Seiffert, M. D. Shellard, P. Smoot, G. F. Starck, J. -L. Stassi, P. Stivoli, F. Stolyarov, V. Stompor, R. Sudiwala, R. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J. -P. Tristram, M. Tuovinen, J. Valenziano, L. Vibert, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Watson, C. White, S. D. M. Wilkinson, A. Wilson, P. Yvon, D. Zacchei, A. Zhang, B. Zonca, A. CA Planck Collaboration TI Planck early results. II. The thermal performance of Planck SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; space vehicles: instruments; instrumentation: detectors ID PRE-LAUNCH STATUS; HIGH-FREQUENCY INSTRUMENT; MISSION; DESIGN; ARCHITECTURE; CALIBRATION; SYSTEM; TESTS; 1ST AB The performance of the Planck instruments in space is enabled by their low operating temperatures, 20 K for LFI and 0.1 K for HFI, achieved through a combination of passive radiative cooling and three active mechanical coolers. The scientific requirement for very broad frequency coverage led to two detector technologies with widely different temperature and cooling needs. Active coolers could satisfy these needs; a helium cryostat, as used by previous cryogenic space missions (IRAS, COBE, ISO, Spitzer, AKARI), could not. Radiative cooling is provided by three V-groove radiators and a large telescope baffle. The active coolers are a hydrogen sorption cooler (<20 K), a He-4 Joule-Thomson cooler (4.7 K), and a He-3-He-4 dilution cooler (1.4 K and 0.1 K). The flight system was at ambient temperature at launch and cooled in space to operating conditions. The HFI bolometer plate reached 93 mK on 3 July 2009, 50 days after launch. The solar panel always faces the Sun, shadowing the rest of Planck, and operates at a mean temperature of 384 K. At the other end of the spacecraft, the telescope baffle operates at 42.3 K and the telescope primary mirror operates at 35.9 K. The temperatures of key parts of the instruments are stabilized by both active and passive methods. Temperature fluctuations are driven by changes in the distance from the Sun, sorption cooler cycling and fluctuations in gas-liquid flow, and fluctuations in cosmic ray flux on the dilution and bolometer plates. These fluctuations do not compromise the science data. C1 [Bhandari, P.; Bock, J. J.; Borders, J.; Bowman, B.; Chambelland, J. P.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Israelsson, U.; Keskitalo, R.; Lawrence, C. R.; Lee, R.; Mora, J.; Nash, A.; O'Dwyer, I. J.; Pearson, D.; Prezeau, G.; Prina, M.; Rocha, G.; Seiffert, M. D.; Wade, L. A.; Wilson, P.; Zhang, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana, Sci Data Ctr, Frascati, Italy. [Breelle, E.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.; Stompor, R.] Univ Paris 07, CNRS, UMR 7164, Paris, France. [Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile. [Bond, J. 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C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Smoot, G. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Leonardi, R.; Lubin, P. M.; Meinhold, P. R.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Natoli, P.] Univ Ferrara, Dipartmento Fis, I-44100 Ferrara, Italy. [Balbi, A.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartmento Fis, Rome, Italy. 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[Aghanim, N.; Aumont, J.; Charra, J.; Charra, M.; Douspis, M.; Fourmond, J. -J.; Lagache, G.; Lami, P.; Leroy, C.; Miville-Deschenes, M. -A.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Torre, J. -P.; Vibert, L.] Univ Paris 11, CNRS, UMR 8617, Inst Astrophys Spatiale, F-91405 Orsay, France. [Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, Paris, France. [Fosalba, P.] Fac Ciencies, CSIC IEEC, Inst Ciencies Espai, Bellaterra 08193, Spain. [Chiang, L. -Y.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Donzelli, S.; Eriksen, H. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Hildebrandt, S. R.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. 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EM charles.r.lawrence@jpl.nasa.gov RI Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Fosalba Vela, Pablo/I-5515-2016; Novikov, Igor/N-5098-2015; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Collaudin, Bernard/H-7149-2015; Lilje, Per/A-2699-2012; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Vielva, Patricio/F-6745-2014; Butler, Reginald/N-4647-2015 OI Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; Melchiorri, Alessandro/0000-0001-5326-6003; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Collaudin, Bernard/0000-0003-0114-3014; de Gasperis, Giancarlo/0000-0003-2899-2171; Vielva, Patricio/0000-0003-0051-272X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Savini, Giorgio/0000-0003-4449-9416; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115; Matarrese, Sabino/0000-0002-2573-1243; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996 FU CNES; CNRS/INSU-IN2P3; ASI; ESA; CNRS/INSU-IN2P3-INP (France); CNR; INAF (Italy); NASA; DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU) FX Planck is too large a project to allow full acknowledgement of all contributions by individuals, institutions, industries, and funding agencies. The main entities involved in the mission operations are as follows. The European Space Agency operates the satellite via its Mission Operations Centre located at ESOC (Darmstadt, Germany) and coordinates scientific operations via the Planck Science Office located at ESAC (Madrid, Spain). Two Consortia, comprising around 50 scientific institutes within Europe, the USA, and Canada, and funded by agencies from the participating countries, developed the scientific instruments LFI and HFI, and continue to operate them via Instrument Operations Teams located in Trieste (Italy) and Orsay (France). The Consortia are also responsible for scientific processing of the acquired data. The Consortia are led by the Principal Investigators: J.-L. Puget in France for HFI (funded principally by CNES and CNRS/INSU-IN2P3) and N. Mandolesi in Italy for LFI (funded principally via ASI). NASA's US Planck Project, based at JPL and involving scientists at many US institutions, contributes significantly to the efforts of these two Consortia. A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at (http://www.rssd.esa.int/index.php?project=PLANCK&page=Planck_Collaborat ion). The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). We acknowledge the use of thermal models from Thales for the payload, IAS for the HFI, JPL for the sorption cooler, and Laben for the LFI. Some of the results in this paper have been derived using the HEALPix package (Gorski et al. 2005). The HFI team wishes to thank warmly the Herschel-Planck project team under the leadership of Thomas Passvogel for their time, effort, and competence in solving the crises following failures of several parts of the cyrochain during Planck system tests. We acknowledge very useful discussions on the thermal behaviour of Planck during the system tests from the CSL team, who went far beyond their formal responsibilities. NR 54 TC 69 Z9 69 U1 1 U2 20 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A2 DI 10.1051/0004-6361/201116486 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100003 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartelmann, M Bartlett, JG Battaner, E Battye, R Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Brown, ML Bucher, M Burigana, C Cabella, P Cantalupo, CM Cardoso, JF Carvalho, P Catalano, A Cayon, L Challinor, A Chamballu, A Chary, RR Chiang, LY Chiang, C Chon, G Christensen, PR Churazov, E Clements, DL Colafrancesco, S Colombi, S Couchot, F Coulais, A Crill, BP Cuttaia, F Da Silva, A Dahle, H Danese, L Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dickinson, C Diego, JM Dolag, K Dole, H Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Eisenhardt, P Ensslin, TA Feroz, F Finelli, F Flores-Cacho, I Forni, O Fosalba, P Frailis, M Franceschi, E Fromenteau, S Galeotta, S Ganga, K Genova-Santos, RT Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gonzalez-Riestra, R Gorski, KM Grainge, KJB Gratton, S Gregorio, A Gruppuso, A Harrison, D Heinamaki, P Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Hurier, G Hurley-Walker, N Jaffe, AH Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Le Jeune, M Leach, S Leonardi, R Li, C Liddle, A Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Maffei, B Maino, D Mandolesi, N Mann, R Maris, M Marleau, F Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, P Mei, S Meinhold, PR Melchiorri, A Melin, JB Mendes, L Mennella, A Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Olamaie, M Osborne, S Pajot, F Pasian, F Patanchon, G Pearson, TJ Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Piffaretti, R Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rubino-Martin, JA Rusholme, B Saar, E Sandri, M Santos, D Saunders, RDE Savini, G Schaefer, BM Scott, D Seiffert, MD Shellard, P Smoot, GF Stanford, A Starck, JL Stivoli, F Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sutton, D Sygnet, JF Taburet, N Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Tristram, M Tuovinen, J Valenziano, L Vibert, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Weller, J White, SDM White, M Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartelmann, M. Bartlett, J. G. Battaner, E. Battye, R. Benabed, K. Benoit, A. Bernard, J-P Bersanelli, M. Bhatia, R. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Brown, M. L. Bucher, M. Burigana, C. Cabella, P. Cantalupo, C. M. Cardoso, J-F Carvalho, P. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chary, R-R Chiang, L-Y Chiang, C. Chon, G. Christensen, P. R. Churazov, E. Clements, D. L. Colafrancesco, S. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Cuttaia, F. Da Silva, A. Dahle, H. Danese, L. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J-M Desert, F-X Dickinson, C. Diego, J. M. Dolag, K. Dole, H. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Eisenhardt, P. Ensslin, T. A. Feroz, F. Finelli, F. Flores-Cacho, I. Forni, O. Fosalba, P. Frailis, M. Franceschi, E. Fromenteau, S. Galeotta, S. Ganga, K. Genova-Santos, R. T. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gonzalez-Riestra, R. Gorski, K. M. Grainge, K. J. B. Gratton, S. Gregorio, A. Gruppuso, A. Harrison, D. Heinamaki, P. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Hurier, G. Hurley-Walker, N. Jaffe, A. H. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Lamarre, J-M Lasenby, A. Laureijs, R. J. Lawrence, C. R. Le Jeune, M. Leach, S. Leonardi, R. Li, C. Liddle, A. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Maino, D. Mandolesi, N. Mann, R. Maris, M. Marleau, F. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. Mei, S. Meinhold, P. R. Melchiorri, A. Melin, J-B Mendes, L. Mennella, A. Mitra, S. Miville-Deschenes, M-A Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Olamaie, M. Osborne, S. Pajot, F. Pasian, F. Patanchon, G. Pearson, T. J. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Piffaretti, R. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J-L Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rubino-Martin, J. A. Rusholme, B. Saar, E. Sandri, M. Santos, D. Saunders, R. D. E. Savini, G. Schaefer, B. M. Scott, D. Seiffert, M. D. Shellard, P. Smoot, G. F. Stanford, A. Starck, J-L Stivoli, F. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sutton, D. Sygnet, J-F Taburet, N. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J-P Tristram, M. Tuovinen, J. Valenziano, L. Vibert, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Weller, J. White, S. D. M. White, M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. VIII. The all-sky early Sunyaev-Zeldovich cluster sample SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; galaxies: clusters: general; catalogs ID SOUTH-POLE TELESCOPE; X-RAY-PROPERTIES; MICROWAVE BACKGROUND TEMPERATURE; CORONA BOREALIS SUPERCLUSTER; MASSIVE GALAXY CLUSTERS; COSMIC DISTANCE SCALE; COSMOLOGICAL PARAMETERS; HYDRODYNAMICAL SIMULATIONS; NEARBY CLUSTERS; HUBBLE CONSTANT AB We present the first all-sky sample of galaxy clusters detected blindly by the Planck satellite through the Sunyaev-Zeldovich (SZ) effect from its six highest frequencies. This early SZ (ESZ) sample is comprised of 189 candidates, which have a high signal-to-noise ratio ranging from 6 to 29. Its high reliability (purity above 95%) is further ensured by an extensive validation process based on Planck internal quality assessments and by external cross-identification and follow-up observations. Planck provides the first measured SZ signal for about 80% of the 169 previously-known ESZ clusters. Planck furthermore releases 30 new cluster candidates, amongst which 20 meet the ESZ signal-to-noise selection criterion. At the submission date, twelve of the 20 ESZ candidates were confirmed as new clusters, with eleven confirmed using XMM-Newton snapshot observations, most of them with disturbed morphologies and low luminosities. The ESZ clusters are mostly at moderate redshifts (86% with z below 0.3) and span more than a decade in mass, up to the rarest and most massive clusters with masses above 1 x 10(15) M-circle dot. 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EM marian.douspis@ias.u-psud.fr RI Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015; Pearson, Timothy/N-2376-2015; Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Fosalba Vela, Pablo/I-5515-2016; Novikov, Igor/N-5098-2015; Nati, Federico/I-4469-2016; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Lilje, Per/A-2699-2012; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Churazov, Eugene/A-7783-2013; Hurley-Walker, Natasha/B-9520-2013; Lopez-Caniego, Marcos/M-4695-2013; Da Silva, Antonio/A-2693-2010; Bartelmann, Matthias/A-5336-2014; Bouchet, Francois/B-5202-2014; Vielva, Patricio/F-6745-2014; OI Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; Melchiorri, Alessandro/0000-0001-5326-6003; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Zonca, Andrea/0000-0001-6841-1058; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070; Pearson, Timothy/0000-0001-5213-6231; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Nati, Federico/0000-0002-8307-5088; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; de Gasperis, Giancarlo/0000-0003-2899-2171; Hurley-Walker, Natasha/0000-0002-5119-4808; Da Silva, Antonio/0000-0002-6385-1609; Vielva, Patricio/0000-0003-0051-272X; Pierpaoli, Elena/0000-0002-7957-8993; Hurier, Guillaume/0000-0002-1215-0706; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Savini, Giorgio/0000-0003-4449-9416; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Weller, Jochen/0000-0002-8282-2010; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269 FU National Aeronautics and Space Administration; Centre National d'Etudes Spatiales (CNES) FX The authors thank N. Schartel, ESA XMM-Newton project scientist, for granting the Director Discretionary Time used for confirmation of SZ Planck candidates. This research has made use of the following databases: SIMBAD, operated at CDS, Strasbourg, France; the NED database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; BAX, operated by the Laboratoire d'Astrophysique de Tarbes-Toulouse (LATT), under contract with the Centre National d'Etudes Spatiales (CNES), SZ repository operated by IAS Data and Operation Center (IDOC) under contract with CNES. The authors acknowledge the use of software provided by the US National Virtual Observatory. A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.rssd.esa.int/Planck. NR 135 TC 236 Z9 237 U1 4 U2 37 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A8 DI 10.1051/0004-6361/201116459 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100009 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Baker, M Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Bennett, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Bradshaw, T Bremer, M Bucher, M Burigana, C Butler, RC Cabella, P Cantalupo, CM Cappellini, B Cardoso, JF Carr, R Casale, M Catalano, A Cayon, L Challinor, A Chamballu, A Charra, J Chary, RR Chiang, LY Chiang, C Christensen, PR Clements, DL Colombi, S Couchot, F Coulais, A Crill, BP Crone, G Crook, M Cuttaia, F Danese, L D'Arcangelo, O Davies, RD Davis, RJ de Bernardis, P de Bruin, J de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dick, J Dickinson, C Dolag, K Dole, H Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Foley, S Forni, O Fosalba, P Frailis, M Franceschi, E Freschi, M Gaier, TC Galeotta, S Gallegos, J Gandolfo, B Ganga, K Giard, M Giardino, G Gienger, G Giraud-Heraud, Y Gonzalez, J Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Guyot, G Haissinski, J Hansen, FK Harrison, D Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Hoyland, RJ Huffenberger, KM Jaffe, AH Jagemann, T Jones, WC Juillet, JJ Juvela, M Kangaslahti, P Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Krassenburg, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lange, AE Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leahy, JP Leonardi, R Leroy, C Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lowe, S Lubin, PM Macias-Perez, JF Maciaszek, T MacTavish, CJ Maffei, B Maino, D Mandolesi, N Mann, R Maris, M Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P McDonald, A McGehee, P Meinhold, PR Melchiorri, A Melin, JB Mendes, L Mennella, A Mevi, C Miniscalco, R Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Morisset, N Mortlock, D Munshi, D Murphy, A Naselsky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I O'Dwyer, IJ Ortiz, I Osborne, S Osuna, P Oxborrow, CA Pajot, F Paladini, R Partridge, B Pasian, F Passvogel, T Patanchon, G Pearson, D Pearson, TJ Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Plaszczynski, S Platania, P Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Reix, JM Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Salerno, E Sandri, M Santos, D Savini, G Schaefer, BM Scott, D Seiffert, MD Shellard, P Simonetto, A Smoot, GF Sozzi, C Starck, JL Sternberg, J Stivoli, F Stolyarov, V Stompor, R Stringhetti, L Sudiwala, R Sunyaev, R Sygnet, JF Tapiador, D Tauber, JA Tavagnacco, D Taylor, D Terenzi, L Texier, D Toffolatti, L Tomasi, M Torre, JP Tristram, M Tuovinen, J Turler, M Tuttlebee, M Umana, G Valenziano, L Valiviita, J Varis, J Vibert, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Watson, C White, SDM White, M Wilkinson, A Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Baker, M. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Bennett, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bhatia, R. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Bradshaw, T. Bremer, M. Bucher, M. Burigana, C. Butler, R. C. Cabella, P. Cantalupo, C. M. Cappellini, B. Cardoso, J. -F. Carr, R. Casale, M. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Charra, J. Chary, R. -R. Chiang, L. -Y. Chiang, C. Christensen, P. R. Clements, D. L. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Crone, G. Crook, M. Cuttaia, F. Danese, L. D'Arcangelo, O. Davies, R. D. Davis, R. J. de Bernardis, P. de Bruin, J. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dick, J. Dickinson, C. Dolag, K. Dole, H. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Foley, S. Forni, O. Fosalba, P. Frailis, M. Franceschi, E. Freschi, M. Gaier, T. C. Galeotta, S. Gallegos, J. Gandolfo, B. Ganga, K. Giard, M. Giardino, G. Gienger, G. Giraud-Heraud, Y. Gonzalez, J. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Guyot, G. Haissinski, J. Hansen, F. K. Harrison, D. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Jaffe, A. H. Jagemann, T. Jones, W. C. Juillet, J. J. Juvela, M. Kangaslahti, P. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Krassenburg, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lange, A. E. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leahy, J. P. Leonardi, R. Leroy, C. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lowe, S. Lubin, P. M. Macias-Perez, J. F. Maciaszek, T. MacTavish, C. J. Maffei, B. Maino, D. Mandolesi, N. Mann, R. Maris, M. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. McDonald, A. McGehee, P. Meinhold, P. R. Melchiorri, A. Melin, J. -B. Mendes, L. Mennella, A. Mevi, C. Miniscalco, R. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Morisset, N. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. O'Dwyer, I. J. Ortiz, I. Osborne, S. Osuna, P. Oxborrow, C. A. Pajot, F. Paladini, R. Partridge, B. Pasian, F. Passvogel, T. Patanchon, G. Pearson, D. Pearson, T. J. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Plaszczynski, S. Platania, P. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Reix, J. -M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Salerno, E. Sandri, M. Santos, D. Savini, G. Schaefer, B. M. Scott, D. Seiffert, M. D. Shellard, P. Simonetto, A. Smoot, G. F. Sozzi, C. Starck, J. -L. Sternberg, J. Stivoli, F. Stolyarov, V. Stompor, R. Stringhetti, L. Sudiwala, R. Sunyaev, R. Sygnet, J. -F. Tapiador, D. Tauber, J. A. Tavagnacco, D. Taylor, D. Terenzi, L. Texier, D. Toffolatti, L. Tomasi, M. Torre, J. -P. Tristram, M. Tuovinen, J. Tuerler, M. Tuttlebee, M. Umana, G. Valenziano, L. Valiviita, J. Varis, J. Vibert, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Watson, C. White, S. D. M. White, M. Wilkinson, A. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. I. The Planck mission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; cosmic background radiation; surveys; space vehicles: instruments; instrumentation: detectors; catalogs ID PRE-LAUNCH STATUS AB The European Space Agency's Planck satellite was launched on 14 May 2009, and has been surveying the sky stably and continuously since 13 August 2009. Its performance is well in line with expectations, and it will continue to gather scientific data until the end of its cryogenic lifetime. We give an overview of the history of Planck in its first year of operations, and describe some of the key performance aspects of the satellite. This paper is part of a package submitted in conjunction with Planck's Early Release Compact Source Catalogue, the first data product based on Planck to be released publicly. The package describes the scientific performance of the Planck payload, and presents results on a variety of astrophysical topics related to the sources included in the Catalogue, as well as selected topics on diffuse emission. C1 [Bennett, K.; Bremer, M.; Crone, G.; Giardino, G.; Krassenburg, M.; Laureijs, R. J.; Leonardi, R.; Passvogel, T.; Sternberg, J.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, ESRIN, Frascati, Italy. [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.; Stompor, R.] Univ Paris 07, CNRS, UMR7164, Paris, France. [Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. 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EM jtauber@rssd.esa.int RI Butler, Reginald/N-4647-2015; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; Lilje, Per/A-2699-2012; Salerno, Emanuele/A-2137-2010; de Gasperis, Giancarlo/C-8534-2012; Sozzi, Carlo/F-4158-2012; Gregorio, Anna/J-1632-2012; Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Lahteenmaki, Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015; Pearson, Timothy/N-2376-2015; Gruppuso, Alessandro/N-5592-2015; Valiviita, Jussi/A-9058-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Fosalba Vela, Pablo/I-5515-2016; Novikov, Igor/N-5098-2015 OI Zonca, Andrea/0000-0001-6841-1058; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Lowe, Stuart/0000-0002-2975-9032; Stringhetti, Luca/0000-0002-3961-9068; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115; Lilje, Per/0000-0003-4324-7794; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Masi, Silvia/0000-0001-5105-1439; Melchiorri, Alessandro/0000-0001-5326-6003; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Salerno, Emanuele/0000-0002-3433-3634; de Gasperis, Giancarlo/0000-0003-2899-2171; Sozzi, Carlo/0000-0001-8951-0071; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070; Pearson, Timothy/0000-0001-5213-6231; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; FU CNES; CNRS/INSU-IN2P3; ASI; Danish Natural Research Council; ESA; CNRS/INSU-IN2P3-INP (France); CNR; INAF (Italy); NASA; DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU) FX Planck is too large a project to allow full acknowledgement of all contributions by individuals, institutions, industries, and funding agencies. The main entities involved in the mission operations are as follows. The European Space Agency operates the satellite via its Mission Operations Centre located at ESOC (Darmstadt, Germany) and coordinates scientific operations via the Planck Science Office located at ESAC (Madrid, Spain). Two Consortia, comprising around 100 scientific institutes within Europe, the USA, and Canada, and funded by agencies from the participating countries, developed the scientific instruments LFI and HFI, and continue to operate them via Instrument Operations Teams located in Trieste (Italy) and Orsay (France). The Consortia are also responsible for scientific processing of the acquired data. The Consortia are led by the Principal Investigators: J.-L. Puget in France for HFI (funded principally by CNES and CNRS/INSU-IN2P3) and N. Mandolesi in Italy for LFI (funded principally via ASI). NASA's US Planck Project, based at JPL and involving scientists at many US institutions, contributes significantly to the efforts of these two Consortia. A third Consortium, led by H. U. Norgaard-Nielsen and supported by the Danish Natural Research Council, contributed to the reflector programme. The author list for this paper has been selected by the Planck Science Team from the Planck Collaboration, and is composed of individuals from all of the above entities who have made multi-year contributions to the development of the mission. It does not pretend to be inclusive of all contributions. A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at (http://www.rssd.esa.int/index.php?project=PLANCK\&page=Planck_Collabora tion). The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). NR 34 TC 282 Z9 282 U1 3 U2 55 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A1 DI 10.1051/0004-6361/201116464 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100002 ER PT J AU Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartelmann, M Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Brown, ML Bucher, M Burigana, C Cabella, P Cantalupo, CM Cardoso, JF Carvalho, P Catalano, A Cayon, L Challinor, A Chamballu, A Chiang, LY Chon, G Christensen, PR Churazov, E Clements, DL Colafrancesco, S Colombi, S Couchot, F Coulais, A Crill, BP Cuttaia, F Da Silva, A Dahle, H Danese, L de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Diego, JM Dolag, K Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Finelli, F Flores-Cacho, I Forni, O Frailis, M Franceschi, E Fromenteau, S Galeotta, S Ganga, K Genova-Santos, RT Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gonzalez-Riestra, R Gorski, KM Gratton, S Gregorio, A Gruppuso, A Harrison, D Heinamaki, P Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Hoyland, RJ Huffenberger, KM Hurier, G Jaffe, AH Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knox, L Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Le Jeune, M Leach, S Leonardi, R Liddle, A Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Mann, R Maris, M Marleau, F Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, P Melchiorri, A Melin, JB Mendes, L Mennella, A Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, A Naselsky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Pajot, F Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Piffaretti, R Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rebolo, R Reinecke, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rubino-Martin, JA Rusholme, B Saar, E Sandri, M Santos, D Schaefer, BM Scott, D Seiffert, MD Smoot, GF Starck, JL Stivoli, F Stolyarov, V Sunyaev, R Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Torre, JP Tristram, M Tuovinen, J Valenziano, L Vibert, L Vielva, P Villa, F Vittorio, N Wandelt, BD White, SDM Yvon, D Zacchei, A Zonca, A AF Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartelmann, M. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J-P Bersanelli, M. Bhatia, R. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Brown, M. L. Bucher, M. Burigana, C. Cabella, P. Cantalupo, C. M. Cardoso, J-F Carvalho, P. Catalano, A. Cayon, L. Challinor, A. Chamballu, A. Chiang, L-Y Chon, G. Christensen, P. R. Churazov, E. Clements, D. L. Colafrancesco, S. Colombi, S. Couchot, F. Coulais, A. Crill, B. P. Cuttaia, F. Da Silva, A. Dahle, H. Danese, L. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J-M Desert, F-X Diego, J. M. Dolag, K. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Finelli, F. Flores-Cacho, I. Forni, O. Frailis, M. Franceschi, E. Fromenteau, S. Galeotta, S. Ganga, K. Genova-Santos, R. T. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gonzalez-Riestra, R. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Harrison, D. Heinamaki, P. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Hoyland, R. J. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knox, L. Kurki-Suonio, H. Lagache, G. Lamarre, J-M Lasenby, A. Laureijs, R. J. Lawrence, C. R. Le Jeune, M. Leach, S. Leonardi, R. Liddle, A. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Mann, R. Maris, M. Marleau, F. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. Melchiorri, A. Melin, J-B Mendes, L. Mennella, A. Mitra, S. Miville-Deschenes, M-A Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, A. Naselsky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Pajot, F. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Piffaretti, R. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J-L Rebolo, R. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rubino-Martin, J. A. Rusholme, B. Saar, E. Sandri, M. Santos, D. Schaefer, B. M. Scott, D. Seiffert, M. D. Smoot, G. F. Starck, J-L Stivoli, F. Stolyarov, V. Sunyaev, R. Sygnet, J-F Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Torre, J-P Tristram, M. Tuovinen, J. Valenziano, L. Vibert, L. Vielva, P. Villa, F. Vittorio, N. Wandelt, B. D. White, S. D. M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. IX. XMM-Newton follow-up for validation of Planck cluster candidates SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; galaxies: clusters: general; galaxies: clusters: intracluster medium; cosmic background radiation; X-rays: galaxies: clusters ID PRE-LAUNCH STATUS; X-RAY-PROPERTIES; STRUCTURE SURVEY REXCESS; MASSIVE GALAXY CLUSTERS; PHOTON IMAGING CAMERA; REPRESENTATIVE SAMPLE; SCALING RELATIONS; BACKGROUND MAPS; CATALOG; PROFILES AB We present the XMM-Newton follow-up for confirmation of Planck cluster candidates. Twenty-five candidates have been observed to date using snapshot (similar to 10 ks) exposures, ten as part of a pilot programme to sample a low range of signal-to-noise ratios (4 < S/N < 6), and a further 15 in a programme to observe a sample of S/N > 5 candidates. The sensitivity and spatial resolution of XMM-Newton allows unambiguous discrimination between clusters and false candidates. The 4 false candidates have S/N <= 4.1. A total of 21 candidates are confirmed as extended X-ray sources. Seventeen are single clusters, the majority of which are found to have highly irregular and disturbed morphologies (about similar to 70%). The remaining four sources are multiple systems, including the unexpected discovery of a supercluster at z = 0.45. For 20 sources we are able to derive a redshift estimate from the X-ray Fe K line (albeit of variable quality). The new clusters span the redshift range 0.09 less than or similar to z less than or similar to 0.54, with a median redshift of z similar to 0.37. A first determination is made of their X-ray properties including the characteristic size, which is used to improve the estimate of the SZ Compton parameter, Y-500. The follow-up validation programme has helped to optimise the Planck candidate selection process. It has also provided a preview of the X-ray properties of these newly-discovered clusters, allowing comparison with their SZ properties, and to the X-ray and SZ properties of known clusters observed in the Planck survey. Our results suggest that Planck may have started to reveal a non-negligible population of massive dynamically perturbed objects that is under-represented in X-ray surveys. However, despite their particular properties, these new clusters appear to follow the Y-500-Y-X relation established for X-ray selected objects, where Y-X is the product of the gas mass and temperature. C1 [Banday, A. J.; Bernard, J-P; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Poutanen, T.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Bartlett, J. 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EM etienne.pointecouteau@irap.omp.eu RI Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Piacentini, Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; Herranz, Diego/K-9143-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Churazov, Eugene/A-7783-2013; Lopez-Caniego, Marcos/M-4695-2013; Da Silva, Antonio/A-2693-2010; Bartelmann, Matthias/A-5336-2014; Bouchet, Francois/B-5202-2014; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; OI Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; Hurier, Guillaume/0000-0002-1215-0706; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Pierpaoli, Elena/0000-0002-7957-8993; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272; de Gasperis, Giancarlo/0000-0003-2899-2171; Da Silva, Antonio/0000-0002-6385-1609; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Melchiorri, Alessandro/0000-0001-5326-6003; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243 FU ESA; NASA (USA); CNES; CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy); NASA; DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU) FX The Planck Collaboration thanks Norbert Schartel for his support to the validation process and granting discretionary time for the observation of Planck cluster candidates. The present work is based: on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA); and on observations made with the IAC80 telescope operated on the island of Tenerife by the Instituto de Astrofisica de Canarias (IAC) in the Spanish Observatorio del Teide. This research has made use of the following databases: SIMBAD, operated at CDS, Strasbourg, France; the NED database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; BAX, which is operated by the Laboratoire d'Astrophysique de Tarbes-Toulouse (LATT), under contract with the Centre National d'Etudes Spatiales (CNES); and the SZ repository operated by IAS Data and Operation Center (IDOC) under contract with CNES. A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.rssd.esa.int/Planck_Collaboration. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). NR 85 TC 93 Z9 93 U1 0 U2 10 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 DEC PY 2011 VL 536 AR A9 DI 10.1051/0004-6361/201116460 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100010 ER PT J AU Aghanim, N Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bhatia, R Bohringer, H Bonaldi, A Bond, JR Borgani, S Borrill, J Bouchet, FR Brown, ML Burigana, C Cabella, P Cantalupo, CM Cappellini, B Carvalho, P Catalano, A Cayon, L Chiang, LY Chiang, C Chon, G Christensen, PR Churazov, E Clements, DL Colafrancesco, S Colombi, S Crill, BP Cuttaia, F Da Silva, A Dahle, H Danese, L D'Arcangelo, O Davis, RJ de Bernardis, P de Gasperis, G de Zotti, G Delabrouille, J Delouis, JM Democles, J Desert, FX Dickinson, C Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Flores-Cacho, I Forni, O Fosalba, P Frailis, M Franceschi, E Fromenteau, S Galeotta, S Ganga, K Genova-Santos, RT Giard, M Gonzalez-Nuevo, J Gonzalez-Riestra, R Gorski, KM Gregorio, A Gruppuso, A Hansen, FK Harrison, D Heinamaki, P Hernandez-Monteagudo, C Hildebrandt, SR Hivon, E Hobson, M Hurier, G Jaffe, AH Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lawrence, CR Le Jeune, M Leach, S Leonardi, R Leroy, C Liddle, A Lilje, PB Lopez-Caniego, M Luzzi, G Macias-Perez, JF Maino, D Mandolesi, N Marleau, F Martinez-Gonzalez, E Masi, S Matarrese, S Mazzotta, P Meinhold, PR Melchiorri, A Melin, JB Mendes, L Mennella, A Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Naselsky, P Natoli, P Nevalainen, J Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I O'Dwyer, IJ Osborne, S Paladini, R Pasian, F Patanchon, G Pearson, TJ Perdereau, O Perotto, L Perrotta, F Piacentini, F Pierpaoli, E Piffaretti, R Platania, P Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rubino-Martin, JA Saar, E Sandri, M Savini, G Schaefer, BM Scott, D Smoot, GF Starck, JL Sutton, D Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Turler, M Valenziano, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Weller, J White, SDM White, M Yvon, D Zacchei, A Zonca, A AF Aghanim, N. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bhatia, R. Boehringer, H. Bonaldi, A. Bond, J. R. Borgani, S. Borrill, J. Bouchet, F. R. Brown, M. L. Burigana, C. Cabella, P. Cantalupo, C. M. Cappellini, B. Carvalho, P. Catalano, A. Cayon, L. Chiang, L. -Y. Chiang, C. Chon, G. Christensen, P. R. Churazov, E. Clements, D. L. Colafrancesco, S. Colombi, S. Crill, B. P. Cuttaia, F. Da Silva, A. Dahle, H. Danese, L. D'Arcangelo, O. Davis, R. J. de Bernardis, P. de Gasperis, G. de Zotti, G. Delabrouille, J. Delouis, J. -M. Democles, J. Desert, F. -X. Dickinson, C. Diego, J. M. Dole, H. Donzelli, S. Dore, O. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Flores-Cacho, I. Forni, O. Fosalba, P. Frailis, M. Franceschi, E. Fromenteau, S. Galeotta, S. Ganga, K. Genova-Santos, R. T. Giard, M. Gonzalez-Nuevo, J. Gonzalez-Riestra, R. Gorski, K. M. Gregorio, A. Gruppuso, A. Hansen, F. K. Harrison, D. Heinamaki, P. Hernandez-Monteagudo, C. Hildebrandt, S. R. Hivon, E. Hobson, M. Hurier, G. Jaffe, A. H. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lawrence, C. R. Le Jeune, M. Leach, S. Leonardi, R. Leroy, C. Liddle, A. Lilje, P. B. Lopez-Caniego, M. Luzzi, G. Macias-Perez, J. F. Maino, D. Mandolesi, N. Marleau, F. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Mazzotta, P. Meinhold, P. R. Melchiorri, A. Melin, J. -B. Mendes, L. Mennella, A. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Naselsky, P. Natoli, P. Nevalainen, J. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. O'Dwyer, I. J. Osborne, S. Paladini, R. Pasian, F. Patanchon, G. Pearson, T. J. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Pierpaoli, E. Piffaretti, R. Platania, P. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rubino-Martin, J. A. Saar, E. Sandri, M. Savini, G. Schaefer, B. M. Scott, D. Smoot, G. F. Starck, J. -L. Sutton, D. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tuerler, M. Valenziano, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Weller, J. White, S. D. M. White, M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck early results. XXVI. Detection with Planck and confirmation by XMM-Newton of PLCK G266.6-27.3, an exceptionally X-ray luminous and massive galaxy cluster at z similar to 1 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; galaxies: clusters: general; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters; cosmic background radiation ID STRUCTURE SURVEY REXCESS; PHOTON IMAGING CAMERA; SOUTH-POLE TELESCOPE; REPRESENTATIVE SAMPLE; SCALING RELATIONS; SKY SURVEY; DISCOVERY; PROFILES; CATALOG AB We present first results on PLCK G266.6-27.3, a galaxy cluster candidate detected at a signal-to-noise ratio of 5 in the Planck All Sky survey. An XMM-Newton validation observation has allowed us to confirm that the candidate is a bona fide galaxy cluster. With these X-ray data we measure an accurate redshift, z = 0.94 +/- 0.02, and estimate the cluster mass to be M-500 = (7.8 +/- 0.8) x 10(14) M-circle dot. PLCK G266.6-27.3 is an exceptional system: its luminosity of L-X[0.5-2.0 keV] = (1.4 +/- 0.05) x 10(45) erg s(-1) equals that of the two most luminous known clusters in the z > 0.5 universe, and it is one of the most massive clusters at z similar to 1. Moreover, unlike the majority of high-redshift clusters, PLCK G266.6-27.3 appears to be highly relaxed. This observation confirms Planck's capability of detecting high-redshift, high-mass clusters, and opens the way to the systematic study of population evolution in the exponential tail of the mass function. C1 [Arnaud, M.; Democles, J.; Piffaretti, R.; Pratt, G. W.; Starck, J. -L.] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM,IRFU,Serv Astrophys,CEA,DSM, F-91191 Gif Sur Yvette, France. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Bartlett, J. 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EM monique.arnaud@cea.fr RI Mazzotta, Pasquale/B-1225-2016; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015; Pearson, Timothy/N-2376-2015; Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Fosalba Vela, Pablo/I-5515-2016; Novikov, Igor/N-5098-2015; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Novikov, Dmitry/P-1807-2015; Lahteenmaki, Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Lilje, Per/A-2699-2012; de Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Churazov, Eugene/A-7783-2013; Lopez-Caniego, Marcos/M-4695-2013; Da Silva, Antonio/A-2693-2010; Bouchet, Francois/B-5202-2014; OI Pierpaoli, Elena/0000-0002-7957-8993; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Matarrese, Sabino/0000-0002-2573-1243; Masi, Silvia/0000-0001-5105-1439; Melchiorri, Alessandro/0000-0001-5326-6003; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070; Pearson, Timothy/0000-0001-5213-6231; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Barreiro, Rita Belen/0000-0002-6139-4272; de Gasperis, Giancarlo/0000-0003-2899-2171; Da Silva, Antonio/0000-0002-6385-1609; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Hurier, Guillaume/0000-0002-1215-0706; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Savini, Giorgio/0000-0003-4449-9416; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Borgani, Stefano/0000-0001-6151-6439; Galeotta, Samuele/0000-0002-3748-5115 FU ESA Member States; USA (NASA); ESA; CNES; CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy); NASA; DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU) FX The Planck Collaboration thanks Norbert Schartel for his support of the validation process and for granting discretionary time for the observation of Planck cluster candidates. The present work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). This research has made use of the following databases: SIMBAD, operated at the CDS, Strasbourg, France; the NED database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; BAX, which is operated by the Laboratoire d'Astrophysique de Tarbes-Toulouse (LATT), under contract with the Centre National d'Etudes Spatiales (CNES); and the SZ repository operated by IAS Data and Operation Center (IDOC) under contract with CNES. A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.rssd.esa.int/Planck_Collaboration. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). NR 60 TC 64 Z9 64 U1 0 U2 21 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2011 VL 536 AR A26 DI 10.1051/0004-6361/201117430 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867WI UT WOS:000298485100027 ER EF